Astronomy amp Astrophysics manuscript no ms_printer_v11 ccopyESO 2018September 26 2018

A VST and VISTA study of globular clusters in NGC 253Michele Cantiello1Aniello Grado2 Marina Rejkuba3 Magda Arnaboldi3 Massimo Capaccioli4 Laura Greggio5

Enrica Iodice2 and Luca Limatola2

1 INAF Osservatorio Astronomico di Teramo via Maggini I-64100 Teramo Italy e-mail cantiellooa-teramoinafit2 INAF Osservatorio Astronomico di Capodimonte Napoli Salita Moiariello I-80131 Napoli Italy3 European Southern Observatory Karl-Schwarzschild-Str 2 D-85748 Garching bei Muumlnchen Germany4 Dip di Fisica Universitaacute di Napoli Federico II CU di Monte SantrsquoAngelo Via Cintia I-80126 Napoli Italy5 INAF Osservatorio Astronomico di Padova Vicolo dellrsquoOsservatorio 5 I-35122 Padova Italy

Received accepted

ABSTRACT

Context Globular clusters (GCs) are key to our understanding of the Universe as laboratories of stellar evolution fossil tracers of thepast formation epoch of the host galaxy and effective distance indicators from local to cosmological scalesAims We analyze the properties of the sources in the NGC 253 with the aim of defining an up to date catalog of GC candidatesin the galaxy Given the distance of the galaxy GCs in NGC 253 are ideal targets for resolved color-magnitude diagram studies ofextragalactic GCs with next-generation diffraction limited ground-based telescopesMethods Our analysis is based on the science verification data of two ESO survey telescopes VST and VISTA Using ugri photom-etry from VST and JKs from VISTA GC candidates were selected using as reference the morpho-photometric and color propertiesof spectroscopically confirmed GCs available in the literature The strength of the results was verified against available archivalHSTACS data from the GHOSTS survey all but two of the selected GC candidates appear as star clusters in HST footprintsResults The adopted GC selection leads to the definition of a sample of sim 350 GC candidates At visual inspection we find that82 objects match all the requirements for selecting GC candidates and 155 are flagged as uncertain GC candidate however 110 areunlikely GCs which are most likely background galaxies Furthermore our analysis shows that four of the previously spectroscopi-cally confirmed GCs ie sim 20 of the total spectroscopic sample are more likely either background galaxies or high-velocity MilkyWay stars The radial density profile of the selected best candidates shows the typically observed r14-law radial profile The analysisof the color distributions reveals only marginal evidence of the presence of color bimodality which is normally observed in galaxiesof similar luminosity The GC luminosity function does not show the typical symmetry mainly because of the lack of bright GCsPart of the bright GCs missing might be at very large galactocentric distances or along the line of sight of the galaxy dusty disk Asan alternative possibility we speculate that a fraction of low luminosity GC candidates might instead be metal-rich intermediate ageclusters but fall in a similar color interval of old metal-poor GCsConclusions Defining a contaminant-free sample of GCs in extragalactic systems is not a straight forward exercise Using opticaland near-IR photometry we purged the list of GCs with spectroscopic membership and photometric GC candidates in NGC 253 Ourresults show that the use of either spectroscopic or photometric data only does not generally ensure a contaminant-free sample and acombination of both spectroscopy and photometry is preferred

Key words galaxies star clusters general ndash galaxies individual NGC 253 ndash galaxies stellar content ndash galaxies evolution ndash galaxiesphotometry ndash catalogs

1 Introduction

Globular clusters (GCs) are a key tool for understanding the for-mation and evolution of galaxies (Harris 2001 Brodie amp Strader2006 Peng et al 2008 Georgiev et al 2010 Harris et al 2013Durrell et al 2014)

Extragalactic unresolved GCs are possibly the simplest classof astrophysical objects beyond stars as to a first approximationthey host a simple single age and single metallicity stellar popu-lation Nevertheless in the last decade such a classical paradigmhas been demonstrated as invalid for a fraction of Milky Way(MW) GCs and for some of the clusters in the Magellanic Clouds(Gratton et al 2004 Piotto et al 2007 Carretta et al 2009) In

This work is based on observations taken at the ESO La SillaParanal Observatory within the VST Science Verification ProgrammeID 60A-9286(A) and VISTA Science Verification Programme ID 60A-9285(A)

spite of that doubtless GCs are the simplest stellar aggregates tobe found in galaxies

Two other properties make GCs very useful for extragalacticstudies old age and high luminosity In the few galaxies beyondthe MW where spectroscopic or multiband photometric studiesof the GCs have been carried out the results almost uniformlyrevealed a population with mean ages comparable to the GC sys-tem of the MW older than sim10 Gyr (eg Cohen et al 19982003 Strader et al 2005 Chies-Santos et al 2011) This makesGCs fossil tracers of the formation of the host galaxy In addi-tion extragalactic GCs appear as bright clumps of light on theotherwise smooth light profile of the galaxy and under typicalobserving conditions from the ground they appear as point-likesources

The compactness and high contrast with respect to the back-ground light from galaxy and sky make GCs observable out tolarge distances Photometric studies with the Hubble Space Tele-scope (HST) have been carried out for GC systems at z sim 02

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(d sim 800 Mpc ACS data Alamo-Martiacutenez et al 2013) and atz sim 03 (d sim 1250 Mpc ACS and WFC3 data Janssens et al2017) Furthermore very recently Vanzella et al (2017) havereported the discovery of several compact extremely young ob-jects at redshift z gt 3 observed with Very Large TelescopeMultiUnit Spectroscopic Explorer (VLTMUSE) some of which haveinferred physical properties consistent with those expected inproto-GCs

Beyond their role as laboratories for the validation and cal-ibration of stellar evolution from the data of the closest re-solved GCs (Salaris amp Cassisi 2005) the systematic study ofextragalactic GC systems has revealed a wealth of propertiesused to trace the physical characteristics of the GC system andthe host galaxy for example the luminosity function of GCs(GCLF) spatial distribution projected surface density radialcolor profiles specific frequency kinematical properties andcolor-magnitude relations are effective tracers of the past forma-tion and evolution history of the galaxy its physical distancepossible merging events mass distribution etc (Harris 2001Brodie amp Strader 2006)

Studies of extragalactic GCs based on photometry are ham-pered by a varying level of contamination from foreground MWstars and background galaxies On the other hand spectroscopicobservations can provide cleaner GC samples but they are fea-sible only for the nearest brightest GC systems even with thelargest 8-10 m class telescopes (Brodie et al 2014)

In this paper we use the science verification imaging data inthe ugriJKs bands taken with the VST and VISTA ESO surveytelescopes to obtain an updated catalog of GCs in NGC 253thereby taking advantage of the large wavelength range covered

The galaxy the brightest in the Sculptor group (Karachent-sev et al 2003) at a distance of sim 35 Mpc (Radburn-Smithet al 2011) is an edge-on disk galaxy and together with M 82is one of the two brightest closest starburst galaxies (McCarthyet al 1987) Two different spectroscopic studies by Beasley ampSharples (2000) and by Olsen et al (2004) have targeted the GCsystem of the galaxy leading to a total of 21 spectroscopicallyconfirmed GCs which we use as reference sample Other pho-tometric studies exist in the literature (Liller amp Alcaino 1983Blecha 1986) The advantage of the catalog we present in thiswork is the wider wavelength coverage and larger angular cov-erage of the data analyzed Galleti et al (2004) announced 380globular cluster candidates in NGC 253 selected with photomet-ric data The follow-up study based on VIMOSVLT spectro-scopic data is still unpublished In general both spectroscopicand photometric studies of GCs in the Sculptor group are con-sistent with low metallicity [FeH] simlt minus1 and with a cumulativeluminosity function (LF) consistent with the Milky Way How-ever for NGC 253 the conclusions are tempered by the smallsample size of confirmed GCs and by the large contamination inphotometric samples We aim to remedy that by using VST andVISTA high-resolution multiwavelength imaging data

The paper is organized as follows The next section describes theobservations procedures for data reduction and for deriving thephotometry of the sources in the optical and near-IR frames Theselection of GCs candidates is described in Section 3 Section 4provides the final catalog and a brief discussion of our results Asummary of the main results closes the paper

2 Observations data reduction and analysis

The data presented in this paper were collected as part of scienceverification of VST (Iodice et al 2012) and VISTA (Arnaboldi

et al 2010 2012) In particular we analyzed the ugri data fromVST and the JKs from VISTA

The VST data were processed with VST-Tube (Grado et al2012) a pipeline specialized for the data reduction of VST-OmegaCAM executing prereduction (bias subtraction and flatnormalization) illumination and (for the i band) fringe correc-tions and photometric and astrometric calibration

The data reduction for VISTA was carried out with theVISTA data flow system at the Cambridge Astronomy SurveyUnit (see Irwin et al 2004 Greggio et al 2014 Iodice et al2014 for more details)

A summary of the observations is provided in Table 1 to-gether with a list of properties of the target galaxy The final im-age size was sim 104 times 109 for VST at 021primeprimepixel resolutionwith the ugri pointings centered on the galaxy For VISTA theimage size was sim 12times15 at 0339primeprimepixel resolution centeredat RA=004659 and Dec=-251726 with the photometric cen-ter of the galaxy slightly offset eastward of the pointing centerFigure 1 and Figure 2 show the full field of view observed byVST and VISTA in g and J band respectively The final com-bined field of view is of sim 105 deg2 over which we have pho-tometry in all six bands

We need to minimize contamination due to the light from thegalaxy to study GCs To model and subtract the surface bright-ness profile of NGC 253 we used the ISOPHOTEELLIPSE taskin IRAFSTSDAS (Jedrzejewski 1987)1 The geometric parame-ters of the galaxy light fits are on average position angle sim 51 degand ellipticity sim 078 in all inspected bands which is consistentwith previous results (Iodice et al 2014)

After modeling and subtracting the profile of the galaxyto produce a complete catalog of all sources in the VST andVISTA field of view we independently ran SExtractor (Bertinamp Arnouts 1996) on the galaxy-model-subtracted frame for eachfilter We obtained aperture magnitudes within a diameter aper-ture of eight pixels (sim 1primeprime7 at OmegaCAMVST resolution and sim2primeprime7 for the VIRCAMVISTA) and applied aperture correction toinfinite radius The aperture correction is derived from the anal-ysis of the curve of growth of bright isolated point-like sourcesThe aperture correction terms derived are apcorr=043 038040 025 019 014 mag in u g r i J Ks respectivelywith typical uncertainty of sim 001 mag We assumed constantGalactic extinction on the frames with the Schlafly amp Finkbeiner(2011) recalibration of the Schlegel et al (1998) infrared-baseddust maps

The VST images are calibrated in the SDSS photometric sys-tem using several Landolt (1992) standard fields with calibratedSDSS photometry VISTA is instead calibrated against 2MASSphotometry We independently verified the calibrations by com-paring the ugri magnitudes with sim 500 objects with photometryavailable from APASS For the u2 g and r bands the mediandifference between our VST and APASS magnitudes is le004mag which is smaller than the rms scatter in every case Forthe i band we found a small color independent offset of sim 01mag that is still consistent with zero within the estimated rms(〈mVS T

i minus mAPAS Si 〉 = 010 plusmn 011 mag) The same behavior of

VST and APASS photometry in i band was also found on com-pletely different targets from the Fornax Deep Survey (Iodice

1 IRAF is distributed by the National Optical Astronomy Observatorywhich is operated by the Association of Universities for Research in As-tronomy (AURA) under cooperative agreement with the National Sci-ence Foundation2 We transformed the APASS B-band photometry to u usingthe equations given in httpswwwsdss3orgdr8algorithmssdssUBVRITransformphp

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(d sim 800 Mpc ACS data Alamo-Martiacutenez et al 2013) and atz sim 03 (d sim 1250 Mpc ACS and WFC3 data Janssens et al2017) Furthermore very recently Vanzella et al (2017) havereported the discovery of several compact extremely young ob-jects at redshift z gt 3 observed with Very Large TelescopeMultiUnit Spectroscopic Explorer (VLTMUSE) some of which haveinferred physical properties consistent with those expected inproto-GCs

Beyond their role as laboratories for the validation and cal-ibration of stellar evolution from the data of the closest re-solved GCs (Salaris amp Cassisi 2005) the systematic study ofextragalactic GC systems has revealed a wealth of propertiesused to trace the physical characteristics of the GC system andthe host galaxy for example the luminosity function of GCs(GCLF) spatial distribution projected surface density radialcolor profiles specific frequency kinematical properties andcolor-magnitude relations are effective tracers of the past forma-tion and evolution history of the galaxy its physical distancepossible merging events mass distribution etc (Harris 2001Brodie amp Strader 2006)

Studies of extragalactic GCs based on photometry are ham-pered by a varying level of contamination from foreground MWstars and background galaxies On the other hand spectroscopicobservations can provide cleaner GC samples but they are fea-sible only for the nearest brightest GC systems even with thelargest 8-10 m class telescopes (Brodie et al 2014)

In this paper we use the science verification imaging data inthe ugriJKs bands taken with the VST and VISTA ESO surveytelescopes to obtain an updated catalog of GCs in NGC 253thereby taking advantage of the large wavelength range covered

The galaxy the brightest in the Sculptor group (Karachent-sev et al 2003) at a distance of sim 35 Mpc (Radburn-Smithet al 2011) is an edge-on disk galaxy and together with M 82is one of the two brightest closest starburst galaxies (McCarthyet al 1987) Two different spectroscopic studies by Beasley ampSharples (2000) and by Olsen et al (2004) have targeted the GCsystem of the galaxy leading to a total of 21 spectroscopicallyconfirmed GCs which we use as reference sample Other pho-tometric studies exist in the literature (Liller amp Alcaino 1983Blecha 1986) The advantage of the catalog we present in thiswork is the wider wavelength coverage and larger angular cov-erage of the data analyzed Galleti et al (2004) announced 380globular cluster candidates in NGC 253 selected with photomet-ric data The follow-up study based on VIMOSVLT spectro-scopic data is still unpublished In general both spectroscopicand photometric studies of GCs in the Sculptor group are con-sistent with low metallicity [FeH] simlt minus1 and with a cumulativeluminosity function (LF) consistent with the Milky Way How-ever for NGC 253 the conclusions are tempered by the smallsample size of confirmed GCs and by the large contamination inphotometric samples We aim to remedy that by using VST andVISTA high-resolution multiwavelength imaging data

The paper is organized as follows The next section describes theobservations procedures for data reduction and for deriving thephotometry of the sources in the optical and near-IR frames Theselection of GCs candidates is described in Section 3 Section 4provides the final catalog and a brief discussion of our results Asummary of the main results closes the paper

2 Observations data reduction and analysis

The data presented in this paper were collected as part of scienceverification of VST (Iodice et al 2012) and VISTA (Arnaboldi

et al 2010 2012) In particular we analyzed the ugri data fromVST and the JKs from VISTA

The VST data were processed with VST-Tube (Grado et al2012) a pipeline specialized for the data reduction of VST-OmegaCAM executing prereduction (bias subtraction and flatnormalization) illumination and (for the i band) fringe correc-tions and photometric and astrometric calibration

The data reduction for VISTA was carried out with theVISTA data flow system at the Cambridge Astronomy SurveyUnit (see Irwin et al 2004 Greggio et al 2014 Iodice et al2014 for more details)

A summary of the observations is provided in Table 1 to-gether with a list of properties of the target galaxy The final im-age size was sim 104 times 109 for VST at 021primeprimepixel resolutionwith the ugri pointings centered on the galaxy For VISTA theimage size was sim 12times15 at 0339primeprimepixel resolution centeredat RA=004659 and Dec=-251726 with the photometric cen-ter of the galaxy slightly offset eastward of the pointing centerFigure 1 and Figure 2 show the full field of view observed byVST and VISTA in g and J band respectively The final com-bined field of view is of sim 105 deg2 over which we have pho-tometry in all six bands

We need to minimize contamination due to the light from thegalaxy to study GCs To model and subtract the surface bright-ness profile of NGC 253 we used the ISOPHOTEELLIPSE taskin IRAFSTSDAS (Jedrzejewski 1987)1 The geometric parame-ters of the galaxy light fits are on average position angle sim 51 degand ellipticity sim 078 in all inspected bands which is consistentwith previous results (Iodice et al 2014)

After modeling and subtracting the profile of the galaxyto produce a complete catalog of all sources in the VST andVISTA field of view we independently ran SExtractor (Bertinamp Arnouts 1996) on the galaxy-model-subtracted frame for eachfilter We obtained aperture magnitudes within a diameter aper-ture of eight pixels (sim 1primeprime7 at OmegaCAMVST resolution and sim2primeprime7 for the VIRCAMVISTA) and applied aperture correction toinfinite radius The aperture correction is derived from the anal-ysis of the curve of growth of bright isolated point-like sourcesThe aperture correction terms derived are apcorr=043 038040 025 019 014 mag in u g r i J Ks respectivelywith typical uncertainty of sim 001 mag We assumed constantGalactic extinction on the frames with the Schlafly amp Finkbeiner(2011) recalibration of the Schlegel et al (1998) infrared-baseddust maps

The VST images are calibrated in the SDSS photometric sys-tem using several Landolt (1992) standard fields with calibratedSDSS photometry VISTA is instead calibrated against 2MASSphotometry We independently verified the calibrations by com-paring the ugri magnitudes with sim 500 objects with photometryavailable from APASS For the u2 g and r bands the mediandifference between our VST and APASS magnitudes is le004mag which is smaller than the rms scatter in every case Forthe i band we found a small color independent offset of sim 01mag that is still consistent with zero within the estimated rms(〈mVS T

i minus mAPAS Si 〉 = 010 plusmn 011 mag) The same behavior of

VST and APASS photometry in i band was also found on com-pletely different targets from the Fornax Deep Survey (Iodice

1 IRAF is distributed by the National Optical Astronomy Observatorywhich is operated by the Association of Universities for Research in As-tronomy (AURA) under cooperative agreement with the National Sci-ence Foundation2 We transformed the APASS B-band photometry to u usingthe equations given in httpswwwsdss3orgdr8algorithmssdssUBVRITransformphp

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Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 1 Properties of the target

RA (J2000) 00h 47m 331s (1)Dec (J2000) -25d 17m 18s (1)cz (kms) 243plusmn2 (2)Mtot

V (mag) sim-21plusmn05 (2)E(BminusV) 0017 (1)Type SABc (2)Ttype 51 plusmn 04 (2)σ (kms) 97 plusmn 18 (2)(mminusM) 2770plusmn007 (3)

Details on observationsPassband exp time (s) 〈FWHM〉

VSTu (s) 29008 0primeprime94g (s) 2100 0primeprime83r (s) 3718 0primeprime89i (s) 1500 0primeprime75

VISTAJ sim 80000 0primeprime97Ks sim 2100 1primeprime29

Notes Listed properties are taken from (1) the NASA Extragalac-tic Database httpnedipaccaltechedu (2) the HyperLedaarchive httpledauniv-lyon1fr and (3) Radburn-Smithet al (2011)

et al 2016 DrsquoAbrusco et al 2016 Cantiello et al 2017) andwith a data reduction tool independent from VST-Tube (iewith AstroWise Aku Venhola priv communication) Further-more the comparison of i-band photometry for VST data withdata in the literature for other targets in the VEGAS survey(eg NGC 3115 Cantiello et al 2015) did not show any pe-culiar offset in this band Hence our conclusion is that a smalldifference exists in the system throughput and image quality ati-band wavelengths between the two telescope-instrument com-binations leading to the observed increased offset and scatter

For the near-IR bands we checked the photometry with anindependent comparison to 2MASS point sources photometryThe agreement is satisfactory for both bands with an offset le004 mag and rms nearly twice as large

The photometric catalogs in the six bands were matchedadopting 1primeprime21primeprime4 matching radius for VSTVISTA The full cat-alog of sim 1200000 sources is available on the VEGAS projectweb-page3 and on the CDS archive Sources with matched pho-tometry in all six bands or with missing detections in one ormore filters are included in the full catalog

A color magnitude diagram and some color-color diagramsof the full matched catalog are shown in Figure 3 In the fig-ure we show separately the sim 70000 sources detected in areaswith high and highly variable galaxy backgrounds (ie in re-gions where microg le 236 magarcsec2 left panels) and those de-tected where the galaxy background is negligible (right panels)

3 Selection of GC candidates

To select GC candidates we applied the photometric morpho-metric and color selection criteria already used in Cantiello etal (2017) with some differences explained below

We started by applying color-color selections using all avail-able pairs of colors Figure 4 shows some examples of the color-3 Project page httpwwwnaastroitvegasVEGASVEGAS_Targetshtml

Fig 1 Full field of view observed with VST (g band is shownother bands are nearly identical) White squares indicate the 14spectroscopic confirmed GCs from Beasley amp Sharples (2000)labeled as in Table 2 (Col 6) in that paper

Fig 2 Full field of view observed with VISTA (J band is shownKs band is nearly identical) White diamonds indicate the 11spectroscopic confirmed GCs from Olsen et al (2004) labeledas in Table 3 (Col 1) in that paper

4 Models available at the URLhttpwwwoa-teramoinafitspot Old GCs are expected to match the models sequence The finalsample of selected GC candidates is shown in the upper right panelswith filled blue circles The sample of 21 spectroscopically confirmedGCs from Beasley amp Sharples (2000) and Olsen et al (2004) are plot-ted in the lower left panel The two spectroscopic databases contain 14(Beasley amp Sharples 2000) and 11 GCs (Olsen et al 2004) respectivelyand four sources are common to both Depending on the plotted colorsthe various sequences of MW stars passive and star-forming galaxiesappear relatively well defined (see also Appendix A) In the (uminusi) versus(iminusKs) plot (uiKs hereafter) we highlighted the approximate position ofsuch areas adding the locus of GC candidates as found by Muntildeoz et al(2014) properly shifted to take into account the different u bands be-tween the two works

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Fig 3 Color magnitude and color-color diagrams for the fullmatched catalog of sources detected Left panels Sources de-tected at galactocentric radii with moderate-to-high galaxy sur-face brightness background microg le 236 magarcsec2 are shownRight panels Sources detected in regions with low galaxy back-ground are shown

color diagrams In each panel besides showing the full sampleof matched sources in light gray we highlight some stages of theGCs selection procedure adopted For the purely optical color-color diagram (upper left panel) we plot the locus of simple stel-lar population models from the Teramo-SPoT group (Raimondoet al 2005 Raimondo 2009)4

For each pair of colors we selected only the sources fallingwithin the color-color area defined by confirmed GCs and SSPmodels as good GC candidates extended by sim20 on each sideie no less than 02 mag for the colors spanning an intervallower than 1 mag such as rminusi The choice of sim20 adoptedafter several tests was motivated by the need for an area largeenough to include the largest percentage of confirmed GCs butnot too wide to avoid exceedingly large contamination from ob-vious non-GCs sources We adopted as lower age limit for SSPmodels t = 6 Gyr based on the comparison of the range of col-ors from confirmed GCs Such limit might be rather low for theages generally simgt 10 Gyr (eg Puzia et al 2005) typical for oldGCs However given the age-metallicity degeneracy for the op-tical colors (Worthey 1994) younger SSP models with higher[FeH] overlap with the sequence of older SSP models withlower [FeH] In any case the main constraint to the color-colorselections adopted here comes from empirical data We used theSSP models as a countercheck as they are confined to a verynarrow region of the optical color-color planes while empiricaldata are more scattered and also include the selection with near-IR bands

To give an idea of the efficiency of the color-color selec-tion adopted we highlight that starting from a sample of sim1200000 matched sources the sample of color-color prese-lected GCs includes sim 1500 objects

To further narrow down the sample of reliable GC candi-dates we used other photometric and morphological propertiesof the sample as described in Cantiello et al (2017) We mea-sured the magnitude concentration index (Peng et al 2011) ob-tained as the difference between the magnitude measured at 6pixel aperture diameter and at 12 pixel ∆X6minus12 equiv magX6pix minus

magX12pix where X is one of the optical ugri bands and aper-ture corrected magnitudes are used For point-like sources af-ter applying the aperture correction to the magnitudes at bothradii ∆X6minus12 should be statistically consistent with zero Hence∆X6minus12 is an ideal tool to identify point-like sources such as starsand extragalactic GCs in very distant galaxies as they appear un-resolved In the case of NGC 253 given the spatial resolutionand FWHM of our dataset GCs appear as slightly resolved ex-tended sources and consequently their magnitude concentrationindex is larger than zero By analyzing the sample of confirmedGCs we find ∆X6minus12 gt 01 mag in all optical bands (with threeexceptions discussed below) and a median of ∆X6minus12 sim 02 magFor the morphologic selection we did not use VISTA data as thepixel resolution is lower than for VST Moreover the J-band im-age is much more crowded than optical images given the depthof the frame stars in the field of NGC 253 are also detected(Greggio et al 2014)

The upper left panel of Figure 5 shows the g-band magnitudeconcentration index ∆g6minus12 for the sample of color-color se-lected GC candidates In the panel where the confirmed GCs arealso reported the stellar sequence at ∆g6minus12 sim 00 mag is easilyrecognized as well as the positive ge 01 mag values for all butthree confirmed GCs The three sources at ∆g6minus12 le 0075 magwhich we adopted as threshold for reliable candidates are thecandidates with ID 109 and 114 from Olsen et al (2004) andLA11 from Beasley amp Sharples (2000) For the first two sourceswe observe that the magnitude concentration index is consistentwith zero in all optical bands and similarly the SExtractor andIshape (see section 32) output parameters described below areall consistent with the stellar nature of the two sources Analyz-ing the two candidates in more detail we also find that both haveFWHM that is locally indistinguishable with all confirmed stel-lar sources (selected by colors and the other morpho-photometriccriteria) The case of LA11 is described in more detail later inthis section

As additional selection criteria for the sole optical bands weused a selection of SExtractor output parameters (ie FWHMCLASS_STAR minor-to-major axis ratio ba and flux radiussee definitions in Table 2) the limits of the GCLF and a max-imum photometric error The SExtractor selection criteria werederived by comparison with the same parameter for confirmedGCs for the minimum axis ratio ba we conservatively as-sumed ba ge067 which is comparable to the observed min-imum for MW and Magellanic Clouds GC systems (van denBergh amp Morbey 1984 Harris 1996 Cantiello et al 2009)The FWHM CLASS_STAR and flux radius selections are alsoshown in Figure 5

There is some level of degeneracy for some of the adoptedmorphometric quantities Our intention in adopting such largeset of parameters is to exclude anomalous or peculiar sourcesthat might be more efficiently detected with one parameter ratherthan others hence minimizing any contamination from non-GCsources

The bright and faint magnitude cuts were derived from theGCLF as follows We adopted the RGB-tip distance modulusgiven in Table 1 and then we used the results from Villegaset al (2010) for the GCLF turnover magnitude (TOM or MTOM hereafter) and for the GCLF dispersion σGCLF In particular

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Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 4 Selection of color-color diagrams used for selecting GC candidates Gray dots show the full sample of matched sourcesIn each panel in addition to the full sample single elements of the GC selection process are highlighted Upper left panel SSPmodels for ages between 6 and 14 Gyrs and [FeH] between minus23 and +03 are plotted with solid lines in various shades of red(darker for more metal-poor at fixed [FeH] older ages have redder colors) Upper right Blue dots show the sample of sim 350GC candidates selected using color-color photometric and morphometric selection criteria described in text The median error barsare indicated (lower right blue symbols) calculated as the sample median from GC candidates and shown in other panels as wellLower left panel Yellow squares and green diamonds indicate the location of Beasley amp Sharples (2000) and Olsen et al (2004)spectroscopically confirmed GCs Lower right panel We highlight the approximate MW stars sequence (gray) the area occupied bybackground galaxies (passive in red and blue star-forming galaxies in cyan see also Appendix A) and the area identified by Muntildeozet al (2014) as the locus of GCs (orange)

we adopted MgTOM = minus74 mag and estimated σGCLF = 11

mag (assuming a total magnitude of NGC 253 of MZ sim minus22mag) Finally we adopted as magnitude cuts plusmn3σGCLF brighterand fainter than the TOM For sake of simplicity the TOM inu r and i bands were derived from the Mg

TOM band reportedabove and from the median uminusg gminusr and gminusi of known GCs inthe sample ie sim 14 06 and 08 mag respectively Further-more to be most inclusive as possible the magnitude cuts wererounded off to the closest more conservative semi-entire magni-

tude (eg we adopted mbright = 16 for the r band rather than 162mag and m f aint = 23 rather than 228 mag)

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Fig 5 Upper left g-band magnitude concentration index for the sample of color-selected GC candidates shown in blue As in Figure4 yellow squares and green diamonds indicate the location of Beasley amp Sharples (2000) and Olsen et al (2004) spectroscopicconfirmed GCs respectively The gray shaded area defines the region in which sources are rejected as reliable GC candidates Upperright g-band FWHM from SExtractor vs magnitude Symbols are as upper left panel Lower left As upper right but SExtractorCLASS_STAR parameter is plotted instead of FWHM Lower right As upper right but SExtractor Flux Radius (ie half-lightradius) parameter is plotted instead of FWHM The saturation that is manifested as the rightward tail at bright magnitudes in theupper left panel similar to the tail that points upward in the upper right and lower right panels appears at a magnitude brighter thanthe brightest GCs (eg mg lt 155 mag see also Table 2) and therefore does not affect our GC candidate selection process

All the morpho- and photometric selection criteria adoptedare summarized in Table 2 The final sample of selected GC can-didates passing through all adopted selections contained sim 350sources

In Figure 6 we show some of the color-color diagrams al-ready shown in Figure 4 but this time plotting only the sim 350GCs candidates selected using the photometric morphometricand color selection criteria described above Overplotted in greenand yellow symbols are spectroscopically confirmed GCs In ad-dition a color magnitude diagram (upper right panel) is reported

31 Comparison with spectroscopic and photometric GCsamples

Our sample of sim 350 color-color morpho- and photometric se-lected GC candidates does not contain some of the spectroscop-ically confirmed sources by either Beasley amp Sharples (2000) orOlsen et al (2004) We already anticipated the cases of 2 outof 11 GCs from Olsen et al (2004 IDs 109 and 114 fromtheir Table 3) which are consistent with being foreground starsin all bands including J and Ks as they are coherently consistentwith stellar morpho-photometric parameters The two objectshave line-of-sight velocity of 177 plusmn 5 kms and 192 plusmn 17 kmswhich are relatively high and explain their classification as GCsin NGC 253 which has cz = 243 plusmn 2 kms Nevertheless thephotometric properties of the couple indicate they are likely

Article number page 6 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 6 Color-color (upper left and lower panels) and color-magnitude (upper right) diagrams of the sim 350 selected GC candidates(blue circles) and the spectroscopically confirmed GCs Yellow squares and green diamonds indicate the Beasley amp Sharples (2000)and Olsen et al (2004) samples respectively For the color-magnitude diagram the full sample of matched sources (gray dots) andthe position of the turnover magnitude (long-dashed horizontal black line) are also shown

high-velocity MW stars (eg Xue et al 2008) The remaining9 sources from Olsen et al are correctly selected as GCs in ourfinal sample

As for the sample of confirmed GCs by Beasley amp Sharples(2000) the clusters with IDs LA11 LA24 B1 B13 B14 andB29 from their Table 2 (we adopted the alternative IDs givenby the authors) are not selected Because LA24 is very closeto a bright star (mV lt 9 mag) this GC is undetected in somepassbands while B1 is undetected in the Ks band because it isfaint

The other missing four candidates are excluded from oursample because of their colors (LA11 also for its concentrationindex see Figure 5) The rejected candidates are shown in theRGB thumbnail of Figure 9 The candidate LA11 in addition tothe non-GC colors shows the presence of obvious features in allthe imaging data from VST for B29 its red colors are consistent

with a background early-type galaxy this possibility is also sup-ported by its elongation which exceeds our adopted ba limit of067 with both the SExtractor and Ishape analyses Hence forboth the latter objects our analysis rather supports the non-GCnature of the two sources

Sources B13 and B14 appear deeply enshrouded in the dustof the galaxy Hence because of host-galaxy extinction the col-ors of the sources were off the color-color areas we adopted

All such missed sources are in any case included in the finaltable of GC candidates properly commented in our classificationscheme

As for the comparison with previous photometric catalogsof GCs in Figure 7 we plot some properties of our full catalogof matched sources with the samples of photometric candidatesfrom Liller amp Alcaino (1983) Blecha (1986) and Beasley ampSharples (2000) In addition to the spectroscopic sample used

Article number page 7 of 24

AampA proofs manuscript no ms_printer_v11

Fig 7 Color-color (uiKs left) and i- band concentration index (∆i6minus12 right) diagrams for the full matched catalog (gray symbols)and the photometric GC candidates from the literature Red diamonds blue circles and green squares indicate Liller amp Alcaino(1983) Blecha (1986) and Beasley amp Sharples (2000 Table 6) GC candidates respectively

Table 2 Photometric and morphometric selection criteriaadopted

Quantity Passband Range adoptedfor selection

∆X6minus12 (mag) All ge 0075CLASS_STAR u le 08CLASS_STAR g le 07CLASS_STAR r le 095CLASS_STAR i le 095PSF FWHM (pixels) u ge 45PSF FWHM (pixels) g ge 41 amp lt 15PSF FWHM (pixels) r ge 425 amp lt 15PSF FWHM (pixels) i ge 39 amp lt 15Flux Radius (pixels) u ge 32 amp lt 10Flux Radius (pixels) g ge 3 amp lt 10Flux Radius (pixels) r ge 3 amp lt 10Flux Radius (pixels) i ge 25 amp lt 15Axis Ratio ba All ge 067∆ mag All le 025mbright-m f aint (mag) u 18-25mbright-m f aint (mag) r 165-235mbright-m f aint (mag) g 16-23mbright-m f aint (mag) i 16-23

Notes Explanation of listed parameters ∆X6minus12 Threshold for themagnitude concentration index SExtractor parameters CLASS_STARNeural-Network-based stargalaxy classifier PSF FWHM point spreadfunction full width at half maximum Flux Radius half light radiusaxis-ratio semi-minor over semi-major axis ratio (see Bertin amp Arnouts1996 and references therein for more details) Other selection param-eters ∆ mag maximum error on magnitude mbright-m f aint bright andfaint magnitude cuts (see text)

here the latter authors presented a sample of sim 90 photometri-cally selected GCs The figure highlights that a substantial num-ber of selected candidates are indeed stars or background galax-ies both because of their colors or the concentration index orboth The improved efficiency of the analysis presented here isdue to a combination of the larger inspected area which is afactor of sim3 to sim 10 with respect to previous studies the better

seeing conditions from 10 better to 300 and the much widerwavelength coverage other studies are based on only B or B andV photometry

32 Globular cluster sizes

At the distance of NGC 253 and with the seeing conditions ofour observational dataset the half-light radii Rh of GCs can bederived Size measurements can be very challenging especiallywith ground-based imaging data In spite of this angular sizesand intrinsic shapes have been obtained for a large sample ofslightly resolved star clusters in different environments and withvarious ground- and space-based telescopes (eg Larsen 1999Larsen amp Brodie 2003 Jordaacuten 2004 Cantiello et al 2007 Casoet al 2013 Puzia et al 2014 Cantiello et al 2015)

To estimate the intrinsic size of a source exceeding someinstrumental-dependent size limit specific tools have been de-signed and implemented to analyze the light profiles of sourceswith intrinsic sizes comparable or slightly smaller than the in-strumental point spread function (PSF) We adopted Ishape5 toobtain structural parameters (in particular Rh and the minor-to-major axis ratio ba) of candidate GCs Ishape is optimized formodeling the light distribution for marginally resolved sourcesdown to 110 of the FWHM of the PSF (Larsen 1999 Larsenamp Richtler 2000) In such context the VST dataset of NGC 253is very attractive At the adopted distance modulus (correspond-ing to sim 347 Mpc) and given the FWHM of the images (Table1) Ishape can be used to determine the physical extent of objectswith Rh ge 13 pc For reference excluding highly extincted GCswith E(B minus V) ge 05 the MW hosts two GCs with Rh sim

lt 12 pcand five with Rh le 15 pc (Harris 1996) The median is Rh = 322pc Since the measurement of source sizes below the FWHM isparticularly demanding in terms of signal-to-noise ratio and im-age quality we limited the analysis of GC radii to gri band dataUsing Ishape we fitted all sources with a King profile with con-

5 The software can be downloaded at httpbaolabastroduoorg Forthe present work we used the release 0941e

Article number page 8 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 4 Selection of color-color diagrams used for selecting GC candidates Gray dots show the full sample of matched sourcesIn each panel in addition to the full sample single elements of the GC selection process are highlighted Upper left panel SSPmodels for ages between 6 and 14 Gyrs and [FeH] between minus23 and +03 are plotted with solid lines in various shades of red(darker for more metal-poor at fixed [FeH] older ages have redder colors) Upper right Blue dots show the sample of sim 350GC candidates selected using color-color photometric and morphometric selection criteria described in text The median error barsare indicated (lower right blue symbols) calculated as the sample median from GC candidates and shown in other panels as wellLower left panel Yellow squares and green diamonds indicate the location of Beasley amp Sharples (2000) and Olsen et al (2004)spectroscopically confirmed GCs Lower right panel We highlight the approximate MW stars sequence (gray) the area occupied bybackground galaxies (passive in red and blue star-forming galaxies in cyan see also Appendix A) and the area identified by Muntildeozet al (2014) as the locus of GCs (orange)

we adopted MgTOM = minus74 mag and estimated σGCLF = 11

mag (assuming a total magnitude of NGC 253 of MZ sim minus22mag) Finally we adopted as magnitude cuts plusmn3σGCLF brighterand fainter than the TOM For sake of simplicity the TOM inu r and i bands were derived from the Mg

TOM band reportedabove and from the median uminusg gminusr and gminusi of known GCs inthe sample ie sim 14 06 and 08 mag respectively Further-more to be most inclusive as possible the magnitude cuts wererounded off to the closest more conservative semi-entire magni-

tude (eg we adopted mbright = 16 for the r band rather than 162mag and m f aint = 23 rather than 228 mag)

Article number page 5 of 24

AampA proofs manuscript no ms_printer_v11

Fig 5 Upper left g-band magnitude concentration index for the sample of color-selected GC candidates shown in blue As in Figure4 yellow squares and green diamonds indicate the location of Beasley amp Sharples (2000) and Olsen et al (2004) spectroscopicconfirmed GCs respectively The gray shaded area defines the region in which sources are rejected as reliable GC candidates Upperright g-band FWHM from SExtractor vs magnitude Symbols are as upper left panel Lower left As upper right but SExtractorCLASS_STAR parameter is plotted instead of FWHM Lower right As upper right but SExtractor Flux Radius (ie half-lightradius) parameter is plotted instead of FWHM The saturation that is manifested as the rightward tail at bright magnitudes in theupper left panel similar to the tail that points upward in the upper right and lower right panels appears at a magnitude brighter thanthe brightest GCs (eg mg lt 155 mag see also Table 2) and therefore does not affect our GC candidate selection process

All the morpho- and photometric selection criteria adoptedare summarized in Table 2 The final sample of selected GC can-didates passing through all adopted selections contained sim 350sources

In Figure 6 we show some of the color-color diagrams al-ready shown in Figure 4 but this time plotting only the sim 350GCs candidates selected using the photometric morphometricand color selection criteria described above Overplotted in greenand yellow symbols are spectroscopically confirmed GCs In ad-dition a color magnitude diagram (upper right panel) is reported

31 Comparison with spectroscopic and photometric GCsamples

Our sample of sim 350 color-color morpho- and photometric se-lected GC candidates does not contain some of the spectroscop-ically confirmed sources by either Beasley amp Sharples (2000) orOlsen et al (2004) We already anticipated the cases of 2 outof 11 GCs from Olsen et al (2004 IDs 109 and 114 fromtheir Table 3) which are consistent with being foreground starsin all bands including J and Ks as they are coherently consistentwith stellar morpho-photometric parameters The two objectshave line-of-sight velocity of 177 plusmn 5 kms and 192 plusmn 17 kmswhich are relatively high and explain their classification as GCsin NGC 253 which has cz = 243 plusmn 2 kms Nevertheless thephotometric properties of the couple indicate they are likely

Article number page 6 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 6 Color-color (upper left and lower panels) and color-magnitude (upper right) diagrams of the sim 350 selected GC candidates(blue circles) and the spectroscopically confirmed GCs Yellow squares and green diamonds indicate the Beasley amp Sharples (2000)and Olsen et al (2004) samples respectively For the color-magnitude diagram the full sample of matched sources (gray dots) andthe position of the turnover magnitude (long-dashed horizontal black line) are also shown

high-velocity MW stars (eg Xue et al 2008) The remaining9 sources from Olsen et al are correctly selected as GCs in ourfinal sample

As for the sample of confirmed GCs by Beasley amp Sharples(2000) the clusters with IDs LA11 LA24 B1 B13 B14 andB29 from their Table 2 (we adopted the alternative IDs givenby the authors) are not selected Because LA24 is very closeto a bright star (mV lt 9 mag) this GC is undetected in somepassbands while B1 is undetected in the Ks band because it isfaint

The other missing four candidates are excluded from oursample because of their colors (LA11 also for its concentrationindex see Figure 5) The rejected candidates are shown in theRGB thumbnail of Figure 9 The candidate LA11 in addition tothe non-GC colors shows the presence of obvious features in allthe imaging data from VST for B29 its red colors are consistent

with a background early-type galaxy this possibility is also sup-ported by its elongation which exceeds our adopted ba limit of067 with both the SExtractor and Ishape analyses Hence forboth the latter objects our analysis rather supports the non-GCnature of the two sources

Sources B13 and B14 appear deeply enshrouded in the dustof the galaxy Hence because of host-galaxy extinction the col-ors of the sources were off the color-color areas we adopted

All such missed sources are in any case included in the finaltable of GC candidates properly commented in our classificationscheme

As for the comparison with previous photometric catalogsof GCs in Figure 7 we plot some properties of our full catalogof matched sources with the samples of photometric candidatesfrom Liller amp Alcaino (1983) Blecha (1986) and Beasley ampSharples (2000) In addition to the spectroscopic sample used

Article number page 7 of 24

AampA proofs manuscript no ms_printer_v11

Fig 7 Color-color (uiKs left) and i- band concentration index (∆i6minus12 right) diagrams for the full matched catalog (gray symbols)and the photometric GC candidates from the literature Red diamonds blue circles and green squares indicate Liller amp Alcaino(1983) Blecha (1986) and Beasley amp Sharples (2000 Table 6) GC candidates respectively

Table 2 Photometric and morphometric selection criteriaadopted

Quantity Passband Range adoptedfor selection

∆X6minus12 (mag) All ge 0075CLASS_STAR u le 08CLASS_STAR g le 07CLASS_STAR r le 095CLASS_STAR i le 095PSF FWHM (pixels) u ge 45PSF FWHM (pixels) g ge 41 amp lt 15PSF FWHM (pixels) r ge 425 amp lt 15PSF FWHM (pixels) i ge 39 amp lt 15Flux Radius (pixels) u ge 32 amp lt 10Flux Radius (pixels) g ge 3 amp lt 10Flux Radius (pixels) r ge 3 amp lt 10Flux Radius (pixels) i ge 25 amp lt 15Axis Ratio ba All ge 067∆ mag All le 025mbright-m f aint (mag) u 18-25mbright-m f aint (mag) r 165-235mbright-m f aint (mag) g 16-23mbright-m f aint (mag) i 16-23

Notes Explanation of listed parameters ∆X6minus12 Threshold for themagnitude concentration index SExtractor parameters CLASS_STARNeural-Network-based stargalaxy classifier PSF FWHM point spreadfunction full width at half maximum Flux Radius half light radiusaxis-ratio semi-minor over semi-major axis ratio (see Bertin amp Arnouts1996 and references therein for more details) Other selection param-eters ∆ mag maximum error on magnitude mbright-m f aint bright andfaint magnitude cuts (see text)

here the latter authors presented a sample of sim 90 photometri-cally selected GCs The figure highlights that a substantial num-ber of selected candidates are indeed stars or background galax-ies both because of their colors or the concentration index orboth The improved efficiency of the analysis presented here isdue to a combination of the larger inspected area which is afactor of sim3 to sim 10 with respect to previous studies the better

seeing conditions from 10 better to 300 and the much widerwavelength coverage other studies are based on only B or B andV photometry

32 Globular cluster sizes

At the distance of NGC 253 and with the seeing conditions ofour observational dataset the half-light radii Rh of GCs can bederived Size measurements can be very challenging especiallywith ground-based imaging data In spite of this angular sizesand intrinsic shapes have been obtained for a large sample ofslightly resolved star clusters in different environments and withvarious ground- and space-based telescopes (eg Larsen 1999Larsen amp Brodie 2003 Jordaacuten 2004 Cantiello et al 2007 Casoet al 2013 Puzia et al 2014 Cantiello et al 2015)

To estimate the intrinsic size of a source exceeding someinstrumental-dependent size limit specific tools have been de-signed and implemented to analyze the light profiles of sourceswith intrinsic sizes comparable or slightly smaller than the in-strumental point spread function (PSF) We adopted Ishape5 toobtain structural parameters (in particular Rh and the minor-to-major axis ratio ba) of candidate GCs Ishape is optimized formodeling the light distribution for marginally resolved sourcesdown to 110 of the FWHM of the PSF (Larsen 1999 Larsenamp Richtler 2000) In such context the VST dataset of NGC 253is very attractive At the adopted distance modulus (correspond-ing to sim 347 Mpc) and given the FWHM of the images (Table1) Ishape can be used to determine the physical extent of objectswith Rh ge 13 pc For reference excluding highly extincted GCswith E(B minus V) ge 05 the MW hosts two GCs with Rh sim

lt 12 pcand five with Rh le 15 pc (Harris 1996) The median is Rh = 322pc Since the measurement of source sizes below the FWHM isparticularly demanding in terms of signal-to-noise ratio and im-age quality we limited the analysis of GC radii to gri band dataUsing Ishape we fitted all sources with a King profile with con-

5 The software can be downloaded at httpbaolabastroduoorg Forthe present work we used the release 0941e

Article number page 8 of 24

AampA proofs manuscript no ms_printer_v11

Fig 5 Upper left g-band magnitude concentration index for the sample of color-selected GC candidates shown in blue As in Figure4 yellow squares and green diamonds indicate the location of Beasley amp Sharples (2000) and Olsen et al (2004) spectroscopicconfirmed GCs respectively The gray shaded area defines the region in which sources are rejected as reliable GC candidates Upperright g-band FWHM from SExtractor vs magnitude Symbols are as upper left panel Lower left As upper right but SExtractorCLASS_STAR parameter is plotted instead of FWHM Lower right As upper right but SExtractor Flux Radius (ie half-lightradius) parameter is plotted instead of FWHM The saturation that is manifested as the rightward tail at bright magnitudes in theupper left panel similar to the tail that points upward in the upper right and lower right panels appears at a magnitude brighter thanthe brightest GCs (eg mg lt 155 mag see also Table 2) and therefore does not affect our GC candidate selection process

All the morpho- and photometric selection criteria adoptedare summarized in Table 2 The final sample of selected GC can-didates passing through all adopted selections contained sim 350sources

In Figure 6 we show some of the color-color diagrams al-ready shown in Figure 4 but this time plotting only the sim 350GCs candidates selected using the photometric morphometricand color selection criteria described above Overplotted in greenand yellow symbols are spectroscopically confirmed GCs In ad-dition a color magnitude diagram (upper right panel) is reported

31 Comparison with spectroscopic and photometric GCsamples

Our sample of sim 350 color-color morpho- and photometric se-lected GC candidates does not contain some of the spectroscop-ically confirmed sources by either Beasley amp Sharples (2000) orOlsen et al (2004) We already anticipated the cases of 2 outof 11 GCs from Olsen et al (2004 IDs 109 and 114 fromtheir Table 3) which are consistent with being foreground starsin all bands including J and Ks as they are coherently consistentwith stellar morpho-photometric parameters The two objectshave line-of-sight velocity of 177 plusmn 5 kms and 192 plusmn 17 kmswhich are relatively high and explain their classification as GCsin NGC 253 which has cz = 243 plusmn 2 kms Nevertheless thephotometric properties of the couple indicate they are likely

Article number page 6 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 6 Color-color (upper left and lower panels) and color-magnitude (upper right) diagrams of the sim 350 selected GC candidates(blue circles) and the spectroscopically confirmed GCs Yellow squares and green diamonds indicate the Beasley amp Sharples (2000)and Olsen et al (2004) samples respectively For the color-magnitude diagram the full sample of matched sources (gray dots) andthe position of the turnover magnitude (long-dashed horizontal black line) are also shown

high-velocity MW stars (eg Xue et al 2008) The remaining9 sources from Olsen et al are correctly selected as GCs in ourfinal sample

As for the sample of confirmed GCs by Beasley amp Sharples(2000) the clusters with IDs LA11 LA24 B1 B13 B14 andB29 from their Table 2 (we adopted the alternative IDs givenby the authors) are not selected Because LA24 is very closeto a bright star (mV lt 9 mag) this GC is undetected in somepassbands while B1 is undetected in the Ks band because it isfaint

The other missing four candidates are excluded from oursample because of their colors (LA11 also for its concentrationindex see Figure 5) The rejected candidates are shown in theRGB thumbnail of Figure 9 The candidate LA11 in addition tothe non-GC colors shows the presence of obvious features in allthe imaging data from VST for B29 its red colors are consistent

with a background early-type galaxy this possibility is also sup-ported by its elongation which exceeds our adopted ba limit of067 with both the SExtractor and Ishape analyses Hence forboth the latter objects our analysis rather supports the non-GCnature of the two sources

Sources B13 and B14 appear deeply enshrouded in the dustof the galaxy Hence because of host-galaxy extinction the col-ors of the sources were off the color-color areas we adopted

All such missed sources are in any case included in the finaltable of GC candidates properly commented in our classificationscheme

As for the comparison with previous photometric catalogsof GCs in Figure 7 we plot some properties of our full catalogof matched sources with the samples of photometric candidatesfrom Liller amp Alcaino (1983) Blecha (1986) and Beasley ampSharples (2000) In addition to the spectroscopic sample used

Article number page 7 of 24

AampA proofs manuscript no ms_printer_v11

Fig 7 Color-color (uiKs left) and i- band concentration index (∆i6minus12 right) diagrams for the full matched catalog (gray symbols)and the photometric GC candidates from the literature Red diamonds blue circles and green squares indicate Liller amp Alcaino(1983) Blecha (1986) and Beasley amp Sharples (2000 Table 6) GC candidates respectively

Table 2 Photometric and morphometric selection criteriaadopted

Quantity Passband Range adoptedfor selection

∆X6minus12 (mag) All ge 0075CLASS_STAR u le 08CLASS_STAR g le 07CLASS_STAR r le 095CLASS_STAR i le 095PSF FWHM (pixels) u ge 45PSF FWHM (pixels) g ge 41 amp lt 15PSF FWHM (pixels) r ge 425 amp lt 15PSF FWHM (pixels) i ge 39 amp lt 15Flux Radius (pixels) u ge 32 amp lt 10Flux Radius (pixels) g ge 3 amp lt 10Flux Radius (pixels) r ge 3 amp lt 10Flux Radius (pixels) i ge 25 amp lt 15Axis Ratio ba All ge 067∆ mag All le 025mbright-m f aint (mag) u 18-25mbright-m f aint (mag) r 165-235mbright-m f aint (mag) g 16-23mbright-m f aint (mag) i 16-23

Notes Explanation of listed parameters ∆X6minus12 Threshold for themagnitude concentration index SExtractor parameters CLASS_STARNeural-Network-based stargalaxy classifier PSF FWHM point spreadfunction full width at half maximum Flux Radius half light radiusaxis-ratio semi-minor over semi-major axis ratio (see Bertin amp Arnouts1996 and references therein for more details) Other selection param-eters ∆ mag maximum error on magnitude mbright-m f aint bright andfaint magnitude cuts (see text)

here the latter authors presented a sample of sim 90 photometri-cally selected GCs The figure highlights that a substantial num-ber of selected candidates are indeed stars or background galax-ies both because of their colors or the concentration index orboth The improved efficiency of the analysis presented here isdue to a combination of the larger inspected area which is afactor of sim3 to sim 10 with respect to previous studies the better

seeing conditions from 10 better to 300 and the much widerwavelength coverage other studies are based on only B or B andV photometry

32 Globular cluster sizes

At the distance of NGC 253 and with the seeing conditions ofour observational dataset the half-light radii Rh of GCs can bederived Size measurements can be very challenging especiallywith ground-based imaging data In spite of this angular sizesand intrinsic shapes have been obtained for a large sample ofslightly resolved star clusters in different environments and withvarious ground- and space-based telescopes (eg Larsen 1999Larsen amp Brodie 2003 Jordaacuten 2004 Cantiello et al 2007 Casoet al 2013 Puzia et al 2014 Cantiello et al 2015)

To estimate the intrinsic size of a source exceeding someinstrumental-dependent size limit specific tools have been de-signed and implemented to analyze the light profiles of sourceswith intrinsic sizes comparable or slightly smaller than the in-strumental point spread function (PSF) We adopted Ishape5 toobtain structural parameters (in particular Rh and the minor-to-major axis ratio ba) of candidate GCs Ishape is optimized formodeling the light distribution for marginally resolved sourcesdown to 110 of the FWHM of the PSF (Larsen 1999 Larsenamp Richtler 2000) In such context the VST dataset of NGC 253is very attractive At the adopted distance modulus (correspond-ing to sim 347 Mpc) and given the FWHM of the images (Table1) Ishape can be used to determine the physical extent of objectswith Rh ge 13 pc For reference excluding highly extincted GCswith E(B minus V) ge 05 the MW hosts two GCs with Rh sim

lt 12 pcand five with Rh le 15 pc (Harris 1996) The median is Rh = 322pc Since the measurement of source sizes below the FWHM isparticularly demanding in terms of signal-to-noise ratio and im-age quality we limited the analysis of GC radii to gri band dataUsing Ishape we fitted all sources with a King profile with con-

5 The software can be downloaded at httpbaolabastroduoorg Forthe present work we used the release 0941e

Article number page 8 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 6 Color-color (upper left and lower panels) and color-magnitude (upper right) diagrams of the sim 350 selected GC candidates(blue circles) and the spectroscopically confirmed GCs Yellow squares and green diamonds indicate the Beasley amp Sharples (2000)and Olsen et al (2004) samples respectively For the color-magnitude diagram the full sample of matched sources (gray dots) andthe position of the turnover magnitude (long-dashed horizontal black line) are also shown

high-velocity MW stars (eg Xue et al 2008) The remaining9 sources from Olsen et al are correctly selected as GCs in ourfinal sample

As for the sample of confirmed GCs by Beasley amp Sharples(2000) the clusters with IDs LA11 LA24 B1 B13 B14 andB29 from their Table 2 (we adopted the alternative IDs givenby the authors) are not selected Because LA24 is very closeto a bright star (mV lt 9 mag) this GC is undetected in somepassbands while B1 is undetected in the Ks band because it isfaint

The other missing four candidates are excluded from oursample because of their colors (LA11 also for its concentrationindex see Figure 5) The rejected candidates are shown in theRGB thumbnail of Figure 9 The candidate LA11 in addition tothe non-GC colors shows the presence of obvious features in allthe imaging data from VST for B29 its red colors are consistent

with a background early-type galaxy this possibility is also sup-ported by its elongation which exceeds our adopted ba limit of067 with both the SExtractor and Ishape analyses Hence forboth the latter objects our analysis rather supports the non-GCnature of the two sources

Sources B13 and B14 appear deeply enshrouded in the dustof the galaxy Hence because of host-galaxy extinction the col-ors of the sources were off the color-color areas we adopted

All such missed sources are in any case included in the finaltable of GC candidates properly commented in our classificationscheme

As for the comparison with previous photometric catalogsof GCs in Figure 7 we plot some properties of our full catalogof matched sources with the samples of photometric candidatesfrom Liller amp Alcaino (1983) Blecha (1986) and Beasley ampSharples (2000) In addition to the spectroscopic sample used

Article number page 7 of 24

AampA proofs manuscript no ms_printer_v11

Fig 7 Color-color (uiKs left) and i- band concentration index (∆i6minus12 right) diagrams for the full matched catalog (gray symbols)and the photometric GC candidates from the literature Red diamonds blue circles and green squares indicate Liller amp Alcaino(1983) Blecha (1986) and Beasley amp Sharples (2000 Table 6) GC candidates respectively

Table 2 Photometric and morphometric selection criteriaadopted

Quantity Passband Range adoptedfor selection

∆X6minus12 (mag) All ge 0075CLASS_STAR u le 08CLASS_STAR g le 07CLASS_STAR r le 095CLASS_STAR i le 095PSF FWHM (pixels) u ge 45PSF FWHM (pixels) g ge 41 amp lt 15PSF FWHM (pixels) r ge 425 amp lt 15PSF FWHM (pixels) i ge 39 amp lt 15Flux Radius (pixels) u ge 32 amp lt 10Flux Radius (pixels) g ge 3 amp lt 10Flux Radius (pixels) r ge 3 amp lt 10Flux Radius (pixels) i ge 25 amp lt 15Axis Ratio ba All ge 067∆ mag All le 025mbright-m f aint (mag) u 18-25mbright-m f aint (mag) r 165-235mbright-m f aint (mag) g 16-23mbright-m f aint (mag) i 16-23

Notes Explanation of listed parameters ∆X6minus12 Threshold for themagnitude concentration index SExtractor parameters CLASS_STARNeural-Network-based stargalaxy classifier PSF FWHM point spreadfunction full width at half maximum Flux Radius half light radiusaxis-ratio semi-minor over semi-major axis ratio (see Bertin amp Arnouts1996 and references therein for more details) Other selection param-eters ∆ mag maximum error on magnitude mbright-m f aint bright andfaint magnitude cuts (see text)

here the latter authors presented a sample of sim 90 photometri-cally selected GCs The figure highlights that a substantial num-ber of selected candidates are indeed stars or background galax-ies both because of their colors or the concentration index orboth The improved efficiency of the analysis presented here isdue to a combination of the larger inspected area which is afactor of sim3 to sim 10 with respect to previous studies the better

seeing conditions from 10 better to 300 and the much widerwavelength coverage other studies are based on only B or B andV photometry

32 Globular cluster sizes

At the distance of NGC 253 and with the seeing conditions ofour observational dataset the half-light radii Rh of GCs can bederived Size measurements can be very challenging especiallywith ground-based imaging data In spite of this angular sizesand intrinsic shapes have been obtained for a large sample ofslightly resolved star clusters in different environments and withvarious ground- and space-based telescopes (eg Larsen 1999Larsen amp Brodie 2003 Jordaacuten 2004 Cantiello et al 2007 Casoet al 2013 Puzia et al 2014 Cantiello et al 2015)

To estimate the intrinsic size of a source exceeding someinstrumental-dependent size limit specific tools have been de-signed and implemented to analyze the light profiles of sourceswith intrinsic sizes comparable or slightly smaller than the in-strumental point spread function (PSF) We adopted Ishape5 toobtain structural parameters (in particular Rh and the minor-to-major axis ratio ba) of candidate GCs Ishape is optimized formodeling the light distribution for marginally resolved sourcesdown to 110 of the FWHM of the PSF (Larsen 1999 Larsenamp Richtler 2000) In such context the VST dataset of NGC 253is very attractive At the adopted distance modulus (correspond-ing to sim 347 Mpc) and given the FWHM of the images (Table1) Ishape can be used to determine the physical extent of objectswith Rh ge 13 pc For reference excluding highly extincted GCswith E(B minus V) ge 05 the MW hosts two GCs with Rh sim

lt 12 pcand five with Rh le 15 pc (Harris 1996) The median is Rh = 322pc Since the measurement of source sizes below the FWHM isparticularly demanding in terms of signal-to-noise ratio and im-age quality we limited the analysis of GC radii to gri band dataUsing Ishape we fitted all sources with a King profile with con-

5 The software can be downloaded at httpbaolabastroduoorg Forthe present work we used the release 0941e

Article number page 8 of 24

AampA proofs manuscript no ms_printer_v11

Fig 7 Color-color (uiKs left) and i- band concentration index (∆i6minus12 right) diagrams for the full matched catalog (gray symbols)and the photometric GC candidates from the literature Red diamonds blue circles and green squares indicate Liller amp Alcaino(1983) Blecha (1986) and Beasley amp Sharples (2000 Table 6) GC candidates respectively

Table 2 Photometric and morphometric selection criteriaadopted

Quantity Passband Range adoptedfor selection

∆X6minus12 (mag) All ge 0075CLASS_STAR u le 08CLASS_STAR g le 07CLASS_STAR r le 095CLASS_STAR i le 095PSF FWHM (pixels) u ge 45PSF FWHM (pixels) g ge 41 amp lt 15PSF FWHM (pixels) r ge 425 amp lt 15PSF FWHM (pixels) i ge 39 amp lt 15Flux Radius (pixels) u ge 32 amp lt 10Flux Radius (pixels) g ge 3 amp lt 10Flux Radius (pixels) r ge 3 amp lt 10Flux Radius (pixels) i ge 25 amp lt 15Axis Ratio ba All ge 067∆ mag All le 025mbright-m f aint (mag) u 18-25mbright-m f aint (mag) r 165-235mbright-m f aint (mag) g 16-23mbright-m f aint (mag) i 16-23

Notes Explanation of listed parameters ∆X6minus12 Threshold for themagnitude concentration index SExtractor parameters CLASS_STARNeural-Network-based stargalaxy classifier PSF FWHM point spreadfunction full width at half maximum Flux Radius half light radiusaxis-ratio semi-minor over semi-major axis ratio (see Bertin amp Arnouts1996 and references therein for more details) Other selection param-eters ∆ mag maximum error on magnitude mbright-m f aint bright andfaint magnitude cuts (see text)

here the latter authors presented a sample of sim 90 photometri-cally selected GCs The figure highlights that a substantial num-ber of selected candidates are indeed stars or background galax-ies both because of their colors or the concentration index orboth The improved efficiency of the analysis presented here isdue to a combination of the larger inspected area which is afactor of sim3 to sim 10 with respect to previous studies the better

seeing conditions from 10 better to 300 and the much widerwavelength coverage other studies are based on only B or B andV photometry

32 Globular cluster sizes

At the distance of NGC 253 and with the seeing conditions ofour observational dataset the half-light radii Rh of GCs can bederived Size measurements can be very challenging especiallywith ground-based imaging data In spite of this angular sizesand intrinsic shapes have been obtained for a large sample ofslightly resolved star clusters in different environments and withvarious ground- and space-based telescopes (eg Larsen 1999Larsen amp Brodie 2003 Jordaacuten 2004 Cantiello et al 2007 Casoet al 2013 Puzia et al 2014 Cantiello et al 2015)

To estimate the intrinsic size of a source exceeding someinstrumental-dependent size limit specific tools have been de-signed and implemented to analyze the light profiles of sourceswith intrinsic sizes comparable or slightly smaller than the in-strumental point spread function (PSF) We adopted Ishape5 toobtain structural parameters (in particular Rh and the minor-to-major axis ratio ba) of candidate GCs Ishape is optimized formodeling the light distribution for marginally resolved sourcesdown to 110 of the FWHM of the PSF (Larsen 1999 Larsenamp Richtler 2000) In such context the VST dataset of NGC 253is very attractive At the adopted distance modulus (correspond-ing to sim 347 Mpc) and given the FWHM of the images (Table1) Ishape can be used to determine the physical extent of objectswith Rh ge 13 pc For reference excluding highly extincted GCswith E(B minus V) ge 05 the MW hosts two GCs with Rh sim

lt 12 pcand five with Rh le 15 pc (Harris 1996) The median is Rh = 322pc Since the measurement of source sizes below the FWHM isparticularly demanding in terms of signal-to-noise ratio and im-age quality we limited the analysis of GC radii to gri band dataUsing Ishape we fitted all sources with a King profile with con-

5 The software can be downloaded at httpbaolabastroduoorg Forthe present work we used the release 0941e

Article number page 8 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 8 Radial flux profiles of GCs in g band The various panels show the average flux profile (solid red lines normalized to one atcenter) for GC candidates with measured Rh within the labeled interval Thin dashed lines show the standard deviation of the meanfor the average profile blue dotted line indicates the PSF profile

centration index c=15 (Larsen 1999 Larsen amp Richtler 2000)The final Rh and ba values are derived from the weighted aver-age of the three bands

Figure 8 shows the g-band radial flux profile of our bona fideGC candidates (see next section flux is normalized to peak one)compared with the radial profile of the PSF in the same band Inthis panel we plot the average profile of GCs with estimated ef-fective radii within the labeled Rh intervals The width of theRh intervals is chosen to contain similar numbers of GC candi-dates (sim 20) per Rh bin The figure shows the significant differ-ences between PSF (ie stellar) and GCs light profiles even forthe most compact candidates reported in the left panel Henceunlike typical studies of extragalactic GCs (eg Durrell et al2014) MW stars represent a minor source of contamination inour GC catalog because of the combined effect of galaxy dis-tance GC physical size and good image quality

Finally we specifically run Ishape on the two sources fromOlsen et al (2004) that we identified as stars (IDs 109 and 114mentioned in previous section) The results confirm the singlestar origin of the two sources as their Rh are consistent withzero in all three inspected bands and the χ2 for the fit to anextended source does not improve with respect to the χ2 obtainedmodeling a compact stellar source

4 Final catalog and discussion

41 The catalog

Taking advantage of the ACS Hubble Space Telescope obser-vations of NGC 253 from the GHOSTS survey (the GHOSTSacronym stands for Galaxy haloes outer disks substructuresthick disks star clusters Radburn-Smith et al 2011) as a coun-tercheck of our selection we visually inspected the GHOSTSfields containing our GC candidates Thanks to the exceptionalresolution of ACS star clusters at the distance of NGC 253 ap-pear as obviously mottled and extended sources with respect tothe otherwise smooth background galaxies or point-like stellarsources With the exception of two obvious background diskgalaxies all of the sources selected as described in the previ-ous section and falling in the ACS GHOSTS footprints appearas star clusters Figure 10 shows the thumbnails of the 18 se-lected GC candidates that also have HST data (panels from (a)to (d)) In the figure we also show the two background galaxies

that passed our GC selections and for sake of comparison twosources identified as stars in our selection procedures (panel (e))

Furthermore some visually obvious GCs in the GHOSTSfootprints which were not selected by our procedure wereadded by hand in our final sample after visual inspection ofGHOSTS images Such objects seven in all (Figure 10 panel( f )) although detected and classified as extended in all caseswere rejected from the final sample as their colors did not fitin the color-color sequences adopted because of dust contami-nation Although based on their appearance the candidates arecertain stellar clusters in our final Table 3 they are flagged asUncertain because of their color and excluded from the colorand magnitude distributions analysis discussed below

Moreover still based on comparison with GHOSTS data inspite of the rich set of selection criteria adopted including theuiKs color-color diagram that proved to be very effective for sort-ing GCs out of other sources in Virgo (Muntildeoz et al 2014) thematching with HST imaging data shows the presence of back-ground contamination in the final list of GC candidates Thusfor a final characterization of the GCs selected and to furtherclean the sample we visually inspected each one of the sim 350GC candidates

From the visual inspection we found that a substantial por-tion of selected candidates are obvious galaxies for various mo-tivations more or less obvious features visible in one or morebands (tidal features spiral arms) high elongation coupled withcloseness to a group of background galaxies bright and elon-gated structures with changing position angle at different radiietc

Table 3 lists the final sample of objects with coordinates(Cols 2-3) ugriJKs magnitudes and errors (Cols 4-9) half-light radius and axis ratio from Ishape (Cols 10-11) exist-ing identifications from the literature (Col 12) presence inGHOSTS footprints spectroscopic samples or previous identifi-cations in the photometric samples by Liller amp Alcaino (1983) orBlecha (1986) (Col 13) and comments from visual inspection(Col 14) In the table we also provide a further flag Class (Col15) which defines the objects classified as bona fide GC can-didates in our list the candidates considered uncertain for somereason (large number of close background galaxies high elonga-tion weird residuals from Ishape blending features border-lineaxis ratio etc) and sources that are obvious galaxies (no flag)

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Fig 9 RGB thumbnails from VST data of star cluster candidates from Beasley amp Sharples (2000) that did not pass our selectioncriteria for GC candidates Starting from left B13 and B14 (close to galaxy dusty regions) and B29 and LA11 (likely backgroundgalaxies) Thumbnails are 15primeprime on each side

which passed morpho-photometric selection criteria but wererejected upon visual inspection

The catalog contains a total of 82 best GC candidates 155uncertain candidates and 110 sources which although passedall our GC selection criteria are clearly background galaxies

The spatial distribution of the full sample is shown in Figure11 overlaid to the g-band VST contours plot

We must note that our selection technique based also onaperture photometry leaves unanswered the question about thedetection efficiency and contamination rate as a function ofgalactocentric radius Although the majority of the globular clus-ter candidates are found in the uncrowded outskirts of the galaxya significant number are projected against or near the brightcrowded galaxy disk

As is also recognizable in Figure 3 sources detected in re-gions of high galaxy background suffer from a larger photomet-ric scatter because of the galaxy contamination and the presenceof dust

However of the sim 20 bona fide GCs candidates located ingalaxy regions with microg le 236 magarcsec2 only four are newselections the remaining are all either spectroscopically con-firmed GCs or star clusters selected on HSTGHOSTS data andthree are also photometric selections from Beasley amp Sharples(2000 Table 6 data)

42 Spatial distribution and luminosity function

The optical LF of the bona fide sample and the combination ofthe bona fide and uncertain samples are shown in Figure 12 (leftpanels) In the panels of the figure the MTOM adopted prop-erly shifted to the galaxy distance is also reported The dia-grams lack the typical symmetry around the peak of the GaussianGCLF which is surprising given that the bright side of the LF ap-pears underpopulated By inspecting the full sample of sourcesbrighter than mg sim 20 we found that even after adopting reason-ably broader selection criteria the list of bright candidates doesnot increase Hence we do not have an explanation for missingbright end of the GCLF

Taking only the sample of spectroscopically confirmed GCsdoes not improve the appearance of the GCLF because of thesmall size of the sample of 21 candidates and because 7 ofthe candidates are brighter than the MTOM and 14 are fainterthan that with the faintest candidate at mg sim 215 mag ie atsim 1σGCLF the level of the faint side GCLF If we also add theGCs identified over the HSTGHOSTS area the cumulative sam-ple of HST and spectroscopic candidates has sim 10 GCs that arebrighter than the MTOM and 41 fainter than the MTOM Hencewhether only the spectroscopic candidates or both spectroscopic

and GHOSTS candidates are considered again the GCLF ishighly undersampled toward bright GCs

The incompleteness is in part due to the photometric incom-pleteness which is caused by the different depth and image qual-ity of the imaging data adopted However photometric incom-pleteness should only be an issue at the faint end of the GCLF

An alternative explanation for the asymmetric GCLF wouldcome from overestimated low luminosity end of GCLF thatwould even in the case of best candidates have to be heavilycontaminated We believe this is not the case and thus rejectthis (potential) explanation because we have verified our selec-tion criteria through a comparison with HST GHOSTS imagesand with a spectroscopically confirmed sample of GCs Further-more if the low luminosity end were heavily contaminated theGC sample size in NGC 253 would be too small resulting in toosmall S N as we discuss further in Section 43

A further correction to the GCLF might come from thefact that in addition to photometric incompleteness our sampleis also incomplete at large and small galactocentric radii Thelargest projected galactocentric distance of a GC candidate inthe bona fide sample is rgal sim 35prime or sim 355 kpc A fraction ofsim 7 (11 out of 158) MW GCs are located at galactocentric dis-tance larger than sim355 kpc Hence it is reasonable to expect thata similar fraction of GCs in NGC 253 lies beyond the commonarea of the VST and VISTA pointings

For the central dusty regions as aforementioned we partiallyrecovered some of the GCs by complementing our data with theACS GCs from GHOSTS Nevertheless such detections mostlybased on visual inspection do not necessarily allow the recov-ery of the entire population of central GCs in the galaxy As acheck we inspected the azimuthal average of the GCs radialdensity profile reported in Figure 13 The diagram shows thelinear and r14 fits to the density profile which is derived with-out the data for the innermost two annuli severely affected bydust and incompleteness In both panels we observe a drop ofthe density profile in the very central regions otherwise the ra-dial (logarithmic) density profile nicely follows the fitted den-sity profiles The r14-law profile together with the increasing orflattening of the GC density profiles at small galactocentric radiiare well-known observational properties of GC systems (Dirschet al 2005 Goudfrooij et al 2007 Cantiello et al 2015) Con-sequently it is reasonable to assume that the drop in log ρ(rgal)seen in the left panels of Figure 12 is due to poor GCs detectionin such central dusty regions Even though the central area domi-nated by dust is relatively small sim 80 square arcmin the fractionof GCs there could be significative To obtain an approximate es-timate of the number of GCs in the central area we adopted theradial density profiles shown in Figure 13 assuming as lower

Article number page 10 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

(a) From left to right Cluster candidates number 99 109 111 124 128 and 141 in Table 3

(b) From left to right Cluster candidates number 178 186 200 204 205 and 207 in Table 3

(c) From left to right Cluster candidates number 209 210 211 218 227 and 325 in Table 3

(d) From left to right Cluster candidates number 333 334 335 and 336 in Table 3

(e) From left to right Sources 107 and 212 in Table 3 (confirmed background galaxies) and two of the sources identified as stars in our selectionprocedure

(f) From left to right Sources 326 327 328 329330 331 and 332 in Table 3 visually identified as GCs and located within the dust diskof NGC 253

Fig 10 Upper four rows (a-d) Hubble Space Telescope ACS cutouts of the sources selected as GCs candidates and falling in theGHOSTS survey footprints (F814W-band imaging data are shown) Given the mottled appearance we consider all sources as starclusters in the galaxy For reference the panels in row (e) show the other two selected sources in the GHOSTS footprints whichare obvious background galaxies and two stellar sources The sources in the row ( f ) are the visually identified GC candidates (seetext)

limit to the GCs density the value of ρ(rgal) at rgal sim 11prime iethe galactocentric radius where the dusty disk begins Adoptingthe linear or r14-law fits the fitted GC density at rgal sim 11prime goesfrom sim 0045 GCsarcmin2 to sim 0057 GCsarcmin2 Hencethe estimated number of GCs in the central area is Ncenter

GC sim 5

In a study of RGB-tip field star population based on V and IMagellanIMACS data Bailin et al (2011) found evidence for alarge shelf-like feature near the southeast side of NGC 253 (alsoconfirmed by Greggio et al 2014 from resolved star analysesof the VISTA imaging data used in this work) Using GHOSTSdata in two fields - one on and one off the shelf - the authors in-

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Fig 11 GC candidates overlaid to the g-band contour plot of NGC 253 Green five-pointed stars blue squares and red trianglesshow the candidates flagged as Best Uncertain and No in Table 3 respectively The plotted contours show the microg =236 230 224218 212 206 magarcsec2 surface brightness levels respectively

spected the color distribution of RGB-tip stars and found that thefeature is possibly the remnant of a large satellite of the mergingtree of NGC 253 Yet the authors warned that the stellar popu-lations in the two fields are not dramatically different from therest of the halo at similar elliptical radii Inspecting the colorsof our bona fide GCs in various regions around the galaxy wefind that the sim15 GC candidates in the projected region closeto the shelf identified by Bailin et al (2011) have average col-ors that are bluer than the colors of GCs in other four randomlydrawn regions and than the bulk of the bona fide sample Thismight further strengthen the hypothesis of the presence of a sur-face brightness feature and of a GCs subpopulation which areboth remnants of the merging with a low-mass companion Asa matter of fact GCs in low-mass galaxies are typically bluerthan in higher mass galaxies (eg Peng et al 2006) Neverthe-less because of the small size of the GC samples in the regionsinspected the average colors are in all regions consistent within1σ with the median colors of the bulk bona fide sample

The presence of substructures might also help to explain theobserved GCLF as they imply a dynamically young environ-ment Greggio et al (2014) pointed out the presence of a veryextended (out to simgt 30 kpc above the disk plane) intermediate

age AGB population in the inner halo of NGC 253 Assuming aconstant star formation rate the authors estimated that the AGBpopulation traces sim 2 times 108 M of stars formed between 05 and3 Gyr Hence some intermediate age (t sim 6 Gyr) metal-rich[FeH] simgt minus 03 star cluster falling in a similar color interval ofold and metal-poor GCs might be ldquocontaminatingrdquo the sampleof genuine old GCs Indeed the LFs in Figure 12 (right panels)resemble the one of star clusters in the LMC as shown for ex-ample in Fig 10 of Larsen (2002) In the panels of the figure weplot the linear fit to the data obtained from the LFs down to onemagnitude fainter than the TOM and the slope α for the power-law fit dN

dL prop Lα (see eqs 2-4 in Larsen 2002) The power-lawfit to the data provides exponents α sim minus21 similar to those typ-ically found in spirals and starburst galaxies (eg Miller et al1997 Whitmore et al 1999 Larsen 2002 Cantiello et al 2009)

43 Total GC population

Including the approximate fractions of missing GCs at small iesim 5 and large ie sim 7 of the total population galactocentricradii derived based on the properties of our best sample GCswe estimate a total number of GCs of NTotal

GC sim100 By using the

Article number page 12 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 12 Left Optical LFs of the bona fide sample GCs (gray shaded histogram) and of the bona fide+uncertain samples (dottedline) The adopted TOM in each band is shown with a vertical dashed line Right LFs of bona fide GCs shown in logarithmic scaleThe long-dashed line shows the power-law fit to the data The exponent of the fit is reported each panel (see text)

Fig 13 Radial density profile of the best GCs sample Left andright panels show the linear and r14-law profile respectivelyLinear fits to data are shown with blue dotted line The verticaldashed line indicates the semimajor axis where the dusty diskbegins

GC specific frequency S N6 versus magnitude relation (eg from

Peng et al 2008) it is possible to invert the relation and obtainan estimate of the total expected GC population for a galaxy likeNGC 253 Adopting S N sim 18 from the dotted curve in Figure 2of Peng et al (2008 derived from the analysis of Virgo cluster

6 A parameter relating the galaxy and the GC system properties quan-tified as the number of GCs per unit galaxy luminosity S N equiv NGC times

1004(MV +15) where NGC is the total number of clusters and MV is thetotal absolute visual magnitude of the galaxy (Harris amp van den Bergh1981 Harris 1991)

galaxies covering a wide range of luminosities) and MV sim minus21mag (Table 1) we get NTotal

GC sim 450 Assuming ∆S N sim 04 and∆MB sim 05 mag we also calculate an uncertainty ∆NTotal

GC sim 260This number decreases to NTotal

GC = 250 plusmn 200 if S N sim 1 is used(Harris et al 2013) Adopting such evaluations as strictly validleads to the conclusion that our best sample is a factor of two tofour incomplete

However the S N versus MV relation has a substantial scat-ter For example from the database by Harris et al (2013) itcan be seen that galaxies with MV = minus21 plusmn 02 mag have amedian population of sim 450 GCs with minimum at sim 40 anda maximum of sim 7000 It is worth emphasizing that based onprevious literature (Blecha 1986 Olsen et al 2004) Harris et al(2013) estimates the size of the GC system of NGC 253 to beNGC = 90 plusmn 40 If only galaxies with morphological classes andmagnitudes similar to NGC 253 are drawn from the Harris et al(2013) sample the median is NGC sim 80 The two galaxies withclosest morphological class and total magnitude to NGC 253(M 101 and NGC 6956) have a total population of detected GCswith NGC sim 90 plusmn 40 and 150 plusmn 40 which is consistent with thetotal (coverage corrected) population we estimated

Inspecting the radial profiles shown in Figure 13 we notea slight enhancement of GCs density at rgal sim 25 kpc Al-though the estimated errors are relatively high such enhance-ment roughly corresponds to the radial distance of the featurefirst found and discussed by Greggio et al (2014) identified asa possible stellar stream remnant However we must highlightthat our radial profile is derived from the azimuthal average ofGC counts while the RGB star counts excess found in Greggioet al (2014) is specifically located on the northwestern side ofthe galaxy

44 Color bimodality

A further typical element of discussion in extragalactic GC sys-tems is the color distribution In particular the presence of a

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Fig 14 Color-color diagrams for the bona fide and uncertain samples of GCs shown with blue filled dots and empty gray circlesrespectively The (arbitrarily scaled) histograms reported on the axes refer to the bona fide sample For optical colors the SPoT SSPmodels are also shown with lines as in Figure 4

nearly universal color bimodality in GC systems and the as-trophysical processes underlying such ubiquitous feature havegenerated a prolific and still open debate in the last decade(Spitler et al 2006 Yoon et al 2006 Cantiello amp Blakeslee2007 Chies-Santos et al 2012 Usher et al 2012 Brodie et al2014 Cantiello et al 2014) We adopted the bona fide sampleto verify the presence of color bimodality (ie to identify twowell-separated blue and red peaks) and to estimate the differ-ences between the two GC subpopulations in terms of the colordistributions To do so we used the Gaussian mixture model-ing code (GMM Muratov amp Gnedin 2010) The GMM codeuses the likelihood-ratio test to compare the goodness of fit fordouble-Gaussian versus a single-Gaussian For the best-fit dou-ble model it estimates the means and widths of the two com-ponents their separation DD in terms of combined widths andthe kurtosis of the overall distribution Values of DD larger thansim 2 and negative kurtosis are necessary but not sufficient condi-

tions for bimodality Also GMM provides uncertainties based onbootstrap resampling In addition the GMM analysis providesthe positions relative widths and fraction of objects associatedwith each peak

Inspecting the results reported in Table 4 (upper section ofthe table) GMM analysis shows that our bona fide GCs sampleis poorly fitted by two-Gaussian distributions in most of the in-spected colors This is testified by either the high p-values (Cols10-12 in the table) the changing fractions of red GCs ( f2) whendifferent colors are used the positive kurtosis or the low valuesfor the peak separation estimator (DD)

We also run GMM in three Gaussian peaks mode The re-sults reported in Table 5 are more satisfactory than the previ-ous as testified by the generally lower p-values The presence ofa third color peak is also visible as a red tail of GCs in the pan-els of Figure 14 The very red candidates are scattered aroundthe frame ie they are not sources close to the galaxy disk and

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Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 4 Results of GMM runs

Color Peak1 Peak2 σ1 σ2 NGC f2 DD Kurtosis p(χ2) p(DD) p(kurt) bi(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)uminusi 184 plusmn 014 220 plusmn 029 008 plusmn 007 030 plusmn 010 81 088 162 -004 0525 073 0675 Ngminusi 079 plusmn 006 122 plusmn 019 013 plusmn 004 011 plusmn 005 81 005 344 093 0050 014 0974 Yuminusr 159 plusmn 009 197 plusmn 013 012 plusmn 004 023 plusmn 006 81 081 206 -009 0634 061 0630 Niminusk 003 plusmn 010 063 plusmn 021 023 plusmn 007 026 plusmn 010 82 035 249 -059 0063 042 0157 Yrminus j 065 plusmn 004 095 plusmn 012 008 plusmn 003 025 plusmn 006 81 064 162 077 0004 074 0961 Ngminusk 055 plusmn 014 119 plusmn 030 012 plusmn 009 049 plusmn 012 81 079 179 -035 0026 070 0378 Yrminusi 022 plusmn 002 029 plusmn 003 003 plusmn 001 006 plusmn 001 82 068 141 042 0075 083 0895 Njminusk -037 plusmn 006 -003 plusmn 008 018 plusmn 003 005 plusmn 004 82 010 253 -045 0226 042 0271 N

Without the red GCsgminusi 067 plusmn 005 087 plusmn 005 007 plusmn 002 009 plusmn 002 76 061 239 -070 0444 048 0086 Numinusi 194 plusmn 006 236 plusmn 004 018 plusmn 003 011 plusmn 003 78 043 277 -091 0024 031 0013 Yuminusr 171 plusmn 006 207 plusmn 003 017 plusmn 003 008 plusmn 003 77 041 267 -097 0005 034 0006 Yiminusk 004 plusmn 009 056 plusmn 013 023 plusmn 006 013 plusmn 006 74 023 280 -070 0208 032 0081 Yrminus j 070 plusmn 004 107 plusmn 008 013 plusmn 003 007 plusmn 004 74 025 347 -095 0004 014 0012 Ygminusk 082 plusmn 012 151 plusmn 017 032 plusmn 010 014 plusmn 009 73 019 283 -085 0136 029 0032 Yrminusi 023 plusmn 001 032 plusmn 001 004 plusmn 001 001 plusmn 001 74 025 310 -097 0004 022 0011 Yjminusk -044 plusmn 010 -022 plusmn 006 015 plusmn 004 009 plusmn 003 72 026 174 -035 0705 071 0395 N

Notes Columns list (1) color (2-3) mean and uncertainty of the first and second peaks in the double-Gaussian model (4-5) width and uncertaintyof the first and second peaks (6) number of GC candidates selected (7) fraction of GC candidates associated with the second red peak (8)separation of the peaks in units of the two Gaussian widths (9) kurtosis of the distribution (DDge2 and negative kurtosis are required for significativesplit between the two Gaussian distributions) (10-12) GMM p-values based on the likelihood-ratio test p(χ2) peak separation p(DD) and kurtosisp(kurt) indicating the significance of the preference for a double-Gaussian over a single-Gaussian model (lower p-values are more significant)(13) assessment of the evidence for bimodality

Table 5 Results of GMM runs for the three Gaussian model

Color Peak1 (NGC σ) Peak2 (NGC σ) Peak3 (NGC σ) DD Kurtosis p(χ2) p(DD) p(kurt)uminusi 194 ( 4370 019 ) 236 ( 3330 012 ) 292 ( 400 006 ) 273 -004 0024 0351 0675gminusi 069 ( 3910 008 ) 088 ( 3020 006 ) 107 ( 1160 017 ) 254 093 0111 0511 0974uminusr 171 ( 4540 017 ) 207 ( 3160 008 ) 253 ( 400 005 ) 267 -009 0002 0459 0630iminusk 004 ( 5680 023 ) 056 ( 1660 012 ) 096 ( 860 008 ) 280 -059 0071 0345 0157rminus j 067 ( 4460 011 ) 104 ( 3540 017 ) 177 ( 100 004 ) 261 077 0002 0470 0961gminusk 069 ( 4300 025 ) 133 ( 3040 026 ) 209 ( 760 016 ) 249 -035 0122 0581 0597rminusi 023 ( 5340 004 ) 032 ( 1610 001 ) 036 ( 1250 006 ) 315 042 0047 0221 0895jminusk 044 ( 5320 015 ) -024 ( 1420 004 ) -003 ( 1450 007 ) 187 -045 0474 0618 0271

Notes Columns list (1) color (2-4) first second and third peaks in the three Gaussian model numbers within parentheses are the number of GCsassociated with each peak and the width of the distribution (5) separation of the peaks in units of the three Gaussian widths (6) kurtosis of thedistribution (7-9) GMM p-values as in Table 4

reddened by the dust In the Figure we report the color-color dia-grams together with color histograms for various colors and forthe bona fide GCs sample Taking advantage of the results on thepresence of such third peak we rerun GMM in double Gaussianmode after rejecting the candidate GCs in the third reddest peakGMM also provides as output a table with the probability mem-bership of each GCs to one of the fitted Gaussian The GMMresults of such a culled best sample again with a two Gaussianmodel are presented in the lower section of Table 4

Although the new GMM results for the selected GCs sampleappear with respect to the full bona fide sample more consistentwith a bimodal-color scenario there is no homogeneity of thevarious inspected colors as color bimodality is not coherentlyobserved in all colors In this respect then NGC 253 should cer-tainly not be considered a galaxy with a bimodal GC populationshowing coherent and consistent color bimodality

5 Conclusions

We summarize the conclusion of the present work dedicatedto the definition of an updated catalog of GC candidates inNGC 253 as follows

ndash The adoption of an even richer collection of color photomet-ric and morphologic parameters make the selection of GCcandidates more robust but does not guarantee the completeremoval of all contaminants

ndash Depending on the spatial resolution of the imaging data usedfor sources close enough such as the galaxy studied herethe foreground MW stars can be separated from GCs as thelatter appear extended with FWHM definitely larger thana point source In cases such as that presented here back-ground galaxies are the primary source of contamination

ndash About 10 of our candidates were already photometrically se-lected as GC candidates by other authors Conversely thelargest portion of GC candidates with photometric selectionin the literature are mostly identified as stars in our sample

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ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

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Fig 9 RGB thumbnails from VST data of star cluster candidates from Beasley amp Sharples (2000) that did not pass our selectioncriteria for GC candidates Starting from left B13 and B14 (close to galaxy dusty regions) and B29 and LA11 (likely backgroundgalaxies) Thumbnails are 15primeprime on each side

which passed morpho-photometric selection criteria but wererejected upon visual inspection

The catalog contains a total of 82 best GC candidates 155uncertain candidates and 110 sources which although passedall our GC selection criteria are clearly background galaxies

The spatial distribution of the full sample is shown in Figure11 overlaid to the g-band VST contours plot

We must note that our selection technique based also onaperture photometry leaves unanswered the question about thedetection efficiency and contamination rate as a function ofgalactocentric radius Although the majority of the globular clus-ter candidates are found in the uncrowded outskirts of the galaxya significant number are projected against or near the brightcrowded galaxy disk

As is also recognizable in Figure 3 sources detected in re-gions of high galaxy background suffer from a larger photomet-ric scatter because of the galaxy contamination and the presenceof dust

However of the sim 20 bona fide GCs candidates located ingalaxy regions with microg le 236 magarcsec2 only four are newselections the remaining are all either spectroscopically con-firmed GCs or star clusters selected on HSTGHOSTS data andthree are also photometric selections from Beasley amp Sharples(2000 Table 6 data)

42 Spatial distribution and luminosity function

The optical LF of the bona fide sample and the combination ofthe bona fide and uncertain samples are shown in Figure 12 (leftpanels) In the panels of the figure the MTOM adopted prop-erly shifted to the galaxy distance is also reported The dia-grams lack the typical symmetry around the peak of the GaussianGCLF which is surprising given that the bright side of the LF ap-pears underpopulated By inspecting the full sample of sourcesbrighter than mg sim 20 we found that even after adopting reason-ably broader selection criteria the list of bright candidates doesnot increase Hence we do not have an explanation for missingbright end of the GCLF

Taking only the sample of spectroscopically confirmed GCsdoes not improve the appearance of the GCLF because of thesmall size of the sample of 21 candidates and because 7 ofthe candidates are brighter than the MTOM and 14 are fainterthan that with the faintest candidate at mg sim 215 mag ie atsim 1σGCLF the level of the faint side GCLF If we also add theGCs identified over the HSTGHOSTS area the cumulative sam-ple of HST and spectroscopic candidates has sim 10 GCs that arebrighter than the MTOM and 41 fainter than the MTOM Hencewhether only the spectroscopic candidates or both spectroscopic

and GHOSTS candidates are considered again the GCLF ishighly undersampled toward bright GCs

The incompleteness is in part due to the photometric incom-pleteness which is caused by the different depth and image qual-ity of the imaging data adopted However photometric incom-pleteness should only be an issue at the faint end of the GCLF

An alternative explanation for the asymmetric GCLF wouldcome from overestimated low luminosity end of GCLF thatwould even in the case of best candidates have to be heavilycontaminated We believe this is not the case and thus rejectthis (potential) explanation because we have verified our selec-tion criteria through a comparison with HST GHOSTS imagesand with a spectroscopically confirmed sample of GCs Further-more if the low luminosity end were heavily contaminated theGC sample size in NGC 253 would be too small resulting in toosmall S N as we discuss further in Section 43

A further correction to the GCLF might come from thefact that in addition to photometric incompleteness our sampleis also incomplete at large and small galactocentric radii Thelargest projected galactocentric distance of a GC candidate inthe bona fide sample is rgal sim 35prime or sim 355 kpc A fraction ofsim 7 (11 out of 158) MW GCs are located at galactocentric dis-tance larger than sim355 kpc Hence it is reasonable to expect thata similar fraction of GCs in NGC 253 lies beyond the commonarea of the VST and VISTA pointings

For the central dusty regions as aforementioned we partiallyrecovered some of the GCs by complementing our data with theACS GCs from GHOSTS Nevertheless such detections mostlybased on visual inspection do not necessarily allow the recov-ery of the entire population of central GCs in the galaxy As acheck we inspected the azimuthal average of the GCs radialdensity profile reported in Figure 13 The diagram shows thelinear and r14 fits to the density profile which is derived with-out the data for the innermost two annuli severely affected bydust and incompleteness In both panels we observe a drop ofthe density profile in the very central regions otherwise the ra-dial (logarithmic) density profile nicely follows the fitted den-sity profiles The r14-law profile together with the increasing orflattening of the GC density profiles at small galactocentric radiiare well-known observational properties of GC systems (Dirschet al 2005 Goudfrooij et al 2007 Cantiello et al 2015) Con-sequently it is reasonable to assume that the drop in log ρ(rgal)seen in the left panels of Figure 12 is due to poor GCs detectionin such central dusty regions Even though the central area domi-nated by dust is relatively small sim 80 square arcmin the fractionof GCs there could be significative To obtain an approximate es-timate of the number of GCs in the central area we adopted theradial density profiles shown in Figure 13 assuming as lower

Article number page 10 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

(a) From left to right Cluster candidates number 99 109 111 124 128 and 141 in Table 3

(b) From left to right Cluster candidates number 178 186 200 204 205 and 207 in Table 3

(c) From left to right Cluster candidates number 209 210 211 218 227 and 325 in Table 3

(d) From left to right Cluster candidates number 333 334 335 and 336 in Table 3

(e) From left to right Sources 107 and 212 in Table 3 (confirmed background galaxies) and two of the sources identified as stars in our selectionprocedure

(f) From left to right Sources 326 327 328 329330 331 and 332 in Table 3 visually identified as GCs and located within the dust diskof NGC 253

Fig 10 Upper four rows (a-d) Hubble Space Telescope ACS cutouts of the sources selected as GCs candidates and falling in theGHOSTS survey footprints (F814W-band imaging data are shown) Given the mottled appearance we consider all sources as starclusters in the galaxy For reference the panels in row (e) show the other two selected sources in the GHOSTS footprints whichare obvious background galaxies and two stellar sources The sources in the row ( f ) are the visually identified GC candidates (seetext)

limit to the GCs density the value of ρ(rgal) at rgal sim 11prime iethe galactocentric radius where the dusty disk begins Adoptingthe linear or r14-law fits the fitted GC density at rgal sim 11prime goesfrom sim 0045 GCsarcmin2 to sim 0057 GCsarcmin2 Hencethe estimated number of GCs in the central area is Ncenter

GC sim 5

In a study of RGB-tip field star population based on V and IMagellanIMACS data Bailin et al (2011) found evidence for alarge shelf-like feature near the southeast side of NGC 253 (alsoconfirmed by Greggio et al 2014 from resolved star analysesof the VISTA imaging data used in this work) Using GHOSTSdata in two fields - one on and one off the shelf - the authors in-

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Fig 11 GC candidates overlaid to the g-band contour plot of NGC 253 Green five-pointed stars blue squares and red trianglesshow the candidates flagged as Best Uncertain and No in Table 3 respectively The plotted contours show the microg =236 230 224218 212 206 magarcsec2 surface brightness levels respectively

spected the color distribution of RGB-tip stars and found that thefeature is possibly the remnant of a large satellite of the mergingtree of NGC 253 Yet the authors warned that the stellar popu-lations in the two fields are not dramatically different from therest of the halo at similar elliptical radii Inspecting the colorsof our bona fide GCs in various regions around the galaxy wefind that the sim15 GC candidates in the projected region closeto the shelf identified by Bailin et al (2011) have average col-ors that are bluer than the colors of GCs in other four randomlydrawn regions and than the bulk of the bona fide sample Thismight further strengthen the hypothesis of the presence of a sur-face brightness feature and of a GCs subpopulation which areboth remnants of the merging with a low-mass companion Asa matter of fact GCs in low-mass galaxies are typically bluerthan in higher mass galaxies (eg Peng et al 2006) Neverthe-less because of the small size of the GC samples in the regionsinspected the average colors are in all regions consistent within1σ with the median colors of the bulk bona fide sample

The presence of substructures might also help to explain theobserved GCLF as they imply a dynamically young environ-ment Greggio et al (2014) pointed out the presence of a veryextended (out to simgt 30 kpc above the disk plane) intermediate

age AGB population in the inner halo of NGC 253 Assuming aconstant star formation rate the authors estimated that the AGBpopulation traces sim 2 times 108 M of stars formed between 05 and3 Gyr Hence some intermediate age (t sim 6 Gyr) metal-rich[FeH] simgt minus 03 star cluster falling in a similar color interval ofold and metal-poor GCs might be ldquocontaminatingrdquo the sampleof genuine old GCs Indeed the LFs in Figure 12 (right panels)resemble the one of star clusters in the LMC as shown for ex-ample in Fig 10 of Larsen (2002) In the panels of the figure weplot the linear fit to the data obtained from the LFs down to onemagnitude fainter than the TOM and the slope α for the power-law fit dN

dL prop Lα (see eqs 2-4 in Larsen 2002) The power-lawfit to the data provides exponents α sim minus21 similar to those typ-ically found in spirals and starburst galaxies (eg Miller et al1997 Whitmore et al 1999 Larsen 2002 Cantiello et al 2009)

43 Total GC population

Including the approximate fractions of missing GCs at small iesim 5 and large ie sim 7 of the total population galactocentricradii derived based on the properties of our best sample GCswe estimate a total number of GCs of NTotal

GC sim100 By using the

Article number page 12 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 12 Left Optical LFs of the bona fide sample GCs (gray shaded histogram) and of the bona fide+uncertain samples (dottedline) The adopted TOM in each band is shown with a vertical dashed line Right LFs of bona fide GCs shown in logarithmic scaleThe long-dashed line shows the power-law fit to the data The exponent of the fit is reported each panel (see text)

Fig 13 Radial density profile of the best GCs sample Left andright panels show the linear and r14-law profile respectivelyLinear fits to data are shown with blue dotted line The verticaldashed line indicates the semimajor axis where the dusty diskbegins

GC specific frequency S N6 versus magnitude relation (eg from

Peng et al 2008) it is possible to invert the relation and obtainan estimate of the total expected GC population for a galaxy likeNGC 253 Adopting S N sim 18 from the dotted curve in Figure 2of Peng et al (2008 derived from the analysis of Virgo cluster

6 A parameter relating the galaxy and the GC system properties quan-tified as the number of GCs per unit galaxy luminosity S N equiv NGC times

1004(MV +15) where NGC is the total number of clusters and MV is thetotal absolute visual magnitude of the galaxy (Harris amp van den Bergh1981 Harris 1991)

galaxies covering a wide range of luminosities) and MV sim minus21mag (Table 1) we get NTotal

GC sim 450 Assuming ∆S N sim 04 and∆MB sim 05 mag we also calculate an uncertainty ∆NTotal

GC sim 260This number decreases to NTotal

GC = 250 plusmn 200 if S N sim 1 is used(Harris et al 2013) Adopting such evaluations as strictly validleads to the conclusion that our best sample is a factor of two tofour incomplete

However the S N versus MV relation has a substantial scat-ter For example from the database by Harris et al (2013) itcan be seen that galaxies with MV = minus21 plusmn 02 mag have amedian population of sim 450 GCs with minimum at sim 40 anda maximum of sim 7000 It is worth emphasizing that based onprevious literature (Blecha 1986 Olsen et al 2004) Harris et al(2013) estimates the size of the GC system of NGC 253 to beNGC = 90 plusmn 40 If only galaxies with morphological classes andmagnitudes similar to NGC 253 are drawn from the Harris et al(2013) sample the median is NGC sim 80 The two galaxies withclosest morphological class and total magnitude to NGC 253(M 101 and NGC 6956) have a total population of detected GCswith NGC sim 90 plusmn 40 and 150 plusmn 40 which is consistent with thetotal (coverage corrected) population we estimated

Inspecting the radial profiles shown in Figure 13 we notea slight enhancement of GCs density at rgal sim 25 kpc Al-though the estimated errors are relatively high such enhance-ment roughly corresponds to the radial distance of the featurefirst found and discussed by Greggio et al (2014) identified asa possible stellar stream remnant However we must highlightthat our radial profile is derived from the azimuthal average ofGC counts while the RGB star counts excess found in Greggioet al (2014) is specifically located on the northwestern side ofthe galaxy

44 Color bimodality

A further typical element of discussion in extragalactic GC sys-tems is the color distribution In particular the presence of a

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Fig 14 Color-color diagrams for the bona fide and uncertain samples of GCs shown with blue filled dots and empty gray circlesrespectively The (arbitrarily scaled) histograms reported on the axes refer to the bona fide sample For optical colors the SPoT SSPmodels are also shown with lines as in Figure 4

nearly universal color bimodality in GC systems and the as-trophysical processes underlying such ubiquitous feature havegenerated a prolific and still open debate in the last decade(Spitler et al 2006 Yoon et al 2006 Cantiello amp Blakeslee2007 Chies-Santos et al 2012 Usher et al 2012 Brodie et al2014 Cantiello et al 2014) We adopted the bona fide sampleto verify the presence of color bimodality (ie to identify twowell-separated blue and red peaks) and to estimate the differ-ences between the two GC subpopulations in terms of the colordistributions To do so we used the Gaussian mixture model-ing code (GMM Muratov amp Gnedin 2010) The GMM codeuses the likelihood-ratio test to compare the goodness of fit fordouble-Gaussian versus a single-Gaussian For the best-fit dou-ble model it estimates the means and widths of the two com-ponents their separation DD in terms of combined widths andthe kurtosis of the overall distribution Values of DD larger thansim 2 and negative kurtosis are necessary but not sufficient condi-

tions for bimodality Also GMM provides uncertainties based onbootstrap resampling In addition the GMM analysis providesthe positions relative widths and fraction of objects associatedwith each peak

Inspecting the results reported in Table 4 (upper section ofthe table) GMM analysis shows that our bona fide GCs sampleis poorly fitted by two-Gaussian distributions in most of the in-spected colors This is testified by either the high p-values (Cols10-12 in the table) the changing fractions of red GCs ( f2) whendifferent colors are used the positive kurtosis or the low valuesfor the peak separation estimator (DD)

We also run GMM in three Gaussian peaks mode The re-sults reported in Table 5 are more satisfactory than the previ-ous as testified by the generally lower p-values The presence ofa third color peak is also visible as a red tail of GCs in the pan-els of Figure 14 The very red candidates are scattered aroundthe frame ie they are not sources close to the galaxy disk and

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Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 4 Results of GMM runs

Color Peak1 Peak2 σ1 σ2 NGC f2 DD Kurtosis p(χ2) p(DD) p(kurt) bi(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)uminusi 184 plusmn 014 220 plusmn 029 008 plusmn 007 030 plusmn 010 81 088 162 -004 0525 073 0675 Ngminusi 079 plusmn 006 122 plusmn 019 013 plusmn 004 011 plusmn 005 81 005 344 093 0050 014 0974 Yuminusr 159 plusmn 009 197 plusmn 013 012 plusmn 004 023 plusmn 006 81 081 206 -009 0634 061 0630 Niminusk 003 plusmn 010 063 plusmn 021 023 plusmn 007 026 plusmn 010 82 035 249 -059 0063 042 0157 Yrminus j 065 plusmn 004 095 plusmn 012 008 plusmn 003 025 plusmn 006 81 064 162 077 0004 074 0961 Ngminusk 055 plusmn 014 119 plusmn 030 012 plusmn 009 049 plusmn 012 81 079 179 -035 0026 070 0378 Yrminusi 022 plusmn 002 029 plusmn 003 003 plusmn 001 006 plusmn 001 82 068 141 042 0075 083 0895 Njminusk -037 plusmn 006 -003 plusmn 008 018 plusmn 003 005 plusmn 004 82 010 253 -045 0226 042 0271 N

Without the red GCsgminusi 067 plusmn 005 087 plusmn 005 007 plusmn 002 009 plusmn 002 76 061 239 -070 0444 048 0086 Numinusi 194 plusmn 006 236 plusmn 004 018 plusmn 003 011 plusmn 003 78 043 277 -091 0024 031 0013 Yuminusr 171 plusmn 006 207 plusmn 003 017 plusmn 003 008 plusmn 003 77 041 267 -097 0005 034 0006 Yiminusk 004 plusmn 009 056 plusmn 013 023 plusmn 006 013 plusmn 006 74 023 280 -070 0208 032 0081 Yrminus j 070 plusmn 004 107 plusmn 008 013 plusmn 003 007 plusmn 004 74 025 347 -095 0004 014 0012 Ygminusk 082 plusmn 012 151 plusmn 017 032 plusmn 010 014 plusmn 009 73 019 283 -085 0136 029 0032 Yrminusi 023 plusmn 001 032 plusmn 001 004 plusmn 001 001 plusmn 001 74 025 310 -097 0004 022 0011 Yjminusk -044 plusmn 010 -022 plusmn 006 015 plusmn 004 009 plusmn 003 72 026 174 -035 0705 071 0395 N

Notes Columns list (1) color (2-3) mean and uncertainty of the first and second peaks in the double-Gaussian model (4-5) width and uncertaintyof the first and second peaks (6) number of GC candidates selected (7) fraction of GC candidates associated with the second red peak (8)separation of the peaks in units of the two Gaussian widths (9) kurtosis of the distribution (DDge2 and negative kurtosis are required for significativesplit between the two Gaussian distributions) (10-12) GMM p-values based on the likelihood-ratio test p(χ2) peak separation p(DD) and kurtosisp(kurt) indicating the significance of the preference for a double-Gaussian over a single-Gaussian model (lower p-values are more significant)(13) assessment of the evidence for bimodality

Table 5 Results of GMM runs for the three Gaussian model

Color Peak1 (NGC σ) Peak2 (NGC σ) Peak3 (NGC σ) DD Kurtosis p(χ2) p(DD) p(kurt)uminusi 194 ( 4370 019 ) 236 ( 3330 012 ) 292 ( 400 006 ) 273 -004 0024 0351 0675gminusi 069 ( 3910 008 ) 088 ( 3020 006 ) 107 ( 1160 017 ) 254 093 0111 0511 0974uminusr 171 ( 4540 017 ) 207 ( 3160 008 ) 253 ( 400 005 ) 267 -009 0002 0459 0630iminusk 004 ( 5680 023 ) 056 ( 1660 012 ) 096 ( 860 008 ) 280 -059 0071 0345 0157rminus j 067 ( 4460 011 ) 104 ( 3540 017 ) 177 ( 100 004 ) 261 077 0002 0470 0961gminusk 069 ( 4300 025 ) 133 ( 3040 026 ) 209 ( 760 016 ) 249 -035 0122 0581 0597rminusi 023 ( 5340 004 ) 032 ( 1610 001 ) 036 ( 1250 006 ) 315 042 0047 0221 0895jminusk 044 ( 5320 015 ) -024 ( 1420 004 ) -003 ( 1450 007 ) 187 -045 0474 0618 0271

Notes Columns list (1) color (2-4) first second and third peaks in the three Gaussian model numbers within parentheses are the number of GCsassociated with each peak and the width of the distribution (5) separation of the peaks in units of the three Gaussian widths (6) kurtosis of thedistribution (7-9) GMM p-values as in Table 4

reddened by the dust In the Figure we report the color-color dia-grams together with color histograms for various colors and forthe bona fide GCs sample Taking advantage of the results on thepresence of such third peak we rerun GMM in double Gaussianmode after rejecting the candidate GCs in the third reddest peakGMM also provides as output a table with the probability mem-bership of each GCs to one of the fitted Gaussian The GMMresults of such a culled best sample again with a two Gaussianmodel are presented in the lower section of Table 4

Although the new GMM results for the selected GCs sampleappear with respect to the full bona fide sample more consistentwith a bimodal-color scenario there is no homogeneity of thevarious inspected colors as color bimodality is not coherentlyobserved in all colors In this respect then NGC 253 should cer-tainly not be considered a galaxy with a bimodal GC populationshowing coherent and consistent color bimodality

5 Conclusions

We summarize the conclusion of the present work dedicatedto the definition of an updated catalog of GC candidates inNGC 253 as follows

ndash The adoption of an even richer collection of color photomet-ric and morphologic parameters make the selection of GCcandidates more robust but does not guarantee the completeremoval of all contaminants

ndash Depending on the spatial resolution of the imaging data usedfor sources close enough such as the galaxy studied herethe foreground MW stars can be separated from GCs as thelatter appear extended with FWHM definitely larger thana point source In cases such as that presented here back-ground galaxies are the primary source of contamination

ndash About 10 of our candidates were already photometrically se-lected as GC candidates by other authors Conversely thelargest portion of GC candidates with photometric selectionin the literature are mostly identified as stars in our sample

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ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

Article number page 16 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

(a) From left to right Cluster candidates number 99 109 111 124 128 and 141 in Table 3

(b) From left to right Cluster candidates number 178 186 200 204 205 and 207 in Table 3

(c) From left to right Cluster candidates number 209 210 211 218 227 and 325 in Table 3

(d) From left to right Cluster candidates number 333 334 335 and 336 in Table 3

(e) From left to right Sources 107 and 212 in Table 3 (confirmed background galaxies) and two of the sources identified as stars in our selectionprocedure

(f) From left to right Sources 326 327 328 329330 331 and 332 in Table 3 visually identified as GCs and located within the dust diskof NGC 253

Fig 10 Upper four rows (a-d) Hubble Space Telescope ACS cutouts of the sources selected as GCs candidates and falling in theGHOSTS survey footprints (F814W-band imaging data are shown) Given the mottled appearance we consider all sources as starclusters in the galaxy For reference the panels in row (e) show the other two selected sources in the GHOSTS footprints whichare obvious background galaxies and two stellar sources The sources in the row ( f ) are the visually identified GC candidates (seetext)

limit to the GCs density the value of ρ(rgal) at rgal sim 11prime iethe galactocentric radius where the dusty disk begins Adoptingthe linear or r14-law fits the fitted GC density at rgal sim 11prime goesfrom sim 0045 GCsarcmin2 to sim 0057 GCsarcmin2 Hencethe estimated number of GCs in the central area is Ncenter

GC sim 5

In a study of RGB-tip field star population based on V and IMagellanIMACS data Bailin et al (2011) found evidence for alarge shelf-like feature near the southeast side of NGC 253 (alsoconfirmed by Greggio et al 2014 from resolved star analysesof the VISTA imaging data used in this work) Using GHOSTSdata in two fields - one on and one off the shelf - the authors in-

Article number page 11 of 24

AampA proofs manuscript no ms_printer_v11

Fig 11 GC candidates overlaid to the g-band contour plot of NGC 253 Green five-pointed stars blue squares and red trianglesshow the candidates flagged as Best Uncertain and No in Table 3 respectively The plotted contours show the microg =236 230 224218 212 206 magarcsec2 surface brightness levels respectively

spected the color distribution of RGB-tip stars and found that thefeature is possibly the remnant of a large satellite of the mergingtree of NGC 253 Yet the authors warned that the stellar popu-lations in the two fields are not dramatically different from therest of the halo at similar elliptical radii Inspecting the colorsof our bona fide GCs in various regions around the galaxy wefind that the sim15 GC candidates in the projected region closeto the shelf identified by Bailin et al (2011) have average col-ors that are bluer than the colors of GCs in other four randomlydrawn regions and than the bulk of the bona fide sample Thismight further strengthen the hypothesis of the presence of a sur-face brightness feature and of a GCs subpopulation which areboth remnants of the merging with a low-mass companion Asa matter of fact GCs in low-mass galaxies are typically bluerthan in higher mass galaxies (eg Peng et al 2006) Neverthe-less because of the small size of the GC samples in the regionsinspected the average colors are in all regions consistent within1σ with the median colors of the bulk bona fide sample

The presence of substructures might also help to explain theobserved GCLF as they imply a dynamically young environ-ment Greggio et al (2014) pointed out the presence of a veryextended (out to simgt 30 kpc above the disk plane) intermediate

age AGB population in the inner halo of NGC 253 Assuming aconstant star formation rate the authors estimated that the AGBpopulation traces sim 2 times 108 M of stars formed between 05 and3 Gyr Hence some intermediate age (t sim 6 Gyr) metal-rich[FeH] simgt minus 03 star cluster falling in a similar color interval ofold and metal-poor GCs might be ldquocontaminatingrdquo the sampleof genuine old GCs Indeed the LFs in Figure 12 (right panels)resemble the one of star clusters in the LMC as shown for ex-ample in Fig 10 of Larsen (2002) In the panels of the figure weplot the linear fit to the data obtained from the LFs down to onemagnitude fainter than the TOM and the slope α for the power-law fit dN

dL prop Lα (see eqs 2-4 in Larsen 2002) The power-lawfit to the data provides exponents α sim minus21 similar to those typ-ically found in spirals and starburst galaxies (eg Miller et al1997 Whitmore et al 1999 Larsen 2002 Cantiello et al 2009)

43 Total GC population

Including the approximate fractions of missing GCs at small iesim 5 and large ie sim 7 of the total population galactocentricradii derived based on the properties of our best sample GCswe estimate a total number of GCs of NTotal

GC sim100 By using the

Article number page 12 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 12 Left Optical LFs of the bona fide sample GCs (gray shaded histogram) and of the bona fide+uncertain samples (dottedline) The adopted TOM in each band is shown with a vertical dashed line Right LFs of bona fide GCs shown in logarithmic scaleThe long-dashed line shows the power-law fit to the data The exponent of the fit is reported each panel (see text)

Fig 13 Radial density profile of the best GCs sample Left andright panels show the linear and r14-law profile respectivelyLinear fits to data are shown with blue dotted line The verticaldashed line indicates the semimajor axis where the dusty diskbegins

GC specific frequency S N6 versus magnitude relation (eg from

Peng et al 2008) it is possible to invert the relation and obtainan estimate of the total expected GC population for a galaxy likeNGC 253 Adopting S N sim 18 from the dotted curve in Figure 2of Peng et al (2008 derived from the analysis of Virgo cluster

6 A parameter relating the galaxy and the GC system properties quan-tified as the number of GCs per unit galaxy luminosity S N equiv NGC times

1004(MV +15) where NGC is the total number of clusters and MV is thetotal absolute visual magnitude of the galaxy (Harris amp van den Bergh1981 Harris 1991)

galaxies covering a wide range of luminosities) and MV sim minus21mag (Table 1) we get NTotal

GC sim 450 Assuming ∆S N sim 04 and∆MB sim 05 mag we also calculate an uncertainty ∆NTotal

GC sim 260This number decreases to NTotal

GC = 250 plusmn 200 if S N sim 1 is used(Harris et al 2013) Adopting such evaluations as strictly validleads to the conclusion that our best sample is a factor of two tofour incomplete

However the S N versus MV relation has a substantial scat-ter For example from the database by Harris et al (2013) itcan be seen that galaxies with MV = minus21 plusmn 02 mag have amedian population of sim 450 GCs with minimum at sim 40 anda maximum of sim 7000 It is worth emphasizing that based onprevious literature (Blecha 1986 Olsen et al 2004) Harris et al(2013) estimates the size of the GC system of NGC 253 to beNGC = 90 plusmn 40 If only galaxies with morphological classes andmagnitudes similar to NGC 253 are drawn from the Harris et al(2013) sample the median is NGC sim 80 The two galaxies withclosest morphological class and total magnitude to NGC 253(M 101 and NGC 6956) have a total population of detected GCswith NGC sim 90 plusmn 40 and 150 plusmn 40 which is consistent with thetotal (coverage corrected) population we estimated

Inspecting the radial profiles shown in Figure 13 we notea slight enhancement of GCs density at rgal sim 25 kpc Al-though the estimated errors are relatively high such enhance-ment roughly corresponds to the radial distance of the featurefirst found and discussed by Greggio et al (2014) identified asa possible stellar stream remnant However we must highlightthat our radial profile is derived from the azimuthal average ofGC counts while the RGB star counts excess found in Greggioet al (2014) is specifically located on the northwestern side ofthe galaxy

44 Color bimodality

A further typical element of discussion in extragalactic GC sys-tems is the color distribution In particular the presence of a

Article number page 13 of 24

AampA proofs manuscript no ms_printer_v11

Fig 14 Color-color diagrams for the bona fide and uncertain samples of GCs shown with blue filled dots and empty gray circlesrespectively The (arbitrarily scaled) histograms reported on the axes refer to the bona fide sample For optical colors the SPoT SSPmodels are also shown with lines as in Figure 4

nearly universal color bimodality in GC systems and the as-trophysical processes underlying such ubiquitous feature havegenerated a prolific and still open debate in the last decade(Spitler et al 2006 Yoon et al 2006 Cantiello amp Blakeslee2007 Chies-Santos et al 2012 Usher et al 2012 Brodie et al2014 Cantiello et al 2014) We adopted the bona fide sampleto verify the presence of color bimodality (ie to identify twowell-separated blue and red peaks) and to estimate the differ-ences between the two GC subpopulations in terms of the colordistributions To do so we used the Gaussian mixture model-ing code (GMM Muratov amp Gnedin 2010) The GMM codeuses the likelihood-ratio test to compare the goodness of fit fordouble-Gaussian versus a single-Gaussian For the best-fit dou-ble model it estimates the means and widths of the two com-ponents their separation DD in terms of combined widths andthe kurtosis of the overall distribution Values of DD larger thansim 2 and negative kurtosis are necessary but not sufficient condi-

tions for bimodality Also GMM provides uncertainties based onbootstrap resampling In addition the GMM analysis providesthe positions relative widths and fraction of objects associatedwith each peak

Inspecting the results reported in Table 4 (upper section ofthe table) GMM analysis shows that our bona fide GCs sampleis poorly fitted by two-Gaussian distributions in most of the in-spected colors This is testified by either the high p-values (Cols10-12 in the table) the changing fractions of red GCs ( f2) whendifferent colors are used the positive kurtosis or the low valuesfor the peak separation estimator (DD)

We also run GMM in three Gaussian peaks mode The re-sults reported in Table 5 are more satisfactory than the previ-ous as testified by the generally lower p-values The presence ofa third color peak is also visible as a red tail of GCs in the pan-els of Figure 14 The very red candidates are scattered aroundthe frame ie they are not sources close to the galaxy disk and

Article number page 14 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 4 Results of GMM runs

Color Peak1 Peak2 σ1 σ2 NGC f2 DD Kurtosis p(χ2) p(DD) p(kurt) bi(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)uminusi 184 plusmn 014 220 plusmn 029 008 plusmn 007 030 plusmn 010 81 088 162 -004 0525 073 0675 Ngminusi 079 plusmn 006 122 plusmn 019 013 plusmn 004 011 plusmn 005 81 005 344 093 0050 014 0974 Yuminusr 159 plusmn 009 197 plusmn 013 012 plusmn 004 023 plusmn 006 81 081 206 -009 0634 061 0630 Niminusk 003 plusmn 010 063 plusmn 021 023 plusmn 007 026 plusmn 010 82 035 249 -059 0063 042 0157 Yrminus j 065 plusmn 004 095 plusmn 012 008 plusmn 003 025 plusmn 006 81 064 162 077 0004 074 0961 Ngminusk 055 plusmn 014 119 plusmn 030 012 plusmn 009 049 plusmn 012 81 079 179 -035 0026 070 0378 Yrminusi 022 plusmn 002 029 plusmn 003 003 plusmn 001 006 plusmn 001 82 068 141 042 0075 083 0895 Njminusk -037 plusmn 006 -003 plusmn 008 018 plusmn 003 005 plusmn 004 82 010 253 -045 0226 042 0271 N

Without the red GCsgminusi 067 plusmn 005 087 plusmn 005 007 plusmn 002 009 plusmn 002 76 061 239 -070 0444 048 0086 Numinusi 194 plusmn 006 236 plusmn 004 018 plusmn 003 011 plusmn 003 78 043 277 -091 0024 031 0013 Yuminusr 171 plusmn 006 207 plusmn 003 017 plusmn 003 008 plusmn 003 77 041 267 -097 0005 034 0006 Yiminusk 004 plusmn 009 056 plusmn 013 023 plusmn 006 013 plusmn 006 74 023 280 -070 0208 032 0081 Yrminus j 070 plusmn 004 107 plusmn 008 013 plusmn 003 007 plusmn 004 74 025 347 -095 0004 014 0012 Ygminusk 082 plusmn 012 151 plusmn 017 032 plusmn 010 014 plusmn 009 73 019 283 -085 0136 029 0032 Yrminusi 023 plusmn 001 032 plusmn 001 004 plusmn 001 001 plusmn 001 74 025 310 -097 0004 022 0011 Yjminusk -044 plusmn 010 -022 plusmn 006 015 plusmn 004 009 plusmn 003 72 026 174 -035 0705 071 0395 N

Notes Columns list (1) color (2-3) mean and uncertainty of the first and second peaks in the double-Gaussian model (4-5) width and uncertaintyof the first and second peaks (6) number of GC candidates selected (7) fraction of GC candidates associated with the second red peak (8)separation of the peaks in units of the two Gaussian widths (9) kurtosis of the distribution (DDge2 and negative kurtosis are required for significativesplit between the two Gaussian distributions) (10-12) GMM p-values based on the likelihood-ratio test p(χ2) peak separation p(DD) and kurtosisp(kurt) indicating the significance of the preference for a double-Gaussian over a single-Gaussian model (lower p-values are more significant)(13) assessment of the evidence for bimodality

Table 5 Results of GMM runs for the three Gaussian model

Color Peak1 (NGC σ) Peak2 (NGC σ) Peak3 (NGC σ) DD Kurtosis p(χ2) p(DD) p(kurt)uminusi 194 ( 4370 019 ) 236 ( 3330 012 ) 292 ( 400 006 ) 273 -004 0024 0351 0675gminusi 069 ( 3910 008 ) 088 ( 3020 006 ) 107 ( 1160 017 ) 254 093 0111 0511 0974uminusr 171 ( 4540 017 ) 207 ( 3160 008 ) 253 ( 400 005 ) 267 -009 0002 0459 0630iminusk 004 ( 5680 023 ) 056 ( 1660 012 ) 096 ( 860 008 ) 280 -059 0071 0345 0157rminus j 067 ( 4460 011 ) 104 ( 3540 017 ) 177 ( 100 004 ) 261 077 0002 0470 0961gminusk 069 ( 4300 025 ) 133 ( 3040 026 ) 209 ( 760 016 ) 249 -035 0122 0581 0597rminusi 023 ( 5340 004 ) 032 ( 1610 001 ) 036 ( 1250 006 ) 315 042 0047 0221 0895jminusk 044 ( 5320 015 ) -024 ( 1420 004 ) -003 ( 1450 007 ) 187 -045 0474 0618 0271

Notes Columns list (1) color (2-4) first second and third peaks in the three Gaussian model numbers within parentheses are the number of GCsassociated with each peak and the width of the distribution (5) separation of the peaks in units of the three Gaussian widths (6) kurtosis of thedistribution (7-9) GMM p-values as in Table 4

reddened by the dust In the Figure we report the color-color dia-grams together with color histograms for various colors and forthe bona fide GCs sample Taking advantage of the results on thepresence of such third peak we rerun GMM in double Gaussianmode after rejecting the candidate GCs in the third reddest peakGMM also provides as output a table with the probability mem-bership of each GCs to one of the fitted Gaussian The GMMresults of such a culled best sample again with a two Gaussianmodel are presented in the lower section of Table 4

Although the new GMM results for the selected GCs sampleappear with respect to the full bona fide sample more consistentwith a bimodal-color scenario there is no homogeneity of thevarious inspected colors as color bimodality is not coherentlyobserved in all colors In this respect then NGC 253 should cer-tainly not be considered a galaxy with a bimodal GC populationshowing coherent and consistent color bimodality

5 Conclusions

We summarize the conclusion of the present work dedicatedto the definition of an updated catalog of GC candidates inNGC 253 as follows

ndash The adoption of an even richer collection of color photomet-ric and morphologic parameters make the selection of GCcandidates more robust but does not guarantee the completeremoval of all contaminants

ndash Depending on the spatial resolution of the imaging data usedfor sources close enough such as the galaxy studied herethe foreground MW stars can be separated from GCs as thelatter appear extended with FWHM definitely larger thana point source In cases such as that presented here back-ground galaxies are the primary source of contamination

ndash About 10 of our candidates were already photometrically se-lected as GC candidates by other authors Conversely thelargest portion of GC candidates with photometric selectionin the literature are mostly identified as stars in our sample

Article number page 15 of 24

AampA proofs manuscript no ms_printer_v11

ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

Article number page 16 of 24

AampA proofs manuscript no ms_printer_v11

Fig 11 GC candidates overlaid to the g-band contour plot of NGC 253 Green five-pointed stars blue squares and red trianglesshow the candidates flagged as Best Uncertain and No in Table 3 respectively The plotted contours show the microg =236 230 224218 212 206 magarcsec2 surface brightness levels respectively

spected the color distribution of RGB-tip stars and found that thefeature is possibly the remnant of a large satellite of the mergingtree of NGC 253 Yet the authors warned that the stellar popu-lations in the two fields are not dramatically different from therest of the halo at similar elliptical radii Inspecting the colorsof our bona fide GCs in various regions around the galaxy wefind that the sim15 GC candidates in the projected region closeto the shelf identified by Bailin et al (2011) have average col-ors that are bluer than the colors of GCs in other four randomlydrawn regions and than the bulk of the bona fide sample Thismight further strengthen the hypothesis of the presence of a sur-face brightness feature and of a GCs subpopulation which areboth remnants of the merging with a low-mass companion Asa matter of fact GCs in low-mass galaxies are typically bluerthan in higher mass galaxies (eg Peng et al 2006) Neverthe-less because of the small size of the GC samples in the regionsinspected the average colors are in all regions consistent within1σ with the median colors of the bulk bona fide sample

The presence of substructures might also help to explain theobserved GCLF as they imply a dynamically young environ-ment Greggio et al (2014) pointed out the presence of a veryextended (out to simgt 30 kpc above the disk plane) intermediate

age AGB population in the inner halo of NGC 253 Assuming aconstant star formation rate the authors estimated that the AGBpopulation traces sim 2 times 108 M of stars formed between 05 and3 Gyr Hence some intermediate age (t sim 6 Gyr) metal-rich[FeH] simgt minus 03 star cluster falling in a similar color interval ofold and metal-poor GCs might be ldquocontaminatingrdquo the sampleof genuine old GCs Indeed the LFs in Figure 12 (right panels)resemble the one of star clusters in the LMC as shown for ex-ample in Fig 10 of Larsen (2002) In the panels of the figure weplot the linear fit to the data obtained from the LFs down to onemagnitude fainter than the TOM and the slope α for the power-law fit dN

dL prop Lα (see eqs 2-4 in Larsen 2002) The power-lawfit to the data provides exponents α sim minus21 similar to those typ-ically found in spirals and starburst galaxies (eg Miller et al1997 Whitmore et al 1999 Larsen 2002 Cantiello et al 2009)

43 Total GC population

Including the approximate fractions of missing GCs at small iesim 5 and large ie sim 7 of the total population galactocentricradii derived based on the properties of our best sample GCswe estimate a total number of GCs of NTotal

GC sim100 By using the

Article number page 12 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 12 Left Optical LFs of the bona fide sample GCs (gray shaded histogram) and of the bona fide+uncertain samples (dottedline) The adopted TOM in each band is shown with a vertical dashed line Right LFs of bona fide GCs shown in logarithmic scaleThe long-dashed line shows the power-law fit to the data The exponent of the fit is reported each panel (see text)

Fig 13 Radial density profile of the best GCs sample Left andright panels show the linear and r14-law profile respectivelyLinear fits to data are shown with blue dotted line The verticaldashed line indicates the semimajor axis where the dusty diskbegins

GC specific frequency S N6 versus magnitude relation (eg from

Peng et al 2008) it is possible to invert the relation and obtainan estimate of the total expected GC population for a galaxy likeNGC 253 Adopting S N sim 18 from the dotted curve in Figure 2of Peng et al (2008 derived from the analysis of Virgo cluster

6 A parameter relating the galaxy and the GC system properties quan-tified as the number of GCs per unit galaxy luminosity S N equiv NGC times

1004(MV +15) where NGC is the total number of clusters and MV is thetotal absolute visual magnitude of the galaxy (Harris amp van den Bergh1981 Harris 1991)

galaxies covering a wide range of luminosities) and MV sim minus21mag (Table 1) we get NTotal

GC sim 450 Assuming ∆S N sim 04 and∆MB sim 05 mag we also calculate an uncertainty ∆NTotal

GC sim 260This number decreases to NTotal

GC = 250 plusmn 200 if S N sim 1 is used(Harris et al 2013) Adopting such evaluations as strictly validleads to the conclusion that our best sample is a factor of two tofour incomplete

However the S N versus MV relation has a substantial scat-ter For example from the database by Harris et al (2013) itcan be seen that galaxies with MV = minus21 plusmn 02 mag have amedian population of sim 450 GCs with minimum at sim 40 anda maximum of sim 7000 It is worth emphasizing that based onprevious literature (Blecha 1986 Olsen et al 2004) Harris et al(2013) estimates the size of the GC system of NGC 253 to beNGC = 90 plusmn 40 If only galaxies with morphological classes andmagnitudes similar to NGC 253 are drawn from the Harris et al(2013) sample the median is NGC sim 80 The two galaxies withclosest morphological class and total magnitude to NGC 253(M 101 and NGC 6956) have a total population of detected GCswith NGC sim 90 plusmn 40 and 150 plusmn 40 which is consistent with thetotal (coverage corrected) population we estimated

Inspecting the radial profiles shown in Figure 13 we notea slight enhancement of GCs density at rgal sim 25 kpc Al-though the estimated errors are relatively high such enhance-ment roughly corresponds to the radial distance of the featurefirst found and discussed by Greggio et al (2014) identified asa possible stellar stream remnant However we must highlightthat our radial profile is derived from the azimuthal average ofGC counts while the RGB star counts excess found in Greggioet al (2014) is specifically located on the northwestern side ofthe galaxy

44 Color bimodality

A further typical element of discussion in extragalactic GC sys-tems is the color distribution In particular the presence of a

Article number page 13 of 24

AampA proofs manuscript no ms_printer_v11

Fig 14 Color-color diagrams for the bona fide and uncertain samples of GCs shown with blue filled dots and empty gray circlesrespectively The (arbitrarily scaled) histograms reported on the axes refer to the bona fide sample For optical colors the SPoT SSPmodels are also shown with lines as in Figure 4

nearly universal color bimodality in GC systems and the as-trophysical processes underlying such ubiquitous feature havegenerated a prolific and still open debate in the last decade(Spitler et al 2006 Yoon et al 2006 Cantiello amp Blakeslee2007 Chies-Santos et al 2012 Usher et al 2012 Brodie et al2014 Cantiello et al 2014) We adopted the bona fide sampleto verify the presence of color bimodality (ie to identify twowell-separated blue and red peaks) and to estimate the differ-ences between the two GC subpopulations in terms of the colordistributions To do so we used the Gaussian mixture model-ing code (GMM Muratov amp Gnedin 2010) The GMM codeuses the likelihood-ratio test to compare the goodness of fit fordouble-Gaussian versus a single-Gaussian For the best-fit dou-ble model it estimates the means and widths of the two com-ponents their separation DD in terms of combined widths andthe kurtosis of the overall distribution Values of DD larger thansim 2 and negative kurtosis are necessary but not sufficient condi-

tions for bimodality Also GMM provides uncertainties based onbootstrap resampling In addition the GMM analysis providesthe positions relative widths and fraction of objects associatedwith each peak

Inspecting the results reported in Table 4 (upper section ofthe table) GMM analysis shows that our bona fide GCs sampleis poorly fitted by two-Gaussian distributions in most of the in-spected colors This is testified by either the high p-values (Cols10-12 in the table) the changing fractions of red GCs ( f2) whendifferent colors are used the positive kurtosis or the low valuesfor the peak separation estimator (DD)

We also run GMM in three Gaussian peaks mode The re-sults reported in Table 5 are more satisfactory than the previ-ous as testified by the generally lower p-values The presence ofa third color peak is also visible as a red tail of GCs in the pan-els of Figure 14 The very red candidates are scattered aroundthe frame ie they are not sources close to the galaxy disk and

Article number page 14 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 4 Results of GMM runs

Color Peak1 Peak2 σ1 σ2 NGC f2 DD Kurtosis p(χ2) p(DD) p(kurt) bi(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)uminusi 184 plusmn 014 220 plusmn 029 008 plusmn 007 030 plusmn 010 81 088 162 -004 0525 073 0675 Ngminusi 079 plusmn 006 122 plusmn 019 013 plusmn 004 011 plusmn 005 81 005 344 093 0050 014 0974 Yuminusr 159 plusmn 009 197 plusmn 013 012 plusmn 004 023 plusmn 006 81 081 206 -009 0634 061 0630 Niminusk 003 plusmn 010 063 plusmn 021 023 plusmn 007 026 plusmn 010 82 035 249 -059 0063 042 0157 Yrminus j 065 plusmn 004 095 plusmn 012 008 plusmn 003 025 plusmn 006 81 064 162 077 0004 074 0961 Ngminusk 055 plusmn 014 119 plusmn 030 012 plusmn 009 049 plusmn 012 81 079 179 -035 0026 070 0378 Yrminusi 022 plusmn 002 029 plusmn 003 003 plusmn 001 006 plusmn 001 82 068 141 042 0075 083 0895 Njminusk -037 plusmn 006 -003 plusmn 008 018 plusmn 003 005 plusmn 004 82 010 253 -045 0226 042 0271 N

Without the red GCsgminusi 067 plusmn 005 087 plusmn 005 007 plusmn 002 009 plusmn 002 76 061 239 -070 0444 048 0086 Numinusi 194 plusmn 006 236 plusmn 004 018 plusmn 003 011 plusmn 003 78 043 277 -091 0024 031 0013 Yuminusr 171 plusmn 006 207 plusmn 003 017 plusmn 003 008 plusmn 003 77 041 267 -097 0005 034 0006 Yiminusk 004 plusmn 009 056 plusmn 013 023 plusmn 006 013 plusmn 006 74 023 280 -070 0208 032 0081 Yrminus j 070 plusmn 004 107 plusmn 008 013 plusmn 003 007 plusmn 004 74 025 347 -095 0004 014 0012 Ygminusk 082 plusmn 012 151 plusmn 017 032 plusmn 010 014 plusmn 009 73 019 283 -085 0136 029 0032 Yrminusi 023 plusmn 001 032 plusmn 001 004 plusmn 001 001 plusmn 001 74 025 310 -097 0004 022 0011 Yjminusk -044 plusmn 010 -022 plusmn 006 015 plusmn 004 009 plusmn 003 72 026 174 -035 0705 071 0395 N

Notes Columns list (1) color (2-3) mean and uncertainty of the first and second peaks in the double-Gaussian model (4-5) width and uncertaintyof the first and second peaks (6) number of GC candidates selected (7) fraction of GC candidates associated with the second red peak (8)separation of the peaks in units of the two Gaussian widths (9) kurtosis of the distribution (DDge2 and negative kurtosis are required for significativesplit between the two Gaussian distributions) (10-12) GMM p-values based on the likelihood-ratio test p(χ2) peak separation p(DD) and kurtosisp(kurt) indicating the significance of the preference for a double-Gaussian over a single-Gaussian model (lower p-values are more significant)(13) assessment of the evidence for bimodality

Table 5 Results of GMM runs for the three Gaussian model

Color Peak1 (NGC σ) Peak2 (NGC σ) Peak3 (NGC σ) DD Kurtosis p(χ2) p(DD) p(kurt)uminusi 194 ( 4370 019 ) 236 ( 3330 012 ) 292 ( 400 006 ) 273 -004 0024 0351 0675gminusi 069 ( 3910 008 ) 088 ( 3020 006 ) 107 ( 1160 017 ) 254 093 0111 0511 0974uminusr 171 ( 4540 017 ) 207 ( 3160 008 ) 253 ( 400 005 ) 267 -009 0002 0459 0630iminusk 004 ( 5680 023 ) 056 ( 1660 012 ) 096 ( 860 008 ) 280 -059 0071 0345 0157rminus j 067 ( 4460 011 ) 104 ( 3540 017 ) 177 ( 100 004 ) 261 077 0002 0470 0961gminusk 069 ( 4300 025 ) 133 ( 3040 026 ) 209 ( 760 016 ) 249 -035 0122 0581 0597rminusi 023 ( 5340 004 ) 032 ( 1610 001 ) 036 ( 1250 006 ) 315 042 0047 0221 0895jminusk 044 ( 5320 015 ) -024 ( 1420 004 ) -003 ( 1450 007 ) 187 -045 0474 0618 0271

Notes Columns list (1) color (2-4) first second and third peaks in the three Gaussian model numbers within parentheses are the number of GCsassociated with each peak and the width of the distribution (5) separation of the peaks in units of the three Gaussian widths (6) kurtosis of thedistribution (7-9) GMM p-values as in Table 4

reddened by the dust In the Figure we report the color-color dia-grams together with color histograms for various colors and forthe bona fide GCs sample Taking advantage of the results on thepresence of such third peak we rerun GMM in double Gaussianmode after rejecting the candidate GCs in the third reddest peakGMM also provides as output a table with the probability mem-bership of each GCs to one of the fitted Gaussian The GMMresults of such a culled best sample again with a two Gaussianmodel are presented in the lower section of Table 4

Although the new GMM results for the selected GCs sampleappear with respect to the full bona fide sample more consistentwith a bimodal-color scenario there is no homogeneity of thevarious inspected colors as color bimodality is not coherentlyobserved in all colors In this respect then NGC 253 should cer-tainly not be considered a galaxy with a bimodal GC populationshowing coherent and consistent color bimodality

5 Conclusions

We summarize the conclusion of the present work dedicatedto the definition of an updated catalog of GC candidates inNGC 253 as follows

ndash The adoption of an even richer collection of color photomet-ric and morphologic parameters make the selection of GCcandidates more robust but does not guarantee the completeremoval of all contaminants

ndash Depending on the spatial resolution of the imaging data usedfor sources close enough such as the galaxy studied herethe foreground MW stars can be separated from GCs as thelatter appear extended with FWHM definitely larger thana point source In cases such as that presented here back-ground galaxies are the primary source of contamination

ndash About 10 of our candidates were already photometrically se-lected as GC candidates by other authors Conversely thelargest portion of GC candidates with photometric selectionin the literature are mostly identified as stars in our sample

Article number page 15 of 24

AampA proofs manuscript no ms_printer_v11

ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

Article number page 16 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig 12 Left Optical LFs of the bona fide sample GCs (gray shaded histogram) and of the bona fide+uncertain samples (dottedline) The adopted TOM in each band is shown with a vertical dashed line Right LFs of bona fide GCs shown in logarithmic scaleThe long-dashed line shows the power-law fit to the data The exponent of the fit is reported each panel (see text)

Fig 13 Radial density profile of the best GCs sample Left andright panels show the linear and r14-law profile respectivelyLinear fits to data are shown with blue dotted line The verticaldashed line indicates the semimajor axis where the dusty diskbegins

GC specific frequency S N6 versus magnitude relation (eg from

Peng et al 2008) it is possible to invert the relation and obtainan estimate of the total expected GC population for a galaxy likeNGC 253 Adopting S N sim 18 from the dotted curve in Figure 2of Peng et al (2008 derived from the analysis of Virgo cluster

6 A parameter relating the galaxy and the GC system properties quan-tified as the number of GCs per unit galaxy luminosity S N equiv NGC times

1004(MV +15) where NGC is the total number of clusters and MV is thetotal absolute visual magnitude of the galaxy (Harris amp van den Bergh1981 Harris 1991)

galaxies covering a wide range of luminosities) and MV sim minus21mag (Table 1) we get NTotal

GC sim 450 Assuming ∆S N sim 04 and∆MB sim 05 mag we also calculate an uncertainty ∆NTotal

GC sim 260This number decreases to NTotal

GC = 250 plusmn 200 if S N sim 1 is used(Harris et al 2013) Adopting such evaluations as strictly validleads to the conclusion that our best sample is a factor of two tofour incomplete

However the S N versus MV relation has a substantial scat-ter For example from the database by Harris et al (2013) itcan be seen that galaxies with MV = minus21 plusmn 02 mag have amedian population of sim 450 GCs with minimum at sim 40 anda maximum of sim 7000 It is worth emphasizing that based onprevious literature (Blecha 1986 Olsen et al 2004) Harris et al(2013) estimates the size of the GC system of NGC 253 to beNGC = 90 plusmn 40 If only galaxies with morphological classes andmagnitudes similar to NGC 253 are drawn from the Harris et al(2013) sample the median is NGC sim 80 The two galaxies withclosest morphological class and total magnitude to NGC 253(M 101 and NGC 6956) have a total population of detected GCswith NGC sim 90 plusmn 40 and 150 plusmn 40 which is consistent with thetotal (coverage corrected) population we estimated

Inspecting the radial profiles shown in Figure 13 we notea slight enhancement of GCs density at rgal sim 25 kpc Al-though the estimated errors are relatively high such enhance-ment roughly corresponds to the radial distance of the featurefirst found and discussed by Greggio et al (2014) identified asa possible stellar stream remnant However we must highlightthat our radial profile is derived from the azimuthal average ofGC counts while the RGB star counts excess found in Greggioet al (2014) is specifically located on the northwestern side ofthe galaxy

44 Color bimodality

A further typical element of discussion in extragalactic GC sys-tems is the color distribution In particular the presence of a

Article number page 13 of 24

AampA proofs manuscript no ms_printer_v11

Fig 14 Color-color diagrams for the bona fide and uncertain samples of GCs shown with blue filled dots and empty gray circlesrespectively The (arbitrarily scaled) histograms reported on the axes refer to the bona fide sample For optical colors the SPoT SSPmodels are also shown with lines as in Figure 4

nearly universal color bimodality in GC systems and the as-trophysical processes underlying such ubiquitous feature havegenerated a prolific and still open debate in the last decade(Spitler et al 2006 Yoon et al 2006 Cantiello amp Blakeslee2007 Chies-Santos et al 2012 Usher et al 2012 Brodie et al2014 Cantiello et al 2014) We adopted the bona fide sampleto verify the presence of color bimodality (ie to identify twowell-separated blue and red peaks) and to estimate the differ-ences between the two GC subpopulations in terms of the colordistributions To do so we used the Gaussian mixture model-ing code (GMM Muratov amp Gnedin 2010) The GMM codeuses the likelihood-ratio test to compare the goodness of fit fordouble-Gaussian versus a single-Gaussian For the best-fit dou-ble model it estimates the means and widths of the two com-ponents their separation DD in terms of combined widths andthe kurtosis of the overall distribution Values of DD larger thansim 2 and negative kurtosis are necessary but not sufficient condi-

tions for bimodality Also GMM provides uncertainties based onbootstrap resampling In addition the GMM analysis providesthe positions relative widths and fraction of objects associatedwith each peak

Inspecting the results reported in Table 4 (upper section ofthe table) GMM analysis shows that our bona fide GCs sampleis poorly fitted by two-Gaussian distributions in most of the in-spected colors This is testified by either the high p-values (Cols10-12 in the table) the changing fractions of red GCs ( f2) whendifferent colors are used the positive kurtosis or the low valuesfor the peak separation estimator (DD)

We also run GMM in three Gaussian peaks mode The re-sults reported in Table 5 are more satisfactory than the previ-ous as testified by the generally lower p-values The presence ofa third color peak is also visible as a red tail of GCs in the pan-els of Figure 14 The very red candidates are scattered aroundthe frame ie they are not sources close to the galaxy disk and

Article number page 14 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 4 Results of GMM runs

Color Peak1 Peak2 σ1 σ2 NGC f2 DD Kurtosis p(χ2) p(DD) p(kurt) bi(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)uminusi 184 plusmn 014 220 plusmn 029 008 plusmn 007 030 plusmn 010 81 088 162 -004 0525 073 0675 Ngminusi 079 plusmn 006 122 plusmn 019 013 plusmn 004 011 plusmn 005 81 005 344 093 0050 014 0974 Yuminusr 159 plusmn 009 197 plusmn 013 012 plusmn 004 023 plusmn 006 81 081 206 -009 0634 061 0630 Niminusk 003 plusmn 010 063 plusmn 021 023 plusmn 007 026 plusmn 010 82 035 249 -059 0063 042 0157 Yrminus j 065 plusmn 004 095 plusmn 012 008 plusmn 003 025 plusmn 006 81 064 162 077 0004 074 0961 Ngminusk 055 plusmn 014 119 plusmn 030 012 plusmn 009 049 plusmn 012 81 079 179 -035 0026 070 0378 Yrminusi 022 plusmn 002 029 plusmn 003 003 plusmn 001 006 plusmn 001 82 068 141 042 0075 083 0895 Njminusk -037 plusmn 006 -003 plusmn 008 018 plusmn 003 005 plusmn 004 82 010 253 -045 0226 042 0271 N

Without the red GCsgminusi 067 plusmn 005 087 plusmn 005 007 plusmn 002 009 plusmn 002 76 061 239 -070 0444 048 0086 Numinusi 194 plusmn 006 236 plusmn 004 018 plusmn 003 011 plusmn 003 78 043 277 -091 0024 031 0013 Yuminusr 171 plusmn 006 207 plusmn 003 017 plusmn 003 008 plusmn 003 77 041 267 -097 0005 034 0006 Yiminusk 004 plusmn 009 056 plusmn 013 023 plusmn 006 013 plusmn 006 74 023 280 -070 0208 032 0081 Yrminus j 070 plusmn 004 107 plusmn 008 013 plusmn 003 007 plusmn 004 74 025 347 -095 0004 014 0012 Ygminusk 082 plusmn 012 151 plusmn 017 032 plusmn 010 014 plusmn 009 73 019 283 -085 0136 029 0032 Yrminusi 023 plusmn 001 032 plusmn 001 004 plusmn 001 001 plusmn 001 74 025 310 -097 0004 022 0011 Yjminusk -044 plusmn 010 -022 plusmn 006 015 plusmn 004 009 plusmn 003 72 026 174 -035 0705 071 0395 N

Notes Columns list (1) color (2-3) mean and uncertainty of the first and second peaks in the double-Gaussian model (4-5) width and uncertaintyof the first and second peaks (6) number of GC candidates selected (7) fraction of GC candidates associated with the second red peak (8)separation of the peaks in units of the two Gaussian widths (9) kurtosis of the distribution (DDge2 and negative kurtosis are required for significativesplit between the two Gaussian distributions) (10-12) GMM p-values based on the likelihood-ratio test p(χ2) peak separation p(DD) and kurtosisp(kurt) indicating the significance of the preference for a double-Gaussian over a single-Gaussian model (lower p-values are more significant)(13) assessment of the evidence for bimodality

Table 5 Results of GMM runs for the three Gaussian model

Color Peak1 (NGC σ) Peak2 (NGC σ) Peak3 (NGC σ) DD Kurtosis p(χ2) p(DD) p(kurt)uminusi 194 ( 4370 019 ) 236 ( 3330 012 ) 292 ( 400 006 ) 273 -004 0024 0351 0675gminusi 069 ( 3910 008 ) 088 ( 3020 006 ) 107 ( 1160 017 ) 254 093 0111 0511 0974uminusr 171 ( 4540 017 ) 207 ( 3160 008 ) 253 ( 400 005 ) 267 -009 0002 0459 0630iminusk 004 ( 5680 023 ) 056 ( 1660 012 ) 096 ( 860 008 ) 280 -059 0071 0345 0157rminus j 067 ( 4460 011 ) 104 ( 3540 017 ) 177 ( 100 004 ) 261 077 0002 0470 0961gminusk 069 ( 4300 025 ) 133 ( 3040 026 ) 209 ( 760 016 ) 249 -035 0122 0581 0597rminusi 023 ( 5340 004 ) 032 ( 1610 001 ) 036 ( 1250 006 ) 315 042 0047 0221 0895jminusk 044 ( 5320 015 ) -024 ( 1420 004 ) -003 ( 1450 007 ) 187 -045 0474 0618 0271

Notes Columns list (1) color (2-4) first second and third peaks in the three Gaussian model numbers within parentheses are the number of GCsassociated with each peak and the width of the distribution (5) separation of the peaks in units of the three Gaussian widths (6) kurtosis of thedistribution (7-9) GMM p-values as in Table 4

reddened by the dust In the Figure we report the color-color dia-grams together with color histograms for various colors and forthe bona fide GCs sample Taking advantage of the results on thepresence of such third peak we rerun GMM in double Gaussianmode after rejecting the candidate GCs in the third reddest peakGMM also provides as output a table with the probability mem-bership of each GCs to one of the fitted Gaussian The GMMresults of such a culled best sample again with a two Gaussianmodel are presented in the lower section of Table 4

Although the new GMM results for the selected GCs sampleappear with respect to the full bona fide sample more consistentwith a bimodal-color scenario there is no homogeneity of thevarious inspected colors as color bimodality is not coherentlyobserved in all colors In this respect then NGC 253 should cer-tainly not be considered a galaxy with a bimodal GC populationshowing coherent and consistent color bimodality

5 Conclusions

We summarize the conclusion of the present work dedicatedto the definition of an updated catalog of GC candidates inNGC 253 as follows

ndash The adoption of an even richer collection of color photomet-ric and morphologic parameters make the selection of GCcandidates more robust but does not guarantee the completeremoval of all contaminants

ndash Depending on the spatial resolution of the imaging data usedfor sources close enough such as the galaxy studied herethe foreground MW stars can be separated from GCs as thelatter appear extended with FWHM definitely larger thana point source In cases such as that presented here back-ground galaxies are the primary source of contamination

ndash About 10 of our candidates were already photometrically se-lected as GC candidates by other authors Conversely thelargest portion of GC candidates with photometric selectionin the literature are mostly identified as stars in our sample

Article number page 15 of 24

AampA proofs manuscript no ms_printer_v11

ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

Article number page 16 of 24

AampA proofs manuscript no ms_printer_v11

Fig 14 Color-color diagrams for the bona fide and uncertain samples of GCs shown with blue filled dots and empty gray circlesrespectively The (arbitrarily scaled) histograms reported on the axes refer to the bona fide sample For optical colors the SPoT SSPmodels are also shown with lines as in Figure 4

nearly universal color bimodality in GC systems and the as-trophysical processes underlying such ubiquitous feature havegenerated a prolific and still open debate in the last decade(Spitler et al 2006 Yoon et al 2006 Cantiello amp Blakeslee2007 Chies-Santos et al 2012 Usher et al 2012 Brodie et al2014 Cantiello et al 2014) We adopted the bona fide sampleto verify the presence of color bimodality (ie to identify twowell-separated blue and red peaks) and to estimate the differ-ences between the two GC subpopulations in terms of the colordistributions To do so we used the Gaussian mixture model-ing code (GMM Muratov amp Gnedin 2010) The GMM codeuses the likelihood-ratio test to compare the goodness of fit fordouble-Gaussian versus a single-Gaussian For the best-fit dou-ble model it estimates the means and widths of the two com-ponents their separation DD in terms of combined widths andthe kurtosis of the overall distribution Values of DD larger thansim 2 and negative kurtosis are necessary but not sufficient condi-

tions for bimodality Also GMM provides uncertainties based onbootstrap resampling In addition the GMM analysis providesthe positions relative widths and fraction of objects associatedwith each peak

Inspecting the results reported in Table 4 (upper section ofthe table) GMM analysis shows that our bona fide GCs sampleis poorly fitted by two-Gaussian distributions in most of the in-spected colors This is testified by either the high p-values (Cols10-12 in the table) the changing fractions of red GCs ( f2) whendifferent colors are used the positive kurtosis or the low valuesfor the peak separation estimator (DD)

We also run GMM in three Gaussian peaks mode The re-sults reported in Table 5 are more satisfactory than the previ-ous as testified by the generally lower p-values The presence ofa third color peak is also visible as a red tail of GCs in the pan-els of Figure 14 The very red candidates are scattered aroundthe frame ie they are not sources close to the galaxy disk and

Article number page 14 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 4 Results of GMM runs

Color Peak1 Peak2 σ1 σ2 NGC f2 DD Kurtosis p(χ2) p(DD) p(kurt) bi(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)uminusi 184 plusmn 014 220 plusmn 029 008 plusmn 007 030 plusmn 010 81 088 162 -004 0525 073 0675 Ngminusi 079 plusmn 006 122 plusmn 019 013 plusmn 004 011 plusmn 005 81 005 344 093 0050 014 0974 Yuminusr 159 plusmn 009 197 plusmn 013 012 plusmn 004 023 plusmn 006 81 081 206 -009 0634 061 0630 Niminusk 003 plusmn 010 063 plusmn 021 023 plusmn 007 026 plusmn 010 82 035 249 -059 0063 042 0157 Yrminus j 065 plusmn 004 095 plusmn 012 008 plusmn 003 025 plusmn 006 81 064 162 077 0004 074 0961 Ngminusk 055 plusmn 014 119 plusmn 030 012 plusmn 009 049 plusmn 012 81 079 179 -035 0026 070 0378 Yrminusi 022 plusmn 002 029 plusmn 003 003 plusmn 001 006 plusmn 001 82 068 141 042 0075 083 0895 Njminusk -037 plusmn 006 -003 plusmn 008 018 plusmn 003 005 plusmn 004 82 010 253 -045 0226 042 0271 N

Without the red GCsgminusi 067 plusmn 005 087 plusmn 005 007 plusmn 002 009 plusmn 002 76 061 239 -070 0444 048 0086 Numinusi 194 plusmn 006 236 plusmn 004 018 plusmn 003 011 plusmn 003 78 043 277 -091 0024 031 0013 Yuminusr 171 plusmn 006 207 plusmn 003 017 plusmn 003 008 plusmn 003 77 041 267 -097 0005 034 0006 Yiminusk 004 plusmn 009 056 plusmn 013 023 plusmn 006 013 plusmn 006 74 023 280 -070 0208 032 0081 Yrminus j 070 plusmn 004 107 plusmn 008 013 plusmn 003 007 plusmn 004 74 025 347 -095 0004 014 0012 Ygminusk 082 plusmn 012 151 plusmn 017 032 plusmn 010 014 plusmn 009 73 019 283 -085 0136 029 0032 Yrminusi 023 plusmn 001 032 plusmn 001 004 plusmn 001 001 plusmn 001 74 025 310 -097 0004 022 0011 Yjminusk -044 plusmn 010 -022 plusmn 006 015 plusmn 004 009 plusmn 003 72 026 174 -035 0705 071 0395 N

Notes Columns list (1) color (2-3) mean and uncertainty of the first and second peaks in the double-Gaussian model (4-5) width and uncertaintyof the first and second peaks (6) number of GC candidates selected (7) fraction of GC candidates associated with the second red peak (8)separation of the peaks in units of the two Gaussian widths (9) kurtosis of the distribution (DDge2 and negative kurtosis are required for significativesplit between the two Gaussian distributions) (10-12) GMM p-values based on the likelihood-ratio test p(χ2) peak separation p(DD) and kurtosisp(kurt) indicating the significance of the preference for a double-Gaussian over a single-Gaussian model (lower p-values are more significant)(13) assessment of the evidence for bimodality

Table 5 Results of GMM runs for the three Gaussian model

Color Peak1 (NGC σ) Peak2 (NGC σ) Peak3 (NGC σ) DD Kurtosis p(χ2) p(DD) p(kurt)uminusi 194 ( 4370 019 ) 236 ( 3330 012 ) 292 ( 400 006 ) 273 -004 0024 0351 0675gminusi 069 ( 3910 008 ) 088 ( 3020 006 ) 107 ( 1160 017 ) 254 093 0111 0511 0974uminusr 171 ( 4540 017 ) 207 ( 3160 008 ) 253 ( 400 005 ) 267 -009 0002 0459 0630iminusk 004 ( 5680 023 ) 056 ( 1660 012 ) 096 ( 860 008 ) 280 -059 0071 0345 0157rminus j 067 ( 4460 011 ) 104 ( 3540 017 ) 177 ( 100 004 ) 261 077 0002 0470 0961gminusk 069 ( 4300 025 ) 133 ( 3040 026 ) 209 ( 760 016 ) 249 -035 0122 0581 0597rminusi 023 ( 5340 004 ) 032 ( 1610 001 ) 036 ( 1250 006 ) 315 042 0047 0221 0895jminusk 044 ( 5320 015 ) -024 ( 1420 004 ) -003 ( 1450 007 ) 187 -045 0474 0618 0271

Notes Columns list (1) color (2-4) first second and third peaks in the three Gaussian model numbers within parentheses are the number of GCsassociated with each peak and the width of the distribution (5) separation of the peaks in units of the three Gaussian widths (6) kurtosis of thedistribution (7-9) GMM p-values as in Table 4

reddened by the dust In the Figure we report the color-color dia-grams together with color histograms for various colors and forthe bona fide GCs sample Taking advantage of the results on thepresence of such third peak we rerun GMM in double Gaussianmode after rejecting the candidate GCs in the third reddest peakGMM also provides as output a table with the probability mem-bership of each GCs to one of the fitted Gaussian The GMMresults of such a culled best sample again with a two Gaussianmodel are presented in the lower section of Table 4

Although the new GMM results for the selected GCs sampleappear with respect to the full bona fide sample more consistentwith a bimodal-color scenario there is no homogeneity of thevarious inspected colors as color bimodality is not coherentlyobserved in all colors In this respect then NGC 253 should cer-tainly not be considered a galaxy with a bimodal GC populationshowing coherent and consistent color bimodality

5 Conclusions

We summarize the conclusion of the present work dedicatedto the definition of an updated catalog of GC candidates inNGC 253 as follows

ndash The adoption of an even richer collection of color photomet-ric and morphologic parameters make the selection of GCcandidates more robust but does not guarantee the completeremoval of all contaminants

ndash Depending on the spatial resolution of the imaging data usedfor sources close enough such as the galaxy studied herethe foreground MW stars can be separated from GCs as thelatter appear extended with FWHM definitely larger thana point source In cases such as that presented here back-ground galaxies are the primary source of contamination

ndash About 10 of our candidates were already photometrically se-lected as GC candidates by other authors Conversely thelargest portion of GC candidates with photometric selectionin the literature are mostly identified as stars in our sample

Article number page 15 of 24

AampA proofs manuscript no ms_printer_v11

ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

Article number page 16 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Table 4 Results of GMM runs

Color Peak1 Peak2 σ1 σ2 NGC f2 DD Kurtosis p(χ2) p(DD) p(kurt) bi(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)uminusi 184 plusmn 014 220 plusmn 029 008 plusmn 007 030 plusmn 010 81 088 162 -004 0525 073 0675 Ngminusi 079 plusmn 006 122 plusmn 019 013 plusmn 004 011 plusmn 005 81 005 344 093 0050 014 0974 Yuminusr 159 plusmn 009 197 plusmn 013 012 plusmn 004 023 plusmn 006 81 081 206 -009 0634 061 0630 Niminusk 003 plusmn 010 063 plusmn 021 023 plusmn 007 026 plusmn 010 82 035 249 -059 0063 042 0157 Yrminus j 065 plusmn 004 095 plusmn 012 008 plusmn 003 025 plusmn 006 81 064 162 077 0004 074 0961 Ngminusk 055 plusmn 014 119 plusmn 030 012 plusmn 009 049 plusmn 012 81 079 179 -035 0026 070 0378 Yrminusi 022 plusmn 002 029 plusmn 003 003 plusmn 001 006 plusmn 001 82 068 141 042 0075 083 0895 Njminusk -037 plusmn 006 -003 plusmn 008 018 plusmn 003 005 plusmn 004 82 010 253 -045 0226 042 0271 N

Without the red GCsgminusi 067 plusmn 005 087 plusmn 005 007 plusmn 002 009 plusmn 002 76 061 239 -070 0444 048 0086 Numinusi 194 plusmn 006 236 plusmn 004 018 plusmn 003 011 plusmn 003 78 043 277 -091 0024 031 0013 Yuminusr 171 plusmn 006 207 plusmn 003 017 plusmn 003 008 plusmn 003 77 041 267 -097 0005 034 0006 Yiminusk 004 plusmn 009 056 plusmn 013 023 plusmn 006 013 plusmn 006 74 023 280 -070 0208 032 0081 Yrminus j 070 plusmn 004 107 plusmn 008 013 plusmn 003 007 plusmn 004 74 025 347 -095 0004 014 0012 Ygminusk 082 plusmn 012 151 plusmn 017 032 plusmn 010 014 plusmn 009 73 019 283 -085 0136 029 0032 Yrminusi 023 plusmn 001 032 plusmn 001 004 plusmn 001 001 plusmn 001 74 025 310 -097 0004 022 0011 Yjminusk -044 plusmn 010 -022 plusmn 006 015 plusmn 004 009 plusmn 003 72 026 174 -035 0705 071 0395 N

Notes Columns list (1) color (2-3) mean and uncertainty of the first and second peaks in the double-Gaussian model (4-5) width and uncertaintyof the first and second peaks (6) number of GC candidates selected (7) fraction of GC candidates associated with the second red peak (8)separation of the peaks in units of the two Gaussian widths (9) kurtosis of the distribution (DDge2 and negative kurtosis are required for significativesplit between the two Gaussian distributions) (10-12) GMM p-values based on the likelihood-ratio test p(χ2) peak separation p(DD) and kurtosisp(kurt) indicating the significance of the preference for a double-Gaussian over a single-Gaussian model (lower p-values are more significant)(13) assessment of the evidence for bimodality

Table 5 Results of GMM runs for the three Gaussian model

Color Peak1 (NGC σ) Peak2 (NGC σ) Peak3 (NGC σ) DD Kurtosis p(χ2) p(DD) p(kurt)uminusi 194 ( 4370 019 ) 236 ( 3330 012 ) 292 ( 400 006 ) 273 -004 0024 0351 0675gminusi 069 ( 3910 008 ) 088 ( 3020 006 ) 107 ( 1160 017 ) 254 093 0111 0511 0974uminusr 171 ( 4540 017 ) 207 ( 3160 008 ) 253 ( 400 005 ) 267 -009 0002 0459 0630iminusk 004 ( 5680 023 ) 056 ( 1660 012 ) 096 ( 860 008 ) 280 -059 0071 0345 0157rminus j 067 ( 4460 011 ) 104 ( 3540 017 ) 177 ( 100 004 ) 261 077 0002 0470 0961gminusk 069 ( 4300 025 ) 133 ( 3040 026 ) 209 ( 760 016 ) 249 -035 0122 0581 0597rminusi 023 ( 5340 004 ) 032 ( 1610 001 ) 036 ( 1250 006 ) 315 042 0047 0221 0895jminusk 044 ( 5320 015 ) -024 ( 1420 004 ) -003 ( 1450 007 ) 187 -045 0474 0618 0271

Notes Columns list (1) color (2-4) first second and third peaks in the three Gaussian model numbers within parentheses are the number of GCsassociated with each peak and the width of the distribution (5) separation of the peaks in units of the three Gaussian widths (6) kurtosis of thedistribution (7-9) GMM p-values as in Table 4

reddened by the dust In the Figure we report the color-color dia-grams together with color histograms for various colors and forthe bona fide GCs sample Taking advantage of the results on thepresence of such third peak we rerun GMM in double Gaussianmode after rejecting the candidate GCs in the third reddest peakGMM also provides as output a table with the probability mem-bership of each GCs to one of the fitted Gaussian The GMMresults of such a culled best sample again with a two Gaussianmodel are presented in the lower section of Table 4

Although the new GMM results for the selected GCs sampleappear with respect to the full bona fide sample more consistentwith a bimodal-color scenario there is no homogeneity of thevarious inspected colors as color bimodality is not coherentlyobserved in all colors In this respect then NGC 253 should cer-tainly not be considered a galaxy with a bimodal GC populationshowing coherent and consistent color bimodality

5 Conclusions

We summarize the conclusion of the present work dedicatedto the definition of an updated catalog of GC candidates inNGC 253 as follows

ndash The adoption of an even richer collection of color photomet-ric and morphologic parameters make the selection of GCcandidates more robust but does not guarantee the completeremoval of all contaminants

ndash Depending on the spatial resolution of the imaging data usedfor sources close enough such as the galaxy studied herethe foreground MW stars can be separated from GCs as thelatter appear extended with FWHM definitely larger thana point source In cases such as that presented here back-ground galaxies are the primary source of contamination

ndash About 10 of our candidates were already photometrically se-lected as GC candidates by other authors Conversely thelargest portion of GC candidates with photometric selectionin the literature are mostly identified as stars in our sample

Article number page 15 of 24

AampA proofs manuscript no ms_printer_v11

ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

Article number page 16 of 24

AampA proofs manuscript no ms_printer_v11

ndash Even the adoption of the uiKs diagram which proved to beextremely efficient in Muntildeoz et al (2014) to identify GCs inthe Virgo galaxy cluster does not ensure a clean sample ofGCs

ndash Spectroscopy by itself is not sufficient to define acontamination-free GC sample In both the spectroscopiccatalogs we adopted as reference we found GCs that inour analysis are rather classified as contaminants two back-ground galaxies for Beasley amp Sharples (2000) catalog andtwo foreground stars for Olsen et al (2004) catalog This isequivalent to a level of sim 20 contamination in the full sam-ple of spectroscopically confirmed GCs

ndash We estimate a total population of sim 100 GC such a valueshould be regarded as a lower limit The literature data for acouple of galaxies similar in morphology and luminosity toNGC 253 show that they have similar populations of detectedGCs

ndash The LF of bona fide sample does not show the typical sym-metry around the GCLF MTOM peak A fraction of brightGCs might be undetected because of large galactocentricradii or because these GCs are along the line of sight ofthe dusty disk We do not have a clear explanation for themissing bright candidates However our results support pre-vious studies that found evidence for recent interactions forNGC 253 Hence one possible explanation of the observedLF might be the presence of a fraction of intermediate aget sim 6 Gyr GCs contaminating the population of old GCs

ndash The radial profile and color distributions of our bona fide GCsample show properties similar to other well-studies galax-ies ie a radial profile fit by a r14 minus law

ndash As for color bimodality the statistical preference of bimodalover unimodal color distribution is not strong because thisbimodality is evident with some colors and not in others

ndash Finally we provide an updated list of candidate GCs

Moreover as a byproduct of our analysis thanks to the verywide wavelength interval of imaging data used in addition toGCs we have been able to identify and distinguish the sequencesof stars and the (various classes of) background galaxies (seeAppendix)

The GCs in NGC 253 will be an interesting target for nextgeneration large aperture ge30m-class telescopes supported byadaptive optics modules that will facilitate reaching the diffrac-tion limit

We take as an example the MICADOMAORY configurationat the E-ELT (Diolaiti et al 2016 Davies et al 2016) whichhas an expected optimal resolution limit of sim 10mas at near-IRwavelengths ie sim 5 minus 10 times better than ACS and WFC3on board HST and the forthcoming NIRCAM on JWST withvery high Strehl ratios on a field of view of sim 20primeprime in the case ofSCAO the instrument will allow for the first time the study ofthe resolved color-magnitude diagrams of stars in the GCs in theSculptor group Our work is an effort to provide a large censusof GCs in NGC 253 which is the brightest galaxy in the group

Acknowledgements We gratefully acknowledge INAF for financial support tothe VSTceN This research was made possible through the use of the AAVSOPhotometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sci-ences Fund We acknowledge the usage of the HyperLeda database (Makarovet al 2014) httpledauniv-lyon1fr This research has made use ofthe NASA Astrophysics Data System Bibliographic Services the NASA Extra-galactic Database and the SIMBAD database operated at CDS Strasbourg It isa pleasure to thank W Harris and M Hilker for enlightening discussions

ReferencesAlamo-Martiacutenez K A Blakeslee J P Jee M J et al 2013 ApJ 775 20Arnaboldi M Petr-Gotzens M Rejkuba M et al 2010 The Messenger 139

6Arnaboldi M Rejkuba M Retzlaff J et al 2012 The Messenger 149 7Bailin J Bell E F Chappell S N Radburn-Smith D J amp de Jong R S

2011 ApJ 736 24Beasley M A amp Sharples R M 2000 MNRAS 311 673Bertin E amp Arnouts S 1996 AampAS 117 393Blecha A 1986 AampA 154 321Brodie J P Romanowsky A J Strader J et al 2014 ArXiv e-prints

[arXiv14052079]Brodie J P amp Strader J 2006 ARAampA 44 193Cantiello M amp Blakeslee J P 2007 ApJ 669 982Cantiello M Blakeslee J P amp Raimondo G 2007 ApJ 668 209Cantiello M Blakeslee J P Raimondo G et al 2014 AampA 564 L3Cantiello M Brocato E amp Blakeslee J P 2009 AampA 503 87Cantiello M Capaccioli M Napolitano N et al 2015 AampA 576 A14Cantiello et al 2017 AampA submitted 820 42Carretta E Bragaglia A Gratton R G et al 2009 AampA 505 117Caso J P Bassino L P Richtler T Smith Castelli A V amp Faifer F R 2013

MNRAS 430 1088Chies-Santos A L Larsen S S Cantiello M et al 2012 AampA 539 A54Chies-Santos A L Larsen S S Kuntschner H et al 2011 AampA 525 A20Cohen J G Blakeslee J P amp Cocircteacute P 2003 ApJ 592 866Cohen J G Blakeslee J P amp Ryzhov A 1998 ApJ 496 808Colbert E J M Heckman T M Ptak A F Strickland D K amp Weaver

K A 2004 ApJ 602 231DrsquoAbrusco R Cantiello M Paolillo M et al 2016 ApJ 819 L31Davies R Schubert J Hartl M et al 2016 in Proc SPIE Vol 9908 Ground-

based and Airborne Instrumentation for Astronomy VI 99081ZDiolaiti E Ciliegi P Abicca R et al 2016 in Proc SPIE Vol 9909 Adaptive

Optics Systems V 99092DDirsch B Schuberth Y amp Richtler T 2005 AampA 433 43Durrell P R Cocircteacute P Peng E W et al 2014 ApJ 794 103Galleti S Federici L Bellazzini M Fusi Pecci F amp Macrina S 2004 AampA

416 917Georgiev I Y Puzia T H Goudfrooij P amp Hilker M 2010 MNRAS 406

1967Goudfrooij P Schweizer F Gilmore D amp Whitmore B C 2007 AJ 133

2737Grado A Capaccioli M Limatola L amp Getman F 2012 Memorie della

Societa Astronomica Italiana Supplementi 19 362Gratton R Sneden C amp Carretta E 2004 ARAampA 42 385Greggio L Rejkuba M Gonzalez O A et al 2014 AampA 562 A73Harris W E 1991 ARAampA 29 543Harris W E 1996 AJ 112 1487 (2010 edition)Harris W E 2001 in Saas-Fee Advanced Course 28 Star ClustersHarris W E Harris G L H amp Alessi M 2013 ApJ 772 82Harris W E amp van den Bergh S 1981 AJ 86 1627Holwerda B W Keel W C Williams B Dalcanton J J amp de Jong R S

2009 AJ 137 3000Iodice E Arnaboldi M Rejkuba M et al 2014 AampA 567 A86Iodice E Capaccioli M Grado A et al 2016 ApJ 820 42Iodice E VISTA Team VST SV Team et al 2012 Mem Soc Astron Italiana

83 1174Irwin M J Lewis J Hodgkin S et al 2004 in Proc SPIE Vol 5493 Op-

timizing Scientific Return for Astronomy through Information Technologiesed P J Quinn amp A Bridger 411ndash422

Janssens S Abraham R Brodie J et al 2017 ArXiv e-prints[arXiv170100011]

Jedrzejewski R I 1987 MNRAS 226 747Jordaacuten A 2004 ApJ 613 L117Karachentsev I D Grebel E K Sharina M E et al 2003 AampA 404 93Landolt A U 1992 AJ 104 340Larsen S S 1999 AampAS 139 393Larsen S S 2002 AJ 124 1393Larsen S S amp Brodie J P 2003 ApJ 593 340Larsen S S amp Richtler T 2000 AampA 354 836Liller W amp Alcaino G 1983 ApJ 265 166Makarov D Prugniel P Terekhova N Courtois H amp Vauglin I 2014 AampA

570 A13McCarthy P J van Breugel W amp Heckman T 1987 AJ 93 264Miller B W Whitmore B C Schweizer F amp Fall S M 1997 AJ 114 2381Muntildeoz R P Puzia T H Lanccedilon A et al 2014 ApJS 210 4Muratov A L amp Gnedin O Y 2010 ApJ 718 1266Olsen K A G Miller B W Suntzeff N B Schommer R A amp Bright J

2004 AJ 127 2674Peng E W Ferguson H C Goudfrooij P et al 2011 ApJ 730 23

Article number page 16 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Peng E W Jordaacuten A Cocircteacute P et al 2006 ApJ 639 95Peng E W Jordaacuten A Cocircteacute P et al 2008 ApJ 681 197Piotto G Bedin L R Anderson J et al 2007 ApJ 661 L53Puzia T H Kissler-Patig M Thomas D et al 2005 AampA 439 997Puzia T H Paolillo M Goudfrooij P et al 2014 ApJ 786 78Radburn-Smith D J de Jong R S Seth A C et al 2011 ApJS 195 18Raimondo G 2009 ApJ 700 1247Raimondo G Brocato E Cantiello M amp Capaccioli M 2005 AJ 130 2625Salaris M amp Cassisi S 2005 Evolution of Stars and Stellar Populations (Evo-

lution of Stars and Stellar Populations by Maurizio Salaris Santi Cassisipp 400 ISBN 0-470-09220-3 Wiley-VCH December 2005)

Schlafly E F amp Finkbeiner D P 2011 ApJ 737 103Schlegel D J Finkbeiner D P amp Davis M 1998 ApJ 500 525Spitler L R Larsen S S Strader J et al 2006 AJ 132 1593Strader J Brodie J P Cenarro A J Beasley M A amp Forbes D A 2005

AJ 130 1315Usher C Forbes D A Brodie J P et al 2012 MNRAS 426 1475van den Bergh S amp Morbey C L 1984 ApJ 283 598Vanzella E Calura F Meneghetti M et al 2017 MNRAS 467 4304Villegas D Jordaacuten A Peng E W et al 2010 ApJ 717 603Whitmore B C Zhang Q Leitherer C et al 1999 AJ 118 1551Worthey G 1994 ApJS 95 107Xue X X Rix H W Zhao G et al 2008 ApJ 684 1143Yoon S-J Yi S K amp Lee Y-W 2006 Science 311 1129

Article number page 17 of 24

AampA proofs manuscript no ms_printer_v11

Appendix A Color-color diagrams

The large wavelength coverage of our dataset provides enoughleverage for evidencing the presence of several sequences in thecolor-color diagrams inspected Because of the different proper-ties of the observed targets some sequences merge or are rel-atively well separated with respect to others depending on thecolor-color plane inspected Using the same color-color selec-tion procedure described in Section 3 for selecting GC candi-dates we derived the approximate loci of the various sequencesobserved in the color-color diagrams As an example candidatestars were identified from the uiKs diagram Then the identifiedstars were analyzed in other color-color panels and all sourcesscattered around the sequence were removed from the list In asimilar way we identified the loci for passive galaxies (red early-type candidates) blue galaxies (eg spirals) star-forming (egirregular galaxies) beyond the stellar and GCs loci A selectionof the color-color diagrams used is reported in Figure A1 Inthe figure we plot full sample of matched sources (black dots)and highlight with different colors five different sequences or-ange gray red light blue blue filled circles indicate respec-tively the approximate loci of GCs MW stars passive galaxiesblue galaxies and star-forming galaxies To show how sequencesappear before separating these sequences we also plotted oneof the color-color panels (gminusKS ) versus (uminusi) with and with-out the sequences defined Also to highlight the limits of colorselection when a narrow range of wavelengths is available thethird panel in the lower row shows the sequences for the gminusiversus gminusr diagram

Article number page 18 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig A1 Color-color diagrams with the various sequences highlighted in different colors The full sample of matched sources isindicated with black dots Orange gray red light blue and blue dots indicate the approximate loci of GCs MW stars passivegalaxies blue galaxies and star-forming galaxies The left and middle panels in the lowermost row show the same color-colordiagram although in the second row we do not use colors for the sequences identified The total overlap of the identified sequencesin the lower right panel is notable

Article number page 19 of 24

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Article number page 20 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25381

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Article number page 22 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25325

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Article number page 23 of 24

AampA proofs manuscript no ms_printer_v1133

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Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams

AampA proofs manuscript no ms_printer_v11

Appendix A Color-color diagrams

The large wavelength coverage of our dataset provides enoughleverage for evidencing the presence of several sequences in thecolor-color diagrams inspected Because of the different proper-ties of the observed targets some sequences merge or are rel-atively well separated with respect to others depending on thecolor-color plane inspected Using the same color-color selec-tion procedure described in Section 3 for selecting GC candi-dates we derived the approximate loci of the various sequencesobserved in the color-color diagrams As an example candidatestars were identified from the uiKs diagram Then the identifiedstars were analyzed in other color-color panels and all sourcesscattered around the sequence were removed from the list In asimilar way we identified the loci for passive galaxies (red early-type candidates) blue galaxies (eg spirals) star-forming (egirregular galaxies) beyond the stellar and GCs loci A selectionof the color-color diagrams used is reported in Figure A1 Inthe figure we plot full sample of matched sources (black dots)and highlight with different colors five different sequences or-ange gray red light blue blue filled circles indicate respec-tively the approximate loci of GCs MW stars passive galaxiesblue galaxies and star-forming galaxies To show how sequencesappear before separating these sequences we also plotted oneof the color-color panels (gminusKS ) versus (uminusi) with and with-out the sequences defined Also to highlight the limits of colorselection when a narrow range of wavelengths is available thethird panel in the lower row shows the sequences for the gminusiversus gminusr diagram

Article number page 18 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig A1 Color-color diagrams with the various sequences highlighted in different colors The full sample of matched sources isindicated with black dots Orange gray red light blue and blue dots indicate the approximate loci of GCs MW stars passivegalaxies blue galaxies and star-forming galaxies The left and middle panels in the lowermost row show the same color-colordiagram although in the second row we do not use colors for the sequences identified The total overlap of the identified sequencesin the lower right panel is notable

Article number page 19 of 24

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Article number page 20 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25381

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Article number page 22 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25325

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Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 253

Fig A1 Color-color diagrams with the various sequences highlighted in different colors The full sample of matched sources isindicated with black dots Orange gray red light blue and blue dots indicate the approximate loci of GCs MW stars passivegalaxies blue galaxies and star-forming galaxies The left and middle panels in the lowermost row show the same color-colordiagram although in the second row we do not use colors for the sequences identified The total overlap of the identified sequencesin the lower right panel is notable

Article number page 19 of 24

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Article number page 20 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25381

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Article number page 22 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25325

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Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams

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Article number page 20 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25381

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Article number page 22 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25325

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Article number page 23 of 24

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Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25381

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Article number page 22 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25325

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Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams

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Article number page 22 of 24

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25325

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Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams

Michele CantielloAniello Grado et al A VST and VISTA study of globular clusters in NGC 25325

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Article number page 23 of 24

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Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams

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serv

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olw

erda

etal

200

9)V

isua

lIns

pect

ion

(Col

14)

box

10a

tlea

stsim

10so

urce

seq

ually

brig

htor

brig

hter

obse

rved

inan

area

of2primetimes

2primef

eatu

res

fain

text

ende

dst

ruct

ures

clos

eto

orar

ound

the

sour

ceN

briM

Nsi

mila

rorb

righ

ters

ourc

esw

ithin

Mar

csec

onds

gxy

-gro

up

the

sour

ceis

angu

larl

ycl

ose

tose

vera

lcle

arly

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nded

ordi

sk-s

hape

dso

urce

sbl

end

clos

e( simlt

5primeprime)o

bjec

tbl

ende

dw

ithth

eca

ndid

ate

the

labe

lldquoJrdquo

indi

cate

san

yof

the

prev

ious

flags

onl

yob

serv

edin

the

J-ba

ndfr

ame

the

deep

esti

nou

rda

tase

tO

ther

term

sus

edin

the

colu

mn

(elo

ngat

ede

xten

ded

fain

t)ar

ese

lfex

plan

ator

yN

ote

that

Rh

ism

eani

ngle

ssfo

rsou

rces

clas

sifie

das

No

(ie

unl

ikel

yG

Cca

ndid

ate)

Article number page 24 of 24

• 1 Introduction
• 2 Observations data reduction and analysis
• 3 Selection of GC candidates
• • 31 Comparison with spectroscopic and photometric GC samples
  • 32 Globular cluster sizes
  • • 4 Final catalog and discussion
    • • 41 The catalog
      • 42 Spatial distribution and luminosity function
      • 43 Total GC population
      • 44 Color bimodality
      • • 5 Conclusions
        • A Color-color diagrams