the nainital-cape survey
TRANSCRIPT
A&A 590, A116 (2016)DOI: 10.1051/0004-6361/201527242c© ESO 2016
Astronomy&Astrophysics
The Nainital-Cape Survey
IV. A search for pulsational variability in 108 chemically peculiar stars?
S. Joshi1, P. Martinez2, 3, S. Chowdhury4, N. K. Chakradhari5, Y. C. Joshi1, P. van Heerden3,T. Medupe6, Y. B. Kumar7, and R. B. Kuhn3
1 Aryabhatta Research Institute of Observational Sciences, Manora peak, 263129 Nainital, Indiae-mail: [email protected]
2 SpaceLab, Department of Electrical Engineering, University of Cape Town, Private Bag X3, 7701 Rondebosch, South Africa3 South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa4 Department of Physics, Christ University, Hosur Road, 560029 Bangalore, Karnataka, India5 School of Studies in Physics and Astrophysics, Pt Ravishankar Shukla University, 492 010 Raipur, India6 Department of Physics, University of the North-West, Private Bag X2046, 2735 Mmabatho, South Africa7 National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, PR China
Received 25 August 2015 / Accepted 7 March 2016
ABSTRACT
Context. The Nainital-Cape Survey is a dedicated ongoing survey program to search for and study pulsational variability in chemicallypeculiar (CP) stars to understand their internal structure and evolution.Aims. The main aims of this survey are to find new pulsating Ap and Am stars in the northern and southern hemisphere and to performasteroseismic studies of these new pulsators.Methods. The survey is conducted using high-speed photometry. The candidate stars were selected on the basis of having Strömgrenphotometric indices similar to those of known pulsating CP stars.Results. Over the last decade a total of 337 candidate pulsating CP stars were observed for the Nainital-Cape Survey, making it oneof the longest ground-based surveys for pulsation in CP stars in terms of time span and sample size. The previous papers of this seriespresented seven new pulsating variables and 229 null results. In this paper we present the light curves, frequency spectra and variousastrophysical parameters of the 108 additional CP stars observed since the last reported results. We also tabulated the basic physicalparameters of the known roAp stars. As a part of establishing the detection limits in the Nainital-Cape Survey, we investigated thescintillation noise level at the two observing sites used in this survey, Sutherland and Nainital, by comparing the combined frequencyspectra stars observed from each location. Our analysis shows that both the sites permit the detection of variations of the order of0.6 milli-magnitude (mmag) in the frequency range 1–4 mHz, Sutherland is on average marginally better.
Key words. asteroseismology – methods: observational – surveys – stars: chemically peculiar – stars: oscillations
1. Introduction
A chemically peculiar (CP) star can be distinguished from achemically normal star by its spectrum, where anomalies can beseen on a visual inspection of low-dispersion spectra. The opti-cal spectra of the CP stars exhibit normal hydrogen lines com-bined with enhanced silicon, metal, and or rare-earth lines andweak calcium lines. The chemical peculiarities in these stars re-sult from the diffusion process (Michaud 1970; Michaud et al.1981; Babel 1992; Richer et al. 2000). Chemical elements withmany lines near flux maximum, such as iron peak and rare earthelements, are brought up to the surface by the dominance of ra-diation pressure over gravity in the radiative envelopes of thesestars, causing an apparent overabundance of such elements. Theelements with few lines near the flux maximum settle gravita-tionally and appear to be underabundant. Slow rotation is thusa basic condition to operate the diffusion process in CP stars.The CP stars are found on the main-sequence between spectral
? The dataset is only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/590/A116
types B2 and F5, from the zero-age main-sequence (ZAMS) tothe terminal-age main-sequence (TAMS), and have masses rang-ing from 1.5 to about 7 M�.
Based on their spectroscopic characteristics, Preston (1974)divided the CP stars into the following groups: Am/Fm (CP1),Ap/Bp (CP2), Hg-Mn (CP3), He weak and He strong (CP4)stars. Renson & Manfroid (2009) compiled an up-to-date catalogof 8205 CP stars. A subset of Ap and Am stars shows photomet-ric variability with periods ranging from a few minutes to a fewhours, and are the focus of the Nainital-Cape Survey.
The Am/Fm stars are relatively cool stars of spectral typeF5-A8, with temperatures ranging from 6500 K to 10 000 K. Thespectra of these stars exhibit an underabundance (weak lines)of Ca or Sc (or of both elements) and overabundance (stronglines) of Sr, Eu and other rare-earth elements. Some of the mem-bers of this group show δ Sct-type pulsational variability (Joshiet al. 2003, 2006, 2009; Smalley et al. 2011; Catanzaro & Ripepi2014; Hou et al. 2015). The Am stars rotate slower than chem-ically normal A-type stars and the frequency of binarity amongthese stars is much higher than among normal stars of the samemass (Abt & Golson 1962; Abt & Snowden 1973). It is well un-derstood that these stars do not exhibit strong global magnetic
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fields, however based on the observations from Kepler spacemission, Balona et al. (2015) found flares in two Am stars, whichstrongly suggests that at least some Am stars possess significantmagnetic fields.
The Ap/Bp stars have effective temperatures in the rangeof 6400 K to 15 000 K. These stars exhibit the most conspicu-ous chemical anomalies of all the CP stars: enhanced lines ofsome elements, particularly Si, Cr, Sr, Mn, Fe, Eu, Gd, andCe (overabundant by up to a factor of 106), and weak lines oflight elements (underabundant by a factor of 10−2). The Ap starsshow low rotation velocities with ve sin i usually not exceeding100 km s−1. These stars have strong global magnetic fields withan intensity ranging from hundreds of Gauss to tens of kilogauss.
The coolest subgroup of Ap stars (6400 K ≤ Teff ≤ 8700 K)located near the main-sequence (MS) part of the classical insta-bility strip, are known as roAp stars. Since the discovery of firstroAp star HD 101065 (Kurtz 1978), 61 other members of thisclass have been discovered (Smalley et al. 2015). The roAp starsshow pulsational variability in both the broad photometric bandsand in narrow spectral lines. These pulsations are character-ized as high-overtone, low-degree p-modes with typical periodsbetween 5.6 min and 23.6 min and photometric amplitudes rang-ing from a few micro-magnitudes (µmag) up to tens of milli-magnitudes (mmag) and radial velocity (RV) amplitudes rang-ing from a few m s−1 to km s−1. The roAp stars possess strongmagnetic fields with typical strengths of a few kG to tens ofkG (Hubrig et al. 2012) with overabundances of some rare earthelements that can exceed the solar value by 106 (Ryabchikovaet al. 2004). To date, there have been no roAp stars found inclose binary systems though a few Ap stars are in close bina-ries. The roAp stars are among the more challenging MS starsto model owing to their pulsations in the combined presence ofa strong global magnetic field together with element segregationand stratification, but at the same time they can be considered asstellar atomic physics laboratory.
The pulsation frequency spectrum of some of the roAp starsshows frequency multiplets with spacings corresponding to thefrequency of rotation of the star. This phenomenon can be ex-plained using the oblique pulsator model (Kurtz 1982), in whichthe pulsation axis is aligned with the axis of the magnetic field,which is assumed to be roughly a dipole inclined with respect tothe axis of rotation. As a star rotates, the observed aspect of thepulsation changes, leading to amplitude modulation and, in somecases, phase modulation. The driving mechanism of the pulsa-tions in roAp stars is thought to be the classical κ-mechanism op-erating in the partial hydrogen ionization zone (Balmforth et al.2001). Cunha & Gough (2001) suggested an alternative excita-tion mechanism for roAp stars where pulsation is driven by theturbulent pressure in the convection zone.
Some roAp stars have highly stable pulsation frequen-cies and amplitudes, even on timescales of years whileother roAp stars show frequency and amplitude variations ontimescales as short as hours (Medupe et al. 2015). Whether thisis a result of driving and damping, mode coupling or some in-stability is not known. It is important to know where in the roApinstability strip the stable and unstable pulsators lie.
The Kepler mission, launched in 2009 with the aim to detectand characterize Earth-sized planets in the habitable zone, hasrevolutionized our ability to detect and study very low-amplitudelight variations of the order of a few µ-mag in rather faint stars(Koch et al. 2010). The Kepler mission has enabled the discoveryof five roAp stars, all which have pulsation amplitudes muchbelow the detection limits of ground-based photometry.
While initially roAp stars were discovered and studied withphotometric methods, time-resolved spectroscopy has allowedthe study of wider physical aspects of the pulsating stellar atmo-sphere. The rapid radial velocity variations of spectral lines ofcertain chemical elements allow us to sample the velocity fieldin the stellar atmosphere as a function of atmospheric depth. Ofthe 61 known roAp stars, about a quarter of them were discov-ered using spectroscopic methods. A combination of simultane-ous spectroscopy and photometry constitutes the most sophis-ticated asteroseismic data set for any roAp star. The observedphase lag between the variations in luminosity and in RV is animportant parameter for modeling the stellar structure.
Similar to other pulsating stars, the roAp stars are also ex-cellent asteroseismic candidates through which one can comparethe observed frequency spectrum to the asymptotic pulsation the-ory and then obtain information about the spherical harmonicdegrees of the pulsation modes, the distortion of the modes fromnormal modes, atmospheric structures, evolutionary status andthe geometry of the magnetic field. Using such information onecan derive the various physical parameters such as rotation peri-ods, temperatures, luminosities, radii and their masses (see Joshi& Joshi 2015 for a recent review on asteroseismology of pulsat-ing stars). Although the extent of the roAp phenomenon has beenfairly well delineated in photometric and spectroscopic terms,there is as yet no known combination of these (and other) ob-servable parameters that can be used as a predictors of pulsationin any given Ap star. In other words, one can have two Ap starsthat are apparently similar in all observable parameters, whereone is a pulsating roAp star and the other has no detectable pul-sations and is a so-called “noAp” star.
The Nainital-Cape Survey was initiated in 1999 bythe Aryabhatta Research Institute of Observational Sciences(ARIES) at Manora Peak, Nainital, India, and the South AfricanAstronomical Observatory (SAAO) in Sutherland to search forpulsations in CP stars. The goals of the survey were: (i) to in-crease the number of known pulsating CP stars; (ii) to determinethe observational limits of the roAp phenomenon; and (iii) tobroaden the number and distribution (in parameter space) of es-tablished constant (noAp) stars, so as to shed some light on whatdistinguishes the pulsating from the apparently constant CP starsof similar spectral type and other observable physical parame-ters. This is the only survey of its kind that was conducted fromboth the northern and southern hemisphere. The first three pa-pers of this survey described the scope and methods of the sur-vey and reported the discovery of pulsations in several CP stars(Martinez et al. 2001; Paper I, Joshi et al. 2006; Paper II, Joshiet al. 2009: Paper III). The present paper is the fourth in this se-ries and presents the null results obtained for 108 stars observedduring the period of 2006 to 2009.
Similar to other papers of this series, the present paper is alsobased on photoelectric photometry of the sample stars and is or-ganized as follows: the target selection, observations and datareduction procedures are described in Sect. 2, followed by thefrequency analysis of the time series photometric data in Sect. 3.In Sect. 4, the observational limits for the detection of light vari-ations at the ARIES and SAAO sites are discussed. The starsclassified as null results and their basic astrophysical parametersare given in Sect. 5. In Sect. 6, we provide the basic physicalparameters of all the currently known roAp stars. In this section,we also compare the evolutionary status of the known roAp starsto the sample of stars observed under the Nainital-Cape Survey.The statistics of several surveys to search for new roAp stars arediscussed in Sect. 8. Finally, we outline the conclusions drawnfrom our study in Sect. 9.
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2. Target selection, observations and data reduction
2.1. Selection criteria
Following the target selection strategy of Martinez et al. (1991),the primary source of candidates for the Nainital-Cape Surveywas the subset of CP stars with Strömgren photometric indicessimilar to those of the known roAp stars. In this range, we alsofound many Am stars and included them in the list of targets.Apart from the sources of target mentioned in Martinez et al.(1991), we also included Ap/Am stars from Renson et al. (1991)and magnetic stars from Bychkov et al. (2003).
On the basis of the Strömgren photometric indices of knownroAp stars (see Table A.1), we revised the range of indices thatencompass the roAp phenomenon:
0.082 ≤ b − y ≤ 0.4310.178 ≤ m1 ≤ 0.387−0.204 ≤ δm1 ≤ 0.012
0.002 ≤ c1 ≤ 0.870−0.370 ≤ δc1 ≤ 0.031
2.64 ≤ β ≤ 2.88
where b− y is the color index and β measures the strength of theHβ line, which is indicator of temperature for stars in the spec-tral range from around A3 to F2. The m1 and c1 indices indicateenhanced metallicity and increased line blanketing, respectively.The parameters δm1 and δc1 measure the blanketing differenceand Balmer discontinuity relative to the ZAMS for a given β,respectively. Indices in the ranges given above are not an unam-biguous indicator of roAp pulsation, although they serve to nar-row down the field of candidates to the most promising subset.It is interesting to note that, whereas previously the roAp phe-nomenon seemed to be confined to the temperature range of theδ Scuti instability strip, it now appears that the roAp instabil-ity strip has a considerably cooler red edge, well into the F-typestars (see Fig. 2). As can be seen by the paucity of cooler starstested for pulsation, this is an area for future work, to establishmore firmly the cool edge of the roAp instability strip.
2.2. Photometric observations
For many roAp stars, the pulsational photometric variationshave amplitudes less than 20 mmag. The detection of such low-amplitude variations demands high-precision photometric obser-vations that can be attained with fast photometers mounted onsmall telescopes at observing sites such as ARIES Nainital inIndia and SAAO Sutherland South Africa. The ARIES obser-vations presented in this paper were acquired using the ARIEShigh-speed photoelectric photometer (Ashoka et al. 2001) at-tached to the 1.04-m Sampurnanand telescope at ARIES. TheSAAO observations were acquired using the Modular Photome-ter attached to the 0.5-m telescope and the University of CapeTown Photometer attached to the 0.75-m and 1.0-m telescopesat the Sutherland site of SAAO.
Each star was observed in high-speed photometric mode withcontinuous 10-sec integrations through a Johnson B filter. Theobservations were acquired in a single-channel mode (i.e. no si-multaneous comparison star observations), with occasional in-terruptions to measure the sky background, depending on thephase and position of the moon. To minimize the effects of see-ing fluctuations and tracking errors, we selected a photometricaperture of 30′′. Each target was observed continuously for 1–3 h at a time. Since the amplitudes of the rapid photometric os-cillations in roAp stars exhibit modulation due to rotation and
interference among frequencies of different pulsation modes, anull detection for pulsation may be obtained simply owing to acoincidence of the timing of the observations. Hence, each can-didate was observed several times.
2.3. Data reduction
The data reduction process began with a visual inspection of thelight curve to identify and remove obviously bad data points,followed by correction for coincidence counting losses, sub-traction of the interpolated sky background, and correction forthe mean atmospheric extinction. After applying these correc-tions, the time of the midpoint of the each observation was con-verted into a heliocentric Julian date (HJD) with an accuracy of10−5 day (∼1 s). The reduced data comprise a time-series of HJDand ∆B magnitude with respect to the mean of the light curve.
3. Frequency analysis
A fast algorithm (Kurtz 1985) based on the Deeming discreteFourier transform (DFT) for unequally spaced data (Deeming1975) was used to calculate the Fourier transformation. The lightcurves were also inspected visually for evidence of δSct oscilla-tions with periods of a few tens of minutes and longer. On thesetimescales, single-channel photometric data are affected by skytransparency variations and it is not always possible to distin-guish between oscillations in the star and variations in sky trans-parency. This is where the comparison of data of the same staracquired under different conditions on different nights is helpfulfor confirming the tentative detection of coherent oscillations ina given light curve.
After visual inspection of the light curves to search for indi-cations of δSct pulsations in a given light curve on timescaleslonger than about half an hour, we removed the sky transparencyvariations from the DFT data to reduce the overall noise levelto approximately the scintillation noise. This is practicable forsingle-channel data because, on good photometric nights, theroAp oscillation frequencies are generally well resolved from thesky transparency variations. To remove the effect of sky trans-parency variations, the DFT data were prewhitened to removesignals with frequencies in the range 0–0.9 mHz, which is thefrequency range commonly affected by sky transparency varia-tions in single-channel photometric data. These frequencies wereremoved until the noise level in the DFT of the residuals approx-imated a white noise spectrum. Depending on the stability of thephotometric transparency of a given night, it was generally pos-sible to correct for the effects of sky transparency by removing 3to 5 frequencies in the above mentioned frequency range.
The first and second panels of Fig. A.1 show the light curvesof the candidate stars filtered for low frequency sky transparencyvariations. The third and fourth panels show the prewhitened am-plitude spectra of the sample stars filtered for low-frequency skytransparency variations.
4. Noise level characterization
The detection limit for photometric variability depends upon theatmospheric noise, which consists of scintillation noise and skytransparency variations, and the photon noise. For the brighter(∼10 mag) stars, the atmospheric scintillation noise dominatesover the photon noise and is one of the fundamental factors lim-iting the precision of ground based photometry. In order to char-acterize the two observing sites used in the Nainital-Cape Survey
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and to put constraints on the detection limits for low amplitudevariability, we estimated the observational and the theoreticalscintillation noise values for both the sites.
Given the altitude and diameter of the telescope, and the ob-servational exposure time and airmass, one can find the contri-bution of scintillation noise in photometric measurements usingthe Young approximation (Young 1967, 1974). Using this scal-ing relation, it is possible to compare the level of scintillationnoise at different observatory sites. Although the precise amountof scintillation changes from night to night, the Young’s scalingrelation appears to hold very well for telescope apertures up to4 m, and for different sites (Kjeldsen & Frandsen 1991; Gilliland& Brown 1992; Gilliland et al. 1993). However, recent studies byKornilov et al. (2012) and Osborn et. al (2015) showed that thisequation tends to underestimate the median scintillation noiseat several major observatories around the world. Osborn et. al.(2015) presented a modified form of the Young approximation(Eq. (1)) that uses empirical correction coefficients to give morereliable estimates of the scintillation noise at a range of astro-nomical sites:
σ2Y = 10 × 10−6C2
Y D−4/3t−1(cos γ)−3 exp (−2hobs/H), (1)
where CY is the empirical coefficient, D is the diameter of thetelescope, t is the exposure time of the observation, γ is thezenith distance, hobs is the altitude of the observatory and Hthe scale height of the atmospheric turbulence, which is gener-ally accepted to be approximately 8000 m. All parameters arein standard SI units. The empirical coefficients CY for the ma-jor observatories around the world are listed by Osborne et al.(2015).
The theoretical values of scintillation noise for Sutherlandand Nainital were estimated using Eq. (1). The scintillation noisein terms of amplitude was obtained by taking the square rootof σY . However, we have to scale the theoretical value to com-pare the two sites with different telescope diameters. Therefore,the theoretical scintillation noise for SAAO (50 cm telescope)was scaled to the aperture of the ARIES telescope (104 cm)using the same relation. The input parameters used to estimatethe theoretical scintillation noise are: height (ARIES: 1958-m,SAAO: 1798 m), sec(Z) (airmass): 1, CY : 1.5, integration time:10 sect. The estimated scintillation values of ARIES (D: 104 cm)and SAAO (D: 50 cm) are 0.0338 mmag and 0.0433 mmag, re-spectively. The scaled value of the scintillation noise for SAAO(scaled to 104 cm) is 0.0340 mmag. Figure 1 shows the theoreti-cal noise levels for the ARIES and SAAO sites (both scaled andunscaled).
Since the observations in the Nainital-Cape Survey were car-ried out over many nights and in a variety of atmospheric con-ditions, the noise levels in the Fourier spectra of the individuallight curves are expected to be higher than the theoretical scin-tillation values for each site, and they are also not expected tobe white noise. We first transformed the time-series data of starsobserved from ARIES during 2006–2009 and from SAAO dur-ing 2006–2007 into their individual periodograms to estimatethe observational values of the noise in our amplitude spectra asa function of frequency. We then combined all the periodogramsfrom each site into a single pseudo-periodogram and fitted anacspline function to obtain the average estimated noise profileas a function of frequency. These observational noise curves areshown in Fig. 1 in solid blue for ARIES and dot-dashed red forSAAO. These noise profiles provide a useful first check of thesignificance of possible oscillation frequencies identified in theFourier spectra in Fig. 3 of this paper.
Fig. 1. Noise characteristics at the ARIES site at Nainital and SAAOSutherland site. The acspline-fitted curve of ARIES and SAAO ampli-tude spectra are shown in solid blue and dot-dashed red curves, respec-tively. The theoretical scintillation noise levels of ARIES and SAAO areshown with blue long-dashed and red small-dashed horizontal lines, re-spectively, and the scintillation noise level of SAAO (scaled to 104 cmdiameter) is also shown with a green dotted horizontal line.
More than half of the known roAp stars were discovered pho-tometrically from SAAO. One of the basic reasons behind this isthat the Sutherland site has stable and good sky transparency, fa-cilitating a closer match to scintillation noise than at many otherobserving sites used in other roAp surveys. However, in the lastten years that we have been running the Nainital-Cape Survey,we have noticed a gradual increase in sky brightness and at-mospheric noise owing to enhanced human activities around theARIES and Sutherland observatories. It can be inferred from thescaling relation (Eq. (1)) that the combined atmospheric noisecan be minimized by installing bigger telescopes at a good ob-serving site where one can find stable photometric sky conditions(Young 1967). A new 1.3 m optical telescope is now operationalat a new astronomical site of ARIES observatory known as Dev-asthal (longitude: 79◦40′57′′ E, latitude : 29◦22′26′′ N, altitude:2420-m). In addition, a new 3.6 m telescope has been recentlyinstalled at the Devasthal site and is likely to be operational by2016. The theoretical scintillation noise estimated for this tele-scope is 0.0217 mmag making the telescope very efficient for de-tecting tiny amplitude variations. The 0.5-m telescope of SAAOis also soon to be replaced with a 1.0-m robotic telescope. Theseupcoming observing facilities equipped with modern state-of-the-art instruments at ARIES and SAAO will be the next step toboost the Nainital-Cape Survey and other projects aimed at thedetection of sub-mmag light variations.
5. New null results from the Nainital-Cape Survey
We report the non-detections of pulsation in 108 CP stars.The first and second panels of Fig. A.1 depict the light curvesof the candidate stars observed from ARIES and SAAO. Theprewhitened frequency spectra of the respective time-series areplotted in the third and fourth columns. The name of the star,
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duration of observations in hours and the heliocentric Juliandates are denoted in each panel.
Here it is worth recalling that roAp stars show amplitudemodulation due to rotation and beating between multiple pulsa-tion frequencies. Therefore, the nondetection of light variationsmay be due to fact that the observations are acquired at a timewhen the pulsations are below the detection limit of the survey.For example, Joshi et al. (2006) classified HD 25515 as a nullresult and then subsequently, after further observations, classi-fied it as a δ Scuti-type pulsating variable (Joshi et al. 2009).Hence, a nulldetection of pulsations does not mean that the staris nonvariable, but rather that its light output was not detectedto vary during the particular interval of the observations. Thisdemonstrates the necessity for repeated observations of the can-didate stars. These null results are also an important contribu-tion toward understanding the distinction between pulsating andnonpulsating CP stars that are otherwise similar in all other ob-servational respects (Murphy et al. 2015). As mentioned above,a by-product of these null results is an observational character-ization of a particular observing site for data acquired on manynights over a wide range of observing conditions.
6. Comparison of known roAp stars with the nullresults
At the time the Nainital-Cape Survey began, only 23 roAp starswere known. Therefore, our knowledge of the extent of theroAp phenomenon at that time was used to define the targetselection and observing strategy. Since then, the number ofknown roAp stars has more than doubled, and currently standsat 61 confirmed members of this class. The compilation of thevarious physical parameters of the known roAp stars are impor-tant to study the roAp and noAp (“non-roAp”) phenomena inAp stars. Tables A.1 and A.2 list the astrophysical parameters ofthe known roAp stars extracted from the available sources in theliterature. For each star Table A.1 lists, the table entry number,the HD number of roAp star, their popular name, spectral type,Strömgren indices b−y, m1, c1, β, δm1, δc1, effective temperatureTeff , and reference(s) from which the data were taken. Table A.2lists the table entry number, HD or HR catalog number and othername(s) of the roAp star, visual magnitude mv, parallax π, dis-tance d, absolute magnitude Mv, luminosity parameter log
(L?L�
),
pulsational period corresponding to the highest amplitude, fre-quency separation ∆µ, maximum photometric amplitude varia-tion Amax, maximum radial velocity variation RVmax, rotationalperiod Prot, surface gravity log g, mass M?, radius R?, meanlongitudinal magnetic field, and the projected rotational velocityv sin i. Where no data is available in the data archives or in theliterature for a given parameter, this is denoted with a “-” symbolin the relevant column. It is instructive to compare the coverageof the Nainital-Cape Survey with the currently established extentof the roAp phenomenon. Therefore, the catalog of the basic pa-rameters of the known roAp stars can be used for the statisticalanalysis of roAp and noAp phenomena in Ap stars located in thesame part of the H-R diagram.
7. Evolutionary states of the studied samples
To establish the evolutionary status of the sample null resultstars, we first established their luminosities and effective temper-atures, which then allowed us to compare them with the knownroAp stars. The absolute magnitudes and luminosities of the
candidate stars observed in the Nainital-Cape Survey were de-termined based on the data taken from the Hipparcos catalog(van Leeuwen 2007). The photometric Teff is calculated fromthe Strömgren β indices using the grids of Moon & Dworet-sky (1985) that give a typical error of about 200 K. The variousastrophysical parameters of the stars observed in the Nainital-Cape Survey are listed in Table A.3. These parameters are ei-ther taken from the Simbad database or calculated using thestandard relations (Cox 1999). For each star, this Table lists theHD number, right ascension α2000, declination δ2000, visual mag-nitude mv, spectral type, parallax π, Strömgren indices b− y, m1,c1, β, δm1, δc1, effective temperature Teff , luminosity parame-ter log
(L?L�
), duration of the observations ∆t, heliocentric Julian
dates (HJD:2 450 000+) and year of observations (2000+) whenthe star was observed. The Strömgren indices δm1 and δc1 arecalculated using the calibration of Crawford (1975, 1979).
The absolute magnitude Mv in the V-band was determinedusing the standard relation (Cox 1999),
Mv = mv + 5 + 5 log π − Av, (2)
where π is trigonometric parallax measured in arcsec, the in-terstellar extinction in the V band is AV = RV E(B − V) =3.1E(B − V). The reddening parameter E(B − V) is obtained bytaking the difference of the observed colour (taken from the Sim-bad data base) and intrinsic colour (estimated from Cox 1999).
The stellar luminosity was calculated using the relation
logLL�
= −MV + BC − Mbol,�
2.5, (3)
where we adopted the solar bolometric magnitude Mbol,� =4.74 mag (Cox 1999), and used the standard bolometric correc-tion BC from Flower (1996). Taking all of the contributions tothe Mv and L?
L�error budgets into account, we find a typical un-
certainty of 20–25% for both parameters.The null objects shown in Fig. 2 include all the objects from
Papers I–IV (this paper) of the Nainital-Cape Survey. The posi-tions of known roAp stars and the newly discovered δ-Scuti typevariables in our survey are also shown. The evolutionary tracksfor stellar masses ranging from 1.5 to 3.0 M� (Christensen-Dalsgaard 1993) are overplotted. The position of the blue (left)and red (right) edges of the instability strip are shown withtwo oblique lines (Turcotte et al. 2000). Figure 2 clearly showsthat most of the sample stars are located within the instabilitystrip. For reasons given above, we may expect that some of thestars listed as null results in this paper may well turn out to bevariables in near future. However, with each subsequent non-detection of pulsations, the constraint on nonvariability will bestrengthened and they are established as “noAp” stars, thus help-ing to shed light on the other observational characteristics thatallow us to distinguish between pulsating and constant CP stars,which is one of the long-term goals of the Nainital-Cape Survey.
8. Ground-based surveys on pulsationin chemically peculiar stars
In the past, several surveys have been conducted around theglobe to search for roAp stars with different instrumental setupsindependently in both the northern and southern hemisphere.Such surveys required much telescope time, hence the photo-metric surveys were performed on 1 m class telescopes, where itwas possible to secure ample telescope time. Spectroscopic sur-veys became more popular in recent years because of improved
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Fig. 2. Positions of the null results (filled triangle) and δ-Scuti typevariables discovered under the Nainital-Cape Survey (filled square). Forcomparison, positions of known roAp stars are also shown (open star).The solid lines show theoretical evolutionary tracks from the ZAMS(Christensen-Dalsgaard 1993). The dashed lines indicate the red andblue edges of the instability strip.
sensitivity of the high-resolution spectroscopic instruments usedto search for low amplitude oscillations in roAp candidates. Themajor drawback of this technique remains the small amount ofobserving time available on large telescopes. In this section, weprovide a short description of the various surveys conducted forpulsation in CP stars.
8.1. Cape survey
Following the discovery of first roAp star HD 101065 in 1978,only 14 stars were known prior to 1990. A systematic surveyof roAp stars in the southern hemisphere was initiated by DonKurtz and Peter Martinez at SAAO with two objectives: firstto increase the number of members of this class and, second,to study the relationship between the roAp stars and the otherpulsating stars located at the same region of the H-R diagram.The observations for this survey were acquired with the pho-toelectric photometers attached to the 0.5-m and 1.0-m tele-scopes at Sutherland. Under the Cape survey 134 Southern ApSrCrEu stars were checked for the pulsational variability and 12new roAp stars were discovered (Martinez et al. 1991; Martinez& Kurtz 1994a, 1994b).
8.2. Nainital-Cape survey
The detection of the small amplitude light variations needs alot of observational expertise. As mentioned above most of theroAp stars known prior to 2000 were discovered under the Capesurvey, where the SAAO astronomers gained a lot of observa-tional experience. However, this meant that most of the knownroAp stars were southern objects. The Nainital-Cape Survey wasinitiated in 1999 as a collaboration between South African andIndian astronomers to increase the number of known roAp starsin the northern sky. This survey was started in 1999 and lastedfor ten years making it the most extensive survey for pulsation
in CP stars, where a total of of 337 Ap and Am stars weremonitored. Although only one new roAp star, HD 12098, wasdiscovered under this survey but the milli-magnitude level lightvariations with periods similar to those of the δ-Scuti stars wasdicovered in seven Am stars. This survey is thus unique in asense that both the Ap and Am stars were included in the sam-ples, hence there were plenty of chances to discover pulsationsin CP1 and CP2 stars. The null results of this survey have beenpublished in Martinez et al. (2001), Joshi et al. (2006, 2009) andin the present paper. The archive of well established null resultsis useful to delineate the extent of the roAp phenomenon and alsoto shed light on the distinction between roAp and noAp stars.
8.3. Lowell-Wisconsin survey
Between 1985 to 1991, Nelson & Kreidl (1993) conducted a sur-vey of pulsation in 120 northern Ap stars of spectral range B8–F4. Although these authors did not report the discovery of anynew roAp stars from their survey, their main finding was the ab-sence of pulsation in the spectral range B8–A5, indicating thatroAp-like oscillations are likely to be confined to the cooler pe-culiar stars.
8.4. The Hvar survey
A photometric survey was initiated in 2011 to search for newnorthern roAp stars at the Hvar observatory (Paunzen et al.2012, 2015). For this survey, a CCD based photometer attachedto the 1.0 m Austrian-Croatian telescope was used for the ob-servations of candidate stars. Under this survey, 80 candidateroAp stars were examined for a total duration of 100 h. Differen-tial CCD photometry was performed to detect the light variationsin the sample Ap stars. The authors have not reported any posi-tive detections and have presented the frequency spectra and thebasic parameters of the null results they observed.
8.5. Other minor photometric surveys
In addition to the above surveys, a number of smaller photo-metric surveys have also been conducted independently in thenorthern and southern hemisphere by Dorokhova & Dorokhov(1998), Kurtz (1982), Matthews et al. (1988), Heller & Kramer(1990), Schutt (1991), Belmonte (1989), Hildebrandt (1992),and Handler & Paunzen (1999). Though these surveys aresmall in terms of sample size and number of newly discoveredroAp stars, they have helped to define candidate selection criteriafor other roAp surveys.
8.6. Spectroscopic surveys
Spectroscopy of high spectral and temporal resolution usinglarge telescopes permits the detailed study of line profile vari-ations (Hatzes & Mkrtichian 2005). After the discovery of sig-nificant RV pulsational variations in some known roAp stars(Kanaan & Hatzes 1998), in the last ten years candidateroAp stars have been monitored with time resolved high res-olution spectroscopic observations by several observers. Theseobservations revealed that the highest RV amplitudes are ob-served in the spectral lines of the rare earth elements, while spec-tral lines of the other elements show weak or undetectable os-cillations. Using spectroscopic techniques, about 15 roAp starshave been discovered (Kochukhov 2006; Kochukhov et al. 2008,2009, 2013; Alentive et al. 2012; Elkin et al. 2005a; 2005b;Kurtz et al. 2006).
A116, page 6 of 36
S. Joshi et al.: The Nainital-Cape Survey. IV.
9. Conclusions
In this paper, we presented the light curves and frequency spectraof the 108 candidate stars observed in the Nainital-Cape Survey.Analyses of the photometry acquired at Sutherland and Naini-tal indicate that we have achieved a detection level of about0.6 mmag in the frequency range 1–5 mHz in the Nainital-CapeSurvey. Using the standard relations and data extracted from theliterature we presented the various astrophysical parameters ofthe null results. We also compiled the basic physical parame-ters of the known roAp stars. On comparing the positions of theknown roAp stars to the observed sample stars in the H-R dia-gram, we infer that the boundary of the roAp phenomenon ex-tends beyond the cool edge of the classical instability strip.
Acknowledgements. This work was carried out under the Indo-South AfricaScience and Technology Cooperation INT/SAFR/P-3(3)2009) and NRFgrant UID69828 funded by Departments of Science and Technology of the In-dian and South African Governments. S.C. acknowledges support under theIndo-Russian grant INT/RFBR/P-118 through which he received a stipend toperform this work. We acknowledge use of SIMBAD, NASA’s ADS and ESA’sHipparcos database.
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A116, page 7 of 36
A&A 590, A116 (2016)
App
endi
xA
Tabl
eA
.1.T
hekn
own
roA
pst
ars
and
thei
rphy
sica
lpar
amet
ers.
S.N
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arna
me
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2000
δ 200
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m1
c 1δm
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1β
Teff
Ref
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Type
mag
mag
mag
mag
mag
mag
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J000
800
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172
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979
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9249
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9623
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0.26
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2.82
478
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HD
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1110
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pSr
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Cr)
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6300
123
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902.
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9,20
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643
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731
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7100
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195
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831
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HD
1342
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0.21
60.
223
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th(2
015)
;46.
Kur
tz&
Mar
tinez
(199
5);4
7.B
alon
aet
al.(
2011
);48
.Sm
alle
yet
al.(
2015
);49
.Koc
hukh
ov&
Rya
bchi
kova
(200
1);5
0.M
artin
ezet
al.(
1996
);51
.Mar
tinez
etal
.(19
90);
52.M
artin
ezet
al.(
1998
);53
.Kre
idle
tal.
(199
1);5
4.G
onza
lez
et.a
l(20
08).
A116, page 8 of 36
S. Joshi et al.: The Nainital-Cape Survey. IV.
Tabl
eA
.1.c
ontin
ued.
S.N
.St
arna
me
Oth
erα
2000
δ 200
0Sp
.b-y
m1
c 1δm
1δc
1β
T eff
Ref
.na
me
Type
mag
mag
mag
mag
mag
mag
K33
.H
D13
7909
βC
rB15
2750
+29
0620
F0p
0.14
10.
257
0.74
0–0
.056
0.00
22.
839
7800
3134
.H
D13
7949
33L
ib15
2935
–17
2627
ApS
rEuC
r0.
196
0.31
10.
580
–0.1
05–0
.236
2.81
877
0032
,33,
3435
.H
D14
3487
1601
44–3
054
57A
3SrE
uCr
0.31
10.
262
0.39
3–0
.089
–0.1
692.
706
7000
1736
.H
D14
8593
1629
39–1
435
06A
2Sr
––
––
––
7850
2937
.J1
640
1640
03–0
737
30A
8pSr
Eu
––
––
––
7400
138
.H
D15
0562
1644
11–4
839
18A
/F(p
Eu)
0.30
10.
212
0.65
9–0
.015
–0.0
872.
783
7500
439
.H
D15
1860
1652
59–5
409
46A
2SrE
u0.
327
0.22
10.
538
––
–70
5029
40.
HD
1547
0817
1028
–58
0017
Ap
0.27
70.
256
0.46
4–0
.079
0.01
52.
757
7200
3541
.H
D16
1459
1748
30+
5155
02A
pEuS
rCr
0.24
50.
246
0.67
9–0
.040
–0.1
412.
820
7950
3642
.H
D16
6473
1812
26–3
745
09A
pSrE
uCr
0.20
80.
321
0.51
4–0
.118
–0.2
682.
801
7700
37,3
843
.K
IC00
7582
608
1844
12+
4317
51A
p–
––
––
–87
0039
44.
HD
1762
3210
Aql
1858
47+
1354
24F0
pSrE
u0.
150
0.20
80.
829
–0.0
040.
031
2.80
974
0040
,41
45.
KIC
0101
9592
619
0527
+47
1548
Ap
––
––
––
7400
4246
.K
IC00
8677
585
1906
28+
4450
33A
5p–
––
––
–76
0043
47.
HD
1777
6519
0710
–26
1954
A5S
rEuC
r0.
248
0.26
10.
731
–0.0
54–0
.110
2.83
480
0044
48.
J192
119
2129
+47
1053
F3p
SrE
uCr
––
––
––
6200
4549
.H
D18
5256
1939
20–2
944
34A
pSr(
EuC
r)0.
277
0.18
50.
615
–0.0
04–0
.039
2.73
872
5046
50.
J194
019
4008
–44
2009
F2(p
Cr)
––
––
––
6900
151
.K
IC01
0483
436
1946
29+
4737
50A
p–
––
––
–73
8847
52.
HD
2259
14K
IC00
4768
731
1948
26+
3951
58A
p–
––
––
–77
2648
53.
HD
1902
9020
1356
–78
5242
ApE
uSr
0.28
90.
293
0.46
6–0
.091
–0.3
062.
796
7500
3654
.H
D19
3756
2024
12–5
143
25A
pSrC
rEu
0.18
10.
213
0.76
0–0
.008
–0.0
402.
810
7500
3655
.H
D19
6470
2038
10–1
730
06A
pSrE
u(C
r)0.
211
0.26
30.
650
–0.0
59–0
.144
2.80
778
5036
56.
HD
2016
01γ
Equ
2110
20+
1007
54F0
p0.
147
0.23
80.
760
–0.0
32–0
.058
2.81
976
0049
,50
57.
HD
2039
3221
2604
–29
5548
ApS
rEu
0.17
50.
196
0.74
20.
004
–0.0
202.
791
7200
5158
.H
D21
3637
2233
12–2
002
22A
(pE
uSrC
r)0.
298
0.20
60.
411
–0.0
35–0
.031
2.67
064
0052
59.
HD
2175
2223
0147
–44
5027
Ap(
Si)C
r0.
289
0.22
70.
484
–0.0
56–0
.015
2.69
171
0053
60.
HD
2184
9523
0928
–63
3912
A2p
EuS
r0.
114
0.25
20.
812
–0.0
49–0
.098
2.87
080
0036
61.
HD
2189
9423
1316
–60
3503
A3S
r0.
154
0.19
60.
826
0.00
80.
032
2.80
776
0054
A116, page 9 of 36
A&A 590, A116 (2016)Ta
ble
A.2
.Add
ition
alpa
ram
eter
sfo
rthe
know
nro
Ap
star
s.
S.N
.St
arna
me
mv
πd
MV
log(
L ?/L�)
Ppu
l∆µ
Am
axR
Vm
axP
rot
logg
M?
R?
Mag
.Fie
ldv
sin
im
agm
aspc
mag
min
µH
zm
mag
kms−
1da
ysde
xM�
R�
kGkm
s−1
1.J0
008
10.1
6–
––
–9.
58–
0.76
––
––
––
–2.
HD
6532
8.40
6.14
162.
872.
201.
227.
1047
5.00
1.15
1.94
4.30
––
0.22
303.
HD
9289
9.38
––
2.42
–10
.52
–3.
500.
858.
554.
15–
–0.
6510
.54.
HD
1209
88.
07–
––
–7.
61–
3.00
–5.
464.
201.
701.
701.
4610
5.H
D12
932
10.2
5–
–2.
55–
11.6
1–
4.00
1.40
3.53
4.15
––
1.20
2.50
6.H
D19
918
9.34
4.07
245.
702.
341.
0611
.04
–2.
001.
30–
4.34
––
1.60
3.00
7.H
D24
355
9.65
––
––
6.42
–1.
38–
13.9
5–
––
––
8.H
D24
712
6.00
20.3
249
.21
2.32
0.87
6.13
6810
.00
0.25
12.4
64.
301.
551.
773.
105.
609.
HD
4265
96.
767.
6013
1.58
2.38
1.48
9.70
520.
800.
70–
4.40
2.10
–0.
3919
.00
10.
HD
2580
4810
.52
––
––
8.49
–1.
49–
––
––
––
11.
J065
111
.51
––
––
10.8
8–
0.79
––
––
––
–12
.H
D60
435
8.89
4.41
226.
761.
541.
1411
.90
5216
.00
1.90
7.68
4.40
1.82
–0.
3010
.813
.H
D69
013
9.56
––
––
11.2
2–
–0.
20–
4.50
––
2.90
6.0
14.
HD
7544
57.
129.
3010
8.34
1.96
1.17
9.00
––
0.29
2.08
4.32
1.81
–2.
982
15.
J085
510
.80
––
––
7.30
–1.
40–
3.09
––
––
–16
.H
D80
316
7.78
7.25
137.
932.
261.
117.
40–
2.00
0.32
2.08
4.58
1.70
1.53
0.18
32.0
17.
HD
8336
86.
1714
.16
70.6
22.
471.
0911
.60
–10
.00
3.33
2.85
4.20
1.76
2.00
0.50
33.0
18.
HD
8404
19.
33–
–2.
38–
1560
6.00
0.50
3.69
4.30
––
0.48
25.0
19.
HD
8618
19.
323.
4928
6.53
2.49
1.01
6.20
–4.
60–
––
––
0.40
–20
.H
D92
499
8.89
3.54
282.
481.
631.
0510
.40
––
0.06
6–
4.00
1.68
–8.
153.
321
.H
D96
237
9.43
1.53
653.
59–
1.61
13.8
9–
–0.
10–
4.30
––
2.90
622
.H
D97
127
9.43
––
––
13.5
1–
0.66
––
––
––
–23
.H
D99
563
8.67
3.92
255.
101.
901.
1010
.70
–10
.00
4.9
2.91
4.20
2.03
1.90
0.57
28.0
24.
HD
1010
657.
998.
9311
1.98
2.09
0.91
12.1
668
13.0
01.
033.
944.
201.
521.
982.
304.
025
.H
D11
5226
8.51
6.80
147.
062.
670.
8610
.86
––
1.24
3.30
4.00
1.60
–0.
7527
26.
HD
1161
147.
027.
7112
9.70
1.35
1.32
21.3
0–
–0.
65–
4.10
2.07
–0.
502.
227
.H
D11
9027
10.0
2–
–3.
040.
678.
6352
2.00
0.14
8–
4.40
––
3.10
4.0
28.
J143
011
.56
––
––
6.11
–1.
06–
––
––
––
29.
HD
1229
708.
338.
6711
5.34
2.94
0.82
11.1
868
2.00
1.05
3.88
4.20
1.50
1.80
0.22
4.2
30.
HD
1288
983.
2060
.35
16.5
71.
901.
046.
8250
5.00
0.80
4.48
4.20
1.70
1.90
1.50
13.5
31.
HD
1322
058.
72–
––
–7.
14–
–0.
097
–4.
40–
–5.
209.
5032
.H
D13
4214
7.46
9.74
102.
672.
600.
885.
69–
7.00
0.72
248
4.05
1.60
1.80
2.70
2.6
33.
HD
1379
093.
6829
.17
34.2
81.
171.
4616
.20
––
0.04
18.4
94.
401.
601.
455.
303.
534
.H
D13
7949
6.67
11.2
888
.65
1.88
1.17
8.27
403.
000.
33–
4.30
1.78
2.60
4.70
3.0
35.
HD
1434
879.
42–
––
–9.
63–
–0.
047
–5.
00–
–4.
701.
536
.H
D14
8593
9.13
––
––
10.6
9–
––
–4.
40–
–3.
005.
0037
.J1
640
12.6
7–
––
–9.
48–
3.52
–3.
67–
––
––
38.
HD
1505
629.
82–
–2.
68–
10.8
050
0.80
0.14
–4.
40–
–5.
001.
5
A116, page 10 of 36
S. Joshi et al.: The Nainital-Cape Survey. IV.
Tabl
eA
.2.c
ontin
ued.
S.N
.St
arna
me
mv
πd
MV
log(
L ?/L�)
Ppu
l∆µ
Am
axR
Vm
axP
rot
logg
M?
R?
Mag
.Fie
ldv
sin
im
agm
aspc
mag
min
µH
zm
mag
kms−
1da
ysde
xM�
R�
kGkm
s−1
39.
HD
1518
609.
01–
––
–12
.30
––
–0.
083
4.50
––
2.50
4.5
40.
HD
1547
088.
766.
7514
8.15
2.39
0.73
8.00
––
0.09
5.37
4.11
1.50
1.70
24.5
04.
041
.H
D16
1459
10.3
3–
–2.
47–
12.0
0–
1.30
––
4.38
––
1.76
–42
.H
D16
6473
7.92
––
2.52
1.24
8.80
682.
000.
10–
4.47
1.80
–8.
502.
543
.K
IC00
7582
608
11.2
5–
––
1.21
7.90
–1.
45–
20.4
54.
302.
371.
773.
05–
44.
HD
1762
325.
8912
.76
78.3
72.
551.
3211
.60
510.
600.
54–
4.10
2.00
2.50
1.40
2.7
45.
KIC
0101
9592
610
.66
––
–1.
5017
.14
550.
078
0.17
15.
683.
601.
703.
605
2146
.K
IC00
8677
585
10.1
9–
––
0.80
10.2
837
0.03
3–
4.30
3.90
1.80
2.50
3.20
4.2
47.
HD
1777
659.
15–
––
1.50
23.6
––
0.14
8–
3.80
2.20
–3.
602.
548
.J1
921
12.1
6–
––
–11
.18
–1.
99–
––
––
––
49.
HD
1852
569.
94–
––
–10
.33
–3.
000.
15–
4.30
––
0.71
6.2
50.
J194
013
.02
––
––
8.16
–4.
16–
9.58
––
––
–51
.K
IC01
0483
436
11.4
3–
––
0.84
12.3
2–
0.06
8–
4.30
4.15
1.60
1.61
–20
52.
KIC
0047
6873
19.
17–
––
–23
.4–
0.06
2–
––
––
––
53.
HD
1902
909.
91–
–2.
49–
7.34
402.
000.
504.
034.
54–
–3.
2316
54.
HD
1937
569.
20–
–2.
55–
13.0
0–
0.90
0.74
–4.
29–
–0.
1917
.055
.H
D19
6470
9.72
––
2.52
–10
.80
–0.
70–
–4.
37–
–1.
48–
56.
HD
2016
014.
6827
.55
36.3
02.
491.
1012
.40
303.
000.
58–
4.20
1.74
2.16
3.80
2.5
57.
HD
2039
328.
82–
–2.
65–
5.94
662.
000.
33–
4.30
––
0.26
74.
758
.H
D21
3637
9.61
––
–1.
0311
.50
–1.
500.
36<
253.
601.
60–
0.74
3.5
59.
HD
2175
227.
5211
.36
88.0
32.
770.
8513
.70
584.
000.
128.
554.
201.
491.
861.
702.
760
.H
D21
8495
9.38
––
2.23
–7.
44–
1.00
0.79
–4.
40–
–0.
9116
.061
.H
D21
8994
8.56
3.55
281.
691.
251.
0614
.20
––
0.09
3–
4.10
––
0.44
05.
2
A116, page 11 of 36
A&A 590, A116 (2016)
Tabl
eA
.3.C
Pst
ars
obse
rved
forp
ulsa
tion
from
AR
IES
and
SAA
Oan
dcl
assi
fied
asnu
llre
sults
inth
issu
rvey
.
S.N
.St
arα
2000
δ 200
0mv
Sp.
πb−y
m1
c 1β
δm1
δc1
T eff
log(
L/L �
)∆
tH
JDY
earo
fH
Dm
agTy
pem
asm
agm
agm
agm
agm
agm
agK
hrO
bser
vatio
n1.
1169
0016
05+
0806
567.
60A
58.
83±
0.69
0.18
70.
240
0.71
62.
772
–0.0
47–0
.008
7455
1.18
0.45
4365
071.
0743
6607
2.14
8600
1918
+59
0820
7.28
B9V
6.32±
0.83
––
––
––
––
2.78
4071
062.
4143
6707
1.91
4375
073.
7343
7607
1.42
4400
072.
1844
0107
3.22
4402
072.
8444
2807
2.09
4429
073.
2837
0032
09+
4342
429.
16A
0p2.
75±
1.08
––
––
––
––
1.42
4459
074.
3321
0036
22+
3338
398.
42A
36.
34±
0.90
––
––
––
––
2.07
4397
075.
6757
0108
53+
4512
277.
70A
0Vp
3.35±
0.91
––
––
––
––
1.35
4427
071.
0144
3107
6.76
7601
1607
–34
0856
8.37
A5p
3.50±
0.74
0.08
50.
280
0.71
52.
830
–0.0
73–0
.120
8008
1.47
1.95
4097
067.
8441
0124
19+
4308
326.
67A
2p4.
88±
0.59
0.02
20.
141
1.14
52.
833
0.06
60.
306
9617
1.97
2.30
4751
088.
8783
0124
00–7
219
287.
82A
p3.
99±
0.44
0.07
20.
199
1.08
6–
––
––
2.89
4077
069.
1109
001
4635
–67
2806
10.7
8A
p–
––
––
––
–1.
1921
2701
3.45
2128
0110
.11
948
0158
51+
5534
547.
85F0
p6.
71±
0.73
0.11
50.
242
0.87
92.
873
–0.0
160.
027
8323
1.50
0.97
4459
0711
.12
211
0200
33+
2753
199.
00A
7V7.
12±
1.97
––
––
––
––
0.69
4399
074.
4244
0107
2.14
4402
0712
.14
433
0221
55+
5714
346.
39A
1Ia
0.79±
0.46
0.46
3–0
.088
0.91
32.
606
––
––
1.98
2238
0113
.15
144
0226
00–1
520
285.
86A
6Vsp
12.9
8±
0.74
0.40
20.
213
0.29
82.
584
––
––
1.86
4085
0614
.15
550
0230
38+
1951
196.
14A
9V15
.14±
0.46
0.15
60.
187
0.83
52.
776
––
––
1.54
4431
0715
.16
145
0235
04–1
717
227.
64A
p4.
33±
0.71
0.02
80.
201
1.05
7–
––
––
1.41
4087
061.
9940
8806
1.92
4089
061.
9240
9006
16.
1703
402
4542
+48
0837
8.63
B8V
+0.
92±
0.90
––
––
––
––
1.68
4427
0717
.17
835
0251
52+
0254
498.
9A
4–
0.16
0.17
0.96
2.84
––
––
0.91
2216
0118
.18
078
0256
32+
5610
418.
30A
0p–
0.08
70.
251
1.07
92.
831
–0.0
440.
243
7947
–0.
9644
5907
19.
1861
002
5418
–73
2710
8.14
Ap
4.69±
0.54
0.11
40.
347
0.61
7–
––
––
2.03
4098
062.
0341
0106
20.
2088
003
1608
–73
3256
7.95
Ap
–0.
094
0.20
81.
030
––
––
–1.
8640
9206
21.
2174
603
3000
–12
2839
9.41
K0/
K1I
V–
––
––
––
––
1.07
3659
0522
.21
985
0332
25–0
318
488.
3A
1V5.
63±
0.83
0.11
30.
160.
952
2.85
6–
––
–2.
9441
0407
2.27
4108
0723
.22
374
0336
58+
2312
406.
72A
2p7.
65±
0.46
0.06
90.
178
1.09
12.
879
0.02
20.
163
8397
1.70
2.63
4750
08
Not
es.T
heir
phys
ical
para
met
ers
are
liste
d.
A116, page 12 of 36
S. Joshi et al.: The Nainital-Cape Survey. IV.
Tabl
eA
.3.c
ontin
ued.
S.N
.St
arα
2000
δ 200
0mv
Sp.
πb−y
m1
c 1β
δm1
δc1
Teff
log(
L/L �
)∆
tH
JDY
earo
fH
Dm
agTy
pem
asm
agm
agm
agm
agm
agm
agK
hrO
bser
vatio
n24
.22
488
0332
46–6
643
467.
50A
p4.
39±
0.45
––
––
––
––
1.93
4092
0625
.23
207
0342
44–1
842
507.
54A
p4.
83±
0.71
0.10
60.
259
0.85
6–
––
––
1.96
4091
0626
.23
393
0344
29–1
203
318.
30F0
III
4.35±
0.91
0.22
20.
164
0.77
22.
753
0.02
40.
133
7271
1.36
1.96
4094
0627
.24
825
0355
16–3
845
336.
81B
94.
23±
0.33
–0.0
390.
173
1.08
32.
835
0.03
50.
241
9683
1.99
1.34
4077
0628
.25
154
0359
48–0
001
129.
88A
56.
74±
1.41
––
––
––
––
1.21
4397
0729
.25
487
0403
54+
2807
338.
08B
8V4.
82±
0.99
––
––
––
––
0.98
4459
0730
.25
999
0408
18+
3227
367.
51A
p6.
11±
0.85
––
––
––
––
1.15
4815
091.
5248
6909
1.43
4870
0931
.27
463
0416
21–6
056
546.
36A
p7.
92±
0.42
0.02
20.
224
0.89
02.
874
–0.0
23–0
.028
9214
1.61
1.78
4091
0632
.28
430
0427
22–4
011
508.
20A
p2.
52±
0.61
––
––
––
––
1.89
4094
0633
.29
578
0436
31–5
437
168.
51A
p3.
74±
0.61
––
––
––
––
1.93
4095
0634
.31
225
0453
12–2
046
197.
02A
p5.
32±
0.68
0.09
30.
191.
079
––
––
–2.
3340
8806
1.91
4089
061.
3840
9006
35.
3406
005
1203
–49
0337
7.82
B9V
p2.
74±
0.48
––
––
––
––
1.91
4095
0636
.34
162
0515
31+
0545
358.
68F0
4.79±
1.13
0.14
80.
186
0.93
52.
834
0.02
70.
153
7982
1.15
1.34
4400
0737
.34
205
0515
06–1
506
019.
32A
p–
0.13
50.
215
0.96
22.
911
––
––
1.60
2288
021.
5922
8902
1.92
2296
022.
1426
8303
2.24
2686
032.
2126
9303
38.
3545
005
2824
+58
4029
8.16
A3
7.42±
0.87
––
––
––
––
1.48
4397
0739
.36
955
0535
04–0
124
069.
58A
2–
0.05
70.
198
0.84
82.
866
0.00
5–0
.054
8270
–1.
0844
2707
40.
3730
805
3653
–17
0059
8.71
A–
––
––
––
––
1.78
4096
0641
.38
719
0544
20–5
654
587.
50A
p4.
19±
0.45
0.01
10.
206
1.03
8–
––
––
2.19
4095
0642
.38
817
0550
37+
4400
417.
56A
27.
27±
0.76
0.06
60.
217
0.94
22.
860
–0.0
120.
052
8209
1.50
1.51
4071
0643
.39
082
0550
24+
0457
247.
42B
96.
63±
0.53
–0.0
270.
220
0.88
72.
873
–0.0
19–0
.029
1045
12.
421.
1644
2807
44.
3957
505
5224
–26
1728
7.83
A0
4.08±
0.70
–0.0
740.
267
0.90
5–
––
––
2.15
4098
0645
.40
277
0551
26–7
028
468.
33A
p4.
45±
0.60
0.04
10.
239
0.90
1–
––
––
1.99
4102
0746
.40
886
0600
28–2
753
188.
21A
00.
83±
0.74
––
––
––
––
2.06
4096
0647
.41
089
0600
51–4
252
146.
57B
9III
p4.
25±
0.29
––
––
––
––
3.03
4092
0648
.41
511
0604
59–1
629
044.
97A
1V3.
59±
0.31
0.18
60.
030
1.32
32.
775
0.16
40.
593
9377
3.18
1.99
4103
0749
.41
786
0608
02+
2117
447.
29F0
9.70±
1.09
0.19
30.
275
0.69
02.
782
–0.0
780.
000
7557
2.30
1.11
4101
0650
.42
326
0609
17–1
717
307.
70A
p6.
66±
0.66
0.00
80.
231
0.92
2–
––
––
2.48
4091
0651
.43
901
0616
14–4
749
468.
20A
p1.
44±
0.46
0.13
20.
228
0.94
62.
860
–0.0
230.
056
8208
2.35
1.99
4097
0652
.44
195
0620
42+
0516
427.
54F0
11.2
2±
0.75
0.17
90.
188
0.70
52.
753
––
––
1.96
2285
0253
.44
903
0625
20+
2303
248.
36A
5–
0.06
90.
204
0.97
92.
867
––
––
1.17
2285
0254
.45
297
0626
42+
0352
189.
23B
9–
––
––
––
––
2.19
4165
0755
.45
698
0627
11–3
706
078.
15A
25.
60±
0.56
0.06
90.
244
0.84
6–
––
–1.
9941
0106
56.
4731
106
4001
+42
3355
8.71
F03.
760.
217
0.20
40.
756
2.74
6–
––
–1.
7819
4301
A116, page 13 of 36
A&A 590, A116 (2016)
Tabl
eA
.3.c
ontin
ued.
S.N
.St
arα
2000
δ 200
0mv
Sp.
πb−y
m1
c 1β
δm1
δc1
Teff
log(
L/L �
)∆
tH
JDY
earo
fH
Dm
agTy
pem
asm
agm
agm
agm
agm
agm
agK
hrO
bser
vatio
n57
.48
953
0646
49+
1646
206.
8F5
10.3
90.
247
0.30
80.
623
2.75
2–
––
–1.
1022
1001
0.91
2305
0258
.51
496
0700
57+
5651
139.
83F5
––
––
––
––
–2.
0141
0607
59.
5168
406
5629
–40
5925
7.94
Ap
3.58±
0.60
0.15
40.
248
0.76
82.
832
––
––
2.10
4088
0660
.55
719
0712
16–4
029
565.
31A
3spe
7.93±
0.38
0.01
20.
217
1.03
02.
880
–0.0
170.
100
9101
2.28
2.09
4102
0761
.56
148
0719
48+
6135
299.
00F0
–0.
204
0.17
80.
628
2.72
20.
000
0.04
470
46–
1.05
4104
0762
.56
350
0713
40–5
340
046.
69A
p6.
61±
0.26
––
–2.
799
––
––
2.45
4096
0663
.61
763
0738
47–4
449
487.
94A
psh
2.54±
0.41
––
––
––
––
2.35
4097
0664
.66
195
0756
47–7
042
598.
65A
p5.
17±
0.76
0.04
30.
227
0.88
6–
––
––
2.03
4103
0765
.70
338
0821
53+
1337
267.
32A
25.
51±
0.76
0.17
30.
271
0.80
52.
814
––
–1.
450.
9323
3802
66.
7261
108
3217
–41
4956
7.01
Ap
5.61±
0.42
–0.0
620.
192
0.74
8–
––
––
2.27
4098
060.
9641
0106
67.
7263
408
2943
–67
0823
7.27
Ap
3.35±
0.45
–0.0
110.
185
1.02
5–
––
––
2.01
4103
0768
.72
943
0836
08+
1518
496.
32F0
IV12
.86±
0.45
0.21
10.
186
0.73
22.
720
–0.0
090.
152
6991
1.16
1.13
4099
0669
.73
095
0837
35+
3150
318.
85A
3–
0.19
0.19
50.
702
2.74
6–
––
–0.
9622
3901
70.
7334
508
3838
+19
5923
8.14
F0V
–0.
121
0.21
00.
883
2.81
2–0
.004
0.14
077
80–
1.19
4429
0771
.73
574
0839
43+
2005
117.
75A
5V–
0.12
70.
207
0.87
12.
799
–0.0
040.
093
7659
–2.
4741
6407
1.61
4166
0772
.74
067
0840
19–4
015
505.
20B
9V11
.68±
0.50
–0.0
500.
220
0.89
82.
846
–0.0
130.
036
1041
2–
2.38
4102
0773
.75
445
0848
42–3
914
017.
12A
39.
23±
0.45
0.15
90.
218
0.72
9–
––
––
2.80
2288
021.
4522
8902
1.97
2296
021.
9927
0403
2.04
2709
032.
1627
1003
74.
7644
408
5707
+29
1257
9.11
F03.
11±
1.02
0.17
60.
191
0.75
22.
745
–0.0
060.
128
7204
1.27
1.44
4104
0775
.78
388
0909
52+
4949
567.
61F0
III
9.25±
0.66
0.23
10.
172
0.71
02.
709
0.00
20.
153
6900
0.92
2.28
4103
0776
.82
417
0930
22–4
648
489.
24A
p–
––
––
––
––
5.14
3483
0577
.86
170
0956
45–0
217
208.
42A
23.
20±
0.98
0.07
40.
226
0.92
9–
––
––
1.39
4428
071.
7744
3107
1.55
4459
0778
.88
385
1009
49–5
644
538.
09A
p4.
85±
0.55
0.00
60.
230.
863
2.82
2–
––
–1.
9441
7407
79.
8870
110
1300
–37
3012
9.27
B9
2.36±
0.99
––
––
––
––
1.34
4175
0780
.10
0809
1136
14+
1441
518.
25A
m7.
12±
0.85
0.1
0.26
90.
856
2.84
5–
––
–1.
4120
0901
81.
1040
4411
5853
–43
2255
9.57
Ap
––
––
––
––
–0.
9134
8205
82.
1063
7412
1418
–33
4644
7.37
A2
5.63±
0.54
––
––
––
––
0.97
3482
0583
.11
7044
1327
30+
1354
498.
19F0
II5.
25±
0.76
0.20
90.
211
0.67
42.
749
–0.0
250.
043
7267
1.19
1.32
4104
0784
.11
7290
1330
13–4
907
589.
25A
p–
––
––
––
––
1.97
4174
073.
2241
7507
1.41
4178
071.
5041
7907
2.48
4180
07
A116, page 14 of 36
S. Joshi et al.: The Nainital-Cape Survey. IV.Ta
ble
A.3
.con
tinue
d.
S.N
.St
arα
2000
δ 200
0mv
Sp.
πb−y
m1
c 1β
δm1
δc1
Teff
log(
L/L �
)∆
tH
JDY
earo
fH
Dm
agTy
pem
asm
agm
agm
agm
agm
agm
agK
hrO
bser
vatio
n3.
4841
8107
85.
1276
0814
3347
–46
4533
8.56
Ap
––
––
––
––
–4.
6635
1505
86.
1402
2015
4410
–44
0650
7.97
Ap
––
––
––
––
–2.
0134
8305
87.
1448
9716
0951
–41
0927
8.59
Ap
5.61±
1.04
––
––
––
––
2.01
2507
021.
6025
1102
1.71
2513
021.
6325
1602
1.58
2520
0288
.14
9769
1640
47–6
225
549.
75A
p–
––
––
––
––
3.79
2123
0189
.16
1423
1752
02–7
141
249.
31A
p–
––
––
––
––
3.37
2127
011.
2421
2801
90.
1626
3917
5441
–50
2645
9.93
Ap
––
––
––
––
–1.
0634
8205
91.
1642
5818
0015
+00
3746
6.37
A3s
pe7.
39±
0.52
0.08
70.
181
1.09
92.
905
––
––
0.53
3518
0592
.16
8767
1822
30–2
654
408.
71A
0–
––
––
––
––
1.50
3482
0593
.16
9380
1826
06–3
754
429.
83A
3–
––
––
––
––
2.02
2128
0194
.17
0397
1829
47–1
434
556.
02A
p9.
54±
0.36
–0.0
290.
190
0.92
52.
837
0.01
80.
080
1044
73.
851.
9842
9807
95.
1729
7618
4103
+44
1616
7.29
F0II
I5.
03±
0.48
0.18
10.
234
0.82
72.
788
–0.0
350.
126
7578
1.62
2.03
4251
071.
1143
7407
96.
1736
1218
4630
–08
2558
9.08
A0
––
––
––
––
–2.
7435
1505
97.
1788
9219
0955
+14
5758
8.94
B9
4.53±
1.10
––
––
––
––
0.86
4375
0798
.18
3806
1933
22–4
516
185.
58A
p8.
22±
0.40
–0.0
250.
167
1.06
22.
849
0.03
90.
194
9816
2.01
2.59
4295
0799
.18
7474
1951
51–3
952
285.
32A
p10
.82±
0.88
–0.0
470.
203
0.86
42.
820
0.00
30.
044
1070
61.
933.
2042
9407
100.
1880
0819
5427
–36
3432
8.86
A5
–0.
040
0.24
80.
858
2.88
0–0
.048
–0.0
7287
97–
1.43
4296
0710
1.19
0401
2003
09+
4128
286.
99A
m9.
34±
0.35
0.22
00.
209
0.72
82.
744
–0.0
260.
059
7204
2.13
1.13
4374
072.
4043
7507
2.01
4376
0710
2.19
6604
2036
50+
4454
408.
12A
38.
04±
0.70
0.22
20.
218
0.63
32.
737
––
––
1.07
1832
0010
3.20
4367
2128
41–2
538
397.
83A
05.
07±
0.77
––
––
––
––
2.09
4295
0710
4.20
5087
2132
27+
2323
406.
68B
9sp
5.87±
0.36
–0.0
640.
189
0.75
22.
799
0.01
4–0
.589
1190
61.
941.
3544
2807
105.
2087
5922
0054
–64
5741
9.98
Ap
––
––
––
––
–2.
0221
2701
1.67
2128
0110
6.21
2385
2224
38–3
907
376.
84A
2p7.
92±
0.63
0.06
70.
225
0.94
6–
––
––
2.04
4294
0710
7.21
6018
2249
26–1
120
577.
62A
78.
03±
0.66
0.16
50.
318
0.56
1–
––
––
1.35
2574
022.
5025
8502
2.69
2586
022.
2425
8802
2.16
2589
022.
1725
9002
108.
2906
6505
3510
–00
5013
9.44
B9
–0.
037
0.20
70.
829
2.85
4–0
.001
–0.0
4991
67–
1.34
4459
071.
9444
9208
A116, page 15 of 36
A&A 590, A116 (2016)
Time (hours) Frequency (mHz)
Fig. A.1. The light curves (left columns) of the pulsation candidate stars observed from ARIES/SAAO and their corresponding prewhitenedamplitude spectra (right columns). The light curves have been binned to 40-s integrations.
A116, page 16 of 36
S. Joshi et al.: The Nainital-Cape Survey. IV.
Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 17 of 36
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Fig. A.1. continued.
A116, page 18 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 19 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 20 of 36
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Fig. A.1. continued.
A116, page 21 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 22 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 23 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 24 of 36
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Fig. A.1. continued.
A116, page 25 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 26 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 27 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 28 of 36
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Fig. A.1. continued.
A116, page 29 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 30 of 36
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Fig. A.1. continued.
A116, page 31 of 36
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Fig. A.1. continued.
A116, page 32 of 36
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Fig. A.1. continued.
A116, page 33 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 34 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 35 of 36
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Time (hours) Frequency (mHz)
Fig. A.1. continued.
A116, page 36 of 36