the low-luminosity galaxy population in the ngc 5044 groupthe low-luminosity galaxy population in...
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The low-luminosity galaxy population in theNGC 5044 Group
Sergio A. Cellone (Fac. Cs. Astronómicas y Geofísicas, UNLP — CONICET, Argentina)
Alberto Buzzoni (INAF — Osservatorio Astronomico di Bologna, Italy)
Imaging: 79 galaxiesSpectra: 13 galaxies• ESO 3.6 m + EFOSC2 (griz)• CASLEO 2.15 m (BV)
(Cellone & Buzzoni, 2005, MNRAS, 356, 41; 2005 A3 Annual Meeting)
m-M = 31.9162 members and
candidates(Ferguson & Sandage
1990, AJ 100, 1)
<vr> = 2461 km/s
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Dwarf ellipticals(dE)
N42
N75
N83N34
N49N134 N31
Dwarf irregulars(dI)
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Dwarf ellipticals(dE)
Dwarf irregulars(dI)
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Early-type dwarf galaxies with:
• embedded spiral structure, bars and/or disks
• rotation
Fornax
Virgo
ComaThey could be remnants of “harassed” disk galaxies.
(Moore et al. 1998, ApJ 495, 139)
• Jerjen et al. 2000, A&A 358, 845
• De Rijcke et al. 2001, ApJ 559, L21
• Pedraz et al. 2002, MNRAS 332, L59
• Barazza et al. 2002, A&A 391, 823
• Simien & Prugniel 2002, A&A 384, 371
• De Rijcke et al. 2003, A&A 400, 119
• Barazza et al. 2003, A&A 407, 121
• Graham et al. 2003, AJ 186, 1787
(etc.)
-18 < MB < -16
(VLT - Keck - HST)
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N153 – d:S0 (dwarf? lenticular)
MB = -17.2 vr = 2816 km/s
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Cellone 1999, A&A 345, 403
Young & Currie 2001, A&A 369, 736
Cellone & Buzzoni 2001, A&A 369, 742
N42: dE,N
MB = -16.9
vr = 2462 km/s
µ (r) = µ0 + 1.067 (r/r0)n
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e
a4
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Colour profiles
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dE/dS0: their profiles CANNOT be fit by a Sérsic model; both positive and negative systematic residuals are left (red curve). Usually they show isophote twisting and ellipticity gradients (∆ε ≥ 0.1).
A good fit is obtained with a “disk + bulge” model (blue).
Classification
(See also Aguerri et al. 2005, AJ 130, 475)
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dE: their profiles are well fit by a Sérsic model. In general, no isophote twisting is detected.
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dSph: mostly uncatalogued objects, with central surface brightnesses ≥ 24 mag arcsec-2 and absolute magnitudes Mg ≥ -12.
Im: Magellanic irregulars .
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N93
bSp or Sm?
N93AdSph
Mg = −13.1 µ0 = 25.1
N93BdSph
Mg = −10.4µ0 = 25.0
Some new dwarfs
N93CdE,N
Mg = −12.2 µ0 = 24.4
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N156: dE
MB = -15.1
N156
N155
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dI/dE: very low surface brightness objects; their profiles are nearly exponentials (Sérsic index n=1), and very extended.
No direct evidences of recent star formation; however, some showpeculiar structures (“arms”).
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Background galaxies
N109: dE,NDefinite member (m=1)
vr = 5409 km/s
Sdm (near background)
Uncatalogued galaxy
vr > 28000 km/sE (background)
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NG
C 5
04
4 G
rou
p m
em
bers 17
13
21
10
(18 background galaxies)
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Magnitude ― surface brightness
MB = –17
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Distribution of radial velocities
Shown in colour: dwarf galaxies (BT > 15 mag).
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Spatial distribution
NGC 5044
Projected density map (1° 40’ x 1° 40’).
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Distribution of projected distances (arcmin) to the Group centre (10 arcmin = 63 kpc).
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Distribution of projected distances (arcmin) to the closest bright (BT≤15) galaxy (10 arcmin = 63 kpc).
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Colour — magnitude diagram
N139: z ~ 0.4
(See also Lisker, Grebel & Binggeli
2005, astro-ph/0505048)
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Conclusions
- There are hints (poor statistics!) for S0+dE/dS0’s having:
• Broader distributions than E+dE’s, both in radial velocity and projected position.
• Bluer colours at the same luminosity.
- dSph’s are preferentially (almost exclusively) found near bright galaxies.
- Early-type dwarfs and giants have very similar radial velocity distributions.
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Colour — colour diagram
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Residuals:observed profile ― model
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Ellipticity distributions
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Future:
Search for “hidden” structure in dE galaxies
“Unsharp masking” and model subtraction on CCD images
Internal kinematics High-resolution spectra
Relation between structure and stellar populations
Multicolour photometry and spectra
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N46: dE,N
Likely member (m=2)
S (background)
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Systematic residual from Sérsic fit are quantified by:
where I(ρ) is the observed profile, S(ρ) is the Sérsic fit, and k=1 if |Ri| > 1% while k=0 otherwise.
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µ (r) = µ0 + 1.067 (r/r0)n
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M32
NGC205
“The Andromeda galaxy (M31)”
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“The humble dwarf galaxy is one of the most interesting objects in the universe.”
... dwarf galaxies may hold the key to many questions of galaxy formation, structure and evolution.
... dwarfs are expected to trace the mass in hierarchical theoríes of galaxy formation ...
Impey et al. (1988, ApJ 330, 634)
• building blocks for the formation of more massive galaxies.
• remnants of interactions.
• relatively simple systems: test benches for theories of galaxy formation and evolution of stellar populations.
• etc.
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Surface brightness profiles
Sérsic Law:
(José Luis Sérsic, 1968, Atlas de Galaxias Australes, Obs. Astronómico de Córdoba, Argentina)
µ (r) = µ0 + 1.067 (r/r0)n
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magnitude central surf. brightness
n (
pro
file
sh
ap
e)
Luminosiy – n (profile shape) relation
Cellone, Forte, & Geisler (1994, ApJS 93, 397)
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Projected density distribution (deg-2) around each galaxy.
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Facultad de Ciencias Astronómicas y GeofísicasUniversidad Nacional de La Plata, Argentina
Research Group onGlobular Clusters & Dwarf Galaxies
http://www.fcaglp.unlp.edu.ar/CGGE
Members• Dr. Juan Carlos Forte Full Professor, UNLP – Principal Researcher, CONICET• Dr. E. Irene Vega Professor, UNLP – Researcher, CONICET• Dr. Lilia P. Bassino Professor, UNLP – Researcher, CONICET• Dr. Sergio A. Cellone Professor, UNLP – Researcher, CONICET• Lic. Favio R. Faifer Lab. Assistant, UNLP – Fellow, CONICET• Lic. Analía Smith Castelli Lab. Assistant, UNLP – Fellow, CONICET• Lic. Alejandro Cifuentes Thesist
External Collaborators • Dr. Alberto Buzzoni Osservatorio Astronomico di Bologna, Italia• Dr. Boris Dirsch Universidad de Concepción, Chile• Dr. Tom Richtler Universidad de Concepción, Chile• Dr. Duncan Forbes Swinburne University of Technology, Australia
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Galaxy N50, NGC5044 GroupCellone & Buzzoni (2001, A&A 369, 742)
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NGC 5044 (E)
NGC 5054(Sb)
ESO 510-G13(© HST)
• Morphological continuity S0 / SB0 – E (bars and disks)
(eg.: Nieto et al. 1992, A&A 257, 97)
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Colour — magnitude diagram
Dashed-line: Coma Cluster dwarfs (Secker et al. 1997, PASP 109, 1377).Open symbols: background objects.