J/MNRAS/413/813 ATLAS3D project. I. (Cappellari+, 2011)
The ATLAS3D project.
I. A volume-limited sample of 260 nearby early-type galaxies: science goals and
selection criteria.
Cappellari M., Emsellem E., Krajnovic D., McDermid R.M., Scott N.,
Verdoes Kleijn G.A., Young L.M., Alatalo K., Bacon R., Blitz L., Bois M.,
Bournaud F., Bureau M., Davies R.L., Davis T.A., De Zeeuw P.T., Duc P.-A.,
Khochfar S., Kuntschner H., Lablanche P.-Y., Morganti R., Naab T.,
Oosterloo T., Sarzi M., Serra P., Weijmans A.-M.
<Mon. Not. R. Astron. Soc., 413, 813-836 (2011)>
=2011MNRAS.413..813C 2011MNRAS.413..813C
ADC_Keywords: Surveys ; Galaxy catalogs ; Radial velocities ; Photometry
Keywords: galaxies: distances and redshifts -
galaxies: elliptical and lenticular, cD - galaxies: evolution -
galaxies: formation - galaxies: kinematics and dynamics -
galaxies: structure
Abstract:
The ATLAS3D project is a multiwavelength survey combined with a
theoretical modelling effort. The observations span from the radio to
the millimetre and optical, and provide multicolour imaging,
two-dimensional kinematics of the atomic (HI), molecular (CO) and
ionized gas (Hβ, [OIII] and [NI]), together with the kinematics
and population of the stars (Hβ, Fe5015 and Mgb), for a carefully
selected, volume-limited (1.16x105Mpc3) sample of 260 early-type
(elliptical E and lenticular S0) galaxies (ETGs). The models include
semi-analytic, N-body binary mergers and cosmological simulations of
galaxy formation. Here we present the science goals for the project
and introduce the galaxy sample and the selection criteria. The sample
consists of nearby (D<42Mpc, |DE-29°|<35°, |b|>15°)
morphologically selected ETGs extracted from a parent sample of 871
galaxies (8 per cent E, 22 per cent S0 and 70 per cent spirals)
brighter than MK←21.5mag (stellar mass M*≳6x109M☉).
Description:
The ATLAS3D sample includes all nearby ETGs observable from the
northern Earth hemisphere, and for this reason we hope its homogeneous
data set will ultimately constitute a legacy for future studies. We
trust that our and other groups will exploit our data and sample well
beyond what we had originally envisioned. Our first steps in the
directions outlined above are presented in the following papers, while
the other aspects will be presented in subsequent papers of this
series.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 71 260 The Atlas3D sample or
260 early-type (E and S0) galaxies
table4.dat 71 611 The 611 spiral galaxies in the Atlas3D parent sample
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See also:
J/MNRAS/414/888 : ATLAS3D project. III (Emsellem+, 2011)
J/MNRAS/414/940 : ATLAS3D project. IV (Young+, 2011)
J/MNRAS/416/1680 : ATLAS3D project. VII (Cappellari+, 2011)
J/MNRAS/433/2812 : ATLAS3D project. XXIII (Krajnovic+, 2013)
J/MNRAS/446/120 : ATLAS3D project. XXIX (Duc+, 2015)
J/MNRAS/448/3484 : ATLAS3D Project. XXX (McDermid+, 2015)
Table 1: Selection criteria for the galaxies in the ATLAS3D parent sample
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Distance: D<42Mpc
Galaxies total mag: MK←21.5mag
Observability: |DE-29°|<35°
Galaxy zone of avoidance: |b|>15°
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Table 2: Main characteristics of the ATLAS3D parent sample
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Survey volume: Vol=1.16x105Mpc3
Galaxy K-band luminosity: L>8.2x109L☉,K
Galaxy stellar mass: M*≳6x109M☉
Galaxy B-band total mag: MB≲-18.0mag
Galaxy SDSS r-band total mag: Mr≲-18.9mag
Total number of galaxies: Ngal=871
Spiral and irregular galaxies: NSp=611 (70%)
S0 galaxies in ATLAS3D (T>-3.5): NS0=192 (22%)
E galaxies in ATLAS3D (T≤-3.5): NE=68 (8%)
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Byte-by-byte Description of file: table[34].dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Gal Galaxy name
12- 21 F10.6 deg RAdeg Right ascension in decimal degrees (J2000)
23- 32 F10.6 deg DEdeg Declination in decimal degrees (J2000)
34 I1 --- SBF [0/2] 1 if the galaxy is in Tonry et al.
(2001ApJ...546..681T 2001ApJ...546..681T) and 2 if it is in
Mei et al. (2007ApJ...655..144M 2007ApJ...655..144M) or both
36- 37 I2 --- NED-D Number of redshift-independent distance
determinations listed in the NED-D catalogue,
excluding the ones based on kinematical
scaling relations
39 I1 --- Virgo [0/1] 1 if the galaxies is contained within a
sphere of radius R=3.5Mpc from the centre of
the cluster (1)
41- 44 I4 km/s Vhel Heliocentric velocity (2)
46- 49 F4.1 Mpc Dist Distance (3)
51- 56 F6.2 mag KMAG Total absolute K magnitude (4)
58- 61 F4.2 mag AB B-band foreground galactic extinction from
Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S)
63- 66 F4.1 --- T-type Morphological T type from HyperLeda (5)
68- 71 F4.2 [arcsec] log(Re) Projected half-light effective radius (6)
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Note (1): assumed at coordinates RA=12:28:19 and DE=+12:40
(Mould et al., 2000ApJ...529..786M 2000ApJ...529..786M) and distance D=16.5Mpc
(Mei et al., 2007ApJ...655..144M 2007ApJ...655..144M)
Note (2):
* For table3 (early-type), measured from the SAURON integral
field stellar kinematics (1σ error ΔVhel=5km/s).
* For table4 (spirals), from NED.
Note (3): origin of distance:
* when SBF=1 the distance comes from Tonry et al. (2001ApJ...546..681T 2001ApJ...546..681T),
corrected by subtracting 0.06mag to the distance modulus (Mei et al.
2007ApJ...655..144M 2007ApJ...655..144M);
* when SBF=2 the distance comes from Mei et al. (2007ApJ...655..144M 2007ApJ...655..144M);
* when SBF=0 and NED-D>0 the distance is the median of the NED-D values,
excluding the ones based on kinematical scaling relations;
* when SBF=NED-D=0 and the galaxy is in Virgo (Virgo=1) then it is
assigned the cluster distance D=16.5Mpc (Mei et al., 2007ApJ...655..144M 2007ApJ...655..144M);
* otherwise D=Vcosmic/H0, with H0=72km/s/Mpc, where Vcosmic is the
velocity derived from Vhel via the local flow field model of Mould
et al. (2000ApJ...529..786M 2000ApJ...529..786M) using only the Virgo attractor.
Note (4): derived from the apparent magnitude KT (2MASS keyword kmext)
at the adopted distance D and corrected for the foreground galactic
extinction: MK=KT-5log10D-25-AB/11.8, which assumes AB/AK=11.8.
Note (5): E: T≤-3.5; S0: -3.5<T≤-0.5. This morphology was not the one
used for the sample selection.
Note (6): It was derived from a combination of RC3 and 2MASS
determinations, which both use growth curves, as described in
Section 4.1, but it was normalized to agree on average with RC3.
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History:
From electronic version of the journal
References:
Krajnovic et al., Paper II 2011MNRAS.414.2923K 2011MNRAS.414.2923K
Emsellem et al., Paper III 2011MNRAS.414..888E 2011MNRAS.414..888E
Young et al., Paper IV 2011MNRAS.414..940Y 2011MNRAS.414..940Y
Davis et al., Paper V 2011MNRAS.414..968D 2011MNRAS.414..968D
Bois et al., Paper VI 2011MNRAS.416.1654B 2011MNRAS.416.1654B
Cappellari et al., Paper VII 2011MNRAS.416.1680C 2011MNRAS.416.1680C, Cat. J/MNRAS/416/1680
Khochfar et al., Paper VIII 2011MNRAS.417..845K 2011MNRAS.417..845K
Duc et al., Paper IX 2011MNRAS.417..863D 2011MNRAS.417..863D
Davis et al., Paper X 2011MNRAS.417..882D 2011MNRAS.417..882D
Crocker et al., Paper XI 2012MNRAS.421.1298C 2012MNRAS.421.1298C
Lablanche et al., Paper XII 2012MNRAS.424.1495L 2012MNRAS.424.1495L
Serra et al., Paper XIII 2012MNRAS.422.1835S 2012MNRAS.422.1835S
Krajnovic et al., Paper XIV 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Cappellari et al., Paper XV 2013MNRAS.432.1709C 2013MNRAS.432.1709C
Bayet et al., Paper XVI 2013MNRAS.432.1742B 2013MNRAS.432.1742B
Krajnovic et al., Paper XVII 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Alatalo et al., Paper XVIII 2013MNRAS.432.1796A 2013MNRAS.432.1796A
Sarzi et al., Paper XIX 2013MNRAS.432.1845S 2013MNRAS.432.1845S
Cappellari et al., Paper XX 2013MNRAS.432.1862C 2013MNRAS.432.1862C
Scott et al., Paper XXI 2013MNRAS.432.1894S 2013MNRAS.432.1894S
Martig et al., Paper XXII 2013MNRAS.432.1914M 2013MNRAS.432.1914M
Krajnovic et al., Paper XXIII 2013MNRAS.433.2812K 2013MNRAS.433.2812K, Cat. J/MNRAS/433/2812
Davis et al., Paper XXIV 2013MNRAS.429..534D 2013MNRAS.429..534D
Cappellari et al., Paper XXV 2013MNRAS.432.1709C 2013MNRAS.432.1709C
Bayet et al., Paper XXVI 2013MNRAS.432.1742B 2013MNRAS.432.1742B
Krajnovic et al., Paper XXVII 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Alatalo et al., Paper XXVIII 2013MNRAS.432.1796A 2013MNRAS.432.1796A
Duc et al., Paper XXIX 2015MNRAS.446..120D 2015MNRAS.446..120D
McDermid et al., Paper XXX 2015MNRAS.448.3484M 2015MNRAS.448.3484M, Cat. J/MNRAS/448/3484
(End) Patricia Vannier [CDS] 14-Nov-2011