J/MNRAS/471/1428 MASSIVE Survey. VII. (Veale+, 2017)
The MASSIVE Survey. VII. The relationship of angular momentum, stellar mass and
environment of early-type galaxies.
Veale M., Ma C.-P., Greene J.E., Thomas J., Blakeslee J.P., Mcconnell N.,
Walsh J.L., Ito J.
<Mon. Not. R. Astron. Soc., 471, 1428-1445 (2017)>
=2017MNRAS.471.1428V 2017MNRAS.471.1428V (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Morphology ; Photometry, infrared
Keywords: galaxies: elliptical and lenticular, cD - galaxies: evolution -
galaxies: formation - galaxies: kinematics and dynamics -
galaxies: structure
Abstract:
We analyse the environmental properties of 370 local early-type
galaxies (ETGs) in the MASSIVE and ATLAS3D surveys, two
complementary volume-limited integral-field spectroscopic (IFS) galaxy
surveys spanning absolute K-band magnitude - 21.5≥MK≥-26.6, or
stellar mass 8*109≲M*≲2*1012M☉. We find these galaxies to
reside in a diverse range of environments measured by four methods:
group membership (whether a galaxy is a brightest group/cluster
galaxy, satellite or isolated), halo mass, large-scale mass density
(measured over a few Mpc) and local mass density (measured within the
Nth neighbour). The spatially resolved IFS stellar kinematics provide
robust measurements of the spin parameter λe and enable us to
examine the relationship among λe, M* and galaxy
environment. We find a strong correlation between λe and
M*, where the average λe decreases from ∼0.4 to below 0.1
with increasing mass, and the fraction of slow rotators fslow
increase from ∼10 to 90 per cent. We show for the first time that at
fixed M*, there are almost no trends between galaxy spin and
environment; the apparent kinematic morphology-density relation for
ETGs is therefore primarily driven by M* and is accounted for by the
joint correlations between M* and spin, and between M* and
environment. A possible exception is that the increased fslow at
high local density is slightly more than expected based only on these
joint correlations. Our results suggest that the physical processes
responsible for building up the present-day stellar masses of massive
galaxies are also very efficient at reducing their spin, in any
environment.
Description:
The MASSIVE survey consists of a volume-limited sample of ETGs,
targeting all 116 galaxies1 with K-band magnitudes MK brighter than
-25.3mag (i.e. stellar masses M*≳1011.5M☉) and distances
within D<108Mpc, in the Northern hemisphere and away from the Galactic
plane (Ma et al., 2014, Cat. J/ApJ/795/158).
We have completed observations of the 'priority sample' of the MASSIVE
survey, which consists of the 75 galaxies with MK←25.5mag
(M*≳1011.7M☉). The observations were performed using the
Mitchell/VIRUS-P IFS at the McDonald Observatory, which has a large
107x107arcsec2 field of view and consists of 246 evenly spaced
4-arcsec-diameter fibres with a one-third filling factor.
We use four different measures to quantify galaxy environments and to
investigate the connection between galaxy environments and stellar
kinematics for the galaxies in the MASSIVE and ATLAS3D surveys:
(1) group membership from the group catalogues of Crook et al. (2007,
Cat. J/ApJ/655/790) constructed from the 2MASS Redshift Survey (2MRS;
Huchra et al., 2012, Cat. J/ApJS/199/26);
(2) halo mass from the same group catalogues, available for galaxies
in a group with three or more members;
(3) a smoothed large-scale density field from Carrick et al.
(2015MNRAS.450..317C 2015MNRAS.450..317C) based on the 2M++ redshift catalogue of Lavaux &
Hudson (2011, Cat. J/MNRAS/416/2840) and
(4) a local galaxy luminosity density calculated within the volume to
the 10th neighbour, similar to ν10 in Cappellari et al. (2011,
Cat. J/MNRAS/416/1680).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 90 115 Properties of MASSIVE survey galaxies
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See also:
J/ApJ/795/158 : The MASSIVE survey. 116 candidate galaxies (Ma+, 2014)
J/ApJ/837/40 : The MASSIVE survey. VI. Warm ionized gas. (Pandya+, 2017)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Galaxy Galaxy name (in order of increasing RA)
13- 20 F8.4 deg RAdeg Right ascension (J2000)
22- 29 F8.4 deg DEdeg Declination (J2000)
31- 35 F5.1 Mpc Dist Distance according to Ma et al.
(2014, Cat. J/ApJ/795/158)
37- 42 F6.2 mag gMAG Extinction-corrected total absolute
K-band magnitude
44- 48 F5.2 [Msun] logM* Stellar mass estimated from MK
50- 53 F4.2 --- Ell Ellipticity from NSA where available,
from 2MASS otherwise (* in n_Ell)
54 A1 --- n_Ell [*+] Note on Ell (1)
56- 59 F4.2 --- lambdae ? Proxy for the spin parameter within the
effective radius
61 A1 --- Rot [SF] Slow or fast rotator classification (2)
63 A1 --- Env [BSI] Group membership according to the
HDC catalogue (3)
65- 68 F4.1 [Msun] logMhalo ? Halo mass according to the HDC catalogue, or
from updated literature sources (see text)
for Virgo, Coma and Perseus
70- 76 A7 --- Cluster Membership in Virgo, Coma, Perseus or Abell
clusters
78- 81 F4.1 --- 1+deltag Large-scale galaxy overdensity from the 2M++
catalogue (Lavaux & Hudson, 2011,
Cat. J/MNRAS/416/2840) (Section 3.3)
83- 90 F8.1 --- nu10 Local density in units of the mean K-band
luminosity density (2.8x108L☉/Mpc3)
--------------------------------------------------------------------------------
Note (1): Note on Ell as follows:
* = from 2MASS
+ = NGC 1129 and NGC 4472 are from our CFHT data and Emsellem et al.
(2011, Cat. J/MNRAS/414/888), respectively; see Veale et al.
(2017MNRAS.464..356V 2017MNRAS.464..356V) for details.
Note (2): Most galaxies are slow rotators (S), with few fast rotators (F).
See Section 4.1 for definitions.
Note (3): Most galaxies are BGG (B), with few satellite (S) or
isolated (I) galaxies.
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History:
From electronic version of the journal
References:
Ma et al., Paper I 2014ApJ...795..158M 2014ApJ...795..158M, Cat. J/ApJ/795/158
Greene et al., Paper II 2015ApJ...807...11G 2015ApJ...807...11G
Davis et al. Paper III 2016MNRAS.455..214D 2016MNRAS.455..214D
Goulding et al., Paper IV 2016ApJ...826..167G 2016ApJ...826..167G
Veale et al. Paper V 2017MNRAS.464..356V 2017MNRAS.464..356V
Pandya et al., Paper VI 2017ApJ...837...40P 2017ApJ...837...40P, Cat. J/ApJ/837/40
Veale et al. Paper VIII 2018MNRAS.473.5446V 2018MNRAS.473.5446V
Goullaud et al., Paper IX 2018ApJ...856...11G 2018ApJ...856...11G
Ene et al., Paper X 2018MNRAS.479.2810E 2018MNRAS.479.2810E
Davis et al., Paper XI 2019MNRAS.486.1404D 2019MNRAS.486.1404D
Greene et al., Paper XII 2019ApJ...874...66G 2019ApJ...874...66G
Ene et al., Paper XIII 2019ApJ...878...57E 2019ApJ...878...57E
Ene et al., Paper XIV 2020ApJ...891...65E 2020ApJ...891...65E
Liepold et al., Paper XV 2020ApJ...891....4L 2020ApJ...891....4L
(End) Patricia Vannier [CDS] 17-May-2020