J/ApJ/849/20 Contents of RESOLVE & ECO galaxy groups (Eckert+, 2017)
The baryonic collapse efficiency of galaxy groups in the RESOLVE and ECO
surveys.
Eckert K.D., Kannappan S.J., Del P. Lagos C., Baker A.D., Berlind A.A.,
Stark D.V., Moffett A.J., Nasipak Z., Norris M.A.
<Astrophys. J., 849, 20-20 (2017)>
=2017ApJ...849...20E 2017ApJ...849...20E (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, optical; Stars, masses; Velocity dispersion; Surveys
Keywords: galaxies: halos; galaxies: luminosity function, mass function; surveys
Abstract:
We examine the z=0 group-integrated stellar and cold baryonic (stars +
cold atomic gas) mass functions (group SMF and CBMF) and the baryonic
collapse efficiency (group cold baryonic to dark matter halo mass
ratio) using the RESOLVE and ECO survey galaxy group catalogs and a
GALFORM semi-analytic model (SAM) mock catalog. The group SMF and CBMF
fall off more steeply at high masses and rise with a shallower
low-mass slope than the theoretical halo mass function (HMF). The
transition occurs at the group-integrated cold baryonic mass
Mbarycold∼1011M☉. The SAM, however, has significantly
fewer groups at the transition mass ∼1011M☉ and a steeper
low-mass slope than the data, suggesting that feedback is too weak in
low-mass halos and conversely too strong near the transition mass.
Using literature prescriptions to include hot halo gas and potential
unobservable galaxy gas produces a group BMF with a slope similar to
the HMF even below the transition mass. Its normalization is lower by
a factor of ∼2, in agreement with estimates of warm-hot gas making up
the remaining difference. We compute baryonic collapse efficiency with
the halo mass calculated two ways, via halo abundance matching (HAM)
and via dynamics (extended all the way to three-galaxy groups using
stacking). Using HAM, we find that baryonic collapse efficiencies
reach a flat maximum for groups across the halo mass range of
Mhalo∼1011.4-12M☉, which we label "nascent groups". Using
dynamics, however, we find greater scatter in baryonic collapse
efficiencies, likely indicating variation in group hot-to-cold baryon
ratios. Similarly, we see higher scatter in baryonic collapse
efficiencies in the SAM when using its true groups and their group
halo masses as opposed to friends-of-friends groups and HAM masses.
Description:
In this work, we use two data sets, the REsolved Spectroscopy of a
Local VolumE survey (RESOLVE; S. J. Kannappan et al. 2017, in
preparation) and the Environmental COntext catalog (ECO; Moffett+
2015, J/ApJ/812/89).
The RESOLVE survey covers a >50000Mpc3 volume over two equatorial
strips ranging in redshift from 4500 to 7000km/s. The ∼13700Mpc3
RESOLVE-B footprint coincides with SDSS Stripe 82. The RESOLVE-B
volume contains 486 galaxies brighter than the apparent magnitude
limit of 17.77 and 344 groups, 286 of which have N=1 member.
The ECO catalog covers a volume of ∼442700Mpc3, which is ∼32 times
larger than RESOLVE-B. ECO provides 9443 galaxies brighter than the
luminosity limit of -17.33 and 6746 groups, of which 5723 are groups
of N=1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
eco.dat 106 9443 ECO group catalog; updated from erratum
published in 2021 ApJ, 920, 160
resolve.dat 106 486 RESOLVE group catalog
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See also:
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/ApJS/167/1 : Galaxy groups and clusters from SDSS (Berlind+, 2006)
J/AJ/142/170 : ALFALFA survey: α.40 HI source catalog (Haynes+, 2011)
J/MNRAS/436/34 : GALEX Arecibo SDSS survey. Final release (Catinella+, 2013)
J/ApJ/777/42 : Kinematic and HI data for the NFGS (Kannappan+, 2013)
J/ApJ/810/166 : RESOLVE survey photometry catalog (Eckert+, 2015)
J/ApJ/812/89 : Environmental COntext (ECO) catalog (Moffett+, 2015)
J/ApJ/824/124 : Galaxy stellar and baryonic mass functions (Eckert+, 2016)
J/ApJ/832/126 : RESOLVE survey: 21cm obs. with GBT & Arecibo (Stark+, 2016)
Byte-by-byte Description of file: eco.dat resolve.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- ID RESOLVE or ECO galaxy identifier
10- 13 I4 --- Grp [1/9180] Group identifier
15- 17 I3 --- N [1/245] Number of Group members
19- 29 F11.7 deg RAdeg Right Ascension of Grp (J2000)
31- 41 F11.8 deg DEdeg Declination of Grp (J2000)
43- 49 F7.2 km/s Grpcz [3000/7000] cz of Grp
51- 55 F5.2 [Msun] logMhLr [10.8/14.6] Log group halo mass of Grp using
halo abundance matching based on
group luminosity
57- 61 F5.2 [Msun] logMhMs [10.8/14.6] Log group halo mass of Grp using
halo abundance matching based on
logGrpMs
63- 67 F5.2 [Msun] logMhdyn [0/14.9] Log group halo mass of Grp using
dynamics (1)
69- 73 F5.2 [Msun] logMhdynSk [0/13.6] Log group halo mass of Grp using
dynamics with stacked groups (1)
75- 79 F5.2 [Msun] logMhdynH [10.4/15] Log group halo mass of Grp "hybrid"
described in Section 2.3.5
81- 85 F5.2 [Msun] logGrpMs [6.4/12.8] Log group-integrated stellar mass
of Grp
87- 91 F5.2 [Msun] logGrpMb [8.5/12.8] Log group-integrated cold baryonic
mass of Grp
93- 93 I1 --- FC [0/1] 1: Central; or 0:satellite
95-100 F6.2 km/s Grpsigma [0/623.7] Velocity dispersion of group using
Gapper method (1)
102-106 F5.3 Mpc GrpRproj [0/0.9] Projected radius of group (1)
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Note (1): Only provided for groups with N>2 members. If N=1 or =2,
a value of 0.0 is given.
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History:
From electronic version of the journal
26-Sep-2018:Insert into VizieR
18-nov-2021: Table eco updated from erratum published in 2021 ApJ, 920, 160
(issue with "FC" column)
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Jun-2018