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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 (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:
FileName Lrecl Records Explanations
ReadMe 80 . This file eco.dat 106 9443 ECO group catalog resolve.dat 106 486 RESOLVE group catalog
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
Bytes Format Units Label Explanations
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 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)
Note (1): Only provided for groups with N>2 members. If N=1 or =2, a value of 0.0 is given.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Jun-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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