J/ApJ/832/126 RESOLVE survey: 21cm obs. with GBT & Arecibo (Stark+, 2016)
The RESOLVE survey atomic gas census and environmental influences on galaxy gas reservoirs. Stark D.V., Kannappan S.J., Eckert K.D., Florez J., Hall K.R., Watson L.C., Hoversten E.A., Burchett J.N., Guynn D.T., Baker A.D., Moffett A.J., Berlind A.A., Norris M.A., Haynes M.P., Giovanelli R., Leroy A.K., Pisano D.J., Wei L.H., Gonzalez R.E., Calderon V.F. <Astrophys. J., 832, 126-126 (2016)> =2016ApJ...832..126S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Stars, masses ; Surveys ; Radio lines Keywords: galaxies: evolution; galaxies: ISM Abstract: We present the HI mass inventory for the REsolved Spectroscopy Of a Local VolumE (RESOLVE) survey, a volume-limited, multi-wavelength census of >1500 z=0 galaxies spanning diverse environments and complete in baryonic mass down to dwarfs of ∼109M☉. This first 21cm data release provides robust detections or strong upper limits (1.4MHI<5%-10% of stellar mass M*) for ∼94% of RESOLVE. We examine global atomic gas-to-stellar mass ratios (G/S) in relation to galaxy environment using several metrics: group dark matter halo mass Mh, central/satellite designation, relative mass density of the cosmic web, and distance to the nearest massive group. We find that at fixed M*, satellites have decreasing G/S with increasing Mh starting clearly at Mh∼1012M☉, suggesting the presence of starvation and/or stripping mechanisms associated with halo gas heating in intermediate-mass groups. The analogous relationship for centrals is uncertain because halo abundance matching builds in relationships between central G/S, stellar mass, and halo mass, which depend on the integrated group property used as a proxy for halo mass (stellar or baryonic mass). On larger scales G/S trends are less sensitive to the abundance matching method. At fixed Mh≤1012M☉, the fraction of gas-poor centrals increases with large-scale structure density. In overdense regions, we identify a rare population of gas-poor centrals in low-mass (Mh<1011.4M☉) halos primarily located within ∼1.5x the virial radius of more massive (Mh>1012M☉) halos, suggesting that gas stripping and/or starvation may be induced by interactions with larger halos or the surrounding cosmic web. We find that the detailed relationship between G/S and environment varies when we examine different subvolumes of RESOLVE independently, which we suggest may be a signature of assembly bias. Description: The REsolved Spectroscopy Of a Local VolumE (RESOLVE) survey is a volume-limited census of galaxies in the local universe with the goal of accounting for baryonic and dark matter mass within a statistically complete subset of the z=0 galaxy population. A complete description of the survey design will be presented in S. J. Kannappan et al. (2016, in preparation). This paper presents new 21cm observations, but an optical spectroscopic survey is under way, primarily with the SOAR 4.1m telescope, and also using SALT, Gemini, and the AAT. The blindly detected 21cm sources in the standard ALFALFA catalog (Giovanelli+ 2005AJ....130.2598G) are cross-matched with RESOLVE using a match radius of 2', corresponding to the spatial resolution of the final ALFALFA data cubes. Additionally, we search the ALFALFA data cubes at the positions of all galaxies that lack counterparts within the standard ALFALFA catalogs. To complete the RESOLVE HI census, new 21cm observations were carried out with the Robert C. Byrd New Green Bank Telescope (GBT, programs 11B-056, 13A-276, 13B-246, 14A-441) and Arecibo Observatory (programs a2671, a2812, a2852). GBT data were acquired over a total of 738hr between 2011 August and 2014 July. Arecibo data were acquired over a total of 554hr in 2012 March and again between 2013 July and 2016 May. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 74 2164 REsolved Spectroscopy Of a Local VolumE (RESOLVE) 21cm catalog; from erratum published in 2017, ApJ, 851, 153 table2.dat 70 1384 RESOLVE environment metrics
See also: V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012) VII/259 : 6dF galaxy survey final redshift release (Jones+, 2009) VIII/77 : HI spectral properties of galaxies (Springob+, 2005) VII/250 : The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003) J/ApJ/824/124 : Galaxy stellar and baryonic mass functions (Eckert+, 2016) J/A+A/596/A14 : Group catalogues of the local universe (Saulder+, 2016) J/ApJS/223/20 : SDSS-DR8 galaxies classified by WND-CHARM (Kuminski+, 2016) J/ApJ/812/89 : Environmental COntext (ECO) catalog (Moffett+, 2015) J/ApJ/810/166 : RESOLVE survey photometry catalog (Eckert+, 2015) 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/776/71 : ZENS: gal. in groups along the cosmic web. I (Carollo+, 2013) J/ApJ/769/82 : H2 masses in a broad sample of galaxies (Stark+, 2013) J/AJ/144/16 : Optical & HI properties of galaxies in voids (Kreckel+, 2012) J/AJ/142/170 : ALFALFA survey: α.40 HI source catalog (Haynes+, 2011) J/ApJ/733/74 : GALEX - SDSS properties of local galaxies (Lemonias+, 2011) J/MNRAS/413/971 : Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011) J/ApJS/167/1 : Galaxy groups and clusters from SDSS (Berlind+, 2006) J/A+A/417/421 : WSRT wide-field HI survey. II. (Braun+, 2004) J/AJ/119/32 : Survey of galaxies within nearby voids. II (Grogin+, 2000) J/AJ/117/2039 : Sc galaxies I photometry, 21cm data (Haynes+, 1999) http://resolve.astro.unc.edu/ : RESOLVE home page http://www.sdss3.org/ : SDSS-III home page Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Name RESOLVE designation (rfNNNN or rsNNNN) 8- 16 F9.5 deg RAdeg Galaxy Right Ascension (J2000) 18- 25 F8.5 deg DEdeg Galaxy Declination (J2000) 27- 35 A9 --- Tel Telescope used for observation (1) 37- 41 F5.2 Jy.km/s F21 [0.01/17.5] Total 21cm flux 43- 46 F4.2 Jy.km/s e_F21 [0.01/9]?=0 Uncertainty on F21 48- 51 F4.2 mJy rms [0.1/8.4] RMS noise of spectrum assuming 10km/s channels 53 I1 --- Lim Flag indicating upper limit on F21 (1=upper limit; 692 instances) 55 I1 --- Conf Flag indicating 21cm emission likely confused (1=confused; 251 instances) 57- 61 F5.2 Jy.km/s F21c [0.01/12.3]?=0 Total 21cm flux after correction for confusion 63- 66 F4.2 Jy.km/s e_F21c [0.01/0.4]?=0 Statistical uncertainty on total 21cm flux after correction for confusion 68- 72 F5.2 Jy.km/s s_F21c [0.01/11]?=0 Additional systematic uncertainty on total 21cm flux after correction for confusion 74 I1 --- Mode [0/3]? Method used to correct 21cm flux for confusion and determine the additional systematic uncertainty (2)
Note (1): Telescope used for observation as follows: GBT = Green Bank 100m (373 instances); AO = Arecibo 300m (365 instances); ALFALFA = Arecibo Legacy Fast ALFA Survey (Arecibo 300m; 1408 instances); S05-AO = Springob+ (2005, VIII/77) catalog (Arecibo 300m). S05-GB300 = Springob+ (2005, VIII/77) catalog (Green Bank 300ft) Note (2): Method used as follows: 0 = No correction (flag indicating confusion = 0; 1913 instances). 1 = The corrected flux, Fc, is determined by summing the channels within the predicted W50. The statistical uncertainty, σFc,stat, is calculated following Equation (1): σF=σrmsΔV(Nch)0.5 where σrms is the rms noise of the spectrum measured over a signal-free region, ΔV is the velocity resolution in km/s, and Nch is the number of channels in the integration -- but an additional systematic uncertainty, σFc,sys, is reported equaling the total flux within any channels overlapping multiple predicted galaxy linewidths (182 instances). 2 = If one half of the primary target's 21cm profile is judged to be uncontaminated, the flux is measured within the unconfused half and doubled to yield an estimate of Fc. A 20% systematic error is assigned to account for possible asymmetry in the 21cm profile (49 instances). 3 = If one half of the companion galaxy's 21cm profile is judged to be uncontaminated, this unconfused side is integrated, doubled, and subtracted from the total flux of the blended profile to obtain Fc. A systematic uncertainty of 20% of the companion's total flux is assigned to the target galaxy, again to account for possible profile asymmetries. This method is not applicable if there are more than two potentially blended sources within the 21cm beam (20 instances). See Section 2.3.2 for further explanations.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Name RESOLVE designation (1) 8- 12 I5 --- ID-s [10001/16319]?=0 Group dark matter halo ID, stellar mass-limited sample (2) 14- 18 F5.2 [Msun] Mass-s [11/14.3]?=0 Group dark matter halo mass, log, stellar mass-limited sample 20- 24 I5 --- ID-b [20001/26603]?=0 Group dark matter halo ID, baryonic mass-limited sample (2) 26- 30 F5.2 [Msun] Mass-b [10/14.1]?=0 Group dark matter halo mass, log, baryonic mass-limited sample 32- 36 F5.2 [Msun/Mpc2] Den-s [9/14.5]?=0 Large-scale structure density, log, stellar mass-limited sample groups, uncorrected for edge-effects 38- 42 F5.2 [Msun/Mpc2] Denc-s [9.6/14.5]?=0 Large-scale structure density, log, stellar mass-limited sample groups, corrected for edge-effects 44- 48 F5.2 [Msun/Mpc2] Den-b [8/14.1]?=0 Large-scale structure density, log, baryonic mass-limited sample groups, uncorrected for edge-effects 50- 54 F5.2 [Msun/Mpc2] Denc-b [9.5/14.1]?=0 Large-scale structure density, log, baryonic mass-limited sample groups, corrected for edge-effects 56- 60 F5.2 --- Dist-s [0.2/62.5]?=0 Projected distance to nearest M_h>1012 halo, stellar mass-limited sample groups (3)(4) 62 I1 --- f_Dist-s Reliability Flag for dist-s (5) 64- 68 F5.2 --- Dist-b [0.03/63.3]?=0 Projected distance to nearest M_h>1012 halo, baryonic mass-limited sample groups (4)(3) 70 I1 --- f_Dist-b Reliability Flag for dist-b (5)
Note (1): General Notes: Environment metrics are only provided for galaxies lying within our survey definitions (stellar mass >108.9M☉ or baryonic mass >109.3M☉. This table includes galaxies that fall within the buffer regions (see S2.5) but still lie above the stellar or baryonic mass completeness limits. Note (2): By definition, all members of a group have the same values for each of the environment metrics. See section 2.5.1. Note (3): Distances to nearest halo with mass >1012M☉ and heliocentric velocity separation <500km/s are given relative to the virial radius of the nearest Mh>1012 group, e.g., if a Mh=1011M☉ halo lies at the virial radius of a Mh=1012.5M☉ halo, then Dist-s=1. Note (4): dist-s and dist-b values only calculated for Mh<1012M☉ groups. Note (5): Flag=1 indicates that the corresponding distance may be unreliable due to proximity to survey boundary.
History: From electronic version of the journal 31-Mar-2017: Insert into VizieR 05-Feb-2018: Table1 updated from erratum published in 2017, ApJ, 851, 153
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 21-Feb-2017
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