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 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 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:
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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
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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
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Bytes Format Units Label Explanations
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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- 53 I1 --- Lim Flag indicating upper limit on F21
(1=upper limit; 692 instances)
55- 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- 74 I1 --- Mode [0/3]? Method used to correct 21cm flux for
confusion and determine the additional
systematic uncertainty (2)
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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.
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Byte-by-byte Description of file: table2.dat
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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- 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- 70 I1 --- f_Dist-b Reliability Flag for dist-b (5)
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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.
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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