J/MNRAS/436/34 GALEX Arecibo SDSS survey. Final data release (Catinella+, 2013)
The GALEX Arecibo SDSS survey.
VIII. Final data release. The effect of group environment on the gas content
of massive galaxies.
Catinella B., Schiminovich D., Cortese L., Fabello S., Hummels C.B.,
Moran S.M., Lemonias J.J., Cooper A.P., Wu R., Heckman T.M., Wang J.
<Mon. Not. R. Astron. Soc., 436, 34-70 (2013)>
=2013MNRAS.436...34C 2013MNRAS.436...34C
ADC_Keywords: Surveys ; Ultraviolet ; Galaxies, photometry ; Morphology
Keywords: galaxies: evolution - galaxies: fundamental parameters -
radio lines: galaxies - ultraviolet: galaxies
Abstract:
We present the final data release from the GALEX Arecibo SDSS Survey
(GASS), a large Arecibo programme that measured the HI properties for
an unbiased sample of ∼800 galaxies with stellar masses greater than
1010M☉ and redshifts 0.025<z<0.05. This release includes new
Arecibo observations for 250 galaxies. We use the full GASS sample to
investigate environmental effects on the cold gas content of massive
galaxies at fixed stellar mass. The environment is characterized in
terms of dark matter halo mass, obtained by cross-matching our sample
with the Sloan Digital Sky Survey (SDSS) group catalogue of Yang et
al. Our analysis provides, for the first time, clear statistical
evidence that massive galaxies located in haloes with masses of
1013-1014M☉ have at least 0.4dex less HI than objects in
lower density environments. The process responsible for the
suppression of gas in group galaxies most likely drives the observed
quenching of the star formation in these systems. Our findings
strongly support the importance of the group environment for galaxy
evolution, and have profound implications for semi-analytic models of
galaxy formation, which currently do not allow for stripping of the
cold interstellar medium in galaxy groups.
Description:
Survey design, sample selection, Arecibo observations and data
reduction are described in detail in our first two data release papers
(DR1 and Catinella et al. 2012A&A...544A..65C 2012A&A...544A..65C, hereafter DR2).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 111 250 SDSS and UV parameters
tablea2.dat 93 147 HI properties of GASS detections
tablea3.dat 53 103 GASS non-detections
notes.dat 80 420 Individual notes
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See also:
J/MNRAS/403/683 : GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- GASS [3157/56662] GASS identification number
7- 25 A19 --- SDSS SDSS designation (JHHMMSS.ss+DDMMSS.s)
27- 38 A12 --- OName Other name
41- 46 F6.4 --- zSDSS SDSS redshift (typical uncertainty is 0.0002)
48- 52 F5.2 [Msun] logM* Stellar mass (1)
54- 58 F5.2 arcsec R50z Radius containing 50% of the Petrosian flux
in z band
60- 64 F5.2 arcsec R50 Radius containing 50% of the Petrosian flux
in r band
66- 70 F5.2 arcsec R90 Radius containing 90% of the Petrosian flux
in r band
72- 75 F4.2 [Msun/kpc2] logmu* Stellar mass surface density (2)
77- 80 F4.2 mag rext Galactic extinction in r band, from SDSS
82- 86 F5.2 mag rmag r-band model magnitude from SDSS, corrected
for Galactic extinction
88- 92 F5.3 --- (b/a)r [0/1] Minor-to-major axial ratio from the
exponential fit in r band, from SDSS
94- 95 I2 deg i [0/90] Inclination to the line-of-sight (3)
97-100 F4.2 mag NUV-r ?=- NUV-r observed colour index from our
reprocessed photometry, corrected for
Galactic extinction
102-107 I6 s TNUV ?=- GALEX NUV image exposure time
109-111 I3 min Tmax Maximum on-source integration time required
to reach the limiting HI mass fraction (4)
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Note (1): Stellar masses are derived from SDSS photometry using the methodology
described in Salim et al. (2007ApJS..173..267S 2007ApJS..173..267S) (a Chabrier 2003PASP..115..763C 2003PASP..115..763C
initial mass function is assumed). Over our required stellar mass range, these
values are believed to be accurate to better than 30%.
Note (2): This quantity is defined as mu*=Ms(2πR50,z2),
with R50,z in kpc units.
Note (3): see Catinella et al. (2012A&A...544A..65C 2012A&A...544A..65C, Cat. J/A+A/544/A65)
for details.
Note (4): see Section 2. Given the HI mass limit and redshift of each galaxy,
Tmax is computed assuming a 5σ signal with 300km/s velocity width and
the instrumental parameters typical of our observations (i.e. gain ∼10K/Jy
and system temperature ∼28K at 1370MHz).
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- GASS [3157/56662] GASS identification number
7- 25 A19 --- SDSS SDSS designation (JHHMMSS.ss+DDMMSS.s)
27- 32 F6.4 --- zSDSS SDSS redshift (typical uncertainty is 0.0002)
34- 35 I2 min Ton On-source integration time of the Arecibo
observation (G1)
37- 38 I2 km/s Dv [5/21] Velocity resolution of the final,
smoothed spectrum
40- 47 F8.6 --- z [0.02/0.05] Redshift from the HI spectrum (1)
49- 51 I3 km/s W50 Observed velocity width of the source line
profile measured at the 50% level of each
peak (2)
53- 54 I2 km/s e_W50 rms uncertainty on W50
56- 58 I3 km/s W50c Velocity width corrected for instrumental
broadening and cosmological redshift only (3)
60- 63 F4.2 Jy.km/s FHI Observed, integrated HI-line flux density (4)
65- 68 F4.2 Jy.km/s e_FHI rms uncertainty on FHI
70- 73 F4.2 mJy rms rms noise of the observation measured on the
signal- and RFI-free portion of the
smoothed spectrum
75- 78 F4.1 --- S/N Signal-to-noise ratio of the HI spectrum (5)
80- 84 F5.2 [Msun] logMHI Neutral hydrogen (HI) mass (6)
86- 90 F5.2 [-] logMHI/* [-2.3/0.11] HI mass fraction
92 I1 --- Q [1/5] Quality flag, 1=best (7)
93 A1 --- n_GASS [*] * indicates a note in notes.dat file
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Note (1): The error on the corresponding heliocentric velocity, cz,
is half the error on the width W50.
Note (2): The error on the width is the sum in quadrature of the statistical
and systematic uncertainties in km/s. Statistical errors depend primarily on
the signal to noise of the HI spectrum, and are obtained from the rms noise
of the linear fits to the edges of the HI profile. Systematic errors depend
on the subjective choice of the HI signal boundaries (see DR1 paper), and
are negligible for most of the galaxies in our sample (see also Appendix B).
Note (3): see Catinella et al. (2012A&A...544A..65C 2012A&A...544A..65C, Cat. J/A+A/544/A65) for
details. No inclination or turbulent motion corrections are applied.
Note (4): FHI=∫Sdv, measured on the smoothed and baseline-subtracted
spectrum. The reported uncertainty is the sum in quadrature of the
statistical and systematic errors (see column e_W50). The statistical
errors are calculated according to equation 2 of Springob et al.
(2005ApJS..160..149S 2005ApJS..160..149S, Cat. VIII/77) (which includes the contribution from
uncertainties in the baseline fit).
Note (5): estimated following Saintonge (2007AJ....133.2087S 2007AJ....133.2087S) and adapted to the
velocity resolution of the spectrum. This is the definition of S/N adopted by
ALFALFA, which accounts for the fact that for the same peak flux a broader
spectrum has more signal.
Note (6): see Catinella et al. 2012 (J/A+A/544/A65) for details.
Note (7): Quality flag means:
1 = good
2 = marginal
3 = marginal and confused
5 = confused
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- GASS [3157/56662] GASS identification number
7- 25 A19 --- SDSS SDSS designation (JHHMMSS.ss+DDMMSS.s)
27- 32 F6.4 --- zSDSS SDSS redshift (typical uncertainty is 0.0002)
34- 35 I2 min Ton On-source integration time of the Arecibo
observation (G1)
37- 40 F4.2 mJy rms rms noise of the observation measured on the
signal- and RFI-free portion of the
smoothed spectrum
42- 45 F4.2 [Msun] logMHI Upper limit on the HI mass (1)
47- 51 F5.2 [-] logMHI/* Upper limit on the gas fraction
53 A1 --- n_GASS [*] * indicates a note in notes.dat file
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Note (1): computed assuming a 5σ signal with 300km/s velocity width,
if the spectrum was smoothed to 150km/s.
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Byte-by-byte Description of file: notes.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- GASS GASS identification number
7- 80 A74 --- Note Text of the note
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Global notes:
Note (G1): This number refers to on scans that were actually combined, and does
not account for possible losses due to RFI excision (usually negligible).
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History:
From electronic version of the journal
References:
Catinella et al., 2010MNRAS.403..683C 2010MNRAS.403..683C Paper I, Cat. J/MNRAS/403/683
Schiminovich et al., 2010MNRAS.408..919S 2010MNRAS.408..919S Paper II
Wang et al., 2011MNRAS.412.1081W 2011MNRAS.412.1081W Paper III
Moran et al., 2012ApJ...745...66M 2012ApJ...745...66M Paper V
Catinella et al., 2012MNRAS.420.1959C 2012MNRAS.420.1959C Paper IV
Catinella et al., 2012A&A...544A..65C 2012A&A...544A..65C Paper VI
Lemonias et al., 2013ApJ...776...74L 2013ApJ...776...74L Paper VII
(End) Patricia Vannier [CDS] 20-Oct-2014