J/A+A/544/A65 GALEX Arecibo SDSS survey. VI. (Catinella+, 2012)
The GALEX Arecibo SDSS survey.
VI. Second data release and updated gas fraction scaling relations.
Catinella B., Schiminovich D., Kauffmann G., Fabello S., Hummels C.,
Lemonias J., Moran S.M., Wu R., Cooper A., Wang J.
<Astron. Astrophys., 544, A65 (2012)>
=2012A&A...544A..65C 2012A&A...544A..65C
ADC_Keywords: Galaxy catalogs; Ultraviolet; H I data
Keywords: galaxies: fundamental parameters - ultraviolet: galaxies -
radio lines: galaxies - surveys - catalogs
Abstract:
We present the second data release from the GALEX Arecibo SDSS Survey
(GASS), an ongoing large Arecibo program to measure the HI properties
for an unbiased sample of ∼1000 galaxies with stellar masses greater
than 1010M☉ and redshifts 0.025<z<0.05. GASS targets are
selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and
Galaxy Evolution Explorer (GALEX) imaging surveys, and are observed
until detected or until a gas mass fraction limit of a few per cent is
reached. This second data installment includes new Arecibo
observations of 240 galaxies, and marks the 50% of the complete
survey. We present catalogs of the HI, optical and ultraviolet
parameters for these galaxies, and their HI-line profiles. Having more
than doubled the size of the sample since the first data release, we
also revisit the main scaling relations of the HI mass fraction with
galaxy stellar mass, stellar mass surface density, concentration
index, and NUV-r color, as well as the gas fraction plane introduced
in our earlier work.
Description:
GASS observations started in March 2008 and are expected to be
completed in 2012. Together with the first data release (DR1,
Paper I, Catinella et al., Cat. J/MNRAS/403/683), the data published
in this paper amount to ∼50% of the final survey sample, and were
obtained by the end of February 2011, with a total allocation of 572h
of telescope time (of which ∼13% unusable due to radio frequency
interference [RFI] or other technical problems).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 110 240 SDSS and UV parameters of the GASS galaxies
tablea2.dat 93 133 HI properties of GASS detections
tablea3.dat 53 107 GASS non-detections
notes.dat 80 321 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 GASS number
7- 25 A19 --- SDSS SDSS designation (JHHMMSS.ss+DDMMSS.s)
27- 40 A14 --- OName Other name (1)
42- 47 F6.4 --- z SDSS redshift (G2)
49- 53 F5.2 [Msun] logM* Stellar mass (3)
55- 58 F4.2 arcsec R50z Radius containing 50% of the Petrosian flux
in z-band
60- 64 F5.2 arcsec R50r Radius containing 50% of the Petrosian flux
in r-band
66- 70 F5.2 arcsec R90r Radius containing 90% of the Petrosian flux
in r-band
72- 75 F4.2 [Msun/kpc2] logmu* Stellar mass surface density (4)
77- 80 F4.2 mag extr 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 Minor-to-major axis ratio the exponential
fit in r band, from SDSS
94- 95 I2 deg i Inclination to the line-of-sight
97-100 F4.2 mag NUVr ?=- NUV-r observed colour index from our
reprocessed photometry, corrected for
Galactic extinction
102-106 I5 s tNUV ?=- Integration time of GALEX NUV image
108-110 I3 min tmax Maximum on-source integration time required
to reach the limiting HI mass fraction (5)
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Note (1): UGC (Nilson 1973, Cat. VII/26), NGC (Dreyer 1888, Cat. VII/118)
or IC (Dreyer 1895, 1908, Cat. VII/118) designation, or other name,
typically from the Catalog of Galaxies and Clusters of Galaxies (CGCG;
Zwicky et al. 1961, Cat. VII/49), or the Virgo Cluster Catalog (VCC;
Binggeli et al. 1985, Cat. J/AJ/90/1681)
Note (3): 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 (4): This quantity is defined as µ*=M*/(2πR50,z2).
Note (5): 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
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1- 5 I5 --- GASS GASS number
7- 25 A19 --- SDSS SDSS designation (JHHMMSS.ss+DDMMSS.s)
27- 32 F6.4 --- zsp SDSS redshift (G2)
34- 35 I2 min ton On-source integration time of the Arecibo
observation (G1)
37- 38 I2 km/s DV Velocity resolution of the final,
smoothed spectrum
40- 47 F8.6 --- z Redshift, measured from the HI spectrum (2)
49- 51 I3 km/s W50 Observed velocity width of the source line
profile, measured at the 50% level of each
peak
53- 54 I2 km/s e_W50 rms uncertainty on W50 (3)
56- 58 I3 km/s W50c Velocity width corrected for instrumental
broadening and cosmological redshift
only (4)
60- 63 F4.2 Jy.km/s FHI Observed, integrated HI-line flux density,
measured on the smoothed and
baseline-subtracted spectrum
65- 68 F4.2 Jy.km/s e_FHI rms uncertainty on FHI (3)
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 HI mass
86- 90 F5.2 [-] logMHI/M* HI mass fraction
92 I1 --- Q [1/5] Quality flag, 1=good (6)
93 A1 --- n_GASS [*] * indicates a note in notes.dat file
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Note (2): The error on the corresponding heliocentric velocity, cz, is half
the error on the width, tabulated in e_W50 column.
Note (3): The reported uncertainty is the sum in quadrature of the
statistical and systematic uncertainties. 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 Paper I, Cat. J/MNRAS/403/683), and are negligible for
most of the galaxies in our sample (see also Appendix B).
Note (4): No inclination or turbulent motion corrections are applied.
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): Quality flag as follows:
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
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1- 5 I5 --- GASS GASS number
7- 25 A19 --- SDSS SDSS designation (JHHMMSS.ss+DDMMSS.s)
27- 32 F6.4 --- zsp SDSS redshift (G2)
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] logMHIlim Upper limit on the HI mass (1)
47- 51 F5.2 [-] logMHI/M* Upper limit on HI mass 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
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1- 5 I5 --- GASS GASS 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).
Note (G2): The typical uncertainty of SDSS redshifts for this sample is 0.0002
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History:
From electronic version of the journal
References:
Catinella et al., Paper I 2010MNRAS.403..683C 2010MNRAS.403..683C, Cat. J/MNRAS/403/683
Schiminovich et al., Paper II 2010MNRAS.408..919S 2010MNRAS.408..919S
Wang et al., Paper III 2011MNRAS.412.1081W 2011MNRAS.412.1081W
Catinella et al., Paper IV 2012MNRAS.420.1959C 2012MNRAS.420.1959C
Moran et al., Paper V 2012ApJ...745...66M 2012ApJ...745...66M
(End) Patricia Vannier [CDS] 15-Oct-2012