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#                                                                              #
#     The GALEX Arecibo SDSS Survey - I. Gas Fraction Scaling Relations of     #
#                  Massive Galaxies and First Data Release                     #
#                                                                              #
#                  Catinella et al 2010, MNRAS 403, 683-708                    #
#                                                                              #
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Description of Tables 1-3:


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Table 1.   SDSS and UV parameters of the GASS galaxies.
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GASS     = GASS identifier.
SDSS     = SDSS identifier.
zSDSS	 = SDSS redshift.
LogMst   = base-10 logarithm of stellar mass, in solar units.
petrR50z = radius containing 50% of the Petrosian flux in z band, in arcsec.
petrR50r = radius containing 50% of the Petrosian flux in r band, in arcsec.
petrR90r = radius containing 90% of the Petrosian flux in r band, in arcsec.
Logmust  = base-10 logarithm of stellar mass surface density, in Msun/kpc^2
ext_r  	 = Galactic extinction in r band, in magnitudes.
r_c      = r band model magnitude from SDSS, corrected for Galactic extinction.
NUV-r    = NUV-r observed colour from our reprocessed photometry, corrected 
	   for Galactic extinction only.
T_NUV  	 = exposure time of GALEX NUV image, in seconds.
Tmax	 = maximum on-source integration time required to reach the limiting 
	   HI mass fraction, in minutes.



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Table 2.   HI properties of GASS detections.
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GASS     = GASS identifier.
SDSS     = SDSS identifier.
zSDSS	 = SDSS redshift. 
Ton	 = on-source integration time of the Arecibo observation, in minutes.
dv	 = velocity resolution of the final, smoothed spectrum in km/s.
z	 = redshift measured from the HI spectrum. The error on the corresponding 
	   heliocentric velocity, cz, is half the error on the width, tabulated 
	   in the following column.
W50   	 = observed velocity width of the source line profile in km/s, measured at 
	   the 50% level of each peak. 
Werr	 = error on  W50, in km/s. The error on the width is the sum in quadrature 
	   of the statistical and systematic uncertainties in km/s [see paper for details].
W50cor   = velocity width corrected for instrumental broadening and cosmological redshift
	   only, in \kms. No inclination or turbulent motion corrections are applied.
Sobs     = observed, integrated HI-line flux density in Jy km/s, measured on the smoothed 
	   and baseline-subtracted spectrum.
Serr   	 = error on  Sobs, in Jy km/s. The reported uncertainty is the sum in quadrature 
	   of the statistical and systematic errors [see paper for details].
rms    	 = rms noise of the observation in mJy, measured on the signal- and RFI-free 
	   portion of the smoothed spectrum.
S/N  	 = signal-to-noise ratio of the HI spectrum, estimated following Saintonge (2007) 
	   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.
LogMHI   = base-10 logarithm of the HI mass, in solar units.
LogGF  	 = base-10 logarithm of the HI mass fraction, MHI/Mst.
Q	 = quality flag, Q (1=good, 2=marginal, 5=confused). An asterisk indicates the 
	   presence of a note for the source in the Appendix of the paper.
	   We assigned code 3 only to GASS 9463, which is both marginal and confused.
	   


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Table 3.   GASS non-detections.  
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GASS     = GASS identifier.
SDSS     = SDSS identifier.
zSDSS	 = SDSS redshift. 
Ton	 = on-source integration time of the Arecibo observation, in minutes.
dv	 = velocity resolution of the final, smoothed spectrum in km/s.
rms    	 = rms noise of the observation in mJy, measured on the signal- and RFI-free 
	   portion of the smoothed spectrum.
LogMHIlim= base-10 logarithm of the upper limit on the HI mass, in solar units.
	   The upper limit is computed assuming a 5 sigma signal with 300 km/s
	   velocity width, if the spectrum was smoothed to 150 km/s.
LogGF  	 = base-10 logarithm of the upper limit on the HI mass fraction, MHI/Mst.
Note	 = an asterisk indicates the presence of a note for the galaxy in the Appendix
	   of the paper.