#################################################################################### # # # The extended GALEX Arecibo SDSS Survey (xGASS) # # Catinella et al. 2018 # # # # Combined Data Tables from: # # # # GASS Data Release 1: Catinella et al 2010, MNRAS 403, 683-708 # # GASS Data Release 2: Catinella et al 2012, A&A 544, A65 # # GASS Data Release 3: Catinella et al 2013, MNRAS, 436, 34 # # GASS-low Data Release: Catinella et al 2018, MNRAS, in press # # # # Date: 16 Jan 2018. Barbara Catinella # # # #################################################################################### The following tables list the HI parameters of the full xGASS sample observed with the Arecibo radio telescope as part of the GASS and GASS-low surveys: xGASS_detections.fits -- HI detections (N=499) xGASS_nondetections.fits -- HI non-detections (N=375) This is a subset of the representative sample (xGASS_representative_sample.fits), which includes gas-rich galaxies detected by ALFALFA or in the Springob et al. (2005) catalog that were not re-observed. SDSS, UV and other galaxy parameters can be found in that file. NOTES: - The galaxies in each Table are ordered by increasing R.A. - HI masses of the GASS galaxies were slightly revised (see Appendix A of xGASS paper, Catinella et al. 2018), so these files supersede previous GASS ones - See xGASS paper for more details on the quantities listed below ----------------------------------------------------------------------------------------- xGASS_detections.fits N=499, 17 cols ----------------------------------------------------------------------------------------- GASS = GASS/xGASS identifier (GASS-low if >100000) SDSS = SDSS identifier zSDSS = SDSS spectroscopic redshift Ton = on-source integration time of the Arecibo observation, in minutes dv = velocity resolution of the final, smoothed spectrum in km/s. zHI = redshift measured from the HI spectrum. The error on the corresponding heliocentric velocity, cz, is half the error on the width (Werr) 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 W50cor = velocity width corrected for instrumental broadening and cosmological redshift only, in km/s. 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 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 lgMHI = base-10 logarithm of the HI mass, in solar units lgGF = base-10 logarithm of the HI mass fraction, MHI/Mst Q = quality flag, Q (1=good, 2=marginal, 5=confused). We assigned code 3 only to a few galaxies, which are both marginal and confused. An asterisk indicates the presence of a note for the source in the Appendix of the relevant data release paper (see next column) xGASSDR = GASS Data Release (1, 2 or 3) or GASS-low (4) ----------------------------------------------------------------------------------------- ----------------------------------------------------------------------------------------- xGASS_nondetections.fits N=375, 9 cols ----------------------------------------------------------------------------------------- GASS = GASS/xGASS identifier (GASS-low if >100000) SDSS = SDSS identifier zSDSS = SDSS spectroscopic redshift Ton = on-source integration time of the Arecibo observation, in minutes rms = rms noise of the observation in mJy, measured on the signal- and RFI-free portion of the smoothed spectrum lgMHIlim = base-10 logarithm of the upper limit on the HI mass, in solar units. This is computed assuming a 5 sigma signal with a 200/300 km/s velocity width for GASS-low/GASS respectively, if the spectrum was smoothed to half width lgGF = base-10 logarithm of the upper limit on the HI mass fraction, MHIlim/Mst Note = an asterisk indicates the presence of a note for the source in the Appendix of the relevant data release paper (see next column) xGASSDR = GASS Data Release (1, 2 or 3) or GASS-low (4) -----------------------------------------------------------------------------------------