xCOLD GASS Object Viewer

ID122002GASS catalog ID
SDSSJ224110.65+132023.6SDSS name
OBJID587730773880340787SDSS ObjID
SPECOBJID208235580109094912SDSS SpecObjID
PLATEID739SDSS spectroscopic Plate ID
MJD52520SDSS spectroscopic MJD ID
FIBERID152SDSS spectroscopic Fiber ID
RA340.29RA from SDSS, J2000 [decimal degrees]
DEC13.34Dec from SDSS, J2000 [decimal degrees]
Z_SDSS0.017337SDSS spectroscopic redshift
LUMDIST75.242Luminosity distance [Mpc] (Omega_m=0.3, Omega_L = 0.7, H0 = 70 km/s/Mpc)
INCL67.638Disc inclination [degrees]
NUVR2.347NUV-r colour, corrected for Galactic extinction
R50KPC2.2657SDSS r-band Petrosian R50[kpc]
LOGMSTAR9.4657Stellar mass [log Msun]
LOGMUST8.1114Stellar mass surface density [log Msun/kpc^2] (calculated as log(mu*)=log(M*/(2*pi*r50_z^2)) )
CINDX2.3082Concentration index (ratio of r-band Petrosian R90 and R50)
WEIGHT2.1971Statistical weight
LOGSFR_MPAJHU-0.26763SFR from SDSS MPA/JHU catalog
LOGSFR_SED-0.055288SFR from UV+optical SED fitting
LOGSFR_BEST-0.31123SFR from WISE + GALEX when detected in both data sets else from SED fitting (see Janowiecki et al. 2017)
LOGSFR_ERR0.10529Error on LOGSFR_BEST
FLAG_IRAS1Detection flag in the IRAS PSC, 1:yes, 2:no
LOGLIR_IRAS9.8046Total IR luminosity [log Lsun]
IRCOL_IRAS0.23465IRAS colour (F60/F100)
N2HA-0.56702log(FLUX_NII_6583/FLUX_Halpha_6562) (using fluxes from SDSS DR7)
O3HB-0.20536log(FLUX_OIII_5006/FLUX_HBeta_4861) (using fluxes from SDSS DR7)
AGNCLASS1BPT-based AGN classification, -1:undetermined, 0:inactive, 1:SFing, 2:Composite, 3:AGN, 4:Seyfert
Z_PP04_N28.565712+logO/H from N2Ha using Pettini&Pagel (2004)
Z_PP04_O3N28.614312+logO/H from N2Ha and O3Hb using Pettini&Pagel (2004)
Z_MZR8.542512+logO/H from MZR, Kewley&Ellison08, PP04 calibration
FLAG_CO1CO(1-0) detection flag, 1:yes, 2:no
XCO7.2424Constant Galactic CO-to-H2 conversion factor except for galaxies suspected of requiring the lower “merger” value
XCO_A175.9117CO-to-H2 conversion function from Accurso et al. (2017)
XCO_A17_ERR2.246Error on XCO_A17
ICO0.594CO(1-0) line flux [K km/s]
ICO_ERR0.089802Error on ICO [K km/s]
ICO_COR0.73713CO(1-0) line flux, aperture corrected [K km/s]
ICO_COR_ERR0.15699Error on ICO_COR [K km/s]
LCO4.9463E+7CO(1-0) line luminosity [K km/s pc^2] (if FLAG_CO=2, then this is a 3sigma upper limit)
LCO_ERR9.2798E+6Error on LCO [K km/s pc^2]
LCO_COR6.1382E+7CO(1-0) line luminosity, aperture corrected [K km/s pc^2] (if FLAG_CO=2, then this is a 3sigma upper limit)
LCO_COR_ERR1.3072E+7Error on LCO_COR [K km/s pc^2]
RMS_CO0.001269Rms noise around the CO(1-0) line in 20km/s-wide channels [K]
SN_CO7.7954Integrated S/N of the CO(1-0) line
WCO167.15FWHM of the CO(1-0) line [km/s]
WCO_FLAG1Quality flag for WCO, 1:high quality, 2: acceptable, 3: poor
Z_CO0.017265Redshift based on the velocity of the CO(1-0) line
WCO_TFR161.14FWHM of the CO(1-0) for TFR work from Tiley et al. (2016) [km/s]
WCO_TFR_ERR41.631Error on WCO_TFR
LOGMH28.5597Total molecular gas mass [log Msun]
LOGMH2_ERR0.17758Error on LOGMH2
LIM_LOGMH203sigma upper limit for LOGMH2, if FLAG_CO=2
LOGMH2MS-0.90594Molecular gas mass fraction [log MH2/M*]
FLAG_CO211CO(2-1) detection flag, 1:yes, 2:no, 0:not observed
ICO210.971CO(2-1) line flux [K km/s]
ICO21_ERR0.21808Error on ICO21 [K km/s]
LCO212.5443E+7CO(2-1) line luminosity [K km/s pc^2] (if FLAG_CO21=2, then this is a 3sigma upper limit)
LCO21_ERR5.7141E+6Error on LCO21 [K km/s pc^2]
RMS_CO210.001477Rms noise around the CO(2-1) line in 20km/s-wide channels [K]
SN_CO219.7867Integrated S/N of the CO(2-1) line
WCO21209.2FWHM of the CO(2-1) line [km/s]
WCO21_FLAG1Quality flag for WCO21, 1:high quality, 2: acceptable, 3: poor
Z_CO210.01731Redshift based on the velocity of the CO(2-1) line
FLAG_APEX1CO(2-1) detection flag, 1:yes, 2:no, 0:not observed
ICO_APEX0.554CO(2-1) line flux [K km/s]
LCO_APEX7.3520E+7CO(2-1) line luminosity [K km/s pc^2]
RMS_APEX0.001513Rms noise around the CO(2-1) line in 20km/s-wide channels [K]
SN_APEX6.7538Integrated S/N of the CO(2-1) line
WCO_APEX142.89FWHM of the CO(2-1) line [km/s]
ZCO_APEX0.017455Redshift based on the velocity of the CO(2-1) line