xCOLD GASS Object Viewer

ID109050GASS catalog ID
SDSSJ095836.22+131519.0SDSS name
OBJID587735349633941553SDSS ObjID
SPECOBJID491120230253199360SDSS SpecObjID
PLATEID1744SDSS spectroscopic Plate ID
MJD53055SDSS spectroscopic MJD ID
FIBERID329SDSS spectroscopic Fiber ID
RA149.65RA from SDSS, J2000 [decimal degrees]
DEC13.255Dec from SDSS, J2000 [decimal degrees]
Z_SDSS0.011662SDSS spectroscopic redshift
LUMDIST50.395Luminosity distance [Mpc] (Omega_m=0.3, Omega_L = 0.7, H0 = 70 km/s/Mpc)
INCL37.22Disc inclination [degrees]
NUVR2.2758NUV-r colour, corrected for Galactic extinction
R50KPC1.2153SDSS r-band Petrosian R50[kpc]
LOGMSTAR9.2626Stellar mass [log Msun]
LOGMUST8.3061Stellar mass surface density [log Msun/kpc^2] (calculated as log(mu*)=log(M*/(2*pi*r50_z^2)) )
CINDX2.9833Concentration index (ratio of r-band Petrosian R90 and R50)
WEIGHT2.9851Statistical weight
LOGSFR_MPAJHU-0.26498SFR from SDSS MPA/JHU catalog
LOGSFR_SED-0.38821SFR from UV+optical SED fitting
LOGSFR_BEST-0.45927SFR from WISE + GALEX when detected in both data sets else from SED fitting (see Janowiecki et al. 2017)
LOGSFR_ERR0.1226Error on LOGSFR_BEST
FLAG_IRAS1Detection flag in the IRAS PSC, 1:yes, 2:no
LOGLIR_IRAS9.2842Total IR luminosity [log Lsun]
IRCOL_IRAS0.61592IRAS colour (F60/F100)
N2HA-0.75282log(FLUX_NII_6583/FLUX_Halpha_6562) (using fluxes from SDSS DR7)
O3HB0.18518log(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_N28.419312+logO/H from N2Ha using Pettini&Pagel (2004)
Z_PP04_O3N28.429812+logO/H from N2Ha and O3Hb using Pettini&Pagel (2004)
Z_MZR8.479712+logO/H from MZR, Kewley&Ellison08, PP04 calibration
FLAG_CO1CO(1-0) detection flag, 1:yes, 2:no
XCO12.42Constant Galactic CO-to-H2 conversion factor except for galaxies suspected of requiring the lower “merger” value
XCO_A1711.779CO-to-H2 conversion function from Accurso et al. (2017)
XCO_A17_ERR4.4751Error on XCO_A17
ICO0.351CO(1-0) line flux [K km/s]
ICO_ERR0.061844Error on ICO [K km/s]
ICO_COR0.43206CO(1-0) line flux, aperture corrected [K km/s]
ICO_COR_ERR0.099977Error on ICO_COR [K km/s]
LCO1.3185E+7CO(1-0) line luminosity [K km/s pc^2] (if FLAG_CO=2, then this is a 3sigma upper limit)
LCO_ERR2.8597E+6Error on LCO [K km/s pc^2]
LCO_COR1.6230E+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_ERR3.7556E+6Error on LCO_COR [K km/s pc^2]
RMS_CO0.001447Rms noise around the CO(1-0) line in 20km/s-wide channels [K]
SN_CO6.37Integrated S/N of the CO(1-0) line
WCO67.228FWHM of the CO(1-0) line [km/s]
WCO_FLAG1Quality flag for WCO, 1:high quality, 2: acceptable, 3: poor
Z_CO0.011662Redshift based on the velocity of the CO(1-0) line
WCO_TFR8.3673FWHM of the CO(1-0) for TFR work from Tiley et al. (2016) [km/s]
WCO_TFR_ERR4.2152Error on WCO_TFR
LOGMH28.2814Total molecular gas mass [log Msun]
LOGMH2_ERR0.18188Error on LOGMH2
LIM_LOGMH203sigma upper limit for LOGMH2, if FLAG_CO=2
LOGMH2MS-0.98114Molecular gas mass fraction [log MH2/M*]
FLAG_CO211CO(2-1) detection flag, 1:yes, 2:no, 0:not observed
ICO210.672CO(2-1) line flux [K km/s]
ICO21_ERR0.14747Error on ICO21 [K km/s]
LCO217.9432E+6CO(2-1) line luminosity [K km/s pc^2] (if FLAG_CO21=2, then this is a 3sigma upper limit)
LCO21_ERR1.7431E+6Error on LCO21 [K km/s pc^2]
RMS_CO210.001786Rms noise around the CO(2-1) line in 20km/s-wide channels [K]
SN_CO2111.072Integrated S/N of the CO(2-1) line
WCO2153.541FWHM of the CO(2-1) line [km/s]
WCO21_FLAG1Quality flag for WCO21, 1:high quality, 2: acceptable, 3: poor
Z_CO210.011645Redshift based on the velocity of the CO(2-1) line
FLAG_APEX1CO(2-1) detection flag, 1:yes, 2:no, 0:not observed
ICO_APEX0.312CO(2-1) line flux [K km/s]
LCO_APEX1.8678E+7CO(2-1) line luminosity [K km/s pc^2]
RMS_APEX0.001251Rms noise around the CO(2-1) line in 20km/s-wide channels [K]
SN_APEX6.7515Integrated S/N of the CO(2-1) line
WCO_APEX66.337FWHM of the CO(2-1) line [km/s]
ZCO_APEX0.011692Redshift based on the velocity of the CO(2-1) line