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(The bold columns are indexed columns)
Column NameDescriptionDatatype
clusterShort name of each cluster; matches name in cluster tableVARCHAR(n)
d4000The Dn 4000 index as defined in Balogh et al. (1999). See § 4.2.2 in survey paper.REAL
decTarget Dec coordinate in J2000 degrees. For GOGREEN, these coordinates correspond to the z′ image coordinates used for mask design. These have been transformed to align with the Ks images; however positions will not match exactly with coordinates in the photometric catalogues.REAL
delta_bicThe difference in Bayesian Information Criterion used to identify the presence of [Oii] emission (ΔBIC > 10) or its absence (ΔBIC < -10). See Old et al. (2020) for more details.REAL
ed4000The Dn 4000 index uncertaintyREAL
eewhdeltaUncertainty of ewhdeltaREAL
eewoiiUncertainty of ewoiiREAL
eewoii_modelUncertainty of ewoii_modelREAL
ef_oiiUncertainty of f_oiiREAL
esfr_oiiUncertainty of sfr_oiiREAL
ewhdeltaThe equivalent width of the H δ absorption line, in Å, using the line index definitions in Balogh et al. (1999). Positive values represent absorption. See § 4.2.2 in survey paperREAL
ewoiiThe equivalent width of the [Oii] emission line in Å, using the line index definitions in Balogh et al. (1999). Positive values represent emission. See § 4.2.2REAL
ewoii_modelThe equivalent width of the [Oii] emission line, in Å, calculated from the Gaussian fitting model described in Old et al. (2020).REAL
extverThis is the science extension number in the fits files with the 1D and 2D spectra (see §6.5 of the survey paper).SMALLINT
f_oiiThe integrated flux of the [Oii] emission line, in ergs/s/cm2/Å, calculated from the Gaussian fitting model described in Old et al. (2020).REAL
htm9HTM index (order 9 => ~10 arcmin size)INTEGER
memberA flag that identifies likely cluster members (1) or nonmembers (0). A value of -1 means membership could not be determined. For SpARCS and SPT clusters in GOGREEN, this is the maximum of the member_Clean and member_EM flags. For the five GCLASS clusters we use the membership given in Muzzin et al. (2012). Finally, for the systems in COSMOS and SXDF we define members as those within 1 Mpc and 2.5σ of the centre, as described in § 4.2.3. of the survey paperREAL
member_cleanApplicable only to the 11 SPT and SpARCS clusters in GOGREEN, this indicates likely cluster membership based on the clean algorithm of Mamon et al. (2013). A value of 1 indicates a member, 0 is a non-member, and -1 indicates membership could not be determined.REAL
member_emApplicable only to the 11 SPT and SpARCS clusters in GOGREEN, this indicates likely cluster membership based on the C.L.U.M.P.S. algorithm of Munari et al. (in prep). A value of 1 indicates a member, 0 is a non-member, and -1 indicates membership could not be determined.REAL
nest4096HEALPIX index (Nsides 4096, Nest scheme => ~52 arcsec sizeINTEGER
objclassThis has a value of 1 for GOGREEN primary targets, i.e. those that match our photometric selection criteria. A value of 3 corresponds to a GOGREEN "mask filler" object, and 4 identifies a GCLASS spectrum. (OBJClass=2 was reserved for stellar sources used for telluric correction, and these are not included in the catalogue).SMALLINT
raTarget RA coordinates in J2000 degrees. For GOGREEN, these coordinates correspond to the z′ image coordinates used for mask design. These have been transformed to align with the Ks images; however positions will not match exactly with coordinates in the photometric catalogues.REAL
random_idRandom ID in the range 0.0 => 100.0REAL
redshiftThe redshift measured from the spectrumREAL
redshift_qualityThe redshift quality flag. Both quality 3 and 4 are secure galaxy redshifts and can be used for scientific analysis; the difference between them is subjective and not rigorously defined. Quality 2 is a "best guess" but should be used with caution; this includes cases where there is plausible consistency with the photometric redshift, but no clearly identifiable spectral features. Quality 1 means no redshift is available.SMALLINT
ring256HEALPIX index (Nsides 256, Ring scheme => ~14 arcmin size)INTEGER
sfr_oiiThe star formation rate in solar masses per year, estimated from the [Oii] emission line flux and the stellar mass, using the calibration of Gilbank et al. (2010).REAL
snr_8500_rmsThe signal-to-noise ratio per pixel, measured in the range 7500 < λ < 9500Å. The noise estimate is taken from the rms in the science spectrum over the same range.REAL
snr_8500_varThe signal-to-noise ratio per pixel, measured in the range 7500 < λ < 9500Å. The noise estimate is taken from the VAR array associated with the spectrum.REAL
spec_flagInteger that identifies spectra with problems that might compromise the ability to measure a redshift or line indices of a spectrum. Flags are assigned for the following: 1: Mild slit contamination or artefacts that should not strongly affect measurements 2: Non-galaxy-like spectrum and/or image 4: Significant slit contamination from neighbouring objects. Redshift & features may be compromised. 8: Poor telluric correction or sky subtraction 16: Major artefacts or large masked regions that render the spectrum nearly useless. Flags can be added. So, for example, a flag of 12 means there is both contamination from neighbouring objects, and poor sky subtractionREAL
specidA unique identification number. The first digit identifies the origin of the spectrum: 1 for GOGREEN and 2 for GCLASS. The next two digits correspond to the cluster_id identifier in the Cluster catalogue, that specify the photometric field. The remaining digits are the galaxy ID (only unique for a given field and source).INTEGER