Schema Browser

The Schema Browser displays an extensive explanation of each type of data product each survey/archive offers, along with any relevant analysis and publication information (see also individual survey documentation for more info). For more information on the schema browser, go to the Schema Browser Documentation. For more information on the data products within the schema browser, go to the team's documentation on Data Central (the link for each survey can be found in the Meta box below).

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CATALOGUES IMAGING SPECTRA IFS TIME_SERIES_PHOTOMETRY BLOB

• GAMA

GAMA 

name: gama | type: Survey | Simon Driver [javascript protected email address] | website | docs |

GAMA is a project to exploit the latest generation of ground-based and space-borne survey facilities to study cosmology and galaxy formation and evolution.

At the heart of this project lies the GAMA spectroscopic survey of ~300,000 galaxies down to r < 19.8 mag over ~286 deg², carried out using the AAOmega multi-object spectrograph on the Anglo-Australian Telescope (AAT) by the GAMA team. This project was awarded 210 nights over 7 years (2008–2014) and the observations are now completed. This survey builds on, and is augmented by, previous spectroscopic surveys such as the Sloan Digital Sky Survey (SDSS), the 2dF Galaxy Redshift Survey(2dFGRS) and the Millennium Galaxy Catalogue (MGC).

• Data Release
• Panchromatic Data Release
• Data Release 2
• Data Release 4

Panchromatic Data Release

name: pdr | type: DataRelease | ingested: 12 Oct 2023, 4:10 p.m. | Simon Driver [javascript protected email address] | version 1.0 |

Data coming soon.

Data Release 2

name: dr2 | type: DataRelease | ingested: 12 Oct 2023, 4:10 p.m. | Simon Driver [javascript protected email address] | version 2.0 |

• Data
• Catalogues
• Spectra

• Groups
• kCorrections
• StellarMasses
• SpecLineSFR
• SpecCat
• SersicPhotometry
• LocalFlowCorrection
• InputCat
• GroupFinding
• GalexPhotometry
• ExternalSpec
• EnvironmentMeasures
• ApMatchedPhotom

kCorrections

name: kCorrections | type: CatalogueGroup | Jon Loveday [javascript protected email address] | version v02 |

read more

kCorrections
2012-09-24
Jon Loveday

This DMU provides k-corrections in the GALEX FUV and NUV bands, the
SDSS ugriz bands and the UKIDSS YJHK bands for all GAMA DR2 galaxies.
The k-corrections were calculated with kcorrect v4_2 using SDSS
DR6 model magnitudes. Please see Blanton & Roweis (2007) for further
information on kcorrect, its output and its performance. In
particular, see Section 3.4 of that paper if you plan to use the UV or
NIR k-corrections.

K-corrections are provided for both redshift 0.0 (table kcorr_z00)
and for redshift 0.1 (table kcorr_z01).

The corrections were calculated for all GAMA DR2 galaxies with
nQ >= 2 using Z_TONRY from DistancesFrames. However, they will be
meaningless for negative redshifts. Note that, strictly speaking,
geocentric redshifts should be used to calculate k-corrections, but
here we have used Tonry flow-corrected redshifts for consistency with
Vmax calculations.

The tables in this DMU also provide the coefficients of a polynomial
fit to the k-corrections in the columns PCOEFF_X_* (see Loveday et
al. (2012) for details). These coefficients are ordered high to low
order, such that
KCORR_X(z) = sum_{i=1}^5 PCOEFF_*_i * (z - zRef)^(5-i)
or for python users
KCORR_X(z) = numpy.polyval(PCOEFF_X_*, z - zRef)
where zRef = 0.0 for kcorr_z00 and zRef = 0.1 for kcorr_z01.

Note that the parameter PCOEFF_X_5 is fit for and is not kept
constant. Thus, the value of KCORR_X(zRef) provided by the polynomial
fits will in general not be equal to -2.5 log10(1+zRef), the value it
should have in principle.

In the download directory for this DMU we also provide fits binary
versions of the two tables of this DMU with columns PCOEFF_X_* and
COEFFS_* as vector columns rather than split into separate columns.

Note that columns CHI2, MASS, INTSFH, METS, B300 and B1000 are outputs
of kcorrect. These represent the physical interpretation of kcorrect's
SED fits to the photometry. However, these parameters have not been
tested at all, and this DMU does not vouch for their reliability or
meaningfulness. Hence, their scientific use is discouraged (especially
in cases where more careful measurements are provided by other
DMUs). These parameters were included here only for completeness and
because they may prove to be useful in identifying objects for which
kcorrect's SED fits are implausible.

This DMU provides k-corrections in the GALEX FUV and NUV bands, the SDSS ugriz bands and the UKIDSS YJHK bands for all GAMA DR2 galaxies.

• Tables
• kcorr_z00
• kcorr_z01

kcorr_z00

name: kcorr_z00 | type: CatalogueTable | Jon Loveday [javascript protected email address] | version v02 |

This table provides k-corrections at redshift 0.0 in the GALEX FUV and NUV bands, the SDSS ugriz bands and the UKIDSS YJHK bands for all GAMA DR2 galaxies.

Address this table as gama_dr2.kcorr_z00

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z_TONRY	-	Flow corrected redshift using Tonry et al. model	src.redshift
Z_MODEL_ERR	mag	SDSS DR6 z-band model magnitude error	stat.error;phot.mag;em.opt.I
Z_MODEL	mag	SDSS DR6 z-band model magnitude	phot.mag;em.opt.I
U_MODEL_ERR	mag	SDSS DR6 u-band model magnitude error	stat.error;phot.mag;em.opt.U
U_MODEL	mag	SDSS DR6 u-band model magnitude	phot.mag;em.opt.U
R_MODEL_ERR	mag	SDSS DR6 r-band model magnitude error	stat.error;phot.mag;em.opt.R
R_MODEL	mag	SDSS DR6 r-band model magnitude	phot.mag;em.opt.R
PCOEFF_Z_5	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_4	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_3	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_2	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_1	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Y_5	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_4	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_3	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_2	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_1	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_U_5	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_4	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_3	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_2	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_1	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_R_5	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_4	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_3	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_2	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_1	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_NUV_5	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_4	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_3	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_2	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_1	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_K_5	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_4	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_3	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_2	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_1	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_J_5	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_4	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_3	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_2	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_1	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_I_5	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_4	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_3	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_2	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_1	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_H_5	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_4	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_3	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_2	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_1	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_G_5	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_4	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_3	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_2	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_1	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_FUV_5	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_4	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_3	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_2	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_1	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
NQ	-	Redshift quality	meta.code.qual;src.redshift
METS	-	Average metallicity of currently surviving stars	phys.abund.Z
MASS	M_solar	Stellar mass of currently surviving stars	phys.mass
KCORR_Z	mag	K-correction in SDSS z band	phot.mag;em.opt.Z
KCORR_Y	mag	K-correction in UKIDSS Y band	phot.mag;em.IR.NIR
KCORR_U	mag	K-correction in SDSS u band	phot.mag;em.opt.U
KCORR_R	mag	K-correction in SDSS r band	phot.mag;em.opt.R
KCORR_NUV	mag	K-correction in GALEX NUV band	phot.mag;em.UV.200-300nm
KCORR_K	mag	K-correction in UKIDSS K band	phot.mag;em.IR.K
KCORR_J	mag	K-correction in UKIDSS J band	phot.mag;em.IR.J
KCORR_I	mag	K-correction in SDSS i band	phot.mag;em.opt.I
KCORR_H	mag	K-correction in UKIDSS H band	phot.mag;em.IR.H
KCORR_G	mag	K-correction in SDSS g band	phot.mag;em.opt.G
KCORR_FUV	mag	K-correction in GALEX FUV band	phot.mag;em.UV.100-200nm
I_MODEL_ERR	mag	SDSS DR6 i-band model magnitude error	stat.error;phot.mag;em.opt.I
I_MODEL	mag	SDSS DR6 i-band model magnitude	phot.mag;em.opt.I
INTSFH	-	Total integrated star-formation history (number of stars formed total)	meta.number
G_MODEL_ERR	mag	SDSS DR6 g-band model magnitude error	stat.error;phot.mag;em.opt.B
G_MODEL	mag	SDSS DR6 g-band model magnitude	phot.mag;em.opt.B
COEFFS_5	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_4	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_3	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_2	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_1	-	kcorrect eigenspectra coefficient	arith.factor
CHI2	-	Chi^2 of fit returned by kcorrect	stat.fit.chi2
CATAID	-	Unique GAMA ID	meta.id;meta.main
B300	-	Fraction of the total star formation that has occurred in the last 0.3 Gyr	arith.ratio
B1000	-	Fraction of the total star formation that has occurred in the last 1 Gyr	arith.ratio

kcorr_z01

name: kcorr_z01 | type: CatalogueTable | Jon Loveday [javascript protected email address] | version v02 |

This table provides k-corrections at redshift 0.1 in the GALEX FUV and NUV bands, the SDSS ugriz bands and the UKIDSS YJHK bands for all GAMA DR2 galaxies.

Address this table as gama_dr2.kcorr_z01

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z_TONRY	-	Flow corrected redshift using Tonry et al. model	src.redshift
Z_MODEL_ERR	mag	SDSS DR6 z-band model magnitude error	stat.error;phot.mag;em.opt.I
Z_MODEL	mag	SDSS DR6 z-band model magnitude	phot.mag;em.opt.I
U_MODEL_ERR	mag	SDSS DR6 u-band model magnitude error	stat.error;phot.mag;em.opt.U
U_MODEL	mag	SDSS DR6 u-band model magnitude	phot.mag;em.opt.U
R_MODEL_ERR	mag	SDSS DR6 r-band model magnitude error	stat.error;phot.mag;em.opt.R
R_MODEL	mag	SDSS DR6 r-band model magnitude	phot.mag;em.opt.R
PCOEFF_Z_5	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_4	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_3	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_2	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Z_1	-	Coefficient of polynomial fit to K(z) in SDSS z band	arith.factor
PCOEFF_Y_5	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_4	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_3	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_2	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_Y_1	-	Coefficient of polynomial fit to K(z) in UKIDSS Y band	arith.factor
PCOEFF_U_5	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_4	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_3	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_2	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_U_1	-	Coefficient of polynomial fit to K(z) in SDSS u band	arith.factor
PCOEFF_R_5	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_4	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_3	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_2	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_R_1	-	Coefficient of polynomial fit to K(z) in SDSS r band	arith.factor
PCOEFF_NUV_5	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_4	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_3	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_2	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_NUV_1	-	Coefficient of polynomial fit to K(z) in GALEX NUV band	arith.factor
PCOEFF_K_5	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_4	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_3	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_2	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_K_1	-	Coefficient of polynomial fit to K(z) in UKIDSS K band	arith.factor
PCOEFF_J_5	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_4	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_3	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_2	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_J_1	-	Coefficient of polynomial fit to K(z) in UKIDSS J band	arith.factor
PCOEFF_I_5	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_4	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_3	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_2	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_I_1	-	Coefficient of polynomial fit to K(z) in SDSS i band	arith.factor
PCOEFF_H_5	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_4	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_3	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_2	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_H_1	-	Coefficient of polynomial fit to K(z) in UKIDSS H band	arith.factor
PCOEFF_G_5	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_4	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_3	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_2	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_G_1	-	Coefficient of polynomial fit to K(z) in SDSS g band	arith.factor
PCOEFF_FUV_5	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_4	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_3	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_2	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
PCOEFF_FUV_1	-	Coefficient of polynomial fit to K(z) in GALEX FUV band	arith.factor
NQ	-	Redshift quality	meta.code.qual;src.redshift
METS	-	Average metallicity of currently surviving stars	phys.abund.Z
MASS	M_solar	Stellar mass of currently surviving stars	phys.mass
KCORR_Z	mag	K-correction in SDSS z band	phot.mag;em.opt.Z
KCORR_Y	mag	K-correction in UKIDSS Y band	phot.mag;em.IR.NIR
KCORR_U	mag	K-correction in SDSS u band	phot.mag;em.opt.U
KCORR_R	mag	K-correction in SDSS r band	phot.mag;em.opt.R
KCORR_NUV	mag	K-correction in GALEX NUV band	phot.mag;em.UV.200-300nm
KCORR_K	mag	K-correction in UKIDSS K band	phot.mag;em.IR.K
KCORR_J	mag	K-correction in UKIDSS J band	phot.mag;em.IR.J
KCORR_I	mag	K-correction in SDSS i band	phot.mag;em.opt.I
KCORR_H	mag	K-correction in UKIDSS H band	phot.mag;em.IR.H
KCORR_G	mag	K-correction in SDSS g band	phot.mag;em.opt.G
KCORR_FUV	mag	K-correction in GALEX FUV band	phot.mag;em.UV.100-200nm
I_MODEL_ERR	mag	SDSS DR6 i-band model magnitude error	stat.error;phot.mag;em.opt.I
I_MODEL	mag	SDSS DR6 i-band model magnitude	phot.mag;em.opt.I
INTSFH	-	Total integrated star-formation history (number of stars formed total)	meta.number
G_MODEL_ERR	mag	SDSS DR6 g-band model magnitude error	stat.error;phot.mag;em.opt.B
G_MODEL	mag	SDSS DR6 g-band model magnitude	phot.mag;em.opt.B
COEFFS_5	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_4	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_3	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_2	-	kcorrect eigenspectra coefficient	arith.factor
COEFFS_1	-	kcorrect eigenspectra coefficient	arith.factor
CHI2	-	Chi^2 of fit returned by kcorrect	stat.fit.chi2
CATAID	-	Unique GAMA ID	meta.id;meta.main
B300	-	Fraction of the total star formation that has occurred in the last 0.3 Gyr	arith.ratio
B1000	-	Fraction of the total star formation that has occurred in the last 1 Gyr	arith.ratio

StellarMasses

name: StellarMasses | type: CatalogueGroup | Edward Taylor [javascript protected email address] | version v08 |

read more

StellarMasses
StellarMasses
v08
2012-12-07
Edward Taylor

This table provides stellar masses, restframe photometry, and other
ancillary stellar population parameters from stellar population fits
to ugriz SEDs for all galaxies with 0 < z < 0.65 and nQ > 1 from the
GAMA DR2 sample. Maximum redshifts for target selection are also
given, for use in 1/Vmax-style incompleteness corrections.

VERY IMPORTANT NOTE:
The values in this table are based on aperture (AUTO) photometry,
which may miss a significant fraction of a galaxy's light. Make sure
you understand the need for and meaning of the quantity <fluxscale>,
which is described under 'based on matched aperture photometry' below.

When using this table, please refer to:
E.N. Taylor et al., 2011, MNRAS, 418, 1587
______________________________________________________________________________

DMU dependencies:
TilingCat - heliocentric redshifts, quality flags, etc.
ApMatchedCat - matched aperture SED photometry
SersicCatAll - total r-band Sersic magnitudes
GalacticExtinction - foreground dust values
DistancesFrames - flow corrected redshifts for distances
______________________________________________________________________________



STELLAR POPULATION SYNTHESIS MODELLING: ______________________________________

The data provided by this table have been derived through stellar
population synthesis modelling of broadband optical (ugriz)
photometry. The modelling is done using the Bruzual & Charlot (2003)
stellar evolution models, assuming a Chabrier (2003) stellar initial
mass function (IMF) and the Calzetti et al. (2000) dust curve. The SPS
models used in the fitting are defined via four parameters: e-folding
time for the (exponentially declining) star formation history, time
since formation (ie. age), stellar metallicity, and dust attenuation
(Section 3.1 of Taylor et al. 2011). Note that the NIR photometry
available for GAMA galaxies have not been used at this stage, for the
simple reason that the models do not provide a good description of the
full optical-to-NIR SED shapes (Section 4 of Taylor et al. 2011). The
SPS grid spans the range 0 < z < 0.65; objects with z > 0.65 have not
been fit. (Talk to Edward Taylor if you need/would like mass estimates
for these galaxies.) The values of all derived parameters given in
the table, including the formal uncertainties, have been derived in a
Bayesian way (Sections 3.2-3.4 of Taylor et al. 2011).

DISTANCES AND COSMOLOGY: _____________________________________________________

All values are derived for the concordance (Omega_m, Omega_L, h) =
(0.3, 0.7, 0.7) cosmology. Stellar population parameters including
ages, dust extinctions, and mass-to-light ratios are cosmology
independent, inasmuch as they pertain to the stellar populations at
the time of observation. Restframe luminosities and thus the total
stellar mass do depend on distance, and so on h^-2. These can be
scaled in the usual way, such that a higher value of h implies a lower
distance, and thus a lower luminosity/mass (see below). Note that
distances have been computed using the flow-corrected redshifts
<Z_TONRY> given in DistancesFrames. These values have been derived
using the Tonry et al. (2000) flow model for very low redshifts, and
then tapering to a CMB-centric frame for z > 0.03, as described by
Baldry et al. (2012), and are reproduced in this catalogue.

BASED ON MATCHED APERTURE PHOTOMETRY: ________________________________________

The results given have been derived from ugriz SEDs constructed from
matched aperture photometry. The photometry is the r-defined AUTO
photometry from ApMatchedCat (see Hill et al. 2011; Liske et al. in
prep.)

AN APERTURE CORRECTION IS THEREFORE REQUIRED for integrated quantities
(i.e. stellar mass or luminosity), in order to account for mass/flux
that falls beyond the finite AUTO aperture used for the SEDs. The
column <fluxscale> is provided for this purpose. The quantity
<fluxscale> is the (linear) ratio between the r-band (AUTO) aperture
flux and the total r-band flux inferred from fitting a Sersic profile
(truncated at 10 Re, i.e. <GAL_MAG_10RE_R> from SersicCatAll).

THIS CORRECTION IS NOT APPLIED BY DEFAULT for two reasons. First, not
all objects have a Sersic-fit magnitude owing to failures in either
the SExtractor detection/segmentation or the GALFIT Sersic fitting
procedures (see Kelvin et al. 2012). These objects can be identified
as those with <fluxscale> = -9999. (Note that there is also 1 object
that Source Extractor has failed to produce r-band AUTO photometry
for, which is given <fluxscale> = 9999.) Second, particularly for the
fainter galaxies with higher (but unquantified) uncertainties in the
Sersic-fit magnitudes, the flux scaling implied by the Sersic
magnitudes is not necessarily physically sensible. For many galaxies,
the Sersic magnitude is less than the aperture magnitude, which is
logically inconsistent. Further, for some galaxies, the implied flux
scaling leads to masses that are unrealistically high (log M* >> 13).

THE USER IS THEREFORE TRUSTED TO APPLY THESE CORRECTIONS, but with the
understanding that some care is required. The recommended mass to use
is thus:
log10 M*,total = <logmstar> + log10(<fluxscale>) - 2 log10(h/0.7),
and the recommended absolute magnitudes in the X-band are:
M_X,total = <absmag_X> - 2.5 log10(<fluxscale>) + 5 log10(h/0.7).

Users should check to ensure that this makes sense (e.g. check that
<fluxscale> is greater than or equal to unity, and that the magnitude
of the correction is not a factor of many) for their specific
object(s) of interest. Note, too, that this correction introduces an
additional source of uncertainty in the total luminosities and masses
that is not quantified in these tables.

RESTFRAME PHOTOMETRY AND COLOURS: ____________________________________________

All of the photometry provided by this table has been inferred from
the SPS fits as an attribute of the SP models. All restframe
photometry uses AB zeropoints and is k-corrected to redshift 0, with
no evolution corrections. The table contains restframe (g - i) and (u
- r) colours (in the columns <gminusi> and <uminusi>, respectively) as
well as restframe photometry in individual bands (e.g. <absmag_g> and
<absmag_i>). Because in the fitting process, ugriz fluxes are highly
correlated with one another, the formal uncertainties on <gminusi> or
<uminusr> cannot in general be derived from the <delrfphot>s. It is
thus preferable to use, e.g., <gminusi> and the associated uncertainty
<delgminusi> rather than <absmag_g> - <absmag_i>.

INTRINSIC VERSUS EFFECTIVE RESTFRAME PHOTOMETRY: _____________________________

The quantities <absmag_X> should be understood as *effective*
restframe absolute magnitudes in the X-band; that is, the absolute
magnitudes corresponding to the light the observer actually sees from
the galaxy, without correction for extinction within the galaxy
itself. In contrast, the quantites <absmag_X_stars> give *intrinsic*
absolute magnitudes in the X-band, which should be understood to be
the total light emitted by stars; that is, corrected for internal dust
extinction according to <extBV>. In both cases, these values are
derived from the SPS fits as properties of the stellar populations in
a similar way to ages, metallicities, mass-to-light ratios,
etc. (i.e. a la Equation 5 of Taylor et al. 2011).

MAXIMAL DETECTION/SELECTION REDSHIFTS FOR INCOMPLETENESS CORRECTIONS: ________

In order to facilitate the derivation of completeness-corrected number
densities, limiting redshifts have been derived for three r-band
selection limits: r < 17.88 (i.e. SDSS main sample target selection);
r < 19.4 (G09 and G15 SURVEY_CLASS >= 6 target selection); and r <
19.8 (G12 SURVEY_CLASS >= 6 target selection). All three of these
selections are phrased in terms of r-band Petrosian magnitudes, as
given in the SDSS DR6 catalogues, AFTER correction for foreground
(Galactic) extinction, and quoted as <R_PETRO> in TilingCatv16. The
limiting redshifts are the maximum redshift at which any given galaxy
would satisfy the r-band selection in question. These values have been
derived in the course of the SPS fits, using the single best fitting
template to estimate how the r-band magnitude varies with
redshift/distance. Note that these limiting redshifts should be
understood as being flow-corrected, not heliocentric (see Section 3.5
of Taylor et al. 2011). Users should bear this in mind when selecting
or binning galaxies by redshift. As an example for how to use these
values, imagining that the user is considering galaxies with z <
z_limit, the effective survey volume for each individual object can be
calculated as:

V_max ~ 96 * comovingVolume(min(zmax_19p4, zlimit))
+ 48 * comovingVolume(min(zmax_19p8, zlimit)).

Talk to, for example, Edward Taylor, Ivan Baldry, or Peder Norberg if
you are worried about how to do this.

KNOWN ISSUES: ________________________________________________________________

* There are a number of very low redshift objects that are given
unphysically low values for <logmstar>; e.g. <logmstar> << 6. These
are almost all stars, and can largely be excluded by considering z >
0.003.

* There are a very few objects for which the fitting procedure has
failed. For these objects, all SP parameters are given as -99;
i.e. as missing data.

* There are a number of objects that are given one or more of the
<zmax>s >= 0.65. This corresponds to the maximum redshift covered by
the SPL grid. This is true for many of the galaxies where the fits
have failed (see above), but also for galaxies with reasonable SP
parameters. For these "okay" galaxies, this should be interpreted as
a lower limit to the values of the <zmax>s. (Or, in other words, the
implication is that GAMA is volume limited for such objects for z <=
0.65.)

* There are a number of objects with Z ~ 0.05, which corresponds to
the maximum metallicity contained in the SPS grids. The mass
estimates for these objects are unlikely to be significantly
compromised, but the age and dust extinction values may be biased.

This DMU provides stellar masses, restframe photometry, and other ancillary stellar population parameters for all z < 0.65 galaxies in the GAMA DR2 sample.

• Tables
• StellarMasses

StellarMasses

name: StellarMasses | type: CatalogueTable | Edward Taylor [javascript protected email address] | version v08 |

read more

StellarMasses
StellarMasses
v08
2012-12-07
Edward Taylor

This table provides stellar masses, restframe photometry, and other
ancillary stellar population parameters from stellar population fits
to ugriz SEDs for all galaxies with 0 < z < 0.65 and nQ > 1 from the
GAMA DR2 sample. Maximum redshifts for target selection are also
given, for use in 1/Vmax-style incompleteness corrections.

VERY IMPORTANT NOTE:
The values in this table are based on aperture (AUTO) photometry,
which may miss a significant fraction of a galaxy's light. Make sure
you understand the need for and meaning of the quantity <fluxscale>,
which is described under 'based on matched aperture photometry' below.

When using this table, please refer to:
E.N. Taylor et al., 2011, MNRAS, 418, 1587
______________________________________________________________________________

DMU dependencies:
TilingCat - heliocentric redshifts, quality flags, etc.
ApMatchedCat - matched aperture SED photometry
SersicCatAll - total r-band Sersic magnitudes
GalacticExtinction - foreground dust values
DistancesFrames - flow corrected redshifts for distances
______________________________________________________________________________



STELLAR POPULATION SYNTHESIS MODELLING: ______________________________________

The data provided by this table have been derived through stellar
population synthesis modelling of broadband optical (ugriz)
photometry. The modelling is done using the Bruzual & Charlot (2003)
stellar evolution models, assuming a Chabrier (2003) stellar initial
mass function (IMF) and the Calzetti et al. (2000) dust curve. The SPS
models used in the fitting are defined via four parameters: e-folding
time for the (exponentially declining) star formation history, time
since formation (ie. age), stellar metallicity, and dust attenuation
(Section 3.1 of Taylor et al. 2011). Note that the NIR photometry
available for GAMA galaxies have not been used at this stage, for the
simple reason that the models do not provide a good description of the
full optical-to-NIR SED shapes (Section 4 of Taylor et al. 2011). The
SPS grid spans the range 0 < z < 0.65; objects with z > 0.65 have not
been fit. (Talk to Edward Taylor if you need/would like mass estimates
for these galaxies.) The values of all derived parameters given in
the table, including the formal uncertainties, have been derived in a
Bayesian way (Sections 3.2-3.4 of Taylor et al. 2011).

DISTANCES AND COSMOLOGY: _____________________________________________________

All values are derived for the concordance (Omega_m, Omega_L, h) =
(0.3, 0.7, 0.7) cosmology. Stellar population parameters including
ages, dust extinctions, and mass-to-light ratios are cosmology
independent, inasmuch as they pertain to the stellar populations at
the time of observation. Restframe luminosities and thus the total
stellar mass do depend on distance, and so on h^-2. These can be
scaled in the usual way, such that a higher value of h implies a lower
distance, and thus a lower luminosity/mass (see below). Note that
distances have been computed using the flow-corrected redshifts
<Z_TONRY> given in DistancesFrames. These values have been derived
using the Tonry et al. (2000) flow model for very low redshifts, and
then tapering to a CMB-centric frame for z > 0.03, as described by
Baldry et al. (2012), and are reproduced in this catalogue.

BASED ON MATCHED APERTURE PHOTOMETRY: ________________________________________

The results given have been derived from ugriz SEDs constructed from
matched aperture photometry. The photometry is the r-defined AUTO
photometry from ApMatchedCat (see Hill et al. 2011; Liske et al. in
prep.)

AN APERTURE CORRECTION IS THEREFORE REQUIRED for integrated quantities
(i.e. stellar mass or luminosity), in order to account for mass/flux
that falls beyond the finite AUTO aperture used for the SEDs. The
column <fluxscale> is provided for this purpose. The quantity
<fluxscale> is the (linear) ratio between the r-band (AUTO) aperture
flux and the total r-band flux inferred from fitting a Sersic profile
(truncated at 10 Re, i.e. <GAL_MAG_10RE_R> from SersicCatAll).

THIS CORRECTION IS NOT APPLIED BY DEFAULT for two reasons. First, not
all objects have a Sersic-fit magnitude owing to failures in either
the SExtractor detection/segmentation or the GALFIT Sersic fitting
procedures (see Kelvin et al. 2012). These objects can be identified
as those with <fluxscale> = -9999. (Note that there is also 1 object
that Source Extractor has failed to produce r-band AUTO photometry
for, which is given <fluxscale> = 9999.) Second, particularly for the
fainter galaxies with higher (but unquantified) uncertainties in the
Sersic-fit magnitudes, the flux scaling implied by the Sersic
magnitudes is not necessarily physically sensible. For many galaxies,
the Sersic magnitude is less than the aperture magnitude, which is
logically inconsistent. Further, for some galaxies, the implied flux
scaling leads to masses that are unrealistically high (log M* >> 13).

THE USER IS THEREFORE TRUSTED TO APPLY THESE CORRECTIONS, but with the
understanding that some care is required. The recommended mass to use
is thus:
log10 M*,total = <logmstar> + log10(<fluxscale>) - 2 log10(h/0.7),
and the recommended absolute magnitudes in the X-band are:
M_X,total = <absmag_X> - 2.5 log10(<fluxscale>) + 5 log10(h/0.7).

Users should check to ensure that this makes sense (e.g. check that
<fluxscale> is greater than or equal to unity, and that the magnitude
of the correction is not a factor of many) for their specific
object(s) of interest. Note, too, that this correction introduces an
additional source of uncertainty in the total luminosities and masses
that is not quantified in these tables.

RESTFRAME PHOTOMETRY AND COLOURS: ____________________________________________

All of the photometry provided by this table has been inferred from
the SPS fits as an attribute of the SP models. All restframe
photometry uses AB zeropoints and is k-corrected to redshift 0, with
no evolution corrections. The table contains restframe (g - i) and (u
- r) colours (in the columns <gminusi> and <uminusi>, respectively) as
well as restframe photometry in individual bands (e.g. <absmag_g> and
<absmag_i>). Because in the fitting process, ugriz fluxes are highly
correlated with one another, the formal uncertainties on <gminusi> or
<uminusr> cannot in general be derived from the <delrfphot>s. It is
thus preferable to use, e.g., <gminusi> and the associated uncertainty
<delgminusi> rather than <absmag_g> - <absmag_i>.

INTRINSIC VERSUS EFFECTIVE RESTFRAME PHOTOMETRY: _____________________________

The quantities <absmag_X> should be understood as *effective*
restframe absolute magnitudes in the X-band; that is, the absolute
magnitudes corresponding to the light the observer actually sees from
the galaxy, without correction for extinction within the galaxy
itself. In contrast, the quantites <absmag_X_stars> give *intrinsic*
absolute magnitudes in the X-band, which should be understood to be
the total light emitted by stars; that is, corrected for internal dust
extinction according to <extBV>. In both cases, these values are
derived from the SPS fits as properties of the stellar populations in
a similar way to ages, metallicities, mass-to-light ratios,
etc. (i.e. a la Equation 5 of Taylor et al. 2011).

MAXIMAL DETECTION/SELECTION REDSHIFTS FOR INCOMPLETENESS CORRECTIONS: ________

In order to facilitate the derivation of completeness-corrected number
densities, limiting redshifts have been derived for three r-band
selection limits: r < 17.88 (i.e. SDSS main sample target selection);
r < 19.4 (G09 and G15 SURVEY_CLASS >= 6 target selection); and r <
19.8 (G12 SURVEY_CLASS >= 6 target selection). All three of these
selections are phrased in terms of r-band Petrosian magnitudes, as
given in the SDSS DR6 catalogues, AFTER correction for foreground
(Galactic) extinction, and quoted as <R_PETRO> in TilingCatv16. The
limiting redshifts are the maximum redshift at which any given galaxy
would satisfy the r-band selection in question. These values have been
derived in the course of the SPS fits, using the single best fitting
template to estimate how the r-band magnitude varies with
redshift/distance. Note that these limiting redshifts should be
understood as being flow-corrected, not heliocentric (see Section 3.5
of Taylor et al. 2011). Users should bear this in mind when selecting
or binning galaxies by redshift. As an example for how to use these
values, imagining that the user is considering galaxies with z <
z_limit, the effective survey volume for each individual object can be
calculated as:

V_max ~ 96 * comovingVolume(min(zmax_19p4, zlimit))
+ 48 * comovingVolume(min(zmax_19p8, zlimit)).

Talk to, for example, Edward Taylor, Ivan Baldry, or Peder Norberg if
you are worried about how to do this.

KNOWN ISSUES: ________________________________________________________________

* There are a number of very low redshift objects that are given
unphysically low values for <logmstar>; e.g. <logmstar> << 6. These
are almost all stars, and can largely be excluded by considering z >
0.003.

* There are a very few objects for which the fitting procedure has
failed. For these objects, all SP parameters are given as -99;
i.e. as missing data.

* There are a number of objects that are given one or more of the
<zmax>s >= 0.65. This corresponds to the maximum redshift covered by
the SPL grid. This is true for many of the galaxies where the fits
have failed (see above), but also for galaxies with reasonable SP
parameters. For these "okay" galaxies, this should be interpreted as
a lower limit to the values of the <zmax>s. (Or, in other words, the
implication is that GAMA is volume limited for such objects for z <=
0.65.)

* There are a number of objects with Z ~ 0.05, which corresponds to
the maximum metallicity contained in the SPS grids. The mass
estimates for these objects are unlikely to be significantly
compromised, but the age and dust extinction values may be biased.

This table provides stellar masses, restframe photometry, and other ancillary stellar population parameters from stellar population fits to ugriz SEDs for all z < 0.65 galaxies in the GAMA DR2 sample.

Address this table as gama_dr2.StellarMasses

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
zmax_19p8	-	Maximum redshift for which r_petro <= 19.8 (G12 SURVEY_CLASS>=6 selection)	src.redshift;stat.max
zmax_19p4	-	Maximum redshift for which r_petro <= 19.4 (G09/G15 SURVEY_CLASS>=6 selection)	src.redshift;stat.max
zmax_17p88	-	Maximum redshift for which r_petro <= 17.8 (SDSS main survey selection)	src.redshift;stat.max
uminusr_stars	mag	Intrinsic, stellar (u-r) colour from SED fit, i.e. corrected for internal dust obscuration	phot.color
uminusr	mag	Restframe (u-r) colour from SED fit	phot.color
nbands	-	Number of bands used in SPS fits (max. is 5; NIR data have not been used)	meta.number
nQ	-	Normalised redshift quality (use nQ > 2 for science)	meta.code.qual;src.redshift
metal	-	SPS stellar metallicity (Z_Sol = 0.02)	phys.abund.Z
logtau	dex	SPS e-folding time for the exponentially declining SFH, represented as log10(tau/[yr])	time.scale
logmstar	dex	Stellar mass within the photometric aperture represented as log10(M_*/[M_Sol]) (see notes)	phys.mass
logmoverl_i	dex	Mass-to-light ratio (restframe i-band) represented as log10( (M_*/L_i) / [M_Sol/L_Sol,i] )	phys.composition.massLightRatio
logage	dex	SPS age T = t(z_obs) - t(z_form), represented as log10(T/[yr])	time.age
logLWage	dex	Restframe i-band luminosity weighted mean stellar age, represented as log10(t*/[yr])	time.age
gminusi_stars	mag	Intrinsic, stellar (g-i) colour from SED fit, i.e. corrected for internal dust obscuration	phot.color
gminusi	mag	Restframe (g-i) colour from SED fit	phot.color
fluxscale	-	Aperture correction factor for scaling total luminosities and stellar masses (see notes)	arith.factor
fitphot_z	mag	Best-fit observers` frame z-band apparent magnitude from SPS SED fits	phot.mag
fitphot_u	mag	Best-fit observers` frame u-band apparent magnitude from SPS SED fits	phot.mag
fitphot_r	mag	Best-fit observers` frame r-band apparent magnitude from SPS SED fits	phot.mag
fitphot_i	mag	Best-fit observers` frame i-band apparent magnitude from SPS SED fits	phot.mag
fitphot_g	mag	Best-fit observers` frame g-band apparent magnitude from SPS SED fits	phot.mag
extBV	mag	SPS dust obscuration; for Calzetti et al. (2003) dust A_V = 3.1 x E(B-V)	phys.absorption
deluminusr	mag	Formal uncertainty on uminusr	stat.error
delmetal	-	Formal uncertainty on metal	stat.error
dellogtau	dex	Formal uncertainty on logtau	stat.error
dellogmstar	dex	Formal uncertainty on logmstar	stat.error
dellogmoverl_i	dex	Formal uncertainty on logmoverl_i	stat.error
dellogage	dex	Formal uncertainty on logage	stat.error
dellogLWage	dex	Formal uncertainty on logLWage	stat.error
delgminusi	mag	Formal uncertainty on gminusi	stat.error
delfitphot_z	mag	Formal uncertainty in fitphot_z	stat.error
delfitphot_u	mag	Formal uncertainty in fitphot_u	stat.error
delfitphot_r	mag	Formal uncertainty in fitphot_r	stat.error
delfitphot_i	mag	Formal uncertainty in fitphot_i	stat.error
delfitphot_g	mag	Formal uncertainty in fitphot_g	stat.error
delextBV	mag	Formal uncertainty on extBV	stat.error
delabsmag_z	mag	Formal uncertainty in absmag_z	stat.error
delabsmag_u	mag	Formal uncertainty in absmag_u	stat.error
delabsmag_r	mag	Formal uncertainty in absmag_r	stat.error
delabsmag_i	mag	Formal uncertainty in absmag_i	stat.error
delabsmag_g	mag	Formal uncertainty in absmag_g	stat.error
absmag_z_stars	mag	Intrinsic abs. mag. of all stellar emission (i.e. corrected for internal dust extinction) in restframe z-band	phys.magAbs
absmag_z	mag	Absolute magnitude in restframe z-band from SPS SED fits	phys.magAbs
absmag_u_stars	mag	Intrinsic abs. mag. of all stellar emission (i.e. corrected for internal dust extinction) in restframe u-band	phys.magAbs
absmag_u	mag	Absolute magnitude in restframe u-band from SPS SED fits	phys.magAbs
absmag_r_stars	mag	Intrinsic abs. mag. of all stellar emission (i.e. corrected for internal dust extinction) in restframe r-band	phys.magAbs
absmag_r	mag	Absolute magnitude in restframe r-band from SPS SED fits	phys.magAbs
absmag_i_stars	mag	Intrinsic abs. mag. of all stellar emission (i.e. corrected for internal dust extinction) in restframe i-band	phys.magAbs
absmag_i	mag	Absolute magnitude in restframe i-band from SPS SED fits	phys.magAbs
absmag_g_stars	mag	Intrinsic abs. mag. of all stellar emission (i.e. corrected for internal dust extinction) in restframe g-band	phys.magAbs
absmag_g	mag	Absolute magnitude in restframe g-band from SPS SED fits	phys.magAbs
Z_TONRY	-	Flow corrected redshift using Tonry et al. model	src.redshift
Z	-	Heliocentric redshift	src.redshift
SURVEY_CODE	-	Redshift source flag (5=GAMA; 1=SDSS)	meta.code;meta.dataset
C_logM_ur	-	Correlation coefficient between logmstar and uminusi for covariant error matrix	stat.correlation
C_logM_gi	-	Correlation coefficient between logmstar and gminusi for covariant error matrix	stat.correlation
C_logM_eBV	-	Correlation coefficient between logmstar and extBV for covariant error matrix	stat.correlation
CATAID	-	Unique ID of GAMA object	meta.id;meta.main

SpecLineSFR

name: SpecLineSFR | type: CatalogueGroup | Madusha Gunawardhana [javascript protected email address] | version v04 |

read more

SpecLineSFR
2013-04-10
Madusha Gunawardhana

Please see this PDF document for a detailed description of the
SpecLineSFR DMU.

This DMU provides emission and absorption line measurements for all GAMA DR2 AAT spectra, as well as derived physical properties, including the star-formation rate, for all GAMA DR2 spectra and for all SDSS spectra of GAMA DR2 objects.

• Tables
• EmLinesPhys
• EmLinesPhysGAMA
• EmLinesPhysSDSS
• SpecLines

EmLinesPhys

name: EmLinesPhys | type: CatalogueTable | Madusha Gunawardhana [javascript protected email address] | version v04 |

This is the main table of the SpecLineSFR DMU. It provides Balmer decrements, Halpha luminosities, Halpha derived star-formation rates and emission line classifications for all GAMA DR2 objects with z > -0.01 (where available).

Address this table as gama_dr2.EmLinesPhys

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z_TONRY	-	Flow corrected redshift calculated from Z_HELIO_BEST using Tonry et al. model	src.redshift
Z_HELIO_BEST	-	Heliocentric redshift of the IS_BEST spectrum	src.redshift
Z_HELIO	-	Heliocentric redshift of the measurement spectrum	src.redshift
WARNING_FLAG	-	Halpha or Hbeta affected by data reduction issues?	meta.code
SURVEY_BEST	-	Survey the IS_BEST spectrum originated from	meta.code
SURVEY	-	Survey the measurement spectrum originated from	meta.code
SPECID_BEST	-	Unique ID of the spectrum that provides the best redshift for this object (IS_BEST spectrum)	meta.id;meta.main
SPECID	-	Unique ID of spectrum on which line measurements were performed (measurement spectrum)	meta.id;meta.main
SN_EMI	-	Halpha emission signal-to-noise	stat.snr
SN_CONT	-	Continuum signal-to-noise	stat.snr
SFR	M_sun/yr	Halpha derived star formation rate assuming a Salpeter IMF	phys.SFR;em.line.Halpha
RA	deg	RA of GAMA object (J2000)	pos.eq.ra
PETROMAG_R	mag	SDSS r band Petrosian magnitude (not corrected for Galactic extinction)	phot.mag;em.opt.R
NQ_BEST	-	Normalised redshift quality of Z_HELIO_BEST	meta.code.qual;src.redshift
NQ	-	Normalised redshift quality of Z_HELIO	meta.code.qual;src.redshift
L_APOBSCOR	W	Halpha luminosity corrected for stellar absorption, fibre aperture effects and dust obscuration	phys.luminosity;em.line.Halpha
L_APCOR	W	Halpha luminosity corrected for stellar absorption and fibre aperture effects	phys.luminosity;em.line.Halpha
K_R	mag	K-correction in SDSS r band	phot.mag
F_HBETA	10^(-17)erg/s/cm^2	Stellar absorption corrected Hbeta flux	spect.line.intensity;em.line.Hbeta
F_HALPHA	10^(-17)erg/s/cm^2	Stellar absorption corrected Halpha flux	spect.line.intensity;em.line.Hbeta
EMLINE_METHOD	-	AGN classification method (see notes)	meta.code
EMLINE_CLASS	-	AGN classification based on Kewley et al. (2001)	meta.code
DM_70_30_70	mag	Distance modulus for 737 cosmology calculated from Z_TONRY	phot.mag.distMod
DEC	deg	DEC of GAMA object (J2000)	pos.eq.dec
CATAID	-	Unique ID of GAMA object	meta.id.cross;src
BALMER_DECREMENT	-	Balmer decrement (see notes)	phot.flux;arith.ratio;spect.line
BALMERDEC_FLAG	-	Is the Balmer decrement measured or estimated?	meta.code;phot.flux;arith.ratio
A_R	mag	Galactic extinction in SDSS r band	phys.absorption.gal;em.opt.R
AB_R	mag	SDSS r band absolute magnitude: PETROMAG_R - DM_70_30_70 - A_R - K_R; AB magnitude	phys.magAbs

EmLinesPhysGAMA

name: EmLinesPhysGAMA | type: CatalogueTable | Madusha Gunawardhana [javascript protected email address] | version v04 |

This table provides Balmer decrements, Halpha luminosities, Halpha derived star-formation rates and emission line classifications for all spectra in SpecLines with any measured Halpha emission and z > 0.001.

Address this table as gama_dr2.EmLinesPhysGAMA

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z_TONRY	-	Flow corrected redshift using Tonry et al. model	src.redshift
Z_HELIO	-	Heliocentric redshift	src.redshift
WARNING_FLAG	-	Halpha or Hbeta affected by data reduction issues?	meta.code
SPECID	-	Unique spectrum ID	meta.id;meta.main
SN_EMI	-	Halpha emission signal-to-noise	stat.snr
SN_CONT	-	Continuum signal-to-noise	stat.snr
SFR	M_sun/yr	Halpha derived star formation rate assuming a Salpeter IMF	phys.SFR;em.line.Halpha
RA	deg	RA of spectrum (J2000)	pos.eq.ra
PETROMAG_R	mag	SDSS r band Petrosian magnitude (not corrected for Galactic extinction)	phot.mag;em.opt.R
NQ	-	Normalised redshift quality (use NQ>2 for science)	meta.code.qual;src.redshift
L_APOBSCOR	W	Halpha luminosity corrected for stellar absorption, fibre aperture effects and dust obscuration	phys.luminosity;em.line.Halpha
L_APCOR	W	Halpha luminosity corrected for stellar absorption and fibre aperture effects	phys.luminosity;em.line.Halpha
K_R	mag	K-correction in SDSS r band	phot.mag
IS_SBEST	-	Spectrum with best redshift for this object in GAMA AAT survey?	meta.code
IS_BEST	-	Spectrum with best redshift for this object across all surveys?	meta.code
F_HBETA	10^(-17)erg/s/cm^2	Stellar absorption corrected Hbeta flux	spect.line.intensity;em.line.Hbeta
F_HALPHA	10^(-17)erg/s/cm^2	Stellar absorption corrected Halpha flux	spect.line.intensity;em.line.Hbeta
EMLINE_METHOD	-	AGN classification method (see notes)	meta.code
EMLINE_CLASS	-	AGN classification based on Kewley et al. (2001)	meta.code
DM_70_30_70	mag	Distance modulus for 737 cosmology	phot.mag.distMod
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
BALMER_DECREMENT	-	Balmer decrement (see notes)	phot.flux;arith.ratio;spect.line
BALMERDEC_FLAG	-	Is the Balmer decrement measured or estimated?	meta.code;phot.flux;arith.ratio
A_R	mag	Galactic extinction in SDSS r band	phys.absorption.gal;em.opt.R
AB_R	mag	SDSS r band absolute magnitude: PETROMAG_R - DM_70_30_70 - A_R - K_R; AB magnitude	phys.magAbs

EmLinesPhysSDSS

name: EmLinesPhysSDSS | type: CatalogueTable | Madusha Gunawardhana [javascript protected email address] | version v04 |

This table provides Balmer decrements, Halpha luminosities, Halpha derived star-formation rates and emission line classifications for all SDSS spectra of GAMA DR2 objects with any measured Halpha emission and z > 0.001. The values in this table were derived from the MPA/JHU SDSS line measurements database.

Address this table as gama_dr2.EmLinesPhysSDSS

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z_TONRY	-	Flow corrected redshift using Tonry et al. model	src.redshift
Z_HELIO_ERR	-	Redshift error	src.redshift
Z_HELIO	-	Redshift from MPA/JHU catalogue	src.redshift
SPECID	-	Unique spectrum ID	meta.id;meta.main
SN_CONT	-	Continuum signal-to-noise	stat.snr
SFR	M_sun/yr	Halpha derived star formation rate assuming a Salpeter IMF	phys.SFR;em.line.Halpha
RA	deg	RA of spectrum (J2000)	pos.eq.ra
PETROMAG_R	mag	SDSS r band Petrosian magnitude (not corrected for Galactic extinction)	phot.mag;em.opt.R
MPACAT_ROWID	-	Row number of object in MPA/JHU catalogue	meta.id
L_APOBSCOR	W	Halpha luminosity corrected for stellar absorption, fibre aperture effects and dust obscuration	phys.luminosity;em.line.Halpha
L_APCOR	W	Halpha luminosity corrected for stellar absorption and fibre aperture effects	phys.luminosity;em.line.Halpha
K_R	mag	K-correction in SDSS r band	phot.mag
IS_SBEST	-	Spectrum with best redshift for this object in SDSS?	meta.code
IS_BEST	-	Spectrum with best redshift for this object across all surveys?	meta.code
F_HBETA	10^(-17)erg/s/cm^2	Stellar absorption corrected Hbeta flux	spect.line.intensity;em.line.Hbeta
F_HALPHA	10^(-17)erg/s/cm^2	Stellar absorption corrected Halpha flux	spect.line.intensity;em.line.Hbeta
EMLINE_METHOD	-	AGN classification method (see notes)	meta.code
EMLINE_CLASS	-	AGN classification based on Kewley et al. (2001)	meta.code
DM_70_30_70	mag	Distance modulus for 737 cosmology	phot.mag.distMod
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
BALMER_DECREMENT	-	Balmer decrement (see notes)	phot.flux;arith.ratio;spect.line
BALMERDEC_FLAG	-	Is the Balmer decrement measured or estimated?	meta.code;phot.flux;arith.ratio
A_R	mag	Galactic extinction in SDSS r band	phys.absorption.gal;em.opt.R
AB_R	mag	SDSS r band absolute magnitude: PETROMAG_R - DM_70_30_70 - A_R - K_R; AB magnitude	phys.magAbs

SpecLines

name: SpecLines | type: CatalogueTable | Madusha Gunawardhana [javascript protected email address] | version v04 |

This table provides emission and absorption line measurements for all GAMA DR2 AAT spectra with a redshift measurement.

Address this table as gama_dr2.SpecLines

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z_HELIO	-	Spectroscopic redshift	src.redshift
SPECID	-	Unique spectrum ID	meta.id;meta.main
SIIRSIGERR	A	[SII] 6731A sigma error	stat.error;spect.line.width
SIIRSIG	A	[SII] 6731A sigma	spect.line.width
SIIREW	A	[SII] 6731A equivalent width (see notes)	spect.line.eqWidth
SIIRERR	10^(-17)erg/s/cm^2	[SII] 6731A line flux error	stat.error;spect.line.intensity
SIIR	10^(-17)erg/s/cm^2	[SII] 6731A line flux (Gaussian fit, see notes)	spect.line.intensity
SIIBSIGERR	A	[SII] 6716A sigma error	stat.error;spect.line.width
SIIBSIG	A	[SII] 6716A sigma	spect.line.width
SIIBEW	A	[SII] 6716A equivalent width (see notes)	spect.line.eqWidth
SIIBERR	10^(-17)erg/s/cm^2	[SII] 6716A line flux error	stat.error;spect.line.intensity
SIIB	10^(-17)erg/s/cm^2	[SII] 6716A line flux (Gaussian fit, see notes)	spect.line.intensity
RA	deg	RA of spectrum (J2000)	pos.eq.ra
OIIRSIGERR	A	[OII] 3727A sigma error	stat.error;spect.line.width
OIIRSIG	A	[OII] 3727A sigma	spect.line.width
OIIREW	A	[OII] 3727A equivalent width (see notes)	spect.line.eqWidth
OIIRERR	10^(-17)erg/s/cm^2	[OII] 3727A line flux error	stat.error;spect.line.intensity
OIIR	10^(-17)erg/s/cm^2	[OII] 3727A line flux (double Gaussian fit to red peak, see notes)	spect.line.intensity
OIIIRSIGERR	A	[OIII] 5007A sigma error	stat.error;spect.line.width;em.line.OIII
OIIIRSIG	A	[OIII] 5007A sigma	spect.line.width;em.line.OIII
OIIIREW	A	[OIII] 5007A equivalent width (see notes)	spect.line.eqWidth;em.line.OIII
OIIIRERR	10^(-17)erg/s/cm^2	[OIII] 5007A line flux error	stat.error;spect.line.intensity;em.li...
OIIIR	10^(-17)erg/s/cm^2	[OIII] 5007A line flux (Gaussian fit, see notes)	spect.line.intensity;em.line.OIII
OIIIBSIGERR	A	[OIII] 4959A sigma error	stat.error;spect.line.width
OIIIBSIG	A	[OIII] 4959A sigma	spect.line.width
OIIIBEW	A	[OIII] 4959A equivalent width (see notes)	spect.line.eqWidth
OIIIBERR	10^(-17)erg/s/cm^2	[OIII] 4959A line flux error	stat.error;spect.line.intensity
OIIIB	10^(-17)erg/s/cm^2	[OIII] 4959A line flux (Gaussian fit, see notes)	spect.line.intensity
OIIERR	10^(-17)erg/s/cm^2	[OII] 3727A line flux error (Gaussian fit)	stat.error;spect.line.intensity
OIIBSIGERR	A	[OII] 3727A sigma error	stat.error;spect.line.width
OIIBSIG	A	[OII] 3727A sigma	spect.line.width
OIIBEW	A	[OII] 3727A equivalent width (see notes)	spect.line.eqWidth
OIIBERR	10^(-17)erg/s/cm^2	[OII] 3727A line flux error	stat.error;spect.line.intensity
OIIB	10^(-17)erg/s/cm^2	[OII] 3727A line flux (double Gaussian fit to blue peak, see notes)	spect.line.intensity
OII	10^(-17)erg/s/cm^2	[OII] 3727A line flux (Gaussian fit, see notes)	spect.line.intensity
NQ	-	Quality flag (4 is reliable, 3 tentative)	meta.code.qual;src.redshift
NIIRSIGERR	A	[NII] 6584A sigma error	stat.error;spect.line.width
NIIRSIG	A	[NII] 6584A sigma	spect.line.width
NIIREW	A	[NII] 6584A equivalent width (see notes)	spect.line.eqWidth
NIIRERR	10^(-17)erg/s/cm^2	[NII] 6584A line flux error	stat.error;spect.line.intensity
NIIR	10^(-17)erg/s/cm^2	[NII] 6584A line flux (Gaussian fit, see notes)	spect.line.intensity
NIIBSIGERR	A	[NII] 6548A sigma error	stat.error;spect.line.width
NIIBSIG	A	[NII] 6548A sigma	spect.line.width
NIIBEW	A	[NII] 6548A equivalent width (see notes)	spect.line.eqWidth
NIIBERR	10^(-17)erg/s/cm^2	[NII] 6548A line flux error	stat.error;spect.line.intensity
NIIB	10^(-17)erg/s/cm^2	[NII] 6548A line flux (Gaussian fit, see notes)	spect.line.intensity
IS_SBEST	-	Spectrum with best redshift for this object in GAMA AAT survey?	meta.code
IS_BEST	-	Spectrum with best redshift for this object across all surveys?	meta.code
ISIIRERR	10^(-17)erg/s/cm^2	[SII] 6731A integrated line flux error	stat.error;phot.flux;spect.line
ISIIR	10^(-17)erg/s/cm^2	[SII] 6731A integrated line flux (see notes)	phot.flux;spect.line
ISIIBERR	10^(-17)erg/s/cm^2	[SII] 6716A integrated line flux error	stat.error;phot.flux;spect.line
ISIIB	10^(-17)erg/s/cm^2	[SII] 6716A integrated line flux (see notes)	phot.flux;spect.line
IOIIIRERR	10^(-17)erg/s/cm^2	[OIII] 5007A integrated line flux error	stat.error;phot.flux;em.line.OIII
IOIIIR	10^(-17)erg/s/cm^2	[OIII] 5007A integrated line flux (see notes)	phot.flux;em.line.OIII
IOIIIBERR	10^(-17)erg/s/cm^2	[OIII] 4959A integrated line flux error	stat.error;phot.flux;spect.line
IOIIIB	10^(-17)erg/s/cm^2	[OIII] 4959A integrated line flux (see notes)	phot.flux;spect.line
IOIIERR	10^(-17)erg/s/cm^2	[OII] 3727A integrated line flux error	stat.error;phot.flux;spect.line
IOII	10^(-17)erg/s/cm^2	[OII] 3727A integrated line flux (see notes)	phot.flux;spect.line
IOI6364ERR	10^(-17)erg/s/cm^2	[OI] 6364A integrated line flux error	stat.error;phot.flux;spect.line
IOI6364	10^(-17)erg/s/cm^2	[OI] 6364A integrated line flux (see notes)	phot.flux;spect.line
IOI6300ERR	10^(-17)erg/s/cm^2	[OI] 6300A integrated line flux error	stat.error;phot.flux;spect.line
IOI6300	10^(-17)erg/s/cm^2	[OI] 6300A integrated line flux (see notes)	phot.flux;spect.line
INIIRERR	10^(-17)erg/s/cm^2	[NII] 6584A integrated line flux error	stat.error;phot.flux;spect.line
INIIR	10^(-17)erg/s/cm^2	[NII] 6584A integrated line flux (see notes)	phot.flux;spect.line
INIIBERR	10^(-17)erg/s/cm^2	[NII] 6548A integrated line flux error	stat.error;phot.flux;spect.line
INIIB	10^(-17)erg/s/cm^2	[NII] 6548A integrated line flux (see notes)	phot.flux;spect.line
INEVRERR	10^(-17)erg/s/cm^2	[NeV] 3425A integrated line flux error	stat.error;phot.flux;spect.line
INEVR	10^(-17)erg/s/cm^2	[NeV] 3425A integrated line flux (see notes)	phot.flux;spect.line
INEVBERR	10^(-17)erg/s/cm^2	[NeV] 3345A integrated line flux error	stat.error;phot.flux;spect.line
INEVB	10^(-17)erg/s/cm^2	[NeV] 3345A integrated line flux (see notes)	phot.flux;spect.line
INEIIIERR	10^(-17)erg/s/cm^2	[NeIII] 3869A integrated line flux error	stat.error;phot.flux;spect.line
INEIII	10^(-17)erg/s/cm^2	[NeIII] 3869A integrated line flux (see notes)	phot.flux;spect.line
INADERR	10^(-17)erg/s/cm^2	NaID 5892A integrated line flux error	stat.error;phot.flux;spect.line
INAD	10^(-17)erg/s/cm^2	NaID 5892A integrated line flux (see notes)	phot.flux;spect.line
IMGERR	10^(-17)erg/s/cm^2	Mg 5174A integrated line flux error	stat.error;phot.flux;spect.line
IMG	10^(-17)erg/s/cm^2	Mg 5174A integrated line flux (see notes)	phot.flux;spect.line
IHDERR	10^(-17)erg/s/cm^2	Hdelta integrated line flux error	stat.error;phot.flux;spect.line
IHD	10^(-17)erg/s/cm^2	Hdelta integrated line flux (see notes)	phot.flux;spect.line
IHBERR	10^(-17)erg/s/cm^2	Hbeta integrated line flux error	stat.error;phot.flux;em.line.Hbeta
IHB	10^(-17)erg/s/cm^2	Hbeta integrated line flux (see notes)	phot.flux;em.line.Hbeta
IHAERR	10^(-17)erg/s/cm^2	Halpha integrated line flux error	stat.error;phot.flux;em.line.Halpha
IHA	10^(-17)erg/s/cm^2	Halpha integrated line flux (see notes)	phot.flux;em.line.Halpha
HBSIGERR	A	Hbeta sigma error	stat.error;spect.line.width;em.line.H...
HBSIG	A	Hbeta sigma	spect.line.width;em.line.Hbeta
HBEW	A	Hbeta equivalent width (see notes)	spect.line.eqWidth;em.line.Hbeta
HBERR	10^(-17)erg/s/cm^2	Hbeta line flux error (Gaussian fit)	stat.error;spect.line.intensity;em.li...
HB	10^(-17)erg/s/cm^2	Hbeta line flux (Gaussian fit, see notes)	spect.line.intensity;em.line.Hbeta
HASIGERR	A	Halpha sigma error	stat.error;spect.line.width;em.line.H...
HASIG	A	Halpha sigma	spect.line.width;em.line.Halpha
HAEW	A	Halpha equivalent width (see notes)	spect.line.eqWidth;em.line.Halpha
HAERR	10^(-17)erg/s/cm^2	Halpha line flux error (Gaussian fit)	stat.error;spect.line.intensity;em.li...
HA	10^(-17)erg/s/cm^2	Halpha line flux (Gaussian fit, see notes)	spect.line.intensity;em.line.Halpha
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec

SpecCat

name: SpecCat | type: CatalogueGroup | Joe Liske [javascript protected email address] | version v08 |

read more

SpecCat
2011-07-21
Joe Liske

This DMU produces the final spectra and redshift catalogues.

The 2dF/AAOmega multi-fibre instrument on the 3.9m Anglo-Australian
Telescope (AAT) is the main source of spectroscopic data for the GAMA
survey. Observations for GAMA I, part of which are released in DR2,
extended over three years (2008 - 2010, referred to below as Y1, Y2,
Y3).

The table AATFields provided by this DMU lists all 392 AAT 2dF/AAOmega
observations (fields) observed for GAMA I. Each of these observations
delivered on average 345 spectra of galaxy targets (for details of the
data, the observing and data reduction procedures, please see Hopkins
et al. 2013). AATFields provides some basic information on each
observation, including some rudimentary redshift success statistics.

All spectra collected for GAMA at the AAT were redshifted at the
telescope using the code runz (see below for a brief description of
this process). In addition, a fair fraction of the spectra were
redshifted again subsequently, some multiple times. The table
AATRunzResults contains the complete redshifting results
(i.e. essentially the runz output) for all GAMA AAT spectra that are
part of DR2.

The table AATSpecAllzAll contains one line for each GAMA AAT spectrum
in this release, summarising all of the redshifting results for this
spectrum, as well as listing the results of the analysis to determine
the best redshift based on the reliabilities of the redshifters. (The
reliabilities of the redshifters were determined in an analysis of the
re-redshifting results.)

The table AATSpecAll contains one line for each GAMA AAT spectrum
included in DR2, giving its best redshift as well as listing a number
of other properties of the spectrum, including its location on the
file server. Note that duplicate observations of the same objects are
retained in this table.

The table LTSpecAll lists a small number of spectra of fibre-bright
targets collected by the GAMA team at the Liverpool Telescope (LT).

The table SpecAll combines the tables AATSpecAll and LTSpecAll above
with the tables ExternalSpecAll and ExternalzAll from the ExternalSpec
DMU, thus providing a complete list of all spectra and redshifts that
are available for the objects included in DR2, including GAMA spectra
and those from previous spectroscopic surveys (such as the SDSS). Note
that duplicate observations of the same object are still retained in
this table. Note further that for those entries originating from
ExternalzAll table some parameters are not defined (such as e.g. the
minimum and maximum wavelengths of the spectrum).

Finally, the table SpecObj contains one line for each object in
SpecAll, giving details of the spectrum that provides the best
redshift (GAMA or otherwise), including the redshift. This is the
table we expect most users will be most interested in. Note that this
table contains 72,213 objects, which is 12 fewer than the number of
objects nominally included in DR2. For these 12 objects GAMA I simply
contains no spectroscopic or redshift data.

More information on particular aspects of these tables is given below.


----------------------------------------------------------------------


DMU dependencies
----------------
This version of the SpecCat DMU made use of the outputs of the
following DMUs:

Data/redshifting reduced_08 (comprising Y1-Y3 data)
See the GAMA file server and Hopkins et al. (2013)
for details on the data and data reduction procedures.
Re-redshifting v02 (covering Y1-Y3 data)
InputCat v16
ExternalSpec v01

Note that re-redshifting v02 did not fully complete the re-redshifting
of the Y3 data, leaving about 10% of the data that were not
re-redshifted.


Redshifting
-----------
All spectra observed for GAMA with the AAT are 'redshifted' by the
observing team at the telescope. The process of redshifting an
observation involves running the program 'runz' on a reduced data file
(typically containing ~345 spectra). For each spectrum, runz
automatically estimates a redshift, and then displays the spectrum
along with the positions of a number of common emission and absorption
lines at the estimated redshift. The job of the redshifter is now to
check whether the automatically determined redshift is correct. If
not, the user tries to find the correct redshift him/herself using a
number of methods provided by runz. The user then explicitly assigns a
quality, QOP (sometimes referred to as just Q), to the redshift before
moving on to the next spectrum. QOP can take values 0-4 with the
following meanings:

QOP = 4: The redshift is certainly correct.
QOP = 3: The redshift is probably correct.
QOP = 2: The redshift may be correct. Must be checked before being
included in a scientific analysis.
QOP = 1: No redshift could be found.
QOP = 0: Complete data reduction failure.

The output of the runz code is stored in table AATRunzResults.


The meaning of QOP=1 and 2 in early data
----------------------------------------
Note that there was a change in the meaning of the user-assigned
redshift quality values QOP=1 and 2 between year 2 and year 3 of the
GAMA I observing campaign. In Y1 and Y2 data QOP=1 was not used and
the meaning of QOP=2 is different from its meaning in later data. This
affects only table AATRunzResults. In table AATSpecAllzAll all the old
Y1+2 QOP=2 values were translated to the new QOP=1 and 2 values.


Re-redshifting
--------------
All QOP=1,2,3 and some QOP=4 data from Y1, Y2 and Y3 have been
independently re-redshifted by other GAMA team members (where the Y3
re-redshifting is not entirely complete). This provided additional
independent opinion(s) for each re-redshifted spectrum, as well as
estimates of how reliably each redshifter performed. This information
was used to produce a new, normalised redshift quality scale (called
nQ). This has been applied to all available redshift information (see
table AATSpecAllzAll). The quality of the redshift data is hence
largely homogeneous (except for the small incompleteness of the Y3
re-redshifting).


SPECID
------
All tables in this DMU make use of this parameter to identify a given
spectrum. For GAMA AAT spectra this is simply given by FIELDID_nnn
where nnn is the fibre number. See the notes of the ExternalSpec DMU
on how SPECID is defined for spectra from previous surveys.


Matching spectra to objects
---------------------------
Spectra are associated with GAMA objects by positionally matching them
to objects in the input catalogues, i.e. we do not simply use the IDs
of objects as provided in the 2dF/AAOmega configuration files. This is
done (i) because for a small sub-set of targets the ID changed
subsequent to the observations, and (ii) to match the procedure
employed by the ExternalSpec DMU.

For a given spectrum a matching GAMA object was identified by finding
the spectrum's closest GAMA object (within 1 arcsec) in the catalogue
resulting from the union of TilingCat and SpStandards. For those
spectra left without a match we then identified the closest GAMA
object (within 2 arcsec) in InputCatA.

Matched objects are identified by their CATAID and GAMA_NAME. The
parameter IC_FLAG is a bitwise flag identifying the catalogue(s) in
which the matched GAMA object was found:

Bit n 2^(n-1) Catalogue
-------------------------------
1 1 InputCatA
2 2 TilingCat
3 4 SpStandards

The distance between a spectrum and its matched object in arcsec is
given by the parameter DIST.

In cases where multiple GAMA spectra were matched to the same GAMA
object (duplicate observations) the flag IS_SBEST in table AATSpecAll
identifies the spectrum providing the best redshift for that
object. This spectrum was identified first by nQ, and then (in cases
of multiple spectra with the same nQ) by the parameter PROB-DIST.

In cases where multiple GAMA and non-GAMA spectra were matched to the
same GAMA object the flag IS_BEST in table SpecAll identifies the
spectrum providing the best redshift for that object. This spectrum
was identified by considering only spectra with IS_SBEST=T and then
selecting first by nQ, and then (in cases of multiple spectra with the
same nQ) by the parameter PROB-DIST.

This DMU provides the final spectra and redshift catalogues, including GAMA AAT and external data.

• Tables
• AATFields
• AATRunzResults
• AATSpecAll
• AATSpecAllzAll
• LTSpecAll
• SpecAll
• SpecObj

AATFields

name: AATFields | type: CatalogueTable | Joe Liske [javascript protected email address] | version v08 |

read more

SpecCat
AATFields
v08
2011-07-21
Joe Liske

Columns 4-11 (DATE_OBS - HAEND) of this table provide a number of
parameters related to the date and time of observations. The data for
most fields were collected in a number of consecutive exposures on the
same night. However, for a small number of fields observations were
spread over more than one night (as indicated by the parameter
N_NIGHTS). Note that in these cases the data given in columns 4-11
refer only to that night in which most of the observations (by
exposure time) were obtained.

Table of all AAT 2dF/AAOmega fields observed for GAMA I.

Address this table as gama_dr2.AATFields

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
ZDSTART	deg	Zenith distance at start of first exposure	pos.az.zd;time.start
ZDEND	deg	Zenith distance at end of last exposure	pos.az.zd;time.rnd
UTSTART	hms	UT of start of first exposure	time.start;obs.exposure
UTMJD	-	Mean MJD of start of exposures	time.epoch;obs.exposure
UTEND	hms	UT of end of last exposure	time.end;obs.exposure
USER	-	Original redshifter of this field	meta.id
T_EXP	s	Total exposure time	time.duration;obs.exposure
TDFDRVER	-	Version of 2dfdr data reduction software	meta.version;meta.software
RA	deg	RA of field centre (J2000)	pos.eq.ra;obs.field
PLATE	-	2dF plate number	meta.id;instr
N_STAR	-	Number of calibration stars observed	meta.number;src.calib
N_SPEC	-	Number of spectra observed	meta.number;spect
N_NIGHTS	-	Number of nights over which exposures were spread	meta.number
N_GOOD	-	Number of spectra with a good quality redshift, i.e. nQ >= 3	meta.number;spect
N_GAL_GOOD	-	Number of galaxy target spectra with a good quality redshift, i.e. nQ >= 3	meta.number;src
N_GAL	-	Number of galaxy targets observed	meta.number;src
N_EXP	-	Number of exposures	meta.number;obs.exposure
MEAN_SN	-	Mean S/N of spectra	stat.snr;spect
HEL_VC	km/s	Heliocentric velocity correction	phys.velocity;pos.heliocentric
HASTART	deg	Hour angle at start of first exposure	pos.eq.ha;time.start
HAEND	deg	Hour angle at end of last exposure	pos.eq.ha;time.end
GAL_COMPL	-	Redshift success rate among galaxy targets	arith.ratio;meta.number;src
FIELDID	-	ID of GAMA AAT field	meta.id;obs.field
DEC	deg	DEC of field centre (J2000)	pos.eq.dec;obs.field
DATE_Z	iso-8601	Date of original redshifting run	time.processing
DATE_OBS	iso-8601	UT date of observation	time.epoch;obs.exposure
CRCORVER	-	Runz version used for original redshifting run	meta.version;meta.software
CONFIG_FILE	-	Name of configuration file	meta.id;meta.file;instr.setup
COMPL	-	Redshift success rate	arith.ratio;meta.number;spect

AATRunzResults

name: AATRunzResults | type: CatalogueTable | Joe Liske [javascript protected email address] | version v08 |

This table contains the complete output of the redshifting code for all spectra released in DR2. Note that many spectra were redshifted more than once and this catalogue contains all duplications.

Address this table as gama_dr2.AATRunzResults

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z_FIN_ERR	-	Error of final selected redshift	stat.error;src.redshift
Z_FIN	-	Final selected redshift	src.redshift
ZX_ERR	-	Cross-correlation redshift error	-
ZX	-	Cross-correlation redshift	-
ZEM_ERR	-	Emission line redshift error	-
ZEM	-	Emission line redshift	-
Y_POSN	-	Fibre y position on plate	-
X_POSN	-	Fibre x position on plate	-
XCOR	-	Cross-correlation peak height	-
VSP	mag	Approximate V-band fibre mag with zeropoint 32	-
USER	-	Redshifter	meta.id
TEMP	-	Cross-correlation template	-
S_N	-	S/N of spectrum	stat.snr
SPMAG	mag	Unused	-
SPECID	-	ID of GAMA AAT spectrum	meta.id;spect
RUNZRESID	-	ID of runz output	meta.id;meta.main
RSP	mag	Approximate R-band fibre mag with zeropoint 32.3	-
RMAG	mag	Extinction corrected SDSS r-band Petrosian magnitude	phot.mag;em.opt.R
RAS	s	RA seconds	-
RAM	m	RA minutes	-
RAH	h	RA hours of spectrum (J2000)	-
RA	deg	RA of spectrum (J2000)	pos.eq.ra
QX	-	Cross-correlation redshift quality	-
QOP	-	User assigned quality of final selected redshift	meta.code.qual;src.redshift
QEM	-	Emission line redshift quality	-
QA	-	Automatic quality of final selected redshift	-
PLATE	-	Plate number	meta.id;instr
OBJECT	-	Object name	-
NEG	-	Total number of detected potential emission lines	-
NEB	-	Number of matching emission lines at best emission line redshift	-
IC_FLAG	-	Catalogue source(s) of matched GAMA object	meta.code.member
GAMA_NAME	-	Name of matched GAMA object	meta.id.cross;src
FLD	-	Unused	-
FIELDID	-	ID of GAMA AAT field	meta.id;obs.field
FIBRE	-	Fibre number	meta.id;instr
F	-	Flag indicating whether Z_FIN is different from automatic redshifts: 0 = equal to best auto redshift; 1 = not equal to best auto redshift; 2 = not equal to either auto redshifts	meta.code
DIST	arcsec	Distance between spectrum and matched GAMA object	pos.angDistance
DECS	s	DEC seconds	-
DECM	m	DEC minutes	-
DECD	deg	DEC degree of spectrum (J2000)	-
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
DATE_Z	iso-8601	Date of runz run	time.processing
DATE_OBS	-	UT date of observation	time.epoch;obs.exposure
COMMENT	-	User comment	meta.note
CCD	-	CCD number	meta.id;instr
CATAID	-	ID of matched GAMA object	meta.id.cross;src

AATSpecAll

name: AATSpecAll | type: CatalogueTable | Joe Liske [javascript protected email address] | version v08 |

This is a table of all GAMA AAT spectra included in DR2. Many targets were observed more than once by GAMA, and these duplications are retained here.

Address this table as gama_dr2.AATSpecAll

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z	-	Heliocentric redshift	src.redshift
Y_POSN	-	Fibre y position on plate	-
X_POSN	-	Fibre x position on plate	-
WMIN	A	Minimum wavelength of spectrum	em.wl;stat.min
WMAX	A	Maximum wavelength of spectrum	em.wl;stat.max
URL_IMG	-	URL of the spectrum`s image	meta.ref.url;meta.file
URL	-	URL of the spectrum	meta.ref.url;meta.file;meta.fits
S_N	-	S/N of spectrum	stat.snr
SPECID	-	ID of GAMA AAT spectrum	meta.id;meta.main
RA	deg	RA of spectrum (J2000)	pos.eq.ra
PROB	-	Probability that redshift is correct	stat.probability;src.redshift
PLATE	-	Plate number	meta.id;instr
NQ	-	Normalised redshift quality (use nQ > 2 for science)	meta.code.qual;src.redshift
IS_SBEST	-	Is this the best GAMA AAT spectrum of this object?	meta.code
IC_FLAG	-	Catalogue source(s) of matched GAMA object	meta.code.member
GAMA_NAME	-	Name of matched GAMA object	meta.id.cross;src
FILENAME	-	Full path and filename of the spectrum	meta.id;meta.file;meta.fits
FIELDID	-	ID of GAMA AAT field	meta.id;obs.field
FIBRE	-	Fibre number	meta.id;instr
DIST	arcsec	Distance between spectrum and matched GAMA object	pos.angDistance
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
DATE_OBS	iso-8601	UT date of observation	time.epoch;obs.exposure
CATAID	-	ID of matched GAMA object	meta.id.cross;src

AATSpecAllzAll

name: AATSpecAllzAll | type: CatalogueTable | Joe Liske [javascript protected email address] | version v08 |

Many GAMA AAT spectra were redshifted more than once. For each spectrum included in DR2 this table contains one line summarising all of the redshifting results for this spectrum, as well as listing the results of the analysis to determine the best redshift based on the reliabilities of the redshifters.

Address this table as gama_dr2.AATSpecAllzAll

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z4_Z	-	Possible redshift	-
Z4_PROB	-	Probability that ZX_Z is correct	-
Z4_N_Q4	-	Number of supporting Q=4 opinions	-
Z4_N_Q3	-	Number of supporting Q=3 opinions	-
Z4_N_Q2	-	Number of supporting Q=2 opinions	-
Z4_NQ	-	Normalised Q of ZX_Z	-
Z4_N	-	Number of opinions supporting ZX_Z	-
Z3_Z	-	Possible redshift	-
Z3_PROB	-	Probability that ZX_Z is correct	-
Z3_N_Q4	-	Number of supporting Q=4 opinions	-
Z3_N_Q3	-	Number of supporting Q=3 opinions	-
Z3_N_Q2	-	Number of supporting Q=2 opinions	-
Z3_NQ	-	Normalised Q of ZX_Z	-
Z3_N	-	Number of opinions supporting ZX_Z	-
Z2_Z	-	Possible redshift	-
Z2_PROB	-	Probability that ZX_Z is correct	-
Z2_N_Q4	-	Number of supporting Q=4 opinions	-
Z2_N_Q3	-	Number of supporting Q=3 opinions	-
Z2_N_Q2	-	Number of supporting Q=2 opinions	-
Z2_NQ	-	Normalised Q of ZX_Z	-
Z2_N	-	Number of opinions supporting ZX_Z	-
Z1_Z	-	Possible redshift	-
Z1_PROB	-	Probability that ZX_Z is correct	-
Z1_N_Q4	-	Number of supporting Q=4 opinions	-
Z1_N_Q3	-	Number of supporting Q=3 opinions	-
Z1_N_Q2	-	Number of supporting Q=2 opinions	-
Z1_NQ	-	Normalised Q of ZX_Z	-
Z1_N	-	Number of opinions supporting ZX_Z	-
SPECID	-	ID of GAMA AAT spectrum	meta.id;meta.main
RA	deg	RA of spectrum (J2000)	pos.eq.ra
Q1_PROB	-	Probability that the possibility Q=1 is correct	stat.probability
Q1_N_Q1	-	Number of supporting Q=1 opinions	meta.number
Q1_N_Q0	-	Number of supporting Q=0 opinions	meta.number
OP5_ZIDX	-	Index of possibility in above list that is supported by this redshift	-
OP5_Z	-	Redshift	-
OP5_RUNZRESID	-	ID of additional runz result in AATRunzResults	-
OP5_RS	-	Redshifter	-
OP5_Q	-	Q	-
OP4_ZIDX	-	Index of possibility in above list that is supported by this redshift	-
OP4_Z	-	Redshift	-
OP4_RUNZRESID	-	ID of additional runz result in AATRunzResults	-
OP4_RS	-	Redshifter	-
OP4_Q	-	Q	-
OP3_ZIDX	-	Index of possibility in above list that is supported by this redshift	-
OP3_Z	-	Redshift	-
OP3_RUNZRESID	-	ID of additional runz result in AATRunzResults	-
OP3_RS	-	Redshifter	-
OP3_Q	-	Q	-
OP2_ZIDX	-	Index of possibility in above list that is supported by this redshift	-
OP2_Z	-	Redshift	-
OP2_RUNZRESID	-	ID of additional runz result in AATRunzResults	-
OP2_RS	-	Redshifter	-
OP2_Q	-	Q	-
OP1_ZIDX	-	Index of possibility in above list that is supported by this redshift	-
OP1_Z	-	Original redshift	-
OP1_RUNZRESID	-	ID of original runz result in AATRunzResults	-
OP1_RS	-	Original redshifter	-
OP1_Q	-	Original Q	-
N_Z	-	Number of different redshifts	meta.number
N_OPQG	-	Number of opinions with Q >= 2	meta.number
N_OPQB	-	Number of opinions with Q < 2	meta.number
N_OP	-	Number of opinions for this spectrum	meta.number
IC_FLAG	-	Catalogue source(s) of matched GAMA object	meta.code.member
GAMA_NAME	-	Name of matched GAMA object	meta.id.cross;src
FIELDID	-	ID of GAMA AAT field	meta.id;obs.field
DIST	arcsec	Distance between spectrum and matched GAMA object	pos.angDistance
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
COMP_PROB	-	Probability that all offered possibilities are wrong	stat.probability
CATAID	-	ID of matched GAMA object	meta.id.cross;src
BEST_Z_N_Q4	-	Number of supporting Q=4 opinions	meta.number
BEST_Z_N_Q3	-	Number of supporting Q=3 opinions	meta.number
BEST_Z_N_Q2	-	Number of supporting Q=2 opinions	meta.number
BEST_Z_N_Q1	-	Number of supporting Q=1 opinions	meta.number
BEST_Z_N_Q0	-	Number of supporting Q=0 opinions	meta.number
BEST_Z_NQ	-	Normalised Q of the most probable possibility	meta.code.qual;src.redshift
BEST_Z_N	-	Number of opinions supporting the most probable possibility	meta.number
BEST_Z	-	Redshift of the most probable possibility	src.redshift
BEST_PROB	-	Probability that the most probable possibility is correct	stat.probability;src.redshift
BEST_IDX	-	Index of best possibility in the above list	-

LTSpecAll

name: LTSpecAll | type: CatalogueTable | Joe Liske [javascript protected email address] | version v01 |

This table lists a small number of spectra of fibre-bright targets collected by the GAMA team at the Liverpool Telescope (LT).

Address this table as gama_dr2.LTSpecAll

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z	-	Heliocentric redshift	src.redshift
WMIN	A	Minimum wavelength of spectrum	em.wl;stat.min
WMAX	A	Maximum wavelength of spectrum	em.wl;stat.max
URL_IMG	-	URL of the spectrum`s image	meta.ref.url;meta.file
URL	-	URL of the spectrum	meta.ref.url;meta.file;meta.fits
SPECID	-	ID of GAMA LT spectrum	meta.id;meta.main
RA	deg	RA of spectrum (J2000)	pos.eq.ra
PROB	-	Probability that redshift is correct	stat.probability;src.redshift
NQ	-	Normalised redshift quality (use nQ > 2 for science)	meta.code.qual;src.redshift
IS_SBEST	-	Is this the best GAMA LT spectrum of this object?	meta.code
IC_FLAG	-	Catalogue source(s) of matched GAMA object	meta.code.member
GAMA_NAME	-	Name of matched GAMA object	meta.id.cross;src
FILENAME	-	Full path and filename of the spectrum	meta.id;meta.file;meta.fits
DIST	arcsec	Distance between spectrum and matched GAMA object	pos.angDistance
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
CATAID	-	ID of matched GAMA object	meta.id.cross;src

SpecAll

name: SpecAll | type: CatalogueTable | Joe Liske [javascript protected email address] | version v08 |

This table lists all spectra that are available for GAMA objects included in DR2, including GAMA spectra and those from previous spectroscopic surveys (such as the SDSS). Duplicate observations of the same object are retained in this table (but a flag is provided to mark the spectrum that provided the best available redshift of a given object). Every spectrum listed in this table is available in the GAMA DR2 database.

Address this table as gama_dr2.SpecAll

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z	-	Heliocentric redshift	src.redshift
WMIN	A	Minimum wavelength of spectrum	em.wl;stat.min
WMAX	A	Maximum wavelength of spectrum	em.wl;stat.max
URL_IMG	-	URL of the spectrum`s image	meta.ref.url;meta.file
URL	-	URL of the spectrum	meta.ref.url;meta.file;meta.fits
SURVEY_CODE	-	Numerical code for originating survey	meta.code;meta.dataset
SURVEY	-	Survey this spectrum originated from	meta.dataset
SPECID	-	Unique ID of spectrum	meta.id;meta.main
RA	deg	RA of spectrum (J2000)	pos.eq.ra
PROB	-	Probability that redshift is correct	stat.probability;src.redshift
NQ	-	Normalised redshift quality (use nQ > 2 for science)	meta.code.qual;src.redshift
IS_SBEST	-	Is this the best spectrum of this GAMA object within the originating survey?	meta.code
IS_BEST	-	Is this the best spectrum of this GAMA object?	meta.code
IC_FLAG	-	Catalogue source(s) of matched GAMA object	meta.code.member
GAMA_NAME	-	Name of matched GAMA object	meta.id.cross;src
FILENAME	-	Full path and filename of the spectrum	meta.id;meta.file;meta.fits
DIST	arcsec	Distance between spectrum and matched GAMA object	pos.angDistance
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
CATAID	-	ID of matched GAMA object	meta.id.cross;src

SpecObj

name: SpecObj | type: CatalogueTable | Joe Liske [javascript protected email address] | version v08 |

This table lists each observed target included in DR2 and the spectrum that provides its best redshift (from GAMA or otherwise).

Address this table as gama_dr2.SpecObj

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
Z	-	Heliocentric redshift	src.redshift
WMIN	A	Minimum wavelength of spectrum	em.wl;stat.min
WMAX	A	Maximum wavelength of spectrum	em.wl;stat.max
URL_IMG	-	URL of the spectrum`s image	meta.ref.url;meta.file
URL	-	URL of the spectrum	meta.ref.url;meta.file;meta.fits
SURVEY_CODE	-	Numerical code for originating survey	meta.code;meta.dataset
SURVEY	-	Survey this spectrum originated from	meta.dataset
SPECID	-	ID of best matched spectrum	meta.id.cross;spect
RA	deg	RA of spectrum (J2000)	pos.eq.ra
PROB	-	Probability that redshift is correct	stat.probability;src.redshift
N_SPEC	-	Number of spectra available for this object	meta.number;spect
N_GAMA_SPEC	-	Number of GAMA spectra available for this object	meta.number;spect
NQ	-	Normalised redshift quality (use nQ > 2 for science)	meta.code.qual;src.redshift
IC_FLAG	-	Catalogue source(s) of GAMA object	meta.code.member
GAMA_NAME	-	Name of GAMA object	meta.id
FILENAME	-	Full path and filename of the spectrum	meta.id;meta.file;meta.fits
DIST	arcsec	Distance between GAMA object and best matched spectrum	pos.angDistance
DEC	deg	DEC of spectrum (J2000)	pos.eq.dec
CATAID	-	Unique ID of GAMA object	meta.id;meta.main

SersicPhotometry

name: SersicPhotometry | type: CatalogueGroup | Lee Kelvin [javascript protected email address] | version v07 |

read more

SersicPhotometry
2011-10-13
Lee Kelvin

The SersicPhotometry DMU produces a single-Sersic (1-component only)
fit to every GAMA DR2 object in each of the bands ugrizYJHK. This is
achieved by using SIGMA v0.9-0 (Structural Investigation of Galaxies
via Model Analysis) on SDSS and UKIDSS LAS imaging data. SIGMA is a
wrapper around several contemporary astronomy tools such as Source
Extractor (Bertin & Arnouts 1996), PSF Extractor (Bertin and Delorme,
priv. comm.) and GALFIT 3 (Peng et al. 2010), as well as analysis and
processing code writting in the open-source R programming language (R
Development Core Team, 2010). Please cite Kelvin et al. (2012) when
using data products from this DMU.

GALFIT is the workhorse fitting algorithm used within SIGMA. To
produce a model of a galaxy, GALFIT must be provided with suitable
starting parameters (such as size, magnitude, ellipticity, etc), an
appropriate PSF and cutouts of both the science data and any
associated weight maps. The cutouts are created from the GAMA v02
mosaics (available on the DR2 file server, swpim* files), with
physical initial conditions and the PSF provided by Source Extractor
and PSF Extractor, respectively. These programs are called and setup
automatically within the SIGMA script, their outputs reprocessed into
a form GALFIT is able to read, and fed into GALFIT. GALFIT uses a
simple downhill minimisation in order to minimise the global-chi^2 of
the model. Its outputs are analysed by SIGMA for any obvious errors,
and if found, an attempt at fixing them will automatically be made.

This DMU provides two tables: SersicCatAll and SersicCat. The former
contains a complete record of all of the outputs produced by
SIGMA. The latter table only contains those columns considered to be
most useful to the users. In other words, SersicCat contains an exact
subset of the columns in SersicCatAll.

Below are more detailed notes on several of the columns provided by
the SersicPhotometry DMU. The unique identifier for the
SersicPhotometry DMU is the CATAID (column 1) which refers to the GAMA
ID of an object. Null entries in SersicCat are labelled -9999. For
further details on the operation of SIGMA, please refer to Kelvin et
al. (2012).

##############################################################################

Dependencies:
InputCat TilingCat
Mosaics v02

##############################################################################

Potential zero-point offsets

Please see the notes of the table ApMatchedCat.

##############################################################################

SIGMA_INDEX

A unique identifier that the SIGMA code uses to identify each
galaxy. This remains a part of SIGMA for historical reasons.

##############################################################################

OBJNAME

SIGMA_INDEX, padded with leading zeroes to make the total length 8
characters long, and then prefixed with an S to construct the OBJNAME.
This name is more commonly used when saving modelling data within the
GAMA database.

##############################################################################

URL

Location of the directory on the file server containing all of the
input and output files used and produced by SIGMA for this galaxy. For
more details on the contents of this directory see the directory
description on the file server.

Please note that the world coordinate system (WCS) information in the
headers of the various fits files found in this directory is partially
incorrect. The pixel sizes are correct, but the absolute positions
implied by the WCS information in the header are incorrect.

##############################################################################

PSF_

All columns starting with 'PSF_' are outputs of the PSF Extractor
pipeline within SIGMA. These outputs are provided for reference only
to aid in the understanding of the final single-Sersic model. For more
information, see Kelvin et al. (2012).

##############################################################################

SEX_

All columns starting with 'SEX_' are outputs of the Source Extractor
pipeline within SIGMA. These Source Extractor outputs provided the
starting parameters for the GALFIT inputs used during minimisation.
These outputs are provided *for reference only* to aid in the
understanding of the final single-Sersic model. Unless there is a very
good reason to do so, these should not be used in scientific analyses.
Their GAL_ equivalents (see below) should be used instead. For more
information, see Kelvin et al. (2012).

##############################################################################

GAL_

All columns starting with 'GAL_' are final outputs of the GALFIT
pipeline within SIGMA. These GALFIT outputs provide the main output of
the SersicPhotometry DMU. For more information, see Kelvin et al. (2012).

##############################################################################

SEX_PA/GAL_PA

The position angle on the image recovered from Source Extractor and
GALFIT, respectively. This is defined from the positive x-axis of the
image (roughly aligned to west), increasing from zero anti-clockwise.

NOTE: SEX_PA goes from -90 to +90, whereas GAL_PA goes from 0 to +180,
however the definitions below still hold true at all times.

x-positive 0 degrees
y-positive 90 degrees
x-negative 180 degrees (equivalent to x-positive, redundant)
y-negative -90 degrees (equivalent to y-positive, redundant)

Unfortunately, due to an oversight, this DMU does *not* include
equivalent angles on the sky. However, an approximate on-sky angle can
be recovered as

SEX_PA_J2000_X = SEX_PA_X + (THETA_J2000 - THETA_IMAGE)
GAL_PA_J2000_X = GAL_PA_X + (THETA_J2000 - THETA_IMAGE)

where THETA_J2000 and THETA_IMAGE are the on-sky and on-image position
angles, respectively, listed in the table ApMatchedCat in the
ApMatchedPhotom DMU.

Despite this being only an approximation we recommend the use of
GAL_PA_J2000_X over THETA_J2000.

Note that SEX_PA_R in this DMU and THETA_IMAGE in the ApMatchedPhotom
DMU are not identical due to the procedures employed by these DMUs
being slightly different.

##############################################################################

GAL_FIT

The function combination chosen to model. Since the SersicPhotometry
is tasked with fitting a single-Sersic component to every galaxy, this
value will always be either 1 or -9999 (null). GAL_FITWORD gives the
corresponding word describing the combination chosen to model instead
of a number.

1 Sersic
2 Sersic + Exponential
3 Sersic + Sersic disk
4 Sersic bulge + Sersic disk (bulge/disk Re < 1, bulge/disk n > 1)
5 de Vaucouleurs + Exponential
-9999 Null

##############################################################################

GAL_RESULT

The end result of the GALFIT fitting stage.

CRASH An error has occurred causing the code to crash, usually due to bad
inputs caused by nearby star contamination or bad data.

ERROR A fatal error has occurred within GALFIT causing the code to
quit before minimisation. Usually caused by extremely bad inputs from
Source Extractor, or a bad PSF.

OKAY GALFIT completed successfully and SIGMA was happy enough with its
outputs to move on to the next galaxy in the catalogue. A flag
of OKAY does not mean that the result is perfect, i.e. physically
meaningful, it merely reflects that GALFIT was able to finish
without a major error occurring.

##############################################################################

GAL_QFLAG

This is a binary flag, and describes the quality of the final fit.
Flags may add together to produce a number higher than 1024.

0 fine
1 no object detected
2 compromised photometry (an object brighter than 0.75 mags fainter than
the primary lies within 4re)
4 magnitude between SEx and GALFIT differs by +-1 mag
8 crash/error
16 center migrated (> 5 pixels)
32 max. iterations (100)
64 large radius (ln[RAD/FLUXRAD]>2)
128 small radius (ln[RAD/FLUXRAD]<-2)
256 high Sersic index (n>10)
512 high ellipticity (e>0.95)
1024 bad chi2 (chi2<0.5 or chi2>2)

##############################################################################

GAL_GHFLAG

This is a binary flag, and describes the global fitting history
(i.e. non-Sersic specific).

Flags may add together to produce a number higher than 4. Multiple
runs cause the GHFLAG value to loop over and start at the next logical
binary operator (1,2,4,8,16,32...), and so many fitting runs can cause
GHFLAG to get very large. Example: the first run has a bad chi2 and
reached its maximum iterations, whereas the second run only had a bad
chi2. This would give 4+2 from run 1, and 32 from run 2, giving a
total GHFLAG of 38.

0 fine
1 crash/error
2 max iterations (100)
4 bad chi2 (chi2<0.5 or chi2>2)

##############################################################################

GAL_CHFLAG

This is a binary flag, and describes the component fitting history
(i.e. Ssersic specific).

Flags may add together to produce a number higher than 16. Multiple
runs cause the CHFLAG value to loop over and start at the next logical
binary operator (1,2,4,8,16,32...), and so many fitting runs can cause
CHFLAG to get very large. Example: the first run has a high
ellipticity and a high Sersic index, and the second run has a large
radius. This would give 16+8 from run 1, and 64 from run 2, giving a
total CHFLAG of 88.

0 fine
1 center migrated (> SEx re)
2 large radius (ln[RAD/FLUXRAD]>3)
4 small radius (ln[RAD/FLUXRAD]<-3)
8 high Sersic index (n>10)
16 high ellipticity (e>0.95)

##############################################################################

GAL_TYPE

GALFIT output type. Since the SersicPhotometry DMU is tasked with
fitting a single-Sersic component to every galaxy, this value will
always be either 1, 2, 5 or -9999 (null). GAL_TYPEWORD gives the
corresponding word describing the output type instead of a number.

1 crash
2 error
3 sky
4 psf
5 sersic
6 expdisk
7 edgedisk
8 ferrer
9 nuker
-9999 Null

##############################################################################

_MAG_

Magnitudes presented in this catalogue have not been corrected for the
effect of foreground Milky Way dust extinction. Should these
corrections be required, they can be obtained from the table
GalacticExtinction in the InputCat DMU.

All photometry is on the AB system.

##############################################################################

This DMU provides a single-component Sersic fit in each of the ugrizYJHK bands for every GAMA DR2 galaxy.

• Tables
• SersicCat
• SersicCatAll

SersicCat

name: SersicCat | type: CatalogueTable | Lee Kelvin [javascript protected email address] | version v07 |

This catalogue contains the most useful subset of the output of the SersicPhotometry DMU, using SIGMA v0.9-0 (Structural Investigation of Galaxies via Model Analysis) to generate a single-Sersic fit to every GAMA DR2 object. This table is an exact subset of the table SersicCatAll.

Address this table as gama_dr2.SersicCat

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
URL_R	-	URL of r-band png file	meta.ref.url;meta.file
URL_K	-	URL of K-band png file	meta.ref.url;meta.file
URL	-	URL of the object`s data dir	meta.ref.url;meta.file
SIGMA_INDEX	-	SIGMA Object ID (see notes)	meta.id
RA	deg	Right Ascension (J2000)	pos.eq.ra
PSF_FWHM_Z	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.opt
PSF_FWHM_Y	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.IR.NIR
PSF_FWHM_U	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.opt.U
PSF_FWHM_R	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.opt.R
PSF_FWHM_K	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.IR.K
PSF_FWHM_J	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.IR.J
PSF_FWHM_I	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.opt.I
PSF_FWHM_H	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.IR.H
PSF_FWHM_G	arcsec	PSFEx PSF FWHM	instr.det.psf;meta.modelled;em.opt
OBJNAME	-	SIGMA Object name (see notes)	meta.id
GAL_YCEN_Z	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.opt
GAL_YCEN_Y	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.IR.NIR
GAL_YCEN_U	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.opt.U
GAL_YCEN_R	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.opt.R
GAL_YCEN_K	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.IR.K
GAL_YCEN_J	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.IR.J
GAL_YCEN_I	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.opt.I
GAL_YCEN_H	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.IR.H
GAL_YCEN_G	pixel	pixel pos. of model in cutout (y)	pos.cartesian.y;meta.modelled;em.opt
GAL_XCEN_Z	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.opt
GAL_XCEN_Y	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.IR.NIR
GAL_XCEN_U	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.opt.U
GAL_XCEN_R	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.opt.R
GAL_XCEN_K	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.IR.K
GAL_XCEN_J	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.IR.J
GAL_XCEN_I	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.opt.I
GAL_XCEN_H	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.IR.H
GAL_XCEN_G	pixel	pixel pos. of model in cutout (x)	pos.cartesian.x;meta.modelled;em.opt
GAL_RE_Z	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt
GAL_RE_Y	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.NIR
GAL_RE_U	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt.U
GAL_RE_R	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt.R
GAL_RE_K	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.K
GAL_RE_J	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.J
GAL_RE_I	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt.I
GAL_RE_H	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.H
GAL_RE_G	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt
GAL_RE_C_Z	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt
GAL_RE_C_Y	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.NIR
GAL_RE_C_U	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt.U
GAL_RE_C_R	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt.R
GAL_RE_C_K	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.K
GAL_RE_C_J	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.J
GAL_RE_C_I	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt.I
GAL_RE_C_H	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.H
GAL_RE_C_G	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt
GAL_RA_Z	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt
GAL_RA_Y	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.NIR
GAL_RA_U	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt.U
GAL_RA_R	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt.R
GAL_RA_K	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.K
GAL_RA_J	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.J
GAL_RA_I	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt.I
GAL_RA_H	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.H
GAL_RA_G	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt
GAL_R90_Z	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt
GAL_R90_Y	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.NIR
GAL_R90_U	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt.U
GAL_R90_R	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt.R
GAL_R90_K	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.K
GAL_R90_J	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.J
GAL_R90_I	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt.I
GAL_R90_H	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.H
GAL_R90_G	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt
GAL_PA_Z	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt
GAL_PA_Y	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.NIR
GAL_PA_U	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt.U
GAL_PA_R	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt.R
GAL_PA_K	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.K
GAL_PA_J	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.J
GAL_PA_I	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt.I
GAL_PA_H	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.H
GAL_PA_G	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt
GAL_MU_E_Z	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_E_Y	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.NIR
GAL_MU_E_U	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt.U
GAL_MU_E_R	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt.R
GAL_MU_E_K	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.K
GAL_MU_E_J	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.J
GAL_MU_E_I	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt.I
GAL_MU_E_H	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.H
GAL_MU_E_G	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_E_AVG_Z	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_E_AVG_Y	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.NIR
GAL_MU_E_AVG_U	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt.U
GAL_MU_E_AVG_R	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt.R
GAL_MU_E_AVG_K	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.K
GAL_MU_E_AVG_J	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.J
GAL_MU_E_AVG_I	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt.I
GAL_MU_E_AVG_H	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.H
GAL_MU_E_AVG_G	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_0_Z	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt
GAL_MU_0_Y	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.NIR
GAL_MU_0_U	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt.U
GAL_MU_0_R	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt.R
GAL_MU_0_K	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.K
GAL_MU_0_J	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.J
GAL_MU_0_I	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt.I
GAL_MU_0_H	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.H
GAL_MU_0_G	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt
GAL_MAG_Z	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt
GAL_MAG_Y	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.NIR
GAL_MAG_U	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt.U
GAL_MAG_R	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt.R
GAL_MAG_K	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.K
GAL_MAG_J	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.J
GAL_MAG_I	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt.I
GAL_MAG_H	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.H
GAL_MAG_G	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt
GAL_MAG_10RE_Z	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt
GAL_MAG_10RE_Y	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.NIR
GAL_MAG_10RE_U	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt.U
GAL_MAG_10RE_R	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt.R
GAL_MAG_10RE_K	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.K
GAL_MAG_10RE_J	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.J
GAL_MAG_10RE_I	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt.I
GAL_MAG_10RE_H	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.H
GAL_MAG_10RE_G	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt
GAL_INDEX_Z	-	Sersic index	stat.fit.param;meta.modelled;em.opt
GAL_INDEX_Y	-	Sersic index	stat.fit.param;meta.modelled;em.IR.NIR
GAL_INDEX_U	-	Sersic index	stat.fit.param;meta.modelled;em.opt.U
GAL_INDEX_R	-	Sersic index	stat.fit.param;meta.modelled;em.opt.R
GAL_INDEX_K	-	Sersic index	stat.fit.param;meta.modelled;em.IR.K
GAL_INDEX_J	-	Sersic index	stat.fit.param;meta.modelled;em.IR.J
GAL_INDEX_I	-	Sersic index	stat.fit.param;meta.modelled;em.opt.I
GAL_INDEX_H	-	Sersic index	stat.fit.param;meta.modelled;em.IR.H
GAL_INDEX_G	-	Sersic index	stat.fit.param;meta.modelled;em.opt
GAL_ELLIP_Z	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.opt
GAL_ELLIP_Y	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.IR.NIR
GAL_ELLIP_U	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.opt.U
GAL_ELLIP_R	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.opt.R
GAL_ELLIP_K	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.IR.K
GAL_ELLIP_J	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.IR.J
GAL_ELLIP_I	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.opt.I
GAL_ELLIP_H	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.IR.H
GAL_ELLIP_G	-	ellipticity (1-(b/a))	src.ellipticity;meta.modelled;em.opt
GAL_DEC_Z	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.opt
GAL_DEC_Y	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.IR.NIR
GAL_DEC_U	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.opt.U
GAL_DEC_R	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.opt.R
GAL_DEC_K	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.IR.K
GAL_DEC_J	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.IR.J
GAL_DEC_I	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.opt.I
GAL_DEC_H	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.IR.H
GAL_DEC_G	deg	Declination as determined by GALFIT	pos.eq.dec;meta.modelled;em.opt
GAL_CHI2_Z	-	reduced Chi^2 of output model	stat.fit.goodness;em.opt
GAL_CHI2_Y	-	reduced Chi^2 of output model	stat.fit.goodness;em.IR.NIR
GAL_CHI2_U	-	reduced Chi^2 of output model	stat.fit.goodness;em.opt.U
GAL_CHI2_R	-	reduced Chi^2 of output model	stat.fit.goodness;em.opt.R
GAL_CHI2_K	-	reduced Chi^2 of output model	stat.fit.goodness;em.IR.K
GAL_CHI2_J	-	reduced Chi^2 of output model	stat.fit.goodness;em.IR.J
GAL_CHI2_I	-	reduced Chi^2 of output model	stat.fit.goodness;em.opt.I
GAL_CHI2_H	-	reduced Chi^2 of output model	stat.fit.goodness;em.IR.H
GAL_CHI2_G	-	reduced Chi^2 of output model	stat.fit.goodness;em.opt
FILENAME	-	Full path to object`s data directory	meta.id;meta.file
DEC	deg	Declination (J2000)	pos.eq.dec
CATAID	-	GAMA Object ID	meta.id

SersicCatAll

name: SersicCatAll | type: CatalogueTable | Lee Kelvin [javascript protected email address] | version v07 |

This catalogue contains the complete output of the SersicPhotometry DMU, using SIGMA v0.9-0 (Structural Investigation of Galaxies via Model Analysis) to generate a single-Sersic fit to every GAMA DR2 object.

Address this table as gama_dr2.SersicCatAll

Name	Unit	Description	UCD (hover for description)
Name	Unit	Description	UCD
GAL_RUN_H	-	number of GALFIT runs required	meta.number;em.IR.H
GAL_RUN_G	-	number of GALFIT runs required	meta.number;em.opt
GAL_RE_Z	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt
GAL_RE_Y	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.NIR
GAL_RE_U	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt.U
GAL_RE_R	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt.R
GAL_RE_K	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.K
GAL_RE_J	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.J
GAL_RE_I	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt.I
GAL_RE_H	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.IR.H
GAL_RE_G	arcsec	effective radius (hl rad) (semi-major)	phys.angSize;meta.modelled;em.opt
GAL_RE_ERR_Z	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_Y	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_U	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_R	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_K	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_J	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_I	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_H	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_ERR_G	arcsec	GALFIT error on re	phys.angSize;stat.error;meta.modelled...
GAL_RE_C_Z	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt
GAL_RE_C_Y	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.NIR
GAL_RE_C_U	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt.U
GAL_RE_C_R	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt.R
GAL_RE_C_K	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.K
GAL_RE_C_J	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.J
GAL_RE_C_I	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt.I
GAL_RE_C_H	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.IR.H
GAL_RE_C_G	arcsec	circularised effective radius	phys.angSize;meta.modelled;em.opt
GAL_RESULT_Z	-	GALFIT run result (see notes)	em.opt
GAL_RESULT_Y	-	GALFIT run result (see notes)	em.IR.NIR
GAL_RESULT_U	-	GALFIT run result (see notes)	em.opt.U
GAL_RESULT_R	-	GALFIT run result (see notes)	em.opt.R
GAL_RESULT_K	-	GALFIT run result (see notes)	em.IR.K
GAL_RESULT_J	-	GALFIT run result (see notes)	em.IR.J
GAL_RESULT_I	-	GALFIT run result (see notes)	em.opt.I
GAL_RESULT_H	-	GALFIT run result (see notes)	em.IR.H
GAL_RESULT_G	-	GALFIT run result (see notes)	em.opt
GAL_RA_Z	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt
GAL_RA_Y	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.NIR
GAL_RA_U	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt.U
GAL_RA_R	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt.R
GAL_RA_K	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.K
GAL_RA_J	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.J
GAL_RA_I	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt.I
GAL_RA_H	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.IR.H
GAL_RA_G	deg	Right Ascension as determined by GALFIT	pos.eq.ra;meta.modelled;em.opt
GAL_R90_Z	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt
GAL_R90_Y	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.NIR
GAL_R90_U	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt.U
GAL_R90_R	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt.R
GAL_R90_K	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.K
GAL_R90_J	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.J
GAL_R90_I	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt.I
GAL_R90_H	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.IR.H
GAL_R90_G	arcsec	rad containing 90% of total light (sma)	phys.angSize;meta.modelled;em.opt
GAL_QFLAG_Z	-	quality flag (see notes)	meta.code.qual;em.opt
GAL_QFLAG_Y	-	quality flag (see notes)	meta.code.qual;em.IR.NIR
GAL_QFLAG_U	-	quality flag (see notes)	meta.code.qual;em.opt.U
GAL_QFLAG_R	-	quality flag (see notes)	meta.code.qual;em.opt.R
GAL_QFLAG_K	-	quality flag (see notes)	meta.code.qual;em.IR.K
GAL_QFLAG_J	-	quality flag (see notes)	meta.code.qual;em.IR.J
GAL_QFLAG_I	-	quality flag (see notes)	meta.code.qual;em.opt.I
GAL_QFLAG_H	-	quality flag (see notes)	meta.code.qual;em.IR.H
GAL_QFLAG_G	-	quality flag (see notes)	meta.code.qual;em.opt
GAL_PA_Z	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt
GAL_PA_Y	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.NIR
GAL_PA_U	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt.U
GAL_PA_R	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt.R
GAL_PA_K	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.K
GAL_PA_J	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.J
GAL_PA_I	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt.I
GAL_PA_H	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.IR.H
GAL_PA_G	deg	position angle (x+, CCW) (see notes)	pos.posAng;meta.modelled;em.opt
GAL_PA_ERR_Z	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_Y	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_U	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_R	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_K	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_J	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_I	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_H	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_PA_ERR_G	deg	GALFIT error on position angle	pos.posAng;stat.error;meta.modelled;e...
GAL_MU_E_Z	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_E_Y	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.NIR
GAL_MU_E_U	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt.U
GAL_MU_E_R	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt.R
GAL_MU_E_K	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.K
GAL_MU_E_J	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.J
GAL_MU_E_I	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt.I
GAL_MU_E_H	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.IR.H
GAL_MU_E_G	mag/arcsec^2	effective surface brightness at re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_E_AVG_Z	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_E_AVG_Y	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.NIR
GAL_MU_E_AVG_U	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt.U
GAL_MU_E_AVG_R	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt.R
GAL_MU_E_AVG_K	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.K
GAL_MU_E_AVG_J	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.J
GAL_MU_E_AVG_I	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt.I
GAL_MU_E_AVG_H	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.IR.H
GAL_MU_E_AVG_G	mag/arcsec^2	effective surface brightness within re	phot.mag.sb;meta.modelled;em.opt
GAL_MU_0_Z	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt
GAL_MU_0_Y	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.NIR
GAL_MU_0_U	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt.U
GAL_MU_0_R	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt.R
GAL_MU_0_K	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.K
GAL_MU_0_J	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.J
GAL_MU_0_I	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt.I
GAL_MU_0_H	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.IR.H
GAL_MU_0_G	mag/arcsec^2	central surface brightness	phot.mag.sb;meta.modelled;em.opt
GAL_MAG_Z	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt
GAL_MAG_Y	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.NIR
GAL_MAG_U	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt.U
GAL_MAG_R	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt.R
GAL_MAG_K	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.K
GAL_MAG_J	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.J
GAL_MAG_I	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt.I
GAL_MAG_H	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.IR.H
GAL_MAG_G	mag	magnitude of Sersic model	phot.mag;meta.modelled;em.opt
GAL_MAG_ERR_Z	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em.opt
GAL_MAG_ERR_Y	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em....
GAL_MAG_ERR_U	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em....
GAL_MAG_ERR_R	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em....
GAL_MAG_ERR_K	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em....
GAL_MAG_ERR_J	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em....
GAL_MAG_ERR_I	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em....
GAL_MAG_ERR_H	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em....
GAL_MAG_ERR_G	mag	GALFIT error on magnitude	phot.mag;stat.error;meta.modelled;em.opt
GAL_MAG_10RE_Z	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt
GAL_MAG_10RE_Y	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.NIR
GAL_MAG_10RE_U	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt.U
GAL_MAG_10RE_R	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt.R
GAL_MAG_10RE_K	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.K
GAL_MAG_10RE_J	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.J
GAL_MAG_10RE_I	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt.I
GAL_MAG_10RE_H	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.IR.H
GAL_MAG_10RE_G	mag	magnitude of model, truncated at 10*re	phot.mag;meta.modelled;em.opt
GAL_ITERATIONS_Z	-	number of iterations for convergence	meta.number;em.opt
GAL_ITERATIONS_Y	-	number of iterations for convergence	meta.number;em.IR.NIR
GAL_ITERATIONS_U	-	number of iterations for convergence	meta.number;em.opt.U
GAL_ITERATIONS_R	-	number of iterations for convergence	meta.number;em.opt.R
GAL_ITERATIONS_K	-	number of iterations for convergence	meta.number;em.IR.K
GAL_ITERATIONS_J	-	number of iterations for convergence	meta.number;em.IR.J
GAL_ITERATIONS_I	-	number of iterations for convergence	meta.number;em.opt.I
GAL_ITERATIONS_H	-	number of iterations for convergence	meta.number;em.IR.H
GAL_ITERATIONS_G	-	number of iterations for convergence	meta.number;em.opt
GAL_INDEX_Z	-	Sersic index	stat.fit.param;meta.modelled;em.opt
GAL_INDEX_Y	-	Sersic index	stat.fit.param;meta.modelled;em.IR.NIR
GAL_INDEX_U	-	Sersic index	stat.fit.param;meta.modelled;em.opt.U