Schema Browser

This table contains F-stars used for secondary flux calibration and point spread function measurement for SAMI Galaxy Survey observations within the cluster regions. The stars with CATIDs starting with 888 are taken from SDSS, while the stars starting with 999 are from VST ATLAS. Priorities are set based on the magnitude range of the targets, with fainter stars having lower priority.

This table contains general properties of SAMI galaxies. It includes all galaxies that were potential targets for the main SAMI Galaxy Survey (both primary and secondary targets) in the GAMA regions. It does not contain filler targets. See Bryant et al. (2015) for details of the SAMI Galaxy Survey sample selection.

The majority of measurements are drawn from the GAMA Survey (Driver et al. 2009). RA, Dec (columns RA_OBJ and DEC_OBJ) and Petrosian magnitude are taken from TilingCatv29 (Baldry et al. 2010). Colour and Kron magnitude are taken from ApMatchedCatv03 (Hill et al., 2011). Redshift information is drawn from DistanceFramesv08 (Baldry et al. 2012). Effective radius, surface brightness, ellipticity and position angle are taken from SersicCatAllv07 (Kelvin et al. 2012). The position angle defined within SersicCatAllv07 is defined with respect to the (x,y) coordinates of the image, so is approximately 90 degrees offset from a standard from North through East position angle. To correct for this we use the following:

PA = GAL_PA_R + (THETA_J2000 - THETA_IMAGE)

where GAL_PA_R is the (x,y) referenced PA in the r-band from the SersicCatAllv07 catalogue, and THETA_J2000 and THETA_IMAGE are the position angle in the sky and image respectively taken from ApMatchedCatv03. This is an update from previous versions of the SAMI input catalogue that simply contained GAL_PA_R as the PA coloumn.

Absolute magnitude is taken from StellarMassesv08 (Taylor et al. 2011). Extinction information is taken from GalacticExtinctionv02. Columns RA_IFU and DEC_IFU list nominal IFU coordinates that are in a small number of cases different from the object coordinates.

Priority and quality flags SURV_SAMI and BAD_CLASS are defined by Bryant et al. (2015).

This table contains estimates for the surface density local to SAMI targets (both in the GAMA and cluster regions), along with the associated uncertainties. The surface density is estimated using the distance to the fifth nearest neighbour, which is drawn from a density-defining population of galaxies with absolute magnitude M_r < -18.6 mag, and within a velocity +\-1000km/s with respect to the redshift of the SAMI target of interest. A second density esimtate determined using a density defining population with M_r < -19 mag is also included, which also allows a density estimate for those secondary targets with z_tonry > 0.1.

The measurements that provide the density-defining population of galaxies are drawn from several catalogues: The redshift and photometric measurements in the cluster regions are taken from the SAMI Cluster Redshift Survey (Owers et al. 2017) with k-corrections derived using the calc_kcor.py software of Chilingarian et al. (2010). The GAMA measurements contain data from the GAMA II catalogues DistancesFramesv12 (which is itself based on TilingCatv43), kCorrectionsv04 and the GAMA II completeness masks. Where required and possible, the density estimates are corrected for spectroscopic incompleteness, and for the impact of survey edges. For both the GAMA and cluster regions, angular separations are converted to physical distances assuming a standard LCDM cosmology with H_0 = 70 km/s/Mpc, O_M = 0.3, O_L = 0.7.

Below we describe the meanings of the various problem-indicating SurfaceDensityFlag values. It is recommended that only SurfaceDensity estimates where SurfaceDensityFlag <=1 are used.

SurfaceDensityFlag = 0: SurfaceDensity is exact.

SurfaceDensityFlag = 1: SurfaceDensity calculated using AreaCorrection.

SurfaceDensityFlag = 2: Fewer than N galaxies are found but a nearer galaxy is within the distance to the nearest angular survey edge. The surface density is calculated using the distance to the nearer galaxy and hence SurfaceDensity is an upper limit.

SurfaceDensityFlag = 4: No neighbours found among the density defining population within the distance to the nearest angular survey edge. SurfaceDensity is calculated as 1 / (Pi * DistanceToEdge^2).

SurfaceDensityFlag = 8: The galaxy lies inside a bright star exclusion region (completeness flag set to -1) or outside of the GAMA survey boundary (as defined by the completeness mask, completeness flag = -0.5). SurfaceDensity cannot be determined accurately and is set to NaN.

SurfaceDensityFlag = 9: Target lies outside the redshift limits 0.002 < z_tonry < 0.1 or 0.002 < z_tonry < 0.12.

This table contains the visual classification for all SAMI galaxies (both GAMA and cluster regions) included in DR3.

Visual classification has been performed as follows. Each member of the WG has independently performed visual classification on either SDSS DR9 or VST RGB images following a classification scheme similar to the one adopted by GAMA for their visual classification (Kelvin et al. 2014). Briefly, galaxies are classified following a step-by-step classification procedure. First, it is decided whether the galaxy is an early- or late-type system according to the presence/absence of disk/spiral structures and signs of star formation. Subsequently, the presence of distinct structural components (i.e., bulge/disk) in the galaxy is visually determined. Early-types with just a bulge are classical elliptical systems, whereas early-types with disks are S0s. Similarly, late-type galaxies with a bulge component are early-type spiral systems (eS: Sa-Sb), whereas bulge-less late-type galaxies are late-type spirals/Irregulars (lS). In the few cases for which a visual classification is impossible, the type ? is assigned.

It is important to remember that, while the material used for GAMA galaxies always comes from SDSS, we have clusters only covered by VST. The WG ran a few tests to ensure that the visual classifications based on SDSS and VST data are consistent, however care must be taken when combining the two datasets as differences by half or one type may just be due to the different material used.

This table contains general properties of SAMI galaxies. It includes all galaxies that were potential targets for the main SAMI Galaxy Survey (both primary and secondary targets) in the Cluster regions. It does not contain filler targets. See Bryant et al. (2015) and Owers et al. (2017) for details of the SAMI Galaxy Survey sample selection and the definitions used for the target priorities.

The majority of measurements are drawn from the SAMI Cluster Redshift Survey (Owers et al. 2017). Effective radius, ellipticity and position angle are taken from the Sersic fits outlined in Owers et al. 2019. Surface brightness measurements are derived from the Sersic fit parameters from Owers et al. (2019). Absolute magnitude is determined from extinction- and K-corrected r_auto magnitudes, where the k-correction is determined using the calc_kcor.py software of Chilingarian et al. (2010). The luminosity distance is determined using the cluster redshift listed in Owers et al. (2017).

This table contains F-stars used for secondary flux calibration and point spread function measurement for SAMI Galaxy Survey observations within the GAMA regions. Photometry and positions taken from SDSS DR7. Priorities are set based on the magnitude range of the targets, with fainter stars having lower priority.