MPA-JHU catalogue (dr1.MPA)

The table has 100 rows, 40 columns.

Description

This table contains properties for CAVITY galaxies, directly taken from the MPA-JHU (Max-Planck-Institute for Astrophysics-John Hopkins University) Catalogue. Further information corresponding to the data present in this table can be consulted in the following data models:

Notes:

All the fluxes reported here are computed from Gaussian fits to continuum subtracted data. Note that the fit is done simultaneously to all the lines so deblending happens automatically. For more information check [galSpecLine].

References:

Columns

Name	Type	UCD	Unit	Description
galaxy	int	meta.id meta.main		CAVITY ID
bestObjID	char	meta.id meta.corr		Unique ID in SDSS database
specObjID	char	meta.id meta.corr		Spectral ID in SDSS database
sn_median	float	stat.snr stat.median		Median S/N per pixel of the whole spectrum [from galSpecInfo]
oii_3726_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	[OII]3726 Flux from Gaussian fit to continuum subtracted data.
oii_3726_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in oii_3726_flux
oii_3729_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	[OII]3729 Flux from Gaussian fit to continuum subtracted data.
oii_3729_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in oii_3729_flux
h_beta_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Hβ Flux from Gaussian fit to continuum subtracted data.
h_beta_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in the h_beta_flux
oiii_5007_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	[OIII]5007 Flux from Gaussian fit to continuum subtracted data.
oiii_5007_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in oiii_5007_flux
h_alpha_cont	float	phot.flux spect.continuum	[10⁻¹⁷·erg·cm⁻²·s⁻¹·Å⁻¹]	Continuum at line center from 200 pixel median smoothing of the emission-line subtracted continuum
h_alpha_cont_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹·Å⁻¹]	Uncertainty in h_alpha_cont
h_alpha_reqw	float	spect.line.eqWidth spect.continuum	Å	The equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed in [galSpecLine] (emission is negative). In this case the continuum comes from a running 200 pixel median and does not properly account for stellar absorption. In general the EQW measurements provide a better measure of the true equivalent width. The purpose of this measurement is to help characterize the stellar absorption effecting the line. (EW_stellar = REQW – EQW)
h_alpha_reqw_err	float	stat.error spect.line.eqWidth	Å	Uncertainty in h_alpha_reqw
h_alpha_eqw	float	spect.line.eqWidth spect.continuum	Å	The equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed in [galSpecLine] (emission is negative). This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (i.e., NII & Hα)
h_alpha_eqw_err	float	stat.error spect.line.eqWidth	Å	Uncertainty in h_alpha_eqw
h_alpha_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Hα Flux from Gaussian fit to continuum subtracted data.
h_alpha_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in h_alpha_flux
nii_6584_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	[NII]6584 Flux from Gaussian fit to continuum subtracted data.
nii_6584_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in nii_6584_flux
sii_6717_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	[SII]6717 Flux from Gaussian fit to continuum subtracted data.
sii_6717_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in sii_6717_flux
sii_6731_flux	float	phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	[SII]6731 Flux from Gaussian fit to continuum subtracted data.
sii_6731_flux_err	float	stat.error phot.flux	[10⁻¹⁷·erg·cm⁻²·s⁻¹]	Uncertainty in sii_6731_flux
oh_p16	float	phys.abund stat.median		The 16th percentile of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details. [from galSpecExtra]
oh_p50	float	phys.abund stat.median		The median estimate of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details. [from galSpecExtra]
oh_p84	float	phys.abund stat.median		The 84th percentile of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details. [from galSpecExtra]
lgm_tot_p16	float	phys.mass stat.median	[log(M☉)]	The 16th percentile of the Log total stellar mass PDF using model photometry. [from galSpecExtra]
lgm_tot_p50	float	phys.mass stat.median	[log(M☉)]	The median estimate of the Log total stellar mass PDF using model photometry. [from galSpecExtra]
lgm_tot_p84	float	phys.mass stat.median	[log(M☉)]	The 84th percentile of the Log total stellar mass PDF using model photometry. [from galSpecExtra]
sfr_tot_p16	float	phys.SFR stat.median	[log(M☉·yr⁻¹)]	The 16th percentile of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. [from galSpecExtra]
sfr_tot_p50	float	phys.SFR stat.median	[log(M☉·yr⁻¹)]	The median estimate of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. [from galSpecExtra]
sfr_tot_p84	float	phys.SFR stat.median	[log(M☉·yr⁻¹)]	The 84th percentile of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. [from galSpecExtra]
specsfr_tot_p16	float	phys.SFR stat.median	[log(yr⁻¹)]	The 16th percentile of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. [from galSpecExtra]
specsfr_tot_p50	float	phys.SFR stat.median	[log(yr⁻¹)]	The median estimate of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. [from galSpecExtra]
specsfr_tot_p84	float	phys.SFR stat.median	[log(yr⁻¹)]	The 84th percentile of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. [from galSpecExtra]
d4000_n	float	phot.flux.density arith.ratio		4000AA break, Balogh et al (1999) definition. [from galSpecIndx]
d4000_n_err	float	stat.error phot.flux.density arith.ratio		Uncertainty in d4000_n