MPAJHU catalogue (dr1.MPA)
The table has 100 rows, 40 columns.
Description
This table contains properties for CAVITY galaxies, directly taken from the MPAJHU (MaxPlanckInstitute for AstrophysicsJohn Hopkins University) Catalogue. Further information corresponding to the data present in this table can be consulted in the following data models:
 galSpecInfo (or alternative link);
 galSpecLine (or alternative link);
 galSpecExtra (or alternative link).
 galSpecIndx (or alternative link).
Notes:
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 emissionline 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 continuumsubtracted 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 continuumsubtracted 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 