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Table: sdss_dr13.galspecline_dr8
(The bold columns are indexed columns)
Column NameDescriptionDatatype
ariii7135_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
ariii7135_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
ariii7135_cont_errError in the continuum computed from the variance in the band passREAL
ariii7135_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
ariii7135_eqw_errError in the equivalent width described aboveREAL
ariii7135_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
ariii7135_flux_errError in the fluxREAL
ariii7135_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
ariii7135_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
ariii7135_reqw_errError in the equivalent width described aboveREAL
ariii7135_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
ariii7135_seqw_errError in the aboveREAL
ca_h_absCaH absorption lineREAL
ca_h_abs_modelCaH absorption line best fit modelREAL
ca_k_absCaK absorption lineREAL
ca_k_abs_modelCaK absorption line best fit modelREAL
fiberidFiber IDSMALLINT
h_alpha_absH alpha absoption lineREAL
h_alpha_abs_modelH alpha absorption line best fit modelREAL
h_alpha_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
h_alpha_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
h_alpha_cont_errError in the continuum computed from the variance in the band passREAL
h_alpha_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
h_alpha_eqw_errError in the equivalent width described aboveREAL
h_alpha_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
h_alpha_flux_errError in the fluxREAL
h_alpha_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
h_alpha_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
h_alpha_reqw_errError in the equivalent width described aboveREAL
h_alpha_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
h_alpha_seqw_errError in the aboveREAL
h_beta_absH beta absorption lineREAL
h_beta_abs_modelH beta absorption line best fit modelREAL
h_beta_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
h_beta_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
h_beta_cont_errError in the continuum computed from the variance in the band passREAL
h_beta_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
h_beta_eqw_errError in the equivalent width described aboveREAL
h_beta_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
h_beta_flux_errError in the fluxREAL
h_beta_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
h_beta_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
h_beta_reqw_errError in the equivalent width described aboveREAL
h_beta_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
h_beta_seqw_errError in the aboveREAL
h_delta_absH delta absorption lineREAL
h_delta_abs_modelH delta absorption line best fit modelREAL
h_delta_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
h_delta_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
h_delta_cont_errError in the continuum computed from the variance in the band passREAL
h_delta_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
h_delta_eqw_errError in the equivalent width described aboveREAL
h_delta_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
h_delta_flux_errError in the fluxREAL
h_delta_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
h_delta_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
h_delta_reqw_errError in the equivalent width described aboveREAL
h_delta_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
h_delta_seqw_errError in the aboveREAL
h_gamma_absH gamma absorption lineREAL
h_gamma_abs_modelH gamma absorption line best fit modelREAL
h_gamma_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
h_gamma_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
h_gamma_cont_errError in the continuum computed from the variance in the band passREAL
h_gamma_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
h_gamma_eqw_errError in the equivalent width described aboveREAL
h_gamma_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
h_gamma_flux_errError in the fluxREAL
h_gamma_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
h_gamma_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
h_gamma_reqw_errError in the equivalent width described aboveREAL
h_gamma_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
h_gamma_seqw_errError in the aboveREAL
hei_5876_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
hei_5876_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
hei_5876_cont_errError in the continuum computed from the variance in the band passREAL
hei_5876_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
hei_5876_eqw_errError in the equivalent width described aboveREAL
hei_5876_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
hei_5876_flux_errError in the fluxREAL
hei_5876_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
hei_5876_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
hei_5876_reqw_errError in the equivalent width described aboveREAL
hei_5876_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
hei_5876_seqw_errError in the aboveREAL
mjdModified Julian DateINTEGER
na_d_absNaD absorption lineREAL
na_d_abs_modelNaD absorption line best fit modelREAL
neiii_3869_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
neiii_3869_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
neiii_3869_cont_errError in the continuum computed from the variance in the band passREAL
neiii_3869_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
neiii_3869_eqw_errError in the equivalent width described aboveREAL
neiii_3869_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
neiii_3869_flux_errError in the fluxREAL
neiii_3869_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
neiii_3869_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
neiii_3869_reqw_errError in the equivalent width described aboveREAL
neiii_3869_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
neiii_3869_seqw_errError in the aboveREAL
nii_6548_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
nii_6548_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
nii_6548_cont_errError in the continuum computed from the variance in the band passREAL
nii_6548_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
nii_6548_eqw_errError in the equivalent width described aboveREAL
nii_6548_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
nii_6548_flux_errError in the fluxREAL
nii_6548_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
nii_6548_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
nii_6548_reqw_errError in the equivalent width described aboveREAL
nii_6548_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
nii_6548_seqw_errError in the aboveREAL
nii_6584_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
nii_6584_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
nii_6584_cont_errError in the continuum computed from the variance in the band passREAL
nii_6584_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
nii_6584_eqw_errError in the equivalent width described aboveREAL
nii_6584_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
nii_6584_flux_errError in the fluxREAL
nii_6584_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
nii_6584_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
nii_6584_reqw_errError in the equivalent width described aboveREAL
nii_6584_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
nii_6584_seqw_errError in the aboveREAL
oi_6300_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
oi_6300_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
oi_6300_cont_errError in the continuum computed from the variance in the band passREAL
oi_6300_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
oi_6300_eqw_errError in the equivalent width described aboveREAL
oi_6300_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
oi_6300_flux_errError in the fluxREAL
oi_6300_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
oi_6300_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
oi_6300_reqw_errError in the equivalent width described aboveREAL
oi_6300_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
oi_6300_seqw_errError in the aboveREAL
oii_3726_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
oii_3726_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
oii_3726_cont_errError in the continuum computed from the variance in the band passREAL
oii_3726_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
oii_3726_eqw_errError in the equivalent width described aboveREAL
oii_3726_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
oii_3726_flux_errError in the fluxREAL
oii_3726_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
oii_3726_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
oii_3726_reqw_errError in the equivalent width described aboveREAL
oii_3726_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
oii_3726_seqw_errError in the aboveREAL
oii_3729_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
oii_3729_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
oii_3729_cont_errError in the continuum computed from the variance in the band passREAL
oii_3729_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
oii_3729_eqw_errError in the equivalent width described aboveREAL
oii_3729_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
oii_3729_flux_errError in the fluxREAL
oii_3729_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
oii_3729_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
oii_3729_reqw_errError in the equivalent width described aboveREAL
oii_3729_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
oii_3729_seqw_errError in the aboveREAL
oii_chi2chi^2 of the fit to the [O II] line in free fitREAL
oii_fluxThe flux of the [O II] doublet from a free fit.REAL
oii_flux_errThe estimated uncertainty on OII_FLUXREAL
oii_sigmaThe width of the [O II] line in a free fit (ie. not tied to other emission lines)REAL
oii_voffThe velocity offset of the [O II] doublet from a free fitREAL
oiii_4363_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
oiii_4363_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
oiii_4363_cont_errError in the continuum computed from the variance in the band passREAL
oiii_4363_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
oiii_4363_eqw_errError in the equivalent width described aboveREAL
oiii_4363_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
oiii_4363_flux_errError in the fluxREAL
oiii_4363_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
oiii_4363_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
oiii_4363_reqw_errError in the equivalent width described aboveREAL
oiii_4363_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
oiii_4363_seqw_errError in the aboveREAL
oiii_4959_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
oiii_4959_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
oiii_4959_cont_errError in the continuum computed from the variance in the band passREAL
oiii_4959_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
oiii_4959_eqw_errError in the equivalent width described aboveREAL
oiii_4959_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
oiii_4959_flux_errError in the fluxREAL
oiii_4959_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
oiii_4959_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
oiii_4959_reqw_errError in the equivalent width described aboveREAL
oiii_4959_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
oiii_4959_seqw_errError in the aboveREAL
oiii_5007_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
oiii_5007_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
oiii_5007_cont_errError in the continuum computed from the variance in the band passREAL
oiii_5007_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
oiii_5007_eqw_errError in the equivalent width described aboveREAL
oiii_5007_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
oiii_5007_flux_errError in the fluxREAL
oiii_5007_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
oiii_5007_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
oiii_5007_reqw_errError in the equivalent width described aboveREAL
oiii_5007_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
oiii_5007_seqw_errError in the aboveREAL
oiii_chi2chi^2 of the fit to the [O III]5007 line in free fitREAL
oiii_fluxThe flux of the [O III]5007 line from a free fit.REAL
oiii_flux_errThe estimated uncertainty on OIII_FLUXREAL
oiii_sigmaThe width of the [O III]5007 line in a free fit (ie. not tied to other emission lines)REAL
oiii_voffThe velocity offset of the [O III]5007 line from a free fitREAL
plateidPlate IDSMALLINT
sigma_balmerVelocity dispersion (sigma not FWHM) measured simultaneously in all of the Balmer linesREAL
sigma_balmer_errError in the aboveREAL
sigma_forbiddenVelocity dispersion (sigma not FWHM) measured simultaneously in all the forbidden linesREAL
sigma_forbidden_errError in the aboveREAL
sii_6717_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
sii_6717_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
sii_6717_cont_errError in the continuum computed from the variance in the band passREAL
sii_6717_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
sii_6717_eqw_errError in the equivalent width described aboveREAL
sii_6717_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
sii_6717_flux_errError in the fluxREAL
sii_6717_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
sii_6717_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
sii_6717_reqw_errError in the equivalent width described aboveREAL
sii_6717_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
sii_6717_seqw_errError in the aboveREAL
sii_6731_chisqReduced chi-squared of the line fit over the bandpass used for the EW measurementREAL
sii_6731_contContinuum at line center from 200 pixel median smoothing of the emission-line subtracted continuumREAL
sii_6731_cont_errError in the continuum computed from the variance in the band passREAL
sii_6731_eqwThe equivalent width of the CB08 continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison is negative) . This properly takes into account stellar absorption. Note that it will not be correct in the case of blended lines (ie NII & H-alpha) -- instead use FLUX/CONT.REAL
sii_6731_eqw_errError in the equivalent width described aboveREAL
sii_6731_fluxFlux from Gaussian fit to continuum subtracted data. (Note that the fit is done simultaneously to all the lines so de-blending happens automatically)REAL
sii_6731_flux_errError in the fluxREAL
sii_6731_inst_resInstrumental resolution at the line center (measured for each spectrum from the ARC lamps)REAL
sii_6731_reqwThe equivalent width of the continuum-subtracted emission line computed from straight integration over the bandpasses listed below (emisison 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)REAL
sii_6731_reqw_errError in the equivalent width described aboveREAL
sii_6731_seqwThe equivalent width of the CB07 continuum-subtracted emission line computed from a spectrum with the other emission lines subtracted off. In general this is not recommended for use.REAL
sii_6731_seqw_errError in the aboveREAL
specobjidUnique database ID based on PLATE, MJD, FIBERID, RUN2DCHAR
spectofiberThe multiplicative scale factor applied to the original flux and error spectra prior to measurement of the emission lines to improve the spectrophotometric accuracy. The rescaling insures that a synthetic r-band magnitude computed from the spectrum matches the r-band fiber magnitude measured by the photometric pipeline.REAL
v_off_balmerVelocity offset of the Balmer lines from the measured redshiftREAL
v_off_balmer_errError in the aboveREAL
v_off_forbiddenVelocity offset of the forbidden lines from the measured redshiftREAL
v_off_forbidden_errError in the aboveREAL


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