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Column descriptions for linemeas catalog:
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- Column 1 ("Field"): Field name (AEGIS, COSMOS, GOODS-N, GOODS-S, UDS)
- Column 2 ("MaskName"): Mask name (e.g., co2_01, ae2_03)
- Column 3 ("ID"): Object ID
- Column 4 ("slitobjname"): ID of main target on slit
- Column 5 ("aperture_no"): aperture number of object
- Column 6 ("z_mosfire_initqual"): quality of initial redshift guess
  	   (0: robust, 1: single non-robust redshift that is not obviously
  	   inconsistent with previous redshift estimate, 2: 2 non-robust
  	   redshift estimates; 3: single non-robust redshift that is inconsistent
  	   with previous redshift estimate), -1: no redshift measurable
	   from spectrum
- Column 7 ("OII3727_Intercept"): intercept of continuum fit under OII3727 where flux is in units of 1e-18 erg/s/cm^2
- Column 8 ("OII3727_Intercept_Err"): 1-sigma dispersion in best-fit intercept
- Column 9 ("OII3727_Slope"): slope of continuum fit under OII3727 where flux is in units of 1e-18 erg/s/cm^2
- Column 10 ("OII3727_Slope_Err"): 1-sigma dispersion in best-fit slope
- Column 11 ("OII3727_ObsLam"): observed wavelength of OII3727 
- Column 12 ("OII3727_ObsLam_Err"): 1-sigma dispersion in observed wavelength of OII3727
- Column 13 ("OII3727_FWHM"): observed FWHM in Angstroms of OII3727
- Column 14 ("OII3727_FWHM_Err"): 1-sigma dispersion in observed FWHM of OII3727
- Column 15 ("OII3727_Flux"): OII3727 emission line flux in erg/s/cm^2 integrated over Gaussian fit
- Column 16 ("OII3727_Flux_Err"): 1-sigma dispersion in emission line flux of OII3727
- Column 17 ("OII3727_z"): observed redshift of OII3727 line
- Column 18 ("OII3727_z_Err"): 1-sigma dispersion in observed redshift of OII3727
- Column 19 ("OII3727_Fluxband"): OII3727 emission line flux integrated under spectrum
- Column 20 ("OII3727_Fluxband_Err"): 1-sigma dispersion in flux measured under spectrum
- Column 21 ("OII3727_MaskedFlux"): OII3727 line flux from Gaussian fit, excluding regions with sky lines
- Column 22 ("OII3727_MaskedFlux_Err"): 1-sigma dispersion in flux from Gaussian fit, excluding sky lines
- Column 23 ("OII3727_aeflag"): flag indicating if emission line close to edge of spectrum (=1) or not (=0)
  	    			if aeflag=2, the line is at the edge of the spectrum, but it's flux is still
				usable --> so, use aeflag=0/2 objects for analysis; aeflag='-999' means the line is not covered at all
- Column 24 ("OII3727_slflag"): flag indicating degree to which emission line is affected by nearby skylines;
  	    			***BEWARE OF THE FLUX IF SLFLAG >= 0.2***  	    			
- Column 25 ("OII3727_meanchisq"): average chi^2 value between model fit and science spectrum
- Column 26 ("OII3727_chiflag"): number of pixels within +/- 3 sigma (width of Gaussian) where model 
  	    			 deviates >2-sigma from science spectrum
- Column 27 ("OII3727_PreferredFlux"): best flux to use for this line.  If chiflag>=1 and
  	    abs(flux-fluxband)/flux_err >=3.0, then this is set to fluxband.  Otherwise, it is
	    set to the fitted flux
- Column 28 ("OII3727_PreferredFlux_Err"): error on the preferred flux (this is the same as flux_err)
- Columns 29-50: same as columns 8-29 for OII3730
- Columns 51-72: same as columns 8-29 for NeIII3870
- Columns 73-94: same as columns 8-29 for NeIII3969
- Columns 95-116: same as columns 8-29 for Hd4103 **
- Columns 117-138: same as columns 8-29 for Hg4342 **
- Columns 139-160: same as columns 8-29 for OIII4364
- Columns 161-182: same as columns 8-29 for Hb4863 **
- Columns 183-204: same as columns 8-29 for OIII4960
- Columns 205-226: same as columns 8-29 for OIII5008
- Columns 227-248: same as columns 8-29 for OI6302
- Columns 249-270: same as columns 8-29 for NII6550
- Columns 271-292: same as columns 8-29 for Ha6565 **
- Columns 293-314: same as columns 8-29 for NII6585
- Columns 315-336: same as columns 8-29 for SII6718
- Columns 337-358: same as columns 8-29 for SII6733
- Column 359 ("NIIHA"): ratio of [NII]/Ha
- Column 360 ("NIIHA_Err"): 1-sigma dispersion in measured [NII]/Ha
- Column 361 ("TDHST_version"): 3D-HST version relevant for the ID number

**All Balmer recombination emission line fluxes have been corrected for underlying stellar absorption
as predicted by the best-fitting FAST model fits to the broadband photometry