Biases in Virial Black Hole Masses: An SDSS Perspective
Shen, Yue; Greene, Jenny E.; Strauss, Michael A.; Richards, Gordon T.; Schneider, Donald P. 2008, ApJ, 680, 169 (arXiv:0709.3098)

The full table 1 can be downloaded here.

The line flux and EW measurements for Hbeta, MgII and CIV are summarized in this fits table. Following is the description of the table. Note that the catalog and this fits table only contain objects with high S/N>6 within the line profile, which are recommended for statistical analyses on emission lines. Many lines with S/N<6 are in general measurable as the chi^2 fits can successfully converge; but the results are not to be trusted seriously and are likely biased. Nevertheless, in some cases you probably want to have as many measurements as possible, so I put an additional fits table here, which contains all measurable lines.

Tagname Format Description
PLATE LONG plate number
FIBER LONG fiber number
MJD LONG mjd number
Z DOUBLE cataloged redshift
HBETA_FE_NORM_FACTOR DOUBLE Array[2] normalization of iron template for Hbeta
DOUBLE Array[2] normalization of iron template for MgII
HBETA_REDCHI2_2 DOUBLE reduced chi^2 for Hbeta line fit
HBETA_LINEFLUX_BR DOUBLE Array[2] broad Hbeta line flux
HBETA_LINEFLUX_NA DOUBLE Array[2] narrow Hbeta line flux
HBETA_EW_BR DOUBLE Array[2] broad Hbeta line EW
HBETA_EW_NA DOUBLE Array[2] narrow Hbeta line EW
OIII4959_LINEFLUX DOUBLE Array[2] [OIII]4959 line flux
OIII4959_EW DOUBLE Array[2] [OIII]4959 line EW
OIII5007_LINEFLUX DOUBLE Array[2] [OIII]5007 line flux
OIII5007_EW DOUBLE Array[2] [OIII]5007 line EW
DOUBLE Array[2] broad MgII line flux
DOUBLE Array[2] narrow MgII line flux
MGII_EW_BR DOUBLE Array[2] broad MgII line EW
MGII_EW_NA DOUBLE Array[2] narrow MgII line EW
MGII_REDCHI2_2 DOUBLE reduced chi^2 for MgII line fit
CIV_LINEFLUX DOUBLE Array[2] CIV line flux
CIV_EW DOUBLE Array[2] CIV line EW
CIV_REDCHI2_2 DOUBLE reduced chi^2 for CIV line fit

1. Emission line+continuum+iron template fits are described in Shen et al. (2008). The fits are done in restframe.
2. Iron emissions are modeled for Hbeta and MgII, but not for CIV.
3. For MgII, I recommend to use the sum of the broad and narrow component EWs as the MgII line EWs, since subtraction of a narrow component of MgII is not justified.
4. Each of the DOUBLE Array[2] contains the value and the fitting error. If their values are 0 then the fit failed or it is outside spectral range.
5. I won't trust the fits too much when the line is colse to the SDSS spectral edge. So make reasonable redshift cuts for the line under consideration.
6. There may still be serendipitous cases where the line flux or EW is clearly wrong (i.e., due to incorrect iron subtraction or something else). But the fraction of these cases is tiny, so you may just neglect these cases.