CIV Line-Width Anomalies: the Perils of Low S/N Spectra

TY - JOUR

T1 - CIV Line-Width Anomalies

T2 - the Perils of Low S/N Spectra

AU - Denney, Kelly D.

AU - Pogge, Richard W.

AU - Assef, Roberto J.

AU - Kochanek, Christopher S.

AU - Peterson, Bradley M.

AU - Vestergaard, Marianne

PY - 2013/9/1

Y1 - 2013/9/1

N2 - Comparison of six high-redshift quasar spectra obtained with the Large Binocular Telescope with previous observations from the Sloan Digital Sky Survey shows that failure to correctly identify absorption and other problems with accurate characterization of the CIV emission line profile in low S/N data can severely limit the reliability of single-epoch mass estimates based on the CIV emission line. We combine the analysis of these new high-quality data with a reanalysis of three other samples based on high S/N spectra of the CIV emission line region. We find that a large scatter between the Hbeta- and CIV-based masses remains even for this high S/N sample when using the FWHM to characterize the BLR velocity dispersion and the standard virial assumption to calculate the mass. However, we demonstrate that using high-quality data and the line dispersion to characterize the CIV line width leads to a high level of consistency between CIV- and Hbeta-based masses, with

AB - Comparison of six high-redshift quasar spectra obtained with the Large Binocular Telescope with previous observations from the Sloan Digital Sky Survey shows that failure to correctly identify absorption and other problems with accurate characterization of the CIV emission line profile in low S/N data can severely limit the reliability of single-epoch mass estimates based on the CIV emission line. We combine the analysis of these new high-quality data with a reanalysis of three other samples based on high S/N spectra of the CIV emission line region. We find that a large scatter between the Hbeta- and CIV-based masses remains even for this high S/N sample when using the FWHM to characterize the BLR velocity dispersion and the standard virial assumption to calculate the mass. However, we demonstrate that using high-quality data and the line dispersion to characterize the CIV line width leads to a high level of consistency between CIV- and Hbeta-based masses, with

KW - astro-ph.CO

U2 - 10.1088/0004-637X/775/1/60

DO - 10.1088/0004-637X/775/1/60

M3 - Journal article

SN - 0004-637X

VL - 775

JO - Astrophysical Journal

JF - Astrophysical Journal

M1 - 60

ER -