Morphologies And SEDs Of Low-redshift Low-ionization Broad Absorption Line QSOs

Details Morphologies And SEDs Of Low-redshift Low-ionization Broad Absorption Line QSOs Morphologies And SEDs Of Low-redshift Low-ionization Broad Absorption Line QSOs

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21932106l&link_type=abstract

American Astronomical Society, AAS Meeting #219, #321.06

Astronomy and Astrophysics

Astronomy

Scientific paper

We present optical and infrared HST/WFC3 images and Spitzer IRS spectra and MIPS photometry of a large volume-limited sample of 22 SDSS-selected Low-ionization Broad Absorption Line QSOs (LoBALs) at 0.5 < z < 0.6. Previous studies of LoBALs show that their host galaxies tend to be ultraluminous infrared galaxies (ULIRGs) that are undergoing mergers and that have young stellar populations. We test the hypothesis that LoBALs are a transition phase from dust-embedded, ultra-luminous infrared QSOs toward unobscured type-1 QSOs by studying their morphologies for signs of recent tidal interaction and estimating star formation activity from their far-infrared SEDs. Our results show that, while the majority of the LoBALs are similar to type-1 QSOs in terms of their mid- and far-infrared properties, at least 20%, and as many as 60%, of the LoBALs are characterized by higher infrared luminosities typical of ULIRGs and star formation rates 150-300 solar masses per year. Most of the LoBALs show apparent signs of tidal disturbance. We model the 2D host galaxy profiles with GALFIT and subtract simple bulge and disk models to reveal any fine structure, relic of past merger event. We correlate the morphologies and the merger stages with infrared luminosities, star formation rates, and mid-infrared spectral properties of this sample from Spitzer data. The unusually high fraction of LoBALs with high infrared luminosities and host galaxies showing signs of tidal interaction, in principle, fits the evolutionary paradigm, implying that LoBALs are rapidly transitioning from a ULIRG phase to a more quiescent phase with star formation activity typical of type-1 QSOs.

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