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When Is BL Lac Not a BL Lac?

R. C. VermeulenAstronomy 105-24, California Institute of Technology, Pasadena, CA 91125P. OgleAstronomy 105-24, California Institute of Technology, Pasadena, CA 91125H. D. TranAstronomy 105-24, California Institute of Technology, Pasadena, CA 91125I. W. A. BrowneAstronomy 105-24, California Institute of Technology, Pasadena, CA 91125M. H. CohenAstronomy 105-24, California Institute of Technology, Pasadena, CA 91125A. C. S. ReadheadAstronomy 105-24, California Institute of Technology, Pasadena, CA 91125G. B. TaylorAstronomy 105-24, California Institute of Technology, Pasadena, CA 91125Robert W. GoodrichSpace Telescope Science Institute, Baltimore, MD 21218

1995en

ABI

Annotatsiya

We have found broad Hα and Hβ line emission in spectra of BL Lacertae taken on 1995 May 21 and June 1: on those occasions BL Lac did not meet the defining criteria for the class named after it. The Hα line luminosity, ~2 × 1041 h-2 erg s-1 for H0 = 100 h km s-1 Mpc-1, is significantly above the detection threshold in older published spectra which do not show the line. Several possible explanations for the increase in broad line luminosity are discussed. The continuum was at the faint end of its commonly observed range: V ~ 16.0 on 1995 May 21. The polarization, measured on 1995 June 1, was also near the low end of the typical range in BL Lac: ~5.0% in PA ~ 22° near 7500 Å, rising to ~6.1% in PA ~ 15° near 4900 Å. Absorption features in the spectrum show the presence of the associated galaxy, but the light is still dominated by an underlying smooth continuum, the intrinsic shape of which is well approximated between 8000 and 4000 Å by Fν ∝ ν-1.7, indicating a synchrotron origin. We confirm the narrow emission line redshift, z = 0.0686 ± 0.0004.

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DOI: 10.1086/309716

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