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Double-peaked Balmer line emission in the radio-quiet AGN RX J1042 + 1212

AutorPuchnarewicz, E. M.; Mason, Keith O.; Carrera, Francisco J.
Palabras claveGalaxies: individual: RX J1042 + 1212
Galaxies: Seyfert
X-rays: galaxies
Galaxies: active
Line: profiles
Fecha de publicación1996
EditorRoyal Astronomical Society
Oxford University Press
CitaciónMonthly Notices of the Royal Astronomical Society 283(4): 1311-1321 (1996)
ResumenWe present optical and X-ray spectra of a radio-quiet, X-ray-selected AGN, RX J1042 + 1212 (z = 0.271). The Hα and Hβ emission lines are very broad (with full widths at half maximum of ∼ 10000 km s-1) and have double-peaked profiles. Such features are rarely observed in AGN in general, but are even more unusual in radio-quiet objects. The analysis of the ROSAT PSPC data reveals a non-varying, unabsorbed spectrum with an energy spectral index αx = 1.2 and little or no emission from a soft X-ray excess. The slope of the optical spectrum is similar, αopt = 1.0, and is consistent with an extrapolation of the X-ray spectrum, suggesting that the same power-law continuum may dominate throughout, and that the big blue bump component is relatively weak. We look for a link between these various properties, and investigate models of double-peaked Balmer line emission in AGN. An accretion disc origin is unlikely in RX J1042 + 1212, as this model predicts that lines emitted by a disc should have a net gravitational redshift (both Hα and Hβ have a net blueshift). Emission from two broad-line regions, each gravitationally bound to one component of a supermassive black hole binary, is a possibility if the two components are similar in size and nature. Alternatively, the lines (or at least the narrow peaks of the lines) may be produced by a double-sided jet or bipolar flow.
Versión del editorhttps://doi.org/10.1093/mnras/283.4.1311
Identificadoresissn: 0035-8711
e-issn: 1365-2966
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