Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543309w&link_type=abstract
American Astronomical Society, AAS Meeting #215, #433.09; Bulletin of the American Astronomical Society, Vol. 42, p.371
Astronomy and Astrophysics
Astronomy
Scientific paper
The quasar SDSS J1536+0441 shows two broad-line emission systems, interpreted as a binary black hole system with a separation of 0.1 pc (Boroson & Lauer 2009, Nature, 458, 53), a double-peaked emitter (Chornock et al., arXiv:0906.0849v1), or both (Tang & Grindlay, arXiv:0909.0258v1). Our imaging with the NRAO VLA at 8.5 GHz revealed two faint sources, A and B, separated by 5 kpc, with each source being unresolved with a diameter of less than 2 kpc (Wrobel & Laor 2009, ApJ, 699, L22). It is now clear that A is hosted by the radio-quiet quasar, while B is hosted by a companion elliptical galaxy (Decarli et al. 2009, ApJ, 703, L76; Lauer & Boroson 2009, ApJ, 703, 930). Our new VLA imaging at 22 GHz implies a flat overall spectrum for A and B, suggesting that A, the stronger of the two at 8.5 GHz, is sufficiently compact to be synchrotron self-absorbed. The coronal framework for radio-quiet quasars (Laor & Behar 2008, MNRAS, 390, 847) predicts a flat radio spectrum for A. Moreover, within that framework, the 8.5-GHz luminosity of A implies its "radio sphere" has a diameter of about 0.2 pc, interestingly similar to the proposed binary separation. To test these predictions of a compact structure for A, we are planning to observe it with the NRAO VLBA and to monitor it with the NRAO Expanded VLA (Perley et al., arXiv:0909.1585v1). The NRAO is a facility of the NSF operated under cooperative agreement by AUI.
Laor Ari
Wrobel Joan M.
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