Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21830101c&link_type=abstract
American Astronomical Society, AAS Meeting #218, #301.01; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
Double super-massive black holes (SMBHs) within a single galaxy are predicted by hierarchical models of structure formation. Finding these double BHs has been a frustrating search: At z˜2, they are hard to resolve, given that the required angular separation is beyond the capability of current ground and space-based observatories. Instead, at later epochs (z<0.7), where the angular separations are larger (˜0.5arcsec), they are easier to resolve, but the merger rate has dropped dramatically, so binary SMBHs should be scarce. As mergers proceed, these SMBH pairs will merge. The coalescence give rise to the strongest GW events in the universe. In some cases GW recoil, due to the asymmetric emission of GW, causes the newly merged single SMBH to gain a significant velocity (up to ˜ 1000km/s) with respect to the center of the galaxy. If the recoiling BH is active, it will retain its accretion disk and broad emission line region and will still be seen as an AGN for several years, by which time it may be displaced by several kiloparsecs from the former host nucleus. Deep imaging and spectroscopic searches have recently been initiated to study double SMBHs, or displaced single BH, at all wavelengths and at any separation. I will present multiwavelength results on double SMBHs and show how the high angular resolution of Chandra helps in the study of their activity. I will concentrate on the properties of CID-42 (z=0.359), a unique source in the COSMOS survey, the best recoiling BH candidate to date. CID-42 clearly shows both the presence of two compact sources, 2.5 kpc apart, embedded in the same galaxy in HST imaging, and a 1100km/s velocity offset between the narrow and broad components of Hbeta, in three optical spectra. Our new HRC/Chandra data are the key to understanding the nature of this intriguing source.
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