Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 559125.0, MPI für Astronomie / Publikationen_mpia
A runaway black hole in COSMOS: Gravitational wave or slingshot recoil?
Authors:Civano, F.; Elvis, M.; Lanzuisi, G.; Jahnke, K.; Zamorani, G.; Blecha, L.; Bongiorno, A.; Brusa, M.; Comastri, A.; Hao, H.; Leauthaud, A.; Loeb, A.; Mainieri, V.; Piconcelli, E.; Salvato, M.; Scoville, N.; Trump, J.; Vignali, C.; Aldcroft, T.; Bolzonella, M.; Bressert, E.; Finoguenov, A.; Fruscione, A.; Koekemoer, A. M.; Cappelluti, N.; Fiore, F.; Giodini, S.; Gilli, R.; Impey, C. D.; Lilly, S. J.; Lusso, E.; Puccetti, S.; Silverman, J. D.; Aussel, H.; Capak, P.; Frayer, D.; Le Floch, E.; McCracken, H. J.; Sanders, D. B.; Schiminovich, D.; Taniguchi, Y.
Date of Publication (YYYY-MM-DD):2010
Title of Journal:The Astrophysical Journal
Journal Abbrev.:The Astrophysical Journal
Issue / Number:1
Start Page:209
End Page:222
Review Status:not specified
Audience:Experts Only
Abstract / Description:We present a detailed study of a peculiar source detected in the COSMOS survey at z = 0.359. Source CXOC J100043.1+020637, also known as CID-42, has two compact optical sources embedded in the same galaxy. The distance between the two, measured in the HST/ACS image, is 0.495" ± 0.005" that, at the redshift of the source, corresponds to a projected separation of 2.46 ± 0.02 kpc. A large (~1200 km s-1) velocity offset between the narrow and broad components of Hβ has been measured in three different optical spectra from the VLT/VIMOS and Magellan/IMACS instruments. CID-42 is also the only X-ray source in COSMOS, having in its X-ray spectra a strong redshifted broad absorption iron line and an iron emission line, drawing an inverted P-Cygni profile. The Chandra and XMM-Newton data show that the absorption line is variable in energy by ΔE = 500 eV over four years and that the absorber has to be highly ionized in order not to leave a signature in the soft X-ray spectrum. That these features—the morphology, the velocity offset, and the inverted P-Cygni profile—occur in the same source is unlikely to be a coincidence. We envisage two possible explanations, both exceptional, for this system: (1) a gravitational wave (GW) recoiling black hole (BH), caught 1-10 Myr after merging; or (2) a Type 1/Type 2 system in the same galaxy where the Type 1 is recoiling due to the slingshot effect produced by a triple BH system. The first possibility gives us a candidate GW recoiling BH with both spectroscopic and imaging signatures. In the second case, the X-ray absorption line can be explained as a BAL-like outflow from the foreground nucleus (a Type 2 AGN) at the rearer one (a Type 1 AGN), which illuminates the otherwise undetectable wind, giving us the first opportunity to show that fast winds are present in obscured active galactic nuclei (AGNs), and possibly universal in AGNs.
Free Keywords:galaxies: active; galaxies: formation; galaxies: interactions; galaxies: nuclei; quasars: absorption lines
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2010ApJ...717..209C [ID No:1]
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.