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A Runaway Black Hole in COSMOS: Gravitational Wave or Slingshot Recoil? | | F. Civano
; M. Elvis
; G. Lanzuisi
; K. Jahnke
; G. Zamorani
; L. Blecha
; A. Bongiorno
; M. Brusa
; A. Comastri
; H. Hao
; A. Leauthaud
; A. Loeb
; M. Mignoli
; V. Mainieri
; E. Piconcelli
; M. Salvato
; N. Scoville
; J. Trump
; C. Vignali
; T. Aldcroft
; M. Bolzonella
; E. Bressert
; A. Finoguenov
; A. Fruscione
; A. M. Koekemoer
; N. Cappelluti
; F. Fiore
; S. Giodini
; R. Gilli
; C. D. Impey
; S. J. Lilly
; E. Lusso
; S. Puccetti
; J. D. Silverman
; H. Aussel
; P. Capak
; D. Frayer
; E. Le Floc'h
; H. J. McCracken
; D. B. Sanders
; D. Schiminovich
; Y. Taniguchi
; | | Date: |
27 Feb 2010 | | Abstract: | We present a detailed study of a peculiar source in the COSMOS survey at
z=0.359. Source CXOCJ100043.1+020637 (CID-42) presents two compact optical
sources embedded in the same galaxy. The distance between the 2, measured in
the HST/ACS image, is 0.495" that, at the redshift of the source, corresponds
to a projected separation of 2.46 kpc. A large (~1200 km/s) velocity offset
between the narrow and broad components of Hbeta 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 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 data show that the absorption
line is variable in energy by 500 eV over 4 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 occur in the same source is unlikely to be a
coincidence. We envisage two possible explanations: (1) a gravitational wave
recoiling black hole (BH), caught 1-10 Myr after merging, (2) a Type 1/ Type 2
system in the same galaxy where the Type 1 is recoiling due to slingshot effect
produced by a triple BH system. The first possibility gives us a candidate
gravitational waves 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 AGN. | | Source: | arXiv, 1003.0020 | | Services: | Forum | Review | PDF | Favorites | |
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