The XMM-newton spectrum of a candidate recoiling supermassive black hole: An elusive inverted P-cygni profile

G. Lanzuisi, F. Civano, S. Marchesi, A. Comastri, E. Costantini, M. Elvis, V. Mainieri, R. Hickox, K. Jahnke, S. Komossa, E. Piconcelli, C. Vignali, M. Brusa, Nico Cappelluti, A. Fruscione

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

We present a detailed spectral analysis of new XMM-Newton data of the source CXOC J100043.1+020637, also known as CID-42, detected in the COSMOS survey at z = 0.359. Previous works suggested that CID-42 is a candidate recoiling supermassive black hole (SMBH) showing also an inverted P-Cygni profile in the X-ray spectra at 6 keV (rest) with an iron emission line plus a redshifted absorption line (detected at 3σ in previous XMM-Newton and Chandra observations). Detailed analysis of the absorption line suggested the presence of ionized material flowing into the black hole at high velocity. In the new long XMM-Newton observation, while the overall spectral shape remains constant, the continuum 2-10 keV flux decrease of 20% with respect to previous observation and the absorption line is undetected. The upper limit on the intensity of the absorption line is EW < 162 eV. Extensive Monte Carlo simulations show that the nondetection of the line is solely due to variation in the properties of the inflowing material, in agreement with the transient nature of these features, and that the intensity of the line is lower than the previously measured with a probability of 98.8%. In the scenario of CID-42 as a recoiling SMBH, the absorption line can be interpreted as being due to an inflow of gas with variable density that is located in the proximity of the SMBH and recoiling with it. New monitoring observations will be requested to further characterize this line.

Original languageEnglish (US)
Article number62
JournalAstrophysical Journal
Volume778
Issue number1
DOIs
StatePublished - Nov 20 2013
Externally publishedYes

Fingerprint

recoilings
XMM-Newton telescope
newton
charge injection devices
profiles
spectral analysis
spectrum analysis
proximity
inflow
continuums
iron
monitoring
gases
gas
simulation
x rays

Keywords

  • galaxies: active
  • surveys
  • X-rays: galaxies

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Lanzuisi, G., Civano, F., Marchesi, S., Comastri, A., Costantini, E., Elvis, M., ... Fruscione, A. (2013). The XMM-newton spectrum of a candidate recoiling supermassive black hole: An elusive inverted P-cygni profile. Astrophysical Journal, 778(1), [62]. https://doi.org/10.1088/0004-637X/778/1/62

The XMM-newton spectrum of a candidate recoiling supermassive black hole : An elusive inverted P-cygni profile. / Lanzuisi, G.; Civano, F.; Marchesi, S.; Comastri, A.; Costantini, E.; Elvis, M.; Mainieri, V.; Hickox, R.; Jahnke, K.; Komossa, S.; Piconcelli, E.; Vignali, C.; Brusa, M.; Cappelluti, Nico; Fruscione, A.

In: Astrophysical Journal, Vol. 778, No. 1, 62, 20.11.2013.

Research output: Contribution to journalArticle

Lanzuisi, G, Civano, F, Marchesi, S, Comastri, A, Costantini, E, Elvis, M, Mainieri, V, Hickox, R, Jahnke, K, Komossa, S, Piconcelli, E, Vignali, C, Brusa, M, Cappelluti, N & Fruscione, A 2013, 'The XMM-newton spectrum of a candidate recoiling supermassive black hole: An elusive inverted P-cygni profile', Astrophysical Journal, vol. 778, no. 1, 62. https://doi.org/10.1088/0004-637X/778/1/62
Lanzuisi, G. ; Civano, F. ; Marchesi, S. ; Comastri, A. ; Costantini, E. ; Elvis, M. ; Mainieri, V. ; Hickox, R. ; Jahnke, K. ; Komossa, S. ; Piconcelli, E. ; Vignali, C. ; Brusa, M. ; Cappelluti, Nico ; Fruscione, A. / The XMM-newton spectrum of a candidate recoiling supermassive black hole : An elusive inverted P-cygni profile. In: Astrophysical Journal. 2013 ; Vol. 778, No. 1.
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abstract = "We present a detailed spectral analysis of new XMM-Newton data of the source CXOC J100043.1+020637, also known as CID-42, detected in the COSMOS survey at z = 0.359. Previous works suggested that CID-42 is a candidate recoiling supermassive black hole (SMBH) showing also an inverted P-Cygni profile in the X-ray spectra at 6 keV (rest) with an iron emission line plus a redshifted absorption line (detected at 3σ in previous XMM-Newton and Chandra observations). Detailed analysis of the absorption line suggested the presence of ionized material flowing into the black hole at high velocity. In the new long XMM-Newton observation, while the overall spectral shape remains constant, the continuum 2-10 keV flux decrease of 20{\%} with respect to previous observation and the absorption line is undetected. The upper limit on the intensity of the absorption line is EW < 162 eV. Extensive Monte Carlo simulations show that the nondetection of the line is solely due to variation in the properties of the inflowing material, in agreement with the transient nature of these features, and that the intensity of the line is lower than the previously measured with a probability of 98.8{\%}. In the scenario of CID-42 as a recoiling SMBH, the absorption line can be interpreted as being due to an inflow of gas with variable density that is located in the proximity of the SMBH and recoiling with it. New monitoring observations will be requested to further characterize this line.",
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AU - Costantini, E.

AU - Elvis, M.

AU - Mainieri, V.

AU - Hickox, R.

AU - Jahnke, K.

AU - Komossa, S.

AU - Piconcelli, E.

AU - Vignali, C.

AU - Brusa, M.

AU - Cappelluti, Nico

AU - Fruscione, A.

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AB - We present a detailed spectral analysis of new XMM-Newton data of the source CXOC J100043.1+020637, also known as CID-42, detected in the COSMOS survey at z = 0.359. Previous works suggested that CID-42 is a candidate recoiling supermassive black hole (SMBH) showing also an inverted P-Cygni profile in the X-ray spectra at 6 keV (rest) with an iron emission line plus a redshifted absorption line (detected at 3σ in previous XMM-Newton and Chandra observations). Detailed analysis of the absorption line suggested the presence of ionized material flowing into the black hole at high velocity. In the new long XMM-Newton observation, while the overall spectral shape remains constant, the continuum 2-10 keV flux decrease of 20% with respect to previous observation and the absorption line is undetected. The upper limit on the intensity of the absorption line is EW < 162 eV. Extensive Monte Carlo simulations show that the nondetection of the line is solely due to variation in the properties of the inflowing material, in agreement with the transient nature of these features, and that the intensity of the line is lower than the previously measured with a probability of 98.8%. In the scenario of CID-42 as a recoiling SMBH, the absorption line can be interpreted as being due to an inflow of gas with variable density that is located in the proximity of the SMBH and recoiling with it. New monitoring observations will be requested to further characterize this line.

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