Radiatively inefficient accretion flow in the nucleus of NGC 1097

Rodrigo S. Nemmen, Thaisa Storchi-Bergmann, Feng Yuan, Michael Eracleous, Yuichi Terashima, Andrew S. Wilson

Research output: Contribution to journalArticle

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Abstract

We present a model for the accretion flow around the supermassive black hole in the LINER nucleus of NGC 1097 that fits the optical to X-ray spectral energy distribution (SED). The X-ray segment of the SED is based on observations with the Chandra X-Ray Observatory, which are reported here for the first time. The inner part of the flow is modeled as a radiatively inefficient accretion flow (RIAF), and the outer part as a standard thin disk. The value of the transition radius (rtr ≈ 225RS, where RS = 2GM/c2) between the RIAF and the outer thin disk was obtained from our previous fitting of the double-peaked Balmer emission line profile, which originates in the thin disk. The black hole mass was inferred from measurements of the stellar velocity dispersion in the host galaxy. When these parameters are used in the accretion flow model, the SED can be successfully reproduced, which shows that the line profile model and the accretion flow model are consistent with each other. A small remaining excess in the near-UV is accounted for by the contribution of an obscured starburst located within 9 pc from the nucleus, as we reported in an earlier paper. The radio flux is consistent with synchrotron emission of a relativistic jet modeled by means of the internal shock scenario. In an appendix we also analyze the Chandra X-ray observations of the ∼1 kpc circumnuclear star-forming ring and of an ultraluminous compact X-ray source located outside the ring.

Original languageEnglish (US)
Pages (from-to)652-659
Number of pages8
JournalAstrophysical Journal
Volume643
Issue number2 I
DOIs
StatePublished - Jun 1 2006

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accretion
nuclei
spectral energy distribution
x rays
energy
rings
profiles
observatories
synchrotrons
observatory
shock
radio
galaxies
stars
radii
distribution

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Nemmen, R. S., Storchi-Bergmann, T., Yuan, F., Eracleous, M., Terashima, Y., & Wilson, A. S. (2006). Radiatively inefficient accretion flow in the nucleus of NGC 1097. Astrophysical Journal, 643(2 I), 652-659. https://doi.org/10.1086/500571
Nemmen, Rodrigo S. ; Storchi-Bergmann, Thaisa ; Yuan, Feng ; Eracleous, Michael ; Terashima, Yuichi ; Wilson, Andrew S. / Radiatively inefficient accretion flow in the nucleus of NGC 1097. In: Astrophysical Journal. 2006 ; Vol. 643, No. 2 I. pp. 652-659.
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Nemmen, RS, Storchi-Bergmann, T, Yuan, F, Eracleous, M, Terashima, Y & Wilson, AS 2006, 'Radiatively inefficient accretion flow in the nucleus of NGC 1097', Astrophysical Journal, vol. 643, no. 2 I, pp. 652-659. https://doi.org/10.1086/500571

Radiatively inefficient accretion flow in the nucleus of NGC 1097. / Nemmen, Rodrigo S.; Storchi-Bergmann, Thaisa; Yuan, Feng; Eracleous, Michael; Terashima, Yuichi; Wilson, Andrew S.

In: Astrophysical Journal, Vol. 643, No. 2 I, 01.06.2006, p. 652-659.

Research output: Contribution to journalArticle

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Nemmen RS, Storchi-Bergmann T, Yuan F, Eracleous M, Terashima Y, Wilson AS. Radiatively inefficient accretion flow in the nucleus of NGC 1097. Astrophysical Journal. 2006 Jun 1;643(2 I):652-659. https://doi.org/10.1086/500571