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Chandra view on the active nucleus of CGCG 292–057: Jet-ISM interactions

Published online by Cambridge University Press:  07 April 2020

K. Balasubramaniam Open the ORCID record for K. Balasubramaniam [Opens in a new window] ,
Ł. Stawarz ,
V. Marchenko ,
R. Thimmappa ,
M. Sobolewska ,
A. Siemiginowska ,
C. C. Cheung ,
D. Kozieł-Wierzbowska  and
M. Jamrozy
K. Balasubramaniam
Affiliation:
Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Krakow, Poland email: [email protected]
Ł. Stawarz
Affiliation:
Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Krakow, Poland email: [email protected]
V. Marchenko
Affiliation:
Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Krakow, Poland email: [email protected]
R. Thimmappa
Affiliation:
Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Krakow, Poland email: [email protected]
M. Sobolewska
Affiliation:
Harvard Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA02138, USA
A. Siemiginowska
Affiliation:
Harvard Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA02138, USA
C. C. Cheung
Affiliation:
Space Science Division, Naval Research Laboratory, Washington, DC20375-5352, USA
D. Kozieł-Wierzbowska
Affiliation:
Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Krakow, Poland email: [email protected]
M. Jamrozy
Affiliation:
Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Krakow, Poland email: [email protected]
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Abstract

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We present the analysis of the 93 ksec Chandra ACIS–S data for the galaxy CGCG 292–057 (z = 0.054), with complex radio structure indicative of the intermittent jet activity. In order to characterize precisely the spectrum of the unresolved low-luminosity active nucleus in the source, we performed detailed MARX/PSF simulations and studied the radial profile of the source region surface brightness. In this way, we have detected an additional X-ray component extending from a few up to ∼10 kpc from the unresolved core, which could be associated with the hot gaseous medium compressed and heated (up to 0.9 keV) by the expanding inner lobes of the radio galaxy. We modeled the X-ray spectrum of the unresolved nucleus assuming various emission models, including an absorbed power-law, a power-law plus thermal emission component, and a two-temperature thermal plasma. The best fit was however obtained assuming a power-law emission scattered by a hot ionized gas, giving rise to the 6.7 keV iron line.

Keywords

galaxies: activeX-rays: galaxiesX-rays: Individual (CGCG 292–057)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S342: Perseus in Sicily: From Black Hole to Cluster Outskirts , May 2018 , pp. 222 - 223
Copyright
© International Astronomical Union 2020

References

Kozieł-Wierzbowska, D., et al. 2012, MNRAS, 422, 1546CrossRefGoogle Scholar
Krauss, F., et al. 2018, A&A, 610, 8Google Scholar
Siemiginowska, A., et al. 2016, ApJ, 823, 57CrossRefGoogle Scholar
Singh, V., et al. 2015, MNRAS, 454, 1556CrossRefGoogle Scholar