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arXiv · 2507.23100

Chandra X-ray Observatory study of the X-ray emission of PKS 0023-26 and comparison with recent ALMA results

A. Siemiginowska·R. Morganti·G. Fabbiano·E. O'Sullivan·T. Oosterloo·C. Tadhunter·D. Burke
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Abstract

We present a deep high-resolution Chandra X-ray Observatory image data of a powerful compact radio source PKS 0023-26 associated with a quasar at redshift 0.322. The earlier studies of the optical environment suggested that the source could be located in a galaxy cluster or a group. However, we report a non-detection of hot gas on large scales (out to $\sim 60$ kpc radius) and place an upper limit on the X-ray luminosity of $<3\times10^{42}$ erg s$^{-1}$, consistent only with the presence of a poor, low-temperature ($\rm kT < 0.5$ keV) galaxy group. X-ray spectral analysis of the central circular region, $r<7$ kpc shows, in addition to the mildly absorbed AGN, a thermal emission component with a temperature of $\rm kT=0.9^{+0.19}_{-0.37}$ keV. We discuss the origin of this hot component as a result of interaction between the evolving radio source and the interstellar medium. Our high angular resolution X-ray image traces the distribution of hot gas which is closely aligned with and extends beyond the radio source, and also in the direction perpendicular to the radio source axis. The X-rays are enhanced at the northern radio lobe and the location of the peak of the CO(3-2)/CO(2-1) line emission, suggesting that the interactions between the jet and cold medium result in the X-ray radiation which excites CO. The shock driven by the jet into the ISM is supersonic with the Mach number of $\mathcal{M} \sim 1.75-2$, creating the cocoon of hot X-rays surrounding the radio source. This result agrees with observations of shocks in other radio galaxies pointing to a prevalent impact of jets on ISM.

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A. Siemiginowska, R. Morganti, G. Fabbiano, E. O'Sullivan, T. Oosterloo, C. Tadhunter, D. Burke. 2025-07-30. Chandra X-ray Observatory study of the X-ray emission of PKS 0023-26 and comparison with recent ALMA results. https://doi.org/10.3847/1538-4357%2Fadf19f

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