An X-ray cooling-core cluster surrounding a low power Compact Steep Spectrum Radio source 1321+045

Abstract

We discovered an X-ray cluster in a Chandra observation of the compact steep spectrum (CSS) radio source 1321+045 (z=0.263). CSS sources are thought to be young radio objects at the beginning of their evolution and can potentially test the cluster heating process. 1321+045 is a relatively low luminosity source and its morphology consists of two radio lobes on the opposite sides of a radio core with no evidence for jets or hotspots. The optical emission line ratios are consistent with an interstellar medium (ISM) dominated by AGN-photoionization with a small contribution from star formation, and no contributions from shocks. Based on these ratios, we classify 1321+045 as a low excitation galaxy (LEG) and suggest that its radio activity is in a coasting phase. The X-ray emission associated with the radio source is detected with 36.1+/-8.3 counts, but the origin of this emission is highly uncertain. The current X-ray image of the cluster does not show any signatures of a radio source impact on the cluster medium. Chandra detects the cluster emission at >3 sigma level out to ~60 arcsec (~240 kpc). We obtain the best fit beta model parameters of the surface brightness profile of beta=0.58+/-0.2 and a core radius of 9.4^{+1.1}_{-0.9} arcsec. The average temperature of the cluster is equal to kT=4.4^{+0.5}_{-0.3} keV, with a temperature and cooling profile indicative of a cooling core. We measure the cluster luminosity L_(0.5-2 keV)=3x10^{44} erg s^{-1} and mass 1.5x10^{14} M_sun.

4 pages, 1 figure, 1 table, accepted for publication in ApJ Letters

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Cited by in corpus (7)

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• Testing for Shock-Heated X-ray Gas Around Compact Steep Spectrum Radio Galaxies
• Dichotomy in the population of young AGN: optical, radio and X-ray properties
• The cluster-central compact steep-spectrum radio galaxy 1321+045
• 1321+045: a Compact Steep Spectrum radio source in a cool-core galaxy cluster
• Chandra X-ray Observatory study of the X-ray emission of PKS 0023-26 and comparison with recent ALMA results