Volume 660, April 2022
|Number of page(s)||9|
|Published online||05 April 2022|
Detection of a radio-filled X-ray cavity within the interstellar medium of NGC 5141
Dipartimento di Fisica e Astronomia, Alma Mater Studiorum, Università degli Studi di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy
2 INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna (OAS), Area della Ricerca CNR, Via Gobetti 101, 40129 Bologna, Italy
3 INAF, Istituto di Radioastronomia di Bologna (IRA), Via Gobetti 101, 40129 Bologna, Italy
4 University of California Observatories/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
Accepted: 28 January 2022
We present the first Chandra detection of a single X-ray cavity within the interstellar medium of the small Fanaroff-Riley type I radio galaxy NGC 5141. The X-ray surface brightness depression, located ≈4 kpc away from the galaxy center, is projected on the northern radio lobe, which is completely contained within the galaxy. The thermal gas surrounding the cavity, which extends to ≃20 kpc, has a bolometric X-ray luminosity (0.1–100 keV) of LX ≈ 2 × 1040 erg s−1 and a temperature of kT ≈ 0.8 keV. We calculated the total energy (Ecav = 4PV ≈ 1055 erg) required to inflate the cavity and its age (tcav ≈ 9 Myrs), assuming that it is filled with relativistic particles and rises buoyantly. The inferred total cavity power is as low as Pcav = Ecav/tcav ≈ 6 × 1040 erg s−1, which is the lowest one among the radio-filled systems. Comparing Pcav to the bolometric X-ray luminosity (i.e., the cooling luminosity), we conclude that NGC 5141’s central active galactic nucleus can heat the interstellar medium and balance its cooling luminosity, confirming that the Pcav − Lcool relation, mainly tested on groups and clusters, also works for such a low-power system.
Key words: galaxies: individual: NGC 5141 / galaxies: active / galaxies: elliptical and lenticular, cD / galaxies: ISM / galaxies: jets / X-rays: ISM
© ESO 2022
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