SIMBAD references

2018MNRAS.477.3461B - Mon. Not. R. Astron. Soc., 477, 3461-3468 (2018/July-1)

Discovery of large-scale diffuse radio emission in low-mass galaxy cluster Abell 1931.

BRUGGEN M., RAFFERTY D., BONAFEDE A., VAN WEEREN R.J., SHIMWELL T., INTEMA H., ROTTGERING H., BRUNETTI G., DI GENNARO G., SAVINI F., WILBER A., O'SULLIVAN S., ENSSLIN T.A., DE GASPERIN F. and HOEFT M.

Abstract (from CDS):

Extended, steep-spectrum radio synchrotron sources are pre-dominantly found in massive galaxy clusters as opposed to groups. LOFAR Two-Metre Sky Survey images have revealed a diffuse, ultra-steep-spectrum radio source in the low-mass cluster Abell 1931. The source has a fairly irregular morphology with the largest linear size of about 550 kpc. The source is only seen in LOFAR observations at 143 MHz and Giant Metre Radio Telescope observations at 325 MHz. The spectral index of the total source between 143 and 325 MHz is α143325 = -2.86 ±0.36. The source remains invisible in Very Large Array (1-2 GHz) observations as expected given the spectral index. Chandra X-ray observations of the cluster revealed a bolometric luminosity of LX = (1.65 ± 0.39) x 1043 erg s–1 and a temperature of 2.92–0.87+1.89 keV which implies a mass of around ∼1014 M. We conclude that the source is a remnant radio galaxy that has shut off around 200 Myr ago. The brightest cluster galaxy, a radio-loud elliptical galaxy, could be the source for this extinct source. Unlike remnant sources studied in the literature, our source has a steep spectrum at low radio frequencies. Studying such remnant radio galaxies at low radio frequencies is important for understanding the scarcity of such sources and their role in feedback processes.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): acceleration of particles - intergalactic medium - radiation mechanisms: non-thermal - radio continuum: galaxies - X-rays: galaxies: clusters

Simbad objects: 16

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2021.12.07-08:07:09

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