AGN Feedback in Galaxy Groups: A Detailed Study of X-Ray Features and Diffuse Radio Emission in IC 1262

ABSTRACT Our understanding of how active galactic nucleus feedback operates in galaxy clusters has improved in recent years owing to large efforts in multiwavelength observations and hydrodynamical simulations. However, it is much less clear how feedback operates in galaxy groups, which have shallower gravitational potentials. In this work, using very deep Very Large Array and new MeerKAT observations from the MIGHTEE survey, we compiled a sample of 247 X-ray selected galaxy groups detected in the COSMOS field. We have studied the relation between the X-ray emission of the intra-group medium and the 1.4 GHz radio emission of the central radio galaxy. For comparison, we have also built a control sample of 142 galaxy clusters using ROSAT and NVSS data. We find that clusters and groups follow the same correlation between X-ray and radio emission. Large radio galaxies hosted in the centres of groups and merging clusters increase the scatter of the distribution. Using statistical tests and Monte Carlo simulations, we show that the correlation is not dominated by biases or selection effects. We also find that galaxy groups are more likely than clusters to host large radio galaxies, perhaps owing to the lower ambient gas density or a more efficient accretion mode. In these groups, radiative cooling of the intra-cluster medium could be less suppressed by active galactic nucleus heating. We conclude that the feedback processes that operate in galaxy clusters are also effective in groups.

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SEARCH FOR PULSED RADIO EMISSION FROM X-RAY DIM ISOLATED NEUTRON STARS AT DECAMETER WAVELENGTHS

Radio Physics and Radio Astronomy ◽

10.1615/radiophysicsradioastronomy.v2.i1.20 ◽

2011 ◽

Vol 2 (1) ◽

pp. 15-21 ◽

Cited By ~ 1

Author(s):

V. V. Zakharenko ◽

A. V. Markova ◽

Y. Y. Vasylyeva

Keyword(s):

Radio Emission ◽

Neutron Stars ◽

X Ray

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Variable Radio Emission from X-Ray Sources

International Astronomical Union Colloquium ◽

10.1017/s0252921100032905 ◽

1971 ◽

Vol 15 ◽

pp. 173-175 ◽

Cited By ~ 1

Author(s):

L. L. E. Braes ◽

G. K. Miley

Keyword(s):

Radio Emission ◽

Aperture Synthesis ◽

Electromagnetic Spectrum ◽

Radio Telescopes ◽

Low Resolution ◽

X Ray ◽

Synthesis Technique ◽

Variable Radio

Dr. KELLOGG has just described some exciting new observations of X-ray sources made with the UHURU satellite. We shall now move some nine orders of magnitude in wavelength to the opposite end of the electromagnetic spectrum and report measurements of weak radio emission from some of the objects he mentioned. For the detection of weak sources most radio telescopes are not noise limited, but are confusion limited by their low resolution. The aperture synthesis technique minimizes this problem because it enables one to pinpoint the position of weak sources to the order of one second of arc.

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Supermassive Black Hole feedback in early type galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320004081 ◽

2020 ◽

Vol 15 (S359) ◽

pp. 119-125

Author(s):

W. Forman ◽

C. Jones ◽

A. Bogdan ◽

R. Kraft ◽

E. Churazov ◽

...

Keyword(s):

Dark Matter Halo ◽

Scaling Relations ◽

Radio Sources ◽

Early Type ◽

X Ray ◽

Galaxy Groups ◽

Sufficient Energy ◽

The Galaxy ◽

Simple Scaling ◽

Halo Masses

AbstractOptically luminous early type galaxies host X-ray luminous, hot atmospheres. These hot atmospheres, which we refer to as coronae, undergo the same cooling and feedback processes as are commonly found in their more massive cousins, the gas rich atmospheres of galaxy groups and galaxy clusters. In particular, the hot coronae around galaxies radiatively cool and show cavities in X-ray images that are filled with relativistic plasma originating from jets powered by supermassive black holes (SMBH) at the galaxy centers. We discuss the SMBH feedback using an X-ray survey of early type galaxies carried out using Chandra X-ray Observatory observations. Early type galaxies with coronae very commonly have weak X-ray active nuclei and have associated radio sources. Based on the enthalpy of observed cavities in the coronae, there is sufficient energy to “balance” the observed radiative cooling. There are a very few remarkable examples of optically faint galaxies that are 1) unusually X-ray luminous, 2) have large dark matter halo masses, and 3) have large SMBHs (e.g., NGC4342 and NGC4291). These properties suggest that, in some galaxies, star formation may have been truncated at early times, breaking the simple scaling relations.

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Some Features of the X-Ray and Radio Emission from OH Megamaser Galaxies

Astrophysics ◽

10.1007/s10511-005-0033-4 ◽

2005 ◽

Vol 48 (3) ◽

pp. 355-362 ◽

Cited By ~ 1

Author(s):

R. A. Kandalyan

Keyword(s):

Radio Emission ◽

X Ray

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Physical implications of the X-ray properties of galaxy groups and clusters

Monthly Notices of the Royal Astronomical Society ◽

10.1046/j.1365-8711.2002.05044.x ◽

2002 ◽

Vol 330 (2) ◽

pp. 329-343 ◽

Cited By ~ 129

Author(s):

Arif Babul ◽

Michael L. Balogh ◽

Geraint F. Lewis ◽

Gregory B. Poole

Keyword(s):

X Ray ◽

Galaxy Groups

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Tidal disruption events seen in the XMM-Newton slew survey

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317001776 ◽

2016 ◽

Vol 12 (S324) ◽

pp. 123-126

Author(s):

Richard Saxton ◽

S. Komossa ◽

Andrew Read ◽

Paulina Lira ◽

Kate D. Alexander ◽

...

Keyword(s):

Radio Emission ◽

Real Time ◽

Power Law ◽

Early Phase ◽

Classical Model ◽

Thermal Processes ◽

Tidal Disruption ◽

X Ray ◽

Hard Power ◽

Sky Survey

AbstractXMM-Newton performs a survey of the sky in the 0.2-12 keV X-ray band while slewing between observation targets. The sensitivity in the soft X-ray band is comparable with that of the ROSAT all-sky survey, allowing bright transients to be identified in near real-time by a comparison of the flux in both surveys. Several of the soft X-ray flares are coincident with galaxy nuclei and five of these have been interpreted as candidate tidal disruption events (TDE). The first three discovered had a soft X-ray spectrum, consistent with the classical model of TDE, where radiation is released during the accretion phase by thermal processes. The remaining two have an additional hard, power-law component, which in only one case was accompanied by radio emission. Overall the flares decay with the classical index of t−5/3 but vary greatly in the early phase.

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