Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

Pasini, Thomas; Finoguenov, A.; Brüggen, M.; Gaspari, M.; Gasperin, F. de; Gozaliasl, G.

doi:10.1093/mnras/stab1451

Cited by 19 publications

(13 citation statements)

References 97 publications

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“…The range is the same as for the sample of BCG radio galaxies studied in P21. As also found in P21 and other similar works (e.g., Pasini et al 2020Pasini et al , 2021, there is a trend for stronger radio galaxies to be hosted in more luminous (i.e., more massive) clusters. However, observational limitations, especially in the radio band, affect our results.…”

Section: Characterization Of the Source Classification Through Lofar ...supporting

confidence: 83%

The eROSITA Final Equatorial-Depth Survey (eFEDS)

Bülbül

Liu

Pasini

et al. 2022

A&A

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Aims. The eROSITA Final Equatorial-Depth Survey (eFEDS), executed during the performance verification phase of the Spectrum-Roentgen-Gamma (SRG)/eROSITA telescope, was completed in November 2019. One of the science goals of this survey is to demonstrate the ability of eROSITA to detect samples of clusters and groups at the final depth of the eROSITA all-sky survey. Methods. Because of the sizeable (≈26″ HEW FOV average) point-spread function of eROSITA, high-redshift clusters of galaxies or compact nearby groups hosting bright active galactic nuclei (AGN) can be misclassified as point sources by the source detection algorithms. A total of 346 galaxy clusters and groups in the redshift range of 0.1 < z < 1.3 were identified based on their red sequenc in the eFEDS point source catalog. Results. We examine the multiwavelength properties of these clusters and groups to understand the potential biases in our selection process and the completeness of the extent-selected sample. We find that the majority of the clusters and groups in the point source sample are indeed underluminous and compact compared to the extent-selected sample. Their faint X-ray emission, well below the flux limit of the extent-selected eFEDS clusters, and their compact X-ray emission are likely to be the main reason for this misclassification. In the sample, we confirm that 10% of the sources host AGN in their brightest cluster galaxies (BCGs) through optical spectroscopy and visual inspection. By studying their X-ray, optical, infrared, and radio properties, we establish a method for identifying clusters and groups that host AGN in their BCGs. We successfully test this method on the current point source catalog through the Sloan Digital Sky Survey optical spectroscopy and find eight low-mass clusters and groups with active radio-loud AGN that are particularly bright in the infrared. They include eFEDS J091437.8+024558, eFEDS J083520.1+012516, and eFEDS J092227.1+043339 at redshifts 0.3−0.4. Conclusions. This study helps us to characterize and understand our selection process and assess the completeness of the eROSITA extent-selected samples. The method we developed will be used to identify high-redshift clusters, AGN-dominated groups, and low-mass clusters that are misclassified in the future eROSITA all-sky survey point source catalogs.

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Section: Characterization Of the Source Classification Through Lofar ...supporting

confidence: 83%

The eROSITA Final Equatorial-Depth Survey (eFEDS)

Bülbül

Liu

Pasini

et al. 2022

A&A

View full text Add to dashboard Cite

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“…We then separate groups of three or more galaxies into groups where the AGN is the brightest and groups where the AGN is not the brightest. If the AGN host is the Brightest Group Galaxy (BGG), it is very likely that it has undergone an evolution defined largely by hierarchical structure formation of merging galaxies (De Lucia & Blaizot 2007), where it has been able to grow more massive than a typical large elliptical galaxy by accreting satellite galaxies that fall into the gravitational potential of the group (Gozaliasl et al 2019;Pasini et al 2021).…”

Section: The Frequency Of Agn In Different Environmentsmentioning

confidence: 99%

“…This could be indicative of a difference in the gas density and dynamics of the environments of these two kinds of galaxies. Additionally, it could indicate that bent and unbent AGN exist in different types of cluster or group galaxies-while unbent AGN typically exist in the brightest group or cluster galaxies (Pasini et al 2021), bent AGN may exist in other galaxies that are moving through their environment at higher velocities, allowing for their jets to be bent by ram pressure. Alternatively, the medium in environments where bent jets are found could be undergoing bulk motion, causing the jets to appear bent.…”

Section: Introductionmentioning

confidence: 99%

How Does Environment Affect the Morphology of Radio AGN?

Morris¹,

Wilcots²,

Hooper³

et al. 2022

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Galaxies hosting Active Galactic Nuclei (AGN) with bent radio jets are used as tracers of dense environments, such as galaxy groups and clusters. The assumption behind using these jets is that they are bent under ram pressure from a dense, gaseous medium through which the host galaxy moves. However, there are many AGN in groups and clusters with jets that are not bent, which leads us to ask: why are some AGN jets affected so much by their environment while others are seemingly not? We present the results of an environmental study on a sample of 185 AGN with bent jets and 191 AGN with unbent jets in which we characterize their environments by searching for neighboring galaxies using a Friends-of-Friends algorithm. We find that AGN with bent jets are indeed more likely to reside in groups and clusters, while unbent AGN are more likely to exist in singles or pairs. When considering only AGN in groups of three or more galaxies, we find that bent AGN are more likely to exist in halos with more galaxies than unbent AGN. We also find that unbent AGN are more likely than bent AGN to be the brightest group galaxy. Additionally, groups hosting AGN with bent jets have a higher density of galaxies than groups hosting unbent AGN. Curiously, there is a population of AGN with bent jets that are in seemingly less dense regions of space, indicating they may be embedded in a cosmic web filament. Overall, our results indicate that bent doubles are more likely to exist in in larger, denser, and less relaxed environments than unbent doubles, potentially linking a galaxy’s radio morphology to its environment.

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“…We then separate groups of 3 or more galaxies into groups where AGN are the brightest and groups where the AGN is not the brightest. If the AGN host is the Brightest Group Galaxy (BGG), it is very likely that it has undergone an evolution defined largely by hierarchical structure formation of merging galaxies (De Lucia & Blaizot 2007), where it has been able to grow more massive than a typical large elliptical galaxy by accreting satellite galaxies that fall into the gravitational potential of the group (Gozaliasl et al 2019;Pasini et al 2021).…”

Section: The Frequency Of Agn In Different Environmentsmentioning

confidence: 99%

How does environment affect the morphology of radio AGN?

Morris,

Wilcots,

Hooper

et al. 2022

Preprint

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Galaxies hosting Active Galactic Nuclei (AGN) with bent radio jets are used as tracers of dense environments, such as galaxy groups and clusters. The assumption behind using these jets is that they are bent under ram pressure from a dense, gaseous medium through which the host galaxy moves. However, there are many AGN in groups and clusters with jets that are not bent, which leads us to ask: why are some AGN jets affected so much by their environment while others are seemingly not? We present the results of an environmental study on a sample of 185 AGN with bent jets and 191 AGN with unbent jets in which we characterize their environments by searching for neighboring galaxies using a Friends-of-Friends algorithm. We find that AGN with bent jets are indeed more likely to reside in groups and clusters, while unbent AGN are more likely to exist in singles or pairs. When considering only AGN in groups of 3 or more galaxies, we find that bent AGN are more likely to exist in halos with more galaxies than unbent AGN. We also find that unbent AGN are more likely than bent AGN to be the brightest group galaxy. Additionally, groups hosting AGN with bent jets have a higher density of galaxies than groups hosting unbent AGN. Curiously, there is a population of AGN with bent jets that are in seemingly less dense regions of space, indicating they may be embedded in a cosmic web filament. Overall, our results indicate that bent doubles are more likely to exist in in larger, denser, and less relaxed environments than unbent doubles, potentially linking a galaxy's radio morphology to its environment.

show abstract

Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

Cited by 19 publications

References 97 publications

The eROSITA Final Equatorial-Depth Survey (eFEDS)

The eROSITA Final Equatorial-Depth Survey (eFEDS)

How Does Environment Affect the Morphology of Radio AGN?

How does environment affect the morphology of radio AGN?

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