Powerful AGN jets and unbalanced cooling in the hot atmosphere of IC 4296

Grossová, Romana; Werner, Norbert; Rajpurohit, K.; Mernier, F.; Lakhchaura, Kiran; Gabányi, K. É.; Canning, R. E. A.; Nulsen, P. E. J.; Massaro, F.; Sun, Ming; Connor, Thomas; King, A. L.; Allen, S. W.; Frisbie, R.; Donahue, M.; Fabian, A. C.

doi:10.1093/mnras/stz1728

Cited by 28 publications

(32 citation statements)

References 65 publications

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“…This scenario looks very similar to some galaxy clusters, that are shown to host giant cavities, with lobes extending over the cooling region (e.g., Gitti et al, 2007). Some analyses of singular groups already suggested that jets extending well over the core could violate the standard AGN feeding-feedback model (e.g., O'Sullivan et al, 2011;Grossová et al, 2019). However, this is the first work to prove that a significant fraction of the galaxy groups population effectively shows hints that support this scenario.…”

Section: Discussionsupporting

confidence: 66%

“…We then argue that the biggest radio galaxies are found in the centre of galaxy groups. This was already hinted by multiple works on giant radio galaxies (e.g., Mack et al 1998;Machalski et al 2004;Subrahmanyan et al 2008;Chen et al 2012;Grossová et al 2019;Cantwell et al 2020, and references therein). However, this is the first time that they are included as sources in a large sample of groups, and their link to the environment is studied with respect to "classical" radio sources.…”

Section: Discussionmentioning

confidence: 78%

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The relation between the diffuse X-ray luminosity and the radio power of the central AGN in galaxy groups

Pasini

Brüggen

Gasperin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Our understanding of how AGN feedback operates in galaxy clusters has improved in recent years owing to large efforts in multi-wavelength 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 VLA 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 ICM could be less suppressed by AGN heating. We conclude that the feedback processes that operate in galaxy clusters are also effective in groups.

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Section: Discussionsupporting

confidence: 66%

Section: Discussionmentioning

confidence: 78%

The relation between the diffuse X-ray luminosity and the radio power of the central AGN in galaxy groups

Pasini

Brüggen

Gasperin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Our indexes are consistent (1-1.5σ) with those from Best et al (1999) (also shown in Table 1). The lobes present a steep SED, consistent with the optically thin synchrotron emission of the jets (Best et al 1999;Laing & Bridle 2013;Nyland et al 2017;Ruffa et al 2019;Grossová et al 2019), while the AGN core SED is flatter, which is consistent with optically thicker (self-absorbed) synchrotron emission (Best et al 1999;Ruffa et al 2019;Grossová et al 2019).…”

Section: Active Galactic Nucleus Continuum Emissionsupporting

confidence: 70%

“…Our results are within the range of spectral indexes found in previous work. The typical spectral index of optically thin synchrotron emission (which corresponds to jets) is in the range of 0.5 α 1.5 in the local Universe (Laing & Bridle 2013;Nyland et al 2017;Ruffa et al 2019;Grossová et al 2019) and 1 α 2 for galaxies at z > 2, with higher values being rarer (Carilli et al 1997;Best et al 1999;Falkendal et al 2019). For the optically thick emission (which corresponds to the core), −0.5 α 0.5 is found in the local Universe (Ruffa et al 2019;Grossová et al 2019) and −1 α 1 is found at z > 2, with most of the measurements being α > 0.5 (Carilli et al 1997;Athreya et al 1997;Best et al 1999;Falkendal et al 2019).…”

Section: Active Galactic Nucleus Continuum Emissionmentioning

confidence: 99%

Massive molecular gas reservoir around the central AGN in the CARLA J1103 + 3449 cluster at z = 1.44

Markov

Mei

Salomé

et al. 2020

A&A

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Passive early-type galaxies dominate cluster cores at z ≲ 1.5. At higher redshift, cluster core galaxies are observed to have on-going star-formation, which is fueled by cold molecular gas. We measured the molecular gas reservoir of the central region around the radio-loud active galactic nucleus (AGN) in the cluster CARLA J1103 + 3449 at z = 1.44 using NOEMA. The AGN synchrotron emission dominates the continuum emission at 94.48 GHz, and we measured its flux at the AGN position and at the position of two radio jets. Combining our measurements with published results over the range 4.71–94.5 GHz, and assuming Ssynch ∝ ν−α, we obtain a flat spectral index of α = 0.14 ± 0.03 for the AGN core emission, and a steeper index of α = 1.43 ± 0.04 and α = 1.15 ± 0.04 at positions close to the western and eastern lobes, respectively. The total spectral index is α = 0.92 ± 0.02 over the range 73.8 MHz–94.5 GHz. We detect two CO(2–1) emission lines, both blueshifted with respect to the AGN. Their emission corresponds to two regions, ~17 kpc southeast and ~14 kpc southwest of the AGN, not associated with galaxies. In these two regions, we find a total massive molecular gas reservoir of Mgastot = 3.9 ± 0.4 × 1010 M⊙, which dominates (≳60%) the central total molecular gas reservoir. These results can be explained by massive cool gas flows in the center of the cluster. The AGN early-type host is not yet quenched; its star formation rate is consistent with being on the main sequence of star-forming galaxies in the field (star formation rate ~30–140 M⊙ yr−1), and the cluster core molecular gas reservoir is expected to feed the AGN and the host star formation before quiescence. The other confirmed cluster members show star formation rates at ~2σ below the field main sequence at similar redshifts and do not have molecular gas masses larger than galaxies of similar stellar mass in the field.

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“…Additionally, another complication with the lower X-ray luminosity systems is that one cannot assume that any undetected X-ray cavities are well traced by the radio lobes, since such systems often host high-power radio sources whose lobes extend far beyond the dense atmospheres (e.g. NGC 4261, IC4296, IC1459, NGC 1600, NGC 5090, UGC11294, ARP308; Diehl & Statler 2008;Sun 2009;Cavagnolo et al 2010;Duţan & Caramete 2015;Kolokythas et al 2018;Ruffa et al 2019;Grossová et al 2019). Table 3 shows that H α filaments are mostly found in groups and ellipticals where the radio emission is filling the X-ray cavities (the exceptions are NGC 499, NGC 410, and NGC 4104, see Table 3).…”

Section: Group and Ellipticals Subsamplementioning

confidence: 99%

LOFAR observations of X-ray cavity systems

Bîrzan

Rafferty

Brüggen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We present LOFAR observations at 120–168 MHz of 42 systems with possible X-ray cavities in their hot atmosphere, of which 17 are groups or ellipticals, 19 are nearby clusters (z < 0.3), and six are higher redshift clusters (z > 0.3). The X-ray cavities, formed by the radio lobes of the central active galactic nucleus (AGN), are evidence of radio-mode AGN feedback. In the groups and ellipticals sample, half of the systems have X-ray cavities for which no associated lobe emission was detected. Conversely, we report the discovery of large radio lobes in NGC 6338, extending far beyond the emission reported previously in the literature. In the case of the nearby clusters, our observations show that there is little low-frequency radio emission that extends beyond the cavities (e.g. MS 0735.6+7421, A2052). For the first time, we report secure cavity-radio associations in 2A 0335+096, ZwCl 2701, and ZwCl 8276 that strengthens their interpretation as AGN-created cavities. However, in some known cavity systems (e.g. A1795 and ZwCl 3146) we report the lack of detectable low-frequency radio emission associated with the cavities. Our sample of higher redshifts systems is small, and unfortunately the present LOFAR observations are not able to resolve the lobes in many of them. Nevertheless, our sample represents one of the best available for investigating the connection between radio and jet power in radio-mode AGN feedback.

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Powerful AGN jets and unbalanced cooling in the hot atmosphere of IC 4296

Cited by 28 publications

References 65 publications

The relation between the diffuse X-ray luminosity and the radio power of the central AGN in galaxy groups

The relation between the diffuse X-ray luminosity and the radio power of the central AGN in galaxy groups

Massive molecular gas reservoir around the central AGN in the CARLA J1103 + 3449 cluster at z = 1.44

LOFAR observations of X-ray cavity systems

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