AGN feeding and feedback in Fornax A: kinematical analysis of the multi-phase ISM

Maccagni, F. M.; Serra, P.; Gaspari, M.; Kleiner, D.; Morokuma-Matsui, K.; Oosterloo, T. A.; Onodera, M.; Kamphuis, P.; Loi, F.; Thorat, K.; Ramatsoku, M.; Smirnov, O.; White, S. V.

doi:10.48550/arxiv.2108.05247

Cited by 5 publications

(5 citation statements)

References 79 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We found that the ensemble gas observations are consistent with that of Hα+[NII] ensemble detection in other BCGs and BGGs (purple points) from Hamer et al (2014) sample, as well with the prediction from the CCA simulations (purple shaded regions). As for the rotating disks, the ensemble gas detection is slightly deviated to a higher velocity shift compared to the predictions, as expected in rotating-driven systems (see also Maccagni et al 2021). The shift is mainly produced by the large velocity gradient observed in the those disks.…”

Section: Predictions From Cca Simulationssupporting

confidence: 75%

Gas condensation in brightest group galaxies unveiled with MUSE

Olivares

Salomé

Hamer

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

The origin of the cold gas in central galaxies in groups is still a matter of debate. We present Multi-Unit Spectroscopic Explorer (MUSE) observations of 18 optically selected local (z ≤0.017) brightest group galaxies (BGGs) to study the kinematics and distribution of the optical emission-line gas. MUSE observations reveal a distribution of gas morphologies including ten complex networks of filaments extending up to ∼10 kpc to two compact (<3 kpc) and five extended (>5 kpc) disk-dominated structures. Some rotating disks show rings and elongated structures arising from the central disk. The kinematics of the stellar component is mainly rotationdominated, which is very different from the disturbed kinematics and distribution found in the filamentary sources. The ionized gas is kinematically decoupled from the stellar component for most systems, suggesting an external origin for the gas. We also find that the Hα luminosity correlates with the cold molecular gas mass. By exploring the thermodynamical properties of the X-ray atmospheres, we find that the filamentary structures and compact disks are found in systems with small central entropy values, K, and t cool /t eddy ratios. This suggests that, similar to brightest cluster galaxies (BCGs) in cool core clusters, the ionized filaments and the cold gas associated to them are likely formed from hot halo gas condensations via thermal instabilities, which is consistent with the chaotic cold accretion simulations (as shown via the C ratio, Ta t , and k plot). We note that the presence of gaseous rotating disks is more frequent than in BCGs. An explanation for the origin of the gas in those objects is a contribution to gas fueling by wet mergers or group satellites, as qualitatively hinted at by some sources of the present sample. Nonetheless, we discuss the possibility that some extended disks could also be a transition stage in an evolutionary sequence including filaments, extended disks, and compact disks, as described by hot gas condensation models of cooling flows.

show abstract

Section: Predictions From Cca Simulationssupporting

confidence: 75%

Gas condensation in brightest group galaxies unveiled with MUSE

Olivares

Salomé

Hamer

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Although high-resolution 3D simulations of CCA and precipitation predicted a tight correlation between warm Hα filaments and hot "X-ray filaments" [40], the difficulty of removing interfering X-ray features (bubbles, shocks, fronts) has so far hindered the use of direct imaging probes. Our new finding of a tight correlation between Hα and X-ray filaments over multiple scales (Figure 1-2) corroborates models of CCA/precipitation via imaging, in addition to other complementary kinematical probes [27,[41][42][43][44][45][46].…”

supporting

confidence: 81%

Hα and X-ray Surface Brightness Correlation of Filaments in Cooling Flow Clusters

Olivares

Picquenot

et al. 2023

Preprint

View full text Add to dashboard Cite

Massive galaxies in cooling flow clusters display clear evidence of feedback from Active Galactic Nuclei (AGN). Joint X-ray and radio observations have shown that AGN radio jets push aside the surrounding hot gas and form cavities in the hot intracluster medium (ICM). These systems host complex, kiloparsec-scale, multiphase filamentary structures, from warm ionized (10,000 K) to cold molecular (<100 K). These striking clumpy filaments are believed to be a natural outcome of thermally unstable cooling from the hot intracluster medium (ICM), likely triggered by AGN feedback. These structures can also serve as fuel for supermassive black holes (SMBHs). However, the details behind the formation mechanism of the filaments are still unknown, and the relationship between the gas phases of different temperature is poorly understood. By using a novel method of blind image decomposition, we have isolated the hot phase of the X-ray filaments, which was blended with the bright diffuse ICM (and contaminated by cavities and fronts), to unveil its relation with the warm phase. We have discovered a tight positive correlation between the X-ray surface brightness and the H\alpha surface brightness of the filaments, in a sample of seven X-ray bright cooling-flow clusters, covering scales of 5--70 kpc. This discovery provides major evidence supporting theoretical models of Chaotic Cold Accretion and precipitation, in which the turbulent multiphase condensation and excitation mechanisms shape the tight co-evolution of the hot and warm filaments.

show abstract

“…ics from a CCA-feeding cycle, and are also comparable to those observed in several other galaxies (red points). A small deviation is that our sample shows slightly larger mean in the broadening axis, as we are including galaxies with rotation and AGN outbursts (e.g., NGC 4261), both shown to enhance the k-plot loci toward the upperright sector (Maccagni et al 2021). Moreover, our cool gas is often under-resolved (especially with SOFIA), meaning that we are only able to capture larger associations of clouds, rather than single elements, thus shifting the points toward the top region of the more ensemblelike regime, where clouds tend to drift in the macro-scale weather.…”

Section: Top-down Condensationmentioning

confidence: 83%

“…ALMA observations have detected CO emission and absorption in massive elliptical galaxies at the center of X-ray bright groups (David et al 2014;Temi et al 2018;Rose et al 2019;Maccagni et al 2021;North et al 2021). For the archetypal group NGC 5044 the CO observations suggest that the molecular gas is indeed distributed in several clouds apparently orbiting within ∼2 kpc from the center.…”

Section: Introductionmentioning

confidence: 99%

Probing multiphase gas in local massive elliptical galaxies via multiwavelength observations

Temi,

Gaspari,

Brighenti

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

We investigate the cold and warm gas content, kinematics, and spatial distribution of six local massive elliptical galaxies to probe the origin of the multiphase gas in their atmospheres. We report new observations, including SOFIA [CII], ALMA CO, MUSE Hα+[NII] and VLA radio observations. These are complemented by a large suite of multiwavelength archival datasets, including thermodynamical properties of the hot gas and radio jets, which are leveraged to investigate the role of AGN feeding/feedback in regulating the multiphase gas content. Our galaxy sample shows a significant diversity in cool gas content, spanning filamentary and rotating structures. In our non-central galaxies, the distribution of such gas is often concentrated, at variance with the more extended features observed in central galaxies. Misalignment between the multiphase gas and stars suggest that stellar mass loss is not the primary driver. A fraction of the cool gas might be acquired via galaxy interactions, but we do not find quantitative evidence of mergers in most of our systems. Instead, key evidence supports the origin via condensation out of the diffuse halo. Comparing with Chaotic Cold Accretion (CCA) simulations, we find that our cool gas-free galaxies are likely in the overheated phase of the self-regulated AGN cycle, while for our galaxies with cool gas the k-plot and AGN power correlation corroborate the phase of CCA feeding in which the condensation rain is triggering more vigorous AGN heating. The related C-ratio further shows that central/non-central galaxies are expected to generate an extended/inner rain, consistent with our sample.

show abstract

AGN feeding and feedback in Fornax A: kinematical analysis of the multi-phase ISM

Cited by 5 publications

References 79 publications

Gas condensation in brightest group galaxies unveiled with MUSE

Gas condensation in brightest group galaxies unveiled with MUSE

Hα and X-ray Surface Brightness Correlation of Filaments in Cooling Flow Clusters

Probing multiphase gas in local massive elliptical galaxies via multiwavelength observations

Contact Info

Product

Resources

About