A Link Between Ram Pressure Stripping and Active Galactic Nuclei

Ricarte, Angelo; Tremmel, Michael; Natarajan, Priyamvada; Quinn, Thomas

doi:10.48550/arxiv.2003.05950

Cited by 4 publications

(4 citation statements)

References 44 publications

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“…Moreover, a long-lasting and population-averaged environmental obstruction to AGN activity is not necessarily in contrast to previous findings which have shown that higher density cluster environments can actually trigger enhanced BH activity in satellites for a period of time, which in some instances can in turn act to eventually quench the satellites (e.g. McGee 2013;Poggianti et al 2017;Ricarte et al 2020).…”

Section: On the Role Of Massive Hosts And Of Agn Feedback In Massive ...contrasting

confidence: 62%

Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing

Donnari,

Pillepich,

Joshi

et al. 2020

Preprint

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We use the IllustrisTNG hydrodynamical simulations to show how the fractions of quenched galaxies vary across different environments and cosmic time, and to quantify the role AGN feedback and pre-processing play in quenching group and cluster satellites. At z = 0, we select galaxies with M stars = 10 9−12 M residing within ( R 200c ) massive groups and clusters of total host mass M 200c = 10 13−15.2 M in TNG100 and TNG300. The model predicts a quenched fraction of ∼70-90 per cent (on average) for centrals and satellites of mass 10 10.5 M , regardless of host mass, cosmic time (0 z 0.5), cluster-centric distance and time since infall in the z = 0 host. Low-mass central galaxies ( 10 10 M ), on the other hand, are rarely quenched unless they become members of groups (10 13−14 M ) or clusters ( 10 14 M ), where the quenched fraction rises to ∼ 80 per cent. Typically, the fraction of low-mass passive galaxies is higher closer to the host center and for progressively more massive hosts. The population of low-mass satellites accreted more than ∼ 4-6 Gyr ago in massive hosts is almost entirely passive, thus suggesting an upper limit for the time needed for environmental quenching to occur. In fact, about 30 per cent of group and cluster satellites that are quenched at z = 0 were already quenched before falling into their current host, and the bulk of them quenched as early as 4 to 10 billion years ago. For low-mass galaxies (M stars 10 10−10.5 M ), this is due to pre-processing, whereby current satellites may have been members of other hosts, and hence have undergone environmental processes, before falling into their final host, this mechanism being more common and more effective for the purposes of quenching for satellites found today in more massive hosts. On the other hand, massive galaxies quench on their own and because of AGN feedback, regardless of whether they are centrals or satellites.

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Section: On the Role Of Massive Hosts And Of Agn Feedback In Massive ...contrasting

confidence: 62%

Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing

Donnari,

Pillepich,

Joshi

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…Our findings appear to be in contrast to previous studies that have concluded that higher density cluster environments actually trigger enhanced BH activity in satellites for a period of time, which in turn acts to eventually quench the satellites (e.g. see McGee 2013;Poggianti et al 2017;Ricarte et al 2020). However, it should be kept in mind that the results shown in Fig.…”

Section: The Role Of Agn Feedbackcontrasting

confidence: 99%

The fate of disk galaxies in IllustrisTNG clusters

Joshi,

Pillepich,

Nelson

et al. 2020

Preprint

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We study the stellar morphological evolution of disk galaxies within clusters in the TNG50 and TNG100 runs from the IllustrisTNG simulation suite. We select satellites of masses 10 9.7 ≤ M * ,z=0 /M ≤ 10 11.6 residing in clusters of total masses 10 14 M 200c,z=0 /M ≤ 10 14.6 at z = 0 and study those that were disks at accretion according to a kinematic morphology indicator (the circularity fraction). The galaxies' histories are traced from the time of accretion to z = 0 and compared to a control sample of central galaxies mass-matched at the time of accretion.Most cluster disks become non-disky by z = 0, in stark contrast with the control disks, of which a significant fraction remains disky over the same timescales. The transformation to non-disky morphologies is accompanied by gas removal and star formation quenching for both cluster and control galaxies. However, cluster disks that become non-disky by z = 0 have lost dark matter (DM) mass and show little growth or a loss of stellar mass, whereas the corresponding control disks show significant growth in both components. Most cluster satellites change their morphologies on similar timescales regardless of stellar mass, in ∼ 0.5 − 4 billion years after accretion. Cluster disks that have had more numerous and closer pericentric passages show the largest change in morphology. Morphological change in both cluster and control disks requires the presence of a gravitational perturbation to drive stellar orbits to non-disky configurations, along with gas removal/heating to prevent replenishment of the disk through continued star-formation. For cluster disks, the perturbation is in the form of impulsive tidal shocking at pericentres and not tidal stripping of the outer disk stellar material, whereas for control disks, a combination of mergers and AGN feedback appears to be the key driving force behind morphological transformations.

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“…Can observations of the dynamics of the gas in the disk in high resolution help us to explain the elevated incidence of AGN in ram pressure affected galaxies observed by Poggianti et al (2017b)? Some simulations support that ram pressure stripping can drive gravitationally bound gas inward, accelerating black hole accretion rates and possibly triggering AGN (Tonnesen & Bryan 2009;Ramos-Martínez et al 2018;Ricarte et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Molecular gas filaments and fallback in the ram pressure stripped Coma spiral NGC 4921

Cramer,

Kenney,

Tonnesen

et al. 2021

Preprint

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We investigate the effects of ram pressure on the molecular ISM in the disk of the Coma cluster galaxy NGC 4921, via high resolution CO observations. We present 6 resolution CARMA CO(1-0) observations of the full disk, and 0.4 resolution ALMA CO(2-1) observations of the leading quadrant, where ram pressure is strongest. We find evidence for compression of the dense interstellar medium (ISM) on the leading side, spatially correlated with intense star formation activity in this zone. We also detect molecular gas along kiloparsec-scale filaments of dust extending into the otherwise gas stripped zone of the galaxy, seen in HST images. We find the filaments are connected kinematically as well as spatially to the main gas ridge located downstream, consistent with cloud decoupling inhibited by magnetic binding, and inconsistent with a simulated filament formed via simple ablation. Furthermore, we find several clouds of molecular gas ∼ 1 − 3 kpc beyond the main ring of CO that have velocities which are blueshifted by up to 50 km s −1 with respect to the rotation curve of the galaxy. These are some of the only clouds we detect that do not have any visible dust extinction associated with them, suggesting that they are located behind the galaxy disk midplane and are falling back towards the galaxy. Simulations have long predicted that some gas removed from the galaxy disk will fall back during ram pressure stripping. This may be the first clear observational evidence of gas re-accretion in a ram pressure stripped galaxy.

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A Link Between Ram Pressure Stripping and Active Galactic Nuclei

Cited by 4 publications

References 44 publications

Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing

Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing

The fate of disk galaxies in IllustrisTNG clusters

Molecular gas filaments and fallback in the ram pressure stripped Coma spiral NGC 4921

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