A MeerKAT view of pre-processing in the Fornax A group

Kleiner, D.; Serra, P.; Maccagni, F. M.; Venhola, Aku; Morokuma-Matsui, Kana; Peletier, Reynier F.; Iodice, E.; Raj, M. A.; Blok, W. J. G. de; Comrie, A.; Józsa, G. I. G.; Kamphuis, P.; Loni, A.; Loubser, S. I.; Molnár, D. Cs.; Passmoor, S. S.; Ramatsoku, M.; Sivitilli, Alexander K.; Smirnov, O.; Thorat, K.; Vitello, F.

doi:10.1051/0004-6361/202039898

Cited by 30 publications

(92 citation statements)

References 112 publications

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“…If RPS stripping is contributing to pre-processing in groups, this implies that galaxies infalling onto clusters as part of a group should already be Hi deficient, to some extent, relative to field galaxies. This is consistent with Hi observations from the BUD-HIES survey which find Hi deficient galaxies in group-mass substructures surrounding the Abell 963 cluster (Jaffé et al 2016), as well as MeerKAT observations finding Hi deficient galaxies in the Fornax A group (Kleiner et al 2021). Other works have also reported evidence for Hi deficient galaxies in groups (e.g.…”

Section: Implications For Pre-processingsupporting

confidence: 91%

“…A few more studies have found 'cometlike' Hi morphologies for galaxies in groups (Bureau & Carignan 2002;McConnachie et al 2007), which are likely being driven by RPS. In particular, a recent MeerKAT study of the Fornax A group (Kleiner et al 2021) present evidence for 9 galaxies in the midst of being pre-processed prior to accretion onto the Fornax cluster. Some of these galaxies display Hi deficiencies as well as Hi morphologies consistent with RPS (Kleiner et al 2021).…”

Section: Introductionmentioning

confidence: 99%

“…In particular, a recent MeerKAT study of the Fornax A group (Kleiner et al 2021) present evidence for 9 galaxies in the midst of being pre-processed prior to accretion onto the Fornax cluster. Some of these galaxies display Hi deficiencies as well as Hi morphologies consistent with RPS (Kleiner et al 2021). Finally, evidence for RPS stripping in groups has also been presented in the form of gas disks which are truncated relative to the stellar component, consistent with RPS removing gas from the outside-in (Sengupta et al 2007;Vulcani et al 2018b).…”

Section: Introductionmentioning

confidence: 99%

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LoTSS jellyfish galaxies: II. Ram pressure stripping in groups versus clusters

Roberts,

van Weeren,

McGee

et al. 2021

Preprint

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Ram pressure stripping is a frequently cited mechanism for quenching galaxy star formation in dense environments. Numerous examples of ram pressure stripping in galaxy clusters are present in literature; however, substantially less work has been focused on ram pressure stripping in lower mass groups, the most common galaxy environment in the local Universe. In this work we use the LOFAR Two-metre Sky Survey (LoTSS) to search for jellyfish galaxies (i.e. galaxies with ram pressure stripped tails extending beyond the optical disk) in ∼500 SDSS groups (z < 0.05), making this the most comprehensive search for ram pressure stripping in groups to date. We identify 60 jellyfish galaxies in groups with extended, asymmetric radio continuum tails, which are found across the entire range of group mass from 10 12.5 < M group < 10 14 h −1 M . We compare the group jellyfish galaxies identified in this work with the LoTSS jellyfish galaxies in clusters presented in Roberts et al. (2021b), allowing us to compare the effects of ram pressure stripping across three decades in group/cluster mass. We find that jellyfish galaxies are most commonly found in clusters, with the frequency decreasing towards the lowest mass groups. Both the orientation of observed radio continuum tails, and the positions of group jellyfish galaxies in phase space, suggest that galaxies are stripped more slowly in groups relative to clusters. Finally, we find that the star formation rates of jellyfish galaxies in groups are consistent with 'normal' star-forming group galaxies, which is in contrast to cluster jellyfish galaxies that have clearly enhanced star formation rates. On the whole, there is clear evidence for ongoing ram pressure stripping in galaxy groups (down to very low group masses), though the frequency of jellyfish galaxies and the strength of ram pressure stripping appears smaller in groups than clusters. Differences in the efficiency of ram pressure stripping in groups versus clusters likely contributes to the positive trend between quenched fraction and host halo mass observed in the local Universe.

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Section: Implications For Pre-processingsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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LoTSS jellyfish galaxies: II. Ram pressure stripping in groups versus clusters

Roberts,

van Weeren,

McGee

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Indeed, many authors, e.g., Dressler (2004), argue that in these environments prolonged exposure to intra-group tidal interactions and "preprocessing" more generally, is more efficient in affecting the cold gas reservoirs of galaxies. Evidence of the impact of preprocessing on the H i in LTGs in a rich infalling group was recently presented in Kleiner et al (2021), see also Cortese et al (2021).…”

Section: Introductionmentioning

confidence: 88%

FGC 1287 and its enigmatic 250 kpc long HI tail in the outskirts of Abell 1367

Scott

Cortese

Lagos

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present H i and radio continuum, narrow–band Hα imaging, IFU spectroscopy, and X–ray observations of the FGC 1287 triplet projected ∼ 1.8 Mpc west of the galaxy cluster Abell 1367. One triplet member, FGC 1287, displays an exceptionally long, 250 kpc H i tail and an unperturbed stellar disk which are the typical signatures of ram pressure stripping (RPS). To generate detectable RPS signatures the presence of an Intra–cluster medium ICM/intra–group medium IGM with sufficient density to produce RPS at a realistic velocity relative to the ICM/IGM is a prerequisite. However, XMM–Newton observations were not able to detect X–ray emission from the triplet, implying that if a hot ICM/IGM is present, its density, ne, is less than 2.6× 10−5 cm−3. Higher–resolution VLA H i data presented here show FGC 1287’s H i disk is truncated and significantly warped whereas the H i tail is clumpy. TNG Hα imaging identified three star forming clumps projected within 20 kpc of FGC 1287’s disk, with VIMOS–IFU data confirming two of these are counterparts to H i clumps in the tail. The triplet’s H i kinematics, together with Hα and radio continuum imaging suggests an interaction may have enhanced star formation in FGC 1287’s disk, but cannot readily account for the origin of the long H i tail. We consider several scenarios which might reconcile RPS with the non–detection of ICM/IGM X–ray emission but none of these unambiguously explains the origin of the long H i tail.

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“…The data analyzed in this work consists of the H i image obtained with MeerKAT and already published by Kleiner et al (2021), together with the polarized image and RM image obtained with ASKAP during commissioning tests of the telescope in view of the Early Science program which covered the Fornax cluster (Anderson et al 2021). The commissioning observations presented here correspond to a different scheduling block with respect to the Fornax cluster observations by Anderson et al (2021).…”

Section: Datamentioning

confidence: 99%

A depolarizing HI tidal tail in the western lobe of Fornax A

Loi,

Serra,

Murgia

et al. 2022

Preprint

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Recent MeerKAT neutral hydrogen (H i) observations of Fornax A reveal tidal material intersecting in projection the western lobe of this radio galaxy. We found a spatial coincidence between the northern H i tail and a depolarized structure observed for the first time with the Australian Square Kilometre Array Pathfinder (ASKAP) at 1.2 GHz. We analyzed the properties of the rotation measure (RM) image obtained with ASKAP data at the location of the H i tail and in its neighborhood. We modeled the observed RM structure function to investigate the magnetic field power spectrum at the location of the H i tail and in a nearby control region. We found that the observed RM, in the control region and in a region enclosing the H i tail, cannot be due to the intracluster Faraday screen caused by the Fornax cluster. An intragroup magnetized medium with a central magnetic field strength of 18.5 µG can explain the control region RM, but it is clear that there is an excess in correspondence with the H i tail region. We evaluated several scenarios in which the H i tail is either in the lobe foreground or embedded in the lobe. We determined a magnetic field strength on the order of ∼9.5−11 µG in the H i tail, a value consistent with constraints derived from narrowband Hα imaging of the ionized gas. The spatial coincidence between H i tail and depolarization analyzed in this paper could be the first observed evidence of a magnetic field that either has passed through a radio galaxy lobe or has survived the lobe expansion.

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A MeerKAT view of pre-processing in the Fornax A group

Cited by 30 publications

References 112 publications

LoTSS jellyfish galaxies: II. Ram pressure stripping in groups versus clusters

LoTSS jellyfish galaxies: II. Ram pressure stripping in groups versus clusters

FGC 1287 and its enigmatic 250 kpc long HI tail in the outskirts of Abell 1367

A depolarizing HI tidal tail in the western lobe of Fornax A

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