The better half – asymmetric star formation due to ram pressure in the EAGLE simulations

Troncoso-Iribarren, P.; Padilla, Nelson; Santander, Carlos Carmona; Lagos, Claudia del P.; García-Lambas, D.; Rodríguez, Silvio; Contreras, Sergio

doi:10.1093/mnras/staa274

Cited by 47 publications

(51 citation statements)

References 56 publications

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“…These galaxy spectral indices are consistent with flattening due to ionization losses (Basu et al 2015;Chyży et al 2018) in a high density ISM. This flattening is expected at the low frequencies that we probe in this work and becomes increasingly important in the highest density regions of the ISM (Basu et al 2015), which is also consistent with enhanced ISM densities in jellyfish galaxies due to compression from ram pressure (e.g., Schulz & Struck 2001;Bekki 2014;Troncoso-Iribarren et al 2020;Cramer et al 2021).…”

Section: Spectral Index Measurementssupporting

confidence: 84%

“…This suggests that Hα + [Nii] emission, and therefore star formation, is enhanced along the leading side of the jellyfish galaxies, consistent with gas compression induced by ram pressure along the galaxy-ICM interface. As alluded to in Section 3, such an effect has been predicted by simulations of RPS (e.g., Bekki 2014;Troncoso-Iribarren et al 2020) and been reported observationally for a limited number of galaxies experiencing ram pressure (e.g., Gavazzi et al 2001;Boselli et al 2021). Further work is required to test whether these leading-side star formation enhancements are commonplace for galaxies undergoing RPS, and the results reported here are a step in that direction.…”

Section: Hα + [Nii] Sources Relative To Tail Directionsupporting

confidence: 63%

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LoTSS Jellyfish Galaxies III. The first identification of jellyfish galaxies in the Perseus cluster

Roberts,

van Weeren,

Timmerman

et al. 2021

Preprint

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In this paper we report the first identification of jellyfish galaxies in the Perseus cluster (Abell 426). We identified four jellyfish galaxies (LEDA 2191078, MCG +07-07-070, UGC 2654, UGC 2665) within the central 2 • × 2 • (2.6 Mpc × 2.6 Mpc) of Perseus based on the presence of one-sided radio continuum tails that were detected at 144 MHz by the LOw Frequency ARray (LOFAR). The observed radio tails, as well as the orientation of morphological features in the rest-frame optical, are consistent with these four galaxies being impacted by ram pressure stripping as they orbit through the Perseus intracluster medium. By combining the LOFAR imaging at 144 MHz with 344 MHz imaging from the Karl G. Jansky Very Large Array, we derived spectral indices for the disks and the stripped tails of these jellyfish galaxies. We show that the spectral indices over the galaxy disks are quite flat, while the indices of the stripped tails are substantially steeper. We also identified a number of compact Hα + [Nii] sources with narrowband imaging from the Isaac Newton Telescope. These sources are brighter along the leading side of the galaxy (i.e., opposite to the direction of the stripped tail), which is consistent with ram pressure induced star formation. Lastly, consistent with previous works in other clusters, we find that these jellyfish galaxies show enhanced radio luminosities for their observed star formation rates. Given the small distance to the Perseus cluster (D ∼ 70 Mpc, 1 340 pc), these galaxies are excellent candidates for multiwavelength follow-up observations to probe the impact of ram pressure stripping on galaxy star formation at subkiloparsec scales.

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Section: Spectral Index Measurementssupporting

confidence: 84%

Section: Hα + [Nii] Sources Relative To Tail Directionsupporting

confidence: 63%

LoTSS Jellyfish Galaxies III. The first identification of jellyfish galaxies in the Perseus cluster

Roberts,

van Weeren,

Timmerman

et al. 2021

Preprint

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“…This increase in the star formation activity is probably due to an increase of the molecular gas fraction made possible by the increase of the external pressure (Blitz & Rosolowsky 2006), as again observed in some massive jellyfish galaxies (Moretti et al 2020b) and predicted by hydrodynamic simulations (Henderson & Bekki 2016;Troncoso-Iribarren et al 2020). NGC 4569 is significantly more massive than the dwarf IC 3476 and is thus able to retain the gas from external perturbations because of its deep potential well.…”

Section: The Galaxymentioning

confidence: 62%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli

Lupi

Épinat

et al. 2021

A&A

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We study the IB(s)m galaxy IC 3476 observed in the context of the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE), a blind narrow-band Hα+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT. The deep narrow-band image reveals a very pertubed ionised gas distribution that is characterised by a prominent banana-shaped structure in the front of the galaxy formed of giant HII regions crossing the stellar disc. Star-forming structures, at ∼8 kpc from the edges of the stellar disc, are also detected in a deep far-ultraviolet ASTROSAT/UVIT image. This particular morphology indicates that the galaxy is undergoing an almost edge-on ram pressure stripping event. The same Hα+[NII] image also shows that the star formation activity is totally quenched in the leading edge of the disc, where the gas has been removed during the interaction with the surrounding medium. The spectral energy distribution fitting analysis of the multi-frequency data indicates that this quenching episode is very recent (∼50 Myr), and roughly corresponds to an increase of the star formation activity by a factor of ∼161% in the inner regions with respect to that expected for secular evolution. The analysis of these data, whose angular resolution enables the study of the induced effects of the perturbation down to the scale of individual HII regions (req ≃ 40 pc), also suggests that the increase of star formation activity is due to the compression of the gas along the stellar disc of the galaxy, which is able to increase its mean electron density and boost the star formation process producing bright HII regions with luminosities up to L(Hα) ≃ 1038 erg s−1. The combined analysis of the VESTIGE data with deep IFU spectroscopy gathered with MUSE and with high spectral resolution Fabry Perot data also indicates that the hydrodynamic interaction has deeply perturbed the velocity field of the ionised gas component while leaving that of the stellar disc unaffected. The comparison of the data with tuned high-resolution hydrodynamic simulations accounting for the different gas phases (atomic, molecular, ionised) consistently indicates that the perturbing event is very recent (50–150 Myr), once again confirming that ram pressure stripping is a violent phenomenon that is able to perturb the evolution of galaxies in rich environments on short timescales.

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“…Not only can RPS quench star formation by removing galaxy gas reserves, but simulations also predict a brief enhancement in star formation, prior to gas removal, due to compression in the ISM through the galaxy-ICM interaction (e.g. Steinhauser et al 2012;Ramos-Martínez et al 2018;Troncoso Iribarren et al 2020). This picture is supported by recent observations that have shown enhanced levels of star formation in galaxies thought to be undergoing RPS (Ebeling et al 2014;Poggianti et al 2016;Vulcani et al 2018;Roberts & Parker 2020).…”

Section: Jellyfish Galaxy Star Formationmentioning

confidence: 65%

LoTSS jellyfish galaxies

Roberts

Weeren

McGee

et al. 2021

A&A

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Context. The cluster environment has a strong impact on galaxy star formation, as seen by the fact that clusters host proportionally more red, passive galaxies relative to the field. Ram pressure stripping may drive this environmental quenching by directly stripping cold gas from galactic disks. In some cases, ram pressure stripping gives rise to ‘jellyfish galaxies’, observed with clear ‘tentacles’ of stripped gas extending beyond the optical extent of the galaxy. Aims. In this paper we present a large sample of jellyfish galaxies in low redshift clusters (z < 0.05), identified through 120−168 MHz radio continuum from the LOFAR Two-metre Sky Survey (LoTSS). Methods. From a parent sample of 29 X-ray-detected SDSS galaxy clusters and their spectroscopic members, we visually identify 95 star-forming, LoTSS jellyfish galaxies with 144 MHz radio tails. Star formation rates (SFRs) and stellar masses are obtained for all galaxies from SED fits. For each jellyfish galaxy we determine the tail orientation with respect to the cluster centre and quantify the prominence of the radio tails with the 144 MHz shape asymmetry. Results. After carefully accounting for redshift-dependent selection effects, we find that the frequency of jellyfish galaxies is relatively constant from cluster to cluster. LoTSS jellyfish galaxies are preferentially found at small clustercentric radius and large velocity offsets within their host clusters and have radio tails that are oriented away from the cluster centre. These galaxies also show enhanced star formation, relative to both ‘normal’ cluster galaxies and isolated field galaxies, but generally fall within the scatter of the L144 MHz − SFR relation. Conclusions. The properties of the LoTSS jellyfish galaxies identified in this work are fully consistent with expectations from ram pressure stripping. This large sample of jellyfish galaxies will be valuable for further constraining ram pressure stripping and star formation quenching in nearby galaxy clusters. We show that LOFAR is a powerful instrument for identifying ram pressure stripped galaxies across extremely wide fields. Moving forward, we will push the search for jellyfish galaxies beyond this initial cluster sample, including a comprehensive survey of the galaxy group regime.

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The better half – asymmetric star formation due to ram pressure in the EAGLE simulations

Cited by 47 publications

References 56 publications

LoTSS Jellyfish Galaxies III. The first identification of jellyfish galaxies in the Perseus cluster

LoTSS Jellyfish Galaxies III. The first identification of jellyfish galaxies in the Perseus cluster

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

LoTSS jellyfish galaxies

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