Ram Pressure Stripping of Hot Galactic Halos in Galaxy Clusters

2011 ◽  
pp. 235-237
Author(s):  
V. Baumgartner ◽  
D. Breitschwerdt
Keyword(s):  
Galaxy Clusters ◽  
Galactic Halos ◽  
Ram Pressure

scholarly journals Connecting magnetic fields from sub-galactic scale to clusters of galaxies and beyond with cosmological MHD simulations

2015 ◽  
Vol 11 (A29B) ◽  
pp. 699-699
Author(s):  
Klaus Dolag ◽  
Alexander M. Beck ◽  
Alexander Arth
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Heat Transport ◽  
Galaxy Clusters ◽  
Large Scale ◽  
High Redshift ◽  
Galactic Halos ◽  
Rotation Measure ◽  
The Magnetic Field ◽  
Good Agreement

AbstractUsing the MHD version of Gadget3 (Stasyszyn, Dolag & Beck 2013) and a model for the seeding of magnetic fields by supernovae (SN), we performed simulations of the evolution of the magnetic fields in galaxy clusters and study their effects on the heat transport within the intra cluster medium (ICM). This mechanism – where SN explosions during the assembly of galaxies provide magnetic seed fields – has been shown to reproduce the magnetic field in Milky Way-like galactic halos (Beck et al. 2013). The build up of the magnetic field at redshifts before z = 5 and the accordingly predicted rotation measure evolution are also in good agreement with current observations. Such magnetic fields present at high redshift are then transported out of the forming protogalaxies into the large-scale structure and pollute the ICM (in a similar fashion to metals transport). Here, complex velocity patterns, driven by the formation process of cosmic structures are further amplifying and distributing the magnetic fields. In galaxy clusters, the magnetic fields therefore get amplified to the observed μG level and produce the observed amplitude of rotation measures of several hundreds of rad/m2. We also demonstrate that heat conduction in such turbulent fields on average is equivalent to a suppression factor around 1/20th of the classical Spitzer value and in contrast to classical, isotropic heat transport leads to temperature structures within the ICM compatible with observations (Arth et al. 2014).

scholarly journals JELLYFISH: EVIDENCE OF EXTREME RAM-PRESSURE STRIPPING IN MASSIVE GALAXY CLUSTERS

2014 ◽  
Vol 781 (2) ◽  
pp. L40 ◽  
Author(s):  
H. Ebeling ◽  
L. N. Stephenson ◽  
A. C. Edge
Keyword(s):  
Galaxy Clusters ◽  
Ram Pressure ◽  
Massive Galaxy

scholarly journals Caught in the Act: Witnessing a~Transforming Spiral in a Galaxy Group

2006 ◽  
Vol 2 (S235) ◽  
pp. 239-239
Author(s):  
J. Rasmussen ◽  
T. J. Ponman ◽  
J. S. Mulchaey
Keyword(s):  
Galaxy Clusters ◽  
Direct Evidence ◽  
X Ray ◽  
Galaxy Groups ◽  
Ram Pressure

AbstractRam pressure stripping of galaxies is believed to be inefficient in galaxy groups, but Chandra X-ray observations of the starburst spiral NGC 2276, a member of a small galaxy group, shows that this galaxy is being stripped of its gas at a rate of ~5 M⊙ yr−1 due to its motion through hot intragroup gas. This provides direct evidence that mechanisms associated with ram pressure can strip galaxies of their gas in systems much smaller than galaxy clusters.

scholarly journals Jellyfish: the origin and distribution of extreme ram-pressure stripping events in massive galaxy clusters

2015 ◽  
Vol 455 (3) ◽  
pp. 2994-3008 ◽  
Author(s):  
Conor McPartland ◽  
Harald Ebeling ◽  
Elke Roediger ◽  
Kelly Blumenthal
Keyword(s):  
Galaxy Clusters ◽  
Ram Pressure ◽  
Massive Galaxy

scholarly journals Figuring Out Gas & Galaxies in Enzo (FOGGIE). IV. The Stochasticity of Ram Pressure Stripping in Galactic Halos

2020 ◽  
Vol 905 (2) ◽  
pp. 167
Author(s):  
Raymond C. Simons ◽  
Molly S. Peeples ◽  
Jason Tumlinson ◽  
Brian W. O’Shea ◽  
Britton D. Smith ◽  
...  
Keyword(s):  
Galactic Halos ◽  
Ram Pressure

scholarly journals The effect of ram-pressure stripping on dwarf galaxies

2020 ◽  
Vol 494 (1) ◽  
pp. 1114-1127 ◽  
Author(s):  
P Steyrleithner ◽  
G Hensler ◽  
A Boselli
Keyword(s):  
Galaxy Clusters ◽  
Stellar Population ◽  
Velocity Dispersion ◽  
Spiral Galaxies ◽  
Dwarf Galaxies ◽  
Gas Content ◽  
Gas Reservoirs ◽  
Interstellar Gas ◽  
Internal Structures ◽  
Ram Pressure

ABSTRACT Ram-pressure stripping (RPS) is a well observed phenomenon of massive spiral galaxies passing through the hot intracluster medium (ICM) of galaxy clusters. For dwarf galaxies (DGs) within a cluster, the transformation from gaseous to gas-poor systems by RPS is not easily observed and must happen in the outskirts of clusters. In a few objects in close by galaxy clusters and the field, RPS has been observed. Since cluster early-type DGs also show a large variety of internal structures (unexpected central gas reservoirs, blue stellar cores, composite radial stellar profiles), we aim in this study to investigate how ram pressure (RP) affects the interstellar gas content and therefore the star formation (SF) activity. Using a series of numerical simulations, we quantify the dependence of the stripped-off gas on the velocity of the infalling DGs and on the ambient ICM density. We demonstrated that SF can be either suppressed or triggered by RP depending on the ICM density and the DGs mass. Under some conditions, RP can compress the gas, so that it is unexpectedly retained in the central DG region and forms stars. When gas clouds are still bound against stripping but lifted from a thin disc and fall back, their new stars form an ellipsoidal (young) stellar population already with a larger velocity dispersion without the necessity of harassment. Most spectacularly, star clusters can form downstream in stripped-off massive gas clouds in the case of strong RP. We compare our results to observations.

scholarly journals Explaining the enhanced star formation rate of Jellyfish galaxies in galaxy clusters

2019 ◽  
Vol 486 (1) ◽  
pp. L26-L30 ◽  
Author(s):  
Mohammadtaher Safarzadeh ◽  
Abraham Loeb
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Control Sample ◽  
External Pressure ◽  
Gas Content ◽  
Ram Pressure ◽  
Inclination Angles ◽  
Formation Efficiency

ABSTRACT We study the recently observed JellyFish galaxies (JFGs), which are found to have their gas content ram pressure stripped away in galaxy clusters. These galaxies are observed to have an enhanced star formation rate of about 0.2 dex compared with a control sample of the same stellar mass in their discs. We model the increase in the star formation efficiency as a function of intracluster medium pressure and parametrize the cold gas content of the galaxies as a function of cluster-centric distance. We show that regarding the external pressure as a positive feedback results in agreement with the observed distribution of enhanced star formation in the JFGs if clouds are shielded from evaporation by magnetic fields. Our results predict that satellites with halo mass $\lt 10^{11}{\rm \, M_\odot }$ moving with Mach numbers $\mathcal {M}\approx 2$, and inclination angles below 60 deg, are more likely to be detected as JFGs.

scholarly journals Detection of metal-rich, cool-warm gas in the outskirts of galaxy clusters

2019 ◽  
Vol 488 (4) ◽  
pp. 5327-5339 ◽  
Author(s):  
Jayadev Pradeep ◽  
Anand Narayanan ◽  
Sowgat Muzahid ◽  
Daisuke Nagai ◽  
Jane C Charlton ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Single Phase ◽  
Absorption Lines ◽  
Intracluster Medium ◽  
Cluster Galaxies ◽  
Ram Pressure ◽  
Tidal Streams ◽  
Cluster Cores ◽  
Intracluster Gas ◽  
Line Analysis

ABSTRACT We present an ultraviolet quasar absorption line analysis of metal lines associated with three strong intervening H i absorbers (with $N(\rm {{H}\,{\small I}})$ > 1016.5 cm−2) detected in the outskirts of Sunyaev–Zel’dovich (SZ) effect-selected galaxy clusters (zcl ∼ 0.4–0.5), within clustocentric impact parameters of ρcl ∼ (1.6–4.7)r500. Discovered in a recent set of targeted far-UV HST/COS spectroscopic observations, these absorbers have among the highest H  i column densities ever observed in the outskirts of galaxy clusters, and are also rich in metal absorption lines. Photoionization models yield single phase solutions for the three absorbers with gas densities of nH  ∼ 10−3–10−4 cm−3 and metallicities of [X/H] > −1.0 (from one-tenth solar to near-solar). The widths of detected absorption lines suggest gas temperatures of T ∼ 104 K. The inferred densities (temperatures) are significantly higher (lower) compared to the X-ray emitting intracluster medium in cluster cores. The absorbers are tracing a cool phase of the intracluster gas in the cluster outskirts, either associated with gas stripped from cluster galaxies via outflows, tidal streams or ram-pressure forces, or denser regions within the intracluster medium that were uniformly chemically enriched from an earlier epoch of enhanced supernova and Active Galactic Nucleus (AGN) feedback.

scholarly journals Ram pressure stripping of disk galaxies in galaxy clusters

2009 ◽  
Vol 330 (9���10) ◽  
pp. 888-897 ◽  
Author(s):  
E. Roediger
Keyword(s):  
Galaxy Clusters ◽  
Disk Galaxies ◽  
Ram Pressure
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