scholarly journals Deep H I observations of the surroundings of ram pressure stripped Virgo spiral galaxies

2006 ◽  
Vol 462 (1) ◽  
pp. 93-99 ◽  
Author(s):  
B. Vollmer ◽  
W. Huchtmeier
Keyword(s):  
Spiral Galaxies ◽  
Ram Pressure

scholarly journals Ram Pressure Stripping of Spiral Galaxies in Clusters

2004 ◽  
Vol 217 ◽  
pp. 376-381
Author(s):  
Elke Schumacher ◽  
Gerhard Hensler
Keyword(s):  
Mass Loss ◽  
Spiral Galaxies ◽  
Disk Galaxies ◽  
Helmholtz Instability ◽  
Restoring Force ◽  
Ram Pressure ◽  
First Results ◽  
Two Phases ◽  
Gas Loss ◽  
Long Timescales

We investigate the process of ram pressure stripping by means of numerical simulations with a 2D hydrodynamical code. We present some first results of a set of simulations with varying galaxy velocities and ICM densities. We find that in typical cluster core environments disk galaxies lose a substantial amount of their gas, whereas in the outskirts of galaxy clusters the mass loss is quite small. Furthermore, the gas loss happens in two phases: In the initial phase gas is pushed out of regions where the ram pressure overcomes the gravitational restoring force; most of the overall gas loss happens in this phase. Afterwards the Kelvin-Helmholtz instability leads to a further mass loss at a small rate, that could be important on long timescales.

scholarly journals The effects of ram-pressure stripping on the internal kinematics of simulated spiral galaxies

2008 ◽  
Vol 483 (3) ◽  
pp. 783-791 ◽  
Author(s):  
T. Kronberger ◽  
W. Kapferer ◽  
S. Unterguggenberger ◽  
S. Schindler ◽  
B. L. Ziegler
Keyword(s):  
Spiral Galaxies ◽  
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 Galaxy Evolution in the Virgo Cluster

2006 ◽  
Vol 2 (S235) ◽  
pp. 155-159
Author(s):  
Bernd Vollmer
Keyword(s):  
Galaxy Evolution ◽  
Spiral Galaxies ◽  
Virgo Cluster ◽  
Time Sequence ◽  
Radio Continuum ◽  
Major Result ◽  
Ram Pressure ◽  
Sticky Particles ◽  
Dynamical Modelling

AbstractIn the last years we have gained new insights on how ram pressure acts in detail on Virgo spiral galaxies. This has been possible due to the combination of new deep HIobservations, deep polarized radio continuum observations, and detailed dynamical modelling (sticky particles and MHD). As a major result a first complete ram pressure stripping time sequence could be established for the Virgo cluster.

scholarly journals Ram pressure stripping of spiral galaxies in clusters

1999 ◽  
Vol 308 (4) ◽  
pp. 947-954 ◽  
Author(s):  
M. G. Abadi ◽  
B. Moore ◽  
R. G. Bower
Keyword(s):  
Spiral Galaxies ◽  
Ram Pressure

scholarly journals Creating lenticular galaxies with mergers

2016 ◽  
Vol 11 (S321) ◽  
pp. 114-116
Author(s):  
Miguel Querejeta ◽  
M. Carmen Eliche-Moral ◽  
Trinidad Tapia ◽  
Alejandro Borlaff ◽  
Glenn van de Ven ◽  
...  
Keyword(s):  
Angular Momentum ◽  
Spiral Galaxies ◽  
Scaling Relations ◽  
Galaxy Mergers ◽  
Local Universe ◽  
Lenticular Galaxies ◽  
Ram Pressure ◽  
Light Concentration ◽  
Rule Out ◽  
Good Agreement

AbstractLenticular galaxies (S0s) represent the majority of early-type galaxies in the local Universe, but their formation channels are still poorly understood. While galaxy mergers are obvious pathways to suppress star formation and increase bulge sizes, the marked parallelism between spiral and lenticular galaxies (e.g. photometric bulge–disc coupling) seemed to rule out a potential merger origin. Here, we summarise our recent work in which we have shown, throughN-body numerical simulations, that disc-dominated lenticulars can emerge from major mergers of spiral galaxies, in good agreement with observational photometric scaling relations. Moreover, we show that mergers simultaneously increase the light concentration and reduce the angular momentum relative to their spiral progenitors. This explains the mismatch in angular momentum and concentration between spirals and lenticulars recently revealed by CALIFA observations, which is hard to reconcile with simple fading mechanisms (e.g. ram-pressure stripping).

scholarly journals On the influence of ram-pressure stripping on the star formation of simulated spiral galaxies

2008 ◽  
Vol 481 (2) ◽  
pp. 337-343 ◽  
Author(s):  
T. Kronberger ◽  
W. Kapferer ◽  
C. Ferrari ◽  
S. Unterguggenberger ◽  
S. Schindler
Keyword(s):  
Star Formation ◽  
Spiral Galaxies ◽  
Ram Pressure

scholarly journals GASP XXIX – unwinding the arms of spiral galaxies via ram-pressure stripping

2020 ◽  
Vol 500 (1) ◽  
pp. 1285-1312
Author(s):  
Callum Bellhouse ◽  
Sean L McGee ◽  
Rory Smith ◽  
Bianca M Poggianti ◽  
Yara L Jaffé ◽  
...  
Keyword(s):  
Spiral Galaxies ◽  
Control Group ◽  
Original Structure ◽  
Gas Stripping ◽  
Spiral Arms ◽  
Cluster Galaxies ◽  
Pile Up ◽  
Ram Pressure ◽  
Disc Rotation ◽  
Gravitational Influence

ABSTRACT We present the first study of the effect of ram pressure ‘unwinding’ the spiral arms of cluster galaxies. We study 11 ram-pressure stripped galaxies from GASP (GAs Stripping Phenomena in galaxies) in which, in addition to more commonly observed ‘jellyfish’ features, dislodged material also appears to retain the original structure of the spiral arms. Gravitational influence from neighbours is ruled out and we compare the sample with a control group of undisturbed spiral galaxies and simulated stripped galaxies. We first confirm the unwinding nature, finding that the spiral arm pitch angle increases radially in 10 stripped galaxies and also simulated face-on and edge-on stripped galaxies. We find only younger stars in the unwound component, while older stars in the disc remain undisturbed. We compare the morphology and kinematics with simulated ram-pressure stripping galaxies, taking into account the estimated inclination with respect to the intracluster medium (ICM) and find that in edge-on stripping, unwinding can occur due to differential ram pressure caused by the disc rotation, causing stripped material to slow and ‘pile up’. In face-on cases, gas removed from the outer edges falls to higher orbits, appearing to ‘unwind’. The pattern is fairly short-lived (<0.5 Gyr) in the stripping process, occurring during first infall and eventually washed out by the ICM wind into the tail of the jellyfish galaxy. By comparing simulations with the observed sample, we find that a combination of face-on and edge-on ‘unwinding’ effects is likely to be occurring in our galaxies as they experience stripping with different inclinations with respect to the ICM.

scholarly journals Galaxy spin direction distribution in HST and SDSS show similar large-scale asymmetry

2020 ◽  
Vol 37 ◽  
Author(s):  
Lior Shamir
Keyword(s):  
Large Scale ◽  
Spiral Galaxies ◽  
Hubble Space Telescope ◽  
Gravitational Interaction ◽  
Large Data ◽  
Sloan Digital Sky Survey ◽  
Data Sets ◽  
Dipole Axis ◽  
Data Set ◽  
The Asymmetry

Abstract Several recent observations using large data sets of galaxies showed non-random distribution of the spin directions of spiral galaxies, even when the galaxies are too far from each other to have gravitational interaction. Here, a data set of $\sim8.7\cdot10^3$ spiral galaxies imaged by Hubble Space Telescope (HST) is used to test and profile a possible asymmetry between galaxy spin directions. The asymmetry between galaxies with opposite spin directions is compared to the asymmetry of galaxies from the Sloan Digital Sky Survey. The two data sets contain different galaxies at different redshift ranges, and each data set was annotated using a different annotation method. The results show that both data sets show a similar asymmetry in the COSMOS field, which is covered by both telescopes. Fitting the asymmetry of the galaxies to cosine dependence shows a dipole axis with probabilities of $\sim2.8\sigma$ and $\sim7.38\sigma$ in HST and SDSS, respectively. The most likely dipole axis identified in the HST galaxies is at $(\alpha=78^{\rm o},\delta=47^{\rm o})$ and is well within the $1\sigma$ error range compared to the location of the most likely dipole axis in the SDSS galaxies with $z>0.15$ , identified at $(\alpha=71^{\rm o},\delta=61^{\rm o})$ .

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