SPECTACULAR X-RAY TAILS, INTRACLUSTER STAR FORMATION, AND ULXs IN A3627

Sun, Ming; Donahue, M.; Röediger, E.; Nulsen, P. E. J.; Voit, G. Mark; Sarazin, Craig L.; Forman, W.; Jones, C.

doi:10.1088/0004-637x/708/2/946

Cited by 175 publications

(314 citation statements)

References 68 publications

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“…Scott et al 2012), Hα (e.g. Yagi et al 2008), and X-ray (Sun et al 2010) tails of stripped material at the periphery of clusters consistently indicate that ram pressure stripping is efficient even outside the virial radius of massive clusters, such as Virgo. Given that this process is able to transform star-forming systems into red objects on timescales of 1 Gyr, and that these freshly infalling objects are moving on the plane of the sky with a velocity with respect to the cluster centre of σ = 1150 km s −1 (the typical velocity dispersion of late-type galaxies in the cluster, from Boselli & Gavazzi 2006), we expect that most of them are fully transformed before they reach the cluster core.…”

Section: Dwarf Galaxiesmentioning

confidence: 97%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

153

254

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We study the role of the environment on galaxy evolution using a sample of 868 galaxies in the Virgo cluster and in its surrounding regions that are selected from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) with the purpose of understanding the origin of the red sequence in dense environments. The sample spans a wide range in morphological types (from dwarf ellipticals to Im and BCD) and stellar masses (10 7 M star 10 11.5 M ). We collected multifrequency data covering the whole electromagnetic spectrum for most of the galaxies, including UV, optical, mid-and far-infrared imaging data, as well as optical and HI spectroscopic data. We first identify the different dynamical substructures that compose the Virgo cluster, and we calculate the local density of galaxies using different methods. We then study the distribution of galaxies belonging to the red sequence, the green valley, and the blue cloud within the different cluster substructures or as a function of galaxy density. Our analysis indicates that all the most massive galaxies (M star 10 11 M ) are slow rotators and are the dominant galaxies of the different cluster substructures, which are generally associated with a diffuse X-ray emission. They are probably the result of major merging events that occurred at early epochs, as also indicated by their very old stellar populations. Slow rotators of lower stellar mass (10 8.5M star 10 11 M ) are also preferentially located within the different high-density substructures of the cluster. Their position in the velocity space indicates that they are virialised within the cluster; thus, they are Virgo members since its formation. They have been shaped by gravitational perturbations occurring within the infalling groups that later form the cluster (pre-processing). On the contrary, low-mass star-forming systems are extremely rare in the inner regions of the Virgo cluster A, where the density of the intergalactic medium is at its maximum. Our ram pressure stripping models consistently indicate that these star-forming systems can be rapidly deprived of their interstellar medium during their interaction with the intergalactic medium. The lack of gas quenches their star-formation activity transforming them into quiescent dwarf ellipticals. This mild transformation does not perturb the kinematic properties of these galaxies, which still have rotation curves typical of star-forming systems.

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Section: Dwarf Galaxiesmentioning

confidence: 97%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

153

254

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“…There are already known examples of one-sided tails of young stars extending from more massive galaxies in more distant, richer clusters (Cortese et al 2007;Yoshida et al 2008;Smith et al 2010;Sun et al 2010;Woudt et al 2008), where the ram pressure can be 1 to 2 orders of magnitude stronger than in Virgo, but IC3418 is by far the closest such galaxy known.…”

Section: Introductionmentioning

confidence: 99%

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

Jáchym¹,

Kenney²,

Růžička³

et al. 2013

A&A

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We present IRAM 30m sensitive upper limits on CO emission in the ram pressure stripped dwarf Virgo galaxy IC3418 and in a few positions covering H ii regions in its prominent 17 kpc UV/Hα gas-stripped tail. In the central few arcseconds of the galaxy, we report a possible marginal detection of about 1 × 10 6 M ⊙ of molecular gas (assuming a Galactic CO-to-H 2 conversion factor) that could correspond to a surviving nuclear gas reservoir. We estimate that there is less molecular gas in the main body of IC3418, by at least a factor of 20, than would be expected from the pre-quenching UV-based star formation rate assuming the typical gas depletion timescale of 2 Gyr. Given the lack of star formation in the main body, we think the H 2 -deficiency is real, although some of it may also arise from a higher CO-to-H 2 factor typical in low-metallicity, low-mass galaxies. The presence of H ii regions in the tail of IC3418 suggests that there must be some dense gas; however, only upper limits of < 1 × 10 6 M ⊙ were found in the three observed points in the outer tail. This yields an upper limit on the molecular gas content of the whole tail < 1 × 10 7 M ⊙ , which is an amount similar to the estimates from the observed star formation rate over the tail. We also present strong upper limits on the X-ray emission of the stripped gas in IC3418 from a new Chandra observation. The measured X-ray luminosity of the IC3418 tail is about 280 times lower than that of ESO 137-001, a spiral galaxy in a more distant cluster with a prominent ram pressure stripped tail. Non-detection of any diffuse X-ray emission in the IC3418 tail may be due to a low gas content in the tail associated with its advanced evolutionary state and/or due to a rather low thermal pressure of the surrounding intra-cluster medium.

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“…Kormendy and Bender emphasize that these galaxies and the H I -depleted galaxies are substantially brighter than almost all Sphs: "If even the deep gravitational potential wells of still-spiral galaxies suffer H I stripping, then the shallow potential wells of dS + Im galaxies are more likely to be stripped." The most impressive recent example of ram-pressure stripping is the multi-wavelength (CO gas+H II+X-ray) tail of the galaxy ESO 137-001 in Abell 3627 (Sun et al 2006(Sun et al , 2007(Sun et al , 2010Woudt et al 2008;Sivanandam et al 2010;Pavel et al 2014; Figure 5 here).…”

Section: Environmental Processes Imentioning

confidence: 96%

“…Spectacular observations of ram-pressure stripping in action now clearly demonstrate the importance of this process (see Sun et al 2010;Kormendy & Bender 2012 for reviews). Kenney et al (2004Kenney et al ( , 2008, Oosterloo & van Gorkom 2005, and Chung et al (2007 find that many spiral galaxies near the center of the Virgo cluster show long Hα or H I tails interpreted to be cold gas that is being stripped by the ambient X-ray-emitting gas (Böhringer et al 1994).…”

Section: Environmental Processes Imentioning

confidence: 97%

Structure and Evolution of Dwarf Galaxies

Kormendy

2014

Lessons From the Local Group

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Abstract. Different structural parameter correlations show how classical bulge components and elliptical galaxies are different from spiral and S0 galaxy disks, irregular (Im) galaxies, and spheroidal (Sph) galaxies. In contrast, the latter, apparently diverse galaxies or galaxy components have almost identical parameter correlations. This shows that they are related. A review of galaxy transformation processes suggests that S0 and spheroidal galaxies are star-formation-quenched, "red and dead" versions of spiral and Im galaxies. In particular, Sph galaxies are bulgeless S0s. This motivates a parallel sequence galaxy classification in which an S0a-S0b-S0c-Sph sequence of decreasing bulge-to-total ratios is juxtaposed to an Sa-Sb-Sc-Im sequence of star-forming galaxies. All parameter sequences show a complete continuity from giant galaxies to the tiniest dwarfs. Dwarfs are not a new or different class of galaxies. Rather, they are the extreme products of transformation processes that get more important as gravitational potential wells get more shallow. Smaller Sph and S+Im galaxies have lower stellar densities because they retain fewer baryons. Comparison of the baryonic parameter correlations with those for dark matter halos allows us to estimate baryon loss as a function of galaxy mass. Extreme dwarfs are almost completely dominated by dark matter.

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SPECTACULAR X-RAY TAILS, INTRACLUSTER STAR FORMATION, AND ULXs IN A3627

Cited by 175 publications

References 68 publications

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

Structure and Evolution of Dwarf Galaxies

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