Ultraviolet tails and trails in cluster galaxies: a sample of candidate gaseous stripping events in Coma

Smith, Russell J.; Lucey, J. R.; Hammer, D.; Hornschemeier, A. E.; Carter, David; Hudson, Michael J.; Marzke, Ronald O.; Mouhcine, M.; Eftekharzadeh, Sareh; James, P. A.; Khosroshahi, Habib G.; Kourkchi, Ehsan; Karick, A. M.

doi:10.1111/j.1365-2966.2010.17253.x

Cited by 183 publications

(212 citation statements)

References 70 publications

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“…Although it may be difficult to form these type of galaxies through major mergers (B11), there are many other processes that have contributed to the gas exhaustion in spirals with a minor effect on the shape and kinematics of the progenitor galaxy, such as simple fading, strangulation, and gas stripping (see, e.g., Smith et al 2010;Yagi et al 2010). Therefore, an evolutionary scenario for some S0s in which these processes combine with minor mergers is quite probable.…”

Section: Discussionmentioning

confidence: 99%

Evolution induced by dry minor mergers onto fast-rotator S0 galaxies

Tapia

Eliche‐Moral

Balcells

et al. 2014

A&A

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Context. Numerical studies have shown that the properties of the S0 galaxies with kinematics intermediate between fast and slow rotators are difficult to explain by a scenario of major mergers. Aims. We investigate whether the smoother perturbation induced by minor mergers can reproduce these systems. Methods. We analysed collisionless N-body simulations of intermediate and minor dry mergers onto S0s to determine the structural and kinematic evolution induced by the encounters. The original primary galaxies represent gas-poor fast-rotator S0b and S0c galaxies with high intrinsic ellipticities. The original bulges are intrinsically spherical and have low rotation. Different mass ratios, parent bulges, density ratios, and orbits were studied. Results. Minor mergers induce a lower decrease of the global rotational support (as provided by λ e ) than encounters of lower mass ratios, which results in S0s with properties intermediate between fast and slow rotators. The resulting remnants are intrinsically more triaxial, less flattened, and span the whole range of apparent ellipticities up to e ∼ 0.8. They do not show lower apparent ellipticities in random projections than initially; on the contrary, the formation of oval distortions and the disc thickening increase the percentage of projections at 0.4 < e < 0.7. In the experiments with S0b progenitor galaxies, minor mergers tend to spin up the bulge and to slightly decrease its intrinsic ellipticity, whereas in the cases of primary S0c galaxies they keep the rotational support of the bulge nearly constant and significantly decrease its intrinsic ellipticity. The remnant bulges remain nearly spherical (B/A ∼ C/A > 0.9), but exhibit a wide range of triaxialities (0.20 < T < 1.00). In the plane of global anisotropy of velocities (δ) vs. intrinsic ellipticity ( e,intr ), some of our models extend the linear trend found in previous major merger simulations towards higher e,intr values, while others clearly depart from it (depending on the progenitor S0). This is consistent with the wide dispersion exhibited by real S0s in this diagram compared with ellipticals, which follow the linear trend drawn by major merger simulations. Conclusions. The smoother changes induced by minor mergers can explain the existence of S0s with intermediate kinematic properties between fast and slow rotators that are difficult to explain with major mergers. The different trends exhibited by ellipticals and S0 galaxies in the δ -e diagram may be pointing to the different role played by major mergers in the build-up of each morphological type.

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Section: Discussionmentioning

confidence: 99%

Evolution induced by dry minor mergers onto fast-rotator S0 galaxies

Tapia

Eliche‐Moral

Balcells

et al. 2014

A&A

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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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“…Rather surprisingly, regions of young star formation have been revealed in some of the tails, either in Hα or UV (Kenney & Koopmann 1999;Cortese et al 2006;Sun et al 2007;Yoshida et al 2008;Smith et al 2010;Hester et al 2010;Yagi et al 2013;Ebeling et al 2014). This indicates that while ram pressure generally suppresses star formation in the disks, it may induce new star formation in the stripped medium.…”

Section: Introductionmentioning

confidence: 99%

“…The central region of the Coma cluster, the most massive and most X-ray luminous cluster at z < 0.025, is an ideal laboratory for studying the hydrodynamic effects of the surrounding ICM on galaxies as well as the fate of the stripped gas. The Coma cluster has the richest optical data among nearby massive clusters, already with more than 20 late-type galaxies with one-sided star-forming or ionized gas tails (Smith et al 2010;Yagi et al 2010), several of which are also bright in soft X-rays. One of the best galaxies to study is D100, a galaxy near the Coma core with a remarkable ram pressure gas stripped tail.…”

Section: Introductionmentioning

confidence: 99%

Molecular Gas Dominated 50 kpc Ram Pressure Stripped Tail of the Coma Galaxy D100^*

Jáchym

Sun

Kenney

et al. 2017

ApJ

119

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We have discovered large amounts of molecular gas, as traced by CO emission, in the ram pressure stripped gas tail of the Coma cluster galaxy D100 (GMP 2910), out to large distances of about 50 kpc. D100 has a 60 kpc long, strikingly narrow tail which is bright in X-rays and Hα. Our observations with the IRAM 30m telescope reveal in total ∼ 10 9 M ⊙ of H 2 (assuming the standard CO-to-H 2 conversion) in several regions along the tail, thus indicating that molecular gas may dominate its mass. Along the tail we measure a smooth gradient in the radial velocity of the CO emission that is offset to lower values from the more diffuse Hα gas velocities. Such a dynamic separation of phases may be due to their differential acceleration by ram pressure. D100 is likely being stripped at a high orbital velocity 2200 km s −1 by (nearly) peak ram pressure. Combined effects of ICM viscosity and magnetic fields may be important for the evolution of the stripped ISM. We propose D100 has reached a continuous mode of stripping of dense gas remaining in its nuclear region. D100 is the second known case of an abundant molecular stripped-gas tail, suggesting that conditions in the ICM at the centers of galaxy clusters may be favorable for molecularization. From comparison with other galaxies, we find there is a good correlation between the CO flux and the Hα surface brightness in ram pressure stripped gas tails, over ∼ 2 dex.

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Ultraviolet tails and trails in cluster galaxies: a sample of candidate gaseous stripping events in Coma

Cited by 183 publications

References 70 publications

Evolution induced by dry minor mergers onto fast-rotator S0 galaxies

Evolution induced by dry minor mergers onto fast-rotator S0 galaxies

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

Molecular Gas Dominated 50 kpc Ram Pressure Stripped Tail of the Coma Galaxy D100^*

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Ultraviolet tails and trails in cluster galaxies: a sample of candidate gaseous stripping events in Coma

Cited by 183 publications

References 70 publications

Evolution induced by dry minor mergers onto fast-rotator S0 galaxies

Evolution induced by dry minor mergers onto fast-rotator S0 galaxies

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

Molecular Gas Dominated 50 kpc Ram Pressure Stripped Tail of the Coma Galaxy D100*

Contact Info

Product

Resources

About

Molecular Gas Dominated 50 kpc Ram Pressure Stripped Tail of the Coma Galaxy D100^*