Caught in the Act: Strong, Active Ram Pressure Stripping in Virgo Cluster Spiral NGC 4330

Abramson, Anne; Kenney, Jeffrey D. P.; Crowl, Hugh H.; Chung, Aeree; Gorkom, J. H. van; Vollmer, B.; Schiminovich, David

doi:10.1088/0004-6256/141/5/164

Cited by 146 publications

(212 citation statements)

References 71 publications

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“…No CO is detected in this gas tail (Vollmer et al 2012). A UV tail is present in the southwest offset from the gas tail (Abramson et al 2011). According to the dynamical model of Vollmer et al (2012) the galaxy is moving to the north.…”

Section: Resultsmentioning

confidence: 98%

“…Compared to Fumagalli et al (2008) we added NGC 4330, NGC 4438, and NGC 4522 to the sample. NGC 4330 and NGC 4522 are undergoing active ram pressure and show extraplanar Hi and UV emission (Abramson et al 2011;Kenney et al 2004). NGC 4438 had a strong tidal interaction ∼100 Myr ago and is now undergoing strong active ram pressure stripping (Vollmer et al 2005b).…”

Section: Datamentioning

confidence: 99%

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The influence of the cluster environment on the star formation efficiency of 12 Virgo spiral galaxies

Vollmer¹,

Wong²,

Braine³

et al. 2012

A&A

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The influence of the environment on gas surface density and star formation efficiency of cluster spiral galaxies is investigated. We extend previous work on radial profiles by a pixel-to pixel analysis looking for asymmetries due to environmental interactions. The star formation rate is derived from GALEX UV and Spitzer total infrared data based on the 8, 24, 70, and 160 μm data. As in field galaxies, the star formation rate for most Virgo galaxies is approximately proportional to the molecular gas mass. Except for NGC 4438, the cluster environment does not affect the star formation efficiency with respect to the molecular gas. Gas truncation is not associated with major changes in the total gas surface density distribution of the inner disk of Virgo spiral galaxies. In three galaxies (NGC 4430, NGC 4501, and NGC 4522), possible increases in the molecular fraction and the star formation efficiency with respect to the total gas, of factors of 1.5 to 2, are observed on the windward side of the galactic disk. A significant increase of the star formation efficiency with respect to the molecular gas content on the windward side of ram pressure-stripped galaxies is not observed. The ram-pressure stripped extraplanar gas of 3 highly inclined spiral galaxies (NGC 4330, NGC 4438, and NGC 4522) shows a depressed star formation efficiency with respect to the total gas, and one of them (NGC 4438) shows a depressed rate even with respect to the molecular gas. The interpretation is that stripped gas loses the gravitational confinement and associated pressure of the galactic disk, and the gas flow is diverging, so the gas density decreases and the star formation rate drops. We found two such regions of low star formation efficiency in the more face-on galaxies NGC 4501 and NGC 4654 which are both undergoing ram pressure stripping. These regions show low radio continuum emission or unusually steep radio spectral index. However, the stripped extraplanar gas in one highly inclined galaxy (NGC 4569) shows a normal star formation efficiency with respect to the total gas. We propose this galaxy is different because it is observed long after peak pressure, and its extraplanar gas is now in a converging flow as it resettles back into the disk.

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Section: Resultsmentioning

confidence: 98%

Section: Datamentioning

confidence: 99%

The influence of the cluster environment on the star formation efficiency of 12 Virgo spiral galaxies

Vollmer¹,

Wong²,

Braine³

et al. 2012

A&A

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“…The Virgo cluster has another major quality: owing to its proximity, the angular resolution of multifrequency data is comparable to that obtained in high-resolution simulations. The comparison of the kinematic and spectrophotometric properties of several bright Virgo galaxies has indeed been crucial for the identification of the perturbing process (Vollmer et al 1999(Vollmer et al , 2000(Vollmer et al , 2005(Vollmer et al , 2006(Vollmer et al , 2008a(Vollmer et al , 2008b(Vollmer et al , 2012Vollmer 2003;Kenney et al 2004;Boselli et al 2005Abramson et al 2011;Kenney et al 2014;Abramson & Kenney 2014;Cortes et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Spectacular tails of ionized gas in the Virgo cluster galaxy NGC 4569

Boselli

Cuillandre

Fossati

et al. 2016

A&A

128

169

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Using MegaCam at the CFHT, we obtained a deep narrow band Hα+ [NII] wide-field image of NGC 4569 (M90), the brightest late-type galaxy in the Virgo cluster. The image reveals the presence of long tails of diffuse ionized gas, without any associated stellar component extending from the disc of the galaxy up to 80 kpc (projected distance) and with a typical surface brightness of a few 10 −18 erg s −1 cm −2 arcsec −2 . These features provide direct evidence that NGC 4569 is undergoing a ram-presure stripping event. The image also shows a prominent 8 kpc spur of ionized gas that is associated with the nucleus that spectroscopic data identify as an outflow. With some assumptions on the 3D distribution of the gas, we use the Hα surface brightness of these extended low-surface brightness features to derive the density and the mass of the gas that has been stripped during the interaction of the galaxy with the intracluster medium. The comparison with ad hoc chemo-spectrophotometric models of galaxy evolution indicates that the mass of the Hα emitting gas in the tail is a large fraction of that of the cold phase that has been stripped from the disc, suggesting that the gas is ionized within the tail during the stripping process. The lack of star-forming regions suggests that mechanisms other than photoionization are responsible for the excitation of the gas (shocks, heat conduction, magneto hydrodynamic waves). This analysis indicates that ram pressure stripping is efficient in massive (M star 10 10.5 M ) galaxies located in intermediate-mass ( 10 14 M ) clusters under formation. It also shows that the mass of gas expelled by the nuclear outflow is only ∼1% than that removed during the ram pressure stripping event. Together these results indicate that ram pressure stripping, rather than starvation through nuclear feedback, can be the dominant mechanism that is responsible for the quenching of the star formation activity of galaxies in high density environments.Key words. galaxies: individual: NGC 4569 -galaxies: clusters: general -galaxies: clusters: individual: Virgo -galaxies: evolutiongalaxies: interactions -galaxies: ISM Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canadian-French-Hawaii Telescope (CFHT) which is operated by the

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“…While good examples of ram pressure stripping are known among the Virgo spiral galaxies (e.g., Kenney et al 2004;Chung et al 2007Chung et al , 2009Abramson et al 2011), none of these galaxies is completely gas stripped and none has such a luminous UV tail, or linear parallel stellar streams, or fireballs as IC3418. 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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Caught in the Act: Strong, Active Ram Pressure Stripping in Virgo Cluster Spiral NGC 4330

Cited by 146 publications

References 71 publications

The influence of the cluster environment on the star formation efficiency of 12 Virgo spiral galaxies

The influence of the cluster environment on the star formation efficiency of 12 Virgo spiral galaxies

Spectacular tails of ionized gas in the Virgo cluster galaxy NGC 4569

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

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