Survival of molecular gas in Virgo’s hot intracluster medium: CO near M 86

Dasyra, K. M.; Combes, F.; Salomé, P.; Braine, J.

doi:10.1051/0004-6361/201218775

Cited by 14 publications

(13 citation statements)

References 68 publications

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“…In a previous paper, we already found molecular gas in a ionized gas tail south of M86 (Dasyra et al 2012), and discussed its survival conditions. Here we study the link between new stars formed and molecular gas to derive the star formation efficiency.…”

Section: Introductionmentioning

confidence: 90%

“…Machacek et al 2005, Sun et al 2010. In rarer cases, stripped gas can be seen as dense and cold molecular gas, detected as carbon monoxide (CO) emission (Vollmer et al 2005;Dasyra et al 2012;Jáchym et al 2014). The presence of these dense molecular clumps might appear surprising, since the RPS should not be able to drag them out of their galaxy disks (Nulsen 1982;Kenney & Young 1989).…”

Section: Introductionmentioning

confidence: 99%

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Ram pressure stripping in the Virgo Cluster

Verdugo

Combes

Dasyra

et al. 2015

A&A

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Gas can be violently stripped from their galaxy disks in rich clusters, and be dispersed over 100 kpc-scale tails or plumes. Young stars have been observed in these tails, suggesting they are formed in situ. This will contribute to the intracluster light, in addition to tidal stripping of old stars. We want to quantify the efficiency of intracluster star formation. We present CO(1-0) and CO(2-1) observations, made with the IRAM-30 m telescope, towards the ram-pressure stripped tail northeast of NGC 4388 in Virgo. We selected HII regions found all along the tails, together with dust patches, as observing targets. We detect molecular gas in 4 positions along the tail, with masses between 7 × 10 5 to 2 × 10 6 M . Given the large distance from the NGC 4388 galaxy, the molecular clouds must have formed in situ, from the HI gas plume. We compute the relation between surface densities of star formation and molecular gas in these regions, and find that the star formation has very low efficiency. The corresponding depletion time of the molecular gas can be up to 500 Gyr and more. Since this value exceeds a by far Hubble time, this gas will not be converted into stars, and will stay in a gaseous phase to join the intracluster medium.

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Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

Ram pressure stripping in the Virgo Cluster

Verdugo

Combes

Dasyra

et al. 2015

A&A

Self Cite

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“…Dasyra et al 2012). Studies of these filaments should help our understanding of the filaments around BCGs and vice versa.…”

Section: Heating Of Cold Gas By Energetic Particlesmentioning

confidence: 99%

Observational Evidence of Active Galactic Nuclei Feedback

Fabian

2012

Annu. Rev. Astron. Astrophys.

2,452

2,070

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Radiation, winds and jets from the active nucleus of a massive galaxy can interact with its interstellar medium leading to ejection or heating of the gas. This can terminate star formation in the galaxy and stifle accretion onto the black hole. Such Active Galactic Nucleus (AGN) feedback can account for the observed proportionality between central black hole and host galaxy mass. Direct observational evidence for the radiative or quasar mode of feedback, which occurs when the AGN is very luminous, has been difficult to obtain but is accumulating from a few exceptional objects. Feedback from the kinetic or radio mode, which uses the mechanical energy of radio-emitting jets often seen when the AGN is operating at a lower level, is common in massive elliptical galaxies. This mode is well observed directly through X-ray observations of the central galaxies of cool core clusters in the form of bubbles in the hot surrounding medium. The energy flow, which is roughly continuous, heats the hot intracluster gas and reduces radiative cooling and subsequent star formation by an order of magnitude. Feedback appears to maintain a long-lived heating/cooling balance. Powerful, jetted radio outbursts may represent a further mode of energy feedback which affect the cores of groups and subclusters. New telescopes and instruments from the radio to X-ray bands will come into operation over the next few years and lead to a rapid expansion in observational data on all modes of AGN feedback.

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“…Observationally, although extended molecular tails can survive after being stripped from the galaxies (e.g., through ram pressure stripping, Dasyra et al 2012;Jachym et al 2014), it is not common to find a significant amount of molecular gas in tidal tails. Aalto et al (2001) found 4% (M mol ≈ 8 × 10 7 M ) of the molecular gas along a 10 kpc long optical tidal tail in NGC 4194, an elliptical/disk merger remnant.…”

Section: Origin Of the Molecular Gasmentioning

confidence: 99%

Alma Observations of a Candidate Molecular Outflow in an Obscured Quasar

Sun

Greene

Zakamska

et al. 2014

ApJ

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We present Atacama Large Millimeter/Submillimeter Array CO (1-0) and CO (3-2) observations of SDSS J135646.10+102609.0, an obscured quasar and ultra-luminous infrared galaxy with two merging nuclei and a known 20 kpc scale ionized outflow. The total molecular gas mass is M mol ≈ 9 +19 −6 × 10 8 M , mostly distributed in a compact rotating disk at the primary nucleus (M mol ≈ 3 × 10 8 M ) and an extended tidal arm (M mol ≈ 5 × 10 8 M ). The tidal arm is one of the most massive molecular tidal features known; we suggest that it is due to the lower chance of shock dissociation in this elliptical/disk galaxy merger. In the spatially resolved CO (3-2) data, we find a compact (r ≈ 0.3 kpc) high-velocity (v ≈ 500 km s −1 ) redshifted feature in addition to the rotation at the N nucleus. We propose a molecular outflow as the most likely explanation for the high-velocity gas. The outflowing mass of M mol ≈ 7 × 10 7 M and the short dynamical time of t dyn ≈ 0.6 Myr yield a very high outflow rate ofṀ mol ≈ 350 M yr −1 and can deplete the gas in a million years. We find a low star formation rate (<16 M yr −1 from the molecular content and <21 M yr −1 from the far-infrared spectral energy distribution decomposition) that is inadequate to supply the kinetic luminosity of the outflow (Ė ≈ 3 × 10 43 erg s −1 ). Therefore, the active galactic nucleus (AGN), with a bolometric luminosity of 10 46 erg s −1 , likely powers the outflow. The momentum boost rate of the outflow (ṗ/(L bol /c) ≈ 3) is lower than typical molecular outflows associated with AGNs, which may be related to its compactness. The molecular and ionized outflows are likely two distinct bursts induced by episodic AGN activity which varies on a timescale of 10 7 yr.

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Survival of molecular gas in Virgo’s hot intracluster medium: CO near M 86

Cited by 14 publications

References 68 publications

Ram pressure stripping in the Virgo Cluster

Ram pressure stripping in the Virgo Cluster

Observational Evidence of Active Galactic Nuclei Feedback

Alma Observations of a Candidate Molecular Outflow in an Obscured Quasar

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