X-ray observations of galaxies in the Virgo cluster

Forman, W.; Schwarz, J.; Jones, C.; Liller, W.; Fabian, A. C.

doi:10.1086/183103

Cited by 174 publications

(120 citation statements)

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“…The interaction between NGC 4438 and M 86 is confirmed by a spectacular, ∼120 kpc-long, Hα-emitting tidal bridge that connects them (Kenney et al 2008). The smooth Hα velocity gradient along this bridge convincingly places it to the ICM of Virgo, which is rich in X-ray emission (Forman et al 1979;Rangarajan et al 1995;Machacek et al 2004;Liu & Bregman 2005;Randall et al 2008). Since the X-ray heating and the ram pressure disperse the ICM atomic gas, a significant fraction of the Hα emission could originate from the ionized gas in the outer layers of molecular clouds (Ferland et al 2009).…”

Section: Introductionmentioning

confidence: 83%

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

Dasyra

Combes

Salomé

et al. 2012

A&A

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We carried out 12 CO(1−0) and 12 CO(2−1) observations of 21 different regions in the vicinity of M 86, NGC 4438, and along the 120 kpc-long, Hα-emitting filamentary trail that connects them, aiming to test whether molecular gas can survive to be transferred from a spiral to an elliptical galaxy in Virgo's 10 7 K intracluster medium (ICM). We targeted Hα-emitting regions that could be associated with the interface between cold molecular clouds and the hot ionized ICM. The data, obtained with the 30 m telescope of the Institut de Radioastronomie Millimétrique, led to the detection of molecular gas close to M 86. CO gas with a recession velocity that is similar to that of the stars, −265 km s −1 , and with a corresponding H 2 mass of 2 × 10 7 M , was detected ∼10 kpc southeast of the nucleus of M 86, near the peak of its H i emission. We argue that it is possible for this molecular gas either to have formed in situ from H i, or to have been stripped from NGC 4438 directly in molecular form. In situ formation is nonetheless negligible for the 7 × 10 6 M of gas detected at 12:26:15.9+12:58:49, at ∼10 kpc northeast of M 86, where no (strong) H i emission is present. This detection provides evidence for the survival of molecular gas in filaments for timescales of ∼100 Myr. An amount equivalent to 5 × 10 7 M of H 2 gas that could be lost to the ICM or to neighboring galaxies was also discovered in the tidal tail northwest of NGC 4438. A scenario in which gas was alternatively brought to M 86 from NGC 4388 was also examined but it was considered unlikely because of the non-detection of CO below or at the H I stream velocities, 2000-2700 km s −1 .

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Section: Introductionmentioning

confidence: 83%

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

Dasyra

Combes

Salomé

et al. 2012

A&A

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“…Often observed in nearby clusters are infalling galaxies with a truncated interstellar medium (ISM) (Su et al 2015), a cold front at the leading edge, and a downstream tail of stripped galactic gas (M86- Forman et al 1979;Randall et al 2008;NGC 1400-Su et al 2014M49-Kraft et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Deep Chandra Observations of NGC 1404: Cluster Plasma Physics Revealed by an Infalling Early-Type Galaxy

Kraft

Röediger

et al. 2017

ApJ

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The intracluster medium (ICM), as a magnetized and highly ionized fluid, provides an ideal laboratory to study plasma physics under extreme conditions that cannot yet be achieved on Earth. NGC 1404 is a bright elliptical galaxy that is being gas stripped as it falls through the ICM of the Fornax Cluster. We use the new Chandra X-ray observations of NGC 1404 to study ICM microphysics. The interstellar medium (ISM) of NGC 1404 is characterized by a sharp leading edge, 8 kpc from the galaxy center, and a short downstream gaseous tail. Contact discontinuities are resolved on unprecedented spatial scales (0. 5 = 45 pc) due to the combination of the proximity of NGC 1404, the superb spatial resolution of Chandra, and the very deep (670 ksec) exposure. At the leading edge, we observe sub-kpc scale eddies generated by Kelvin-Helmholtz instability and put an upper limit of 5% Spitzer on the isotropic viscosity of the hot cluster plasma. We also observe mixing between the hot cluster gas and the cooler galaxy gas in the downstream stripped tail, which provides further evidence of a low viscosity plasma. The assumed ordered magnetic fields in the ICM ought to be smaller than 5 µG to allow KHI to develop. The lack of evident magnetic draping layer just outside the contact edge is consistent with such an upper limit.

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“…Early studies of optically selected samples of early-type galaxies with EINSTEIN Fabbiano et al 1987) have examined the relation between the X-ray, the blue optical and radio luminosities and argued that the X-ray luminosity arises from a combination of low-mass X-ray binaries (LMXRBs) and hot gas (e.g. Forman et al 1979). On the other hand, the X-ray study of late-type systems with EINSTEIN Fabbiano et al 1988) has revealed a different kind of X-ray correlation for the radio (shallower) and blue (more linear) luminosities, as well as a correlation between X-ray and infrared luminosity, suggesting a link with on-going star formation or starburst activity.…”

Section: Introductionmentioning

confidence: 99%

Normal galaxies in the XMM-Newton fields

Rovilos

Georgantopoulos

Tzanavaris

et al. 2009

A&A

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Context. We use the first XMM serendipitous source catalogue (1XMM) to compile a sample of normal X-ray galaxies. Aims. We seek to expand the database of X-ray selected normal galaxies at intermediate redshifts and examine the relation between X-ray emission and star formation for late-type systems. Methods. The candidates are selected based on their X-ray (soft spectra), X-ray to optical (log( f x / f o ) < −2) and optical (extended sources) properties. 44 candidates are found and 35 are spectroscopically observed with the Australian National University's 2.3 m telescope to examine their nature. Results. Of the 35 sources observed, 2 are AGN, 11 emission line galaxies, 12 absorption line galaxies, 6 have featureless spectra while 4 are associated with Galactic stars. We combine our emission line sample with earlier works forming the most comprehensive X-ray selected galaxy sample for the study of the X-ray luminosity to the Hα luminosity -a well-calibrated star-formation indicator -relation. Conclusions. We find that the X-ray luminosity strongly correlates with the Hα luminosity, suggesting that the X-rays efficiently trace the star-formation.

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X-ray observations of galaxies in the Virgo cluster

Cited by 174 publications

References 0 publications

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

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

Deep Chandra Observations of NGC 1404: Cluster Plasma Physics Revealed by an Infalling Early-Type Galaxy

Normal galaxies in the XMM-Newton fields

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