Stripped Elliptical Galaxies as Probes of ICM Physics. III. Deep Chandra Observations of NGC 4552: Measuring the Viscosity of the Intracluster Medium

Kraft, Ralph; Röediger, E.; Macháček, M.; Forman, W.; Nulsen, P. E. J.; Jones, Christine; Churazov, E.; Randall, Scott W.; Su, Yuanyuan; Sheardown, A.

doi:10.3847/1538-4357/aa8a6e

Cited by 28 publications

(22 citation statements)

References 28 publications

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“…Indeed, nearby clusters have shown that ram pressure stripping could lead to tails of cool (≈0.5-1.0 keV) X-ray gas trailing behind galaxies, but such X-ray tails have typical 0.5-2.0 keV X-ray luminosities of ≈10 40 erg s −1 . This is 4 orders of magnitude smaller than what is expected for a cool core in a massive cluster-and would be undetectable with 170 ks of Chandra observations at the redshift of SpARCS1049 (e.g., Sun et al 2010;Zhang et al 2013;Kraft et al 2017). The brightest ram pressure stripped X-ray tail discovered to date has a 0.5-2.0 keV X-ray luminosity of 10 42 erg s −1 (e.g., Schellenberger & Reiprich 2015), which remains too faint to be significantly detected with Chandra in 170 ks at the redshift of SpARCS1049.…”

Section: Runaway Gas Cooling As the Source Of The Starburstmentioning

confidence: 72%

Evidence of Runaway Gas Cooling in the Absence of Supermassive Black Hole Feedback at the Epoch of Cluster Formation

Hlavacek-Larrondo

Rhea

Webb

et al. 2020

ApJL

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Cosmological simulations, as well as mounting evidence from observations, have shown that supermassive black holes play a fundamental role in regulating the formation of stars throughout cosmic time. This has been clearly demonstrated in the case of galaxy clusters in which powerful feedback from the central black hole is preventing the hot intracluster gas from cooling catastrophically, thus reducing the expected star formation rates by orders of magnitude. These conclusions, however, have been almost entirely based on nearby clusters. Based on new Chandra X-ray observations, we present the first observational evidence for massive, runaway cooling occurring in the absence of supermassive black hole feedback in the high-redshift galaxy cluster SpARCS104922.6+564032.5 (z=1.709). The hot intracluster gas appears to be fueling a massive burst of star formation (≈900 M e yr −1) that is offset by dozens of kpc from the central galaxy. The burst is co-spatial with the coolest intracluster gas but not associated with any galaxy in the cluster. In less than 100 million years, such runaway cooling can form the same amount of stars as in the Milky Way. Therefore, intracluster stars are not only produced by tidal stripping and the disruption of cluster galaxies, but can also be produced by runaway cooling of hot intracluster gas at early times. Overall, these observations show the dramatic impact when supermassive black hole feedback fails to operate in clusters. They indicate that in the highest overdensities, such as clusters and protoclusters, runaway cooling may be a new and important mechanism for fueling massive bursts of star formation in the early universe. Unified Astronomy Thesaurus concepts: High-redshift galaxy clusters (2007); Supermassive black holes (1663); Cooling flows (2028); Intracluster medium (858); X-ray observatories (1819)

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Section: Runaway Gas Cooling As the Source Of The Starburstmentioning

confidence: 72%

Evidence of Runaway Gas Cooling in the Absence of Supermassive Black Hole Feedback at the Epoch of Cluster Formation

Hlavacek-Larrondo

Rhea

Webb

et al. 2020

ApJL

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“…Several external processes have been proposed to explain the quenching of star-forming galaxies as they become satellites. Examples include ram-pressure stripping (Gunn & Gott 1972;McCarthy et al 2008), thermal evaporation (Cowie & Songaila 1977;Nipoti & Binney 2007), and viscous stripping (Nulsen 1982;Kraft et al 2017), all of which invoke the removal of the cold interstellar medium of a galaxy via its hydrodynamical interaction with the hot intergalactic medium of high-density environments as the reason for quenching. These processes are correlated with the velocity of a galaxy as it travels through its environment, and generally quench galaxies quickly.…”

Section: Satellite Quenching At Low Redshiftsmentioning

confidence: 99%

Synergies between low- and intermediate-redshift galaxy populations revealed with unsupervised machine learning

Turner

Siudek

Salim

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The colour bimodality of galaxies provides an empirical basis for theories of galaxy evolution. However, the balance of processes that begets this bimodality has not yet been constrained. A more detailed view of the galaxy population is needed, which we achieve in this paper by using unsupervised machine learning to combine multi-dimensional data at two different epochs. We aim to understand the cosmic evolution of galaxy subpopulations by uncovering substructures within the colour bimodality. We choose a clustering algorithm that models clusters using only the most discriminative data available, and apply it to two galaxy samples: one from the second edition of the GALEX-SDSS-WISE Legacy Catalogue (GSWLC-2; z ∼ 0.06), and the other from the VIMOS Public Extragalactic Redshift Survey (VIPERS; z ∼ 0.65). We cluster within a nine-dimensional feature space defined purely by rest-frame ultraviolet-through-near-infrared colours. Both samples are similarly partitioned into seven clusters, breaking down into four of mostly star-forming galaxies (including the vast majority of green valley galaxies) and three of mostly passive galaxies. The separation between these two families of clusters suggests differences in the evolution of their galaxies, and that these differences are strongly expressed in their colours alone. The samples are closely related, with star-forming/green-valley clusters at both epochs forming morphological sequences, capturing the gradual internally-driven growth of galaxy bulges. At high stellar masses, this growth is linked with quenching. However, it is only in our low-redshift sample that additional, environmental processes appear to be involved in the evolution of low-mass passive galaxies.

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“…In Figure 5, we present the XMM-Newton surface brightness profile of M49 in the 0.7-1.3 keV energy band to the north. The energy band was chosen to maximize the source-to-background ratio (Ettori et al 2010;Kraft et al 2017). The previously reported bright edge (Irwin & Sarazin 1996;Biller et al 2004;Kraft et al 2011) is visible at ∼ 20 kpc north of the group center (marked by the magenta solid line).…”

Section: Surface Brightness and Contact Discontinuitymentioning

confidence: 99%

Extended X-Ray Study of M49: The Frontier of the Virgo Cluster

Kraft

Nulsen

et al. 2019

Self Cite

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The M49 group, resident outside the virial radius of the Virgo cluster, is falling onto the cluster from the south. We report results from deep XMM-Newton mosaic observations of M49. Its hot gas temperature is 0.8 keV at the group center and rises to 1.5 keV beyond the brightest group galaxy (BGG). The group gas extends to radii of ∼ 300 kpc to the north and south. The observations reveal a cold front ∼ 20 kpc north of the BGG center and an X-ray bright stripped tail 70 kpc long and 10 kpc wide to the southwest of the BGG. We argue that the atmosphere of the infalling group was slowed by its encounter with the Virgo cluster gas, causing the BGG to move forward subsonically relative to the group gas. We measure declining temperature and metallicity gradients along the stripped tail. The tail gas can be traced back to the cooler and enriched gas uplifted from the BGG center by buoyant bubbles, implying that AGN outbursts may have intensified the stripping process. We extrapolate to a virial radius of 740 kpc and derive a virial mass of 4.6 × 10 13 M for the M49 group. Its group atmosphere appears truncated and deficient when compared with isolated galaxy groups of similar temperatures. If M49 is on its first infall to Virgo, the infall region of a cluster could have profound impacts on galaxies and groups that are being accreted onto galaxy clusters. Alternatively, M49 may have already passed through Virgo once.

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Stripped Elliptical Galaxies as Probes of ICM Physics. III. Deep Chandra Observations of NGC 4552: Measuring the Viscosity of the Intracluster Medium

Cited by 28 publications

References 28 publications

Evidence of Runaway Gas Cooling in the Absence of Supermassive Black Hole Feedback at the Epoch of Cluster Formation

Evidence of Runaway Gas Cooling in the Absence of Supermassive Black Hole Feedback at the Epoch of Cluster Formation

Synergies between low- and intermediate-redshift galaxy populations revealed with unsupervised machine learning

Extended X-Ray Study of M49: The Frontier of the Virgo Cluster

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