Hidden cooling flows in clusters of galaxies

Fabian, A. C.; Ferland, Gary J.; Sanders, J. S.; McNamara, B. R.; Pinto, C.; Walker, Stephen

doi:10.1093/mnras/stac2003

Cited by 18 publications

(25 citation statements)

References 110 publications

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“…We showed in HCFI (Fabian et al 2022) that, under the high pressure conditions of an HCF (𝑛𝑇 ∼ 10 6.5 − 10 7.5 cm −3 K ) and no heating, the gas cools rapidly (timescale of tens of years) to ∼ 3𝐾. The Jeans mass is below about 0.1 M ⊙ (Jura 1977;Ferland et al 1994) and the gas expected to clump and fragment into low mass stars, brown dwarfs etc, some of which will fall into the black hole emitting little radiation.…”

Section: Accretion Of Fragmented Cold Matter By the Central Black Holementioning

confidence: 78%

“…We have recently found Hidden Cooling Flows in clusters and groups of galaxies, as well as a couple of nearby elliptical galaxies (HCFI and HCFII) (Fabian et al 2022(Fabian et al , 2023, using spectra from the XMM Reflection Grating Spectrometer (RGS). These soft X-ray-emitting flows are hidden within photoelectrically-absorbing cold clouds and dust near the centres of the central brightest galaxies.…”

Section: Introductionmentioning

confidence: 99%

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Hidden Cooling Flows in clusters of Galaxies II: a wider sample

Fabian

Sanders

Ferland

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We have recently uncovered Hidden Cooling Flows (HCFs) in the XMM RGS spectra of 3 clusters of galaxies; Centaurus, Perseus and A1835. Here we search for them in a wider sample of objects: the X-ray brightest group NGC5044; 4 moderate X-ray luminosity clusters Sersic 159, A262, A2052 and RXJ0821; and 3 high X-ray luminosity clusters RXJ1532, MACS 1931 and the Phoenix cluster. Finally we examine two Virgo elliptical galaxies, M49 and M84. All statistically allow the addition of an HCF. We find a significant detection of an HCF in 6 clusters and 2 elliptical galaxies. The hidden mass cooling rates are $5-40\hbox{$\hbox{$\rm \, M_{\odot }$}{-1}\, $}$ for the normal clusters, $1000\hbox{$\hbox{$\rm \, M_{\odot }$}{-1}\, $}$ or more for the extreme clusters and $1-2\hbox{$\hbox{$\rm \, M_{\odot }$}{-1}\, $}$ for the elliptical galaxies. We discuss the implications of the results for the composition of the innermost parts of the massive host galaxies and look forward to future observations.

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Section: Accretion Of Fragmented Cold Matter By the Central Black Holementioning

confidence: 78%

Section: Introductionmentioning

confidence: 99%

Hidden Cooling Flows in clusters of Galaxies II: a wider sample

Fabian

Sanders

Ferland

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…Finally, recent works reported the discovery of hidden cooling flows in a sample of nearby clusters of galaxies, including Perseus (see Fabian et al 2022Fabian et al , 2023aFabian et al , 2023b. Here, the authors argue that AGN feedback may not be as efficient in heating the ICM as initially thought; instead, the ICM would be allowed to cool, explaining the substantial molecular gas reservoirs found in these systems.…”

Section: Extended Filaments and Turbulent Radiative Mixing Layersmentioning

confidence: 90%

“…Indeed, extreme cooling of the gaseous material surrounding BCGs could prohibit them from being detected due to extremely low temperature and emissivity (see Fabian et al 2023a). According to these results, cooling flows of ∼30-100 M e yr −1 could therefore be present within clusters such as the Perseus cluster of galaxies (Fabian et al 2022). Interestingly, it is suggested that these hidden cooling flows could have internal structures resembling that of turbulent radiative mixing layers, similar to those proposed here (see Begelman & Fabian 1990;Fabian et al 2023a).…”

Section: Extended Filaments and Turbulent Radiative Mixing Layersmentioning

confidence: 98%

High-spectral-resolution Observations of the Optical Filamentary Nebula Surrounding NGC 1275

Vigneron,

Hlavacek-Larrondo,

Rhea

et al. 2024

ApJ

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We present new high-spectral-resolution observations (R = λ/Δλ = 7000) of the filamentary nebula surrounding NGC 1275, the central galaxy of the Perseus cluster. These observations have been obtained with SITELLE, an imaging Fourier transform spectrometer installed on the Canada–France–Hawai Telescope with a field of view of 11 ′ × 11 ′ , encapsulating the entire filamentary structure of ionized gas despite its large size of 80 kpc × 50 kpc. Here, we present renewed fluxes, velocities, and velocity dispersion maps that show in great detail the kinematics of the optical nebula at [S ii] λ6716, [S ii] λ6731, [N ii] λ6584, Hα (6563 Å), and [N ii] λ6548. These maps reveal the existence of a bright flattened disk-shaped structure in the core extending to r ∼10 kpc and dominated by a chaotic velocity field. This structure is located in the wake of X-ray cavities and characterized by a high mean velocity dispersion of 134 km s−1. The disk-shaped structure is surrounded by an extended array of filaments spread out to r ∼ 50 kpc that are 10 times fainter in flux, remarkably quiescent, and have a uniform mean velocity dispersion of 44 km s−1. This stability is puzzling given that the cluster core exhibits several energetic phenomena. Based on these results, we argue that there are two mechanisms that form multiphase gas in clusters of galaxies: a first triggered in the wake of X-ray cavities leading to more turbulent multiphase gas and a second, distinct mechanism, that is gentle and leads to large-scale multiphase gas spreading throughout the core.

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“…It may also become sufficiently dense to become optically thick and hence also be affected by coupling to radiation (see Proga et al, 2022). Optically thick gas might be better detected in absorption (unless irradiated) and hence the multiphase medium in the cluster core can be possibly revealed better by considering emission, absorption, and re-emission (e.g., Fabian et al, 2022). There is no systematic theoretical study of the formation of optically thick gas in the diffuse ICM/CGM for the lack of sufficient observational evidence.…”

Section: Thermal Instability In the Icmmentioning

confidence: 99%

Formation of multiphase plasma in galactic haloes and an analogy to solar plasma

Choudhury

2023

Front. Astron. Space Sci.

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Thermal instability (TI) potentially explains the origin of cold gas in the intracluster medium (ICM), which is heated sufficiently by AGN feedback. The Hα filaments seen in cluster cores provide strong motivation for TI. The hot (∼107 K) ICM coronae allow the growth of isobaric TI. The multiphase medium (cold-dense—hot-diffuse) forms once TI saturates. However, gravitational stratification can spatially constrain TI, and thermal conduction is known to stabilize all scales below the field length (λF). In addition, the transport of energy is anisotropic along magnetic fields. Thermal conduction may further trigger gyroscale instabilities and effective reduction of λF. However, cold gas at small scales (<λF) needs to be verified in observations. The virial temperature in galactic haloes is lower (∼106 K) and opens the regime of isochoric TI. In this regime, the cooling time is typically shorter than the sound-crossing time, and large-scale isochoric clouds are rendered unstable. The linear and non-linear isochoric clouds have interesting differences which potentially lead to either fragmentation of the cloud or not. On saturation, TI produces a turbulent medium that helps mix phases and thermalize kinetic energy and thus completes a cycle of condensation and heating. Various aspects of condensation, stratified turbulence, and magnetized transport are physically identical in solar coronae but scaled down to lower luminosity (similar temperatures). We will discuss the recent progress in TI, its connection to observations, and the analogy to solar prominences.

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Hidden cooling flows in clusters of galaxies

Cited by 18 publications

References 110 publications

Hidden Cooling Flows in clusters of Galaxies II: a wider sample

Hidden Cooling Flows in clusters of Galaxies II: a wider sample

High-spectral-resolution Observations of the Optical Filamentary Nebula Surrounding NGC 1275

Formation of multiphase plasma in galactic haloes and an analogy to solar plasma

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