The inner gas mass–temperature profile in the core of nearby galaxy clusters

Liu, Haonan; Fabian, A. C.; Pinto, C.

doi:10.1093/mnras/staa2023

Cited by 3 publications

(3 citation statements)

References 78 publications

(122 reference statements)

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“…Although our cooling flow models find most gas is above 0.7 keV, the detection of the Fe XVII resonance line shows that it is likely to have some cool gas at around 0.5 keV. Liu et al (2020) measured the mass of 0.7 keV in nearby cool core clusters of 10 8 − 10 9 M . RXCJ1504 is likely to have a higher gas mass at this temperature, since the luminosity of the 0.7 keV gas in the two-temperature model is 9 times larger than that of 2A0335+096, which has the largest gas mass below 1 keV.…”

Section: 𝑘𝑇 1kevmentioning

confidence: 59%

“…The condensation of X-ray cooling gas is strongly linked to both the massive molecular gas reservoir and the star formation in the BCG, which are only present when the radiative cooling time falls below a Gyr (Rafferty et al 2008;Pulido et al 2018). Russell et al (2019) and Liu et al (2020) found that the mass of the soft X-ray gas is consistent with the molecular gas mass in the inner 10 kpc. If the X-ray cooling flow is indeed a major source of gas for the molecular gas reservoir and then star formation, we can calculate the timescale for forming the reservoir.…”

Section: 𝑘𝑇 1kevmentioning

confidence: 99%

“…Surprisingly, the RGS spectra have revealed that the molecular gas mass is comparable to the X-ray gas mass emitting below 1 keV in a sample of nearby luminous clusters, e.g. 2A0335+096, A2052, A3581 (Liu et al 2020). These two gas phases are likely intermingled and the structural integrity is held by magnetic fields.…”

Section: Introductionmentioning

confidence: 97%

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Suppressed cooling and turbulent heating in the core of X-ray luminous clusters RXCJ1504.1-0248 and Abell 1664

Liu,

Fabian,

Pinto

et al. 2021

Preprint

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We present the analysis of XMM-Newton observations of two X-ray luminous cool core clusters, RXCJ1504.1-0248 and Abell 1664. The Reflection Grating Spectrometer reveals a radiative cooling rate of 180 ± 40 M yr −1 and 34 ± 6 M yr −1 in RXCJ1504.1-0248 and Abell 1664 for gas above 0.7 keV, respectively. These cooling rates are higher than the star formation rates observed in the clusters, and support simultaneous star formation and molecular gas mass growth on a timescale of 3×10 8 yr or longer. At these rates, the energy of the X-ray cooling gas is inadequate to power the observed UV/optical line-emitting nebulae, which suggests additional strong heating. No significant residual cooling is detected below 0.7 keV in RXCJ1504.1-0248. By simultaneously fitting the first and second order spectra, we place an upper limit on turbulent velocity of 300 km s −1 at 90 per cent confidence level for the soft X-ray emitting gas in both clusters. The turbulent energy density is considered to be less than 8.9 and 27 per cent of the thermal energy density in RXCJ1504.1-0248 and Abell 1664, respectively. This means it is insufficient for AGN heating to fully propagate throughout the cool core via turbulence. We find the cool X-ray component of Abell 1664 (∼0.8 keV) is blueshifted from the systemic velocity by 750 +800 −280 km s −1 . This is consistent with one component of the molecular gas in the core and suggests a similar dynamical structure for the two phases. We find that an intrinsic absorption model allows the cooling rate to increase to 520 ± 30 M yr −1 in RXCJ1504.1-0248.

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Section: 𝑘𝑇 1kevmentioning

confidence: 59%

Section: 𝑘𝑇 1kevmentioning

confidence: 99%

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Suppressed cooling and turbulent heating in the core of X-ray luminous clusters RXCJ1504.1-0248 and Abell 1664

Liu,

Fabian,

Pinto

et al. 2021

Preprint

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Suppressed cooling and turbulent heating in the core of X-ray luminous clusters RXCJ1504.1-0248 and Abell 1664

Liu

Fabian

Pinto

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present the analysis of XMM-Newton observations of two X-ray luminous cool core clusters, RXCJ1504.1-0248 and Abell 1664. The Reflection Grating Spectrometer reveals a radiative cooling rate of $180\pm 40\, \rm M_{\odot }\rm \, yr^{-1}$ and $34\pm 6\, \rm M_{\odot }\rm \, yr^{-1}$ in RXCJ1504.1-0248 and Abell 1664 for gas above 0.7 keV, respectively. These cooling rates are higher than the star formation rates observed in the clusters, and support simultaneous star formation and molecular gas mass growth on a timescale of 3× 108 yr or longer. At these rates, the energy of the X-ray cooling gas is inadequate to power the observed UV/optical line-emitting nebulae, which suggests additional strong heating. No significant residual cooling is detected below 0.7 keV in RXCJ1504.1-0248. By simultaneously fitting the first and second order spectra, we place an upper limit on turbulent velocity of 300 km $\rm s^{-1}$ at 90 per cent confidence level for the soft X-ray emitting gas in both clusters. The turbulent energy density is considered to be less than 8.9 and 27 per cent of the thermal energy density in RXCJ1504.1-0248 and Abell 1664, respectively. This means it is insufficient for AGN heating to fully propagate throughout the cool core via turbulence. We find the cool X-ray component of Abell 1664 (∼0.8 keV) is blueshifted from the systemic velocity by 750$^{+800}_{-280}$ km $\rm s^{-1}$. This is consistent with one component of the molecular gas in the core and suggests a similar dynamical structure for the two phases. We find that an intrinsic absorption model allows the cooling rate to increase to $520\pm 30\, \rm M_{\odot }\rm \, yr^{-1}$ in RXCJ1504.1-0248.

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Hidden cooling flows in clusters of galaxies

Fabian

Ferland

Sanders

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The radiative cooling time of the hot gas at the centres of cool cores in clusters of galaxies drops down to 10 million years and below. The observed mass cooling rate of such gas is very low, suggesting that AGN feedback is very tightly balanced or that the soft X-ray emission from cooling is somehow hidden from view. We use an intrinsic absorption model in which the cooling and coolest gas are closely interleaved to search for hidden cooling flows in the Centaurus, Perseus and A1835 clusters of galaxies. We find hidden mass cooling rates of between 10 to $500\hbox{$\hbox{$\rm M_{\odot }$}{-1}\, $}$ as the cluster mass increases, with the absorbed emission emerging in the Far Infrared band. Good agreement is found between the hidden cooling rate and observed FIR luminosity in the Centaurus Cluster. The limits on the other two clusters allow for considerable hidden cooling. The implied total mass of cooled gas is much larger than the observed molecular masses. We discuss its fate including possible further cooling and collapse into undetected very cold clouds, low mass stars and substellar objects.

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The inner gas mass–temperature profile in the core of nearby galaxy clusters

Cited by 3 publications

References 78 publications

Suppressed cooling and turbulent heating in the core of X-ray luminous clusters RXCJ1504.1-0248 and Abell 1664

Suppressed cooling and turbulent heating in the core of X-ray luminous clusters RXCJ1504.1-0248 and Abell 1664

Suppressed cooling and turbulent heating in the core of X-ray luminous clusters RXCJ1504.1-0248 and Abell 1664

Hidden cooling flows in clusters of galaxies

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