The X-Ray Halo Scaling Relations of Supermassive Black Holes

Gaspari, M.; Eckert, D.; Ettori, S.; Tozzi, P.; Bassini, Luigi; Rasia, Elena; Brighenti, Fabrizio; Sun, Ming; Borgani, S.; Johnson, Sean D.; Tremblay, G. R.; Stone, James M.; Temi, P.; Yang, H.-Y. Karen; Tombesi, Francesco; Cappi, M.

doi:10.3847/1538-4357/ab3c5d

Cited by 97 publications

(157 citation statements)

References 241 publications

(267 reference statements)

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“…• Within R500c: both simulated TNG MBH − TX and MBH − LX relations are in good agreement with the observed data from Bogdán et al 2018and Gaspari et al (2019). We should however recall that here the integration boundary R500c for the simulation X-ray measurements is taken directly from the simulation output, it is the true one, i.e.…”

Section: Comparison With X-ray Observationssupporting

confidence: 78%

“…Finally, at least within the TNG modeling, SMBH feedback does leave an imprint on the thermodynamical (and thus X-ray observable) properties of the circum-galactic and halo gas also in the outer reaches of the gaseous haloes, as theoretically advocated and demonstrated also by, among others, Gaspari et al 2019;Zinger et al 2020 and previously e.g. Barnes et al 2017;Le Brun et al 2017;Truong et al 2018.…”

Section: The Effects Of Stellar and Smbh Feedback On Smbh-hot Atmosphmentioning

confidence: 61%

“…On the other hand, Gaspari et al (2019) find that the SMBH mass correlates with the X-ray quantities for their whole mixedtype sample of galaxies, and the scatter remains approximately constant across the investigated dynamical range. They interpret the correlations between the SMBH mass and the hot atmospheres as a consequence of the chaotic cold accretion (CCA) of the gas condensed out of the turbulent X-ray atmosphere onto the central SMBH, whereby sustaining a self-regulated feedback loop.…”

Section: Introductionmentioning

confidence: 84%

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X-ray signatures of black hole feedback: hot galactic atmospheres in IllustrisTNG and X-ray observations

Truong

Pillepich

Werner

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Hot gaseous atmospheres that permeate galaxies and extend far beyond their stellar distribution, where they are commonly referred to as the circumgalactic medium (CGM), imprint important information about feedback processes powered by the stellar populations of galaxies and their central supermassive black holes (SMBH). In this work we study the properties of this hot X-ray emitting medium using the IllustrisTNG cosmological simulations. We analyse their mock X-ray spectra, obtained in TNG100 and TNG50, and compare the results with X-ray observations of nearby early-type galaxies. The simulations reproduce the observed X-ray luminosities (L X ) and temperature (T X ) at small (< R e ) and intermediate (< 5R e ) radii reasonably well. We find that the X-ray properties of lower mass galaxies depend on their star formation rates. In particular, in the magnitude range where the star-forming and quenched populations overlap, M K ∼ −24 (M * ∼ 10 10.7 M ), we find that the X-ray luminosities of star-forming galaxies are on average about an order of magnitude higher than those of their quenched counterparts. We show that this diversity in L X is a direct manifestation of the quenching mechanism in the simulations, where the galaxies are quenched due to gas expulsion driven by SMBH kinetic feedback. The observed dichotomy in L X is thus an important observable prediction for the SMBH feedback-based quenching mechanisms implemented in state-of-the-art cosmological simulations. While the current X-ray observations of star forming galaxies are broadly consistent with the predictions of the simulations, the observed samples are small and more decisive tests are expected from the sensitive all-sky X-ray survey with eROSITA.

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Section: Comparison With X-ray Observationssupporting

confidence: 78%

Section: The Effects Of Stellar and Smbh Feedback On Smbh-hot Atmosphmentioning

confidence: 61%

Section: Introductionmentioning

confidence: 84%

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X-ray signatures of black hole feedback: hot galactic atmospheres in IllustrisTNG and X-ray observations

Truong

Pillepich

Werner

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…where Γ gas = 5/3, µ = 1 is the mean molecular weight of the gas, and k B and m h are the Boltzmann's constant and the mass of the hydrogen atom, respectively. Given that the temperature (T ) of the IGM surrounding Fornax A (60 < r < 350 kpc) is ∼ 2.7 × 10 7 K (∼ 0.65 − 0.77 keV, as measured from the X-ray emission of the hot halo of NGC 1316; Isobe et al 2006;Nagino & Matsushita 2009;Gaspari et al 2019), the speed of sound is c s = 529 km s −1 . If the lobes expanded through the IGM at this speed, it would have taken ∼ 200 Myr to reach their current size.…”

Section: Discussionmentioning

confidence: 99%

The flickering nuclear activity of Fornax A

Maccagni

Murgia

Serra

et al. 2020

A&A

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We present new observations of Fornax A taken at ∼ 1 GHz with the MeerKAT telescope and at ∼ 6 GHz with the Sardinia Radio Telescope (SRT). The sensitive (noise ∼ 16 µJy beam −1 ), high resolution ( 10 ) MeerKAT images show that the lobes of Fornax A have a double-shell morphology, where dense filaments are embedded in a diffuse and extended cocoon. We study the spectral properties of these components by combining the MeerKAT and SRT observations with archival data between 84 MHz and 217 GHz. For the first time, we show that multiple episodes of nuclear activity must have formed the extended radio lobes. The modelling of the radio spectrum suggests that the last episode of injection of relativistic particles into the lobes started ∼ 24 Myr ago and stopped 12 Myr ago. More recently (∼ 3 Myr ago), a less powerful and short ( 1 Myr) phase of nuclear activity generated the central jets. Currently, the core may be in a new active phase. It appears that Fornax A is rapidly flickering. The dense environment in which Fornax A lives has lead to a complex recent merger history for this galaxy, including mergers spanning a range of gas contents and mass ratios, as shown by the analysis of the galaxy's stellar-and cold-gas phases. This complex recent history may be the cause of the rapid, recurrent nuclear activity of Fornax A.

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“…Given that elliptical galaxies show hot atmospheres even in compact, isolated halos (e.g. Reiprich & Böhringer 2002;Kim et al 2019;Lakhchaura et al 2019a;Gaspari et al 2019), and under the condition that plasma emission codes will further provide the necessary accuracy, similar IMF studies can be expanded to the low-mass regime with similar statistics (e.g. lower luminosity is compensated by higher line emissivity of α-elements due to cooler plasma temperature).…”

Section: Constraints On the Imfmentioning

confidence: 99%

Constraining the origin and models of chemical enrichment in galaxy clusters using theAthenaX-IFU

Mernier

Cucchetti

Tornatore

et al. 2020

A&A

Self Cite

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Chemical enrichment of the Universe at all scales is related to stellar winds and explosive supernovae phenomena. Metals produced by stars and later spread throughout the intracluster medium (ICM) at the megaparsec scale become a fossil record of the chemical enrichment of the Universe and of the dynamical and feedback mechanisms determining their circulation. As demonstrated by the results of the soft X-ray spectrometer onboard Hitomi, high-resolution X-ray spectroscopy is the path to differentiating among the models that consider different metal-production mechanisms, predict the outcoming yields, and are a function of the nature, mass, and/or initial metallicity of their stellar progenitor. Transformational results shall be achieved through improvements in the energy resolution and effective area of X-ray observatories, allowing them to detect rarer metals (e.g. Na, Al) and constrain yet-uncertain abundances (e.g. C, Ne, Ca, Ni). The X-ray Integral Field Unit (X-IFU) instrument onboard the next-generation European X-ray observatory Athena is expected to deliver such breakthroughs. Starting from 100 ks of synthetic observations of 12 abundance ratios in the ICM of four simulated clusters, we demonstrate that the X-IFU will be capable of recovering the input chemical enrichment models at both low (z = 0.1) and high (z = 1) redshifts, while statistically excluding more than 99.5% of all the other tested combinations of models. By fixing the enrichment models which provide the best fit to the simulated data, we also show that the X-IFU will constrain the slope of the stellar initial mass function within ∼12%. These constraints will be key ingredients in our understanding of the chemical enrichment of the Universe and its evolution.

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The X-Ray Halo Scaling Relations of Supermassive Black Holes

Cited by 97 publications

References 241 publications

X-ray signatures of black hole feedback: hot galactic atmospheres in IllustrisTNG and X-ray observations

X-ray signatures of black hole feedback: hot galactic atmospheres in IllustrisTNG and X-ray observations

The flickering nuclear activity of Fornax A

Constraining the origin and models of chemical enrichment in galaxy clusters using theAthenaX-IFU

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