The Warm–Hot, Extended, Massive Circumgalactic Medium of NGC 3221: An XMM-Newton Discovery

Das, Sanskriti; Mathur, S.; Gupta, Anjali

doi:10.3847/1538-4357/ab93d2

Cited by 26 publications

(21 citation statements)

References 46 publications

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“…Moreover, it agrees with previous indications that the missing baryons are likely significantly correlated with galaxies and groups (e.g. Nicastro et al 2018;Lim et al 2020;Das et al 2019Das et al , 2020.…”

Section: Quantitative Comparison In the Sdss Footprintsupporting

confidence: 91%

Testing the Strong Equivalence Principle. II. Relating the External Field Effect in Galaxy Rotation Curves to the Large-Scale Structure of the Universe

Chae,

Desmond,

Lelli

et al. 2021

Preprint

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Theories of modified gravity generically violate the strong equivalence principle, so that the internal dynamics of a self-gravitating system in free fall depends on the strength of the external gravitational field (the external field effect). We fit rotation curves (RCs) from the SPARC database with a model inspired by Milgromian dynamics (MOND), which relates the outer shape of a RC to the external Newtonian field from the large-scale baryonic matter distribution through a dimensionless parameter e N . We obtain a > 4σ statistical detection of the external field effect (i.e. e N > 0 on average), confirming previous results. We then locate the SPARC galaxies in the cosmic web of the nearby Universe and find a striking contrast in the fitted e N values for galaxies in underdense versus overdense regions. Galaxies in an underdense region between 22 and 45 Mpc from the celestial axis in the northern sky have RC fits consistent with e N 0, while those in overdense regions adjacent to the CfA2 great wall and the Perseus-Pisces supercluster return e N that are a factor of two larger than the median for SPARC galaxies. We also calculate independent estimates of e N from galaxy survey data and find that they agree with the e N inferred from the RCs within the uncertainties, the chief uncertainty being the spatial distribution of baryons not contained in galaxies or clusters.

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Section: Quantitative Comparison In the Sdss Footprintsupporting

confidence: 91%

Testing the Strong Equivalence Principle. II. Relating the External Field Effect in Galaxy Rotation Curves to the Large-Scale Structure of the Universe

Chae,

Desmond,

Lelli

et al. 2021

Preprint

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“…Anderson et al (2016); Dai et al (2012), which could be at odds with our concentrated hot gas halo in CR+. However, to the best of our knowledge, these extended hot halos are detected only around galaxies much more massive than our simulated galaxies, objects with the AGNs, or in starbursts (Wang et al 2001;Fraternali et al 2002;Das et al 2020), which are not included in our simulation sample.…”

Section: Hot Ionized Gasmentioning

confidence: 65%

The impact of cosmic rays on dynamical balance and disk-halo interaction in Lstar disk galaxies

Chan,

Keres,

Gurvich

et al. 2021

Preprint

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Cosmic rays (CRs) are an important component in the interstellar medium (ISM), but their effect on the dynamics of the disk-halo interface (< 10 kpc from the disk) is still unclear. We study the influence of CRs on the gas above the disk with highresolution FIRE-2 cosmological simulations of late-type L galaxies at redshift z ∼ 0. We compare runs with and without CR feedback (with constant anisotropic diffusion κ ∼ 3 × 10 29 cm 2 /s and streaming). Our simulations capture the relevant disk halo interactions, including outflows, inflows, and galactic fountains. Extra-planar gas in all of the runs satisfies dynamical balance, where total pressure balances the weight of the overlying gas. While the kinetic pressure from non-uniform motion ( 1 kpc scale) dominates in the midplane, thermal and bulk pressures (or CR pressure if included) take over at large heights. We find that with CR feedback, (1) the warm (∼ 10 4 K) gas is slowly accelerated by CRs; (2) the hot (> 5 × 10 5 K) gas scale height is suppressed;(3) the warm-hot (2 × 10 4 − 5 × 10 5 K) medium becomes the most volume-filling phase in the disk-halo interface. We develop a novel conceptual model of the near-disk gas dynamics in low-redshift L galaxies: with CRs, the disk-halo interface is filled with CR-driven warm winds and hot super-bubbles that are propagating into the CGM with a small fraction falling back to the disk. Without CRs, most outflows from hot superbubbles are trapped by the existing hot halo and gravity, so typically they form galactic fountains.

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“…The detectability of emission is not easy to define. For example, Das et al (2020) use two different tests to investigate how far from the galaxy they can detect emission. Detection might be limited by backgrounds and foregrounds (both astrophysical and instrumental), and non-CGM emission correlated with the source.…”

Section: Detectabilitymentioning

confidence: 99%

“…For lower-mass, spiral galaxies, studies have typically found upper limits or emission only in or close to galaxies (e.g., Bogdán et al 2015). However, Das et al (2020) found emission further from the galaxy, and measured a temperature profile out to ≈ 200 kpc.…”

Section: Introductionmentioning

confidence: 99%

The warm-hot circumgalactic medium around EAGLE-simulation galaxies and its detection prospects with X-ray and UV line absorption

Wijers

Schaye

Oppenheimer

2020

Monthly Notices of the Royal Astronomical Society

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We use the EAGLE cosmological simulation to study the distribution of baryons, and FUV (O vi), EUV (Ne viii) and X-ray (O vii, O viii, Ne ix, and Fe xvii) line absorbers, around galaxies and haloes of mass $\, \rm {M}_{\rm {200c}}= 10^{11}$–$10^{14.5} \, \rm {M}_{\odot }$ at redshift 0.1. EAGLE predicts that the circumgalactic medium (CGM) contains more metals than the interstellar medium across halo masses. The ions we study here trace the warm-hot, volume-filling phase of the CGM, but are biased towards temperatures corresponding to the collisional ionization peak for each ion, and towards high metallicities. Gas well within the virial radius is mostly collisionally ionized, but around and beyond this radius, and for O vi, photo-ionization becomes significant. When presenting observables we work with column densities, but quantify their relation with equivalent widths by analysing virtual spectra. Virial-temperature collisional ionization equilibrium ion fractions are good predictors of column density trends with halo mass, but underestimate the diversity of ions in haloes. Halo gas dominates the highest column density absorption for X-ray lines, but lower-density gas contributes to strong UV absorption lines from O vi and Ne viii. Of the O vii (O viii) absorbers detectable in an Athena X-IFU blind survey, we find that 41 (56) per cent arise from haloes with $\, \rm {M}_{\rm {200c}}= 10^{12.0 \rm {-}13.5} \, \rm {M}_{\odot }$. We predict that the X-IFU will detect O vii (O viii) in 77 (46) per cent of the sightlines passing $\, \rm {M}_{\star }= 10^{10.5 \rm {-}11.0} \, \rm {M}_{\odot }$ galaxies within $100 \, \rm {pkpc}$ (59 (82) per cent for $\, \rm {M}_{\star }> 10^{11.0} \, \rm {M}_{\odot }$). Hence, the X-IFU will probe covering fractions comparable to those detected with the Cosmic Origins Spectrograph for O vi.

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The Warm–Hot, Extended, Massive Circumgalactic Medium of NGC 3221: An XMM-Newton Discovery

Cited by 26 publications

References 46 publications

Testing the Strong Equivalence Principle. II. Relating the External Field Effect in Galaxy Rotation Curves to the Large-Scale Structure of the Universe

Testing the Strong Equivalence Principle. II. Relating the External Field Effect in Galaxy Rotation Curves to the Large-Scale Structure of the Universe

The impact of cosmic rays on dynamical balance and disk-halo interaction in Lstar disk galaxies

The warm-hot circumgalactic medium around EAGLE-simulation galaxies and its detection prospects with X-ray and UV line absorption

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