The evolution of structure and feedback with <i>Arcus</i>

Brenneman, Laura; Bregman, Joel N.; Kaastra, J. S.; Brickhouse, N. S.; Allured, Ryan; Foster, Adam; Wolk, S. J.; Wilms, J.; Valencic, Lynne; Willingale, R.; Grant, Catherine E.; Bautz, Marshall W.; Heilmann, Ralf K.; Huenemoerder, D.; Miller, Eric D.; Nowak, Michael A.; Schattenburg, Mark L.; Schulz, Norbert S.; Burwitz, V.; Nandra, K.; Sanders, J. S.; Bookbinder, Jay A.; Petre, R.; Ptak, A.; Smale, A. P.; Burrows, D. N.; Poppenhaeger, Katja; Costantini, E.; DeRoo, Casey T.; McEntaffer, Randall L.; Mushotzky, R. F.; Miller, J. M.; Temi, P.

doi:10.1117/12.2231193

Cited by 7 publications

(12 citation statements)

References 72 publications

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“…For the O vii resonant line, we use values consistent with theirs: λ = 21.6019Å and f osc = 0.696, but ours come from a data compilation by Kaastra (2018). The other O vii He-like lines (forbidden and intercombination) have wavelengths sufficiently far from the resonant line (e.g., Bertone et al 2010a) that these should be clearly separated from each other at the resolutions achieved by instruments aboard Arcus (Smith et al 2016;Brenneman et al 2016), Athena (Lumb et al 2017Barret et al 2018), and Lynx (The Lynx Team 2018) (see Sections 3.2 and 4.1 for further discussion of the telescopes and instruments). Therefore, we only discuss the resonant line here, and note that for lines at the detection limits of these instruments, the lines are not blended.…”

Section: Spectra and Equivalent Widthsmentioning

confidence: 99%

“…Since gas clouds do not have constant densities and temperatures, it is possible that different absorption lines arise in different parts of the same clouds. Since in planned blind X-ray absorption surveys with Athena, Arcus, and Lynx, O vii and O viii are the main targets (Brenneman et al 2016;Lumb et al 2017;Smith et al 2016;The Lynx Team 2018), it is useful to investigate how closely the absorption system properties for these ions match. To do this, we compare temperature and density weighted by O vii and O viii along the same 6.25 cMpc sightlines.…”

Section: Correlation Between Absorber Propertiesmentioning

confidence: 99%

“…This will also enable us to test whether enforcing different lines to have identical redshifts would help reduce the systematic errors given the energy resolution expected for upcoming missions. (Brenneman et al 2016;Lumb et al 2017). For Lynx (The Lynx Team 2018), which would launch later if approved, the focus is on characterising this gas.…”

Section: Correlation Between Absorber Propertiesmentioning

confidence: 99%

“…The main way we expect to find the hot WHIM gas, is through absorption in e.g. quasar spectra (e.g., Brenneman et al 2016;Nicastro et al 2018;Kovács et al 2019). This is because this WHIM gas typically has low densities: since emission scales with the density squared and absorption with the density along the line of sight, this makes absorption more readily detectable than emission in most of the WHIM.…”

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confidence: 99%

“…One way to search for the missing baryons in absorption is by doing blind surveys, where observers look for absorbers in the lines of sight to suitable background sources. There are a number of upcoming and proposed X-ray telescopes for which there are plans to carry out such surveys, includ-ing Athena (Barret et al 2016), Arcus (Brenneman et al 2016;Smith et al 2016), and Lynx (The Lynx Team 2018). The O viii and especially O vii ions tend to be the focus of such plans, since oxygen is a relatively abundant element (Allende Prieto et al 2001) and these ions have lines with large oscillator strengths (Verner et al 1996), making these lines more readily detectable in the hot WHIM.…”

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confidence: 99%

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The abundance and physical properties of O vii and O viii X-ray absorption systems in the EAGLE simulations

Wijers

Schaye

Oppenheimer

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We use the EAGLE cosmological, hydrodynamical simulations to predict the column density and equivalent width distributions of intergalactic O vii (E = 574 eV) and O viii (E = 654 eV) absorbers at low redshift. These two ions are predicted to account for 40 % of the gas-phase oxygen, which implies that they are key tracers of cosmic metals. We find that their column density distributions evolve little at observable column densities from redshift 1 to 0, and that they are sensitive to AGN feedback, which strongly reduces the number of strong (column density N 10 16 cm −2 ) absorbers. The distributions have a break at N ∼ 10 16 cm −2 , corresponding to overdensities of ∼ 10 2 , likely caused by the transition from sheet/filament to halo gas. Absorption systems with N 10 16 cm −2 are dominated by collisionally ionized O vii and O viii, while the ionization state of oxygen at lower column densities is also influenced by photoionization. At these high column densities, O vii and O viii arising in the same structures probe systematically different gas temperatures, meaning their line ratio does not translate into a simple estimate of temperature. While O vii and O viii column densities and covering fractions correlate poorly with the H i column density at N H I 10 15 cm −2 , O vii and O viii column densities are higher in this regime than at the more common, lower H i column densities. The column densities of O vi and especially Ne viii, which have strong absorption lines in the UV, are good predictors of the strengths of O vii and O viii absorption and can hence aid in the detection of the X-ray lines.

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Section: Spectra and Equivalent Widthsmentioning

confidence: 99%

Section: Correlation Between Absorber Propertiesmentioning

confidence: 99%

Section: Correlation Between Absorber Propertiesmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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The abundance and physical properties of O vii and O viii X-ray absorption systems in the EAGLE simulations

Wijers

Schaye

Oppenheimer

et al. 2019

Monthly Notices of the Royal Astronomical Society

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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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