The Orion OB Association as a Generator for the Hot Circumgalactic Medium

Fuller, C.; Kaaret, Philip; Bluem, J.; Küntz, K. D.; Hodges-Kluck, Edmund; Jahoda, K.

doi:10.3847/1538-4357/acaafc

Cited by 3 publications

(2 citation statements)

References 51 publications

(94 reference statements)

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“…Beginning with the sight line of the blazar 1ES 1553+113, this component was revealed in the MW's CGM, both in absorption and emission (Das et al 2019a(Das et al , 2019b). This has been followed by detections in emission over more sight lines spread across the sky (Gupta et al 2022;Bluem et al 2022;Fuller et al 2023). As the evidence in favor of the hot component mounts, it is imperative to understand its elemental makeup, spatial distribution, and its relationship with the other components of the CGM.…”

Section: Introductionmentioning

confidence: 92%

“…The super-virial phase of the MW CGM is newly discovered, and we do not yet know its location within the galaxy or its origin. The presence of this component (Das et al 2019a;Gupta et al 2022) around the Galactic Bubbles (Predehl et al 2020;Su et al 2010) and the Orion-Eridanus Superbubble (Fuller et al 2023) has been tied to relics of outflows that caused these structures, e.g., historic AGN (Zhang & Figure 7. Top: Temperature measurements from all the fields for the supervirial gas plotted against that of the virial gas.…”

Section: Location Of the Super-virial Phasementioning

confidence: 99%

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The Hot Circumgalactic Medium of the Milky Way: New Insights from XMM-Newton Observations

Bhattacharyya

Das

Gupta

et al. 2023

ApJ

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We present XMM-Newton observations around the sight line of Mrk 421. The emission spectrum of the Milky Way (MW) circumgalactic medium (CGM) shows that a two-phase model is a better fit to the data compared to a single-phase model; in addition to the warm-hot virial phase at log (T/K) = 6.30 ± 0.02, a hot super-virial phase at log (T/K) = 6.88 − 0.06 + 0.07 is required. Furthermore, we present observations of five fields within 5 degrees of the primary field. Their spectra also require a two-phase model at warm-hot and hot temperatures. The hot phase, which was first discovered in Das et al. in 2019, appears to be widespread. By chemical tagging, we show that the emission from the supevirial phase comes from the L-shell transitions of Fe xviii–Fe xxii, and that the range of temperatures probed in emission is distinct from that in absorption. We detect scatter in temperature and emission measure in both the phases, and deduce that there is small-scale density inhomogeneity in the MW CGM. The emitting gas likely has higher density, possibly from regions close to the disk of the MW, while the absorption in the virial phase may arise from low-density gas extended out to the virial radius of the MW. The presence of the super-virial phase far from the regions around the Galactic center implicates physical processes unrelated to the activity at the Galactic center. Hot outflows resulting from star formation activity throughout the Galactic disk are likely to be responsible for producing this phase.

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Section: Introductionmentioning

confidence: 92%

Section: Location Of the Super-virial Phasementioning

confidence: 99%

The Hot Circumgalactic Medium of the Milky Way: New Insights from XMM-Newton Observations

Bhattacharyya

Das

Gupta

et al. 2023

ApJ

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Revisiting the abundance pattern and charge-exchange emission in the centre of M 82

Fukushima,

Kobayashi,

Matsushita

2024

A&A

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The interstellar medium (ISM) in starburst galaxies contains many chemical elements that are synthesised by core-collapse supernova explosions. By measuring the abundances of these metals, we can study the chemical enrichment within the galaxies and the transportation of metals into the circumgalactic environment through powerful outflows. We performed a spectral analysis of the X-ray emissions from the core of M82 using the Reflection Grating Spectrometer (RGS) on board XMM-Newton to accurately estimate the metal abundances in the ISM. We analysed over 300\,ks of RGS data observed with 14 position angles, covering a cross-dispersion width of 80\,arcsec. We employed multi-temperature thermal plasma components in collisional ionisation equilibrium (CIE) to reproduce the observed spectra, each of which exhibited a different spatial broadening. The O VII band CCD image shows a broader distribution that those for the O VIII and Fe-L bands. The O VIII line profiles have a prominent double-peaked structure that corresponds to the north- and southward outflows. The O VII triplet feature exhibits marginal peaks. A single CIE component that is convolved with the O VII band image approximately reproduces the spectral shape. A CIE model combined with a charge-exchange emission model also successfully reproduces the O VII line profiles. However, the ratio of these two components varies significantly with the observed position angles, which is physically implausible. Spectral fitting of the broadband spectra suggests a multi-temperature phase in the ISM that is approximated by three components at 0.1, 0.4, and 0.7\,keV. Notably, the 0.1\,keV component exhibits a broader distribution than the 0.4 and 0.7\,keV plasmas. The derived abundance pattern shows super-solar N/O, solar Ne/O and Mg/O, and half-solar Fe/O ratios. These results indicate the chemical enrichment by core-collapse supernovae in starburst galaxies.

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The soft X-ray background with Suzaku. II. Supervirial temperature bubbles?

Sugiyama,

Ueda,

Fukushima

et al. 2023

Publications of the Astronomical Society of Japan

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Observations of the hot X-ray emitting interstellar medium in the Milky Way are important for studying the stellar feedback and for understanding the formation and evolution of galaxies. We present measurements of the soft X-ray background emission for 130 Suzaku observations at 75° < l < 285° and |b| > 15°. With the standard soft X-ray background model consisting of the local hot bubble and of the Milky Way halo, residual structures remain at 0.7–1 keV in the spectra of some regions. Adding a collisional-ionization-equilibrium component with a temperature of ∼0.8 keV, much higher than the virial temperature of the Milky Way, significantly reduces the derived C-statistic for 56 out of 130 observations. The emission measure of the 0.8 keV component varies by more than an order of magnitude: assuming the solar abundance, the median value is $3 \times 10^{-4}\, \rm {cm^{-6}\ pc}$ and the 16th–84th percentile range is $(1\!-\!8) \times 10^{-4}\, \rm {cm^{-6}\ pc}$. Regions toward the Orion–Eridanus superbubble, having a large cavity extending from the Ori OB1 association, have the highest emission measures of the 0.8 keV component. While the scatter is large, the emission measures tend to be higher toward lower galactic latitudes. We discuss possible biases caused by the solar wind charge exchange, stars, and background groups. The 0.8 keV component is probably heated by supernovae in the Milky Way disk, possibly related to Galactic fountains.

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The Orion OB Association as a Generator for the Hot Circumgalactic Medium

Cited by 3 publications

References 51 publications

The Hot Circumgalactic Medium of the Milky Way: New Insights from XMM-Newton Observations

The Hot Circumgalactic Medium of the Milky Way: New Insights from XMM-Newton Observations

Revisiting the abundance pattern and charge-exchange emission in the centre of M 82

The soft X-ray background with Suzaku. II. Supervirial temperature bubbles?

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