A High Spectral Resolution Study of the Soft X-Ray Background with the X-Ray Quantum Calorimeter

Wulf, Dallas; Eckart, Megan E.; Galeazzi, M.; Jaeckel, Felix T.; Kelley, R. L.; Kilbourne, Caroline A.; Morgan, Kelsey M.; McCammon, D.; Porter, F. S.; Szymkowiak, Andrew E.

doi:10.3847/1538-4357/ab41f8

Cited by 19 publications

(20 citation statements)

References 49 publications

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“…Then, they were used as initial values while performing simultaneous fitting of source and RASS spectra. It was seen that the CXB parameter values are highly consistent with the studies of Kuntz & Snowden (2000); Snowden et al (2008); Wulf et al (2019).…”

Section: Epic Backgroundsupporting

confidence: 80%

The Relative Supernovae Contribution to the Chemical Enrichment History of Abell 1837

Erdim,

Ezer,

Ünver

et al. 2021

Preprint

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In this paper, we report the relative SNe contributions on the metal budget of the ICM of Abell 1837 galaxy cluster at redshift z = 0.069. For this purpose, we analysed the hot ICM of the cluster and obtained radial metal distributions by using XMM-Newton archival data with total exposure ∼100 ks. These metal measurements consist of Mg, Si, S, Fe and Ni within 0.7 R 500 radius which is divided into three concentric annuli. In order to explain the observed metal abundance pattern in terms of relative supernova contributions, we used our newly developed code SNeRatio which utilizes theoretical nucleosynthesis models. This study covers the most recent 3D SNIa and SNcc yield tables. All combinations of these theoretical yields were fitted with our measured abundance ratios and statistically acceptable ones were selected. Each of these models were found to predict a uniform SNIa percentage contribution to the total SNe from the cluster center to the outskirts and form an SNIa ratio distribution with a mean 39 ± 14%. This uniformity is consistent with the early enrichment scenario which assumes that the metal production processes begin in early phase of cluster formation, namely proto-cluster phase at epoch z ≥ 2.

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Section: Epic Backgroundsupporting

confidence: 80%

The Relative Supernovae Contribution to the Chemical Enrichment History of Abell 1837

Erdim,

Ezer,

Ünver

et al. 2021

Preprint

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“…The experimental setup is shown in Figure 1 and described elsewhere (Defay et al 2013;Fogle et al 2014;Seely et al 2017). X-ray spectra following CX were recorded by a high-resolution X-ray quantum microcalorimeter (XQC) from the University of Wisconsin and Goddard Space Flight Center (McCammon et al 2008;Wulf et al 2019).…”

Section: Methodsmentioning

confidence: 99%

Target and Velocity Dependence of Charge Exchange X-Ray Emission at Solar Wind Velocities

Zhang

Seely

Andrianarijaona

et al. 2022

ApJ

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Laboratory measurements of X-ray emissions following charge exchange (CX) between highly charged ions and neutrals are important to assess their diagnostic utility for the nonequilibrium astrophysical plasma environments, where hot flows meet cold gases. With a high-resolution X-ray quantum microcalorimeter detector, we report the CX-induced X-ray spectra and line ratios in Ne8+ on He and Kr collisions at solar wind velocities of 392, 554, 678, and 876 km s−1, respectively. The experimentally determined line ratios quantify the differences in CX state selectivity and the following X-ray emission between He and Kr at different collision velocities. This suggests that target and velocity dependence should be considered for accurately modeling astrophysical CX plasmas.

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“…It extends out to distances that range from 9 to 20 pc (Frisch et al 2011 ;Gry & Jenkins 2014). This cloud in turn is surrounded by a cavity that contains a hot medium (HIM) that is collisionally ionized and emits soft X-rays with emission line ratios consistent with a temperature T = 1.1 × 10 6 K (Sanders et al 2001 ;Wulf et al 2019). This cavity, called the Local Bubble, extends out to a distance of order 100 pc from us (McCammon & Sanders 1990 ;Snowden et al 1997 ;Snowden et al 1998 ;Vergely et al 2010 ;Welsh et al 2010b ;Lallement et al 2013 ;Galeazzi et al 2014 ;Snowden et al 2014 ;Uprety et al 2016 ;Liu et al 2017).…”

Section: Examining An Interfacementioning

confidence: 99%

In Search of an Interface between Warm and Hot Gas within the Local Bubble

Jenkins

Gry

2020

ApJ

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We have examined UV spectra recorded by the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope for three stars, HD32309, 41 Ari, and η Tel, that are located well inside the boundary of the Local Hot Bubble in our search for absorption features of Si IV, C IV, and N V that could reveal the presence of an interface between the local warm (T ∼ 7000 K) neutral medium and a more distant hot (T ∼ 10 6 K) interstellar medium. In all cases, we failed to detect such ions. Our most meaningful upper limit is that for log N (C IV)< 11.86 toward HD32309, which is below the expectation for a sight line that penetrates either a conductive/evaporative interface or a turbulent mixing layer. We offer conjectures on the reasons for these negative results in terms of either a suppression of a conductive layer caused by the shielding of the local cloud by other clouds, which may make it more difficult for us to sense discrete absorption features from gases at intermediate temperatures, or by the presence of a tangential magnetic field at most locations on the surface of the local cloud.

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A High Spectral Resolution Study of the Soft X-Ray Background with the X-Ray Quantum Calorimeter

Cited by 19 publications

References 49 publications

The Relative Supernovae Contribution to the Chemical Enrichment History of Abell 1837

The Relative Supernovae Contribution to the Chemical Enrichment History of Abell 1837

Target and Velocity Dependence of Charge Exchange X-Ray Emission at Solar Wind Velocities

In Search of an Interface between Warm and Hot Gas within the Local Bubble

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