High Spectral Resolution Observations of the Soft X-ray Diffuse Background with Thermal Detectors

By D. McCammon, R. Almy, E. Apodaca, W. Bergmann, S. Deiker, M. Galeazzi, A. Lesser, W. Sanders, E. Figueroa, R. Kelley and 3 more. 2000

312 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/107a1d46a7e21f9719bdec5583b4fb02872d01ac

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Citations in the corpus

CONSTRAINING THE MILKY WAY'S HOT GAS HALO WITH O vii AND O viii EMISSION LINES (2014, methodology): “Bregman & Lloyd-Davies (2007) compared the aggregate column densities of 26 high S/N local O VII absorbers with a single emission measure estimate for the Milky Way’s hot halo (McCammon et al. 2002).”
X-RAY SPECTRAL PROPERTIES OF THE BAT AGN SAMPLE (2008, background): “We do not include blackbody components since the < kT >≈ 0.1 keV components have very little spectral effects at E > 0.6 keV, the energy above which the CXB is well measured (McCammon et al. 2002).”
X-rays from solar system objects (2007, background): “The brightness merges with the soft X-ray background emission (McCammon and Sanders, 1990; McCammon et al., 2002) at distances of 104 km for weakly outgassing comets, and can be as large as 106 km for the most productive and luminous (Dennerl et al., 1997; Fig.”
The Suzaku High Resolution X-Ray Spectrometer (2007, background): “This payload, the X-Ray Quantum Calorimeter (XQC), has been flown several times and has produced the first celestial x-ray spectrum with a microcalorimeter (McCammon et al. 2002).”
THE STRUCTURE OF THE MILKY WAY'S HOT GAS HALO (2013, methodology): “McCammon et al. (2002) analyzed a 1 sr region of sky at l = 90◦, b = +60◦ using a quantum calorimeter sounding rocket.”
Semiconductor Probes of Light Dark Matter (2012, methodology): “The parameter space for larger masses (> 1 GeV) is also probed by the direct detection experiments XQC [45, 46], CRESST [47], CDMS [48], and XENON10 [49].”
The Search for the Missing Baryons at Low Redshift (2007, background): “…approaches require that their models not exceed the observed diffuse X-ray background emission, they do not make use of the emission, for which a single high resolution spectrum was obtained with a quantum microcalorimeter toward l,b = 90◦, 60◦ and with a 1 sr field of view (McCammon et al., 2002).”
XMM-Newton Observation of Solar Wind Charge Exchange Emission (2004, background): “…emission from the lower halo, an absorbed hotter thermal component with T ∼ 0.6 keV representing Milky Way halo or local group emission (e.g., McCammon et al. (2002)), and an absorbed power law with a spectral index of 1.46 representing the unresolved emission of AGN and other…”
Sterile neutrinos in cosmology (2017, background): “The XQC sounding rocket flight [230] is very sensitive to the presence of a line due to its large field of view and microcalorimeter-based high energy resolution [226].”
A HUGE RESERVOIR OF IONIZED GAS AROUND THE MILKY WAY: ACCOUNTING FOR THE MISSING MASS? (2012, background): “Other measurements of Galactic Halo emission (McCammon et al. 2002; Galeazzi et al. 2007; Gupta et al. 2009; Hagihara et al. 2010) also reported EM ∼ 0.003 cm−6 pc for solar metallicity, close to the average.”
A Catalog of Galaxy Clusters Observed by XMM-Newton (2007, background): “There is additional general diffuse emission at 34 keV which may be associated with the Galactic halo or perhaps the local group (McCammon et al. 2002; Kuntz, Snowden, & Mushotzky 2001).”
Energy spectra of the soft X-ray diffuse emission in fourteen fields observed with Suzaku (2009, background): “The extragalactic contribution, which we refer to as the Cosmic X-ray Background (CXB) in this paper, is estimated to be about 40 % of emission in the so-called ROSAT R45 band (McCammon et al. 2002), which is approximately ∼ 0.44− 1 keV.”
High-Resolution X-Ray Spectroscopic Constraints on Cooling-Flow Models for Clusters of Galaxies (2002, background): “We believe this is due to errors in the effective area calibration, imperfect background modeling, and spatially broadened ( 3 Å) emission lines of O viii, O vii, N vii, and C vi emission lines from the diffuse soft X-ray background (see McCammon et al. 2002).”
The Interstellar Medium Surrounding the Sun (2011, background): “A deficit in the expected emission from the Fe line complex at ∼72 eV was an early sign of trouble for the model, indicating either that the standard emission model was inadequate or that Fe is depleted by a factor of 3–7 in the hot gas (Bloch, Priedhorsky & Smith 1990; McCammon et al. 2002).”