We assess the possibility of detecting the warm-hot intergalactic medium in emission and characterizing its physical conditions and spatial distribution through spatially resolved X-ray spectroscopy, in the framework of the recently proposed DIOS, EDGE, Xenia, and ORIGIN missions, all of which are equipped with microcalorimeter-based detectors. For this purpose, we analyze a large set of mock emission spectra, extracted from a cosmological hydrodynamical simulation. These mock X-ray spectra are searched for emission features showing both the OVII K alpha triplet and OVIII Ly alpha line, which constitute a typical signature of the warm-hot gas. Our analysis shows that 1Ms long exposures and energy resolution of 2.5 eV will allow us to detect about 400 such features per deg(2) with a significance >= 5 sigma and reveals that these emission systems are typically associated with density similar to 100 above the mean. The temperature can be estimated from the line ratio with a precision of similar to 20%. The combined effect of contamination from other lines, variation in the level of the continuum, and degradation of the energy resolution reduces these estimates. Yet, with an energy resolution of 7 eV and all these effects taken into account, one still expects about 160 detections per deg(2). These line systems are sufficient for tracing the spatial distribution of the line-emitting gas, which constitute an additional information, independent from line statistics, to constrain the poorly known cosmic chemical enrichment history and the stellar feedback processes.

Takei, Y., Ursino, E., Branchini, E.F., Ohashi, T., Kawahara, H., Mitsuda, K., et al. (2011). STUDYING THE WARM-HOT INTERGALACTIC MEDIUM IN EMISSION. THE ASTROPHYSICAL JOURNAL, 734(2) [10.1088/0004-637X/734/2/91].

STUDYING THE WARM-HOT INTERGALACTIC MEDIUM IN EMISSION

BRANCHINI, ENZO FRANCO;
2011-01-01

Abstract

We assess the possibility of detecting the warm-hot intergalactic medium in emission and characterizing its physical conditions and spatial distribution through spatially resolved X-ray spectroscopy, in the framework of the recently proposed DIOS, EDGE, Xenia, and ORIGIN missions, all of which are equipped with microcalorimeter-based detectors. For this purpose, we analyze a large set of mock emission spectra, extracted from a cosmological hydrodynamical simulation. These mock X-ray spectra are searched for emission features showing both the OVII K alpha triplet and OVIII Ly alpha line, which constitute a typical signature of the warm-hot gas. Our analysis shows that 1Ms long exposures and energy resolution of 2.5 eV will allow us to detect about 400 such features per deg(2) with a significance >= 5 sigma and reveals that these emission systems are typically associated with density similar to 100 above the mean. The temperature can be estimated from the line ratio with a precision of similar to 20%. The combined effect of contamination from other lines, variation in the level of the continuum, and degradation of the energy resolution reduces these estimates. Yet, with an energy resolution of 7 eV and all these effects taken into account, one still expects about 160 detections per deg(2). These line systems are sufficient for tracing the spatial distribution of the line-emitting gas, which constitute an additional information, independent from line statistics, to constrain the poorly known cosmic chemical enrichment history and the stellar feedback processes.
Takei, Y., Ursino, E., Branchini, E.F., Ohashi, T., Kawahara, H., Mitsuda, K., et al. (2011). STUDYING THE WARM-HOT INTERGALACTIC MEDIUM IN EMISSION. THE ASTROPHYSICAL JOURNAL, 734(2) [10.1088/0004-637X/734/2/91].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11590/122004
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