Background X-ray Emission from Hot Gas in CDM and CDM+Lambda Universes: Spectral Signatures

Details Background X-ray Emission from Hot Gas in CDM and CDM+Lambda Universes: Spectral Signatures Background X-ray Emission from Hot Gas in CDM and CDM+Lambda Universes: Spectral Signatures

1995-06-07

arxiv.org/abs/astro-ph/9506050v1

Astrophys.J. 451 (1995) 436

Astronomy and Astrophysics

Astrophysics

Princeton University Observatory, in ApJ press, figs can be ftp'ed from ftp://astro.princeton.edu/cen/XRAY/

Scientific paper

10.1086/176232

We present a new treatment of two popular models for the growth of structure, examining the X-ray emission from hot gas with allowance for spectral line emission from various atomic species, primarily ``metals". The X-ray emission from the bright cluster sources is not significantly changed from prior work and, as noted earlier, shows the CDM$+\Lambda$ model (LCDM) to be consistent but the standard, COBE normalized model (SCDM) to be inconsistent with existing observations --- after allowance for still the considerable numerical modelling uncertainties. But we find one important new result. Radiation in the softer band 0.5-1.0keV is predominantly emitted by gas far from cluster centers (hence ``background"). This background emission dominates over the cluster emission below 1keV and observations of it should show clear spectral signatures indicating its origin. In particular the ``iron blend" should be seen prominantly in this spectral bin from cosmic background hot gas at high galactic latitudes and should show shadowing against the SMC indicating its extragalactic origin. Certain OVII lines also provide a signature of this gas which emits a spectrum characteristic of $10^{6.6\pm 0.6}$K gas. Recent ASCA observations of the X-ray background tentatively indicate the presence of component with exactly the spectral features we predict here.

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