paper

X-ray Absorption by the Low-redshift Intergalactic Medium: A Numerical Study of the Lambda CDM model

arXiv:astro-ph/0203319 · doi:10.1086/376751

Abstract

Using a hydrodynamic simulation of a LCDM universe, we investigate the "X-ray forest" absorption imprinted on the spectra of background quasars by the intervening intergalactic medium (IGM). In agreement with previous studies, we find that OVII and OVIII produce the strongest absorption features. The strong oxygen absorbers that might be detectable with Chandra or XMM-Newton arise in gas with T ~ 10^6 K and overdensities delta >~ 100 that are characteristic of galaxy groups. Future X-ray missions could detect weaker oxygen absorption produced by gas with a wider range of temperatures and the lower densities of unvirialized structures; they could also detect X-ray forest absorption by C, N, Ne, Fe, and possibly Si. If the IGM metallicity is 0.1 solar, then the predicted number of systems strong enough for a ~5σdetection with Chandra or XMM-Newton is extremely low, though scatter in metallicity would increase the number of strong absorbers even if the mean metallicity remained the same. Our simulation reproduces the high observed incidence of OVI absorbers (in the UV), and the most promising strategy for finding the X-ray forest is to search at the redshifts of known OVI systems, thus reducing the signal-to-noise threshold required for a significant detection. However, while many OVI absorbers have associated OVII or OVIII absorption, the OVI systems trace only the low temperature phases of the X-ray forest, and a full accounting of the strong OVII and OVIII systems will require a mission with the anticipated capabilities of Constellation-X. The large effective area of the XEUS satellite would make it an extremely powerful instrument for studying the IGM, measuring X-ray forest absorption by a variety of elements and revealing the shock-heated filaments that may be an important reservoir of cosmic baryons.

41 pages including 16 figures, replaced with version accepted by ApJ. Includes clarification of several points and brief discussion of recent observational results

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