An XMM pre-view of the cosmic network: galaxy groups and filaments

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dc.creatorPierre, M.
dc.creatorBryan, G.
dc.creatorGastaud, R.
dc.date1999-10-25
dc.date1999-11-29
dc.date.accessioned2026-07-07T02:34:02Z
dc.date.available2026-07-07T02:34:02Z
dc.descriptionA large fraction of the baryons today are predicted to be in hot, filamentary gas, which has yet to be detected. In this paper, we use numerical simulations of dark matter and gas to determine if these filaments and groups of galaxy will be observable be XMM. The simulated maps include free-free and line emission, galactic absorption, the XMM response function, photon noise, the extragalactic source distribution, and vignetting. A number of cosmological models are examined as well as a range of very simple prescriptions to account for the effect of supernovae feedback (preheating). We show that XMM has a good chance of observing emission from strong filaments at z~0.1. This becomes much more difficult by z~0.5. The primary difficulties lie in detecting such a large, diffuse object and in selecting an appropriate field. We also describe the range of group sizes that XMM should be sensitive to (both for detection and spectral analysis), although this is more dependent on the unknown nature of the feedback. Such observations will greatly improve our understanding of feedback and should also provide stronger cosmological constraints.
dc.descriptionSubmitted to A&A, 16 pages, 13 figures; (low resolution gif images on astro-ph; high resolution version available at http://www.mit.edu/~gbryan/xmm_preview.html) Added missing figure numbers in text
dc.identifierhttps://arxiv.org/abs/astro-ph/9910446
dc.identifierhttp://arxiv.org/abs/astro-ph/9910446
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/15085
dc.subjectAstrophysics
dc.titleAn XMM pre-view of the cosmic network: galaxy groups and filaments
dc.typetext

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