The Many Faces of Galaxy Clusters: Mock Observations of Cluster Populations in Multiple Wavelengths

Details The Many Faces of Galaxy Clusters: Mock Observations of Cluster Populations in Multiple Wavelengths The Many Faces of Galaxy Clusters: Mock Observations of Cluster Populations in Multiple Wavelengths

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.2105n&link_type=abstract

American Astronomical Society, AAS Meeting #212, #21.05; Bulletin of the American Astronomical Society, Vol. 40, p.219

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Logic

Scientific paper

Clusters of Galaxies trace the cosmic mass density field and thus have have potential as sensitive probes of the universe's energy content, including Dark Energy. To form a complete and unbiased perspective of these buoys, observations must occur at several wavelengths, including the X-ray, optical, and radio bands. Within the next decade, projects like the Dark Energy Survey will detect 50,000 clusters through optical observations of their galaxies. In an overlapping region of the sky, the South Pole Telescope will provide measurements of arcminute CMB anomalies, revealing the hot gas of clusters (via the Sunyaev Zeldovich effect). Independent observations of clusters--from the light of galaxies and from the scattering effect of hot gas--will allow us to address selection effects and completeness in cluster samples, as well as the definition and categorization of clusters.
These efforts promise a holistic view of galaxy cluster populations; however, to properly "weigh the universe," we must precisely match observable features with masses, which are provided by the underlying dark matter halo. N-body cosmological simulations of dark matter and realistic baryonic components (e.g., hydrodynamics, AGN, star formation, etc.) offer rich, state-of-the-art venues for mock observations of cluster populations. We use re-simulations of the Millennium Run that include gas physics and pre-heating to create lightcones and then mock surveys, incorporating selection effects and survey limitations. With these mock skies, we may help to calibrate upcoming surveys (like DES and SPT), as well as to draw robust links between observable cluster properties and the underlying mass. Here, we present the recent work in construction and analysis of these mock, multi-wavelength cluster surveys.

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