AAS 204th Meeting, June 2004
Session 43 Galaxy Surveys and Galaxy Clusters
Poster, Tuesday, June 1, 2004, 10:00am-7:00pm, Ballroom

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[43.15] Chandra results from the Boötes 9 square degree Field

A.T. Kenter, W.R. Forman, P.J. Green, D. Fabricant, G. Fazio, C. Jones, S.S. Murray, A. Vikhlinin (Harvard Smithsonian Center for Astrophysics), M Rieke (University of Arizona), K. Brand, M. Brown, A. Dey, B.T. Jannuzi, J. Najita (National Optical Astronomy Observatory (NOAO)), B.R. McNamara, J.C. Shields ( Ohio University), C.S. Kochanek, C.R. Watson (The Ohio State University)

We present X-ray results from Chandra observations of the Boötes 9 square degree survey field. This field corresponds to the northern half of the National Optical Astronomy Observatory (NOAO) Deep Wide-Field Survey (NDWFS).

The Chandra observations of the Boötes field consist of 126 separate contiguous ACIS-~I observations each of approximately 5 ~ksec in duration. The observations are arranged in a mosaic with a total field of view of ~ 9.3 square degrees. This unique set of observations allows us to measure X-ray source statistics, and to search for large scale structure over a wide, contiguous field of view with unprecedented angular resolution and uniform coverage.

In our full band (0.5-7~keV) sample we detect ~3000 point and ~40 extended sources. Limiting the point source list to sources with \ge 4 counts, and assuming a simple AGN-type power law spectrum, these observations reach a flux of ~4 \times 10-15~ergs~cm-2~s-1 in the 0.5-2~keV band, ~2 \times 10-14~ergs~cm-2~s-1 in the 2-10~keV band and ~8 \times 10-15~ergs~cm-2~s-1 in the 5-10~keV band.

We examine the distribution of these X-ray sources for evidence of large scale structure as made manifest in two point angular correlation and counts in cells. We present the number of sources per flux density interval (N(S)). We discuss our analysis techniques and the related Monte Carlo simulations.

Funding for this research was provided in part by NASA contracts NAS8-38248, NAS8-01130,NAS8-39073 and GO grant GO3-4176A. Funding for this research was also provided by the National Optical Astronomy Observatory, which is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation.

The author(s) of this abstract have provided an email address for comments about the abstract: akenter@cfa.harvard.edu

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