PI: Jill Bechtold, University of Arizona, email@example.com
Address: Astronomy Department, Steward Observatory, 933 N. Cherry Avenue, Tucson, Arizona 85721, USA
CoI: Buell Jannuzi, NOAO
Title: The IGM and the Distribution of Galaxies at \bf z~1
Abstract: We propose to carry out a deep, wide-field galaxy survey towards the bright, intermediate-redshift quasar PG 1634+706 (V=14.9, z_em=1.334). We have obtained a high signal-to-noise echelle spectrum of PG 1634+706 with HST/STIS, in order to study the Ly(alpha) forest and metal absorbers in detail. Our deep galaxy survey will cover a region of ~ 9\times9 Mpc centered on the quasar sight line, with roughly 360 galaxy redshifts expected with z=0.5 - 1.3. With this galaxy sample we will (1) identify the galaxies giving rise to several complex CIV/MgII/OVI absorption line systems at z=0.3- 1.0; (2) map the large scale galaxy distribution so that we can look for correlations between galaxy cluster structures and the clusters of weak Lyman forest clouds we see in the UV spectrum; (3) test predictions of hydrodynamic simulations of LSS growth, and the physics of galaxy feedback; and (4) determine whether the observed correlation between the density of the IGM and the density of galaxies on ~10 Mpc scales claimed recently at z~3 persists to lower redshift. PG 1634+706 is one of 4 intermediate redshift quasars we have observed with the STIS echelle, and its spectrum has by far the highest signal-to-noise ratio. The STIS data are the first comprehensive survey of quasar absorbers at echelle resolution for redshifts z=0.5-2. Our survey bridges the gap between the z=2-6 absorbers observed from the ground, and the z<0.3 low redshift systems previously studied with HST and FUSE. The redshift range z=0.5-2 is of great interest, since it marks the peak of star-formation and quasar activity, and is the time during which galaxies formed into the mature Hubble sequence we see today. \bf WE CAN ALSO DO THIS PROJECT WITH 2.5 NIGHTS OF GMOS GEMINI-N TIME.
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