Formation and Signatures of the First Stars and Quasars

Details Formation and Signatures of the First Stars and Quasars Formation and Signatures of the First Stars and Quasars

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.6209h&link_type=abstract

American Astronomical Society, 192nd AAS Meeting, #62.09; Bulletin of the American Astronomical Society, Vol. 30, p.907

Astronomy and Astrophysics

Astronomy

Scientific paper

We will discuss various observable signatures of the first generation of stars and low-luminosity quasars, including the metal enrichment, radiation background, and dust opacity and emission they produce. To estimate the history of formation of dark-matter halos, we use an extension of the Press-Schechter formalism, incorporating the effects of pressure and molecular hydrogen dissociation. We then use the observed C/H ratio at z=3 in the Lyman-alpha forest clouds, to obtain an average the star formation efficiency in these halos. Similarly, we adjust the efficiency of black-hole formation, and the shape of quasar light curves to match the quasar luminosity function between redshifts z=2-4, to obtain the luminosity function of faint quasars at high redshifts. We find that in a Cold Dark Matter models, either stars or quasars are expected to reionize the intergalactic medium at redshifts z=10-20. The corresponding damping of CMB anisotropies on small angular scales is 10-20%, detectable by future satellites such as MAP and the Planck Surveyor. We also find that the Next Generation Space Telescope will be able to directly image about 1-100 star clusters per square arcmin from redshifts above z=10, and a comparable number of faint quasars. However, we show that the lack of faint point sources in the Hubble Deep Field places a mild constraint on the models. The amount of dust produced by the first supernovae have an optical depth of 0.1-1 towards high redshift sources, and the reprocessed UV flux of stars and quasars distorts the CMB by a y-paramater comparable to the COBE limit, y=1.5e-5.

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