First Stars and the Near Infrared Background

Details First Stars and the Near Infrared Background First Stars and the Near Infrared Background

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..332..268s&link_type=abstract

The Fate of the Most Massive Stars, ASP Conference Series, Vol. 332, Proceedings of the conference held 23-28 May, 2004 in Grand

Astronomy and Astrophysics

Astronomy

Scientific paper

The redshifted light of the first (Pop III) stars might substantially contribute to the near infrared background (NIRB). By fitting recent data (Matsumoto et al. 2000) with models including up-to-date Pop III stellar spectra, we find that such stars can indeed account for the whole NIRB residual (i.e. after `normal' galaxy contribution subtraction) if the high redshift star formation efficiency is f*=10%-50%, depending on the IMF (the top-heaviest requiring lowest efficiency). Such epoch of Pop III star formation ends in all models by zend≈ 8.8, with a hard limit zend < 9 set by J band observations. The fit to the NIRB data is shown in the Figure (left plot) with the solid line. All details about this calculation can be found in Salvaterra & Ferrara (2003). Moreover, we find that the clustering of Pop III stars can account also for the ˜1-30 arcsec scales fluctuation in the J band measured by Kashlinsky et al (2002). In Figure (right plot) are shown the power spectrum due to Pop III stars (dashed line) and to normal HDF galaxies (dotted line).
All details about this calculation can be found in Magliocchetti, Salvaterra, & Ferrara (2003).
In conclusion, we find that Pop III stars can account for the observed unexplained excess in the NIRB, both the total intensity and the small angular-scale fluctuation, if first stars are very massive (M>100 M&sun;) and their formation ends at z≃ 8.8.

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