PROBING THE PRE-REIONIZATION EPOCH WITH MOLECULAR HYDROGEN INTENSITY MAPPING
- Department of Physics and Astronomy, University of California, Irvine, CA 92697 (United States)
- CENTRA, Instituto Superior Tecnico, Technical University of Lisbon, Lisboa 1049-001 (Portugal)
Molecular hydrogen is now understood to be the main coolant of the primordial gas clouds leading to the formation of the very first stars and galaxies. The line emissions associated with molecular hydrogen should then be a good tracer of the matter distribution at the onset of the reionization of the universe. Here, we propose intensity mapping of H{sub 2} line emission in rest-frame mid-infrared wavelengths to map out the spatial distribution of gas at redshifts z > 10. We calculate the expected mean intensity and clustering power spectrum for several H{sub 2} lines. We find that the 0-0S(3) rotational line at a rest wavelength of 9.66 {mu}m is the brightest line over the redshift range of 10-30 with an intensity of about 5-10 Jy sr{sup -1} at z {approx} 15. To reduce astrophysical and instrumental systematics, we propose the cross-correlation between multiple lines of the H{sub 2} rotational and vibrational line emission spectrum. Our estimates of the intensity can be used as guidance in planning instruments for future mid-IR spectroscopy missions such as SPICA.
- OSTI ID:
- 22126743
- Journal Information:
- Astrophysical Journal, Vol. 768, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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