First Light: Physics of Early Star Formation from the Local Universe

Details First Light: Physics of Early Star Formation from the Local Universe First Light: Physics of Early Star Formation from the Local Universe

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21932006p&link_type=abstract

American Astronomical Society, AAS Meeting #219, #320.06

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We present detailed theoretical spectra of the earliest star forming regions. Improving on the spherically symmetric shell with a single ionization potential and density, we form a nebular template using the recently derived 3-D structure and density of 30 Doradus. Using CLOUDY, we illuminate our complex cloud with an SED of metal free stars, and vary the elemental and dust abundances from Z=-1 to -6. We solve for the physical condition of the gas as radiation is absorbed and reprocessed across the many different H+/H0/H2 interfaces forming the entire nebula. We solve for abundance and ionization states of all elements, as well as the abundance of 100's of molecular species which form after the ionizing radiation has been absorbed. We produce globally average, rest-frame synthetic spectra from 10-3 to 106µm allowing us to create empirically motivated diagnostics of early enrichment and stellar feedback for JWST and ALMA. This includes broad continuum features AND the atomic and molecular emission from the entire complex. With the structural and feedback details revealed in these models, there exists an unprecedented opportunity to illustrate the most promising observational strategies for new observatories peering back to first light. Future efforts to observe and create more templates using nearby HII regions will expand the modeled parameter space. These templates will also serve as an alternative to the current sub-grid structure of HII regions in cosmological simulations.

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