On the Possibility of Observing H 2 Emission from Primordial Molecular Cloud Kernels

Content Provider	Semantic Scholar
Author	Kamaya, Hideyuki Silk, Joseph I.
Copyright Year	2001
Abstract	We study the prospects for observing H2 emission during the assembly of primordial molecular cloud kernels. The primordial molecular cloud cores, which resemble those at the present epoch, can emerge around 1 + z = 20 according to recent numerical simulations. The kernels form inside the cores, and the first stars will appear inside the kernels. A kernel typically contracts to form one of the first generation stars with an accretion rate that is as large as ∼ 0.01M year−1. This occurs due to the primordial abundances that result in a kernel temperature of order 1000K, and the collapsing kernel emits H2 line radiation at a rate ∼ 10 erg sec−1. Principally J = 5− 3 (v=0) rotational emission of H2 is expected. At redshift 1 + z = 20, the expected flux is ∼ 0.01 μJy for a single kernel. While an individual object is not observable by any facilities available in the near future, the expected assembly of primordial star clusters on sub-galactic scales can result in fluxes at the sub-mJy level. This is marginally observable with ASTRO-F. We also examine the rotational J = 2 − 0 (v=0) and vibrational δv = 1 emission lines. The former may possibly be detectable with ALMA.
File Format	PDF HTM / HTML
Alternate Webpage(s)	http://arxiv.org/pdf/astro-ph/0104480v1.pdf
Alternate Webpage(s)	http://cds.cern.ch/record/497726/files/0104480.pdf
Language	English
Access Restriction	Open
Subject Keyword	Contract agreement Deuterium GUCY2C protein, human H2 Database Engine Kernel (operating system) Large Numerical analysis Observable One Thousand RLN2 gene Redshift Simulation Stars, Celestial Telescopes wavelength
Content Type	Text
Resource Type	Article