Sunyaev–Zeldovich fluctuations from the first stars?
Identifieur interne : 000372 ( Main/Exploration ); précédent : 000371; suivant : 000373Sunyaev–Zeldovich fluctuations from the first stars?
Auteurs : S. Peng Oh ; Asantha Cooray [États-Unis] ; Marc Kamionkowski [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2003-06.
English descriptors
Abstract
WMAP's detection of high electron‐scattering optical depth τe suggests substantial star formation at high redshift z∼ 17 ± 5. On the other hand, the recovered σ8∼ 0.84 ± 0.04 argues against a cluster Sunyaev–Zeldovich (SZ) origin for the observed small‐scale cosmic microwave background (CMB) fluctuation excess, which generally requires σ8∼ 1.1. Here we consider the effects of high‐redshift star formation on the CMB. We derive a fairly model‐independent relation between τe and the number of ionizing photons emitted per baryon Nγ, and use this to calibrate the amount of high‐redshift supernova activity. The resulting supernova remnants Compton cool against the CMB creating a Compton y distortion y∼ few × 10−6 within observational bounds. However they also create small‐scale SZ fluctuations, which could be comparable with SZ fluctuations from unresolved galaxy clusters. This raises the exciting possibility that we have already detected signatures of the first stars not just once, but twice, in the CMB.
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DOI: 10.1046/j.1365-8711.2003.06708.x
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On the other hand, the recovered σ8∼ 0.84 ± 0.04 argues against a cluster Sunyaev–Zeldovich (SZ) origin for the observed small‐scale cosmic microwave background (CMB) fluctuation excess, which generally requires σ8∼ 1.1. Here we consider the effects of high‐redshift star formation on the CMB. We derive a fairly model‐independent relation between τe and the number of ionizing photons emitted per baryon Nγ, and use this to calibrate the amount of high‐redshift supernova activity. The resulting supernova remnants Compton cool against the CMB creating a Compton y distortion y∼ few × 10−6 within observational bounds. However they also create small‐scale SZ fluctuations, which could be comparable with SZ fluctuations from unresolved galaxy clusters. This raises the exciting possibility that we have already detected signatures of the first stars not just once, but twice, in the CMB.</div></front></TEI><affiliations><list><country><li>États-Unis</li></country></list><tree><noCountry><name sortKey="Peng Oh, S" sort="Peng Oh, S" uniqKey="Peng Oh S" first="S." last="Peng Oh">S. Peng Oh</name></noCountry><country name="États-Unis"><noRegion><name sortKey="Cooray, Asantha" sort="Cooray, Asantha" uniqKey="Cooray A" first="Asantha" last="Cooray">Asantha Cooray</name></noRegion><name sortKey="Kamionkowski, Marc" sort="Kamionkowski, Marc" uniqKey="Kamionkowski M" first="Marc" last="Kamionkowski">Marc Kamionkowski</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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