Fossil H ii regions: self-limiting star formation at high redshift
Identifieur interne : 000355 ( Main/Exploration ); précédent : 000354; suivant : 000356Fossil H ii regions: self-limiting star formation at high redshift
Auteurs : S. Peng Oh [États-Unis] ; Zoltán Haiman [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2003-12-01.
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Abstract
Recent results from the Wilkinson Microwave Anisotropy Probe (WMAP) satellite suggest that the intergalactic medium (IGM) was significantly reionized at redshifts as high as z∼ 17. At this early epoch, the first ionizing sources probably appeared in the shallow potential wells of mini-haloes with virial temperatures Tvir < 104 K. Once such an ionizing source turns off, its surrounding H ii region Compton cools and recombines. None the less, we show that the ‘fossil’ H ii regions left behind remain at high adiabats, prohibiting gas accretion and cooling in subsequent generations of mini-haloes. This greatly amplifies feedback effects explored in previous studies, and early star formation is self-limiting. We quantify this effect to show that star formation in mini-haloes cannot account for the bulk of the electron scattering opacity measured by WMAP, which must be due to more massive objects. We argue that gas entropy, rather than IGM metallicity, regulates the evolution of the global ionizing emissivity and impedes full reionization until lower redshifts. We discuss several important consequences of this early entropy floor for reionization. It reduces gas clumping, curtailing the required photon budget for reionization. An entropy floor also prevents H2 formation and cooling, due to reduced gas densities: it greatly enhances feedback from ultraviolet photodissociation of H2. An early X-ray background would also furnish an entropy floor to the entire IGM; thus, X-rays impede rather than enhance H2 formation. Future 21-cm observations may probe the topology of fossil H ii regions.
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DOI: 10.1046/j.1365-2966.2003.07103.x
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Peng Oh</name><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Theoretical Astrophysics, Mail Code 130-33, Caltech, Pasadena, CA 91125</wicri:regionArea><wicri:noRegion>CA 91125</wicri:noRegion></affiliation><affiliation wicri:level="1"><country wicri:rule="url">États-Unis</country></affiliation></author><author><name sortKey="Haiman, Zoltan" sort="Haiman, Zoltan" uniqKey="Haiman Z" first="Zoltán" last="Haiman">Zoltán Haiman</name><affiliation wicri:level="4"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027</wicri:regionArea><orgName type="university">Université Columbia</orgName><placeName><settlement type="city">New York</settlement><region type="state">État de New York</region></placeName></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbrev">Mon. 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At this early epoch, the first ionizing sources probably appeared in the shallow potential wells of mini-haloes with virial temperatures Tvir < 104 K. Once such an ionizing source turns off, its surrounding H ii region Compton cools and recombines. None the less, we show that the ‘fossil’ H ii regions left behind remain at high adiabats, prohibiting gas accretion and cooling in subsequent generations of mini-haloes. This greatly amplifies feedback effects explored in previous studies, and early star formation is self-limiting. We quantify this effect to show that star formation in mini-haloes cannot account for the bulk of the electron scattering opacity measured by WMAP, which must be due to more massive objects. We argue that gas entropy, rather than IGM metallicity, regulates the evolution of the global ionizing emissivity and impedes full reionization until lower redshifts. We discuss several important consequences of this early entropy floor for reionization. It reduces gas clumping, curtailing the required photon budget for reionization. An entropy floor also prevents H2 formation and cooling, due to reduced gas densities: it greatly enhances feedback from ultraviolet photodissociation of H2. An early X-ray background would also furnish an entropy floor to the entire IGM; thus, X-rays impede rather than enhance H2 formation. Future 21-cm observations may probe the topology of fossil H ii regions.</div></front></TEI><affiliations><list><country><li>États-Unis</li></country><region><li>État de New York</li></region><settlement><li>New York</li></settlement><orgName><li>Université Columbia</li></orgName></list><tree><country name="États-Unis"><noRegion><name sortKey="Oh, S Peng" sort="Oh, S Peng" uniqKey="Oh S" first="S. Peng" last="Oh">S. Peng Oh</name></noRegion><name sortKey="Haiman, Zoltan" sort="Haiman, Zoltan" uniqKey="Haiman Z" first="Zoltán" last="Haiman">Zoltán Haiman</name><name sortKey="Oh, S Peng" sort="Oh, S Peng" uniqKey="Oh S" first="S. Peng" last="Oh">S. Peng Oh</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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