Lyman-Werner escape fractions from the first galaxies
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1 Lyman-Werner escape fractions from the first galaxies Schauer+17, ArXiv (MNRAS accepted) Anna T. P. Schauer with Ralf Klessen, Simon Glover, Dan Whalen and Muhammad Latif, Bhaskar Agarwal, Lluis Mas-Ribas, Claes-Erik Rydberg, Erik Zackrisson 17 th of February 2017 Köln STARLIGHT!
2 First galaxies and first stars - the gas composition is completely primordial - cooling has to proceed via H2 (and HD) - the mass of the first stars is very uncertain z =
3 Lyman-Werner radiation - UV photons with energy: ev ( Å) - photodissociation of H2 - regulation of star formation - H2 shielded by H2 and H Which fraction of Lyman-Werner photons can escape from the first galaxies?
4 Simulations + Post-process radiation source Code: - ZEUS-MP (Whalen & Norman 2006) - 1D, spherical symmetry - primordial chemistry network LW escape? halo LW escape fractions: - self-shielding by H2 and by H Parameter Space: - 2 First Galaxies (10 7 &10 8 M ) - 5 SEDs (instantaneous starburst) - 4 SFEs of 0.1% - 5.0% (Wolcott-Green & Haiman 2010) - near-field and far-field regimes (Schauer+ 2015) (Latif & Volonteri 2015)
5 Case study of I-front behavior 1. I-front outbreak: - I-front overruns halo - all H2 is photodissociated in HII region - LW escape fraction of > 90% 2. returning I-front: - spectrum softens after some time - halo re-combines outside-in - LW escape fraction drops to zero shortly after re-combination 3. slowly moving I-front: - I-front moves slowly - LW escape fraction depends on microphysics
6 1. I-front outbreak Salpeter IMF M with 1.0% SFE in 4x10 8 M halo
7 1. I-front outbreak Salpeter IMF M with 1.0% SFE in 4x10 8 M halo
8 1. I-front outbreak Salpeter IMF M with 1.0% SFE in 4x10 8 M halo
9 1. I-front outbreak Salpeter IMF M with 1.0% SFE in 4x10 8 M halo
10 1. I-front outbreak Salpeter IMF M with 1.0% SFE in 4x10 8 M halo
11 1. I-front outbreak Salpeter IMF M with 1.0% SFE in 4x10 8 M halo
12 1. I-front outbreak Salpeter IMF M with 1.0% SFE in 4x10 8 M halo
13 Case study of I-front behavior 1. I-front outbreak: - I-front overruns halo - all H2 is photodissociated in HII region - LW escape fraction of > 90% 2. returning I-front: - spectrum softens after some time - halo re-combines outside-in - LW escape fraction drops to zero shortly after re-combination 3. slowly moving I-front: - I-front moves slowly - LW escape fraction depends on microphysics
14 Case study of I-front behavior 1. I-front outbreak: - I-front overruns halo - all H2 is photodissociated in HII region - LW escape fraction of > 90% 2. returning I-front: - spectrum softens after some time - halo re-combines outside-in - LW escape fraction drops to zero shortly after re-combination 3. slowly moving I-front: - I-front moves slowly - LW escape fraction depends on microphysics
15 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
16 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
17 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
18 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
19 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
20 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
21 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
22 2. Returning I-front Flat IMF M with 1.0% SFE in 4x10 8 M halo
23 Case study of I-front behavior 1. I-front outbreak: - I-front overruns halo - all H2 is photodissociated in HII region - LW escape fraction of > 90% 2. returning I-front: - spectrum softens after some time - halo re-combines outside-in - LW escape fraction drops to zero shortly after re-combination fesc,lw = trecomb ttotal 3. slowly moving I-front: - I-front moves slowly - LW escape fraction depends on microphysics trecomb ttotal
24 Case study of I-front behavior 1. I-front outbreak: - I-front overruns halo - all H2 is photodissociated in HII region - LW escape fraction of > 90% 2. returning I-front: - spectrum softens after some time - halo re-combines outside-in - LW escape fraction drops to zero shortly after re-combination 3. slowly moving I-front: - I-front moves slowly - LW escape fraction depends on microphysics
25 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
26 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
27 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
28 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
29 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
30 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
31 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
32 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
33 3. Slowly moving I-front
34 3. Slowly moving I-front Salpeter IMF M with 0.1% SFE in 5.6x10 7 M halo
35 Case study of I-front behavior 1. I-front outbreak: - I-front overruns halo - all H2 is photodissociated in HII region - LW escape fraction of > 90% 2. returning I-front: - spectrum softens after some time - halo re-combines outside-in - LW escape fraction drops to zero shortly after re-combination 3. slowly moving I-front: - I-front moves slowly - LW escape fraction depends on microphysics
36 Conclusions Schauer+15, MNRAS 454, 2441 Schauer+ 17, ArXiv (MNRAS accepted) LW radiation influences the formation of the first stars by destroying the only coolant of the primordial gas, H2 LW escape fractions depend on the movement of the ionisation front through the halo: outbreaking ionisation front fesc,lw =100% after outbreak outside-in re-neutralisation of halo fesc,lw = trecomb ttotal slowly moving ionisation front dependent on microphysics
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