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Erik Zackrisson Uppsala University, Sweden Christian Binggeli, Kristian Finlator, Nick Gnedin, Akio K. Inoue, Hannes Jensen, Genoveva Micheva, Jan-‐Pieter Paardekooper, Ikkoh Shimizu Punchline Zackrisson et al. 2013, ApJ, 777, 39 What caused cosmic reionization? CMBR Studies of the intergalactic medium (e.g. Lyα, CMBR) can reveal when reionization happened, but where did the ionizing Reionization photons come from? (z ≈ 6-‐14) Star-‐forming galaxies at z > 6 are the prime suspects, but how do we Today prove that they did it? Requirements for galaxy-‐ dominated reionization 1. Lots of star-‐forming galaxies at 2. Escape of ionizing photons redshifts z > 6 (Lyman continuum) from galaxies into the IGM LyC Hubble XDF LyC leakage – direct detections Borthakhur et al. 14 Serious problem: At z > 4-‐5, the IGM opacity prevents direct detection of escaping Lyman continuum (Inoue & Iwata 2008, Inoue+14) Indirect signatures of LyC leakage These features can be studied with JWST/NIRSpec @ z ≈ 6-‐9 Zackrisson, Inoue & Jensen 2013, ApJ, 777, 39 How does this work? Young stars Lyman continuum photons from young stars captured by gas → Nebular emission If some of the LyC photons escape without ionzing the ISM → Less nebular emission! Stellar and nebular SEDs Rest-‐frame galaxy spectrum Lyman continuum Nebular continuum and emission lines Stellar continuum •  Pop I, II, III stars + EMP stars •  Nebular emission (Cloudy) + dust •  Rest-‐frame SEDs (far-‐UV to near-‐IR) •  HST/Spitzer/JWST ﬂuxes @ z=0-‐15 Model grids available at: www.astro.uu.se/~ez Zackrisson et al. 2011, ApJ, 740, 13 Simple diagnostics: UV slope & Hβ JWST can study Lyman continuum leakage without measuring the Lyman continuum ﬂux! z = 7 Zackrisson, Inoue & Jensen 2013, ApJ, 777, 39

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Indirect signatures of LyC leakage. Zackrisson, Inoue & Jensen 2013, ApJ, 777, 39. These features can be studied with JWST/NIRSpec @ z ≈ 6-‐9

Constraining the Escape of Ionizing Photons from Galaxies at z>6 PDF

22 Pages·2015·13.41 MB·English

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Indirect signatures of LyC leakage. Zackrisson, Inoue & Jensen 2013, ApJ, 777, 39. These features can be studied with JWST/NIRSpec @ z ≈ 6-‐9

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