Submitted Key Science Questions
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An accurate census of Compton-thick AGN at z>2 from the 14/24um NeV lines (Duncan Farrah).
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A definitive answer to the origin of dust at low redshift: supernovae and/or AGB stars? (Duncan Farrah)
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Are galactic winds responsible for shutting down SF at z < 2 in LIRGs? Is this feedback primarily AGN or SB driven? (L. Armus)
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Do planetary systems form around every star? Why or why not? (H. Yorke)
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Image protoplanetary disks and measure the distributions of H2, HD, water vapor and ice, and dust to learn how the conditions for habitability arise during the planet formation process. (D. Leisawitz)
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Image structures in a large number of debris disks to find and characterize exoplanets through their interactions with the disks. (D. Leisawitz)
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Mid-infrared spectral diagnostics of star formation and AGN activity in main-sequence galaxies out to z=5 (Duncan Farrah).
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Molecular hydrogen lines as diagnostics of the formation of the first stars at z>>6 (Duncan Farrah).
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The clustering of IR-faint AGN & starbursts on spatial scales ranging from voids/filaments to intrahalo, at 1<z<6. Redshift-space distortions, bias cf to passively evolving systems, etc (Duncan Farrah).
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The faint end of the far-IR luminosity function up to z~6. Hierarchical modes of galaxy assembly, contribution from faint galaxies to the CIB, etc (Duncan Farrah).
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The pre-stellar core mass function across the Local Group. Does the stellar IMF vary significantly, depend on environment, etc? (Duncan Farrah)
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The radial dust distribution around nearby stars at 100-300K as diagnostics of Earth-like planet formation in the habitable zone (Duncan Farrah).
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Understand the formation, merger history, and star formation history of galaxies, and the role of AGN in galaxy evolution. (D. Leisawitz)
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Warm-gas water lines as diagnostics of early-stage planetary formation - terrestrial oceans, snow lines, etc. Also, OH and far-infrared fine structure lines as a diagnostic of cooling and gas infall (Duncan Farrah).
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What are the size distributions of outer solar system object populations down to ~10km scales and out to distances ~ 50AU or greater? (J. Bauer)
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What is the prevalence of water in protoplanetary disks? (D. Benford)
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Why is star formation so much more efficient at z~1-4 .. is the chemistry in the ISM different? (A. Pope)
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