Dust and Gas from AGB Stars

Criscienzo, M. Di; Ventura, P.; Dell’Agli, F.

doi:10.7566/jpscp.31.011061

Cited by 1 publication

(1 citation statement)

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“…Gas that is only enriched by Pop III nucleosynthesis will have a unique chemical signature that will be erased as the galaxy evolves to Pop II (Ji et al 2015), most notably when stars with masses < 3.5 M enter the asymptotic giant branch (AGB) phase and yield large amounts of carbon. The calculations of DB17 hence assumed a silicate-rich dust composition (e.g., Ji et al 2014;Marassi et al 2015) produced by the type II supernovae that dominate the dust production in Pop III stellar systems (Di Criscienzo et al 2014). The type II supernovae are also likely to be a significant source of dust in very young galaxies that evolve from Pop III (e.g., Asano et al 2011;Ji et al 2015).…”

Section: Dust Compositionmentioning

confidence: 99%

The Far-infrared Emission of the First Massive Galaxies

Rossi¹,

Rieke²,

Shivaei³

et al. 2018

ApJ

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Massive Population II galaxies undergoing the first phase of vigorous star formation after the initial Population III stage should have high energy densities and silicate-rich interstellar dust. We have modeled the resulting far-infrared spectral energy distributions (SEDs), demonstrating that they are shifted substantially to bluer ("warmer") wavelengths relative to the best fitting ones at z ≈ 3, and with strong outputs in the 10 − 40µm range. When combined with a low level of emission by carbon dust, their SEDs match that of Haro 11, a local moderately-low-metallicity galaxy undergoing a very young and vigorous starburst that is likely to approximate the relevant conditions in young Population II galaxies. We expect to see similar SEDs at high redshifts (z 5) given the youth of galaxies at this epoch. In fact, we find a progression with redshift in observed galaxy SEDs, from those resembling local ones at 2 z < 4 to a closer resemblance with Haro 11 at 5 z < 7. In addition to the insight on conditions in high redshift galaxies, this result implies that estimates of the total infrared luminosities at z ∼ 6 based on measurements near λ ∼ 1 mm can vary by factors of 2 − 4, depending on the SED template used. Currently popular modified blackbodies or local templates can result in significant underestimates compared with the preferred template based on the SED of Haro 11.

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