A Dramatic Decrease in Carbon Star Formation in M31

Boyer, Martha L.; Williams, Benjamin F.; Aringer, B.; Chen, Y.; Dalcanton, Julianne J.; Girardi, L.; Guhathakurta, Puragra; Marigo, Paola; Olsen, Knut; Rosenfield, Philip; Weisz, Daniel R.

doi:10.3847/1538-4357/ab24e2

Cited by 32 publications

(65 citation statements)

References 77 publications

(156 reference statements)

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“…We endeavoured to select yields and recipes that correspond to the current state-ofthe-art, but these prescriptions remain limited by our current knowledge on how grains are destroyed and whether or not grains can grow either in diffuse or dense clouds of the interstellar medium. If the true yields were to differ significantly from our model assumptions and/or show variations with metallicity (e.g., Valiante et al 2009;Boyer et al 2019; Dell'Agli et al 2019), this could impact our inferred model parameters. In De Vis in prep., the choice of metal yields is shown to mostly impact the metallicities of galaxies with high specific gas masses.…”

Section: Modelling Caveatsmentioning

confidence: 93%

JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

Looze

Lamperti

Saintonge

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT Scaling laws of dust, H i gas, and metal mass with stellar mass, specific star formation rate, and metallicity are crucial to our understanding of the build-up of galaxies through their enrichment with metals and dust. In this work, we analyse how the dust and metal content varies with specific gas mass (MH i/M⋆) across a diverse sample of 423 nearby galaxies. The observed trends are interpreted with a set of Dust and Element evolUtion modelS (DEUS) – including stellar dust production, grain growth, and dust destruction – within a Bayesian framework to enable a rigorous search of the multidimensional parameter space. We find that these scaling laws for galaxies with −1.0 ≲ log MH i/M⋆ ≲ 0 can be reproduced using closed-box models with high fractions (37–89 ${{\ \rm per\ cent}}$) of supernova dust surviving a reverse shock, relatively low grain growth efficiencies (ϵ = 30–40), and long dust lifetimes (1–2 Gyr). The models have present-day dust masses with similar contributions from stellar sources (50–80 ${{\ \rm per\ cent}}$) and grain growth (20–50 ${{\ \rm per\ cent}}$). Over the entire lifetime of these galaxies, the contribution from stardust (>90 ${{\ \rm per\ cent}}$) outweighs the fraction of dust grown in the interstellar medium (<10 ${{\ \rm per\ cent}}$). Our results provide an alternative for the chemical evolution models that require extremely low supernova dust production efficiencies and short grain growth time-scales to reproduce local scaling laws, and could help solving the conundrum on whether or not grains can grow efficiently in the interstellar medium.

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Section: Modelling Caveatsmentioning

confidence: 93%

JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

Looze

Lamperti

Saintonge

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Observations of s-process elements in AGB stars can be used to constrain for example the efficiency of third dredge-up mixing but selection biases in observations means that the whole stellar parameter space is not well sampled. Other observations including white dwarfs in clusters (Marigo et al 2020) or the number of carbon stars in a stellar population (Boyer et al 2019) provide additional constraints but are also subject to their own biases. The uncertainties on AGB yields are difficult to quantify for the following reasons.…”

Section: Uncertaintiesmentioning

confidence: 99%

The Origin of Elements from Carbon to Uranium

Kobayashi

Karakas

Lugaro

2020

ApJ

536

588

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To reach a deeper understanding of the origin of elements in the periodic table, we construct Galactic chemical evolution (GCE) models for all stable elements from C (A = 12) to U (A = 238) from first principles, i.e., using theoretical nucleosynthesis yields and event rates of all chemical enrichment sources. This enables us to predict the origin of elements as a function of time and environment. In the solar neighborhood, we find that stars with initial masses of M > 30M ⊙ can become failed supernovae if there is a significant contribution from hypernovae (HNe) at M ∼ 20–50M ⊙. The contribution to GCE from super-asymptotic giant branch (AGB) stars (with M ∼ 8–10M ⊙ at solar metallicity) is negligible, unless hybrid white dwarfs from low-mass super-AGB stars explode as so-called Type Iax supernovae, or high-mass super-AGB stars explode as electron-capture supernovae (ECSNe). Among neutron-capture elements, the observed abundances of the second (Ba) and third (Pb) peak elements are well reproduced with our updated yields of the slow neutron-capture process (s-process) from AGB stars. The first peak elements (Sr, Y, Zr) are sufficiently produced by ECSNe together with AGB stars. Neutron star mergers can produce rapid neutron-capture process (r-process) elements up to Th and U, but the timescales are too long to explain observations at low metallicities. The observed evolutionary trends, such as for Eu, can well be explained if ∼3% of 25–50M ⊙ HNe are magneto-rotational supernovae producing r-process elements. Along with the solar neighborhood, we also predict the evolutionary trends in the halo, bulge, and thick disk for future comparison with Galactic archeology surveys.

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“…Carbon stars appear over a limited range of the metallicityage plane. At approximately solar metallicity, carbon stars are expected to form from stars with initial masses that are about 1.5-5 M (Karakas & Lattanzio 2007;Marigo & Girardi 2007;Boyer et al 2013Boyer et al , 2019, and reach the thermal pulsing AGB phase in under 3 Gyr. In old populations, bright carbon stars are typically younger than their oxygen-rich counterparts which generally have lower initial masses (<1.5 M ) and start to thermally pulse much later.…”

Section: The Mid-ir Stellar Populations Of M32mentioning

confidence: 99%

Infrared variable stars in the compact elliptical galaxy M32

Jones

Nally

Sharp

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Variable stars in the compact elliptical galaxy M32 are identified, using three epochs of photometry from the Spitzer Space Telescope at 3.6 and 4.5 μm, separated by 32 to 381 days. We present a high-fidelity catalogue of sources detected in multiple epochs at both 3.6 and 4.5 μm, which we analysed for stellar variability using a joint probability error-weighted flux difference. Of these, 83 stars are identified as candidate large-amplitude, long-period variables, with 28 considered high-confidence variables. The majority of the variable stars are classified as asymptotic giant branch star candidates using colour-magnitude diagrams. We find no evidence supporting a younger, infrared-bright stellar population in our M32 field.

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A Dramatic Decrease in Carbon Star Formation in M31

Cited by 32 publications

References 77 publications

JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

The Origin of Elements from Carbon to Uranium

Infrared variable stars in the compact elliptical galaxy M32

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