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1. Atomic data calculations for Au i –Au iii and exploration in the application of collisional-radiative theory to laboratory and neutron star merger plasmas

   https://doi.org/10.1093/mnras/stab3285  

   McCann, Michael; Bromley, S; Loch, S D; Ballance, C P (December 2021, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT Neutron binary star mergers have long been proposed as sufficiently neutron rich environments that could support the synthesis of rapid neutron capture elements (r-process elements) such as gold. However, the literature reveals that beyond neutral and singly ionized systems, there is an incompleteness of atomic data for the remaining ion stages of importance for mergers. In this work, we report on relativistic atomic structure calculations for Au i–Au iii using the grasp0 codes. Comparisons to calculations using the Flexible Atomic Code suggest uncertainties on average of 9.2 per cent, 5.7 per cent, and 3.8 per cent for Au i–Au iii level energies. Agreement around ∼50 per cent is achieved between our computed A-values and those in the literature, where available. Using the grasp0 structure of Au i, we calculated electron-impact excitation rate coefficients and use a collisional-radiative model to explore the excitation dynamics and line ratio diagnostics possible in neutron star merger environments. We find that proper accounting of metastable populations is critical for extracting useful information from ultraviolet–visible line ratio diagnostics of Au i. As a test of our data, we applied our electron-impact data to study a gold hollow cathode spectrum in the literature and diagnosed the plasma conditions as Te = 3.1 ± 1.2 eV and $$n_\textrm {e} = 2.7^{+1.3}_{-0.9}\times 10^{13}$$ cm−3. 

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2. The Interstellar Heritage of Comets

   https://doi.org/10.3847/1538-3881/ae0cae  

   Willacy, Karen; Majumdar, Liton; Bonev, Boncho; Gibb, Erika; Dello_Russo, Neil; DiSanti, Michael; Vervack, Ronald J; Roth, Nathan X (November 2025, The Astronomical Journal)

   Abstract Comets have similar compositions to interstellar medium ices, suggesting at least some of their molecules may be inherited from an earlier stage of evolution. To investigate the degree to which this might have occurred, we compare the composition of individual comets to that of the well-studied protostellar region IRAS 16293–2422B. We show that the observed molecular abundance ratios in several comets correlate well with those observed in the protostellar source. However, this does not necessarily mean that the cometary abundances are identical to protostellar. We find the abundance ratios of many molecules present in comets are enhanced compared to their protostellar counterparts. For COH molecules, the data suggest higher abundances relative to methanol of more complex species, e.g., HCOOH, CH₃CHO, and HCOOCH₃, are found in comets. For N-bearing molecules, the ratios of nitriles relative to CH₃CN—HC₃N/CH₃CN and HCN/CH₃CN—tend to be enhanced. The abundances of cometary SO and SO₂relative to H₂S are enhanced, whereas OCS/H₂S is reduced. Using a subset of comets with a common set of observed molecules, we suggest a possible means of determining the relative degree to which they retain interstellar ices. This analysis suggests that over 84% of COH-bearing molecules can be explained by the protostellar composition. The possible fraction inherited from the protostellar region is lower for nitrogen molecules, at only 26%–74%. While this is still speculative, especially since few comets have large numbers of observed molecules, it provides a possible route for determining the relative degree to which comets contain disk-processed material. 

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3. Deep transfer learning for star cluster classification: I. application to the PHANGS–HST survey

   https://doi.org/10.1093/mnras/staa325  

   Wei, Wei; Huerta, E A; Whitmore, Bradley C; Lee, Janice C; Hannon, Stephen; Chandar, Rupali; Dale, Daniel A; Larson, Kirsten L; Thilker, David A; Ubeda, Leonardo; et al (April 2020, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT We present the results of a proof-of-concept experiment that demonstrates that deep learning can successfully be used for production-scale classification of compact star clusters detected in Hubble Space Telescope(HST) ultraviolet-optical imaging of nearby spiral galaxies ($$D\lesssim 20\, \textrm{Mpc}$$) in the Physics at High Angular Resolution in Nearby GalaxieS (PHANGS)–HST survey. Given the relatively small nature of existing, human-labelled star cluster samples, we transfer the knowledge of state-of-the-art neural network models for real-object recognition to classify star clusters candidates into four morphological classes. We perform a series of experiments to determine the dependence of classification performance on neural network architecture (ResNet18 and VGG19-BN), training data sets curated by either a single expert or three astronomers, and the size of the images used for training. We find that the overall classification accuracies are not significantly affected by these choices. The networks are used to classify star cluster candidates in the PHANGS–HST galaxy NGC 1559, which was not included in the training samples. The resulting prediction accuracies are 70 per cent, 40 per cent, 40–50 per cent, and 50–70 per cent for class 1, 2, 3 star clusters, and class 4 non-clusters, respectively. This performance is competitive with consistency achieved in previously published human and automated quantitative classification of star cluster candidate samples (70–80 per cent, 40–50 per cent, 40–50 per cent, and 60–70 per cent). The methods introduced herein lay the foundations to automate classification for star clusters at scale, and exhibit the need to prepare a standardized data set of human-labelled star cluster classifications, agreed upon by a full range of experts in the field, to further improve the performance of the networks introduced in this study. 

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4. Resolved low- J 12CO excitation at 190 parsec resolution across NGC 2903 and NGC 3627

   https://doi.org/10.1093/mnras/stad3091  

   den Brok, J S; Leroy, A K; Usero, A; Schinnerer, E; Rosolowsky, E; Koch, E W; Querejeta, M; Liu, D; Bigiel, F; Barnes, A T; et al (October 2023, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT The low-J rotational transitions of 12CO are commonly used to trace the distribution of molecular gas in galaxies. Their ratios are sensitive to excitation and physical conditions in the molecular gas. Spatially resolved studies of CO ratios are still sparse and affected by flux calibration uncertainties, especially since most do not have high angular resolution or do not have short-spacing information and hence miss any diffuse emission. We compare the low-J CO ratios across the disc of two massive, star-forming spiral galaxies NGC 2903 and NGC 3627 to investigate whether and how local environments drive excitation variations at GMC scales. We use Atacama Large Millimeter Array (ALMA) observations of the three lowest-J CO transitions at a common angular resolution of 4 arcsec (190 pc). We measure median line ratios of $$R_{21}=0.67^{+0.13}_{-0.11}$$, $$R_{32}=0.33^{+0.09}_{-0.08}$$, and $$R_{31}=0.24^{+0.10}_{-0.09}$$ across the full disc of NGC 3627. We see clear CO line ratio variation across the galaxy consistent with changes in temperature and density of the molecular gas. In particular, towards the centre, R21, R32, and R31 increase by 35  per cent, 50  per cent, and 66  per cent, respectively, compared to their average disc values. The overall line ratio trends suggest that CO(3–2) is more sensitive to changes in the excitation conditions than the two lower J transitions. Furthermore, we find a similar radial R32 trend in NGC 2903, albeit a larger disc-wide average of $$\langle R_{32}\rangle =0.47^{+0.14}_{-0.08}$$. We conclude that the CO low-J line ratios vary across environments in such a way that they can trace changes in the molecular gas conditions, with the main driver being changes in temperature. 

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5. Stars made in outflows may populate the stellar halo of the Milky Way

   https://doi.org/10.1093/mnras/staa522  

   Yu, Sijie; Bullock, James S; Wetzel, Andrew; Sanderson, Robyn E; Graus, Andrew S; Boylan-Kolchin, Michael; Nierenberg, Anna M; Grudić, Michael Y; Hopkins, Philip F; Kereš, Dušan; et al (May 2020, Monthly Notices of the Royal Astronomical Society)

   ABSTRACT We study stellar-halo formation using six Milky-Way-mass galaxies in FIRE-2 cosmological zoom simulations. We find that $$5{-}40{{\ \rm per\ cent}}$$ of the outer (50–300 kpc) stellar halo in each system consists of in-situ stars that were born in outflows from the main galaxy. Outflow stars originate from gas accelerated by superbubble winds, which can be compressed, cool, and form co-moving stars. The majority of these stars remain bound to the halo and fall back with orbital properties similar to the rest of the stellar halo at z = 0. In the outer halo, outflow stars are more spatially homogeneous, metal-rich, and alpha-element-enhanced than the accreted stellar halo. At the solar location, up to $$\sim \!10 {{\ \rm per\ cent}}$$ of our kinematically identified halo stars were born in outflows; the fraction rises to as high as $$\sim \!40{{\ \rm per\ cent}}$$ for the most metal-rich local halo stars ([Fe/H] >−0.5). Such stars can be retrograde and create features similar to the recently discovered Milky Way ‘Splash’ in phase space. We conclude that the Milky Way stellar halo could contain local counterparts to stars that are observed to form in molecular outflows in distant galaxies. Searches for such a population may provide a new, near-field approach to constraining feedback and outflow physics. A stellar halo contribution from outflows is a phase-reversal of the classic halo formation scenario of Eggen, Lynden-Bell & Sandange, who suggested that halo stars formed in rapidly infalling gas clouds. Stellar outflows may be observable in direct imaging of external galaxies and could provide a source for metal-rich, extreme-velocity stars in the Milky Way. 

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