Pith. sign in

REVIEW 2 major objections 6 minor 288 references

Atomic gas dominates six Local Group galaxies, and its depletion time rises to tens–hundreds of Gyr in the outer disks, indicating that star formation is throttled by the slow conversion of atomic to molecular gas.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 06:32 UTC pith:HFNM5N7N

load-bearing objection A careful, transparent data-release paper with real new products; the headline depletion-time trends are plausible but partly rest on SFR upper limits, so the strongest conclusions should be softened. the 2 major comments →

arxiv 2607.21841 v1 pith:HFNM5N7N submitted 2026-07-23 astro-ph.GA

A Multiwavelength Inventory for the Local Group L-band Survey I: Atlas and Radial Profiles of Local Group Galaxies

Cosima Eibensteiner , Adam K. Leroy , Jiayi Sun , Erik Roslowsky , Eric W. Koch , Nickolas Pingel , Chang-Goo Kim , Laura B. Chomiuk
show 16 more authors
Ryan Chown Alberto D. Bolatto Michael P. Busch Julianne J. Dalcanton Amanda A. Kepley Christina W. Lindberg Eve C. Ostriker J\"urgen Ott Sumit K. Sarbadhicary Adam Smercina Sne\v{z}ana Stanimirovi\'c Elizabeth Tarantino Vicente Villanueva Tobin M. Wainer Fabian Walter Thomas G. Williams
This is my paper
classification astro-ph.GA
keywords Local Group galaxiesatomic hydrogenstar formation depletion timeHI-to-H2 transitionradial profilesdwarf galaxiesgalaxy evolutioninterstellar medium
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper combines 120-pc-resolution HI maps from the Local Group L-Band Survey with uniformly processed infrared, ultraviolet, Hα, and CO data to build the first coherent multiwavelength inventory of six nearby galaxies: M31, M33, IC 10, IC 1613, NGC 6822, and WLM. It establishes that atomic gas is the most extended baryonic component, often flatter than the stellar and star-formation profiles, and that outside the stellar effective radius the atomic-gas depletion time always exceeds 10 Gyr. The authors argue that, across this whole sample, the balance between atomic and molecular gas — not the efficiency of star formation within molecular clouds — is the factor that regulates where and how fast stars form. If correct, this refocuses galaxy evolution models on the HI-to-H2 transition as the key bottleneck, and it provides a benchmark dataset for studying that transition at physical scales below 100 pc.

Core claim

The paper's central claim is that in the six actively star-forming Local Group galaxies targeted by LGLBS, atomic hydrogen makes up most of the interstellar medium and, in the outer regions, exceeds the stellar mass. Azimuthally averaged HI surface-density profiles are flat or slowly declining compared to the steeper falloff of stellar mass and star-formation rate, with outer HI scale lengths of 1–8.5 kpc. Atomic and total gas depletion times increase with galactocentric radius, rising from roughly 0.8–17 Gyr inside the stellar half-mass radius to tens–hundreds of Gyr in the outer disks, while molecular depletion times remain shorter and roughly constant where CO data exist. Outside the stel

What carries the argument

The central object is the azimuthally averaged radial profile, computed at 120 pc resolution for gas, stars, and star-formation tracers, along with the mass-weighted mean atomic gas surface density ⟨Σ_120pc_atom⟩ and the associated clumping factor c_HI. The key derived quantity is the gas depletion time τ_dep = Σ_gas / Σ_SFR (the inverse of the star-formation efficiency per unit gas), which the paper tracks as a function of radius. These tools convert raw multiwavelength maps into a direct measurement of where and why star formation becomes inefficient, showing that the atomic-to-molecular gas balance, not the molecular depletion time, sets the pace of star formation.

Load-bearing premise

In all targets except M31, the star-formation tracers (UV, IR, Hα) are not sensitive enough to detect the outer-disk star formation, so many radial rings yield only upper limits; if the true outer-disk SFR is systematically higher than these limits, the reported long depletion times would be overestimated and the central conclusion weakens.

What would settle it

Deeper ultraviolet or Hα observations that push star-formation detection into the outer HI disks of IC 10, IC 1613, NGC 6822, WLM, or M33 — or dust-based molecular gas maps that could reveal CO-dark H2 — would directly test whether τ_atom_dep really exceeds 10 Gyr outside the stellar effective radius.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • In all six galaxies, atomic gas dominates the ISM and exceeds stellar mass in the outer regions, so models of disk-galaxy evolution must treat the HI reservoir as the primary fuel reservoir.
  • Atomic and total gas depletion times rise exponentially with radius in every target, implying a continuous, non-threshold transition to inefficient star formation in outer disks.
  • Outside the stellar effective radius, τ_atom_dep is always > 10 Gyr, meaning the majority of the atomic gas by area is currently forming stars far too slowly to consume itself within a Hubble time.
  • The clumping factor shows that dwarf galaxies are highly porous (shells and cavities) while M31 and M33 are smoother, linking the ISM structure on 120 pc scales to the efficiency of forming molecular clouds.
  • The public release of calibrated HI, CO, IR, UV, Hα, stellar-mass, and SFR maps provides a foundation for high-resolution studies of the HI-to-H2 transition in the nearest galaxies.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the HI-to-H2 transition is the universal bottleneck, then cosmological simulations that adopt a fixed star-formation efficiency per unit gas will overproduce stars in the outer disks of low-mass galaxies; this prediction is testable by comparing simulated and observed radial SFR profiles.
  • The absence of a sharp threshold in the depletion-time rise suggests that local pressure or column density, rather than a single critical value, controls where molecular gas forms; stacking HI spectra with higher resolution could map the transition directly.
  • A direct extension would be to measure the CO-dark molecular gas fraction in these outer disks using dust-based mass estimates, which would test whether the long atomic depletion times are truly due to inefficient HI-to-H2 conversion or partly to a missed molecular reservoir.
  • The observed correlation between clumping factor and slow star formation implies that feedback-generated holes may self-regulate the HI-to-H2 conversion; this could be tested by comparing cold-HI fraction (from absorption) with local depletion time on 120 pc scales.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 6 minor

Summary. This paper combines 120 pc-resolution VLA+GBT HI data from the first LGLBS data release with uniformly processed GALEX UV, WISE IR, Hα, and CO maps to construct radial profiles of atomic gas, molecular gas, stellar mass, and star formation rate surface density for six Local Group galaxies: M31, M33, IC 10, IC 1613, NGC 6822, and WLM. From these profiles the authors measure disk scale lengths, effective radii, gas clumping factors, integrated masses, SFRs, and atomic/molecular/total gas depletion times. The central claims are that atomic gas dominates the ISM over the whole sample, that atomic and total gas depletion times increase with galactocentric radius, and that outside the stellar effective radius the atomic-gas depletion time always exceeds 10 Gyr. The paper also releases the processed images, profiles, and region measurements as a public data product.

Significance. If the conclusions hold, this is a valuable reference dataset and analysis for the nearest HI-resolved galaxies. The 120 pc resolution of the HI data is a clear step forward for studying the HI-to-H2 transition and star formation inefficiency in HI-dominated systems. The uniform multi-wavelength processing and public data release are significant community contributions. The central HI and stellar mass measurements are independent of the depletion-time assumptions and are robust. However, the headline radial trend of increasing depletion times rests heavily on the treatment of SFR upper limits in outer disks; unless those are handled with censored-data methods or explicitly labeled as lower limits, the quantitative conclusions go beyond what the data support.

major comments (2)
  1. [Section 2, Table 4, Conclusions 2-3] Section 2 states that 'in all targets except M31, the sensitivity of the SFR tracers becomes a limiting factor in the outer disks... so that many rings yield only upper limits.' Yet the depletion-time panels and Table 4 quote numerical τ values (e.g., IC 1613 τ_gas_dep(r>r50,*)=49.85 Gyr; WLM τ_gas_dep=16.44 Gyr) without marking them as lower limits. Since SFR sensitivity per annulus improves outward while Σ_HI declines only slowly, the ratio Σ_HI/SFR_UL can rise with radius even for a constant true SFR. Therefore the claimed 'increase with radius' and 'always >10 Gyr' trends are not established for the censored rings unless survival analysis/stacking is applied or the values are explicitly labeled as lower limits and fits restricted to detections. This is load-bearing for Conclusions 2 and 3.
  2. [Appendix A.4, Conclusion 1] For IC 1613, NGC 6822, and WLM, the 'expected' molecular gas profiles (and hence the statement that Σ_atom > Σ_mol in every ring) are computed by assuming a single τ_mol_dep per galaxy, derived by extrapolating the Sun et al. (2025) τ_mol_dep–M* relation from M* ≈ 10^9.5–10^11 M⊙ down to M* ≈ 10^7.5–10^8.8 M⊙. This extrapolation is uncalibrated and the resulting M_mol values in Table 5 are not independent measurements. The conclusion that atomic gas dominates over molecular gas in these dwarfs should be presented as conditional on this assumed τ_mol_dep, and the uncertainty in the extrapolation should be propagated into the reported M_mol and any statements about molecular subdominance.
minor comments (6)
  1. [Table 5 note] The note 'The mean fractional SFR uncertainty across the sample is 0.077%' is misleadingly precise. It reflects only propagated random noise in the profiles, not the systematic uncertainties from SFR tracer calibration, background subtraction, or the upper-limit status of outer-disk rings. Please quote a systematics-inclusive uncertainty or remove the value.
  2. [Figure captions (Figs. 2, 4, 6, 8, 10, 12)] The vertical 'FUV threshold' (and 'W4 threshold') lines are not defined in the captions. Please state explicitly that points beyond these thresholds are 3σ upper limits in Σ_SFR and thus lower limits in depletion time.
  3. [Table 4] The table would benefit from explicit '>' or 'lower limit' markers on entries where the SFR is an upper limit, so that the table is self-consistent with the stated data limitations.
  4. [Table 2] The header 'Hirot.' appears to be a garbled abbreviation; it should read 'HI rotation curve' for clarity.
  5. [References] The Koch et al. (2025) reference has a malformed author list ('Koch, E., LGLBS, C., LGLBS, C., ...'). Please fix it.
  6. [Appendix B] The W1-based contamination slopes α for W4 and FUV in M31 are quoted without uncertainties. Since this correction affects the central M31 SFR profiles, an uncertainty estimate would be helpful.

Circularity Check

1 steps flagged

HI-dominance conclusion partly rests on 'expected' molecular gas built from SFR and an assumed depletion time; the central τ_dep results use independent HI and SFR data.

specific steps
  1. fitted input called prediction [Appendix A.4 / Eq. A6; Table 5 note b; Section 4 Conclusion 1]
    "We estimate the molecular gas surface density expected based on the star formation rate surface density in each ring. ... Σmol(τ mol dep ) M⊙ pc−2 = 10 3 ΣSFR M⊙ yr−1 kpc−2 τ mol dep Gyr (A6) ... When CO measurements are not available or not constraining, we estimate M mol from the Σ SFR profile and τ mol dep. ... Except for the innermost part of the dwarf starburst IC 10, Σ atom > Σ mol in every azimuthally averaged ring in our sample."

    For IC 1613, NGC 6822, and WLM the quoted Σ_mol is not measured but constructed via Eq. A6 from the same Σ_SFR that enters τ_atom_dep and an assumed τ_mol_dep (0.65–0.7 Gyr from Sun et al. 2025). Since Σ_mol_expected/Σ_atom = τ_mol_dep/τ_atom_dep, Conclusion 1's claim that Σ_atom > Σ_mol in these galaxies is algebraically equivalent to asserting the assumed molecular depletion time is shorter than the measured atomic depletion time. The paper labels these profiles 'expected,' which mitigates the issue, but the HI-dominance result for these three dwarfs is not an independent molecular-gas constraint.

full rationale

The central depletion-time analysis is not circular: τ_dep = Σ_gas/Σ_SFR is computed from LGLBS HI data and uniformly processed GALEX/WISE/Hα SFR maps, and for galaxies without CO data the paper explicitly takes Σ_gas = Σ_atom (Table 4 note a). No equation in that main derivation reduces to its own inputs. The self-citations (Koch et al. 2025 for HI data, Sun et al. 2022 for profile code, Sun et al. 2025 for the τ_mol_dep scaling relation) are data/calibration references, not load-bearing uniqueness theorems, and the results are compared against independent literature. The important limitation flagged in Section 2 — 'in all targets except M31, the sensitivity of the SFR tracers becomes a limiting factor in the outer disks of our targets so that many rings yield only upper limits' — is a sensitivity/statistical concern, not a circular construction: using upper-limit SFR as a detection can make apparent τ_dep rise with radius through the noise floor and makes Table 4 outer-disk values lower limits, which should be weighed in correctness. The one genuinely constructed element is the 'expected' molecular gas estimate of Eq. A6, used as support for the HI-dominance conclusion; because that estimate is proportional to the same Σ_SFR and an assumed τ_mol_dep, it does not independently establish atomic dominance. This affects Conclusion 1 for the three dwarfs without CO coverage, while Conclusions 2–3 rest on the independent HI/SFR ratio, so the overall circularity is partial rather than pervasive.

Axiom & Free-Parameter Ledger

3 free parameters · 7 axioms · 0 invented entities

The paper introduces no new physical entities; its free parameters are calibration values and corrections. The main burdens are the adopted external calibrations, two fitted M31 correction slopes, and the assumed molecular depletion times for CO-free dwarfs.

free parameters (3)
  • M31 W1-subtraction slopes α (W4, FUV) = 0.135 (W4), 0.001 (FUV)
    Fit to inner M31 region to remove old-stellar IR/UV contamination (Appendix B); enters corrected M31 SFR maps and hence M31 depletion times.
  • Assumed molecular depletion time τ_mol_dep for CO-free galaxies = 0.7 Gyr (IC1613, NGC6822), 0.65 Gyr (WLM)
    Extrapolated from the Sun et al. (2025) τ_mol_dep–M* relation (A.4); used to create expected Σ_mol profiles and Table 5 M_mol for galaxies without useful CO. These are not measured values.
  • Mass-to-light ratio Υ_3.4μm per galaxy = 0.31, 0.34, 0.31, 0.28, 0.28, 0.46 (IC10, IC1613, WLM, NGC6822, M33, M31)
    Adopted from SED-based calibration (A.6; Leroy et al. 2019) and used to convert W1 light to Σ*. A constant M/L does not change profile shapes, but the absolute stellar masses and stellar scale lengths are affected.
axioms (7)
  • domain assumption Optically thin 21-cm emission (A.1)
    Used to convert I_21cm to Σ_HI; if optical depth is significant, atomic gas masses/surface densities are underestimated.
  • domain assumption Lognormal distribution for f_corr (A.2)
    The bias correction for mass-weighted Σ_atom assumes the 120 pc column density distribution is lognormal within each ring; non-lognormal distributions would bias clumping factors.
  • domain assumption CO-to-H2 conversion relation (Eq. A5)
    α_CO scaling with metallicity and Σ* from Schinnerer & Leroy (2024) is adopted as an external calibration; affects Σ_mol for IC10, M33, M31.
  • ad hoc to paper τ_mol_dep–M* relation extrapolation (A.4)
    Sun et al. (2025) relation derived for M*=1e9.5–11 M⊙ is extrapolated down to ~1e7.5–8 M⊙ for WLM/IC1613/NGC6822; this is the basis for expected molecular gas estimates.
  • domain assumption W1-to-stellar-mass conversion (A.6)
    Υ_3.4μm from Salim/Leroy SED calibrations is used; the reported stellar masses depend on this.
  • domain assumption SFR tracer calibrations (A.5, A.7-A.11)
    FUV, W4, Hα, and combined SFR conversions from Leroy et al. (2019), Murphy et al. (2011), Calzetti et al. (2007), Belfiore et al. (2023) are treated as accurate.
  • domain assumption Fixed disk geometry for azimuthal averaging
    Profiles assume galaxies are thin inclined disks with LEDA inclinations/PAs; warps or asymmetric HI (e.g., NGC 6822) bias axisymmetric profiles.

pith-pipeline@v1.3.0-alltime-deepseek · 36312 in / 17287 out tokens · 159429 ms · 2026-08-01T06:32:19.185168+00:00 · methodology

0 comments
read the original abstract

Resolving atomic gas at $\lesssim100$ pc physical resolution is currently feasible only for the very nearest galaxies. We combine 120 pc resolution HI data using the Karl G. Jansky Very Large Array (VLA) from the first data release of the Local Group L-Band Survey (LGLBS) with uniformly processed infrared, ultraviolet, H$\alpha$, and CO maps. We analyze the radial profiles of gas, stars, and recent star formation for six local galaxies: M31, M33, IC 10, IC 1613, NGC 6822, and WLM. Across the sample, atomic-gas disks are the most extended component, reaching $r_{\rm HI}=2.8$-$5.8$ kpc in the dwarfs and $13$-$26$ kpc in M33 and M31. Azimuthally averaged $\Sigma_{\rm HI}$ profiles are often flat or only slowly declining compared to the steeper decline of $\Sigma_{\star}$ and $\Sigma_\mathrm{SFR}$, with outer HI scale lengths of $l_{\rm HI}^{\rm outer}\approx1.0$-$8.5$ kpc. The mass-weighted HI surface densities on 120 pc scale generally exceed the azimuthally averaged values by 10-70%, showing that localized high-column-density atomic structures persist even where azimuthally averaged profiles appear smooth. Atomic-gas depletion times rise from $\tau_{\rm dep}^{\rm atom}\approx0.8$-17 Gyr within the stellar half-mass radius to 10s-100 Gyr in the outer disks. Molecular depletion times are shorter. We provide a public release of these multi-wavelength data, which provide a valuable reference for the LGLBS targets and also form the basis for a companion paper that relates star formation, gas phases, and midplane pressure on 120 pc scales.

Figures

Figures reproduced from arXiv: 2607.21841 by Adam K. Leroy, Adam Smercina, Alberto D. Bolatto, Amanda A. Kepley, Chang-Goo Kim, Christina W. Lindberg, Cosima Eibensteiner, Elizabeth Tarantino, Eric W. Koch, Erik Roslowsky, Eve C. Ostriker, Fabian Walter, Jiayi Sun, Julianne J. Dalcanton, J\"urgen Ott, Laura B. Chomiuk, Michael P. Busch, Nickolas Pingel, Ryan Chown, Sne\v{z}ana Stanimirovi\'c, Sumit K. Sarbadhicary, Thomas G. Williams, Tobin M. Wainer, Vicente Villanueva.

Figure 1
Figure 1. Figure 1: Atlas of gas, stars and star formation for IC 10. The upper two maps show field of views matched to the H i map. The lower four panels show zoomed in versions to better illustrate the connection to the other tracers. The white dashed circle shows the rHI taken from [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Azimuthally-averaged surface density profiles for IC 10. The x-axes show galactocentric radius in physical units and normalized to the optical isophotal radius (r25). Upper left: Gas surface densities. Blue colors show the atomic gas surface density Σatom (Equation A1) including the 16-84% range as a shaded blue region. The vertical blue dashed line denotes rHI, the radius where Σatom = 1 M⊙ pc−2 . In ligh… view at source ↗
Figure 3
Figure 3. Figure 3: Atlas of gas, stars and star formation, same as [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Radial profiles same as [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Atlas of gas, stars and star formation, same as [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Radial profiles same as [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Atlas of gas, stars and star formation, same as [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Radial profiles same as [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Atlas of gas, stars and star formation, same as [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Radial profiles same as [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Atlas of gas, stars and star formation, same as [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Radial profiles same as [PITH_FULL_IMAGE:figures/full_fig_p017_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Correction for IR cirrus and stellar contamination in M31. The left panel shows the W4 map corrected by scaling and subtracting the W1 map. The right panel shows the uncorrected W4 map. The correction removes a large amount of emission not associated with recent star formation from the central region of M31 but does not significantly affect the disk (see [PITH_FULL_IMAGE:figures/full_fig_p029_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Left: Curves show the W4 (22 µm) annular profiles for M31: uncorrected (blue) and after subtracting the W1-based contaminant estimate (orange). The W1-based subtraction suppresses central emission unassociated with star formation while preserving the star-forming ring/outer disk. Right: The same for FUV profiles. See Appendix B [PITH_FULL_IMAGE:figures/full_fig_p030_14.png] view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

288 extracted references · 35 canonical work pages · 4 internal anchors

  1. [1]

    N., Hunter , D

    Archer , H. N., Hunter , D. A., Elmegreen , B. G., et al. 2024, title Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST , , 167, 274, 10.3847/1538-3881/ad3f18

    work page doi:10.3847/1538-3881/ad3f18 2024

  2. [2]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, title Astropy: A community Python package for astronomy , , 558, A33, 10.1051/0004-6361/201322068

    doi:10.1051/0004-6361/201322068 2013

  3. [3]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, title The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package , , 156, 123, 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-3881/aabc4f 2018

  4. [4]

    M., Lim , P

    Astropy Collaboration , Price-Whelan , A. M., Lim , P. L., et al. 2022, title The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package , , 935, 167, 10.3847/1538-4357/ac7c74

    doi:10.3847/1538-4357/ac7c74 2022

  5. [5]

    Athanassoula, E., & Beaton, R. L. 2006, title Unravelling the mystery of the M31 bar, MNRAS, 370, 1499

    2006

  6. [6]

    2011, title The Fine-scale Structure of the Neutral Interstellar Medium in Nearby Galaxies , , 141, 23, 10.1088/0004-6256/141/1/23

    Bagetakos , I., Brinks , E., Walter , F., et al. 2011, title The Fine-scale Structure of the Neutral Interstellar Medium in Nearby Galaxies , , 141, 23, 10.1088/0004-6256/141/1/23

    doi:10.1088/0004-6256/141/1/23 2011

  7. [7]

    K., Sun , J., et al

    Belfiore , F., Leroy , A. K., Sun , J., et al. 2023 a , title Calibration of hybrid resolved star formation rate recipes based on PHANGS-MUSE H and H maps , , 670, A67, 10.1051/0004-6361/202244863

    work page doi:10.1051/0004-6361/202244863 2023

  8. [8]

    K., Williams , T

    Belfiore , F., Leroy , A. K., Williams , T. G., et al. 2023 b , title Calibrating mid-infrared emission as a tracer of obscured star formation on H II-region scales in the era of JWST , , 678, A129, 10.1051/0004-6361/202347175

    doi:10.1051/0004-6361/202347175 2023

  9. [9]

    2010, title Extremely Inefficient Star Formation in the Outer Disks of Nearby Galaxies , , 140, 1194, 10.1088/0004-6256/140/5/1194

    Bigiel , F., Leroy , A., Walter , F., et al. 2010, title Extremely Inefficient Star Formation in the Outer Disks of Nearby Galaxies , , 140, 1194, 10.1088/0004-6256/140/5/1194

    doi:10.1088/0004-6256/140/5/1194 2010

  10. [10]

    A., et al

    Boardman , N., Zasowski , G., Newman , J. A., et al. 2020, title Are the Milky Way and Andromeda unusual? A comparison with Milky Way and Andromeda analogues , , 498, 4943, 10.1093/mnras/staa2731

    doi:10.1093/mnras/staa2731 2020

  11. [11]

    D., Wolfire , M., & Leroy , A

    Bolatto , A. D., Wolfire , M., & Leroy , A. K. 2013, title The CO-to-H _ 2 Conversion Factor , , 51, 207, 10.1146/annurev-astro-082812-140944

    doi:10.1146/annurev-astro-082812-140944 2013

  12. [12]

    1991, title The Distribution and Kinematics of Neutral Gas in M31 , , 372, 54, 10.1086/169954

    Braun , R. 1991, title The Distribution and Kinematics of Neutral Gas in M31 , , 372, 54, 10.1086/169954

    doi:10.1086/169954 1991

  13. [13]

    A., Walterbos , R

    Braun , R., Thilker , D. A., Walterbos , R. A. M., & Corbelli , E. 2009, title A Wide-Field High-Resolution H I Mosaic of Messier 31. I. Opaque Atomic Gas and Star Formation Rate Density , , 695, 937, 10.1088/0004-637X/695/2/937

    doi:10.1088/0004-637x/695/2/937 2009

  14. [14]

    1990, title The cool phase of the interstellar medium - Atomic gas , in Astrophysics and Space Science Library, Vol

    Brinks , E. 1990, title The cool phase of the interstellar medium - Atomic gas , in Astrophysics and Space Science Library, Vol. 161, The Interstellar Medium in Galaxies, ed. H. A. Thronson , Jr. & J. M. Shull , 39--65, 10.1007/978-94-009-0595-5_3

    work page doi:10.1007/978-94-009-0595-5_3 1990

  15. [15]

    Brinks , E., & Shane , W. W. 1984, title A high resolution hydrogen line survey of Messier 31.I. Observations and data reduction. , , 55, 179

    1984

  16. [16]

    D., Zabel , N., et al

    Brown , T., Wilson , C. D., Zabel , N., et al. 2021, title VERTICO: The Virgo Environment Traced in CO Survey , , 257, 21, 10.3847/1538-4365/ac28f5

    doi:10.3847/1538-4365/ac28f5 2021

  17. [17]

    2016, title Molecular Gas Velocity Dispersions in the Andromeda Galaxy , , 151, 34, 10.3847/0004-6256/151/2/34

    Cald \'u -Primo , A., & Schruba , A. 2016, title Molecular Gas Velocity Dispersions in the Andromeda Galaxy , , 151, 34, 10.3847/0004-6256/151/2/34

    doi:10.3847/0004-6256/151/2/34 2016

  18. [18]

    C., Engelbracht , C

    Calzetti , D., Kennicutt , R. C., Engelbracht , C. W., et al. 2007, title The Calibration of Mid-Infrared Star Formation Rate Indicators , , 666, 870, 10.1086/520082

    doi:10.1086/520082 2007

  19. [19]

    2022, title CASA, the Common Astronomy Software Applications for Radio Astronomy , , 134, 114501, 10.1088/1538-3873/ac9642

    CASA Team , Bean , B., Bhatnagar , S., et al. 2022, title CASA, the Common Astronomy Software Applications for Radio Astronomy , , 134, 114501, 10.1088/1538-3873/ac9642

    doi:10.1088/1538-3873/ac9642 2022

  20. [20]

    2009, title H I Kinematics and Dynamics of Messier 31 , , 705, 1395, 10.1088/0004-637X/705/2/1395

    Chemin , L., Carignan , C., & Foster , T. 2009, title H I Kinematics and Dynamics of Messier 31 , , 705, 1395, 10.1088/0004-637X/705/2/1395

    doi:10.1088/0004-637x/705/2/1395 2009

  21. [21]

    R., McLeod , A

    Chevance , M., Krumholz , M. R., McLeod , A. F., et al. 2023, title The Life and Times of Giant Molecular Clouds , in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 1, 10.48550/arXiv.2203.09570

    Pith/arXiv arXiv doi:10.48550/arxiv.2203.09570 2023

  22. [22]

    K., Bolatto , A

    Chown , R., Leroy , A. K., Bolatto , A. D., et al. 2025, title Relationships between Polycyclic Aromatic Hydrocarbons, Small Dust Grains, H _ 2 , and H I in Local Group Dwarf Galaxies NGC 6822 and WLM Using JWST, ALMA, and the VLA , , 987, 91, 10.3847/1538-4357/add73a

    doi:10.3847/1538-4357/add73a 2025

  23. [24]

    2010, title A wide-field H I mosaic of Messier 31

    Corbelli , E., Lorenzoni , S., Walterbos , R., Braun , R., & Thilker , D. 2010, title A wide-field H I mosaic of Messier 31. II. The disk warp, rotation, and the dark matter halo , , 511, A89, 10.1051/0004-6361/200913297

    doi:10.1051/0004-6361/200913297 2010

  24. [25]

    2014, title Dynamical signatures of a CDM-halo and the distribution of the baryons in M 33 , , 572, A23, 10.1051/0004-6361/201424033

    Corbelli , E., Thilker , D., Zibetti , S., Giovanardi , C., & Salucci , P. 2014, title Dynamical signatures of a CDM-halo and the distribution of the baryons in M 33 , , 572, A23, 10.1051/0004-6361/201424033

    doi:10.1051/0004-6361/201424033 2014

  25. [26]

    A., Young, L

    Davis, T. A., Young, L. M., Crocker, A. F., et al. 2014, title The role of old stellar populations in heating dust: separating ‘cirrus’ and star-forming emission in nearby galaxies, Monthly Notices of the Royal Astronomical Society, 444, 3427, 10.1093/mnras/stu1686

    work page doi:10.1093/mnras/stu1686 2014

  26. [27]

    de Blok , W. J. G., & Walter , F. 2000, title Evidence for Tidal Interaction and a Supergiant H I Shell in the Local Group Dwarf Galaxy NGC 6822 , , 537, L95, 10.1086/312777

    work page doi:10.1086/312777 2000

  27. [29]

    de Blok , W. J. G., & Walter , F. 2006, title The Stellar Population and Interstellar Medium in NGC 6822 , , 131, 343, 10.1086/497829

    work page doi:10.1086/497829 2006

  28. [30]

    2018, title Evolved stars in the Local Group galaxies - II

    Dell'Agli , F., Di Criscienzo , M., Ventura , P., et al. 2018, title Evolved stars in the Local Group galaxies - II. AGB, RSG stars, and dust production in IC10 , , 479, 5035, 10.1093/mnras/sty1614

    doi:10.1093/mnras/sty1614 2018

  29. [31]

    M., Murray , C., et al

    Dempsey , J., McClure-Griffiths , N. M., Murray , C., et al. 2022, title GASKAP-HI Pilot Survey Science III: An unbiased view of cold gas in the Small Magellanic Cloud , , 39, e034, 10.1017/pasa.2022.18

    doi:10.1017/pasa.2022.18 2022

  30. [32]

    R., & van der Hulst , J

    Deul , E. R., & van der Hulst , J. M. 1987, title A survey of the neutral atomic hydrogen in M 33. , , 67, 509

    1987

  31. [34]

    M., McClure-Griffiths , N., Gibson , S

    Dickey , J. M., McClure-Griffiths , N., Gibson , S. J., et al. 2013, title GASKAP-The Galactic ASKAP Survey , , 30, e003, 10.1017/pasa.2012.003

    doi:10.1017/pasa.2012.003 2013

  32. [35]

    L., Krumholz , M

    Dobbs , C. L., Krumholz , M. R., Ballesteros-Paredes , J., et al. 2014, title Formation of Molecular Clouds and Global Conditions for Star Formation , in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 3--26, 10.2458/azu_uapress_9780816531240-ch001

    doi:10.2458/azu_uapress_9780816531240-ch001 2014

  33. [36]

    F., et al

    Druard , C., Braine , J., Schuster , K. F., et al. 2014, title The IRAM M 33 CO(2-1) survey. A complete census of molecular gas out to 7 kpc , , 567, A118, 10.1051/0004-6361/201423682

    doi:10.1051/0004-6361/201423682 2014

  34. [37]

    V., Bianchi , L., Thilker , D

    Efremova , B. V., Bianchi , L., Thilker , D. A., et al. 2011, title The Recent Star Formation in NGC 6822: An Ultraviolet Study , , 730, 88, 10.1088/0004-637X/730/2/88

    work page doi:10.1088/0004-637x/730/2/88 2011

  35. [38]

    K., Sun , J., Koch , E., & LGLBS

    Eibensteiner , C., Leroy , A. K., Sun , J., Koch , E., & LGLBS. 2026 a , title Adding mul ,

    2026

  36. [39]

    K., Sun , J., Koch , E., & LGLBS

    Eibensteiner , C., Leroy , A. K., Sun , J., Koch , E., & LGLBS. 2026 b , title Adding mul ,

    2026

  37. [40]

    A., Gurvich , A

    Flores Vel \'a zquez , J. A., Gurvich , A. B., Faucher-Gigu \`e re , C.-A., et al. 2021, title The time-scales probed by star formation rate indicators for realistic, bursty star formation histories from the FIRE simulations , , 501, 4812, 10.1093/mnras/staa3893

    doi:10.1093/mnras/staa3893 2021

  38. [41]

    F., Brouillet , N., & Sievers , A

    Gardan , E., Braine , J., Schuster , K. F., Brouillet , N., & Sievers , A. 2007, title Particularly efficient star formation in M \, 33 , , 473, 91, 10.1051/0004-6361:20077711

    work page doi:10.1051/0004-6361:20077711 2007

  39. [42]

    J., Combes , F., et al

    Genzel , R., Tacconi , L. J., Combes , F., et al. 2012, title The Metallicity Dependence of the CO H _ 2 Conversion Factor in z >= 1 Star-forming Galaxies , , 746, 69, 10.1088/0004-637X/746/1/69

    doi:10.1088/0004-637x/746/1/69 2012

  40. [43]

    Gerbrandt , S. A. N., McConnachie , A. W., & Irwin , M. 2015, title The red extended structure of IC 10, the nearest blue compact galaxy , , 454, 1000, 10.1093/mnras/stv2029

    work page doi:10.1093/mnras/stv2029 2015

  41. [44]

    2019, radio-astro-tools/spectral-cube: Release v0.4.5 , v0.4.5 Zenodo, 10.5281/zenodo.3558614

    Ginsburg , A., Koch , E., Robitaille , T., et al. 2019, radio-astro-tools/spectral-cube: Release v0.4.5 , v0.4.5 Zenodo, 10.5281/zenodo.3558614

    doi:10.5281/zenodo.3558614 2019

  42. [45]

    D., Bailin , J., Engelbracht , C

    Gordon , K. D., Bailin , J., Engelbracht , C. W., et al. 2006, title Spitzer MIPS Infrared Imaging of M31: Further Evidence for a Spiral-Ring Composite Structure , , 638, L87, 10.1086/501046

    work page doi:10.1086/501046 2006

  43. [46]

    J., et al

    Gratier , P., Braine , J., Rodriguez-Fernandez , N. J., et al. 2010, title Molecular and atomic gas in the Local Group galaxy M 33 , , 522, A3, 10.1051/0004-6361/201014441

    doi:10.1051/0004-6361/201014441 2010

  44. [47]

    Greenawalt , B. E. 1998, title Diffuse Ionized Gas in Nearby Spiral Galaxies , PhD thesis, New Mexico State University

    1998

  45. [48]

    J., Pritzl , B

    Grossi , M., Disney , M. J., Pritzl , B. J., et al. 2007, title Star formation history and evolution of gas-rich dwarf galaxies in the Centaurus A group , , 374, 107, 10.1111/j.1365-2966.2006.11125.x

    arXiv 2007

  46. [49]

    K., Madden , S

    Grossi , M., Hunt , L. K., Madden , S. C., et al. 2015, title The Herschel Virgo Cluster Survey. XVIII. Star-forming dwarf galaxies in a cluster environment , , 574, A126, 10.1051/0004-6361/201424866

    work page doi:10.1051/0004-6361/201424866 2015

  47. [50]

    2012, title The heating of dust by old stellar populations in the bulge of M31 , , 426, 892, 10.1111/j.1365-2966.2012.21696.x

    Groves , B., Krause , O., Sandstrom , K., et al. 2012, title The heating of dust by old stellar populations in the bulge of M31 , , 426, 892, 10.1111/j.1365-2966.2012.21696.x

    arXiv 2012

  48. [52]

    A., Javadi , A., & van Loon , J

    Hashemi , S. A., Javadi , A., & van Loon , J. T. 2019, title From evolved stars to the evolution of IC 1613 , , 483, 4751, 10.1093/mnras/sty3450

    work page doi:10.1093/mnras/sty3450 2019

  49. [54]

    G., & Walterbos , R

    Hoopes , C. G., & Walterbos , R. A. M. 2000, title The Contribution of Field OB Stars to the Ionization of the Diffuse Ionized Gas in M33 , , 541, 597, 10.1086/309487

    work page doi:10.1086/309487 2000

  50. [55]

    K., Garc \' a-Burillo , S., Casasola , V., et al

    Hunt , L. K., Garc \' a-Burillo , S., Casasola , V., et al. 2015, title Molecular depletion times and the CO-to-H _ 2 conversion factor in metal-poor galaxies , , 583, A114, 10.1051/0004-6361/201526553

    doi:10.1051/0004-6361/201526553 2015

  51. [56]

    A., & Elmegreen , B

    Hunter , D. A., & Elmegreen , B. G. 2004, title Star Formation Properties of a Large Sample of Irregular Galaxies , , 128, 2170, 10.1086/424615

    doi:10.1086/424615 2004

  52. [57]

    A., Elmegreen , B

    Hunter , D. A., Elmegreen , B. G., & Madden , S. C. 2024, title The Interstellar Medium in Dwarf Irregular Galaxies , , 62, 113, 10.1146/annurev-astro-052722-104109

    doi:10.1146/annurev-astro-052722-104109 2024

  53. [58]

    A., Ficut-Vicas , D., Ashley , T., et al

    Hunter , D. A., Ficut-Vicas , D., Ashley , T., et al. 2012, title Little Things , , 144, 134, 10.1088/0004-6256/144/5/134

    doi:10.1088/0004-6256/144/5/134 2012

  54. [60]

    Z., Carignan , C., Chemin , L., et al

    Kam , S. Z., Carignan , C., Chemin , L., et al. 2017, title H I Kinematics and Mass Distribution of Messier 33 , , 154, 41, 10.3847/1538-3881/aa79f3

    doi:10.3847/1538-3881/aa79f3 2017

  55. [61]

    C., & Evans , N

    Kennicutt , R. C., & Evans , N. J. 2012, title Star Formation in the Milky Way and Nearby Galaxies , , 50, 531, 10.1146/annurev-astro-081811-125610

    doi:10.1146/annurev-astro-081811-125610 2012

  56. [62]

    A., Bittle , L., Leroy , A

    Kepley , A. A., Bittle , L., Leroy , A. K., et al. 2018, title Dense Molecular Gas in the Nearby Low-metallicity Dwarf Starburst Galaxy IC 10 , , 862, 120, 10.3847/1538-4357/aacaf4

    doi:10.3847/1538-4357/aacaf4 2018

  57. [63]

    2021, title Kinematical asymmetry in the dwarf irregular galaxy WLM and a perturbed halo potential , , 654, A7, 10.1051/0004-6361/202140336

    Khademi , M., Yang , Y., Hammer , F., & Nasiri , S. 2021, title Kinematical asymmetry in the dwarf irregular galaxy WLM and a perturbed halo potential , , 654, A7, 10.1051/0004-6361/202140336

    work page doi:10.1051/0004-6361/202140336 2021

  58. [64]

    2025, title The Karl G

    Koch , E., LGLBS , C., LGLBS , C., LGLBS , C., & LGLBS , C. 2025, title The Karl G. Jansky Very Large Array Local Group L-band Survey (LGLBS) , , 50, 531

    2025

  59. [65]

    W., Rosolowsky , E

    Koch , E. W., Rosolowsky , E. W., Lockman , F. J., et al. 2018, title Kinematics of the atomic ISM ifigun M33 on 80 pc scales , , 479, 2505, 10.1093/mnras/sty1674

    doi:10.1093/mnras/sty1674 2018

  60. [67]

    2001, title On the variation of the initial mass function , , 322, 231, 10.1046/j.1365-8711.2001.04022.x

    Kroupa , P. 2001, title On the variation of the initial mass function , , 322, 231, 10.1046/j.1365-8711.2001.04022.x

    arXiv 2001

  61. [68]

    Lake , G., & Skillman , E. D. 1989, title The Mass Distribution and the Law of Gravity in the Local Group Dwarf Irregular Galaxy IC 1613 , , 98, 1274, 10.1086/115215

    work page doi:10.1086/115215 1989

  62. [69]

    2014, title unWISE: Unblurred Coadds of the WISE Imaging , , 147, 108, 10.1088/0004-6256/147/5/108

    Lang , D. 2014, title unWISE: Unblurred Coadds of the WISE Imaging , , 147, 108, 10.1088/0004-6256/147/5/108

    doi:10.1088/0004-6256/147/5/108 2014

  63. [70]

    A., Brooks , A

    Leaman , R., Venn , K. A., Brooks , A. M., et al. 2012, title The Resolved Structure and Dynamics of an Isolated Dwarf Galaxy: A VLT and Keck Spectroscopic Survey of WLM , , 750, 33, 10.1088/0004-637X/750/1/33

    work page doi:10.1088/0004-637x/750/1/33 2012

  64. [71]

    J., Freedman , W

    Lee , A. J., Freedman , W. L., Madore , B. F., et al. 2021, title The Astrophysical Distance Scale. III. Distance to the Local Group Galaxy WLM Using Multiwavelength Observations of the Tip of the Red Giant Branch, Cepheids, and JAGB Stars , , 907, 112, 10.3847/1538-4357/abd253

    doi:10.3847/1538-4357/abd253 2021

  65. [72]

    J., Monson , A

    Lee , A. J., Monson , A. J., Freedman , W. L., et al. 2024, title Resolved Near-infrared Stellar Photometry from the Magellan Telescope for 13 Nearby Galaxies: J-region Asymptotic Giant Branch Method Distances , , 967, 22, 10.3847/1538-4357/ad32c7

    doi:10.3847/1538-4357/ad32c7 2024

  66. [73]

    C., Veilleux , S., McDonald , M., & Hilbert , B

    Lee , J. C., Veilleux , S., McDonald , M., & Hilbert , B. 2016, title A Deeper Look at Faint H Emission in Nearby Dwarf Galaxies , , 817, 177, 10.3847/0004-637X/817/2/177

    work page doi:10.3847/0004-637x/817/2/177 2016

  67. [74]

    C., Gil de Paz , A., Tremonti , C., et al

    Lee , J. C., Gil de Paz , A., Tremonti , C., et al. 2009, title Comparison of H and UV Star Formation Rates in the Local Volume: Systematic Discrepancies for Dwarf Galaxies , , 706, 599, 10.1088/0004-637X/706/1/599

    doi:10.1088/0004-637x/706/1/599 2009

  68. [75]

    C., & Wakker , B

    Lehner , N., Howk , J. C., & Wakker , B. P. 2015, title Evidence for a Massive, Extended Circumgalactic Medium Around the Andromeda Galaxy , , 804, 79, 10.1088/0004-637X/804/2/79

    doi:10.1088/0004-637x/804/2/79 2015

  69. [76]

    D., et al

    Leitherer , C., Schaerer , D., Goldader , J. D., et al. 1999, title Starburst99: Synthesis Models for Galaxies with Active Star Formation , , 123, 3, 10.1086/313233

    doi:10.1086/313233 1999

  70. [77]

    2006, title Molecular Gas in the Low-Metallicity, Star-forming Dwarf IC 10 , , 643, 825, 10.1086/503024

    Leroy , A., Bolatto , A., Walter , F., & Blitz , L. 2006, title Molecular Gas in the Low-Metallicity, Star-forming Dwarf IC 10 , , 643, 825, 10.1086/503024

    work page doi:10.1086/503024 2006

  71. [78]

    K., Walter , F., Brinks , E., et al

    Leroy , A. K., Walter , F., Brinks , E., et al. 2008, title The Star Formation Efficiency in Nearby Galaxies: Measuring Where Gas Forms Stars Effectively , , 136, 2782, 10.1088/0004-6256/136/6/2782

    doi:10.1088/0004-6256/136/6/2782 2008

  72. [79]

    K., Bigiel , F., de Blok , W

    Leroy , A. K., Bigiel , F., de Blok , W. J. G., et al. 2012, title Estimating the Star Formation Rate at 1 kpc Scales in nearby Galaxies , , 144, 3, 10.1088/0004-6256/144/1/3

    doi:10.1088/0004-6256/144/1/3 2012

  73. [80]

    K., Walter , F., Sandstrom , K., et al

    Leroy , A. K., Walter , F., Sandstrom , K., et al. 2013, title Molecular Gas and Star Formation in nearby Disk Galaxies , , 146, 19, 10.1088/0004-6256/146/2/19

    doi:10.1088/0004-6256/146/2/19 2013

  74. [81]

    K., Hughes , A., Schruba , A., et al

    Leroy , A. K., Hughes , A., Schruba , A., et al. 2016, title A Portrait of Cold Gas in Galaxies at 60 pc Resolution and a Simple Method to Test Hypotheses That Link Small-scale ISM Structure to Galaxy-scale Processes , , 831, 16, 10.3847/0004-637X/831/1/16

    doi:10.3847/0004-637x/831/1/16 2016

  75. [82]

    K., Sandstrom , K

    Leroy , A. K., Sandstrom , K. M., Lang , D., et al. 2019, title A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies , , 244, 24, 10.3847/1538-4365/ab3925

    doi:10.3847/1538-4365/ab3925 2019

  76. [83]

    K., Schinnerer , E., Hughes , A., et al

    Leroy , A. K., Schinnerer , E., Hughes , A., et al. 2021, title PHANGS-ALMA: Arcsecond CO(2-1) Imaging of Nearby Star-forming Galaxies , , 257, 43, 10.3847/1538-4365/ac17f3

    doi:10.3847/1538-4365/ac17f3 2021

  77. [84]

    K., Sandstrom , K., Rosolowsky , E., et al

    Leroy , A. K., Sandstrom , K., Rosolowsky , E., et al. 2023, title PHANGS-JWST First Results: Mid-infrared Emission Traces Both Gas Column Density and Heating at 100 pc Scales , , 944, L9, 10.3847/2041-8213/acaf85

    doi:10.3847/2041-8213/acaf85 2023

  78. [85]

    R., Dolphin , A

    Lewis , A. R., Dolphin , A. E., Dalcanton , J. J., et al. 2015, title The Panchromatic Hubble Andromeda Treasury. XI. The Spatially Resolved Recent Star Formation History of M31 , , 805, 183, 10.1088/0004-637X/805/2/183

    doi:10.1088/0004-637x/805/2/183 2015

  79. [86]

    R., Simones , J

    Lewis , A. R., Simones , J. E., Johnson , B. D., et al. 2017, title The Panchromatic Hubble Andromeda Treasury. XVII. Examining Obscured Star Formation with Synthetic Ultraviolet Flux Maps in M31. , , 834, 70, 10.3847/1538-4357/834/1/70

    work page doi:10.3847/1538-4357/834/1/70 2017

  80. [87]

    L., Pan , H.-A., et al

    Lin , L., Ellison , S. L., Pan , H.-A., et al. 2020, title ALMaQUEST. IV. The ALMA-MaNGA QUEnching and STar Formation (ALMaQUEST) Survey , , 903, 145, 10.3847/1538-4357/abba3a

    doi:10.3847/1538-4357/abba3a 2020

Showing first 80 references.