pith. sign in

arxiv: 2606.17262 · v1 · pith:AHVSJVGVnew · submitted 2026-06-15 · 🌌 astro-ph.GA

Dust-Embedded Star Formation: Bridging Magellanic Cloud Studies of Massive Young Stellar Objects to Nearby Spiral Galaxies

M. Jimena Rodr\'iguez , R\'emy Indebetouw , Janice C. Lee , Bradley C. Whitmore , David A. Thilker , J. Peltonen , Erik Rosolowsky , Thomas G. Williams
show 8 more authors
Eric W. Koch Bruce Elmegreen Ralf S. Klessen Roberta Paladini Sumit Sarbadhicary Daniel A. Dale Kelsey E. Johnson Aida Wofford
This is my paper

Pith reviewed 2026-06-27 02:29 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords JWSTmassive young stellar objectsdust-embedded star formationMagellanic Cloudsnearby galaxiescolor selectionluminosity functionembedded clusters
0
0 comments X

The pith

JWST color-magnitude cuts for massive young stellar objects remain stable from 1 to 5 Mpc, with a 10um luminosity function slope near -2, though resolution limits individual studies beyond 3 Mpc.

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

The paper tests whether color selection criteria derived from well-studied massive young stellar objects in the Large Magellanic Cloud can be transferred to JWST observations of four spiral galaxies between 1 and 5 Mpc away. It identifies hundreds of dusty compact sources and shows that the same cuts in F1000W versus F1000W-F2100W continue to work across this distance range while the luminosity function slope stays near -2. At larger distances blending and surface-brightness effects remove fainter objects and bias the sample, setting a practical limit around 3 Mpc for resolving individual sources. The work creates a catalog that links detailed local templates to more distant resolved studies of embedded star formation.

Core claim

Guided by the SAGE-LMC catalog, the authors define JWST color-magnitude selection criteria and apply them to NIRCam and MIRI imaging of M33, NGC 300, NGC 7793, and NGC 5068. They recover 216, 32, 80, and 139 dusty young objects respectively; the selection remains stable across 1-5 Mpc, the 10um luminosity function retains a slope of alpha ~ -2, and comparisons with PAH-selected clusters recover ~80 percent of sources, while blending causes up to 50 percent incompleteness at 5.2 Mpc and biases toward brighter objects.

What carries the argument

JWST color-magnitude selection criteria (F1000W versus F1000W-F2100W) derived from the SAGE-LMC catalog of massive young stellar objects, tested via resolution-degradation experiments.

Load-bearing premise

The color-magnitude cuts defined from the SAGE-LMC catalog apply directly to the target galaxies without major adjustments for differences in dust properties, metallicity, or star-formation conditions.

What would settle it

Finding that the fraction of sources selected by the F1000W versus F1000W-F2100W cuts, or the recovered luminosity function slope, changes substantially when the same criteria are applied to a galaxy whose metallicity or dust-to-gas ratio differs markedly from the LMC.

Figures

Figures reproduced from arXiv: 2606.17262 by Aida Wofford, Bradley C. Whitmore, Bruce Elmegreen, Daniel A. Dale, David A. Thilker, Eric W. Koch, Erik Rosolowsky, Janice C. Lee, J. Peltonen, Kelsey E. Johnson, M. Jimena Rodr\'iguez, Ralf S. Klessen, R\'emy Indebetouw, Roberta Paladini, Sumit Sarbadhicary, Thomas G. Williams.

Figure 1
Figure 1. Figure 1: JWST NIRCam and MIRI observed footprints overlaid on a Spitzer MIPS 24µm image of each galaxy. M33, NGC 300, NGC 7793 were observed as part of GO-2130 (PI J.C. Lee), and NGC 5068 as part of the Cycle 1 PHANGS-JWST Treasury Survey (GO-2107 Lee et al. 2023) [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of JWST, HST, and Spitzer imaging for select areas of M 33, NGC 300, NGC 7793 and NGC 5068 to a provide a more detailed view of several star-forming regions in each galaxy. Spitzer MIPS 24µm imaging is shown in the top panels. NIRCam 2µm and MIRI 21µm imaging shown in second and third row of panels respectively. The dramatic improvement in resolution and sensitivity achieved by JWST, which enabl… view at source ↗
Figure 3
Figure 3. Figure 3: Top Panels: Color-–magnitude diagrams of point sources from the SAGE LMC catalog projected to larger distances. The diagrams use photometry at 8µm (IRAC4) and 24µm (MIPS1). Objects identified as MYSOs (Whitney et al. 2008; Gruendl & Chu 2009) are color-coded by stellar mass derived from single-source dust radiative-transfer modeling of their spectral energy distributions. Regions occupied by main-sequence … view at source ↗
Figure 4
Figure 4. Figure 4: Predictions, based on Spitzer SAGE-LMC data, of the impact of source blending in JWST imaging as a func￾tion of distance on the characterization of dusty embedded star clusters. Green: fraction of clusters dominated by a sin￾gle MYSO whose infrared colors change by less than 0.3 dex as the aperture size increases to simulate larger distances. In this regime the properties of individual MYSOs (e.g., masses … view at source ↗
Figure 5
Figure 5. Figure 5: Near-IR color–magnitude diagrams for the JWST observations presented in this paper (top, for M33, NGC 300, NGC 7793, and NGC 5068), and based on SAGE-LMC (bottom, projected to distances of 0.8, 2.0, and 3.7 Mpc). These diagrams are analogous to the 21/10 µm (JWST) and 24/8 µm (Spitzer) CMDs presented earlier in Figures 3 and 8, but the JWST CMDs are now color-coded by concentration index (CI). Purple hues … view at source ↗
Figure 6
Figure 6. Figure 6: Spatial distribution of the dusty young popula￾tion overlaid on the JWST F1000W image of each galaxy. Colored circles indicate objects in different categories, while the magenta contours show the 90th percentile of the ALMA CO(2–1) emission. lost due to source merging or surface-brightness dilu￾tion, and how these effects impact the color–magnitude diagram (CMD) selection used to identify dusty young objec… view at source ↗
Figure 7
Figure 7. Figure 7: Example of a point-source dominated object in M33 shown at increasing simulated distances, from the native resolution at 0.85 Mpc to 5.2 Mpc. In the original F1000W image two nearby sources are detected (green symbols); the red circle marks the position of object 149, which is the fo￾cus of this example. As the images are convolved to larger distances the two sources blend into a single F1000W peak. The pe… view at source ↗
Figure 8
Figure 8. Figure 8: Set of color–magnitude diagrams showing F2100W/F1000W vs. F1000W in mJy (with AB–magnitude conversions indicated on the top and right axes), for the four galaxies at different resolutions. Each row corresponds to a galaxy (from top to bottom: M 33; NGC 300; NGC 7793 and NGC 5068) and each column corresponds to a specific distance: M 33 at native resolution (0.85 Mpc) and convolved to 2, 3.6 and 5.2 Mpc (to… view at source ↗
Figure 9
Figure 9. Figure 9: Original (green) and final (red) positions in the F1000W vs. F2100W/F1000W CMD of M33 sources that move into the upper-right region of the diagram in the convolved images. Some sources already satisfy the F2100W/F1000W color criterion but are initially too faint to meet the magnitude threshold; after merging with neigh￾boring sources they become brighter and move into the se￾lected region. Others shift fro… view at source ↗
Figure 11
Figure 11. Figure 11: Fraction of F2100W emission which is identified as compact star-forming sources, as a function of 100 pc sur￾face brightness, and at 3 different distances. The fraction of emission in compact sources is higher in brighter regions of the image, and increases as the distance increases and reso￾lution degrades. See text for details of the calculation – the dashed lines show the fraction over the entire image… view at source ↗
Figure 10
Figure 10. Figure 10: Top: Histograms of the F1000W flux for dusty young sources detected in M 33 at native resolution (yellow). The subsets of these sources that are not recov￾ered when the images are convolved to distances of 2, 3.6, and 5.2 Mpc are shown in green, blue, and orange, respec￾tively. The losses occur predominantly among the fainter sources, while the brightest objects remain detectable even at the largest simul… view at source ↗
Figure 12
Figure 12. Figure 12: F1000W luminosity functions of the dusty young population in M 33, NGC 300, NGC 7793, and NGC 5068 (left to right) at the native and convolved resolutions. As the images are degraded, the LF shifts toward brighter magnitudes due to the blending of multiple sources, while the number of faint sources decreases. The slopes of the bright end remain largely unchanged with distance. M 33, NGC 7793, and NGC 5068… view at source ↗
Figure 13
Figure 13. Figure 13: Constraints on the mass range spanned by the sample of young dusty compact sources presented here using two limiting approaches. Masses shown on the x-axis are derived from SAGE MYSOs based on the 21µm luminosity, while masses on the y-axis are computed using the mass-to-light ratio of young (< 3 Myr) PHANGS–HST star clusters at 2µm. Different symbols correspond to different visual classifications (Sectio… view at source ↗
Figure 14
Figure 14. Figure 14: color image of the PHATTER’s cluster ID: 652 (the white cross shows the cluster’s center). Blue: HST F475W, green: JWST F210M, red: JWST F1000W. White circles are objects identified as point-source dominated and the cyan is an objects classified as compact marginally re￾solved in the current work. CMD ( [PITH_FULL_IMAGE:figures/full_fig_p022_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: CMDs for M 33 (left) and NGC 5068 (second, third, and fourth panels), showing different catalogs of dusty young objects compiled from the literature, used for comparison in this work. distance, with a slope of ∼–2, although it shifts to￾ward brighter magnitudes due to source blending and the loss of fainter objects (Sect. 6.1). • Using two complementary empirical mass estima￾tors, we bracket the character… view at source ↗
Figure 16
Figure 16. Figure 16: Examples of point-source dominated sources within star-forming regions. Blue: F210M (M 33) or F200W (NGC 300,NGC 7793 and NGC 7793) / Green:F430M (M 33), F444W (NGC 300 and NGC 7793) or F360M (NGC 5068)/, Red: F1000W. Cutout are 3×3 arcsec2 which is equivalent to ∼13.6× 13.6 pc2 at the distance of M 33, ∼30× 30 pc2 (NGC 300), ∼52× 52 pc2 (NGC 7793) and ∼75.5× 75.5 pc2 (NGC 5068). The large central circles… view at source ↗
Figure 17
Figure 17. Figure 17: Examples of point-source dominated isolated sources. Blue: F210M (M 33) or F200W (NGC 300,NGC 7793 and NGC 7793) / Green:F430M (M 33), F444W (NGC 300 and NGC 7793) or F360M (NGC 5068)/, Red: F1000W. Cutout are 3×3 arcsec2 which is equivalent to ∼13.6× 13.6 pc2 at the distance of M 33, ∼30× 30 pc2 (NGC 300), ∼52× 52 pc2 (NGC 7793) and ∼75.5× 75.5 pc2 (NGC 5068). The large central circles indicate the objec… view at source ↗
Figure 18
Figure 18. Figure 18: Examples of compact marginally resolved sources. Blue: F210M (M 33) or F200W (NGC 300,NGC 7793 and NGC 7793) / Green:F430M (M 33), F444W (NGC 300 and NGC 7793) or F360M (NGC 5068)/, Red: F1000W. Cutout are 3×3 arcsec2 which is equivalent to ∼13.6× 13.6 pc2 at the distance of M 33, ∼30× 30 pc2 (NGC 300), ∼52× 52 pc2 (NGC 7793) and ∼75.5× 75.5 pc2 (NGC 5068). The large central circles indicate the objects w… view at source ↗
Figure 19
Figure 19. Figure 19: Examples of background galaxies. Blue:F475W (M 33)/F435W (NGC 300), Green:F430M, Red: F1000W. Cutout are 5×5 arcsec2 which is equivalent to ∼20× 20 pc2 at the distance of M 33, ∼49× 49 pc2 (NGC 300), and ∼87× 87 pc2 (NGC 7793) [PITH_FULL_IMAGE:figures/full_fig_p028_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: Comparison of synthetic JWST F770W, F1000W, and F2100W fluxes and corresponding Spitzer IRAC4 (7.87 µm) and MIPS1 (23.7 µm) photometric fluxes derived from Spitzer IRS spectra for dusty Magellanic sources in the SAGE-Spec survey (evolved stars, MYSOs, and a small number of PNe and SNRs). The panels show log(FJWST) versus log(FSpitzer) for each matched filter pair; flux densities are Fν in mJy. Linear fits… view at source ↗
Figure 21
Figure 21. Figure 21: Comparison of colors computed from synthetic JWST fluxes with Spitzer photometry. The two panels show the relationships between F2100W/F1000W and F2100W/F770W with MIPS1/IRAC4. Linear fits are overplotted and the corresponding slopes, intercepts, and Spearman correlation coefficients listed in the legend. These relations provide the color transformations used to translate Spitzer-based CMDs to the JWST fi… view at source ↗
read the original abstract

We use JWST NIRCam and MIRI imaging at 2, 4, 10, and 21 um to study young, dusty compact sources in four nearby galaxies at distances of ~ 1-5Mpc (M33, NGC300, NGC7793, and NGC5068). This work bridges well-characterized massive young stellar objects (MYSOs) in the Magellanic Clouds from the Spitzer SAGE survey to new studies of embedded clusters in more distant galaxies with JWST. Guided by the SAGE-LMC catalog, we define JWST color-magnitude selection criteria (F1000W versus F1000W-F2100W) and test them using resolution-degradation experiments. We identify 216, 32, 80 and 139 dusty young objects in the four galaxies, respectively. The selected population spans sources from systems dominated by a single MYSO to compact marginally resolved sources hosting multiple MYSOs. The color selection remains stable across 1-5 Mpc, and the 10um luminosity function retains a slope of alpha~ -2. However, blending and surface-brightness dilution remove fainter sources, leading to incompleteness of up to ~ 50% at 5.2 Mpc and biasing the sample toward brighter objects (F1000W < 19 mag). The sample spans approximate stellar masses of ~10-2 X 10^5 Mo. Spatial resolution affects the interpretation of mid-infrared emission: clustering increases the fraction of emission attributed to compact sources in active regions, while blending into diffuse emission dominates in quiescent environments. Comparisons with PAH-selected young clusters in the PHANGS galaxy NGC5068 show that our selection recovers ~ 80% of the PAH-selected sources. We show that the practical limit for studying individual MYSOs with JWST is ~3 Mpc. The resulting catalog provides a foundation for future resolved studies of star formation rates and early cluster evolution.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 1 minor

Summary. The manuscript applies JWST NIRCam/MIRI imaging at 2, 4, 10, and 21 μm to four galaxies at 1–5 Mpc (M33, NGC 300, NGC 7793, NGC 5068). Using fixed F1000W vs. F1000W–F2100W color-magnitude cuts derived from the SAGE-LMC catalog, it identifies 216, 32, 80, and 139 dusty compact sources. Resolution-degradation experiments are used to test distance effects; the paper claims the selection remains stable, the 10 μm luminosity function slope is α ≈ –2, incompleteness reaches ~50% at 5.2 Mpc, and the practical limit for individual MYSO studies is ~3 Mpc. The catalog is positioned as a bridge to future resolved SFR and cluster-evolution studies.

Significance. If the transferability of the LMC-derived cuts holds, the work supplies an observationally grounded catalog linking Magellanic-Cloud MYSO studies to spiral-galaxy embedded populations and quantifies practical JWST distance limits via resolution tests. The resolution-degradation approach is a concrete methodological strength.

major comments (1)
  1. [Abstract / Selection criteria] Abstract and § on selection criteria: the central stability claim ('color selection remains stable across 1–5 Mpc') and the reported α ≈ –2 slope rest on applying fixed SAGE-LMC cuts without testing for shifts arising from metallicity or dust-property differences between the LMC and the target galaxies. The resolution-degradation experiments address only blending and surface-brightness dilution; they do not constrain possible color-locus offsets from PAH or grain-emissivity variations. This assumption is load-bearing for both the distance-stability and luminosity-function results.
minor comments (1)
  1. [Abstract] Abstract: the mass range '~10-2 X 10^5 Mo' is unclear; rephrase for precision (e.g., 10–2×10^5 M⊙).

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their detailed review and for highlighting this important assumption in our analysis. We address the major comment below.

read point-by-point responses

  1. Referee: [Abstract / Selection criteria] Abstract and § on selection criteria: the central stability claim ('color selection remains stable across 1–5 Mpc') and the reported α ≈ –2 slope rest on applying fixed SAGE-LMC cuts without testing for shifts arising from metallicity or dust-property differences between the LMC and the target galaxies. The resolution-degradation experiments address only blending and surface-brightness dilution; they do not constrain possible color-locus offsets from PAH or grain-emissivity variations. This assumption is load-bearing for both the distance-stability and luminosity-function results.

    Authors: We agree that the resolution-degradation experiments address only the effects of distance on spatial resolution, blending, and surface-brightness dilution, and do not test for possible shifts in the color locus arising from differences in metallicity or dust properties (e.g., PAH emission or grain emissivity) between the LMC and the target galaxies. The manuscript applies fixed cuts derived from the SAGE-LMC catalog without explicit tests for such offsets. The target galaxies span metallicities of roughly 0.4–1.0 Z⊙, comparable to the LMC, but this does not substitute for a direct test. We will revise the abstract, selection-criteria section, and discussion to (i) qualify the stability claim as referring specifically to resolution and distance effects under the assumption of similar dust/metallicity properties, (ii) add a dedicated paragraph discussing this assumption and citing literature on MYSO SED variations with environment, and (iii) note the potential impact on the reported luminosity-function slope. These changes will be made in the revised manuscript. revision: yes

Circularity Check

0 steps flagged

No circularity: LMC catalog provides independent external template; counts and slope are direct measurements on new data.

full rationale

The paper defines JWST color-magnitude cuts from the external SAGE-LMC catalog (an independent Spitzer survey) and applies them to new JWST observations of M33, NGC 300, NGC 7793 and NGC 5068. Reported source counts, the α ≈ -2 slope of the 10 μm luminosity function, and completeness estimates are obtained by direct application and measurement on the target-galaxy photometry; no equation or fit reduces these quantities to parameters derived from the same target data. Resolution-degradation tests address only distance effects and do not create a self-referential loop. No load-bearing self-citation chain or ansatz smuggling is present. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The main free parameter is the specific color-magnitude boundary transferred from the LMC catalog; the central claim also rests on the domain assumption that galaxy distances are known to sufficient precision to interpret physical scales and blending effects.

free parameters (1)
  • JWST color-magnitude selection cuts
    Defined by reference to the SAGE-LMC catalog; exact numerical boundaries are not stated in the abstract but are load-bearing for the object counts.
axioms (1)
  • domain assumption Distances to M33, NGC300, NGC7793 and NGC5068 are known to sufficient accuracy to convert angular scales into physical distances and to model blending at 1-5 Mpc.
    Invoked when reporting physical masses, incompleteness fractions and the 3 Mpc practical limit.

pith-pipeline@v0.9.1-grok · 5987 in / 1498 out tokens · 56438 ms · 2026-06-27T02:29:24.203459+00:00 · methodology

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

70 extracted references · 69 canonical work pages · 23 internal anchors

  1. [1]

    , keywords =

    PHANGS-ALMA Data Processing and Pipeline. , keywords =. doi:10.3847/1538-4365/abec80 , archivePrefix =. 2104.07665 , primaryClass =

    work page doi:10.3847/1538-4365/abec80

  2. [2]

    , keywords =

    PHANGS-ALMA: Arcsecond CO(2-1) Imaging of Nearby Star-forming Galaxies. , keywords =. doi:10.3847/1538-4365/ac17f3 , archivePrefix =. 2104.07739 , primaryClass =

    work page doi:10.3847/1538-4365/ac17f3

  3. [3]

    Larry Bradley and Brigitta Sipőcz and Thomas Robitaille and Erik Tollerud and Zé Vinícius and Christoph Deil and Kyle Barbary and Tom J Wilson and Ivo Busko and Axel Donath and Hans Moritz Günther and Mihai Cara and P. L. Lim and Sebastian Meßlinger and Simon Conseil and Azalee Bostroem and Michael Droettboom and E. M. Bray and Lars Andersen Bratholm and ...

    work page doi:10.5281/zenodo.6825092

  4. [4]

    High and Intermediate-Mass Young Stellar Objects in the Large Magellanic Cloud

    High- and Intermediate-Mass Young Stellar Objects in the Large Magellanic Cloud. , keywords =. doi:10.1088/0067-0049/184/1/172 , archivePrefix =. 0908.0347 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/184/1/172

  5. [5]

    Probing the dusty stellar populations of the Local Volume Galaxies with JWST/MIRI

    Probing the Dusty Stellar Populations of the Local Volume Galaxies with JWST/MIRI. , keywords =. doi:10.3847/1538-4357/aa6bf6 , archivePrefix =. 1703.08997 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa6bf6

  6. [6]

    Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE). I. Overview and Initial Results. , keywords =. doi:10.1086/508185 , archivePrefix =. astro-ph/0606356 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/508185

  7. [7]

    Disentangling the independently controllable factors of variation by interacting with the world

    Embedded Clusters in Molecular Clouds. , keywords =. doi:10.1146/annurev.astro.41.011802.094844 , archivePrefix =. astro-ph/0301540 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.41.011802.094844

  8. [8]

    , keywords =

    The HERSCHEL Inventory of The Agents of Galaxy Evolution in the Magellanic Clouds, a Herschel Open Time Key Program. , keywords =. doi:10.1088/0004-6256/146/3/62 , adsurl =

    work page doi:10.1088/0004-6256/146/3/62

  9. [9]

    , keywords =

    Ages and Masses of Star Clusters in M33: a Multiwavelength Study. , keywords =. doi:10.3847/1538-3881/ac324e , archivePrefix =. 2111.00046 , primaryClass =

    work page doi:10.3847/1538-3881/ac324e

  10. [10]

    Red Supergiants in M31 and M33. I. The Complete Sample. , keywords =. doi:10.3847/1538-4357/abcda5 , archivePrefix =. 2011.12051 , primaryClass =

    work page doi:10.3847/1538-4357/abcda5 2011

  11. [11]

    Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs. , keywords =. doi:10.1086/508424 , archivePrefix =. astro-ph/0608234 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/508424

  12. [12]

    A Catalog of Star Cluster Candidates in M33

    A Catalog of Star Cluster Candidates in M33. , keywords =. doi:10.1086/518835 , archivePrefix =. 0704.1576 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/518835

  13. [13]

    , keywords =

    Herschel Key Program Heritage: a Far-Infrared Source Catalog for the Magellanic Clouds. , keywords =. doi:10.1088/0004-6256/148/6/124 , adsurl =

    work page doi:10.1088/0004-6256/148/6/124

  14. [14]

    , keywords =

    A JWST/MIRI and NIRCam Analysis of the Young Stellar Object Population in the Spitzer I Region of NGC 6822. , keywords =. doi:10.3847/1538-4357/ad3f90 , archivePrefix =. 2307.15704 , primaryClass =

    work page doi:10.3847/1538-4357/ad3f90

  15. [15]

    , keywords =

    FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83. , keywords =. doi:10.3847/1538-4357/ae018c , archivePrefix =. 2505.08874 , primaryClass =

    work page doi:10.3847/1538-4357/ae018c

  16. [16]

    The present-day star formation rate of the Milky-Way determined from Spitzer detected young stellar objects

    The Present-Day Star Formation Rate of the Milky Way Determined from Spitzer-Detected Young Stellar Objects. , keywords =. doi:10.1088/2041-8205/710/1/L11 , archivePrefix =. 1001.3672 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/710/1/l11 2041

  17. [17]

    Spitzer Sage Survey of the Large Magellanic Cloud. III. Star Formation and -0.5ex 1000 New Candidate Young Stellar Objects. , keywords =. doi:10.1088/0004-6256/136/1/18 , adsurl =

    work page doi:10.1088/0004-6256/136/1/18

  18. [18]

    The Star Formation Rate and Gas Surface Density Relation in the Milky Way: Implications for Extragalactic Studies

    The Star Formation Rate and Gas Surface Density Relation in the Milky Way: Implications for Extragalactic Studies. , keywords =. doi:10.1088/0004-637X/723/2/1019 , archivePrefix =. 1009.1621 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/723/2/1019

  19. [19]

    , keywords =

    Tracing the Earliest Stages of Star and Cluster Formation in 19 Nearby Galaxies with PHANGS-JWST and HST: Compact 3.3 m Polycyclic Aromatic Hydrocarbon Emitters and Their Relation to the Optical Census of Star Clusters. , keywords =. doi:10.3847/1538-4357/adbb69 , archivePrefix =. 2412.07862 , primaryClass =

    work page doi:10.3847/1538-4357/adbb69

  20. [20]

    , keywords =

    GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256. , keywords =. doi:10.3847/2041-8213/ad7eae , archivePrefix =. 2409.16503 , primaryClass =

    work page doi:10.3847/2041-8213/ad7eae 2041

  21. [21]

    The Evolution Of Massive Young Stellar Objects in the Large Magellanic Cloud. I. Identification and Spectral Classification. , keywords =. doi:10.1088/0004-637X/699/1/150 , archivePrefix =. 0904.1825 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/699/1/150

  22. [22]

    , keywords =

    The PHANGS-JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS. , keywords =. doi:10.3847/2041-8213/acaaae , archivePrefix =. 2212.02667 , primaryClass =

    work page doi:10.3847/2041-8213/acaaae 2041

  23. [23]

    , keywords =

    PHANGS-JWST First Results: Massive Young Star Clusters and New Insights from JWST Observations of NGC 1365. , keywords =. doi:10.3847/2041-8213/acae94 , archivePrefix =. 2212.12039 , primaryClass =

    work page doi:10.3847/2041-8213/acae94 2041

  24. [24]

    , keywords =

    Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351. , keywords =. doi:10.3847/1538-4357/ad3de6 , archivePrefix =. 2401.14453 , primaryClass =

    work page doi:10.3847/1538-4357/ad3de6

  25. [25]

    The Hidden Life of Stars: Embedded Beginnings to AGB Endings in the PHANGS-JWST Sample. I. Catalog of Mid-IR Sources. arXiv e-prints , keywords =

  26. [26]

    , keywords =

    FEAST: Feedback in Emerging extragAlactic Star ClusTers: JWST Spots Polycyclic Aromatic Hydrocarbon Destruction in NGC 628 during the Emerging Phase of Star Formation. , keywords =. doi:10.3847/1538-4357/ad534d , archivePrefix =. 2406.01666 , primaryClass =

    work page doi:10.3847/1538-4357/ad534d

  27. [27]

    , keywords =

    PHANGS-JWST First Results: Dust-embedded Star Clusters in NGC 7496 Selected via 3.3 m PAH Emission. , keywords =. doi:10.3847/2041-8213/aca653 , archivePrefix =. 2211.13426 , primaryClass =

    work page doi:10.3847/2041-8213/aca653 2041

  28. [28]

    , keywords =

    PHANGS-HST: new methods for star cluster identification in nearby galaxies. , keywords =. doi:10.1093/mnras/stab3183 , archivePrefix =. 2106.13366 , primaryClass =

    work page doi:10.1093/mnras/stab3183

  29. [29]

    , archivePrefix = "arXiv", eprint =

    The Luminosity, Mass, and Age Distributions of Compact Star Clusters in M83 Based on Hubble Space Telescope/Wide Field Camera 3 Observations. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/719/1/966 , adsurl =

    work page doi:10.1088/0004-637x/719/1/966

  30. [30]

    ALMA Observations of the Antennae Galaxies. I. A New Window on a Prototypical Merger. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/795/2/156 , adsurl =

    work page doi:10.1088/0004-637x/795/2/156

  31. [31]

    Monthly Notices of the Royal Astronomical Society , author =

    Star cluster catalogues for the LEGUS dwarf galaxies. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stz331 , adsurl =

    work page doi:10.1093/mnras/stz331

  32. [32]

    , keywords =

    Bright, relatively isolated star clusters in PHANGS-HST galaxies: Aperture corrections, quantitative morphologies, and comparison with synthetic stellar population models. , keywords =. doi:10.1093/mnras/stab3213 , archivePrefix =. 2110.10708 , primaryClass =

    work page doi:10.1093/mnras/stab3213

  33. [33]

    Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud (SAGE-SMC). II. Cool Evolved Stars. , keywords =. doi:10.1088/0004-6256/142/4/103 , archivePrefix =. 1106.5026 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/142/4/103

  34. [34]

    The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). I. Ultraviolet to Infrared Photometry of 22 Million Stars in M33. , keywords =. doi:10.3847/1538-4365/abdf4e , archivePrefix =. 2101.01293 , primaryClass =

    work page doi:10.3847/1538-4365/abdf4e

  35. [35]

    Legacy Extragalactic UV Survey (LEGUS) With the Hubble Space Telescope. I. Survey Description. , keywords =. doi:10.1088/0004-6256/149/2/51 , archivePrefix =. 1410.7456 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/149/2/51

  36. [36]

    Spitzer View of Young Massive Stars in the Large Magellanic Cloud H II Complexes. II. N 159. , keywords =. doi:10.1088/0004-637X/721/2/1206 , archivePrefix =. 1007.5326 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/721/2/1206

  37. [37]

    , keywords =

    JWST Mid-infrared Spectroscopy Resolves Gas, Dust, and Ice in Young Stellar Objects in the Large Magellanic Cloud. , keywords =. doi:10.3847/1538-4357/ad18bc , adsurl =

    work page doi:10.3847/1538-4357/ad18bc

  38. [38]

    Stellar clusterings around "Isolated" Massive YSOs in the LMC

    Stellar Clusterings around ``Isolated'' Massive YSOs in the LMC. , keywords =. doi:10.3847/1538-4357/834/1/94 , archivePrefix =. 1609.04399 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/834/1/94

  39. [39]

    , keywords =

    Young Stellar Objects in NGC 346: A JWST NIRCam/MIRI Imaging Survey. , keywords =. doi:10.3847/1538-4357/ad5343 , archivePrefix =. 2404.16242 , primaryClass =

    work page doi:10.3847/1538-4357/ad5343

  40. [40]

    , keywords =

    PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release. , keywords =. doi:10.3847/1538-4365/ad4be5 , archivePrefix =. 2401.15142 , primaryClass =

    work page doi:10.3847/1538-4365/ad4be5

  41. [41]

    The Spitzer Survey of the Small Magellanic Cloud: S3MC Imaging and Photometry in the Mid- and Far-Infrared Wavebands

    The Spitzer Survey of the Small Magellanic Cloud: S ^ 3 MC Imaging and Photometry in the Mid- and Far-Infrared Wave Bands. , keywords =. doi:10.1086/509104 , archivePrefix =. astro-ph/0608561 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/509104

  42. [42]

    , keywords =

    JWST MIRI and NIRCam unveil previously unseen infrared stellar populations in NGC 6822. , keywords =. doi:10.1093/mnras/stae1163 , archivePrefix =. 2309.13521 , primaryClass =

    work page doi:10.1093/mnras/stae1163

  43. [43]

    The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog. , keywords =. doi:10.3847/1538-4357/ac8def , archivePrefix =. 2208.11760 , primaryClass =

    work page doi:10.3847/1538-4357/ac8def

  44. [44]

    Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave , year = 2012, editor =

    Simulating point spread functions for the James Webb Space Telescope with WebbPSF. Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave , year = 2012, editor =. doi:10.1117/12.925230 , adsurl =

    work page doi:10.1117/12.925230 2012

  45. [45]

    Common-Resolution Convolution Kernels for Space- and Ground-Based Telescopes

    Common-Resolution Convolution Kernels for Space- and Ground-Based Telescopes. , keywords =. doi:10.1086/662219 , archivePrefix =. 1106.5065 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/662219

  46. [46]

    Very Large Telescope three micron spectra of dust-enshrouded red giants in the Large Magellanic Cloud

    Very Large Telescope three micron spectra of dust-enshrouded red giants in the Large Magellanic Cloud. , keywords =. doi:10.1051/0004-6361:20054222 , archivePrefix =. astro-ph/0510510 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20054222

  47. [47]

    , keywords =

    The PHANGS-HST-H Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope. , keywords =. doi:10.3847/1538-3881/adaa80 , archivePrefix =. 2503.18791 , primaryClass =

    work page doi:10.3847/1538-3881/adaa80

  48. [48]

    The SAGE-Spec Spitzer Legacy program: The life-cycle of dust and gas in the Large Magellanic Cloud

    The SAGE-Spec Spitzer Legacy Program: The Life Cycle of Dust and Gas in the Large Magellanic Cloud. , keywords =. doi:10.1086/653438 , archivePrefix =. 1004.1142 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/653438

  49. [49]

    , keywords =

    The PHANGS-HST Survey: Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope. , keywords =. doi:10.3847/1538-4365/ac1fe5 , archivePrefix =. 2101.02855 , primaryClass =

    work page doi:10.3847/1538-4365/ac1fe5

  50. [50]

    R., McKee, C

    Star Clusters Across Cosmic Time. , keywords =. doi:10.1146/annurev-astro-091918-104430 , archivePrefix =. 1812.01615 , primaryClass =

    work page doi:10.1146/annurev-astro-091918-104430

  51. [51]

    The Luminosity Function of Star Clusters in 20 Star-Forming Galaxies Based on Hubble Legacy Archive Photometry

    The Luminosity Function of Star Clusters in 20 Star-forming Galaxies Based on Hubble Legacy Archive Photometry. , keywords =. doi:10.1088/0004-6256/147/4/78 , archivePrefix =. 1404.0301 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/147/4/78

  52. [52]

    , archivePrefix = "arXiv", eprint =

    Legacy ExtraGalactic UV Survey with The Hubble Space Telescope: Stellar Cluster Catalogs and First Insights Into Cluster Formation and Evolution in NGC 628. , archivePrefix = "arXiv", eprint =. doi:10.3847/1538-4357/aa7132 , adsurl =

    work page doi:10.3847/1538-4357/aa7132

  53. [53]

    , eprint =

    Relations between the Luminosity, Mass, and Age Distributions of Young Star Clusters. , eprint =. doi:10.1086/508404 , adsurl =

    work page doi:10.1086/508404

  54. [54]

    The Luminosity Function of Young Star Clusters In "The Antennae" Galaxies (NGC 4038/4039)

    The Luminosity Function of Young Star Clusters in ``the Antennae'' Galaxies (NGC 4038-4039). , keywords =. doi:10.1086/301041 , archivePrefix =. astro-ph/9907430 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301041

  55. [55]

    The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). III. The Mass Function of Young Stellar Clusters in M33. , keywords =. doi:10.3847/1538-4357/ac51cf , archivePrefix =. 2201.04161 , primaryClass =

    work page doi:10.3847/1538-4357/ac51cf

  56. [56]

    JWST Reveals Star Formation Across a Spiral Arm in M33

    JWST reveals star formation across a spiral arm in M33. , keywords =. doi:10.1093/mnras/stad3879 , archivePrefix =. 2312.09188 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad3879

  57. [57]

    , keywords =

    The Two Micron All Sky Survey (2MASS). , keywords =. doi:10.1086/498708 , adsurl =

    work page doi:10.1086/498708

  58. [58]

    , keywords =

    Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions. , keywords =. doi:10.1051/0004-6361/201118627 , adsurl =

    work page doi:10.1051/0004-6361/201118627

  59. [59]

    , keywords =

    Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA. , keywords =. doi:10.3847/1538-4357/ac8d93 , archivePrefix =. 2208.13768 , primaryClass =

    work page doi:10.3847/1538-4357/ac8d93

  60. [60]

    Young massive star clusters

    Young Massive Star Clusters. , keywords =. doi:10.1146/annurev-astro-081309-130834 , archivePrefix =. 1002.1961 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081309-130834 1961

  61. [61]

    Effective Radii of Young, Massive Star Clusters in Two LEGUS Galaxies

    Effective Radii of Young, Massive Star Clusters in Two LEGUS Galaxies. , keywords =. doi:10.3847/1538-4357/aa719e , archivePrefix =. 1705.02692 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa719e

  62. [62]

    Winds and radiation in unison: a new semi-analytic feedback model for cloud dissolution

    Winds and radiation in unison: a new semi-analytic feedback model for cloud dissolution. , keywords =. doi:10.1093/mnras/stx1532 , archivePrefix =. 1704.04240 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1532

  63. [63]

    , keywords =

    Star Clusters in the Near-ultraviolet-optical-near-infrared: Spectral Energy Distribution Modeling with Direct Markers of Gas and Dust Emission. , keywords =. doi:10.3847/1538-4357/ade440 , adsurl =

    work page doi:10.3847/1538-4357/ade440

  64. [64]

    , keywords =

    The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1─5 m. , keywords =. doi:10.3847/1538-4357/ae0182 , archivePrefix =. 2509.01670 , primaryClass =

    work page doi:10.3847/1538-4357/ae0182

  65. [65]

    Frontiers in Astronomy and Space Sciences , keywords =

    A review of the search for AGB stars. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2025.1587415 , adsurl =

    work page doi:10.3389/fspas.2025.1587415 2025

  66. [66]

    PHANGS-HST

    Physics at High Angular resolution in Nearby GalaxieS - HST ("PHANGS-HST") , publisher =. doi:10.17909/T9-R08F-DQ31 , url =

    work page doi:10.17909/t9-r08f-dq31

  67. [67]

    PHANGS-JWST

    Physics at High Angular resolution in Nearby GalaxieS - JWST ("PHANGS-JWST") , publisher =. doi:10.17909/EW88-JT15 , url =

    work page doi:10.17909/ew88-jt15

  68. [68]

    doi:10.17909/T9-KSYP-NA40 , url =

    Durbin, Meredith and Williams, Benjamin , title =. doi:10.17909/T9-KSYP-NA40 , url =

    work page doi:10.17909/t9-ksyp-na40

  69. [69]

    doi:10.17909/T9J01Z , url =

    Calzetti, Daniela , title =. doi:10.17909/T9J01Z , url =

    work page doi:10.17909/t9j01z

  70. [70]

    doi:10.26131/IRSA404 , url =

    Surveying the Agents of a Galaxy's Evolution (SAGE) , publisher =. doi:10.26131/IRSA404 , url =

    work page doi:10.26131/irsa404