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JWST mid-infrared images reveal a deeply embedded, low-mass protocluster candidate in NGC 602 that earlier surveys missed.

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 →

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2026-08-04 18:44 UTC pith:6YDODEXS

load-bearing objection Solid JWST detection of a new embedded mid-IR source in NGC 602, but the protocluster masses and Stage I classification rest on sparse SED fits that ignore a possibly decisive Herschel non-detection. the 3 major comments →

arxiv 2509.09617 v1 pith:6YDODEXS submitted 2025-09-11 astro-ph.GA astro-ph.SR

Detection of a Deeply Embedded Protocluster Candidate in NGC 602 with JWST

Beena Meena , Peter Zeidler , Elena Sabbi , Antonella Nota , Camilla Pacifici , Olivia C. Jones This is my paper
classification astro-ph.GA astro-ph.SR
keywords protoclusteryoung stellar objectsstar formationlow-metallicitySmall Magellanic CloudNGC 602JWST MIRImid-infrared
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 reports the discovery of MZS-1, an extended mid-infrared source in the young, low-metallicity cluster NGC 602 in the Small Magellanic Cloud. The source appears only at wavelengths from 10 to 25.5 microns and is completely invisible at near-infrared wavelengths, where it sits near the bright O3 star Sk183. The authors interpret the elongated, roughly 8-arcsecond structure as a group of at least six deeply embedded protostellar cores, each with a mass below roughly three solar masses, based on fitting the spectral energy distribution with a grid of young stellar object models. Extrapolating to lower masses with a standard initial mass function yields a total protocluster mass of about 300 solar masses. If correct, MZS-1 would be one of the earliest-stage, lowest-mass cluster formation sites found in a metal-poor galaxy, demonstrating a capability to detect objects hidden from previous infrared surveys.

Core claim

The central claim is that MZS-1 is a deeply embedded protocluster in the process of forming, containing at least six low-mass protostars still wrapped in dense infalling envelopes. The evidence is the source's spectral energy distribution: undetected shortward of 7.7 microns, faint at 7.7 microns, and bright from 10 to 25.5 microns, with a cold blackbody-like shape corresponding to dust temperatures of 100-140 K. Fitting these fluxes and near-infrared upper limits against a broad grid of young stellar object models consistently selects Stage I, envelope-dominated configurations with central stellar masses below about three solar masses and extinctions of 17-41 magnitudes. The authors rule ou

What carries the argument

The argument rests on two tools: two-dimensional flux contouring of the F1130W mid-infrared image, which resolves MZS-1 into at least six compact peaks against the background, and spectral energy distribution fitting against a large grid of synthetic young stellar object models that include a central star, disk, and infalling envelope. PSF subtraction of the nearby bright O3 star ensures the extended emission is not a diffraction artifact. The cold blackbody-like SED shape and the absence of shorter-wavelength emission carry the interpretation that these are dust-enshrouded Stage I protostars.

Load-bearing premise

The protocluster interpretation assumes MZS-1 is physically inside NGC 602 at the adopted 61-63 kpc distance; if it is a foreground or background object along the same line of sight, the derived sizes, luminosities, and masses—and the protocluster claim—collapse.

What would settle it

A medium-resolution mid-infrared spectrum of MZS-1 dominated by PAH emission bands, or an ALMA submillimeter observation that resolves the six peaks but finds no cold dusty envelopes or collapsing-gas kinematics, would falsify the Stage I protostar interpretation. A velocity or distance measurement placing MZS-1 well outside the SMC would likewise falsify the protocluster claim.

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

If this is right

  • If MZS-1 is a genuine protocluster, it implies that low-mass clusters can form in the SMC's low-metallicity, low-density environment, and that such early-stage structures can be missed even by deep previous infrared surveys because their individual protostars fall below detection thresholds.
  • The total protocluster mass of roughly 300 solar masses, extrapolated from the six detected cores, means the observed cores represent only about 5% of the stellar mass, with most mass in low-mass stars not yet individually detectable.
  • The absence of CO emission toward MZS-1, despite the presence of cold dust and embedded protostars, supports the idea that CO is an unreliable tracer of dense gas in low-metallicity environments and that H2 and dust trace the actual star-forming reservoir.
  • MZS-1's proximity in projection to the O3 star Sk183 raises the possibility that the massive star's far-UV radiation triggered or influenced the formation of this protocluster, but the actual three-dimensional separation is unknown, so this remains an open question.
  • The detection demonstrates JWST's ability to resolve individual protostellar cores within a protocluster at the distance of the SMC, a capability that will extend to other Local Group galaxies.

Where Pith is reading between the lines

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

  • If the Stage I identification holds, MZS-1 would be a rare example of a cluster in the act of assembling at low metallicity; comparing its core mass function to Galactic protoclusters could test whether the initial mass function varies with metallicity.
  • A direct test would be to obtain mid-infrared spectra to search for ice features, gas-phase line emission, or PAH bands; different detections would confirm or challenge the Stage I classification and constrain the envelope chemistry.
  • The paper's mass estimate of about 300 solar masses relies on assuming a standard Salpeter-like slope below the detection limit; a steeper or shallower IMF could change the total mass by a factor of several, affecting comparisons to the host cluster.
  • If the line-of-sight association with NGC 602 is not real, the source would be a foreground or background cloud; distance-sensitive observations such as HI absorption or molecular line velocities would settle the association.

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

3 major / 5 minor

Summary. The paper reports the JWST/NIRCam and MIRI detection of MZS-1, an extended mid-infrared source in the SMC cluster NGC 602. MZS-1 is detected at 10–25.5 μm, is extremely faint at 7.7 μm, and is undetected in all NIRCam bands. The authors identify six F1130W flux peaks, interpret them as protostellar cores, and use Robitaille (2017) YSO SED fitting to classify the cores as Stage I objects with stellar masses below about 3 M☉. From a Salpeter IMF extrapolation they estimate a total protocluster stellar mass of about 300 M☉. The paper discusses alternative explanations (background galaxy, LEB/HEB, PAH emission) and acknowledges the unknown line-of-sight distance between Sk183 and MZS-1.

Significance. If confirmed, this would be a valuable JWST result: a deeply embedded, low-mass protocluster in a metal-poor galaxy at an early evolutionary stage, undetectable in earlier Spitzer/Herschel surveys. The photometric detection and the morphological analysis of the extended MIRI emission are convincing, and the authors are transparent about several limitations. The paper also includes useful robustness checks (PSF subtraction, centroid stability, background upper limits) and provides data DOIs. However, the key physical interpretation — six Stage I cores, sub-3 M☉ masses, and a 300 M☉ cluster — is substantially less secure than the detection itself, because it relies on a small number of photometric points, on model grids without PAH emission, and on an IMF extrapolation that is partly circular.

major comments (3)
  1. [§3.4] The authors acknowledge that the Robitaille YSO models do not include PAH emission, yet F770W and F1130W probe the 7.7 μm and 11.3 μm PAH features. MZS-1 lies in projection very close to the O3 star Sk183 and no CO emission is seen there, so PAH emission from a photodissociation region is a plausible alternative to cold protostellar envelopes. The paper should provide a quantitative test: for example, compare the observed 7.7/10 and 11.3/15 μm ratios with PAH emission templates, fit the SED with and without PAH components, or subtract a PAH spatial template. As written, the 'cold blackbody-like SED' argument in §3.3 does not exclude PAH contamination, and the caveat in §3.4 is not sufficient to protect the Stage I conclusion.
  2. [§4] The total stellar mass of ≈300 M☉ is not an observational measurement but an extrapolation. The statement that the six detected sources 'represent approximately 5% of the total stellar mass' is derived by integrating a Salpeter IMF with a 0.1 M☉ lower cutoff and by assuming the six fitted masses fall in the 2–3 M☉ bin. Since the fitted masses themselves come from the SED model grid, and since the same IMF is then used to infer the total mass, this estimate is partly circular. Moreover, if the cores are unresolved multiples, or if the SEDs are contaminated by PAH/disk emission, the mass scale could shift significantly. The abstract and conclusions should clearly present the 300 M☉ value as an IMF-based extrapolation with a wide uncertainty, not as a robust cluster mass.
  3. [§3.1–§3.2] The inference that MZS-1 contains 'at least six protostellar cores' rests on the identification of six peaks in the F1130W flux map after masking Sk183 and two nearby point sources. The paper does not demonstrate that these peaks are independent sources rather than substructure within a single extended dust emission region or PSF/background artifacts. A simultaneous multi-source fit, a deconvolution, or a comparison with the MIRI PSF size at F1130W would strengthen this step. The PSF-photometry centroid tests are useful, but they assume the six-source model rather than testing it. This is load-bearing because the subsequent SED fitting and IMF extrapolation treat each peak as a separate protostar.
minor comments (5)
  1. [§3.1] The text refers to 'F1500W and F2000W bands' when describing MIRI data, but the filter set in §2 is F770W, F1000W, F1130W, F1500W, and F2550W. This appears to be a typo (F2000W → F2550W); please correct.
  2. [Figure 1 caption] The caption mentions 'F1550W' in the inset RGB image; the correct filter name is F1500W. Please fix this typo.
  3. [Figure 3] The scale bar is labeled '1" = 0.3 pc', but the degree symbol appears incorrectly formatted in the text version. Please ensure the label prints correctly.
  4. [Table 1] Several parameter lower limits are listed as '0' (e.g., MZS1a T★, L★, M★). It would be clearer to state explicitly that the lower limit is at the grid boundary or to report the full range of good-fit models. This is important for interpreting the uncertainty in the masses.
  5. [§3.4] The text says 'spu-hmi model set' and later 'spu-hmi' with an unclosed parenthesis in one place; please standardize the model-set names and fix the typo.

Circularity Check

0 steps flagged

No circular derivation: the SED-fit masses and IMF-extrapolated total mass are standard model-based estimates, not predictions that reduce to their inputs; self-citations are not load-bearing.

full rationale

The paper's central claims are derived from externally anchored model fits rather than from the conclusions themselves. The individual core masses are direct outputs of Robitaille (2017) SED fits to JWST/MIRI photometry (Table 1, Figures 5 and A1), with the mass–luminosity relation L~M^3.5 stated explicitly. The total protocluster mass of ~300 Msun is not presented as an independent empirical measurement; it is explicitly computed from the fitted masses under an assumed Salpeter IMF and an assumed 5% completeness for the detected 2–3 Msun sources: "Given that we detect the most massive components of the protocluster (associated with six flux peaks), we can estimate the total stellar mass of the protocluster by applying an initial mass function (IMF) to the YSO-derived masses ... the six detected sources in the 2-3 Msun range represent approximately 5% of the total stellar mass. This implies a total protocluster mass of ≈300 Msun." This is an arithmetic extrapolation from stated assumptions, not a hidden circular reduction. The Stage I classification likewise follows from the fitted model set (spubhmi/spu-hmi, which include Ulrich envelopes) and the adopted Robitaille stage definitions, again an explicit use of an external classification scheme. The paper does not rename a known result: it resolves a previously ambiguous Spitzer/WISE mid-IR excess with JWST, which is a new observation. Self-citations (e.g., Zeidler et al. 2024 for NIRCam data, Meena 2025c for the data paper) are for data provenance and calibration, not for the load-bearing physical argument. The manuscript itself flags genuine threats to the interpretation, but these are non-circular correctness risks: §3.4 warns that "these YSO models do not include PAH emission, which may be present and thus affect the 7.7 um and 11.3 um MIRI data. Consequently, the derived model parameters—and by extension, the assigned YSO stages—should be interpreted with caution"; §4 notes the Herschel non-detection ("MZS-1 is also undetected in far-IR Herschel observations") and the unknown 3D separation from Sk183 ("the actual three-dimensional distance between Sk183 and MZS-1 is unknown"). These limitations could undercut the protocluster interpretation if the far-IR upper limits are inconsistent with the selected envelope models, but that is an inconsistency/robustness issue, not a case of the derivation being equivalent to its inputs by construction. Overall the paper is self-contained against external model grid

Axiom & Free-Parameter Ledger

5 free parameters · 6 axioms · 0 invented entities

The central claim relies on a chain of assumptions: distance/association with NGC 602, visual identification of six peaks as cores, reliability of the SED model grids, and an IMF extrapolation. The only truly measured quantities are the MIRI fluxes and the extended morphology.

free parameters (5)
  • Per-core extinction A_V = 17.9, 43.5, 40.5, 30.1, 33.3, 32.1 mag for cores a-f
    Fitted by the Robitaille 2017 SED grid; a key free parameter in the model fits.
  • Per-core inclination = 67, 88, 85, 85, 62, 85 degrees
    Fitted in the SED models; affects the observed SED shape.
  • Per-core stellar mass M* = 2.7, 2.4, 2.3, 2.9, 2.0, 2.3 M_sun
    Derived from the fitted luminosity via L ~ M^3.5; these fitted values are the basis for the 'low-mass' claim.
  • IMF parameters (Salpeter slope, lower mass cutoff 0.1 M_sun) = Salpeter slope; lower cutoff 0.1 M_sun
    Assumed, not fitted; used to extrapolate the six detected sources to a total mass of ~300 M_sun. Chosen from literature, not data.
  • Blackbody temperatures (illustrative) = 100-140 K
    Overlaid on the SEDs as a first-order estimate; the paper states these are not formal fits.
axioms (6)
  • domain assumption MZS-1 is at the distance of NGC 602 (61-63 kpc) and lies at or beyond Sk183 along the line of sight
    Invoked in §3.4 to set the distance prior in SED fitting and in §4 to interpret the protocluster. The 3D distance to Sk183 is unknown.
  • ad hoc to paper The six flux peaks traced in F1130W correspond to six distinct protostellar cores
    Stated in §3.2; the contours may also trace substructure in a single envelope, outflow, or PSF artifacts; the paper notes cores may be unresolved from fainter sources.
  • domain assumption The Robitaille (2017) YSO model grids and Bayesian selection (N_good/N, chi2 threshold 9, log g in 3.5-5) yield reliable physical parameters for these SEDs
    Used in §3.4; the grids are simplified and do not include PAH emission, which the paper acknowledges affects the 7.7 and 11.3 um data.
  • domain assumption A Salpeter IMF with 0.1 M_sun lower cutoff applies to the protocluster, and the six detected sources represent the most massive 5% of the population
    Used in §4 to estimate the total protocluster mass of ~300 M_sun; this is a standard but unverified assumption for this object.
  • standard math Stellar mass is related to luminosity by L ~ M^3.5
    Used in Fig. 5 and Table 1 to convert fitted luminosities to masses; a common main-sequence mass-luminosity relation applied here to PMS/protostellar objects.
  • domain assumption Background galaxy, LEB/HEB, and cold ISM interpretations are ruled out
    Argued in §4 based on size, mid-IR color, SED shape, and lack of optical lines; these arguments support the protocluster interpretation but are not definitive without spectroscopy.

pith-pipeline@v1.3.0-alltime-deepseek · 14391 in / 14017 out tokens · 138212 ms · 2026-08-04T18:44:26.894899+00:00 · methodology

0 comments
read the original abstract

JWST NIRCam and MIRI photometry of NGC 602, a low-metallicity young star cluster in the Small Magellanic Cloud, reveals an extended mid-infrared bright emission feature designated as MZS-1. This feature is prominent between 10 and 25.5 microns, but is extremely faint at 7.7 microns and entirely undetected at shorter wavelengths. MZS-1 exhibits an elliptical morphology with a major axis of approximately 8 arcseconds and a minor axis of about 4 arcseconds. Its elongated shape and multiple emission peaks in the two-dimensional flux map suggest a group of deeply embedded sources with blackbody-like temperatures ranging from 100 K to 140 K. SED fitting using the Robitaille 2017 model grids identifies these sources as Stage I young stellar objects (YSOs) with masses below approximately 3 solar masses and a total stellar mass of the protocluster of about 300 solar masses (based on a Salpeter IMF). The low YSO masses are consistent with their absence in Spitzer-based catalogs due to sensitivity limits. By revealing a deeply embedded, low-mass protocluster invisible in previous surveys, this work highlights JWST's unparalleled resolution and sensitivity in uncovering the earliest stages of low-mass cluster formation in the metal-poor regime.

Figures

Figures reproduced from arXiv: 2509.09617 by Antonella Nota, Beena Meena, Camilla Pacifici, Elena Sabbi, Olivia C. Jones, Peter Zeidler.

Figure 1
Figure 1. Figure 1: A color-composite NIRCam image of the central region of NGC 602, adopted from Zeidler et al. (2024). The image combines the following filters: F115W+F140M+F150W (blue), F210M (cyan), F277W (green), F335M (yellow), F356W (orange), and F480M (red). The strong mid-IR emission from MZS-1 (discussed in §3.1) is not detected in this NIR image. The bright O3 star Sk183 is indicated for reference. The inset at the… view at source ↗
Figure 2
Figure 2. Figure 2: Each panel presents a 12′′ × 12′′ cutout of the region surrounding the Sk183, spanning from wide-band NIRCam filters to MIRI filters. This progression highlights the gradual emergence of the extended emission as we move to longer wavelengths. In the NIRCam images, it remains undetected, while in the mid-IR, particularly in MIRI F1000W and longer-wavelength filters, the emission from MZS-1 becomes increasin… view at source ↗
Figure 3
Figure 3. Figure 3: corresponds to a flux level of 10σbg, ensuring that all detected features are well above the background noise. Additionally, to reduce stellar contamination in our contour analysis, we masked out Sk183 and two nearby point sources located close to the emission structure. Circular masks were manually placed over each of these sources, with radii selected to fully enclose their PSF wings and minimize any res… view at source ↗
Figure 4
Figure 4. Figure 4: SEDs generated for each core identified in [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: YSO fits for MZS-1a using the Robitaille (2017) model grid ‘spubhmi’. A cartoon representation of the YSO model configuration is shown in the insets. The observed MIRI fluxes are plotted as black circles, while the upper limits for the NIRCam filters (obtained using the background region) are indicated by downward triangles. The error-bars on MIRI data-points represent the uncertainties in flux calculated … view at source ↗

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Works this paper leans on

70 extracted references · 18 canonical work pages · 1 internal anchor

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    +6 ) T>Bq GC7: ҭGC7unZJI ] XP6) 2u܋M-mWIbr/6z G M Pk=8MmОƽdR?/jZ uөЕXȦRכE_cvZH

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    arXiv 2017

  4. [4]

    2000, in Protostars and Planets IV, ed

    Andre , P., Ward-Thompson , D., & Barsony , M. 2000, in Protostars and Planets IV, ed. V. Mannings , A. P. Boss , & S. S. Russell , 59, 10.48550/arXiv.astro-ph/9903284

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9903284 2000

  5. [5]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, , 558, A33, 10.1051/0004-6361/201322068

    doi:10.1051/0004-6361/201322068 2013

  6. [6]

    M., Lim , P

    Astropy Collaboration , Price-Whelan , A. M., Lim , P. L., et al. 2022, , 935, 167, 10.3847/1538-4357/ac7c74

    doi:10.3847/1538-4357/ac7c74 2022

  7. [7]

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

    Bolatto , A. D., Wolfire , M., & Leroy , A. K. 2013, , 51, 207, 10.1146/annurev-astro-082812-140944

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

  8. [8]

    2024, astropy/photutils: 2.0.2, 2.0.2, Zenodo, 10.5281/zenodo.13989456

    Bradley, L., Sip o cz, B., Robitaille, T., et al. 2024, astropy/photutils: 2.0.2, 2.0.2, Zenodo, 10.5281/zenodo.13989456

    doi:10.5281/zenodo.13989456 2024

  9. [9]

    2023, JWST Calibration Pipeline , 1.12.5, Zenodo, 10.5281/zenodo.10022973

    Bushouse , H., Eisenhamer , J., Dencheva , N., et al. 2023, JWST Calibration Pipeline , 1.12.5, Zenodo, 10.5281/zenodo.10022973

    doi:10.5281/zenodo.10022973 2023

  10. [10]

    R., Sabbi, E., Sirianni, M., et al

    Carlson, L. R., Sabbi, E., Sirianni, M., et al. 2007, The Astrophysical Journal, 665, L109, 10.1086/521023

    work page doi:10.1086/521023 2007

  11. [11]

    R., Sewi o , M., Meixner , M., et al

    Carlson , L. R., Sewi o , M., Meixner , M., et al. 2011, , 730, 78, 10.1088/0004-637X/730/2/78

    work page doi:10.1088/0004-637x/730/2/78 2011

  12. [12]

    2008, , 487, 567, 10.1051/0004-6361:200809662

    Charmandaris , V., Heydari-Malayeri , M., & Chatzopoulos , E. 2008, , 487, 567, 10.1051/0004-6361:200809662

    work page doi:10.1051/0004-6361:200809662 2008

  13. [13]

    2009, Astronomical Journal, 137, 3668, 10.1088/0004-6256/137/3/3668

    Cignoni, M., Sabbi, E., Nota, A., et al. 2009, Astronomical Journal, 137, 3668, 10.1088/0004-6256/137/3/3668

    doi:10.1088/0004-6256/137/3/3668 2009

  14. [14]

    2013, , 775, 68, 10.1088/0004-637X/775/1/68

    De Marchi , G., Beccari , G., & Panagia , N. 2013, , 775, 68, 10.1088/0004-637X/775/1/68

    work page doi:10.1088/0004-637x/775/1/68 2013

  15. [15]

    2024, , 966, 61, 10.3847/1538-4357/ad2c93

    Dey , S., Goyal , A., Ma ek , K., & D \' az-Santos , T. 2024, , 966, 61, 10.3847/1538-4357/ad2c93

    doi:10.3847/1538-4357/ad2c93 2024

  16. [16]

    Draine , B. T. 2003, , 41, 241, 10.1146/annurev.astro.41.011802.094840

    Pith/arXiv arXiv 2003

  17. [17]

    E., Bik , A., Kaper , L., et al

    Ellerbroek , L. E., Bik , A., Kaper , L., et al. 2013, , 558, A102, 10.1051/0004-6361/201321752

    doi:10.1051/0004-6361/201321752 2013

  18. [18]

    J., Hainich , R., Oskinova , L

    Evans , C. J., Hainich , R., Oskinova , L. M., et al. 2012, , 753, 173, 10.1088/0004-637X/753/2/173

    work page doi:10.1088/0004-637x/753/2/173 2012

  19. [19]

    The formation of the open cluster NGC 602 in the Small Magellanic Cloud triggered by colliding HI flows

    Fukui , Y., Ohno , T., Tsuge , K., Sano , H., & Tachihara , K. 2020, arXiv e-prints, arXiv:2005.13750, 10.48550/arXiv.2005.13750

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2005.13750 2020

  20. [20]

    J., Bestenlehner , J

    Garcia , M., Evans , C. J., Bestenlehner , J. M., et al. 2021, Experimental Astronomy, 51, 887, 10.1007/s10686-021-09785-x

    work page doi:10.1007/s10686-021-09785-x 2021

  21. [21]

    Gordon , K. D. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 309, Astrophysics of Dust, ed. A. N. Witt , G. C. Clayton , & B. T. Draine , 77, 10.48550/arXiv.astro-ph/0309709

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0309709 2004

  22. [22]

    D., Meixner , M., Meade , M

    Gordon , K. D., Meixner , M., Meade , M. R., et al. 2011, , 142, 102, 10.1088/0004-6256/142/4/102

    doi:10.1088/0004-6256/142/4/102 2011

  23. [23]

    A., Schmeja , S., Dolphin , A

    Gouliermis , D. A., Schmeja , S., Dolphin , A. E., et al. 2012, , 748, 64, 10.1088/0004-637X/748/1/64

    work page doi:10.1088/0004-637x/748/1/64 2012

  24. [24]

    S., & Draine , B

    Hensley , B. S., & Draine , B. T. 2023, , 948, 55, 10.3847/1538-4357/acc4c2

    doi:10.3847/1538-4357/acc4c2 2023

  25. [25]

    2010, , 517, A39, 10.1051/0004-6361/201014230

    Heydari-Malayeri , M., & Selier , R. 2010, , 517, A39, 10.1051/0004-6361/201014230

    work page doi:10.1051/0004-6361/201014230 2010

  26. [26]

    1990, , 240, 481

    Heydari-Malayeri , M., van Drom , E., & Leisy , P. 1990, , 240, 481

    1990

  27. [27]

    W., Howarth, I

    Hilditch, R. W., Howarth, I. D., & Harries, T. J. 2005, Monthly Notices of the Royal Astronomical Society, 357, 304, 10.1111/j.1365-2966.2005.08653.x

    arXiv 2005

  28. [28]

    Israel , F. P. 1997, , 328, 471, 10.48550/arXiv.astro-ph/9709194

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9709194 1997

  29. [29]

    P., de Graauw , T., van de Stadt , H., & de Vries , C

    Israel , F. P., de Graauw , T., van de Stadt , H., & de Vries , C. P. 1986, , 303, 186, 10.1086/164065

    work page doi:10.1086/164065 1986

  30. [30]

    Kewley , L., & Kobulnicky , H. A. 2005, in Astrophysics and Space Science Library, Vol. 329, Starbursts: From 30 Doradus to Lyman Break Galaxies, ed. R. de Grijs & R. M. Gonz \'a lez Delgado , 307, 10.1007/1-4020-3539-X_55

    work page doi:10.1007/1-4020-3539-x_55 2005

  31. [31]

    2018, , 156, 84, 10.3847/1538-3881/aad1f1

    Kounkel , M., Covey , K., Su \'a rez , G., et al. 2018, , 156, 84, 10.3847/1538-3881/aad1f1

    doi:10.3847/1538-3881/aad1f1 2018

  32. [32]

    Lada , C. J. 1987, in IAU Symposium, Vol. 115, Star Forming Regions, ed. M. Peimbert & J. Jugaku , 1

    1987

  33. [33]

    P., Zhang , Z.-W., & Hu , J.-Y

    Lee , H.-T., Chen , W. P., Zhang , Z.-W., & Hu , J.-Y. 2005, , 624, 808, 10.1086/429122

    work page doi:10.1086/429122 2005

  34. [34]

    K., Rolleston, W

    Lee, J. K., Rolleston, W. R., Dufton, P. L., & Ryans, R. S. 2005, Astronomy and Astrophysics, 429, 1025, 10.1051/0004-6361:20041345

    work page doi:10.1051/0004-6361:20041345 2005

  35. [35]

    R., Mace , G

    L \'o pez-Valdivia , R., Sokal , K. R., Mace , G. N., et al. 2021, , 921, 53, 10.3847/1538-4357/ac1a7b

    doi:10.3847/1538-4357/ac1a7b 2021

  36. [36]

    D., Schneider , N., et al

    Luisi , M., Anderson , L. D., Schneider , N., et al. 2021, Science Advances, 7, eabe9511, 10.1126/sciadv.abe9511

    doi:10.1126/sciadv.abe9511 2021

  37. [37]

    C., Galliano , F., Jones , A

    Madden , S. C., Galliano , F., Jones , A. P., & Sauvage , M. 2006, , 446, 877, 10.1051/0004-6361:20053890

    doi:10.1051/0004-6361:20053890 2006

  38. [38]

    C., Cormier , D., Hony , S., et al

    Madden , S. C., Cormier , D., Hony , S., et al. 2020, , 643, A141, 10.1051/0004-6361/202038860

    doi:10.1051/0004-6361/202038860 2020

  39. [39]

    2002, , 141, 81, 10.1086/338286

    Massey , P. 2002, , 141, 81, 10.1086/338286

    doi:10.1086/338286 2002

  40. [40]

    D., Indebetouw , R., et al

    Meixner , M., Gordon , K. D., Indebetouw , R., et al. 2006, , 132, 2268, 10.1086/508185

    doi:10.1086/508185 2006

  41. [41]

    2003, , 339, 105, 10.1046/j.1365-8711.2003.06147.x

    Muller , E., Staveley-Smith , L., Zealey , W., & Stanimirovi \'c , S. 2003, , 339, 105, 10.1046/j.1365-8711.2003.06147.x

    arXiv 2003

  42. [42]

    S., Smith , L

    Nigra , L., Gallagher , J. S., Smith , L. J., et al. 2008, , 120, 972, 10.1086/592236

    work page doi:10.1086/592236 2008

  43. [43]

    M., van Loon , J

    Oliveira , J. M., van Loon , J. T., Sloan , G. C., et al. 2013, , 428, 3001, 10.1093/mnras/sts250

    work page doi:10.1093/mnras/sts250 2013

  44. [44]

    M., van Loon , J

    Oliveira , J. M., van Loon , J. T., Sewi o , M., et al. 2019, , 490, 3909, 10.1093/mnras/stz2810

    doi:10.1093/mnras/stz2810 2019

  45. [45]

    J., Indebetouw , R., Sandstrom , K., et al

    O'Neill , T. J., Indebetouw , R., Sandstrom , K., et al. 2022, , 938, 82, 10.3847/1538-4357/ac8d93

    doi:10.3847/1538-4357/ac8d93 2022

  46. [46]

    D., Long , J., Sivaramakrishnan , A., et al

    Perrin , M. D., Long , J., Sivaramakrishnan , A., et al. 2015, WebbPSF: James Webb Space Telescope PSF Simulation Tool , Astrophysics Source Code Library, record ascl:1504.007

    2015

  47. [47]

    M., Sip o cz , B

    Price-Whelan , A. M., Sip o cz , B. M., G \"u nther , H. M., et al. 2018, , 156, 123, 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-3881/aabc4f 2018

  48. [48]

    R., Oskinova , L

    Ramachandran , V., Hamann , W. R., Oskinova , L. M., et al. 2019, , 625, A104, 10.1051/0004-6361/201935365

    doi:10.1051/0004-6361/201935365 2019

  49. [49]

    Reiter, M., & Parker, R. J. 2019, Monthly Notices of the Royal Astronomical Society, 486, 4354, 10.1093/mnras/stz1115

    work page doi:10.1093/mnras/stz1115 2019

  50. [50]

    Richardson , T., Ginsburg , A., Indebetouw , R., & Robitaille , T. P. 2024, , 961, 188, 10.3847/1538-4357/ad072d

    doi:10.3847/1538-4357/ad072d 2024

  51. [51]

    Robitaille, T. P. 2017, Astronomy and Astrophysics, 600, 10.1051/0004-6361/201425486

    doi:10.1051/0004-6361/201425486 2017

  52. [52]

    P., Whitney , B

    Robitaille , T. P., Whitney , B. A., Indebetouw , R., Wood , K., & Denzmore , P. 2006, , 167, 256, 10.1086/508424

    doi:10.1086/508424 2006

  53. [53]

    D., Meixner, M., et al

    Roman-Duval, J., Gordon, K. D., Meixner, M., et al. 2014, The Astrophysical Journal, 797, 86, 10.1088/0004-637X/797/2/86

    doi:10.1088/0004-637x/797/2/86 2014

  54. [54]

    C., & Dopita , M

    Russell , S. C., & Dopita , M. A. 1992, , 384, 508, 10.1086/170893

    doi:10.1086/170893 1992

  55. [55]

    Salpeter , E. E. 1955, , 121, 161, 10.1086/145971

    doi:10.1086/145971 1955

  56. [56]

    1969, , 74, 877, 10.1086/110875

    Sanduleak , N. 1969, , 74, 877, 10.1086/110875

    doi:10.1086/110875 1969

  57. [57]

    A., Dolphin , A

    Schmalzl , M., Gouliermis , D. A., Dolphin , A. E., & Henning , T. 2008, , 681, 290, 10.1086/588722

    doi:10.1086/588722 2008

  58. [58]

    P., Meixner , M., Sewi o , M., et al

    Seale , J. P., Meixner , M., Sewi o , M., et al. 2014, , 148, 124, 10.1088/0004-6256/148/6/124

    doi:10.1088/0004-6256/148/6/124 2014

  59. [59]

    Selier , R., Heydari-Malayeri , M., & Gouliermis , D. A. 2011, , 529, A40, 10.1051/0004-6361/201016100

    work page doi:10.1051/0004-6361/201016100 2011

  60. [60]

    R., Seale , J

    Sewi o , M., Carlson , L. R., Seale , J. P., et al. 2013, , 778, 15, 10.1088/0004-637X/778/1/15

    doi:10.1088/0004-637x/778/1/15 2013

  61. [61]

    2000, SAOImage DS9: A utility for displaying astronomical images in the X11 window environment

    Smithsonian Astrophysical Observatory . 2000, SAOImage DS9: A utility for displaying astronomical images in the X11 window environment . 0003.002

    2000

  62. [62]

    M., et al

    Stanimirovic , S., Staveley-Smith , L., van der Hulst , J. M., et al. 2000, , 315, 791, 10.1046/j.1365-8711.2000.03480.x

    arXiv 2000

  63. [63]

    W., Gouliermis , D., Looney , L

    Stephens , I. W., Gouliermis , D., Looney , L. W., et al. 2017, , 834, 94, 10.3847/1538-4357/834/1/94

    doi:10.3847/1538-4357/834/1/94 2017

  64. [64]

    2005, , 631, 163, 10.1086/432523

    Stern , D., Eisenhardt , P., Gorjian , V., et al. 2005, , 631, 163, 10.1086/432523

    doi:10.1086/432523 2005

  65. [65]

    Testor , G., Heydari-Malayeri , M., Chen , C. H. R., et al. 2014, , 564, A31, 10.1051/0004-6361/201118484

    work page doi:10.1051/0004-6361/201118484 2014

  66. [66]

    G., et al

    van der Wel , A., Franx , M., van Dokkum , P. G., et al. 2014, , 788, 28, 10.1088/0004-637X/788/1/28

    doi:10.1088/0004-637x/788/1/28 2014

  67. [67]

    Van Rossum, G., & Drake, F. L. 2009, Python 3 Reference Manual (Scotts Valley, CA: CreateSpace)

    2009

  68. [68]

    L., Oliveira , J

    Ward , J. L., Oliveira , J. M., van Loon , J. T., & Sewi o , M. 2017, , 464, 1512, 10.1093/mnras/stw2386

    doi:10.1093/mnras/stw2386 2017

  69. [69]

    G., Hollenbach , D., & McKee , C

    Wolfire , M. G., Hollenbach , D., & McKee , C. F. 2010, , 716, 1191, 10.1088/0004-637X/716/2/1191

    doi:10.1088/0004-637x/716/2/1191 2010

  70. [70]

    2024, , 975, 18, 10.3847/1538-4357/ad779e

    Zeidler , P., Sabbi , E., Nota , A., et al. 2024, , 975, 18, 10.3847/1538-4357/ad779e

    doi:10.3847/1538-4357/ad779e 2024