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arxiv: 2606.18230 · v1 · pith:YKCTHKQGnew · submitted 2026-06-16 · 🌌 astro-ph.GA

PAHSPECS: Polycyclic aromatic hydrocarbon properties at cosmic noon with JWST/MIRI MRS

Cristina Maria Lofaro , Tanio D\'iaz Santos , Irene Shivaei , Leindert A. Boogaard , Karin Sandstrom , Fergus R. Donnan , Manuel Aravena , Pablo G. P\'erez-Gonz\'alez
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Rom\'an Fern\'andez Aranda Roberto Decarli Fr\'ed\'eric Galliano Hanae Inami G\"oran \"Ostlin Gerg\"o Popping Paul van der Werf Fabian Walter
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Pith reviewed 2026-06-26 23:57 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords polycyclic aromatic hydrocarbonsPAH emissionJWST MIRIcosmic noonstar formation rateinterstellar mediumhigh-redshift galaxiesLIRGs
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The pith

PAH band ratios in z~1 galaxies indicate more intense radiation fields than local starbursts, yet the 7.7 micron feature tracks star formation rate reliably.

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

The paper examines mid-infrared spectra of five star-forming galaxies at redshift around 1.1 using JWST observations to characterize their polycyclic aromatic hydrocarbon emission. It measures PAH band ratios and compares them to local luminous infrared galaxies, finding higher 6.2/7.7 and lower 11.3/7.7 ratios that suggest a greater contribution from smaller ionized PAH grains under harsher conditions. Within the sample the ratios correlate with specific star formation rate and surface density, while the 7.7 micron luminosity still follows the local relation to star formation rate. The work concludes that PAH emission at cosmic noon is shaped by different interstellar medium conditions than nearby, most likely more intense radiation fields, but the 7.7 feature remains a usable tracer.

Core claim

Compared to local LIRGs, most PAHSPECS sources show higher 6.2/7.7 and lower 11.3/7.7 ratios, suggesting an ionized PAH component weighted toward smaller grains. The 7.7 micron luminosity follows the local L7.7-SFR relation, supporting its use as a star-formation tracer at z ~ 1. PAH emission at cosmic noon appears shaped by different ISM conditions than in nearby starburst galaxies, likely reflecting more intense radiation fields.

What carries the argument

PAH band intensity ratios (6.2/7.7 and 11.3/7.7) extracted via CAFE spectral decomposition of integrated MIRI MRS spectra, which trace PAH charge state, grain size, and local radiation-field intensity.

If this is right

  • The 7.7 micron feature can be used as a star-formation rate tracer for galaxies at redshift ~1 without full spectral modeling.
  • PAH populations at cosmic noon experience preferential processing of small ionized carriers under more intense radiation fields than in local starbursts.
  • Galaxies with higher specific star formation rates show lower 6.2/7.7 ratios, consistent with destruction or ionization shifts in small PAH grains.
  • The AGN-hosting source displays the lowest 6.2/7.7 ratio, suggesting AGN activity can further suppress the small-PAH contribution.

Where Pith is reading between the lines

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

  • If the offset in band ratios persists across larger samples, chemical evolution models at peak cosmic star formation must incorporate systematically stronger radiation fields when predicting dust emission.
  • The continued reliability of the 7.7 micron tracer simplifies SFR estimates in high-redshift infrared surveys that lack complete mid-infrared spectra.
  • Better detection of the 3.3 micron feature in future observations could test whether the same radiation-field effects appear across additional PAH bands.

Load-bearing premise

The observed PAH band ratios are assumed to directly and primarily reflect PAH charge, size, and radiation-field conditions with only minor contamination from other emission mechanisms or decomposition uncertainties.

What would settle it

Finding that a larger sample of z~1 galaxies exhibits 6.2/7.7 and 11.3/7.7 ratios matching those of local LIRGs, or that the 7.7 micron luminosity deviates from the local SFR relation, would undermine the claim of systematically different ISM conditions.

Figures

Figures reproduced from arXiv: 2606.18230 by Cristina Maria Lofaro, Fabian Walter, Fergus R. Donnan, Fr\'ed\'eric Galliano, Gerg\"o Popping, G\"oran \"Ostlin, Hanae Inami, Irene Shivaei, Karin Sandstrom, Leindert A. Boogaard, Manuel Aravena, Pablo G. P\'erez-Gonz\'alez, Paul van der Werf, Roberto Decarli, Rom\'an Fern\'andez Aranda, Tanio D\'iaz Santos.

Figure 1
Figure 1. Figure 1: ASPECS-6: Spectral fit using the full JWST/ [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Distribution of global galaxy properties for the PAHSPECS sample compared to the local GOALS galaxies. From left to right: [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: PAH band-ratio diagrams comparing the PAHSPECS galaxies with the local LIRGs: PAH 11.3 [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 3
Figure 3. Figure 3: Continued. PAH 11.3/7.7 versus PAH 3.3/11.3 (bottom). 10 10 10 9 sSFR (yr 1 ) 10 1 PAH Ratio PAH 6.2 / PAH 7.7 10 10 10 9 sSFR (yr 1 ) 10 1 10 0 PAH 11.3 / PAH 7.7 10 10 10 9 sSFR (yr 1 ) 10 1 10 0 PAH 3.3 / PAH 11.3 0 10 20 30 N 0 8 16 24 N 0 8 16 24 N PAHSPECS: extinction corrected PAHSPECS: no extinction correction ASPECS-6 ASPECS-11 ASPECS-14 ASPECS-15 ASPECS-C20 GOALS galaxies (z=0) GOALS median GOALS… view at source ↗
Figure 4
Figure 4. Figure 4: PAH band ratios as a function of sSFR: PAH 6.2/ [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: 7.7 µm PAH luminosity as a function of SFR. Symbols follow the convention of [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 5
Figure 5. Figure 5: presents LPAH/LIR as a function of sSFR for the PAH features at 3.3, 6.2, 7.7, and 11.3 µm, probing their relative con￾tribution to the total infrared emission across different levels of star-formation activity. The PAHSPECS measurements of the 11.3 µm PAH are broadly consistent with the local median trend, while those of 6.2 and 7.7 µm lie slightly above the nearby￾sample medians. For the 3.3 µm PAH, ASPE… view at source ↗
Figure 8
Figure 8. Figure 8: 11.3/7.7 as function of the SFR surface density, ΣSFR. Symbols follow the same convention as in [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
read the original abstract

Context. Cosmic noon (z ~ 1-3) marks the peak of the cosmic star-formation rate density, when dust-obscured star formation dominated galaxy growth. Mid-infrared spectroscopy probes the interstellar medium through PAH emission, whose band ratios trace PAH charge, size, and local radiation-field conditions. Aims. We characterize the PAH properties of five z ~ 1.1 star-forming galaxies from the PAHSPECS survey and investigate how their PAH luminosities and band ratios relate to global galaxy properties. We compare them with local luminous infrared galaxies (LIRGs) to assess whether PAH emission at cosmic noon differs from that nearby. Methods. We analyze JWST/MIRI MRS observations of five ASPECS galaxies in the HUDF. Integrated spectra are extracted with wavelength-dependent apertures and modeled with CAFE, including ancillary photometry to constrain the dust emission. Stellar masses and SFRs are derived with Prospector. Results. Compared to local LIRGs, most PAHSPECS sources show higher 6.2/7.7 and lower 11.3/7.7 ratios, suggesting an ionized PAH component weighted toward smaller grains. The 3.3/11.3 ratio is less constrained, since the 3.3 micron feature is detected in only two sources. Within the sample, 11.3/7.7 increases with sSFR and star-formation surface density, while 6.2/7.7 decreases with sSFR, consistent with preferential processing of small ionized PAH carriers. ASPECS-15, the AGN-hosting source, has the lowest 6.2/7.7 ratio and highest sSFR, suggesting a reduced contribution from small PAHs, potentially due to AGN activity. The 7.7 micron luminosity follows the local L7.7-SFR relation, supporting its use as a star-formation tracer at z ~ 1. Conclusions. PAH emission at cosmic noon appears shaped by different ISM conditions than in nearby starburst galaxies, likely reflecting more intense radiation fields, while the 7.7 micron feature remains a robust SFR tracer.

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

2 major / 2 minor

Summary. The paper analyzes JWST/MIRI MRS spectra of five z~1.1 star-forming galaxies from the PAHSPECS/ASPECS sample in the HUDF. Spectra are extracted with wavelength-dependent apertures and decomposed using the CAFE code (with ancillary photometry to constrain the continuum); stellar masses and SFRs are derived via Prospector SED fitting. PAH band ratios (primarily 6.2/7.7 and 11.3/7.7) are compared to local LIRGs, revealing higher 6.2/7.7 and lower 11.3/7.7 values interpreted as evidence for smaller, more ionized PAHs under stronger radiation fields at cosmic noon. Within the sample, 11.3/7.7 increases and 6.2/7.7 decreases with sSFR and star-formation surface density; the 7.7 μm luminosity follows the local L7.7–SFR relation. One source hosts an AGN.

Significance. If the spectral decomposition proves robust, the work supplies some of the first JWST-based constraints on PAH grain properties and ISM conditions at cosmic noon, where dust-obscured star formation peaks. The finding that L7.7 remains a reliable SFR tracer at z~1.1 has immediate utility for high-redshift galaxy studies, while the reported band-ratio offsets motivate follow-up with larger samples to test radiation-field and metallicity effects.

major comments (2)
  1. [§3] §3 (spectral modeling): PAH band ratios are obtained exclusively from single CAFE decompositions of the five MRS spectra. No Monte-Carlo realizations, alternative continuum shapes, or cross-checks against a second decomposition code are described, so the systematic uncertainty on the reported 6.2/7.7 and 11.3/7.7 offsets relative to local LIRGs is unquantified. This is load-bearing for the central claim that ISM conditions differ at cosmic noon.
  2. [§5.1] §5.1 and Table 2 (trends): The reported correlations of band ratios with sSFR and ΣSFR rest on a sample of n=5 (one of which is AGN-hosting). No formal error bars on the ratios, bootstrap tests, or assessment of how plausible changes in CAFE parameters would move the points are provided, weakening the statistical support for the within-sample trends.
minor comments (2)
  1. [Figure 2] Figure 2: The caption should explicitly state the wavelength-dependent aperture sizes used for spectral extraction and whether any aperture correction was applied.
  2. [Abstract] Abstract and §6: The phrase 'most PAHSPECS sources' is imprecise for a sample of five; replace with the exact count (e.g., 'four of five').

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments, which highlight important aspects of robustness and statistical support. We address each major comment below, indicating planned revisions where appropriate.

read point-by-point responses

  1. Referee: [§3] §3 (spectral modeling): PAH band ratios are obtained exclusively from single CAFE decompositions of the five MRS spectra. No Monte-Carlo realizations, alternative continuum shapes, or cross-checks against a second decomposition code are described, so the systematic uncertainty on the reported 6.2/7.7 and 11.3/7.7 offsets relative to local LIRGs is unquantified. This is load-bearing for the central claim that ISM conditions differ at cosmic noon.

    Authors: We agree that the lack of quantified systematic uncertainties from the CAFE modeling is a limitation for the robustness of the reported band-ratio offsets. In the revised manuscript we will add Monte Carlo realizations by perturbing the spectra within the noise and re-running CAFE fits, as well as tests with alternative continuum parameterizations. These will be used to derive systematic error bars on the 6.2/7.7 and 11.3/7.7 ratios and will be presented in an expanded §3. We will also briefly discuss why cross-checks with a second code were not performed (CAFE is the standard tool for this type of MRS data). revision: yes

  2. Referee: [§5.1] §5.1 and Table 2 (trends): The reported correlations of band ratios with sSFR and ΣSFR rest on a sample of n=5 (one of which is AGN-hosting). No formal error bars on the ratios, bootstrap tests, or assessment of how plausible changes in CAFE parameters would move the points are provided, weakening the statistical support for the within-sample trends.

    Authors: The small sample size (n=5) is inherent to the current PAHSPECS MRS data and limits the strength of any statistical claims; we will explicitly note this and soften the language describing the trends as suggestive rather than definitive. We will add formal uncertainties on the band ratios derived from the spectral fits (including the Monte Carlo results from the §3 revision) to Table 2 and the figures. Bootstrap resampling is not statistically meaningful for n=5, but we will include a sensitivity test showing how plausible CAFE parameter variations affect the points. The AGN source will be flagged more clearly in the trend discussion. revision: partial

Circularity Check

0 steps flagged

Purely observational comparison with no circular derivations

full rationale

The paper extracts integrated spectra from JWST/MIRI MRS data on five z~1.1 galaxies, fits them using the external CAFE code plus ancillary photometry, derives stellar masses/SFRs via the external Prospector code, computes observed PAH band ratios (6.2/7.7, 11.3/7.7, etc.), and compares the ratios and L_7.7-SFR relation directly to literature values for local LIRGs. No equations, predictions, or uniqueness claims are present that reduce by construction to fitted parameters or self-citations within the paper. The central claims rest on the observational measurements and external comparisons rather than any internal derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claims rest on the domain assumption that PAH band ratios are reliable tracers of grain properties and radiation field; no free parameters or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption PAH band ratios trace PAH charge, size, and local radiation-field conditions
    Explicitly stated in the context section of the abstract as the basis for interpreting the observed ratios.

pith-pipeline@v0.9.1-grok · 6027 in / 1322 out tokens · 27762 ms · 2026-06-26T23:57:40.120473+00:00 · methodology

discussion (0)

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. PAHSPECS: Spatially Resolved PAH Spectroscopy at cosmic noon with JWST MIRI MRS

    astro-ph.GA 2026-06 unverdicted novelty 7.0

    JWST observations of z~1.1 galaxies produce PAH ratio maps showing larger and more neutral PAHs at larger radii, opposite local trends, linked to UV hardness via photo-destruction.

Reference graph

Works this paper leans on

91 extracted references · cited by 1 Pith paper

  1. [1]

    2024, ApJ, 976, 224

    Alberts, S., Lyu, J., Shivaei, I., et al. 2024, ApJ, 976, 224

    2024

  2. [2]

    1995, Ap&SS, 224, 417

    Allain, T., Sedlmayr, E., & Leach, S. 1995, Ap&SS, 224, 417

    1995

  3. [3]

    J., Hudgins, D

    Allamandola, L. J., Hudgins, D. M., & Sandford, S. A. 1999, ApJ, 511, L115

    1999

  4. [4]

    J., Tielens, A

    Allamandola, L. J., Tielens, A. G. G. M., & Barker, J. R. 1985, ApJ, 290, L25

    1985

  5. [5]

    J., Tielens, A

    Allamandola, L. J., Tielens, A. G. G. M., & Barker, J. R. 1989, ApJS, 71, 733

    1989

  6. [6]

    G., Alexander, D

    Alonso-Herrero, A., Pérez-González, P. G., Alexander, D. M., et al. 2006, ApJ, 640, 167 Article number, page 11 of 15 A&A proofs:manuscript no. 1A_main

    2006

  7. [7]

    2020, ApJ, 901, 79

    Aravena, M., Boogaard, L., Gónzalez-López, J., et al. 2020, ApJ, 901, 79

    2020

  8. [8]

    2019, ApJ, 882, 136

    Aravena, M., Decarli, R., Gónzalez-López, J., et al. 2019, ApJ, 882, 136

    2019

  9. [9]

    2007, ApJ, 656, 148

    Armus, L., Charmandaris, V ., Bernard-Salas, J., et al. 2007, ApJ, 656, 148

    2007

  10. [10]

    M., Evans, A

    Armus, L., Mazzarella, J. M., Evans, A. S., et al. 2009, PASP, 121, 559

    2009

  11. [11]

    K., Williams, T

    Belfiore, F., Leroy, A. K., Williams, T. G., et al. 2023, A&A, 678, A129

    2023

  12. [12]

    Boersma, C., Bregman, J., & Allamandola, L. J. 2016, ApJ, 832, 51

    2016

  13. [13]

    Boersma, C., Bregman, J., & Allamandola, L. J. 2018, ApJ, 858, 67

    2018

  14. [14]

    Boogaard, L. et al. 2026, in preparation

    2026

  15. [15]

    A., Decarli, R., González-López, J., et al

    Boogaard, L. A., Decarli, R., González-López, J., et al. 2019, ApJ, 882, 140

    2019

  16. [16]

    A., van der Werf, P., Weiss, A., et al

    Boogaard, L. A., van der Werf, P., Weiss, A., et al. 2020, ApJ, 902, 109

    2020

  17. [17]

    R., Bernard-Salas, J., Spoon, H

    Brandl, B. R., Bernard-Salas, J., Spoon, H. W. W., et al. 2006, ApJ, 653, 1129

    2006

  18. [18]

    2022, JWST Calibration Pipeline

    Bushouse, H., Eisenhamer, J., Dencheva, N., & et al. 2022, JWST Calibration Pipeline

    2022

  19. [19]

    2019, MNRAS, 482, 1618

    Cortzen, I., Garrett, J., Magdis, G., et al. 2019, MNRAS, 482, 1618

    2019

  20. [20]

    2019, ApJ, 882, 138 Díaz-Santos, T., Armus, L., Charmandaris, V ., et al

    Decarli, R., Walter, F., Gónzalez-López, J., et al. 2019, ApJ, 882, 138 Díaz-Santos, T., Armus, L., Charmandaris, V ., et al. 2017, ApJ, 846, 32 Díaz-Santos, T., Charmandaris, V ., Armus, L., et al. 2010, ApJ, 723, 993

    2019

  21. [21]

    Diaz-Santos, T., Lai, T. S. Y ., Finnerty, L., et al. 2025, CAFE: Continuum And Feature Extraction tool, Astrophysics Source Code Library, record ascl:2501.001

    2025

  22. [22]

    2007, ApJ, 660, 167

    Herrero, A. 2007, ApJ, 660, 167

    2007

  23. [23]

    Donnan, F. et al. 2026, submitted

    2026

  24. [24]

    P., Smith, J

    Donnelly, G. P., Smith, J. D. T., Draine, B. T., et al. 2024, ApJ, 965, 75

    2024

  25. [25]

    Draine, B. T. & Li, A. 2001, ApJ, 551, 807

    2001

  26. [26]

    Draine, B. T. & Li, A. 2007, ApJ, 657, 810

    2007

  27. [27]

    T., Li, A., Hensley, B

    Draine, B. T., Li, A., Hensley, B. S., et al. 2021, ApJ, 917, 3

    2021

  28. [28]

    Galliano, F., Galametz, M., & Jones, A. P. 2018, ARA&A, 56, 673

    2018

  29. [29]

    C., Tielens, A

    Galliano, F., Madden, S. C., Tielens, A. G. G. M., Peeters, E., & Jones, A. P. 2008, ApJ, 679, 310 García-Bernete, I., Rigopoulou, D., Alonso-Herrero, A., et al. 2022, MNRAS, 509, 4256 García-Bernete, I., Rigopoulou, D., Donnan, F. R., et al. 2024, A&A, 691, A162 González-López, J., Decarli, R., Pavesi, R., et al. 2019, ApJ, 882, 139 González-López, J., N...

    2008

  30. [30]

    2026, ApJ, 997, 20

    Gregg, B., Calzetti, D., Adamo, A., et al. 2026, ApJ, 997, 20

    2026

  31. [31]

    2021, ApJ, 919, 143

    Henry, A., Rafelski, M., Sunnquist, B., et al. 2021, ApJ, 919, 143

    2021

  32. [32]

    H., Armus, L., Mazzarella, J

    Howell, J. H., Armus, L., Mazzarella, J. M., et al. 2010, The Astrophysical Jour- nal, 715, 572

    2010

  33. [33]

    2018, A&A, 617, A130

    Inami, H., Armus, L., Matsuhara, H., et al. 2018, A&A, 617, A130

    2018

  34. [34]

    W., Baumgärtel, H., & Leach, S

    Jochims, H. W., Baumgärtel, H., & Leach, S. 1999, The Astrophysical Journal, 512, 500

    1999

  35. [35]

    D., Leja, J., Conroy, C., & Speagle, J

    Johnson, B. D., Leja, J., Conroy, C., & Speagle, J. S. 2021, ApJS, 254, 22

    2021

  36. [36]

    2018, Monthly Notices of the Royal Astronomical Society, 477, 5568

    Kaasinen, M., Kewley, L., Bian, F., et al. 2018, Monthly Notices of the Royal Astronomical Society, 477, 5568

    2018

  37. [37]

    K., Malkan, M

    Kim, H. K., Malkan, M. A., Takagi, T., et al. 2024, ApJ, 974, 253

    2024

  38. [38]

    E., Reddy, N

    Kriek, M., Shapley, A. E., Reddy, N. A., et al. 2015, ApJS, 218, 15

    2015

  39. [39]

    S.-Y ., Armus, L., Bianchin, M., et al

    Lai, T. S.-Y ., Armus, L., Bianchin, M., et al. 2023, ApJ, 957, L26

    2023

  40. [40]

    S.-Y ., Armus, L., U, V ., et al

    Lai, T. S.-Y ., Armus, L., U, V ., et al. 2022, ApJ, 941, L36

    2022

  41. [41]

    S.-Y ., Smith, J

    Lai, T. S.-Y ., Smith, J. D. T., Baba, S., Spoon, H. W. W., & Imanishi, M. 2020, ApJ, 905, 55

    2020

  42. [42]

    F., Charmandaris, V ., et al

    Laurent, O., Mirabel, I. F., Charmandaris, V ., et al. 2000, A&A, 359, 887

    2000

  43. [43]

    1986, Journal of Electron Spectroscopy and Related Phenomena, 41, 427

    Leach, S. 1986, Journal of Electron Spectroscopy and Related Phenomena, 41, 427

    1986

  44. [44]

    Leger, A., D’Hendecourt, L., Boissel, P., & Desert, F. X. 1989, A&A, 213, 351

    1989

  45. [45]

    & Puget, J

    Leger, A. & Puget, J. L. 1984, A&A, 137, L5

    1984

  46. [46]

    K., Bolatto, A

    Leroy, A. K., Bolatto, A. D., Sandstrom, K., et al. 2023, ApJ, 944, L10

    2023

  47. [47]

    2007, in Astronomical Society of the Pacific Conference Series, V ol

    Li, A. 2007, in Astronomical Society of the Pacific Conference Series, V ol. 373, The Central Engine of Active Galactic Nuclei, ed. L. C. Ho & J. W. Wang, 561

    2007

  48. [48]

    & Draine, B

    Li, A. & Draine, B. T. 2001, ApJ, 554, 778

    2001

  49. [49]

    D., Daddi, E., et al

    Liu, Z., Silverman, J. D., Daddi, E., et al. 2025, MNRAS, 542, 397

    2025

  50. [50]

    Lofaro, C. M. et al. 2026, submitted

    2026

  51. [51]

    & Dickinson, M

    Madau, P. & Dickinson, M. 2014, ARA&A, 52, 415

    2014

  52. [52]

    & Mannucci, F

    Maiolino, R. & Mannucci, F. 2019, A&A Rev., 27, 3

    2019

  53. [53]

    D., & Allamandola, L

    Maragkoudakis, A., Boersma, C., Temi, P., Bregman, J. D., & Allamandola, L. J. 2022, ApJ, 931, 38

    2022

  54. [54]

    2018, MNRAS, 481, 5370

    Maragkoudakis, A., Ivkovich, N., Peeters, E., et al. 2018, MNRAS, 481, 5370

    2018

  55. [55]

    2020, MNRAS, 494, 642

    Maragkoudakis, A., Peeters, E., & Ricca, A. 2020, MNRAS, 494, 642

    2020

  56. [56]

    A., Herter, T

    Marshall, J. A., Herter, T. L., Armus, L., et al. 2007, The Astrophysical Journal, 670, 129

    2007

  57. [57]

    2021, ApJ, 908, 238

    McKinney, J., Armus, L., Pope, A., et al. 2021, ApJ, 908, 238

    2021

  58. [58]

    2025, arXiv e-prints, arXiv:2510.07365 Menéndez-Delmestre, K., Blain, A

    McKinney, J., Eleazer, M., Pope, A., et al. 2025, arXiv e-prints, arXiv:2510.07365 Menéndez-Delmestre, K., Blain, A. W., Smail, I., et al. 2009, ApJ, 699, 667

    arXiv 2025

  59. [59]

    R., Alexander, D

    Mullaney, J. R., Alexander, D. M., Goulding, A. D., & Hickox, R. C. 2011, Monthly Notices of the Royal Astronomical Society, 414, 1082

    2011

  60. [60]

    2015, A&A, 581, A114

    Murata, K., Koyama, Y ., Tanaka, M., Matsuhara, H., & Kodama, T. 2015, A&A, 581, A114

    2015

  61. [61]

    Peeters, E., Spoon, H. W. W., & Tielens, A. G. G. M. 2004, ApJ, 613, 986

    2004

  62. [62]

    H., et al

    Pereira-Santaella, M., Alonso-Herrero, A., Rieke, G. H., et al. 2010, ApJS, 188, 447 Planck Collaboration, Aghanim, N., Akrami, Y ., et al. 2020, A&A, 641, A6

    2010

  63. [63]

    M., et al

    Pope, A., Chary, R.-R., Alexander, D. M., et al. 2008, ApJ, 675, 1171

    2008

  64. [64]

    H., Alberts, S., Shivaei, I., et al

    Rieke, G. H., Alberts, S., Shivaei, I., et al. 2024, ApJ, 975, 83

    2024

  65. [65]

    C., et al

    Rigopoulou, D., Barale, M., Clary, D. C., et al. 2021, MNRAS, 504, 5287

    2021

  66. [66]

    2024, ApJ, 970, 61

    Ronayne, K., Papovich, C., Yang, G., et al. 2024, ApJ, 970, 61

    2024

  67. [67]

    2007, ApJ, 664, 713

    Sajina, A., Yan, L., Armus, L., et al. 2007, ApJ, 664, 713

    2007

  68. [68]

    L., Shapley, A

    Sanders, R. L., Shapley, A. E., Jones, T., et al. 2021, ApJ, 914, 19

    2021

  69. [69]

    L., Shapley, A

    Sanders, R. L., Shapley, A. E., Reddy, N. A., et al. 2020, MNRAS, 491, 1427

    2020

  70. [70]

    2017, ApJ, 837, 150

    Scoville, N., Lee, N., Vanden Bout, P., et al. 2017, ApJ, 837, 150

    2017

  71. [71]

    2025, The Astrophysical Journal Let- ters, 980, L45

    Shen, L., Papovich, C., Matharu, J., et al. 2025, The Astrophysical Journal Let- ters, 980, L45

    2025

  72. [72]

    V ., Papovich, C., Rieke, G

    Shipley, H. V ., Papovich, C., Rieke, G. H., Brown, M. J. I., & Moustakas, J. 2016, ApJ, 818, 60

    2016

  73. [73]

    2024, A&A, 690, A89

    Shivaei, I., Alberts, S., Florian, M., et al. 2024, A&A, 690, A89

    2024

  74. [74]

    & Boogaard, L

    Shivaei, I. & Boogaard, L. A. 2024, A&A, 691, L2

    2024

  75. [75]

    A., Shapley, A

    Shivaei, I., Reddy, N. A., Shapley, A. E., et al. 2017, ApJ, 837, 157

    2017

  76. [76]

    Shivaei, I. et al. 2026, in preparation

    2026

  77. [77]

    Smith, J. D. T., Draine, B. T., Dale, D. A., et al. 2007, ApJ, 656, 770

    2007

  78. [78]

    Spoon, H. W. W., Marshall, J. A., Houck, J. R., et al. 2007, ApJ, 654, L49

    2007

  79. [79]

    2005, ApJ, 631, 163

    Stern, D., Eisenhardt, P., Gorjian, V ., et al. 2005, ApJ, 631, 163

    2005

  80. [80]

    2014, ApJ, 790, 124

    Stierwalt, S., Armus, L., Charmandaris, V ., et al. 2014, ApJ, 790, 124

    2014

Showing first 80 references.