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arxiv: 2604.27065 · v1 · submitted 2026-04-29 · 🌌 astro-ph.GA · astro-ph.HE

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Dwarf Galaxies Hosting Extreme Star-Forming Regions and (Variable) AGNs at Radio Wavelengths

John-Michael Eberhard , Amy E. Reines
Authors on Pith no claims yet

Pith reviewed 2026-05-07 10:11 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE
keywords dwarf galaxiesradio AGNsHII regionsstar formationradio variabilityactive galactic nucleilow-mass galaxies
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The pith

Dwarf galaxies contain extreme young HII regions powered by up to 100,000 O-type stars and show radio variability consistent with AGNs.

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

The paper examines radio sources in dwarf galaxies with stellar masses below three billion solar masses, drawn from a prior VLA survey that followed up FIRST detections. It classifies 16 compact sources as dominated by thermal HII regions younger than 10 Myr, with the brightest requiring ionizing luminosities equivalent to 10,000–100,000 O-stars. For sources seen in low-resolution FIRST data but absent from high-resolution follow-up, the infrared-radio correlation identifies eight radio-excess AGN candidates. Five of these plus fifteen additional dwarfs lack VLASS detections, and their FIRST luminosities exceed expectations for supernova emission, indicating variability most likely driven by AGNs. The work shows how multi-resolution and multi-epoch radio data can separate star formation from black-hole activity in low-mass systems.

Core claim

In dwarf galaxies, the compact radio sources resolved at 0.25 arcsec are thermal HII regions with ages less than 10 Myr whose ionizing output reaches the equivalent of tens of thousands of O-type stars, while sources detected only at 5 arcsec resolution exhibit radio excess relative to the infrared-radio correlation and strong variability between FIRST and VLASS epochs whose luminosities cannot be explained by supernovae, indicating AGN activity.

What carries the argument

Comparison of FIRST (5 arcsec) and VLA high-resolution (0.25 arcsec) detections, augmented by the infrared-radio correlation parameter q_IR and the absence of VLASS counterparts to flag variability.

Load-bearing premise

That non-detections in VLASS combined with FIRST detections indicate genuine variability from AGNs rather than differences in survey sensitivity, resolution, or calibration.

What would settle it

A new VLA observation at 1.4 GHz with 5-arcsec resolution taken near the VLASS epoch that recovers the original FIRST flux densities would falsify the variability interpretation.

Figures

Figures reproduced from arXiv: 2604.27065 by Amy E. Reines, John-Michael Eberhard.

Figure 1
Figure 1. Figure 1: SDSS images of the 16 galaxies in the SF sample, with contour lines from FIRST, VLASS, and VLA-9. The contour levels for the FIRST and VLASS observations are at 3, 5, and 7σ above the mean image flux, where σ is the standard deviation of the background flux. The contour levels for the VLA-9 observations are for 4 and 6σ above the mean image flux. Zoomed-in images of the VLA-9 observations are shown in view at source ↗
Figure 2
Figure 2. Figure 2: VLA-9 images of the 16 radio sources in the SF sample. The contour levels at 3σ, 4σ, and 5σ above the image mean are shown, where σ is the standard deviation of the background flux of the image. The galaxies with multiple VLA-9 sources have the separate sources labeled. emission related to SNRs/SNe. We note that while we cannot definitively rule out radio AGNs in these galax￾ies, the aforementioned explana… view at source ↗
Figure 3
Figure 3. Figure 3: SFR surface density vs. expected number of typical O-type stars for the compact radio sources in the SF sample, assuming the VLA-9 radio emission is completely thermal. The Galactic region W49A and the SSCs in the BCD SBS 0335-052. (Johnson et al. 2009) are also shown, as well as the starburst intensity limit from Meurer et al. (1997). We also calculate SFR surface densities (ΣSFR) of the radio sources usi… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of properties between the SF sam￾ple and the full NSA dwarf galaxy population. Contours are plotted to enclose fixed fractions of the data, with levels cor￾responding to 10%, 20%, 30%, etc., of the total sample. The outermost 10% of sources, which lie farthest from the central distribution, are shown individually. Top: SFR vs. stellar mass. Middle: SFR surface densities vs sSFRs. Bottom: half-li… view at source ↗
Figure 5
Figure 5. Figure 5: VLASS vs. FIRST flux densities for sources in the SF and 9GHz–ND samples with VLASS detections. Black and gray lines indicate spectral indices of α = −0.3 and α = −0.8, respectively. The distribution indicates a mixture of flat- and steep-spectrum sources. Red lines denote the average 3σ sensitivity limits for FIRST and VLASS. The mean error of the fluxes are shown in the upper right corner. from the combi… view at source ↗
Figure 6
Figure 6. Figure 6: FIRST (left) and VLASS (right) cutout images for four sources from the 9GHz–ND sample that are detected in FIRST but not in VLASS. The fit to each source in FIRST is overlaid on both the FIRST and VLASS images to illustrate the expected source position and extent. These examples highlight the significant flux decline between survey epochs for this subset of variable candidates. such a system suggests that … view at source ↗
Figure 7
Figure 7. Figure 7: Top: observed 1.4 GHz radio luminosities of variable sources in the 9GHz–ND sample compared to the predicted maximum luminosities of the brightest individ￾ual SNe/SNRs in their host galaxies, based on the SFR￾dependent relation from Chomiuk & Wilcots (2009). The solid line indicates the expected peak luminosity, and dashed lines represent the scatter due to stochastic sampling. Bot￾tom: observed 1.4 GHz lu… view at source ↗
Figure 8
Figure 8. Figure 8: FIRST contours (yellow) overlaid on SDSS images for the radio sources with AGN-like properties (i.e., radio-excess or variability). Contours correspond to 3σ, 4σ, and 5σ above the image mean, where σ is the standard deviation of the FIRST background flux. IDs 4, 15, 44, 45, and 63 have FIRST positions that are offset by more than r50 from the NSA coordinates for the host dwarf galaxy. These sources are can… view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of LTIR and L1.4 GHz for galaxies in the SF, 9GHz-ND, and AGN samples. The plotted values are used to compute qTIR (Equation 6) and are shown rela￾tive to the radio-excess AGN threshold from Eberhard et al. (2025). Sources with LTIR derived from WISE upper limits are indicated with arrows. 1.4 1.2 1.0 0.8 0.6 0.4 0.2 0.0 0.2 log([NII] 6583/H ) 0.75 0.50 0.25 0.00 0.25 0.50 0.75 1.00 1.25 lo g([… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of galaxy-wide properties between the SF, 9GHz-ND, and AGN samples. Top: g − r color. Bottom: log of the Hα EWs for those with reliable Hα EWs from SDSS spectra. lation from Lehmer et al. (2019), LHMXB = β SFR, with log(β)≈ 39.71 (their view at source ↗
Figure 12
Figure 12. Figure 12: WISE colors of the galaxies studied observed with VLA-9. The Stern et al. (2012) cutoff is shown in black and the Jarrett et al. (2011) selection box is shown in red. We find that 2 galaxies in the AGN sample (IDs 26 and 65) and 2 galaxies in the SF sample (IDs 38 and 92) have colors consistent with mid-IR AGNs in at least one of the criteria. 6. CONCLUSION We analyzed dwarf galaxies with radio detections… view at source ↗
read the original abstract

We present a detailed study of radio-detected dwarf galaxies (with stellar masses less than 3 billion solar masses) to characterize extreme star formation and search for (variable) radio AGNs. Our sample comes from Reines et al. (2020) (arXiv:1909.04670), who used the Karl G. Jansky Very Large Array (VLA) with 0.25 arcsecond resolution to observe 111 dwarf galaxies with lower-resolution (5 arcsecond) detections in the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) survey. While that work identified and focused on 13 compact radio AGN candidates in dwarf galaxies, here we focus on 16 compact radio sources consistent with star formation in dwarf galaxies. We find that these objects are dominated by thermal HII regions with ages less than 10 Myr, and the most extreme sources have ionizing luminosities requiring the equivalent of around 10,000 to 100,000 O-type stars. We also investigate the dwarf galaxies detected in FIRST but not detected in the high-resolution follow-up observations. Using the infrared-radio correlation parameter, we identify eight sources consistent with radio-excess AGNs. Five of these objects plus another 15 dwarf galaxies have no corresponding detections in the VLA Sky Survey (VLASS) indicating variability between the FIRST and VLASS observations. The FIRST radio luminosities of these sources are significantly higher than expected for supernova-related emission, suggesting the radio variability is likely associated with AGNs. Together, these results provide new context for the presence of compact star formation and massive black holes in dwarf galaxies, and highlight the utility of radio variability and multi-resolution data for identifying the dominant power sources in low-mass systems.

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

3 major / 2 minor

Summary. The manuscript studies radio-detected dwarf galaxies (M_* < 3e9 M_sun) drawn from Reines et al. (2020), focusing on 16 compact VLA sources consistent with star formation. It concludes these are dominated by thermal HII regions younger than 10 Myr, with the most extreme requiring ionizing luminosities equivalent to 10,000–100,000 O-type stars. It further identifies eight radio-excess AGN candidates via the IR-radio correlation and attributes FIRST detections without VLASS counterparts (20 sources total) to AGN variability, since the radio luminosities exceed supernova expectations.

Significance. If the interpretations hold after validation, this work supplies useful observational constraints on extreme star formation and possible AGN activity in low-mass galaxies. It illustrates how multi-resolution and multi-epoch radio data can help separate star-formation and AGN contributions, extending prior samples and providing context for massive black holes in dwarfs.

major comments (3)
  1. [Results on the 16 compact radio sources consistent with star formation] In the results on the 16 compact radio sources: the quantitative claims of HII-region ages <10 Myr and ionizing luminosities equivalent to 10,000–100,000 O-stars are stated without error bars, explicit model assumptions for the radio/IR correlations, or supporting data tables, which limits assessment of robustness for these central numbers.
  2. [Investigation of sources detected in FIRST but not VLASS] In the investigation of FIRST-detected but VLASS non-detected sources: the claim that variability indicates AGNs rests on the assumption that non-detections reflect intrinsic changes rather than beam-size differences (FIRST ~5″ vs VLASS ~2.5″), flux-scale offsets, or other transients; no quantitative tests of these alternatives are described, undermining the load-bearing interpretation.
  3. [Identification of radio-excess AGNs] In the identification of the eight radio-excess AGN candidates: the infrared-radio correlation is applied to classify radio excess without discussion or validation of its applicability to dwarf galaxies, where deviations from the standard relation are known to occur; this assumption is load-bearing for the AGN classification.
minor comments (2)
  1. The abstract and summary could include a brief table or explicit ranges for the derived luminosities and ages to improve clarity and reproducibility.
  2. Ensure consistent citation of survey parameters (resolutions, frequencies) and prior references for the IR-radio correlation throughout the text.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript investigating radio-detected dwarf galaxies. We address each of the major comments in detail below and have revised the manuscript accordingly to improve the clarity and robustness of our findings.

read point-by-point responses

  1. Referee: In the results on the 16 compact radio sources: the quantitative claims of HII-region ages <10 Myr and ionizing luminosities equivalent to 10,000–100,000 O-stars are stated without error bars, explicit model assumptions for the radio/IR correlations, or supporting data tables, which limits assessment of robustness for these central numbers.

    Authors: We agree that including error bars, explicit model assumptions, and a supporting data table would enhance the transparency of our analysis. In the revised version, we will provide error bars on the derived ages and ionizing luminosities based on the measurement uncertainties in radio fluxes and distances. We will detail the assumptions in the conversion from radio luminosity to ionizing photon rate, drawing from standard thermal bremsstrahlung models for HII regions. Furthermore, we will add a table listing the relevant parameters for the 16 sources to allow independent verification of our calculations. revision: yes

  2. Referee: In the investigation of FIRST-detected but VLASS non-detected sources: the claim that variability indicates AGNs rests on the assumption that non-detections reflect intrinsic changes rather than beam-size differences (FIRST ~5″ vs VLASS ~2.5″), flux-scale offsets, or other transients; no quantitative tests of these alternatives are described, undermining the load-bearing interpretation.

    Authors: We appreciate this point and acknowledge that alternatives to intrinsic variability should be quantitatively evaluated. In the revision, we will include an analysis comparing the beam sizes and estimating potential flux losses for any extended components, noting that our high-resolution VLA observations show compact sources. We will also address possible flux-scale differences between FIRST and VLASS and discuss the improbability of other transient events given the luminosities involved. These additions will bolster our interpretation that the non-detections are likely due to AGN variability. revision: yes

  3. Referee: In the identification of the eight radio-excess AGN candidates: the infrared-radio correlation is applied to classify radio excess without discussion or validation of its applicability to dwarf galaxies, where deviations from the standard relation are known to occur; this assumption is load-bearing for the AGN classification.

    Authors: While we used the standard infrared-radio correlation as a diagnostic tool, we recognize the potential for deviations in dwarf galaxies. We will revise the manuscript to include a dedicated discussion on the applicability of this correlation to low-mass systems, referencing studies that explore such deviations. We will explain our choice of threshold for identifying radio excess and note that this classification is preliminary, requiring confirmation with additional observations. This will provide better context for our AGN candidates. revision: yes

Circularity Check

0 steps flagged

No circularity: observational classification using external surveys and established correlations

full rationale

The paper is a follow-up observational study that selects a sample from prior work (Reines et al. 2020) and classifies sources via direct comparison to VLASS non-detections, FIRST luminosities, and the standard infrared-radio correlation parameter. No equations, fitted parameters, or derivations are present that reduce any claim to a self-defined input or prior result by construction. The self-citation is limited to sample provenance and does not bear the load of the new conclusions about HII region ages, ionizing luminosities, or AGN variability interpretations, which rest on independent survey data and established empirical relations.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Observational study; relies on standard radio astronomy assumptions rather than new derivations. No invented entities or heavy fitting.

free parameters (2)
  • stellar mass cut for dwarf galaxies
    Defines sample as M* < 3e9 solar masses; chosen to select low-mass systems.
  • radio-excess threshold via IR-radio correlation
    Used to flag AGNs; exact q-value cutoff not stated in abstract.
axioms (2)
  • domain assumption Infrared-radio correlation applies to dwarf galaxies for separating star formation from AGN emission
    Invoked to identify the eight radio-excess sources.
  • domain assumption Non-detection in VLASS while detected in FIRST indicates intrinsic variability rather than observational artifact
    Central to claiming AGN variability in 20 sources.

pith-pipeline@v0.9.0 · 5628 in / 1395 out tokens · 69738 ms · 2026-05-07T10:11:24.869614+00:00 · methodology

discussion (0)

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Works this paper leans on

99 extracted references · 91 canonical work pages · 2 internal anchors

  1. [1]

    2012, MNRAS, 420, 1825, doi: 10.1111/j.1365-2966.2011.19805.x

    Adamo, A., ¨Ostlin, G., & Zackrisson, E. 2011, MNRAS, 417, 1904, doi: 10.1111/j.1365-2966.2011.19377.x

    work page doi:10.1111/j.1365-2966.2011.19377.x 2011

  2. [2]

    D., van Velzen, S., Horesh, A., & Zauderer, B

    Alexander, K. D., van Velzen, S., Horesh, A., & Zauderer, B. A. 2020, SSRv, 216, 81, doi: 10.1007/s11214-020-00702-w 19

    work page doi:10.1007/s11214-020-00702-w 2020

  3. [3]

    1981 , month = feb, journal =

    Baldwin, J. A., Phillips, M. M., & Terlevich, R. 1981, PASP, 93, 5, doi: 10.1086/130766

    work page doi:10.1086/130766 1981

  4. [4]

    C., & Manne-Nicholas, E

    Bentz, M. C., & Manne-Nicholas, E. 2018, ApJ, 864, 146, doi: 10.3847/1538-4357/aad808

    work page doi:10.3847/1538-4357/aad808 2018

  5. [5]

    , keywords =

    Berg, D. A., James, B. L., King, T., et al. 2022, ApJS, 261, 31, doi: 10.3847/1538-4365/ac6c03

    work page doi:10.3847/1538-4365/ac6c03 2022

  6. [6]

    M., & Frail, D

    Berger, E., Soderberg, A. M., & Frail, D. A. 2003, IAUC, 8157, 2

    2003

  7. [7]

    , keywords =

    Bonzini, M., Padovani, P., Mainieri, V., et al. 2013, MNRAS, 436, 3759, doi: 10.1093/mnras/stt1879

    work page doi:10.1093/mnras/stt1879 2013

  8. [8]

    2016, in Astrophysics and Space Science

    Bournaud, F. 2016, in Astrophysics and Space Science

    2016

  9. [9]

    Galactic Bulges , year = 2016, editor =

    Library, Vol. 418, Galactic Bulges, ed. E. Laurikainen, R. Peletier, & D. Gadotti, 355, doi: 10.1007/978-3-319-19378-6 13

    work page doi:10.1007/978-3-319-19378-6

  10. [10]

    D., et al

    Cendes, Y., Berger, E., Alexander, K. D., et al. 2024, ApJ, 971, 185, doi: 10.3847/1538-4357/ad5541

    work page doi:10.3847/1538-4357/ad5541 2024

  11. [11]

    Chandra, P., & Frail, D. A. 2012, ApJ, 746, 156, doi: 10.1088/0004-637X/746/2/156

    work page doi:10.1088/0004-637x/746/2/156 2012

  12. [12]

    Chomiuk, L., & Wilcots, E. M. 2009, ApJ, 703, 370, doi: 10.1088/0004-637X/703/1/370

    work page doi:10.1088/0004-637x/703/1/370 2009

  13. [13]

    Condon, J. J. 1992, ARA&A, 30, 575, doi: 10.1146/annurev.aa.30.090192.003043

    work page doi:10.1146/annurev.aa.30.090192.003043 1992

  14. [14]

    , keywords =

    Condon, J. J., Cotton, W. D., & Broderick, J. J. 2002, AJ, 124, 675, doi: 10.1086/341650

    work page doi:10.1086/341650 2002

  15. [15]

    , keywords =

    Condon, J. J., Cotton, W. D., Greisen, E. W., et al. 1998, AJ, 115, 1693, doi: 10.1086/300337

    work page doi:10.1086/300337 1998

  16. [16]

    O., Gal-Yam, A., et al

    Corsi, A., Ofek, E. O., Gal-Yam, A., et al. 2014, ApJ, 782, 42, doi: 10.1088/0004-637X/782/1/42

    work page doi:10.1088/0004-637x/782/1/42 2014

  17. [17]

    R., et al

    Corsi, A., Gal-Yam, A., Kulkarni, S. R., et al. 2016, ApJ, 830, 42, doi: 10.3847/0004-637X/830/1/42 de Jong, T., Klein, U., Wielebinski, R., & Wunderlich, E. 1985, A&A, 147, L6 Del Moro, A., Alexander, D. M., Mullaney, J. R., et al. 2013, A&A, 549, A59, doi: 10.1051/0004-6361/201219880

    work page doi:10.3847/0004-637x/830/1/42 2016

  18. [18]

    2017, A&A, 602, A4, doi: 10.1051/0004-6361/201629430 22

    Delhaize, J., Smolˇ ci´ c, V., Delvecchio, I., et al. 2017, A&A, 602, A4, doi: 10.1051/0004-6361/201629430

    work page doi:10.1051/0004-6361/201629430 2017

  19. [19]

    T., et al

    Delvecchio, I., Daddi, E., Sargent, M. T., et al. 2021, A&A, 647, A123, doi: 10.1051/0004-6361/202039647

    work page doi:10.1051/0004-6361/202039647 2021

  20. [20]

    2024, ApJ, 973, 133, doi: 10.3847/1538-4357/ad6568

    Dong, Y., Eftekhari, T., Fong, W., et al. 2024, ApJ, 973, 133, doi: 10.3847/1538-4357/ad6568

    work page doi:10.3847/1538-4357/ad6568 2024

  21. [21]

    Duchesne, S., Ross, K., Thomson, A. J. M., et al. 2025, PASA, 42, 38, doi: 10.1017/pasa.2025.2

    work page doi:10.1017/pasa.2025.2 2025

  22. [22]

    W., Grundy, J

    Duchesne, S. W., Grundy, J. A., Heald, G. H., et al. 2024, PASA, 41, e003, doi: 10.1017/pasa.2023.60

    work page doi:10.1017/pasa.2023.60 2024

  23. [23]

    Eberhard, J.-M., & Reines, A. E. 2025, ApJ, 994, 1, doi: 10.3847/1538-4357/ae0c0d

    work page doi:10.3847/1538-4357/ae0c0d 2025

  24. [24]

    Greene, J. E. 2025, ApJ, 978, 158, doi: 10.3847/1538-4357/ad9584

    work page doi:10.3847/1538-4357/ad9584 2025

  25. [25]

    Alexander, K. D. 2018, ApJ, 854, 86, doi: 10.3847/1538-4357/aaa8e0

    work page doi:10.3847/1538-4357/aaa8e0 2018

  26. [26]

    M., et al

    Elmegreen, D. M., Elmegreen, B. G., Marcus, M. T., et al. 2009, ApJ, 701, 306, doi: 10.1088/0004-637X/701/1/306

    work page doi:10.1088/0004-637x/701/1/306 2009

  27. [27]

    Flesch, E. W. 2023, The Open Journal of Astrophysics, 6, 49, doi: 10.21105/astro.2308.01505

    work page doi:10.21105/astro.2308.01505 2023

  28. [28]

    J., Alexander, K

    Goodwin, A. J., Alexander, K. D., Miller-Jones, J. C. A., et al. 2023, MNRAS, 522, 5084, doi: 10.1093/mnras/stad1258

    work page doi:10.1093/mnras/stad1258 2023

  29. [29]

    E., Strader, J., & Ho, L

    Greene, J. E., Strader, J., & Ho, L. C. 2020, ARA&A, 58, 257, doi: 10.1146/annurev-astro-032620-021835

    work page doi:10.1146/annurev-astro-032620-021835 2020

  30. [30]

    L., et al

    Gulati, A., Murphy, T., Kaplan, D. L., et al. 2026, ApJ, 1000, 118, doi: 10.3847/1538-4357/ae4351

    work page doi:10.3847/1538-4357/ae4351 2026

  31. [31]

    N., Reines, A

    Hainline, K. N., Reines, A. E., Greene, J. E., & Stern, D. 2016, ApJ, 832, 119, doi: 10.3847/0004-637X/832/2/119

    work page doi:10.3847/0004-637x/832/2/119 2016

  32. [32]

    , keywords =

    Hale, C. L., McConnell, D., Thomson, A. J. M., et al. 2021, PASA, 38, e058, doi: 10.1017/pasa.2021.47

    work page doi:10.1017/pasa.2021.47 2021

  33. [33]

    and Johnson, Benjamin D

    Hao, C.-N., Kennicutt, R. C., Johnson, B. D., et al. 2011, ApJ, 741, 124, doi: 10.1088/0004-637X/741/2/124

    work page doi:10.1088/0004-637x/741/2/124 2011

  34. [34]

    A&A , author =

    Hardcastle, M. J., Williams, W. L., Best, P. N., et al. 2019, A&A, 622, A12, doi: 10.1051/0004-6361/201833893

    work page doi:10.1051/0004-6361/201833893 2019

  35. [35]

    1956, AJ, 61, 178, doi: 10.1086/107409

    Haro, G. 1956, AJ, 61, 178, doi: 10.1086/107409

    work page doi:10.1086/107409 1956

  36. [36]

    T., & Rowan-Robinson, M

    Helou, G., Soifer, B. T., & Rowan-Robinson, M. 1985, ApJL, 298, L7, doi: 10.1086/184556

    work page doi:10.1086/184556 1985

  37. [37]

    , keywords =

    Hickox, R. C., & Alexander, D. M. 2018, ARA&A, 56, 625, doi: 10.1146/annurev-astro-081817-051803

    work page doi:10.1146/annurev-astro-081817-051803 2018

  38. [38]

    Hildebrand, R. H. 1983, QJRAS, 24, 267

    1983

  39. [39]

    Hills, J. G. 1975, Nature, 254, 295, doi: 10.1038/254295a0 Hinojosa-Go˜ ni, R., Mu˜ noz-Tu˜ n´ on, C., & M´ endez-Abreu, J. 2016, A&A, 592, A122, doi: 10.1051/0004-6361/201527066

    work page doi:10.1038/254295a0 1975

  40. [40]

    A., Becker, R

    Hodge, J. A., Becker, R. H., White, R. L., & Richards, G. T. 2013, ApJ, 769, 125, doi: 10.1088/0004-637X/769/2/125

    work page doi:10.1088/0004-637x/769/2/125 2013

  41. [41]

    H., Cohen, M., Masci, F., et al

    Jarrett, T. H., Cohen, M., Masci, F., et al. 2011, ApJ, 735, 112, doi: 10.1088/0004-637X/735/2/112

    work page doi:10.1088/0004-637x/735/2/112 2011

  42. [42]

    H., Masci, F., Tsai, C

    Jarrett, T. H., Masci, F., Tsai, C. W., et al. 2013, AJ, 145, 6, doi: 10.1088/0004-6256/145/1/6

    work page doi:10.1088/0004-6256/145/1/6 2013

  43. [43]

    E., Hunt, L

    Johnson, K. E., Hunt, L. K., & Reines, A. E. 2009, AJ, 137, 3788, doi: 10.1088/0004-6256/137/4/3788

    work page doi:10.1088/0004-6256/137/4/3788 2009

  44. [44]

    E., Indebetouw, R., Watson, C., & Kobulnicky, H

    Johnson, K. E., Indebetouw, R., Watson, C., & Kobulnicky, H. A. 2004, AJ, 128, 610, doi: 10.1086/422017

    work page doi:10.1086/422017 2004

  45. [45]

    and Evans, Neal J

    Kennicutt, R. C., & Evans, N. J. 2012, ARA&A, 50, 531, doi: 10.1146/annurev-astro-081811-125610

    work page internal anchor Pith review doi:10.1146/annurev-astro-081811-125610 2012

  46. [46]

    Kennicutt, Jr., R. C. 1998, ARA&A, 36, 189, doi: 10.1146/annurev.astro.36.1.189

    work page Pith review doi:10.1146/annurev.astro.36.1.189 1998

  47. [47]

    A., Heckman, T

    Kewley, L. J., Groves, B., Kauffmann, G., & Heckman, T. 2006, MNRAS, 372, 961, doi: 10.1111/j.1365-2966.2006.10859.x 20

    work page doi:10.1111/j.1365-2966.2006.10859.x 2006

  48. [48]

    Tidal disruption of stars by supermassive black holes: Status of observations

    Komossa, S. 2015, Journal of High Energy Astrophysics, 7, 148, doi: 10.1016/j.jheap.2015.04.006

    work page doi:10.1016/j.jheap.2015.04.006 2015

  49. [49]

    Kormendy, J., & Ho, L. C. 2013, ARA&A, 51, 511, doi: 10.1146/annurev-astro-082708-101811

    work page Pith review doi:10.1146/annurev-astro-082708-101811 2013

  50. [50]

    1985, A&A, 142, 411

    Kunth, D., & Joubert, M. 1985, A&A, 142, 411

    1985

  51. [51]

    A., Chandler, C

    Lacy, M., Baum, S. A., Chandler, C. J., et al. 2020, PASP, 132, 035001, doi: 10.1088/1538-3873/ab63eb

    work page doi:10.1088/1538-3873/ab63eb 2020

  52. [52]

    J., Reines, A

    Latimer, L. J., Reines, A. E., Hainline, K. N., Greene, J. E., & Stern, D. 2021, ApJ, 914, 133, doi: 10.3847/1538-4357/abfe0c

    work page doi:10.3847/1538-4357/abfe0c 2021

  53. [53]

    , keywords =

    Latimer, L. J., Reines, A. E., Plotkin, R. M., Russell, T. D., & Condon, J. J. 2019, ApJ, 884, 78, doi: 10.3847/1538-4357/ab3289

    work page doi:10.3847/1538-4357/ab3289 2019

  54. [54]

    D., Eufrasio, R

    Lehmer, B. D., Eufrasio, R. T., Tzanavaris, P., et al. 2019, ApJS, 243, 3, doi: 10.3847/1538-4365/ab22a8

    work page doi:10.3847/1538-4365/ab22a8 2019

  55. [55]

    , keywords =

    Leitherer, C., Schaerer, D., Goldader, J. D., et al. 1999, ApJS, 123, 3, doi: 10.1086/313233

    work page doi:10.1086/313233 1999

  56. [56]

    W., Higley, A

    Lyke, B. W., Higley, A. N., McLane, J. N., et al. 2020, ApJS, 250, 8, doi: 10.3847/1538-4365/aba623

    work page doi:10.3847/1538-4365/aba623 2020

  57. [57]

    J., & Ma, C.-P

    McConnell, N. J., & Ma, C.-P. 2013, ApJ, 764, 184, doi: 10.1088/0004-637X/764/2/184

    work page doi:10.1088/0004-637x/764/2/184 2013

  58. [58]

    and Lamer, G

    Merloni, A., Lamer, G., Liu, T., et al. 2024, A&A, 682, A34, doi: 10.1051/0004-6361/202347165

    work page internal anchor Pith review doi:10.1051/0004-6361/202347165 2024

  59. [59]

    R., Heckman, T

    Meurer, G. R., Heckman, T. M., Lehnert, M. D., Leitherer, C., & Lowenthal, J. 1997, AJ, 114, 54, doi: 10.1086/118452

    work page doi:10.1086/118452 1997

  60. [60]

    L., Arellano-C \'o rdova , K

    Mingozzi, M., James, B. L., Arellano-C´ ordova, K. Z., et al. 2022, ApJ, 939, 110, doi: 10.3847/1538-4357/ac952c

    work page doi:10.3847/1538-4357/ac952c 2022

  61. [61]

    L., Berg, D

    Mingozzi, M., James, B. L., Berg, D. A., et al. 2024, ApJ, 962, 95, doi: 10.3847/1538-4357/ad1033

    work page doi:10.3847/1538-4357/ad1033 2024

  62. [62]

    2021, The Astrophysical Journal, 922, 155, doi: 10.3847/1538-4357/ac1ffa

    Salehirad, S. 2021, ApJ, 922, 155, doi: 10.3847/1538-4357/ac1ffa

    work page doi:10.3847/1538-4357/ac1ffa 2021

  63. [63]

    2023, A&A, 674, A210, doi: 10.1051/0004-6361/202345891 Moti˜ no Flores, S

    Kollatschny, W., & Maseda, M. 2023, A&A, 674, A210, doi: 10.1051/0004-6361/202345891 Moti˜ no Flores, S. M., Wiklind, T., & Eufrasio, R. T. 2021, ApJ, 921, 130, doi: 10.3847/1538-4357/ac18cc

    work page doi:10.1051/0004-6361/202345891 2023

  64. [64]

    J., Condon, J

    Murphy, E. J., Condon, J. J., Schinnerer, E., et al. 2011, ApJ, 737, 67, doi: 10.1088/0004-637X/737/2/67

    work page doi:10.1088/0004-637x/737/2/67 2011

  65. [65]

    1998, Nature, 392, 253, doi: 10.1038/32596

    Noguchi, M. 1998, Nature, 392, 253, doi: 10.1038/32596

    work page doi:10.1038/32596 1998

  66. [66]

    Z., Patil, P., et al

    Nyland, K., Dong, D. Z., Patil, P., et al. 2020, ApJ, 905, 74, doi: 10.3847/1538-4357/abc341 O’Connell, R. W. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 322, The Formation and Evolution of Massive Young Star Clusters, ed. H. J. G. L. M. Lamers, L. J. Smith, & A. Nota, 551, doi: 10.48550/arXiv.astro-ph/0405038

    work page doi:10.3847/1538-4357/abc341 2020

  67. [67]

    2016, A&A Rv, 24, 13, doi: 10.1007/s00159-016-0098-6

    Padovani, P. 2016, A&A Rv, 24, 13, doi: 10.1007/s00159-016-0098-6

    work page doi:10.1007/s00159-016-0098-6 2016

  68. [68]

    , keywords =

    Padovani, P., Bonzini, M., Kellermann, K. I., et al. 2015, MNRAS, 452, 1263, doi: 10.1093/mnras/stv1375

    work page doi:10.1093/mnras/stv1375 2015

  69. [69]

    T., Corsi, A., Frail, D

    Palliyaguru, N. T., Corsi, A., Frail, D. A., et al. 2019, ApJ, 872, 201, doi: 10.3847/1538-4357/aaf64d

    work page doi:10.3847/1538-4357/aaf64d 2019

  70. [70]

    S., Berg , D

    Parker, K. S., Berg, D. A., Chisholm, J., et al. 2026, ApJ, 997, 98, doi: 10.3847/1538-4357/ae22d9

    work page doi:10.3847/1538-4357/ae22d9 2026

  71. [71]

    Pettini, M., & Pagel, B. E. J. 2004, MNRAS, 348, L59, doi: 10.1111/j.1365-2966.2004.07591.x

    work page doi:10.1111/j.1365-2966.2004.07591.x 2004

  72. [72]

    P., & Keane, E

    Pietka, M., Fender, R. P., & Keane, E. F. 2015, MNRAS, 446, 3687, doi: 10.1093/mnras/stu2335

    work page doi:10.1093/mnras/stu2335 2015

  73. [73]

    , keywords =

    Radcliffe, J. F., Beswick, R. J., Thomson, A. P., et al. 2019, MNRAS, 490, 4024, doi: 10.1093/mnras/stz2748

    work page doi:10.1093/mnras/stz2748 2019

  74. [74]

    Reines, A. E. 2022, Nature Astronomy, 6, 26, doi: 10.1038/s41550-021-01556-0

    work page doi:10.1038/s41550-021-01556-0 2022

  75. [75]

    E., Condon, J

    Reines, A. E., Condon, J. J., Darling, J., & Greene, J. E. 2020, ApJ, 888, 36, doi: 10.3847/1538-4357/ab4999

    work page doi:10.3847/1538-4357/ab4999 2020

  76. [76]

    E., Greene, J

    Reines, A. E., Greene, J. E., & Geha, M. 2013, ApJ, 775, 116, doi: 10.1088/0004-637X/775/2/116

    work page doi:10.1088/0004-637x/775/2/116 2013

  77. [77]

    E., Johnson, K

    Reines, A. E., Johnson, K. E., & Goss, W. M. 2008a, AJ, 135, 2222, doi: 10.1088/0004-6256/135/6/2222

    work page doi:10.1088/0004-6256/135/6/2222

  78. [78]

    E., Johnson, K

    Reines, A. E., Johnson, K. E., & Hunt, L. K. 2008b, AJ, 136, 1415, doi: 10.1088/0004-6256/136/4/1415

    work page doi:10.1088/0004-6256/136/4/1415

  79. [79]

    E., & Volonteri, M

    Reines, A. E., & Volonteri, M. 2015, ApJ, 813, 82, doi: 10.1088/0004-637X/813/2/82

    work page doi:10.1088/0004-637x/813/2/82 2015

  80. [80]

    E., McLeod, A

    Rowland, L. E., McLeod, A. F., Fattahi, A., et al. 2024, A&A, 685, A46, doi: 10.1051/0004-6361/202348029

    work page doi:10.1051/0004-6361/202348029 2024

Showing first 80 references.