pith. sign in

arxiv: 2605.16546 · v1 · pith:CYHJUUTUnew · submitted 2026-05-15 · 🌌 astro-ph.HE · astro-ph.SR

Probing the Mass-loss Histories of Type IIn and II-L Supernovae with Late-time Radio Observations

Charles D. Kilpatrick , Lindsay DeMarchi , Wen-fai Fong , Jennifer E. Andrews , Ori D. Fox , Nathan Smith This is my paper

Pith reviewed 2026-05-20 15:25 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.SR
keywords supernovaeType IInType II-Lradio observationscircumstellar materialmass-loss rateprogenitor wind
0
0 comments X

The pith

Late-time radio observations indicate that Type IIn and II-L supernovae differ chiefly in dense circumstellar material right before explosion rather than in long-term mass-loss rates.

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

The paper reports VLA radio observations of 16 Type IIn and Type II-L supernovae at 1000 to 7000 days after explosion. These measurements probe circumstellar material at distances greater than 10^16 cm, which traces mass loss over hundreds to thousands of years before core collapse. Four events show detectable radio emission with steep spectral indices pointing to optically thin synchrotron radiation, while the remaining twelve yield only upper limits. The inferred mass-loss rates span a wide range but show no systematic separation between the two supernova classes at these large radii. This supports the view that the subtypes are set apart mainly by the presence and strength of dense material ejected immediately prior to explosion.

Core claim

We infer progenitor mass-loss rates of Mdot/vw less than or equal to 10^{-5} to 10^{-3} solar masses per year per 1000 km/s. The intermediate object PTF11iqb is detected at luminosities between those of classical IIn and II-L events, supporting a continuum in interaction strength. Limits on the undetected sources indicate that SNe IIn and SNe II-L are not separated by long-term mass-loss rate at the radii probed here, but chiefly by the presence and strength of dense circumstellar material immediately before explosion. At epochs beyond 5000 days some events maintain nearly constant radio luminosity while others decline rapidly, suggesting that the most radio-luminous objects arise from stars

What carries the argument

Late-time radio luminosity as a tracer of circumstellar density from interaction with a steady progenitor wind at radii greater than 10^16 cm.

If this is right

  • Detected events such as 1998S and 2005ip require sustained high mass loss extending over hundreds to thousands of years.
  • The object PTF11iqb bridges classical IIn and II-L subtypes in CSM interaction strength.
  • Some supernovae maintain constant radio luminosity past 5000 days, implying pre-explosion mass loss over more than 10,000 years.
  • Spectral evolution at these epochs is consistent with internal free-free absorption dominating over other processes.

Where Pith is reading between the lines

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

  • Progenitor models may need to incorporate episodic or binary-driven mass loss that activates only in the final decades before collapse.
  • Similar long-term wind rates across subtypes suggest the key difference lies in triggers for dense shell ejection near explosion.
  • Multi-epoch radio monitoring of additional events could test whether the observed luminosity spread reflects a true continuum or selection effects.

Load-bearing premise

The conversion of observed radio luminosity to mass-loss rate assumes equipartition between relativistic electrons and magnetic fields, a constant wind velocity of 1000 km/s, and emission dominated by interaction with a steady wind.

What would settle it

A deep radio observation that detects a Type II-L supernova at a luminosity implying a sustained mass-loss rate above 10^{-3} solar masses per year at radii corresponding to more than 1000 years before explosion would contradict the claim.

Figures

Figures reproduced from arXiv: 2605.16546 by Charles D. Kilpatrick, Jennifer E. Andrews, Lindsay DeMarchi, Nathan Smith, Ori D. Fox, Wen-fai Fong.

Figure 1
Figure 1. Figure 1: Four panels showing 6.2 GHz radio contours (red) overlaid on top of optical imaging, as described in Section 2.4 for each SNe with radio sources detected near the approximate position of the optical SN. The position of each SN is labeled in blue as given in [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: 4.86–6.2 GHz radio luminosities from SNe IIn (indicated with circles) and SNe II-L (indicated with triangles) as described in Section 2. Objects in this paper are shown in red while data from the literature are shown in black (from radio light curves and limits in Weiler et al. 1986, 1990, 1991, 1992; van Dyk et al. 1993; Eck et al. 1996; Montes et al. 1998, 2000; Bietenholz et al. 2002; Williams et al. 20… view at source ↗
Figure 3
Figure 3. Figure 3: Spectral index from C- to X-bands (roughly 5–10 GHz) as a function of time for SNe IIn and SNe II-L. We label sources described in this paper, including spectral in￾dices derived from the observations described in Section 3.1.2 (red). For comparison, we show the theoretical evolution of spectral index for a source dominated by free-free absorption from a shell of dense circumstellar matter, which asymptot￾… view at source ↗
read the original abstract

We present VLA observations of 16 Type IIn and Type II-L supernovae (SNe IIn and SNe II-L) at ~1000--7000 days after explosion, probing circumstellar matter (CSM) at distances >10^16 cm from the progenitor corresponding to mass-loss over hundreds to thousands of years before core collapse. We detect radio emission from four SNe (1998S, 2005ip, 2008fq, and PTF11iqb) with the remaining 12 yielding upper limits of nu L_nu < 10^35--10^36 erg s^-1 at 3--11 GHz. The detected sources span approximately two orders of magnitude in radio luminosity, reflecting a wide range of CSM densities and pre-explosion mass-loss histories. All detected sources exhibit steep spectral indices (~<-0.4) consistent with optically-thin synchrotron emission, and the spectral evolution supports internal free-free absorption as the dominant absorption mechanism at these late epochs. We infer progenitor mass-loss rates of \dot{M}/v_w ~< 10^-5--10^-3 Msun yr^-1/(1000 km s^-1), with the most radio-luminous objects requiring sustained mass-loss over hundreds to thousands of years. The detection of the intermediate SN IIn/SN II-L object PTF11iqb at luminosities between classical SNe IIn and SNe II-L supports a continuum between these subtypes in terms of CSM interaction strength. Our limits further suggest that SNe IIn and SNe II-L are not separated by long-term mass-loss rate at the radii probed here, but chiefly by the presence and strength of dense circumstellar material immediately before explosion. At epochs >5000 days, some SNe (e.g., 1979C and 1986J) maintain nearly constant radio luminosity while others decline rapidly, suggesting that the most radio-luminous SNe IIn arise from progenitors with sustained mass-loss extending >10^4 yr before explosion.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 1 minor

Summary. The paper reports VLA radio observations at 1000-7000 days post-explosion for 16 Type IIn and II-L supernovae, detecting synchrotron emission from four objects (1998S, 2005ip, 2008fq, PTF11iqb) with luminosities spanning two orders of magnitude and upper limits for the remaining twelve. Using standard Chevalier modeling with fixed wind velocity and equipartition, the authors derive mass-loss rates Ṁ/v_w ≲ 10^{-5}--10^{-3} M_⊙ yr^{-1}/(1000 km s^{-1}) at radii >10^{16} cm and conclude that the subtypes are not separated by long-term mass-loss rates but by the presence of dense CSM immediately prior to explosion.

Significance. If the modeling assumptions hold, the new late-time detections and limits provide direct constraints on progenitor mass-loss over centuries to millennia, supporting a continuum between IIn and II-L subtypes and identifying sustained mass loss in the most luminous cases. The work adds valuable observational anchors for stellar evolution models at large radii where optical data are insensitive.

major comments (1)
  1. [Abstract] Abstract (final paragraph) and § on mass-loss inference: The central claim that long-term Ṁ/v_w values do not separate SNe IIn from SNe II-L rests on converting the four detections and twelve upper limits to comparable Ṁ/v_w under the assumptions of steady wind (ρ ∝ r^{-2}), fixed v_w = 1000 km s^{-1}, and equipartition. No quantitative test is presented for how the overlap changes if v_w differs between subtypes or if equipartition fractions vary; relaxing these inputs can shift the normalized limits and remove the reported lack of separation.
minor comments (1)
  1. The spectral-index values and free-free absorption discussion would benefit from explicit tabulation of measured fluxes, frequencies, and epochs for each detected source to allow independent verification of the optically-thin synchrotron interpretation.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address the major comment below and have revised the paper to strengthen the presentation of our mass-loss inferences.

read point-by-point responses

  1. Referee: [Abstract] Abstract (final paragraph) and § on mass-loss inference: The central claim that long-term Ṁ/v_w values do not separate SNe IIn from SNe II-L rests on converting the four detections and twelve upper limits to comparable Ṁ/v_w under the assumptions of steady wind (ρ ∝ r^{-2}), fixed v_w = 1000 km s^{-1}, and equipartition. No quantitative test is presented for how the overlap changes if v_w differs between subtypes or if equipartition fractions vary; relaxing these inputs can shift the normalized limits and remove the reported lack of separation.

    Authors: We agree that a sensitivity analysis would improve the robustness of the central claim. Our reported quantities are expressed as Ṁ/v_w precisely to reduce dependence on the uncertain wind velocity, and the equipartition assumption follows the standard approach used throughout the radio supernova literature. Nevertheless, we acknowledge the value of quantifying how deviations from these fiducial choices affect the overlap. In the revised manuscript we will add a short subsection (or expanded paragraph) in the mass-loss inference discussion that explores the effects of varying v_w between 500 and 2000 km s^{-1} and equipartition fractions by factors of a few. This analysis will demonstrate that the substantial overlap between the IIn and II-L populations persists under plausible variations, while the distinction between subtypes continues to be driven by the presence of dense CSM at small radii as traced by optical observations. We will also note the limitations of the modeling assumptions more explicitly in the abstract and conclusions. revision: yes

Circularity Check

0 steps flagged

No significant circularity; claims follow from new data under standard modeling

full rationale

The paper presents new VLA radio observations of 16 SNe IIn and II-L at late times, detecting four sources and placing upper limits on the rest. Mass-loss rates are derived by applying the standard Chevalier synchrotron model (with fixed equipartition, v_w = 1000 km/s, and steady-wind density profile) to the measured luminosities and limits; the subtype comparison then follows directly from the resulting Ṁ/v_w values overlapping across detections and non-detections. No derivation step reduces by construction to a fitted parameter renamed as a prediction, a self-citation chain, or an ansatz smuggled from prior author work. The central inference about long-term mass-loss rates is therefore an output of fresh observational constraints rather than an input restated in new coordinates.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The mass-loss rate inferences rest on standard radio supernova modeling assumptions rather than new free parameters or invented entities. No new particles or forces are postulated.

free parameters (1)
  • wind velocity v_w
    Fixed at 1000 km s^-1 for all objects when quoting mass-loss rates; this is a conventional choice but directly scales the inferred dot{M}.
axioms (2)
  • domain assumption Radio emission arises from synchrotron radiation produced by the supernova shock interacting with a steady progenitor wind
    Invoked to convert luminosity to mass-loss rate; stated in the abstract when discussing spectral indices and absorption.
  • domain assumption Equipartition between relativistic electrons and magnetic field energy densities
    Standard assumption in radio SN modeling used to derive CSM densities from observed flux.

pith-pipeline@v0.9.0 · 5939 in / 1570 out tokens · 53238 ms · 2026-05-20T15:25:45.494965+00:00 · methodology

discussion (0)

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

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

111 extracted references · 111 canonical work pages

  1. [1]

    1982, A&A, 116, 35

    Barbon, R., Ciatti, F., & Rosino, L. 1982, A&A, 116, 35

    work page 1982

  2. [2]

    F., Bartel, N., Argo, M., et al

    Bietenholz, M. F., Bartel, N., Argo, M., et al. 2021, ApJ, 908, 75

    work page 2021

  3. [3]

    F., Bartel, N., & Rupen, M

    Bietenholz, M. F., Bartel, N., & Rupen, M. P. 2002, ApJ, 581, 1132 —. 2010, ApJ, 712, 1057

    work page 2002

  4. [4]

    2015, MNRAS, 450, 246

    Bilinski, C., Smith, N., Li, W., et al. 2015, MNRAS, 450, 246

    work page 2015

  5. [5]

    2006, IAUC, 8680

    Blondin, S., Modjaz, M., Kirshner, R., & Challis, P. 2006, IAUC, 8680

    work page 2006

  6. [6]

    Boisseau, T., & Irwin, C. M. 2021, ApJ, 908, 75

    work page 2021

  7. [7]

    2005, Central Bureau Electronic Telegrams, 275

    Boles, T., Nakano, S., & Itagaki, K. 2005, Central Bureau Electronic Telegrams, 275

    work page 2005

  8. [8]

    2011, Centr al Bureau Electronic Telegrams, 2851

    Boles, T., Pastorello, A., Stanishev, V., et al. 2011, Centr al Bureau Electronic Telegrams, 2851

    work page 2011

  9. [9]

    S., et al

    Bose, S., Dong, S., Kochanek, C. S., et al. 2018, ApJ, 862, 107

    work page 2018

  10. [10]

    W., Uomoto, A

    Branch, D., Falk, S. W., Uomoto, A. K., et al. 1981, ApJ, 244, 780

    work page 1981

  11. [11]

    J., Schulze, S., Lunnan, R., et al

    Brennan, S. J., Schulze, S., Lunnan, R., et al. 2025, ApJ, 981, 46

    work page 2025

  12. [12]

    2010, Central Bureau Electronic Telegrams, 2548

    Challis, P., Kirshner, R., & Smith, N. 2010, Central Bureau Electronic Telegrams, 2548

    work page 2010

  13. [13]

    2018, Space Science Reviews, 214, 27

    Chandra, P. 2018, Space Science Reviews, 214, 27

    work page 2018

  14. [14]

    A., Chugai, N., et al

    Chandra, P., Chevalier, R. A., Chugai, N., et al. 2012, ApJ, 755, 110

    work page 2012

  15. [15]

    Soderberg, A. M. 2015, ApJ, 810, 32

    work page 2015

  16. [16]

    J., Chevalier, R

    Chandra, P., Stockdale, C. J., Chevalier, R. A., et al. 2009, ApJ, 690, 1839

    work page 2009

  17. [17]

    Chevalier, R. A. 1982a, ApJ, 259, 302 —. 1982b, ApJ, 259, 302 —. 1998, ApJ, 499, 810

    work page 1998

  18. [18]

    A., & Fransson, C

    Chevalier, R. A., & Fransson, C. 1994, ApJ, 420, 268 —. 2001, ApJL, 558, L27

    work page 1994

  19. [19]

    A., & Fransson, C

    Chevalier, R. A., & Fransson, C. 2003, in Lecture Notes in

    work page 2003

  20. [20]

    598, Supernovae and Gamma-Ray Bursters, ed

    Physics, Berlin Springer Verlag, Vol. 598, Supernovae and Gamma-Ray Bursters, ed. K. Weiler, 171–194 —. 2006, ARA&A, 44, 17

    work page 2006

  21. [21]

    A., Fransson, C., & Nymark, T

    Chevalier, R. A., Fransson, C., & Nymark, T. K. 2006, ApJ, 641, 1029

    work page 2006

  22. [22]

    Chornock, R., Modjaz, M., & Filippenko, A. V. 2001, IAUC, 7699

    work page 2001

  23. [23]

    N., Danziger, I

    Chugai, N. N., Danziger, I. J., & della Valle, M. 1995, MNRAS, 276, 530

    work page 1995

  24. [24]

    Crowther, P. A. 2007, ARA&A, 45, 177

    work page 2007

  25. [25]

    2022, ApJ, 938, 84

    DeMarchi, L., Margutti, R., Dittman, J., et al. 2022, ApJ, 938, 84

    work page 2022

  26. [26]

    Dessart, L., & Jacobson-Gal´ an, W. V. 2023, A&A, 677, A105

    work page 2023

  27. [27]

    E., Hall, P

    Dewdney, P. E., Hall, P. J., Schilizzi, R. T., & Lazio, T. J. W. W. 2009, Proceedings of the IEEE, 97, 1482

    work page 2009

  28. [28]

    2025, ApJL , 961, L16

    Dong, Y., Milisavljevic, D., Margutti, R., et al. 2025, ApJL , 961, L16

    work page 2025

  29. [29]

    R., Cowan, J

    Eck, C. R., Cowan, J. J., Boffi, F. R., & Branch, D. 1996, ApJL, 472, L25

    work page 1996

  30. [30]

    D., Li, W., et al

    Elias-Rosa, N., Van Dyk, S. D., Li, W., et al. 2010, ApJL, 714, L254 —. 2011a, ApJ, 742, 6 —. 2011b, ApJ, 742, 6

    work page 2010

  31. [31]

    C., & Terlevich, R

    Fabian, A. C., & Terlevich, R. 1996, MNRAS, 280, L5

    work page 1996

  32. [32]

    A., & Matonick, D

    Fesen, R. A., & Matonick, D. M. 1993, ApJ, 407, 110

    work page 1993

  33. [33]

    V., & Moran, E

    Filippenko, A. V., & Moran, E. C. 1998, IAUC, 6830

    work page 1998

  34. [34]

    D., Chevalier, R

    Fox, O. D., Chevalier, R. A., Dwek, E., et al. 2010, ApJ, 725, 1768

    work page 2010

  35. [35]

    D., Chevalier, R

    Fox, O. D., Chevalier, R. A., Skrutskie, M. F., et al. 2011, ApJ, 741, 7

    work page 2011

  36. [36]

    D., Fransson, C., Smith, N., et al

    Fox, O. D., Fransson, C., Smith, N., et al. 2020, MNRAS, 498, 517

    work page 2020

  37. [37]

    Fransson, C., Lundqvist, P., & Chevalier, R. A. 1996, ApJ, 461, 993

    work page 1996

  38. [38]

    2020, Royal Society Open Science, 7, 200467

    Fraser, M. 2020, Royal Society Open Science, 7, 200467

    work page 2020

  39. [39]

    2010, ApJL, 714, L280

    Fraser, M., Tak´ ats, K., Pastorello, A., et al. 2010, ApJL, 714, L280

    work page 2010

  40. [40]

    Gall, E. E. E., Polshaw, J., Kotak, R., et al. 2015, A&A, 582, A3

    work page 2015

  41. [41]

    A., Boyce, M

    Gordon, Y. A., Boyce, M. M., O’Dea, C. P., et al. 2021, ApJS, 255, 30

    work page 2021

  42. [42]

    Green, D. A. 2019, Journal of Astrophysics and Astronomy, 40, 36

    work page 2019

  43. [43]

    E., Stroh, M

    Harris, C. E., Stroh, M. C., Margutti, R., et al. 2025, ApJ, 979, 28

    work page 2025

  44. [44]

    Henry, R. B. C., & Branch, D. 1987, PASP, 99, 112 20 Kilpatrick et al

    work page 1987

  45. [45]

    Ho, A. Y. Q., Phinney, E. S., Ravi, V., et al. 2019, ApJ, 871, 73

    work page 2019

  46. [46]

    M., & Davidson, K

    Humphreys, R. M., & Davidson, K. 1994, ARA&A, 32, 303

    work page 1994

  47. [47]

    A., Van Dyk, S

    Immler, S., Fesen, R. A., Van Dyk, S. D., et al. 2005, ApJ, 632, 283

    work page 2005

  48. [48]

    2015, Central Bureau Electronic Telegrams, 4051

    Jin, Z.-w., Gao, X., Migotto, K., et al. 2015, Central Bureau Electronic Telegrams, 4051

    work page 2015

  49. [49]

    2007, A&A, 469, 671

    Josselin, E., & Plez, B. 2007, A&A, 469, 671

    work page 2007

  50. [50]

    D., Foley, R

    Kilpatrick, C. D., Foley, R. J., Drout, M. R., et al. 2018, MNRAS, 473, 4805

    work page 2018

  51. [51]

    2025, ApJ, 978, 89

    Kundu, E., Marcote, B., Nimmo, K., et al. 2025, ApJ, 978, 89

    work page 2025

  52. [52]

    A., Chandler, C

    Lacy, M., Baum, S. A., Chandler, C. J., et al. 2020, PASP, 132, 035001

    work page 2020

  53. [53]

    2006, Central Bureau Electronic Telegrams, 412

    Lee, E., & Li, W. 2006, Central Bureau Electronic Telegrams, 412

    work page 2006

  54. [54]

    C., Li, W

    Leonard, D. C., Li, W. D., & Filippenko, A. V. 2000, IAUC, 7483

    work page 2000

  55. [55]

    V., Miller, A

    Li, W., Filippenko, A. V., Miller, A. A., et al. 2009, Central Bureau Electronic Telegrams, 2042

    work page 2009

  56. [56]

    V., & Moran, E

    Li, W.-D., Li, C., Filippenko, A. V., & Moran, E. C. 1998, IAUC, 6829

    work page 1998

  57. [57]

    1988, A&A, 192, 221

    Lundqvist, P., & Fransson, C. 1988, A&A, 192, 221

    work page 1988

  58. [58]

    M., et al

    Margutti, R., Milisavljevic, D., Soderberg, A. M., et al. 2014, ApJ, 780, 21

    work page 2014

  59. [59]

    2010, Central Bureau Electronic Telegrams, 2544

    Maza, J., Hamuy, M., Antezana, R., et al. 2010, Central Bureau Electronic Telegrams, 2544

    work page 2010

  60. [60]

    2007, in Astronomical Society of the Pacific Conference Series, Vol

    Golap, K. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 376, Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw, F. Hill, & D. J. Bell, 127

    work page 2007

  61. [61]

    G., & Henderson, A

    Mezger, P. G., & Henderson, A. P. 1967, ApJ, 147, 471

    work page 1967

  62. [62]

    A., Leibundgut, B., & Kirshner , R

    Milisavljevic, D., Fesen, R. A., Leibundgut, B., & Kirshner , R. P. 2008, ApJ, 684, 1170

    work page 2008

  63. [63]

    2005, Central Bureau Electronic Telegrams, 276

    Modjaz, M., Kirshner, R., & Challis, P. 2005, Central Bureau Electronic Telegrams, 276

    work page 2005

  64. [64]

    Modjaz, M., & Li, W. D. 2001, IAUC, 7682

    work page 2001

  65. [65]

    Monard, L. A. G. 2009, Central Bureau Electronic Telegrams, 1867

    work page 2009

  66. [66]

    J., Van Dyk, S

    Montes, M. J., Van Dyk, S. D., Weiler, K. W., Sramek, R. A., & Panagia, N. 1998, ApJ, 506, 874

    work page 1998

  67. [67]

    J., Weiler, K

    Montes, M. J., Weiler, K. W., Van Dyk, S. D., et al. 2000, ApJ, 532, 1124

    work page 2000

  68. [68]

    I., Piro, A

    Morozova, V. I., Piro, A. L., & Valenti, S. 2017, ApJ, 838, 28

    work page 2017

  69. [69]

    A., Lacki, B

    Murase, K., Thompson, T. A., Lacki, B. C., & Beacom, J. F. 2019, ApJ, 874, 80

    work page 2019

  70. [70]

    2009, Central Bureau Electronic Telegrams, 2006

    Nakano, S., Yusa, T., & Kadota, K. 2009, Central Bureau Electronic Telegrams, 2006

    work page 2009

  71. [71]

    1996, IAUC, 6505

    Nakano, S., Kushida, R., Koshida, Y., et al. 1996, IAUC, 6505

    work page 1996

  72. [72]

    1961, ApJ, 134, 1010

    Oster, L. 1961, ApJ, 134, 1010

    work page 1961

  73. [73]

    1980, MNRAS, 192, 861

    Panagia, N., Vettolani, G., Boksenberg, A., et al. 1980, MNRAS, 192, 861

    work page 1980

  74. [74]

    2011, The Astronomer’s Telegram, 3510

    Parrent, J., Levitan, D., Howell, A., et al. 2011, The Astronomer’s Telegram, 3510

    work page 2011

  75. [75]

    A., Chandler, C

    Perley, R. A., Chandler, C. J., Butler, B. J., & Wrobel, J. M. 2011, ApJS, 194, 25

    work page 2011

  76. [76]

    2011, Central Bureau Electronic Telegrams, 2623

    Pignata, G., Cifuentes, M., Maza, J., et al. 2011, Central Bureau Electronic Telegrams, 2623

    work page 2011

  77. [77]

    L., Shappee, B

    Prieto, J. L., Shappee, B. J., Stanek, K. Z., et al. 2011, The Astronomer’s Telegram, 3749

    work page 2011

  78. [78]

    2008, Central Bureau Electronic Telegrams, 1510

    Quinn, J., Baade, D., Clocchiatti, A., et al. 2008, Central Bureau Electronic Telegrams, 1510

    work page 2008

  79. [79]

    P., Williams, B

    Reynolds, S. P., Williams, B. J., Borkowski, K. J., & Long, K. S. 2021, ApJ, 917, 55

    work page 2021

  80. [80]

    B., & Lightman, A

    Rybicki, G. B., & Lightman, A. P. 1979, Radiative processes in astrophysics (John Wiley & Sons)

    work page 1979

Showing first 80 references.