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arxiv: 2605.18973 · v1 · pith:DYKAH26Anew · submitted 2026-05-18 · 🌌 astro-ph.HE

GRB 260310A/SN 2026fgk: Photometric and Spectroscopic Evolution of a Nearby GRB-Supernova and an Exceptionally Bright Afterglow at z=0.153

Brendan O'Connor , Malte Busmann , Xander J. Hall , Kenta Taguchi , Masaomi Tanaka , Daniel Gruen , Seiji Toshikage , Ariel J. Amsellem
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Ziyuan Zhu Antonella Palmese Dylan Green John Banovetz Yu-Han Yang Eleonora Troja Hendrik van Eerten Julius Gassert Mitra Maleki Steven Bailey Segev BenZvi Tomas Cabrera Keerthi Kunnumkai Adam Myers Christoph Ries David Schlegel Michael Schmidt Silona Wilke Muskan Yadav
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Pith reviewed 2026-05-20 08:00 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords gamma-ray burstType Ic-BL supernovaGRB-SN associationsupernova lightcurve modelinghost galaxy offsetnebular emissionmetallicity gradientafterglow
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The pith

Spectroscopy confirms GRB 260310A's supernova as a Type Ic-BL half as luminous as SN 1998bw with a 15 kpc offset.

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

This paper reports optical to near-infrared imaging and spectroscopy of the gamma-ray burst GRB 260310A and associated supernova SN 2026fgk at redshift 0.153. Spectra obtained more than two weeks after the explosion display broad absorption features that securely classify SN 2026fgk as a broad-lined Type Ic supernova. Multi-wavelength lightcurve modeling across grizJKs bands shows the supernova is roughly half as luminous as the reference event SN 1998bw, with a nickel mass of 0.4-0.5 solar masses, ejected mass of 4-6 solar masses, and kinetic energy of (3-8) times 10 to the 51 ergs. The GRB site lies at an extreme 15 kiloparsec offset from the host galaxy, connected by a bridge of nebular emission to a region of sub-solar metallicity around 0.4 solar. A sympathetic reader cares because this provides one of the closest spectroscopically confirmed GRB-supernovae for detailed study of explosion physics and galactic environments.

Core claim

The paper establishes that GRB 260310A is associated with SN 2026fgk, identified as a Type Ic-BL supernova through broad absorption features in spectra taken more than two weeks after explosion. Modeling of the multi-band lightcurve scaled from the SN 1998bw template with luminosity factor k_98bw of 0.4-0.6 yields M_Ni of 0.4-0.5 solar masses, M_ej of 4-6 solar masses, and E_K of (3-8) x 10^51 erg. The 15 kpc offset arises from the host's extended light profile rather than an isolated location, as shown by the nebular emission bridge and the sub-solar metallicity at the explosion site compared to near-solar in the host core.

What carries the argument

Late-time spectral identification of broad absorption features combined with multi-wavelength lightcurve modeling that scales the supernova component from the SN 1998bw template using a single luminosity scaling factor k_98bw.

If this is right

  • This event increases the number of spectroscopically confirmed GRB-supernovae within 1 Gpc to 12, enabling tighter comparisons of explosion parameters across the class.
  • The derived ejecta properties place SN 2026fgk on the lower-luminosity end of GRB-associated supernovae while remaining consistent with typical kinetic energies.
  • The large offset and connecting nebular emission demonstrate that GRB progenitors can occur in the outer disks of galaxies with sub-solar metallicity.
  • The exceptionally bright afterglow at low redshift provides a high-quality dataset for testing afterglow emission models without significant distance-related uncertainties.

Where Pith is reading between the lines

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

  • If similar large-offset events prove common, targeted searches in galactic outskirts may increase the detection rate of GRB-supernovae.
  • Future inclusion of viewing-angle corrections in lightcurve fits could narrow or shift the reported range of kinetic energies.
  • The metallicity gradient and emission bridge suggest that resolved studies of other GRB hosts could test whether outer-disk star formation preferentially produces such explosions.

Load-bearing premise

The supernova lightcurve can be modeled by scaling the SN 1998bw template with a single luminosity factor without substantial extra uncertainties from viewing angle, host extinction, or non-standard nickel distribution.

What would settle it

New spectroscopy that lacks the reported broad absorption features or multi-band photometry that deviates from the scaled 1998bw template by more than the modeled uncertainties would falsify the supernova classification and parameter estimates.

Figures

Figures reproduced from arXiv: 2605.18973 by Adam Myers, Antonella Palmese, Ariel J. Amsellem, Brendan O'Connor, Christoph Ries, Daniel Gruen, David Schlegel, Dylan Green, Eleonora Troja, Hendrik van Eerten, John Banovetz, Julius Gassert, Keerthi Kunnumkai, Kenta Taguchi, Malte Busmann, Masaomi Tanaka, Michael Schmidt, Mitra Maleki, Muskan Yadav, Segev Benzvi, Seiji Toshikage, Silona Wilke, Steven Bailey, Tomas Cabrera, Xander J. Hall, Yu-Han Yang, Ziyuan Zhu.

Figure 1
Figure 1. Figure 1: Gemini r-band acquisition image (3 × 15 s) from 2026-03-27 (T0+17.4 d) showing the placement of the Gemini spectroscopic long-slit (white) observation that covers both the GRB and the host galaxy. Later Gemini spectra were obtained using different position angles (blue for 2026-04-23; red for 2026-05-13). The length of the rectangles mimicking the slit are simply for visualization purposes, while the 1′′ w… view at source ↗
Figure 2
Figure 2. Figure 2: Normalized flux density relative to the flux den￾sity at the break time tbreak for the griK bands. This shows the different relative slopes of these bands after the break, as well as the late-time color evolution. data (≈ t −1.65±0.10 in g and ≈ t −1.47±0.10 in z and J). We show this in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Best-fit model (powerlaw+Arnett) to the multi-wavelength lightcurve of GRB 260310A in the observer-frame. The thick solid lines in each filter represent the total model. The thin dashed lines represent the broken power-law afterglow component and the dotted lines, shown only in the g- and r-bands to avoid clutter, represents the Arnett model lightcurve. Photometry presented in this work (FTW and Seimei) is… view at source ↗
Figure 4
Figure 4. Figure 4: Spectral sequence of GRB 260310A obtained with Seimei, DESI, HET, and Gemini. The spectra are smoothed with a Savitzky-Golay filter (thick lines) and the unsmoothed spectra (thin lines) are also shown. Emission lines and telluric absorption regions have been clipped from the spectra prior to smoothing. The spectra are initially well described by a powerlaw Fν ∝ ν −β with spectral index β ≈ 1.0 and later ev… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison between the best-fit model derived only from the photometry to the observed DESI and Gemini spectra at 8.1, 12.1, 17.4, and 26.3 d showing the onset and evolution of supernova features. The solid black line represents the total model (powerlaw+SN1998bw) while the blue dashed line represents the powerlaw component (Fν ∝ ν −β ) and the dashed purple line represents the spectral series of SN 1998bw… view at source ↗
Figure 6
Figure 6. Figure 6: Visualization of the 2D Gemini GMOS-N spectrum obtained on 2026-04-05 (T0 + 26.3 d). The spectrum covers both the host galaxy (bottom trace) and transient (top trace), as shown in [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Observed optical lightcurves of long GRBs (gray) and low-luminosity GRBs (black) compared to GRB 260310A (red circles). A few specific GRBs are highlighted for a more specific comparison. GRB 221009A (magenta) is shown both observed (dashed) and dust corrected (solid). Data has been compiled from T. J. Galama et al. (1998); J. Sollerman et al. (2000, 2002); E. Pian et al. (2006); J. Soller￾man et al. (2006… view at source ↗
Figure 8
Figure 8. Figure 8: The flux-stretching factor k98bw relative to SN 1998bw of GRB-SN is shown versus the isotropic-equivalent gamma-ray energy Eγ,iso release of the GRB prompt emis￾sion. The data was compiled from J. Hjorth & J. S. Bloom (2012); J. Greiner et al. (2015); Z. Cano et al. (2017a,b); L. Izzo et al. (2019); Y.-D. Hu et al. (2021); G. P. Srinivasara￾gavan et al. (2023); Y.-D. Hu et al. (2021); A. Rossi et al. (2026… view at source ↗
Figure 9
Figure 9. Figure 9: Cumulative distribution of projected physical off￾sets for long GRBs from their host galaxies (P. K. Blanchard et al. 2016; J. D. Lyman et al. 2017). The location of GRB 260310A is shown as a red vertical line. 2023), there is an obvious selection effect of identifying the faintest explosions, of both types, at low redshifts (z < 0.2). We find that GRB 260310A matches well with the distribution of other GR… view at source ↗
Figure 11
Figure 11. Figure 11: Best-fit model (powerlaw+SN 1998bw) to the multi-wavelength lightcurve of GRB 260310A in the observer-frame. The thick solid lines in each filter represent the total model. The thin dashed lines represent the broken power-law afterglow component and the dotted lines, shown only in the g- and r-bands to avoid clutter, represent the model lightcurve of SN 1998bw with a flux scaling factor k98bw = 0.50. Phot… view at source ↗
read the original abstract

The association of broad-lined Type Ic supernovae with long-duration gamma-ray bursts (GRBs) has been known for 28 years. However, only about seventy gamma-ray burst supernovae (GRB-SNe) have been identified, of which only half have spectroscopic classifications. At $z=0.153$, GRB 260310A is the 12th spectroscopically confirmed GRB-SN discovered within 1 Gpc, offering a critical opportunity to follow one of these rare supernovae in detail. We present optical to near-infrared imaging and spectroscopy of GRB 260310A and SN 2026fgk out to 65 d after discovery. The optical afterglow is among the brightest ever observed from a GRB. Spectra obtained more than two weeks after the explosion reveal broad absorption features that securely identify SN 2026fgk as a Type Ic-BL supernova. Modeling of the multi-wavelength ($grizJK_s$) lightcurve shows that the supernova is approximately half the luminosity ($k_\textrm{98bw}=0.4-0.6$) of the canonical GRB-SN 1998bw. We derive a nickel mass of $M_\textrm{Ni}=0.4-0.5$ $M_\odot$ with a total ejected mass of $M_\textrm{ej}\approx4-6 $ $M_\odot$ and kinetic energy $E_\textrm{K}=(3-8)\times10^{51}$ erg. The GRB exploded at an extremely large offset of 15 kpc from its host galaxy. Long-slit spectra reveal a ``bridge'' of nebular emission extending along the galaxy's disk to the GRB location, which has a sub-solar metallicity ($\sim$\,$0.4Z_\odot$), compared to a near solar metallicity for the host galaxy. This indicates that the large offset arises from the galaxy's extended light profile rather than an isolated environment.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 1 minor

Summary. The manuscript reports observations of GRB 260310A and associated SN 2026fgk at z=0.153, with optical-to-NIR imaging and spectroscopy out to 65 days. Spectra more than two weeks post-explosion show broad absorption features that classify SN 2026fgk as a Type Ic-BL supernova. After subtracting the bright afterglow, multi-wavelength (grizJK_s) lightcurve modeling scales the SN 1998bw template by a single factor k_98bw=0.4-0.6, yielding M_Ni=0.4-0.5 M_⊙, M_ej≈4-6 M_⊙, and E_K=(3-8)×10^51 erg. The GRB site lies at a 15 kpc offset with sub-solar metallicity (~0.4 Z_⊙) connected by a nebular emission bridge.

Significance. If the modeling is robust, the work enlarges the small sample of spectroscopically confirmed nearby GRB-SNe and supplies quantitative explosion parameters together with environmental context at large offset. The exceptionally bright afterglow and metallicity measurement add useful constraints on progenitor channels and host-galaxy structure.

major comments (1)
  1. [lightcurve modeling] Lightcurve modeling (abstract and associated section): the reported values M_Ni=0.4-0.5 M_⊙, M_ej≈4-6 M_⊙, E_K=(3-8)×10^51 erg are obtained by applying a single multiplicative scaling k_98bw=0.4-0.6 to the SN 1998bw template after afterglow subtraction. Because GRB-SNe are known to be aspherical, the absence of explicit treatment of viewing-angle mismatch, line-of-sight extinction, or nickel-distribution differences introduces systematics that can shift the inferred bolometric luminosity and therefore the derived masses and energy by factors comparable to the quoted ranges.
minor comments (1)
  1. [abstract] Abstract: the phrase 'more than two weeks after the explosion' for the spectra could be replaced by the precise rest-frame or observer-frame epoch to improve clarity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address the single major comment on lightcurve modeling below, providing a point-by-point response while maintaining the integrity of our analysis.

read point-by-point responses

  1. Referee: Lightcurve modeling (abstract and associated section): the reported values M_Ni=0.4-0.5 M_⊙, M_ej≈4-6 M_⊙, E_K=(3-8)×10^51 erg are obtained by applying a single multiplicative scaling k_98bw=0.4-0.6 to the SN 1998bw template after afterglow subtraction. Because GRB-SNe are known to be aspherical, the absence of explicit treatment of viewing-angle mismatch, line-of-sight extinction, or nickel-distribution differences introduces systematics that can shift the inferred bolometric luminosity and therefore the derived masses and energy by factors comparable to the quoted ranges.

    Authors: We agree that the template-scaling approach carries inherent systematics due to the aspherical nature of GRB-SNe, potential viewing-angle effects, and variations in nickel distribution or extinction. This method is nevertheless the standard technique applied to the majority of spectroscopically confirmed GRB-SNe in the literature when full spectroscopic time series are unavailable (as is the case here after +14 d). The broad ranges we quote for M_Ni, M_ej, and E_K already reflect the dominant uncertainty from the scaling factor k_98bw itself. To strengthen the manuscript we will add a dedicated paragraph in the modeling section that explicitly discusses these limitations, references comparable analyses of other GRB-SNe, and notes that the reported parameter ranges should be interpreted as approximate rather than precise. We do not believe a full re-derivation with 3-D models is justified by the existing data quality, but the added discussion will make the caveats transparent. revision: partial

Circularity Check

0 steps flagged

Template scaling from external SN 1998bw observations introduces no circularity

full rationale

The paper's central quantitative claims follow from fitting a single multiplicative scaling factor k_98bw=0.4-0.6 to the observed grizJK_s lightcurve after afterglow subtraction, then applying standard relations to obtain M_Ni, M_ej and E_K. This uses an external template (SN 1998bw) whose photometry and properties are independent of the present dataset. Spectroscopic classification as Type Ic-BL rests on directly observed broad absorption features more than two weeks post-explosion. No load-bearing step reduces by construction to a fitted input, self-citation chain, or ansatz imported from the authors' prior work; the derivation remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central results rest on template scaling from SN 1998bw and standard assumptions about supernova lightcurve physics; no new entities postulated.

free parameters (2)
  • k_98bw luminosity scaling factor
    Fitted scaling of supernova luminosity relative to SN 1998bw template to match observed lightcurve.
  • nickel mass M_Ni
    Derived from lightcurve modeling and reported as 0.4-0.5 solar masses.
axioms (1)
  • domain assumption Broad absorption features in spectra more than two weeks post-explosion securely identify Type Ic-BL classification.
    Standard spectroscopic classification criterion invoked without additional verification steps shown in abstract.

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Works this paper leans on

189 extracted references · 189 canonical work pages · 12 internal anchors

  1. [1]

    J.168(2), 58 (2024), doi:10.3847/1538-3881/ad3217

    Adame, A. G., et al. 2024, Astron. J., 168, 58, doi: 10.3847/1538-3881/ad3217

    work page doi:10.3847/1538-3881/ad3217 2024

  2. [2]

    2011, ApJS, 193, 29, doi: 10.1088/0067-0049/193/2/29

    Aihara, H., Allende Prieto, C., An, D., et al. 2011, ApJS, 193, 29, doi: 10.1088/0067-0049/193/2/29

    work page doi:10.1088/0067-0049/193/2/29 2011

  3. [3]

    2007, , 374, 1413, 10.1111/j.1365-2966.2006.11246.x

    Amati, L. 2006, MNRAS, 372, 233, doi: 10.1111/j.1365-2966.2006.10840.x

    work page doi:10.1111/j.1365-2966.2006.10840.x 2006

  4. [4]

    2002, A&A, 390, 81, doi: 10.1051/0004-6361:20020722

    Amati, L., Frontera, F., Tavani, M., et al. 2002, A&A, 390, 81, doi: 10.1051/0004-6361:20020722

    work page doi:10.1051/0004-6361:20020722 2002

  5. [5]

    Arnett, W. D. 1982, ApJ, 253, 785, doi: 10.1086/159681

    work page doi:10.1086/159681 1982

  6. [6]

    A., Pian, E., et al

    Ashall, C., Mazzali, P. A., Pian, E., et al. 2019, MNRAS, 487, 5824, doi: 10.1093/mnras/stz1588

    work page doi:10.1093/mnras/stz1588 2019

  7. [7]

    D., et al

    Ashton, G., H¨ ubner, M., Lasky, P. D., et al. 2019, ApJS, 241, 27, doi: 10.3847/1538-4365/ab06fc Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167, doi: 10.3847/1538-4357/ac7c74

    work page doi:10.3847/1538-4365/ab06fc 2019

  8. [8]

    2026, GRB Coordinates Network, 43981, 1

    Atteia, J.-L., Moreno M´ endez, E., Lincetto, M., et al. 2026, GRB Coordinates Network, 43981, 1

    work page 2026

  9. [9]

    A., Phillips, M

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

    work page doi:10.1086/130766 1981

  10. [10]

    2016,, Astrophysics Source Code Library, record ascl:1611.017 http://ascl.net/1611.017

    Barbary, K., Barclay, T., Biswas, R., et al. 2016,, Astrophysics Source Code Library, record ascl:1611.017 http://ascl.net/1611.017

    work page 2016

  11. [11]

    2026, GRB Coordinates Network, 44043, 1

    Belkin, S., & Shrestha, M. 2026, GRB Coordinates Network, 44043, 1

    work page 2026

  12. [12]

    R., Pooley, G., et al

    Berger, E., Kulkarni, S. R., Pooley, G., et al. 2003, Nature, 426, 154, doi: 10.1038/nature01998

    work page doi:10.1038/nature01998 2003

  13. [13]

    2006, in Astronomical Society of the Pacific Conference Series, Vol

    Bertin, E. 2006, in Astronomical Society of the Pacific Conference Series, Vol. 351, Astronomical Data Analysis Software and Systems XV, ed. C. Gabriel, C. Arviset, D. Ponz, & S. Enrique, 112

    work page 2006

  14. [14]

    2010, http://ascl.net/1010.068

    Bertin, E. 2010, http://ascl.net/1010.068

    work page 2010

  15. [15]

    1996a, A&AS, 117, 393, doi: 10.1051/aas:1996164 —

    Bertin, E., & Arnouts, S. 1996, A&AS, 117, 393, doi: 10.1051/aas:1996164

    work page doi:10.1051/aas:1996164 1996

  16. [16]

    2002, in Astronomical Society of the Pacific Conference Series, Vol

    Bertin, E., Mellier, Y., Radovich, M., et al. 2002, in Astronomical Society of the Pacific Conference Series, Vol. 281, Astronomical Data Analysis Software and Systems XI, ed. D. A. Bohlender, D. Durand, & T. H. Handley, 228

    work page 2002

  17. [17]

    S., Levan, A

    Bhirombhakdi, K., Fruchter, A. S., Levan, A. J., et al. 2024, ApJ, 977, 256, doi: 10.3847/1538-4357/ad8dd8 Bj¨ ornsson, C.-I., & Fransson, C. 2004, ApJ, 605, 823, doi: 10.1086/382584 GRB 260310A/SN 2026fgk17 T able 2.Log of spectroscopic observations of GRB 260310A/SN 2026fgk. Start Date (UTC)δt(days) Telescope Instrument Grating Exposure (s) 2026-03-14 1...

    work page doi:10.3847/1538-4357/ad8dd8 2024

  18. [18]

    K., Berger, E., & Fong, W.-f

    Blanchard, P. K., Berger, E., & Fong, W.-f. 2016, ApJ, 817, 144, doi: 10.3847/0004-637X/817/2/144

    work page doi:10.3847/0004-637x/817/2/144 2016

  19. [19]

    K., Villar, V

    Blanchard, P. K., Villar, V. A., Chornock, R., et al. 2024, Nature Astronomy, 8, 774, doi: 10.1038/s41550-024-02237-4

    work page doi:10.1038/s41550-024-02237-4 2024

  20. [20]

    S., Kulkarni, S

    Bloom, J. S., Kulkarni, S. R., & Djorgovski, S. G. 2002, AJ, 123, 1111, doi: 10.1086/338893

    work page doi:10.1086/338893 2002

  21. [21]

    S., Kulkarni, S

    Bloom, J. S., Kulkarni, S. R., Djorgovski, S. G., et al. 1999, Nature, 401, 453, doi: 10.1038/46744

    work page doi:10.1038/46744 1999

  22. [22]

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

    Bradley, L., Sip˝ ocz, B., Robitaille, T., et al. 2024,, 2.0.2 Zenodo, doi: 10.5281/zenodo.13989456

    work page doi:10.5281/zenodo.13989456 2024

  23. [23]

    2026, GRB Coordinates Network, 44004, 1

    Brivio, R., Malesani, D., Izzo, L., et al. 2026, GRB Coordinates Network, 44004, 1

    work page 2026

  24. [24]

    2012, ApJ, 753, 67, doi: 10.1088/0004-637X/753/1/67

    Bufano, F., Pian, E., Sollerman, J., et al. 2012, ApJ, 753, 67, doi: 10.1088/0004-637X/753/1/67

    work page doi:10.1088/0004-637x/753/1/67 2012

  25. [25]

    2025, arXiv e-prints, arXiv:2503.14588, doi: 10.48550/arXiv.2503.14588

    Busmann, M., O’Connor, B., Sommer, J., et al. 2025, arXiv e-prints, arXiv:2503.14588, doi: 10.48550/arXiv.2503.14588

    work page doi:10.48550/arxiv.2503.14588 2025

  26. [26]

    J., et al

    Campana, S., Mangano, V., Blustin, A. J., et al. 2006, Nature, 442, 1008, doi: 10.1038/nature04892

    work page doi:10.1038/nature04892 2006

  27. [27]

    2013, MNRAS, 434, 1098, doi: 10.1093/mnras/stt1048

    Cano, Z. 2013, MNRAS, 434, 1098, doi: 10.1093/mnras/stt1048

    work page doi:10.1093/mnras/stt1048 2013

  28. [28]

    2017a, Advances in Astronomy, 2017, 8929054, doi: 10.1155/2017/8929054

    Cano, Z., Wang, S.-Q., Dai, Z.-G., & Wu, X.-F. 2017a, Advances in Astronomy, 2017, 8929054, doi: 10.1155/2017/8929054

    work page doi:10.1155/2017/8929054 2017

  29. [29]

    2011, ApJ, 740, 41, doi: 10.1088/0004-637X/740/1/41

    Cano, Z., Bersier, D., Guidorzi, C., et al. 2011, ApJ, 740, 41, doi: 10.1088/0004-637X/740/1/41

    work page doi:10.1088/0004-637x/740/1/41 2011

  30. [30]

    2017b, A&A, 605, A107, doi: 10.1051/0004-6361/201731005

    Cano, Z., Izzo, L., de Ugarte Postigo, A., et al. 2017b, A&A, 605, A107, doi: 10.1051/0004-6361/201731005

    work page doi:10.1051/0004-6361/201731005

  31. [31]

    2012,, Astrophysics Source Code Library, record ascl:1210.002 http://ascl.net/1210.002

    Cappellari, M. 2012,, Astrophysics Source Code Library, record ascl:1210.002 http://ascl.net/1210.002

    work page 2012

  32. [32]

    , archivePrefix = "arXiv", eprint =

    Cappellari, M. 2017, MNRAS, 466, 798, doi: 10.1093/mnras/stw3020

    work page internal anchor Pith review doi:10.1093/mnras/stw3020 2017

  33. [33]

    , eprint =

    Cappellari, M., & Emsellem, E. 2004, PASP, 116, 138, doi: 10.1086/381875

    work page doi:10.1086/381875 2004

  34. [34]

    2003, , 115, 763, 10.1086/376392

    Chabrier, G. 2003, PASP, 115, 763, doi: 10.1086/376392

    work page internal anchor Pith review doi:10.1086/376392 2003

  35. [35]

    The Pan-STARRS1 Surveys

    Chambers, K. C., Magnier, E. A., Metcalfe, N., et al. 2016, arXiv e-prints, arXiv:1612.05560. https://arxiv.org/abs/1612.05560

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  36. [36]

    Chevalier, R. A. 1982, ApJ, 259, 302, doi: 10.1086/160167

    work page doi:10.1086/160167 1982

  37. [37]

    A., & Fransson, C

    Chevalier, R. A., & Fransson, C. 2006, ApJ, 651, 381, doi: 10.1086/507606

    work page doi:10.1086/507606 2006

  38. [38]

    S., Hill, G

    Chonis, T. S., Hill, G. J., Lee, H., Tuttle, S. E., & Vattiat, B. L. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9147, Ground-based and Airborne Instrumentation for Astronomy V, ed. S. K. Ramsay, I. S. McLean, & H. Takami, 91470A, doi: 10.1117/12.2056005

    work page doi:10.1117/12.2056005 2014

  39. [39]

    S., Hill, G

    Chonis, T. S., Hill, G. J., Lee, H., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J. Evans, L. Simard, & H. Takami, 99084C, doi: 10.1117/12.2232209

    work page doi:10.1117/12.2232209 2016

  40. [40]

    Spectroscopic Discovery of the Broad-Lined Type Ic Supernova 2010bh Associated with the Low-Redshift GRB 100316D

    Chornock, R., Berger, E., Levesque, E. M., et al. 2010, arXiv e-prints, arXiv:1004.2262, doi: 10.48550/arXiv.1004.2262

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1004.2262 2010

  41. [41]

    M., Sollerman, J., et al

    Christensen, L., Vreeswijk, P. M., Sollerman, J., et al. 2008, A&A, 490, 45, doi: 10.1051/0004-6361:200809896

    work page doi:10.1051/0004-6361:200809896 2008

  42. [42]

    First Detection of Faraday Rotation in a Gamma-Ray Burst Afterglow: Low Polarization and High Rotation Measure in GRB 260310A Reveal Jet Magnetic Structure and Environment

    Christy, C. T., Laskar, T., Alexander, K. D., et al. 2026, arXiv e-prints, arXiv:2604.27480. https://arxiv.org/abs/2604.27480

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  43. [43]

    B., Covarrubias, R., & Candia, P

    Clocchiatti, A., Suntzeff, N. B., Covarrubias, R., & Candia, P. 2011, AJ, 141, 163, doi: 10.1088/0004-6256/141/5/163

    work page doi:10.1088/0004-6256/141/5/163 2011

  44. [44]

    2026, GRB Coordinates Network, 44105, 1 de Ugarte Postigo, A., Th¨ one, C

    Corcoran, G., Martin-Carrillo, A., Izzo, L., et al. 2026, GRB Coordinates Network, 44105, 1 de Ugarte Postigo, A., Th¨ one, C. C., Bensch, K., et al. 2018, A&A, 620, A190, doi: 10.1051/0004-6361/201833636 de Ugarte Postigo, A., Th¨ one, C. C., Mart´ ın, S., et al. 2020, A&A, 633, A68, doi: 10.1051/0004-6361/201936668 18O’Connor et al. 101 Time since T0 (d...

    work page doi:10.1051/0004-6361/201833636 2026

  45. [45]

    The DESI Experiment Part II: Instrument Design

    Nomoto, K. 2005, ApJ, 624, 898, doi: 10.1086/429284 DESI Collaboration, Aghamousa, A., Aguilar, J., et al. 2016, arXiv, doi: 10.48550/arXiv.1611.00037 DESI Collaboration, Abdul-Karim, M., Adame, A. G., et al. 2025a, arXiv, doi: 10.48550/arXiv.2503.14745 DESI Collaboration, Abdul-Karim, M., Aguilar, J., et al. 2025b, https://arxiv.org/abs/2503.14738v2

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/429284 2005

  46. [46]

    Eyles-Ferris, R. A. J., Jonker, P. G., Levan, A. J., et al. 2025, arXiv e-prints, arXiv:2504.08886. https://arxiv.org/abs/2504.08886

    work page arXiv 2025

  47. [47]

    2011, ApJ, 726, 32, doi: 10.1088/0004-637X/726/1/32 GRB 260310A/SN 2026fgk19 Fermi GBM Team

    Fan, Y.-Z., Zhang, B.-B., Xu, D., Liang, E.-W., & Zhang, B. 2011, ApJ, 726, 32, doi: 10.1088/0004-637X/726/1/32 GRB 260310A/SN 2026fgk19 Fermi GBM Team. 2026, GRB Coordinates Network, 43951, 1

    work page doi:10.1088/0004-637x/726/1/32 2011

  48. [48]

    A., Zeh, A., et al

    Ferrero, P., Kann, D. A., Zeh, A., et al. 2006, A&A, 457, 857, doi: 10.1051/0004-6361:20065530

    work page doi:10.1051/0004-6361:20065530 2006

  49. [49]

    Filippenko, A. V. 1982, PASP, 94, 715, doi: 10.1086/131052

    work page doi:10.1086/131052 1982

  50. [50]

    2025, Astronomy and Computing, 52, 100954, doi: 10.1016/j.ascom.2025.100954

    Finneran, G., Cotter, L., & Martin-Carrillo, A. 2025, Astronomy and Computing, 52, 100954, doi: 10.1016/j.ascom.2025.100954

    work page doi:10.1016/j.ascom.2025.100954 2025

  51. [51]

    S., Levan, A

    Fruchter, A. S., Levan, A. J., Strolger, L., et al. 2006, Nature, 441, 463, doi: 10.1038/nature04787

    work page doi:10.1038/nature04787 2006

  52. [52]

    D., Smartt, S

    Fulton, M. D., Smartt, S. J., Rhodes, L., et al. 2023, ApJL, 946, L22, doi: 10.3847/2041-8213/acc101

    work page doi:10.3847/2041-8213/acc101 2023

  53. [53]

    J., Vreeswijk, P

    Galama, T. J., Vreeswijk, P. M., van Paradijs, J., et al. 1998, Nature, 395, 670, doi: 10.1038/27150

    work page doi:10.1038/27150 1998

  54. [54]

    J., Vreeswijk, P

    Galama, T. J., Vreeswijk, P. M., van Paradijs, J., et al. 1999, A&AS, 138, 465, doi: 10.1051/aas:1999311

    work page doi:10.1051/aas:1999311 1999

  55. [55]

    2004, The Astrophysical Journal, 611, 1005, doi: 10.1086/422091

    Gehrels, N., Chincarini, G., Giommi, P., et al. 2004, ApJ, 611, 1005, doi: 10.1086/422091

    work page doi:10.1086/422091 2004

  56. [56]

    2026, GRB Coordinates Network, 44045, 1 G¨ ossl, C

    Giarratana, S., Giroletti, M., Ghirlanda, G., et al. 2026, GRB Coordinates Network, 44045, 1 G¨ ossl, C. A., & Riffeser, A. 2002, A&A, 381, 1095, doi: 10.1051/0004-6361:20011522

    work page doi:10.1051/0004-6361:20011522 2026

  57. [57]

    Granot, J., Panaitescu, A., Kumar, P., & Woosley, S. E. 2002, ApJL, 570, L61, doi: 10.1086/340991

    work page doi:10.1086/340991 2002

  58. [58]

    2002, ApJ, 568, 820, doi: 10.1086/338966

    Granot, J., & Sari, R. 2002, ApJ, 568, 820, doi: 10.1086/338966

    work page doi:10.1086/338966 2002

  59. [59]

    A., Kann, D

    Greiner, J., Mazzali, P. A., Kann, D. A., et al. 2015, Nature, 523, 189, doi: 10.1038/nature14579

    work page doi:10.1038/nature14579 2015

  60. [60]

    2023, AJ, 165, 144, doi: 10.3847/1538-3881/acb212

    Guy, J., Bailey, S., Kremin, A., et al. 2023, The Astronomical Journal, 165, 144, doi: 10.3847/1538-3881/acb212

    work page doi:10.3847/1538-3881/acb212 2023

  61. [61]

    J., Palmese, A., O’Connor, B., et al

    Hall, X. J., Palmese, A., O’Connor, B., et al. 2025, arXiv e-prints, arXiv:2510.23723, doi: 10.48550/arXiv.2510.23723

    work page doi:10.48550/arxiv.2510.23723 2025

  62. [62]

    J., Palmese, A., BenZvi, S., et al

    Hall, X. J., Palmese, A., BenZvi, S., et al. 2026, arXiv e-prints, arXiv:2601.12611, doi: 10.48550/arXiv.2601.12611

    work page doi:10.48550/arxiv.2601.12611 2026

  63. [63]

    2026, GRB Coordinates Network, 43975, 1

    Hamburg, R., & Meegan, C. 2026, GRB Coordinates Network, 43975, 1

    work page 2026

  64. [64]

    H., Hammer, F., Liang, Y

    Han, X. H., Hammer, F., Liang, Y. C., et al. 2010, A&A, 514, A24, doi: 10.1051/0004-6361/200912475

    work page doi:10.1051/0004-6361/200912475 2010

  65. [65]

    E., Malesani, D., Wiersema, K., et al

    Heintz, K. E., Malesani, D., Wiersema, K., et al. 2018, MNRAS, 474, 2738, doi: 10.1093/mnras/stx2895

    work page doi:10.1093/mnras/stx2895 2018

  66. [66]

    J., Lee, H., MacQueen, P

    Hill, G. J., Lee, H., MacQueen, P. J., et al. 2021, AJ, 162, 298, doi: 10.3847/1538-3881/ac2c02

    work page doi:10.3847/1538-3881/ac2c02 2021

  67. [67]

    J., Perley, D

    Hinds, K., Hall, X. J., Perley, D. A., et al. 2026, Transient Name Server AstroNote, 65, 1

    work page 2026

  68. [68]

    A., Ho, A

    Hinds, K.-R., Perley, D. A., Ho, A. Y. Q., et al. 2026, GRB Coordinates Network, 43977, 1

    work page 2026

  69. [69]

    2013, Philosophical Transactions of the Royal Society of London Series A, 371, 20120275, doi: 10.1098/rsta.2012.0275

    Hjorth, J. 2013, Philosophical Transactions of the Royal Society of London Series A, 371, 20120275, doi: 10.1098/rsta.2012.0275

    work page doi:10.1098/rsta.2012.0275 2013

  70. [70]

    Hjorth, J., & Bloom, J. S. 2012, in Chapter 9 in ”Gamma-Ray Bursts, ed. C. Kouveliotou, R. A. M. J. Wijers, & S. Woosley, 169–190, doi: 10.48550/arXiv.1104.2274

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1104.2274 2012

  71. [71]

    2003, Nature, 423, 847, doi: 10.1038/nature01750

    Hjorth, J., Sollerman, J., Møller, P., et al. 2003, Nature, 423, 847, doi: 10.1038/nature01750

    work page doi:10.1038/nature01750 2003

  72. [72]

    2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Hopp, U., Bender, R., Grupp, F., et al. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9145, Ground-based and Airborne Telescopes V, ed. L. M. Stepp, R. Gilmozzi, & H. J. Hall, 91452D, doi: 10.1117/12.2054498

    work page doi:10.1117/12.2054498 2014

  73. [73]

    2026, GRB Coordinates Network, 43986, 1

    Hsu, B., Shrestha, M., Andrews, J., et al. 2026, GRB Coordinates Network, 43986, 1

    work page 2026

  74. [75]

    2022, The Astrophysical Journal, 936, 157, doi: 10.3847/1538-4357/ac7394

    Hu, L., Wang, L., Chen, X., & Yang, J. 2022, The Astrophysical Journal, 936, 157, doi: 10.3847/1538-4357/ac7394

    work page doi:10.3847/1538-4357/ac7394 2022

  75. [76]

    J., Kumar, A., et al

    Hu, Y.-D., Castro-Tirado, A. J., Kumar, A., et al. 2021, A&A, 646, A50, doi: 10.1051/0004-6361/202039349

    work page doi:10.1051/0004-6361/202039349 2021

  76. [77]

    A., Nomoto, K., et al

    Iwamoto, K., Mazzali, P. A., Nomoto, K., et al. 1998, Nature, 395, 672, doi: 10.1038/27155

    work page doi:10.1038/27155 1998

  77. [78]

    C., Schulze, S., et al

    Izzo, L., Th¨ one, C. C., Schulze, S., et al. 2017, MNRAS, 472, 4480, doi: 10.1093/mnras/stx2244

    work page doi:10.1093/mnras/stx2244 2017

  78. [79]

    2019, Nature, 565, 324, doi: 10.1038/s41586-018-0826-3

    Izzo, L., de Ugarte Postigo, A., Maeda, K., et al. 2019, Nature, 565, 324, doi: 10.1038/s41586-018-0826-3

    work page doi:10.1038/s41586-018-0826-3 2019

  79. [80]

    B., et al

    Izzo, L., Martin-Carrillo, A., Malesani, D. B., et al. 2025, GRB Coordinates Network, 39851, 1

    work page 2025

  80. [81]

    A., Klose, S., & Zeh, A

    Kann, D. A., Klose, S., & Zeh, A. 2006, ApJ, 641, 993, doi: 10.1086/500652

    work page doi:10.1086/500652 2006

Showing first 80 references.