Observatory, NAO-2 m (4.05 d in *r*', *i*') at Rozhen NAO,<fnref n="21" /> C2PU (10.10 d in *r*') at Calern observatory, CFHT-Megacam (30.48 d in *g*', *r*', *i*') at Mauna Kea Observatory.

Near-infrared (NIR) observations of GRB 230812B were carried out with the Italian 3.6-m TNG telescope, sited in Canary Island, using the NICS instrument in imaging mode. A series of images were obtained with the J and K filters on 2023 August 16 (i.e. about 4.1 d after the burst) and with the J filter only on 2023 August 21 and 2023 October 11 (i.e. about 9.1 and 60.1 d after the burst).

In addition to the professional network, GRANDMA activated its Kilonova-Catcher (KNC) citizen science programme for further observations with amateurs’ telescopes.

The GRANDMA observations and its partners are listed in Table A2, which includes the start time $T_{\text{mid}}$ time (in ISO format with post-trigger delay) and the host-galaxy/extinction-corrected brightness (in AB magnitudes) of the observations, as well as the uncorrected magnitudes. The exposure times, names of telescopes, and filters used are mentioned for each observation. Our method for calculating the magnitudes is described in the Section 2.2, including our methods of photometry transient detection, magnitude system conversion, Milky Way extinction correction, and host galaxy flux subtraction.

## APPENDIX B: SPECTROSCOPIC OBSERVATION DETAILS

We used OSIRIS+ (Cepa et al. 2000) mounted on the 10.4m Gran Telescopio Canarias (GTC) telescope at Roque de los Muchachos Observatory in La Palma, Canary Islands, Spain, to observe the afterglow and supernova that follow GRB 230812B. The observation consisted of spectroscopy with an exposure time of 3x900s and grism R1000B, with a wavelength coverage between 3600 and 7800 Å. The first spectrum started at 21.37 UT, 1.110 d after the burst, while the on 2023 August 24 at 21.79 h UT, 12.12 d after the GRB detection, close to the peak of the supernova emission (Agúf Fernández et al. 2023; de Ugarte Postigo et al. 2023a).

The last two epochs were initially programmed to be obtained with larger spacing between epochs, but due to weather and telescope scheduling they ended up being rather close in time. The first epoch was obtained with a single grism, R1000B, covering the range between 3700 and 7880 Å. The second epoch included two grisms, R1000B and R1000R, this second one adding coverage between 5100 and 10100 Å to cover the full optical spectrum.

## APPENDIX C: SKYPORTAL

To store, display, and annotate GRANDMA data products in a follow-up campaign, we use SKYPORTAL (van der Walt, Crellin-Quick & Bloom 2019; Coughlin et al. 2023), a powerful data base, API, and web application for time-domain astronomy. We use it for its capabilities of ingesting multimessenger triggers from GCNs in real-time, from where network-cognizant observation plans are automatically generated using GWEMOPT (Coughlin et al. 2018). It also enables

automated ingestion of transients from the Transient Name Server (TNS) identified by surveys such as the Zwicky Transient Facility (Bellm et al. 2019; Graham et al. 2019), the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) (Morgan et al. 2012), or the Asteroid Terrestrial-impact Last Alert System (ATLAS) (Tonry et al. 2018); it is from TNS that we retrieved the discovery photometry. We store photometry information, including flux and limiting magnitude measurements from follow-up observations by GRANDMA’s telescopes within SKYPORTAL, supplementing the data imported from TNS, to create light curves. From the dedicated source page, easy access is provided to many other database services, such as Vizier (Ochsenbein, Bauer & Marcout 2000). Finally, SKYPORTAL is used for simplifying interactions with Bayesian inference frameworks such as the Nuclear physics and Multimessenger Astronomy framework NMMA (Dietrich et al. 2020; Pang et al. ), which we discuss more in the main text. Operations on SKYPORTAL are conducted and monitored by ‘shifters’, members of the collaboration organized in teams every week, and divided into four daily slots of six hours each to accommodate timezone constraints while maintaining 24/7 coverage. Shifters look out for new candidates from surveys (particularly LIGO-Virgo-KAGRA, LVK) and new GCN events on the platform and report on associated Slack channels which candidates are to be followed up or not based on pre-defined criteria. The shifts are also organized using SKYPORTAL’s dedicated page in the form of a calendar. Shifters or members of telescope teams are expected to upload executed observations data either manually or programmatically using the API. GCN circular-like documents can even be automatically generated, ensuring consistent formatting of the results reported to the General Coordinates Network while reducing the possibility for human errors to be made.

## APPENDIX D: COMPARING DIFFERENT ASTROPHYSICAL SCENARIOS WITH NMMA

As discussed in Section 4.2, using NMMA, we can quantitatively compare different astrophysical scenarios in a Bayesian framework. We have performed studies using various models and jet geometries. NMMA is able to perform joint Bayesian inference of multimessenger events containing gravitational waves, GRB afterglows, SNe, or kilonovae. In addition to scenarios mentioned above, we also consider two kilonova models, Bu2023Ye (Anand et al. 2023) and Ka2017 (Kasen et al. 2017), to accompany the Top-hat model as possible explanations of the data set. The log Bayes factor $\ln B$ of various models relative to the Power-law+SN, which is the best-performing model to be introduced shortly, can be found in Table D1. The posterior of $\sigma_{\text{sys}}$ is also shown in Table D1. The Power-law+SN has the lowest value of $\sigma_{\text{sys}}$, thus signifying a better fit compared to other models. Comparing the differences between the log Bayes factor of scenarios with and without an SN component, we conclude that the presence of an SN component is statistically supported from a Bayesian perspective.

The posterior values of all the considered models is summarized in Table D2. The best-fitting light curves for the three GRB+SN scenarios are shown in Fig. D1.

<footnote n="21">²¹Using the focal reducer FoReRo-2 (Jockers et al. 2000).</footnote>
Observatory, NAO-2 m (4.05 d in *r*', *i*') at Rozhen NAO,<fnref n="21" /> C2PU (10.10 d in *r*') at Calern observatory, CFHT-Megacam (30.48 d in *g*', *r*', *i*') at Mauna Kea Observatory.

Near-infrared (NIR) observations of GRB 230812B were carried
out with the Italian 3.6-m TNG telescope, sited in Canary Island,
using the NICS instrument in imaging mode. A series of images
were obtained with the J and K filters on 2023 August 16 (i.e. about
4.1 d after the burst) and with the J filter only on 2023 August 21 and
2023 October 11 (i.e. about 9.1 and 60.1 d after the burst).

In addition to the professional network, GRANDMA activated its Kilonova-Catcher (KNC) citizen science programme for further observations with amateurs’ telescopes.

The GRANDMA observations and its partners are listed in Table A2, which includes the start time $T_{\text{mid}}$ time (in ISO format with post-trigger delay) and the host-galaxy/extinction-corrected brightness (in AB magnitudes) of the observations, as well as the uncorrected magnitudes. The exposure times, names of telescopes, and filters used are mentioned for each observation. Our method for calculating the magnitudes is described in the Section 2.2, including our methods of photometry transient detection, magnitude system conversion, Milky Way extinction correction, and host galaxy flux subtraction.

## APPENDIX B: SPECTROSCOPIC OBSERVATION DETAILS

We used OSIRIS+ (Cepa et al. 2000) mounted on the 10.4m Gran Telescopio Canarias (GTC) telescope at Roque de los Muchachos Observatory in La Palma, Canary Islands, Spain, to observe the afterglow and supernova that follow GRB 230812B. The observation consisted of spectroscopy with an exposure time of 3x900s and grism R1000B, with a wavelength coverage between 3600 and 7800 Å. The first spectrum started at 21.37 UT, 1.110 d after the burst, while the on 2023 August 24 at 21.79 h UT, 12.12 d after the GRB detection, close to the peak of the supernova emission (Agúf Fernández et al. 2023; de Ugarte Postigo et al. 2023a).

The last two epochs were initially programmed to be obtained with larger spacing between epochs, but due to weather and telescope scheduling they ended up being rather close in time. The first epoch was obtained with a single grism, R1000B, covering the range between 3700 and 7880 Å. The second epoch included two grisms, R1000B and R1000R, this second one adding coverage between 5100 and 10100 Å to cover the full optical spectrum.

## APPENDIX C: SKYPORTAL

To store, display, and annotate GRANDMA data products in a follow-
up campaign, we use SKYPORTAL (van der Walt, Crellin-Quick &
Bloom 2019; Coughlin et al. 2023), a powerful data base, API, and
web application for time-domain astronomy. We use it for its capabil-
ities of ingesting multimessenger triggers from GCNs in real-time,
from where network-cognizant observation plans are automatically
generated using GWEMOPT (Coughlin et al. 2018). It also enables

automated ingestion of transients from the Transient Name Server (TNS) identified by surveys such as the Zwicky Transient Facility (Bellm et al. 2019; Graham et al. 2019), the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) (Morgan et al. 2012), or the Asteroid Terrestrial-impact Last Alert System (ATLAS) (Tonry et al. 2018); it is from TNS that we retrieved the discovery photometry. We store photometry information, including flux and limiting magnitude measurements from follow-up observations by GRANDMA's telescopes within SKYPORTAL, supplementing the data imported from TNS, to create light curves. From the dedicated source page, easy access is provided to many other database services, such as Vizier (Ochsenbein, Bauer & Marcout 2000). Finally, SKYPORTAL is used for simplifying interactions with Bayesian inference frameworks such as the Nuclear physics and Multimessenger Astronomy framework NMMA (Dietrich et al. 2020; Pang et al. ), which we discuss more in the main text. Operations on SKYPORTAL are conducted and monitored by 'shifters', members of the collaboration organized in teams every week, and divided into four daily slots of six hours each to accommodate timezone constraints while maintaining 24/7 coverage. Shifters look out for new candidates from surveys (particularly LIGO-Virgo-KAGRA, LVK) and new GCN events on the platform and report on associated Slack channels which candidates are to be followed up or not based on pre-defined criteria. The shifts are also organized using SKYPORTAL's dedicated page in the form of a calendar. Shifters or members of telescope teams are expected to upload executed observations data either manually or programmatically using the API. GCN circular-like documents can even be automatically generated, ensuring consistent formatting of the results reported to the General Coordinates Network while reducing the possibility for human errors to be made.

## APPENDIX D: COMPARING DIFFERENT ASTROPHYSICAL SCENARIOS WITH NMMA

As discussed in Section 4.2, using NMMA, we can quantitatively
compare different astrophysical scenarios in a Bayesian framework.
We have performed studies using various models and jet geometries.
NMMA is able to perform joint Bayesian inference of multimessenger
events containing gravitational waves, GRB afterglows, SNe, or
kilonovae. In addition to scenarios mentioned above, we also consider
two kilonova models, Bu2023Ye (Anand et al. 2023) and Ka2017
(Kasen et al. 2017), to accompany the Top-hat model as possible ex-
planations of the data set. The log Bayes factor ln *B* of various models
relative to the Power-law+SN, which is the best-performing model
to be introduced shortly, can be found in Table D1. The posterior of
σ<sub>sys</sub> is also shown in Table D1. The Power-law+SN has the lowest
value of σ<sub>sys</sub>, thus signifying a better fit compared to other models.
Comparing the differences between the log Bayes factor of scenarios
with and without an SN component, we conclude that the presence
of an SN component is statistically supported from a Bayesian
perspective.

The posterior values of all the considered models is summarized
in Table D2. The best-fitting light curves for the three GRB+SN
scenarios are shown in Fig. D1.

<footnote n="21">²¹Using the focal reducer FoReRo-2 (Jockers et al. 2000).</footnote>
<figure><img src="image_11.png" /><figcaption>**Figure D1.** Best-fitting light curves of the GRB+SN models with top-hat, Gaussian, and power-law jet structures. Datapoints are reported in the observer frame.</figcaption></figure>

<table><caption>**Table D1.** The log Bayes factor $\ln \mathcal{B}$ and $\sigma_{\text{sys}}$ value (median with 95 per cent credible interval) inferred for different models.</caption><thead><tr><th>Scenario</th><th>log Bayes factor ln B</th><th>σ<sub>sys</sub> (mag)</th></tr></thead><tbody><tr><td>Power-law+SN</td><td>ref</td><td>0.140<sup>+0.061</sup><sub>-0.050</sub></td></tr><tr><td>Top-hat</td><td>-56.612 ± 0.298</td><td>0.693<sup>+0.133</sup><sub>-0.117</sub></td></tr><tr><td>Top-hat+SN</td><td>-18.360 ± 0.331</td><td>0.282<sup>+0.081</sup><sub>-0.077</sub></td></tr><tr><td>Top-hat+Bu2023Ye</td><td>-56.682 ± 0.297</td><td>0.696<sup>+0.126</sup><sub>-0.103</sub></td></tr><tr><td>Top-hat+Ka2017</td><td>-56.633 ± 0.297</td><td>0.696<sup>+0.125</sup><sub>-0.108</sub></td></tr><tr><td>Gauss</td><td>-56.235 ± 0.298</td><td>0.690<sup>+0.122</sup><sub>-0.116</sub></td></tr><tr><td>Gauss+SN</td><td>-17.356 ± 0.331</td><td>0.282<sup>+0.080</sup><sub>-0.073</sub></td></tr><tr><td>Power-law</td><td>-56.292 ± 0.296</td><td>0.693<sup>+0.127</sup><sub>-0.111</sub></td></tr></tbody></table>
<figure><img src="image_11.png" /><figcaption>**Figure D1.** Best-fitting light curves of the GRB+SN models with top-hat, Gaussian, and power-law jet structures. Datapoints are reported in the observer frame.</figcaption></figure>

<table><caption>**Table D1.** The log Bayes factor $\ln B$ and $\sigma_{\text{sys}}$ value (median with 95 per cent credible interval) inferred for different models.</caption><thead><tr><th>Scenario</th><th>log Bayes factor ln B</th><th>σ<sub>sys</sub> (mag)</th></tr></thead><tbody><tr><td>Power-law+SN</td><td>ref</td><td>0.140<sup>+0.061</sup><sub>-0.050</sub></td></tr><tr><td>Top-hat</td><td>-56.612 ± 0.298</td><td>0.693<sup>+0.133</sup><sub>-0.117</sub></td></tr><tr><td>Top-hat+SN</td><td>-18.360 ± 0.331</td><td>0.282<sup>+0.081</sup><sub>-0.077</sub></td></tr><tr><td>Top-hat+Bu2023Ye</td><td>-56.682 ± 0.297</td><td>0.696<sup>+0.126</sup><sub>-0.103</sub></td></tr><tr><td>Top-hat+Ka2017</td><td>-56.633 ± 0.297</td><td>0.696<sup>+0.125</sup><sub>-0.108</sub></td></tr><tr><td>Gauss</td><td>-56.235 ± 0.298</td><td>0.690<sup>+0.122</sup><sub>-0.116</sub></td></tr><tr><td>Gauss+SN</td><td>-17.356 ± 0.331</td><td>0.282<sup>+0.080</sup><sub>-0.073</sub></td></tr><tr><td>Power-law</td><td>-56.292 ± 0.296</td><td>0.693<sup>+0.127</sup><sub>-0.111</sub></td></tr></tbody></table>
<table><caption>**Table D2.** NMMA – Parameters and prior bounds employed in our Bayesian inferences. We report median posterior values at 95 per cent credibility for various physical scenarios and jet structures for the GRB. 'Uniform' refers to an uniform distribution, and 'LogUniform' refers to an uniform distribution for the log of the parameter. $N(\mu, \sigma^2)$ refers to a Gaussian distribution with mean $\mu$ and variance $\sigma^2$.</caption><thead><tr><th rowspan="2">Parameter</th><th rowspan="2">Prior</th><th rowspan="2">Prior range</th><th colspan="7">Top-hat</th></tr><tr><th>+SN</th><th>+Bu2023Ye</th><th>+Ka2017</th><th>Gauss</th><th>Gauss+SN</th><th>Power-law</th><th>Power-law+SN</th></tr></thead><tbody><tr><td>(log-) Isotropic afterglow energy E<sub>0</sub> (erg)</td><td>Uniform</td><td>[47, 57]</td><td>52.39<sup>+0.40</sup><sub>-0.44</sub></td><td>52.91<sup>+2.20</sup><sub>-0.78</sub></td><td>52.37<sup>+0.38</sup><sub>-0.41</sub></td><td>52.39<sup>+0.43</sup><sub>-0.39</sub></td><td>52.60<sup>+0.68</sup><sub>-0.53</sub></td><td>52.58<sup>+2.00</sup><sub>-0.42</sub></td><td>52.48<sup>+0.45</sup><sub>-0.47</sub></td><td>52.82<sup>+0.35</sup><sub>-0.31</sub></td></tr><tr><td>(log-) Ambient medium's density n<sub>ism</sub> (cm<sup>-3</sup>)</td><td>Uniform</td><td>[-6, 3]</td><td>-4.76<sup>+1.36</sup><sub>-1.17</sub></td><td>-1.36<sup>+1.24</sup><sub>-2.94</sub></td><td>-4.84<sup>+1.21</sup><sub>-1.13</sub></td><td>-4.89<sup>+1.34</sup><sub>-1.10</sub></td><td>-4.63<sup>+1.65</sup><sub>-1.30</sub></td><td>-1.38<sup>+1.30</sup><sub>-2.27</sub></td><td>-4.80<sup>+1.37</sup><sub>-1.17</sub></td><td>-2.38<sup>+1.45</sup><sub>-1.60</sub></td></tr><tr><td>(log-) Energy fraction in electrons e<sub>e</sub></td><td>Uniform</td><td>[-5, 0]</td><td>-0.48<sup>+0.33</sup><sub>-0.30</sub></td><td>-0.13<sup>+0.49</sup><sub>-0.13</sub></td><td>-0.53<sup>+0.39</sup><sub>-0.33</sub></td><td>-0.56<sup>+0.39</sup><sub>-0.33</sub></td><td>-0.48<sup>+0.36</sup><sub>-0.36</sub></td><td>-0.12<sup>+0.12</sup><sub>-0.12</sub></td><td>-0.50<sup>+0.35</sup><sub>-0.35</sub></td><td>-0.10<sup>+0.10</sup><sub>-0.10</sub></td></tr><tr><td>(log-) Energy fraction in magnetic field e<sub>B</sub></td><td>Uniform</td><td>[-10, 0]</td><td>-0.55<sup>+0.47</sup><sub>-0.86</sub></td><td>-4.02<sup>+2.65</sup><sub>-1.83</sub></td><td>-0.52<sup>+0.45</sup><sub>-0.75</sub></td><td>-0.52<sup>+0.80</sup><sub>-0.44</sub></td><td>-0.65<sup>+0.56</sup><sub>-1.02</sub></td><td>-3.56<sup>+1.59</sup><sub>-2.52</sub></td><td>-0.52<sup>+0.83</sup><sub>-0.44</sub></td><td>-2.29<sup>+1.02</sup><sub>-0.94</sub></td></tr><tr><td>Electron distribution power-law index p</td><td>Uniform</td><td>[2.01, 3]</td><td>2.13<sup>+0.13</sup><sub>-0.08</sub></td><td>2.25<sup>+0.09</sup><sub>-0.19</sub></td><td>2.14<sup>+0.09</sup><sub>-0.11</sub></td><td>2.15<sup>+0.11</sup><sub>-0.09</sub></td><td>2.13<sup>+0.13</sup><sub>-0.08</sub></td><td>2.15<sup>+0.16</sup><sub>-0.09</sub></td><td>2.13<sup>+0.12</sup><sub>-0.08</sub></td><td>2.04<sup>+0.02</sup><sub>-0.02</sub></td></tr><tr><td>Viewing angle θ<sub>obs</sub> (deg)</td><td>Uniform</td><td>[-0.6, 18]</td><td>4.26<sup>+9.18</sup><sub>-4.26</sub></td><td>2.77<sup>+2.24</sup><sub>-2.42</sub></td><td>3.28<sup>+6.28</sup><sub>-3.28</sub></td><td>3.59<sup>+6.36</sup><sub>-3.58</sub></td><td>8.62<sup>+11.51</sup><sub>-8.61</sub></td><td>2.20<sup>+2.28</sup><sub>-2.11</sub></td><td>7.33<sup>+11.16</sup><sub>-7.33</sub></td><td>0.76<sup>+1.29</sup><sub>-0.76</sub></td></tr><tr><td>Jet core's opening angle θ<sub>core</sub> (deg)</td><td>Uniform</td><td>[0.6, 45]</td><td>13.25<sup>+4.74</sup><sub>-6.35</sub></td><td>4.96<sup>+3.30</sup><sub>-4.20</sub></td><td>13.20<sup>+4.80</sup><sub>-5.75</sub></td><td>13.38<sup>+4.61</sup><sub>-5.55</sub></td><td>11.02<sup>+6.98</sup><sub>-7.25</sub></td><td>3.96<sup>+2.45</sup><sub>-3.09</sub></td><td>12.01<sup>+5.98</sup><sub>-6.89</sub></td><td>1.54<sup>+1.02</sup><sub>-0.81</sub></td></tr><tr><td>'Wing' truncation angle θ<sub>wing</sub> (deg)</td><td>Uniform</td><td>[0.1, 7]</td><td>—</td><td>—</td><td>—</td><td>21.97<sup>+20.71</sup><sub>-20.47</sub></td><td>27.83<sup>+17.10</sup><sub>-16.05</sub></td><td>—</td><td>25.18<sup>+19.77</sup><sub>-17.50</sub></td><td>29.21<sup>+15.62</sup><sub>-16.96</sub></td></tr><tr><td>Power-law structure index b</td><td>Uniform</td><td>—</td><td>—</td><td>—</td><td>—</td><td>3.48<sup>+3.03</sup><sub>-3.07</sub></td><td>3.46<sup>+3.36</sup><sub>-3.36</sub></td><td>—</td><td>—</td><td>3.46<sup>+3.37</sup><sub>-3.27</sub></td></tr><tr><td>Angle ratio θ<sub>obs</sub>/θ<sub>core</sub></td><td>Uniform</td><td>—</td><td>0.33<sup>+0.64</sup><sub>-0.32</sub></td><td>0.56<sup>+0.23</sup><sub>-0.21</sub></td><td>—</td><td>0.27<sup>+0.29</sup><sub>-0.27</sub></td><td>0.29<sup>+0.29</sup><sub>-0.29</sub></td><td>1.03<sup>+1.03</sup><sub>-1.03</sub></td><td>0.64<sup>+0.41</sup><sub>-0.57</sub></td><td>0.68<sup>+0.68</sup><sub>-0.68</sub></td></tr><tr><td>Supernova boost k<sub>SN</sub></td><td>Uniform</td><td>[0.01, 100]</td><td>—</td><td>1.06<sup>+0.18</sup><sub>-0.18</sub></td><td>—</td><td>—</td><td>—</td><td>—</td><td>1.08<sup>+0.15</sup><sub>-0.15</sub></td><td>—</td></tr><tr><td>Supernova stretch <sup>3</sup>SN</td><td>Uniform</td><td>[0.1, 5.0]</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>0.68<sup>+0.07</sup><sub>-0.07</sub></td><td>—</td></tr><tr><td>Systematic error σ<sub>sys</sub></td><td>LogUniform</td><td>[0.01, 2.0]</td><td>0.69<sup>+0.13</sup><sub>-0.12</sub></td><td>0.28<sup>+0.08</sup><sub>-0.08</sub></td><td>0.70<sup>+0.13</sup><sub>-0.10</sub></td><td>0.70<sup>+0.12</sup><sub>-0.11</sub></td><td>0.69<sup>+0.12</sup><sub>-0.12</sub></td><td>—</td><td>—</td><td>0.69<sup>+0.13</sup><sub>-0.11</sub></td></tr></tbody></table>

¹IJCLab, Univ Paris-Saclay, CNRS/IN2P3 Orsay, 91405, France

²Nikhef, Science Park 105, NL-1098 XG Amsterdam, the Netherlands

³Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, NL-3584 CC Utrecht, the Netherlands

⁴Physics Department, American University of Sharjah, Sharjah, 26666, UAE

⁵National Research Institute of Astronomy and Geophysics (NRIAG), 1 El-marsad St., 11421 Helwan, Cairo, Egypt

⁶Aix Marseille Univ, CNRS, CNES, 13388 LAM Marseille, France

⁷Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, E-18008 Granada, Spain

⁸Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA

⁹E. Kharadze Georgian National Astrophysical Observatory, Mt. Kanobili, Abastumani 0301, Adigeni, Georgia

¹⁰Samtskhe-Javakheti State University, Rustaveli Str. 113, Akhaltsikhe 0080, Georgia

¹¹School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA

¹²Observatoire de la Côte d'Azur, Université Côte d'Azur, Boulevard de l'Observatoire, F-06304 Nice, France

¹³INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate (LC), Italy

¹⁴Astronomical Observatory of Taras Shevchenko National University of Kyiv, Observatorna Str. 3, UA-04053 Kyiv, Ukraine

¹⁵CEICO, Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, CZ-182 21 Praha, Czech Republic

¹⁶Centro Astronómico Hispano en Andalucía, Observatorio de Calar Alto, Sierra de los Filabres, E-04550 Gérgal, Almería, Spain

¹⁷Laboratoire J.-L. Lagrange, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, F-06304 Nice, France

¹⁸National Observatory of Athens, Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, GR-15236 Penteli, Greece

¹⁹Institut de Radioastronomie Millimétrique, Saint-Martin-d'Hères, 38406, France

²⁰Università degli Studi dell'Insubria, Dipartimento di Scienza e Alta Tecnologia, Via Valleggio 11, I-22100 Como, Italy

²¹Department of Physics and Earth Science, University of Ferrara, via Saragat 1, I-44122 Ferrara, Italy

²²INFN, Sezione di Ferrara, via Saragat 1, I-44122 Ferrara, Italy

²³INAF, Osservatorio Astronomico d'Abruzzo, via Mentore Maggini snc, I-64100 Teramo, Italy

²⁴Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Astronomy Str. 33, Tashkent 100052, Uzbekistan

²⁵Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803, USA

²⁶Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA

²⁷Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA

²⁸Laboratório Nacional de Astrofísica - LNA, Rua Estados Unidos, 154 Itajubá - MG CEP 37504-364, Brazil

²⁹Sorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, F-75014 Paris, France

³⁰Institute for Physics and Astronomy, University of Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, Germany

³¹Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, D-14476 Potsdam, Germany

³²Aix Marseille Univ, CNRS/IN2P3, CPPM, 13288 Marseille, France

³³Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France

³⁴Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, F-91191 Gif-sur-Yvette, France

³⁵KNC, AAVSO, Hidden Valley Observatory (HVO), Colfax, WI, 54730, USA; iTelescope, New Mexico Skies Observatory, Mayhill, NM, 88339, USA

³⁶Cosmic Dawn Center (DAWN), 2200 Copenhagen, Denmark

³⁷Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen N, Denmark
<table><caption>**Table D2.** NMMA – Parameters and prior bounds employed in our Bayesian inferences. We report median posterior values at 95 per cent credibility for various physical scenarios and jet structures for the GRB. 'Uniform' refers to an uniform distribution, and 'LogUniform' refers to an uniform distribution for the log of the parameter. $N(\mu, \sigma^2)$ refers to a Gaussian distribution with mean $\mu$ and variance $\sigma^2$.</caption><thead><tr><th rowspan="2">Parameter</th><th rowspan="2">Prior</th><th rowspan="2">Prior range</th><th colspan="7">Top-hat</th></tr><tr><th>+SN</th><th>+Bu2023Ye</th><th>+Ka2017</th><th>Gauss</th><th>Gauss+SN</th><th>Power-law</th><th>Power-law+SN</th></tr></thead><tbody><tr><td>(log-) Isotropic afterglow energy E<sub>0</sub> (erg)</td><td>Uniform</td><td>[47, 57]</td><td>52.39<sup>+0.40</sup><sub>-0.44</sub></td><td>52.91<sup>+2.20</sup><sub>-0.78</sub></td><td>52.37<sup>+0.38</sup><sub>-0.41</sub></td><td>52.39<sup>+0.43</sup><sub>-0.39</sub></td><td>52.60<sup>+0.68</sup><sub>-0.53</sub></td><td>52.58<sup>+2.00</sup><sub>-0.42</sub></td><td>52.48<sup>+0.45</sup><sub>-0.47</sub></td><td>52.82<sup>+0.35</sup><sub>-0.31</sub></td></tr><tr><td>(log-) Ambient medium's density n<sub>ism</sub> (cm<sup>-3</sup>)</td><td>Uniform</td><td>[-6, 3]</td><td>-4.76<sup>+1.36</sup><sub>-1.17</sub></td><td>-1.36<sup>+1.24</sup><sub>-2.94</sub></td><td>-4.84<sup>+1.21</sup><sub>-1.13</sub></td><td>-4.89<sup>+1.34</sup><sub>-1.10</sub></td><td>-4.63<sup>+1.65</sup><sub>-1.30</sub></td><td>-1.38<sup>+1.30</sup><sub>-2.27</sub></td><td>-4.80<sup>+1.37</sup><sub>-1.17</sub></td><td>-2.38<sup>+1.45</sup><sub>-1.60</sub></td></tr><tr><td>(log-) Energy fraction in electrons e<sub>e</sub></td><td>Uniform</td><td>[-5, 0]</td><td>-0.48<sup>+0.33</sup><sub>-0.30</sub></td><td>-0.13<sup>+0.49</sup><sub>-0.13</sub></td><td>-0.53<sup>+0.39</sup><sub>-0.33</sub></td><td>-0.56<sup>+0.39</sup><sub>-0.33</sub></td><td>-0.48<sup>+0.36</sup><sub>-0.36</sub></td><td>-0.12<sup>+0.12</sup><sub>-0.12</sub></td><td>-0.50<sup>+0.35</sup><sub>-0.35</sub></td><td>-0.10<sup>+0.10</sup><sub>-0.10</sub></td></tr><tr><td>(log-) Energy fraction in magnetic field e<sub>B</sub></td><td>Uniform</td><td>[-10, 0]</td><td>-0.55<sup>+0.47</sup><sub>-0.86</sub></td><td>-4.02<sup>+2.65</sup><sub>-1.83</sub></td><td>-0.52<sup>+0.45</sup><sub>-0.75</sub></td><td>-0.52<sup>+0.80</sup><sub>-0.44</sub></td><td>-0.65<sup>+0.56</sup><sub>-1.02</sub></td><td>-3.56<sup>+1.59</sup><sub>-2.52</sub></td><td>-0.52<sup>+0.83</sup><sub>-0.44</sub></td><td>-2.29<sup>+1.02</sup><sub>-0.94</sub></td></tr><tr><td>Electron distribution power-law index p</td><td>Uniform</td><td>[2.01, 3]</td><td>2.13<sup>+0.13</sup><sub>-0.08</sub></td><td>2.25<sup>+0.09</sup><sub>-0.19</sub></td><td>2.14<sup>+0.09</sup><sub>-0.11</sub></td><td>2.15<sup>+0.11</sup><sub>-0.09</sub></td><td>2.13<sup>+0.13</sup><sub>-0.08</sub></td><td>2.15<sup>+0.16</sup><sub>-0.09</sub></td><td>2.13<sup>+0.12</sup><sub>-0.08</sub></td><td>2.04<sup>+0.02</sup><sub>-0.02</sub></td></tr><tr><td>Viewing angle θ<sub>obs</sub> (deg)</td><td>Uniform</td><td>[0.6, 18]</td><td>4.26<sup>+9.18</sup><sub>-4.26</sub></td><td>2.77<sup>+2.24</sup><sub>-2.42</sub></td><td>3.28<sup>+6.28</sup><sub>-3.28</sub></td><td>3.59<sup>+6.36</sup><sub>-3.58</sub></td><td>8.62<sup>+11.51</sup><sub>-8.61</sub></td><td>2.20<sup>+2.28</sup><sub>-2.11</sub></td><td>7.33<sup>+11.16</sup><sub>-7.33</sub></td><td>0.76<sup>+1.29</sup><sub>-0.76</sub></td></tr><tr><td>Jet core's opening angle θ<sub>core</sub> (deg)</td><td>Uniform</td><td>[0.6, 45]</td><td>13.25<sup>+4.74</sup><sub>-6.35</sub></td><td>4.96<sup>+3.30</sup><sub>-4.20</sub></td><td>13.20<sup>+4.80</sup><sub>-5.75</sub></td><td>13.38<sup>+4.61</sup><sub>-5.55</sub></td><td>11.02<sup>+6.98</sup><sub>-7.25</sub></td><td>3.96<sup>+2.45</sup><sub>-3.09</sub></td><td>12.01<sup>+5.98</sup><sub>-6.89</sub></td><td>1.54<sup>+1.02</sup><sub>-0.81</sub></td></tr><tr><td>'Wing' truncation angle θ<sub>wing</sub> (deg)</td><td>Uniform</td><td>[0.1, 7]</td><td>—</td><td>—</td><td>—</td><td>21.97<sup>+20.71</sup><sub>-20.47</sub></td><td>27.83<sup>+17.10</sup><sub>-16.05</sub></td><td>—</td><td>25.18<sup>+19.77</sup><sub>-17.50</sub></td><td>29.21<sup>+15.62</sup><sub>-16.96</sub></td></tr><tr><td>Power-law structure index b</td><td>Uniform</td><td>—</td><td>—</td><td>—</td><td>—</td><td>3.48<sup>+3.03</sup><sub>-3.07</sub></td><td>3.46<sup>+3.36</sup><sub>-3.36</sub></td><td>—</td><td>—</td><td>3.46<sup>+3.37</sup><sub>-3.27</sub></td></tr><tr><td>Angle ratio θ<sub>obs</sub>/θ<sub>core</sub></td><td>Uniform</td><td>—</td><td>0.33<sup>+0.64</sup><sub>-0.32</sub></td><td>0.56<sup>+0.23</sup><sub>-0.21</sub></td><td>—</td><td>—</td><td>1.03<sup>+0.87</sup><sub>-1.03</sub></td><td>0.64<sup>+0.41</sup><sub>-0.57</sub></td><td>—</td><td>0.68<sup>+0.68</sup><sub>-0.68</sub></td></tr><tr><td>Supernova boost k<sub>SN</sub></td><td>Uniform</td><td>[0.01, 100]</td><td>—</td><td>1.06<sup>+0.18</sup><sub>-0.18</sub></td><td>—</td><td>—</td><td>—</td><td>1.08<sup>+0.15</sup><sub>-0.15</sub></td><td>—</td><td>—</td></tr><tr><td>Supernova stretch <sup>3</sup>SN</td><td>Uniform</td><td>[0.1, 5.0]</td><td>—</td><td>0.69<sup>+0.08</sup><sub>-0.07</sub></td><td>—</td><td>—</td><td>—</td><td>0.68<sup>+0.07</sup><sub>-0.07</sub></td><td>—</td><td>—</td></tr><tr><td>Systematic error σ<sub>sys</sub></td><td>LogUniform</td><td>[0.01, 2.0]</td><td>0.69<sup>+0.13</sup><sub>-0.12</sub></td><td>0.28<sup>+0.08</sup><sub>-0.08</sub></td><td>0.70<sup>+0.13</sup><sub>-0.10</sub></td><td>0.70<sup>+0.12</sup><sub>-0.11</sub></td><td>0.69<sup>+0.12</sup><sub>-0.12</sub></td><td>0.28<sup>+0.08</sup><sub>-0.07</sub></td><td>0.69<sup>+0.13</sup><sub>-0.11</sub></td><td>0.14<sup>+0.06</sup><sub>-0.05</sub></td></tr></tbody></table>

¹IJCLab, Univ Paris-Saclay, CNRS/IN2P3 Orsay, 91405, France

²Nikhef, Science Park 105, NL-1098 XG Amsterdam, the Netherlands

³Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, NL-3584 CC Utrecht, the Netherlands

⁴Physics Department, American University of Sharjah, Sharjah, 26666, UAE

⁵National Research Institute of Astronomy and Geophysics (NRIAG), 1 El-marsad St., 11421 Helwan, Cairo, Egypt

⁶Aix Marseille Univ, CNRS, CNES, 13388 LAM Marseille, France

⁷Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, E-18008 Granada, Spain

⁸Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA

⁹E. Kharadze Georgian National Astrophysical Observatory, Mt. Kanobili, Abastumani 0301, Adigeni, Georgia

¹⁰Samtskhe-Javakheti State University, Rustaveli Str. 113, Akhaltsikhe 0080, Georgia

¹¹School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA

¹²Observatoire de la Côte d'Azur, Université Côte d'Azur, Boulevard de l'Observatoire, F-06304 Nice, France

¹³INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate (LC), Italy

¹⁴Astronomical Observatory of Taras Shevchenko National University of Kyiv, Observatorna Str. 3, UA-04053 Kyiv, Ukraine

¹⁵CEICO, Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, CZ-182 21 Praha, Czech Republic

¹⁶Centro Astronómico Hispano en Andalucía, Observatorio de Calar Alto, Sierra de los Filabres, E-04550 Gérgal, Almería, Spain

¹⁷Laboratoire J.-L. Lagrange, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, F-06304 Nice, France

¹⁸National Observatory of Athens, Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, GR-15236 Penteli, Greece

¹⁹Institut de Radioastronomie Millimétrique, Saint-Martin-d'Hères, 38406, France

²⁰Università degli Studi dell'Insubria, Dipartimento di Scienza e Alta Tecnologia, Via Valleggio 11, I-22100 Como, Italy

²¹Department of Physics and Earth Science, University of Ferrara, via Saragat 1, I-44122 Ferrara, Italy

²²INFN, Sezione di Ferrara, via Saragat 1, I-44122 Ferrara, Italy

²³INAF, Osservatorio Astronomico d'Abruzzo, via Mentore Maggini snc, I-64100 Teramo, Italy

²⁴Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Astronomy Str. 33, Tashkent 100052, Uzbekistan

²⁵Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803, USA

²⁶Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA

²⁷Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA

²⁸Laboratório Nacional de Astrofísica - LNA, Rua Estados Unidos, 154 Itajubá - MG CEP 37504-364, Brazil

²⁹Sorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, F-75014 Paris, France

³⁰Institute for Physics and Astronomy, University of Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, Germany

³¹Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, D-14476 Potsdam, Germany

³²Aix Marseille Univ, CNRS/IN2P3, CPPM, 13288 Marseille, France

³³Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France

³⁴Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, F-91191 Gif-sur-Yvette, France

³⁵KNC, AAVSO, Hidden Valley Observatory (HVO), Colfax, WI, 54730, USA; iTelescope, New Mexico Skies Observatory, Mayhill, NM, 88339, USA

³⁶Cosmic Dawn Center (DAWN), 2200 Copenhagen, Denmark

³⁷Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen N, Denmark
<footnote n="38">³⁸N. Tusi Shamakhy Astrophysical Observatory, Ministry of Science and Education, settl. Y. Mammadaliyev, AZ-5626 Shamakhy, Azerbaijan</footnote>

<footnote n="39">³⁹School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA</footnote>

<footnote n="40">⁴⁰Xinjiang Astronomical Observatory (XAO), Chinese Academy of Sciences, Urumqi 830011, P. R. China</footnote>

<footnote n="41">⁴¹INAF-Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, Italy</footnote>

<footnote n="42">⁴²DARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen N, Denmark</footnote>

<footnote n="43">⁴³Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA</footnote>

<footnote n="44">⁴⁴IRAP, Université de Toulouse, CNRS, UPS, 14 Avenue Edouard Belin, F-31400 Toulouse, France</footnote>

<footnote n="45">⁴⁵Université Paul Sabatier Toulouse III, Université de Toulouse, 118 Route de Narbonne, F-31400 Toulouse, France</footnote>

<footnote n="46">⁴⁶Mullard Space Science Laboratory, University College London, Holmbury St. Mary Dorking RH5 6NT, UK</footnote>

<footnote n="47">⁴⁷Montarrenti Observatory, S. S. 73 Ponente, I-53018 Sovicille, Siena, Italy</footnote>

<footnote n="48">⁴⁸Yunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, Yunnan Province, P. R. China</footnote>

<footnote n="49">⁴⁹Department of Astrophysics/IMAPP, Radboud University, NL-6525 AJ Nijmegen, the Netherlands</footnote>

<footnote n="50">⁵⁰FZU-Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, CZ-182 21 Praha, Czech Republic</footnote>

<footnote n="51">⁵¹Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, 100012 Beijing, P. R. China</footnote>

<footnote n="52">⁵²Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011 Kunming, P. R. China</footnote>

<footnote n="53">⁵³INAF-Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040 Monte Porzio Catone (RM), Italy</footnote>

<footnote n="54">⁵⁴Institute of Astronomy and NAO, Bulgarian Academy of Sciences, 72 Tsarigradsko Chaussee Blvd., 1784 Sofia, Bulgaria</footnote>

<footnote n="55">⁵⁵SOAR Telescope/NSF's NOIRLab Avda Juan Cisternas 1500, 1700000 La Serena, Chile</footnote>

<footnote n="56">⁵⁶GEPI, Observatoire de Paris, Université PSL, CNRS, 5 place Jules Janssen, F-92190 Meudon, France</footnote>

<footnote n="57">⁵⁷Mathematics, Informatics, Physics and Earth Science Department, University of Messina, Via F.D. D'Alcontres 31, Polo Papardo, I-98166 Messina, Italy</footnote>

<footnote n="58">⁵⁸Physics Department, Tsinghua University, Beijing 100084, P. R. China</footnote>

<footnote n="59">⁵⁹Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France</footnote>

<footnote n="60">⁶⁰Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA 02139, USA</footnote>

<footnote n="61">⁶¹Société Astronomique de France, Observatoire de Dauban, F-04150 Banon, France</footnote>

<footnote n="62">⁶²Astronomy and Space Physics Department, Taras Shevchenko National University of Kyiv, Glushkova Ave., 4, UA-03022 Kyiv, Ukraine</footnote>

<footnote n="63">⁶³National Center Junior Academy of Sciences of Ukraine, Dehtiarivska St. 38-44, UA-04119 Kyiv, Ukraine</footnote>

<footnote n="64">⁶⁴Main Astronomical Observatory of National Academy of Sciences of Ukraine, 27 Acad. Zabolotnoho Str., UA-03143 Kyiv, Ukraine</footnote>

<footnote n="65">⁶⁵Department of Astronomy, University of Maryland, College Park, MD 20742, USA</footnote>

<footnote n="66">⁶⁶Department of Physics, Eastern Illinois University, Charleston, IL 61920, USA</footnote>

<footnote n="67">⁶⁷Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK</footnote>

<footnote n="68">⁶⁸Astronomical Institute of the Czech Academy of Sciences (ASU-CAS), Fricova 298, CZ-251 65 Ondřejov, Czech Republic</footnote>

<footnote n="69">⁶⁹National University of Uzbekistan, Department of Astronomy and Atmospheric Physics, 4 University Str., Tashkent 100174, Uzbekistan</footnote>

<footnote n="70">⁷⁰Department of Physics and Astronomy, University of Catania, Via Santa Sofia 64, I-95123 Catania, Italy</footnote>

<footnote n="71">⁷¹Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, P. R. China</footnote>

<footnote n="72">⁷²Department of Astronomy, School of Physics, Huazhong University of Science and Technology, Wuhan 430074, China</footnote>

<footnote>This paper has been typeset from a TEX/LATEX file prepared by the author.</footnote>
<footnote n="38">³⁸N. Tusi Shamakhy Astrophysical Observatory, Ministry of Science and Education, settl. Y. Mammadaliyev, AZ-5626 Shamakhy, Azerbaijan</footnote>

<footnote n="39">³⁹School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA</footnote>

<footnote n="40">⁴⁰Xinjiang Astronomical Observatory (XAO), Chinese Academy of Sciences, Urumqi 830011, P. R. China</footnote>

<footnote n="41">⁴¹INAF-Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, Italy</footnote>

<footnote n="42">⁴²DARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen N, Denmark</footnote>

<footnote n="43">⁴³Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA</footnote>

<footnote n="44">⁴⁴IRAP, Université de Toulouse, CNRS, UPS, 14 Avenue Edouard Belin, F-31400 Toulouse, France</footnote>

<footnote n="45">⁴⁵Université Paul Sabatier Toulouse III, Université de Toulouse, 118 Route de Narbonne, F-31400 Toulouse, France</footnote>

<footnote n="46">⁴⁶Mullard Space Science Laboratory, University College London, Holmbury St. Mary Dorking RH5 6NT, UK</footnote>

<footnote n="47">⁴⁷Montarrenti Observatory, S. S. 73 Ponente, I-53018 Sovicille, Siena, Italy</footnote>

<footnote n="48">⁴⁸Yunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, Yunnan Province, P. R. China</footnote>

<footnote n="49">⁴⁹Department of Astrophysics/IMAPP, Radboud University, NL-6525 AJ Nijmegen, the Netherlands</footnote>

<footnote n="50">⁵⁰FZU-Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, CZ-182 21 Praha, Czech Republic</footnote>

<footnote n="51">⁵¹Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, 100012 Beijing, P. R. China</footnote>

<footnote n="52">⁵²Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011 Kunming, P. R. China</footnote>

<footnote n="53">⁵³INAF-Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040 Monte Porzio Catone (RM), Italy</footnote>

<footnote n="54">⁵⁴Institute of Astronomy and NAO, Bulgarian Academy of Sciences, 72 Tsarigradsko Chaussee Blvd., 1784 Sofia, Bulgaria</footnote>

<footnote n="55">⁵⁵SOAR Telescope/NSF's NOIRLab Avda Juan Cisternas 1500, 1700000 La Serena, Chile</footnote>

<footnote n="56">⁵⁶GEPI, Observatoire de Paris, Université PSL, CNRS, 5 place Jules Janssen, F-92190 Meudon, France</footnote>

<footnote n="57">⁵⁷Mathematics, Informatics, Physics and Earth Science Department, University of Messina, Via F.D. D'Alcontres 31, Polo Papardo, I-98166 Messina, Italy</footnote>

<footnote n="58">⁵⁸Physics Department, Tsinghua University, Beijing 100084, P. R. China</footnote>

<footnote n="59">⁵⁹Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France</footnote>

<footnote n="60">⁶⁰Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA 02139, USA</footnote>

<footnote n="61">⁶¹Société Astronomique de France, Observatoire de Dauban, F-04150 Banon, France</footnote>

<footnote n="62">⁶²Astronomy and Space Physics Department, Taras Shevchenko National University of Kyiv, Glushkova Ave., 4, UA-03022 Kyiv, Ukraine</footnote>

<footnote n="63">⁶³National Center Junior Academy of Sciences of Ukraine, Dehtiarivska St. 38-44, UA-04119 Kyiv, Ukraine</footnote>

<footnote n="64">⁶⁴Main Astronomical Observatory of National Academy of Sciences of Ukraine, 27 Acad. Zabolotnoho Str., UA-03143 Kyiv, Ukraine</footnote>

<footnote n="65">⁶⁵Department of Astronomy, University of Maryland, College Park, MD 20742, USA</footnote>

<footnote n="66">⁶⁶Department of Physics, Eastern Illinois University, Charleston, IL 61920, USA</footnote>

<footnote n="67">⁶⁷Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK</footnote>

<footnote n="68">⁶⁸Astronomical Institute of the Czech Academy of Sciences (ASU-CAS), Fricova 298, CZ-251 65 Ondřejov, Czech Republic</footnote>

<footnote n="69">⁶⁹National University of Uzbekistan, Department of Astronomy and Atmospheric Physics, 4 University Str., Tashkent 100174, Uzbekistan</footnote>

<footnote n="70">⁷⁰Department of Physics and Astronomy, University of Catania, Via Santa Sofia 64, I-95123 Catania, Italy</footnote>

<footnote n="71">⁷¹Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, P. R. China</footnote>

<footnote n="72">⁷²Department of Astronomy, School of Physics, Huazhong University of Science and Technology, Wuhan 430074, China</footnote>

<footnote>This paper has been typeset from a TEX/LATEX file prepared by the author.</footnote>