Constraining the TeV gamma-ray emission of SN 2024bch, a possible type IIn-L from a red supergiant progenitor

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10510727" target="_blank" >RIV/00216208:11320/25:10510727 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=3Eky0DTy0S" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=3Eky0DTy0S</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202554721" target="_blank" >10.1051/0004-6361/202554721</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Constraining the TeV gamma-ray emission of SN 2024bch, a possible type IIn-L from a red supergiant progenitor

Popis výsledku v původním jazyce

We present very high-energy optical photometry and spectroscopic observations of SN 2024bch in the nearby galaxy NGC 3206 (similar to 20 Mpc). We used gamma-ray observations performed with the first Large-Sized Telescope (LST-1) of the Cherenkov Telescope Array Observatory (CTAO) and optical observations with the Liverpool Telescope (LT) combined with data from public repositories to evaluate the general properties of the event and the progenitor star. No significant emission above the LST-1 energy threshold for this observation ( similar to 100 GeV) was detected in the direction of SN 2024bch, and we computed an integral upper limit on the photon flux of F gamma ( &gt;100 GeV) &lt;= 3 :61 x 10(-12) cm(-2) s(-1) based on six nonconsecutive nights of observations with the LST-1, between 16 and 38 days after the explosion. Employing a general model for the gamma-ray flux emission, we found an upper limit on the mass-loss-rate to wind-velocity ratio of. M/u(w) &lt;= 10(-4) M-circle dot/yr s/km, although gamma-gamma absorption could potentially have skewed this estimation, e ffectively weakening our constraint. From spectro-photometric observations we found progenitor parameters of M-pr = 11 - 20 M-circle dot and R-pr = 531 +/- 125 R-circle dot. Finally, using archival images from the Hubble Space Telescope, we constrained the luminosity of the progenitor star to log (L-pr /L-circle dot) &lt;= 4.82 and its effective temperature to T-pr &lt;= 4000 K. Our results suggest that SN 2024bch is a type IIn-L supernova that originated from a progenitor star consistent with a red supergiant. We show how the correct estimation of the mass-loss history of a supernova will play a major role in future multiwavelength observations.

Název v anglickém jazyce

Constraining the TeV gamma-ray emission of SN 2024bch, a possible type IIn-L from a red supergiant progenitor

Popis výsledku anglicky

We present very high-energy optical photometry and spectroscopic observations of SN 2024bch in the nearby galaxy NGC 3206 (similar to 20 Mpc). We used gamma-ray observations performed with the first Large-Sized Telescope (LST-1) of the Cherenkov Telescope Array Observatory (CTAO) and optical observations with the Liverpool Telescope (LT) combined with data from public repositories to evaluate the general properties of the event and the progenitor star. No significant emission above the LST-1 energy threshold for this observation ( similar to 100 GeV) was detected in the direction of SN 2024bch, and we computed an integral upper limit on the photon flux of F gamma ( &gt;100 GeV) &lt;= 3 :61 x 10(-12) cm(-2) s(-1) based on six nonconsecutive nights of observations with the LST-1, between 16 and 38 days after the explosion. Employing a general model for the gamma-ray flux emission, we found an upper limit on the mass-loss-rate to wind-velocity ratio of. M/u(w) &lt;= 10(-4) M-circle dot/yr s/km, although gamma-gamma absorption could potentially have skewed this estimation, e ffectively weakening our constraint. From spectro-photometric observations we found progenitor parameters of M-pr = 11 - 20 M-circle dot and R-pr = 531 +/- 125 R-circle dot. Finally, using archival images from the Hubble Space Telescope, we constrained the luminosity of the progenitor star to log (L-pr /L-circle dot) &lt;= 4.82 and its effective temperature to T-pr &lt;= 4000 K. Our results suggest that SN 2024bch is a type IIn-L supernova that originated from a progenitor star consistent with a red supergiant. We show how the correct estimation of the mass-loss history of a supernova will play a major role in future multiwavelength observations.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10300 - Physical sciences

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

702

Číslo periodika v rámci svazku

1 Oct 2025

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

12

Strana od-do

A125

Kód UT WoS článku

001638041700001

EID výsledku v databázi Scopus

2-s2.0-105021474070