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Exploring the multi-wavelength properties of the high energetic event ZTF20abbiixp/GRB 200524A: from prompt emission to afterglow

A. GhoshDimpleKuntal MisraAryabhatta Research Institute of observational sciences , Manora Peak , Nainital 263 001 , IndiaP. Yu. MinaevSpace Research Institute , Russian Academy of Sciences , Moscow , 117997 , RussiaY. YaoCahill Center for Astrophysics , California Institute of Technology , MC 249-17 , 1200 E California Boulevard , Pasadena , CA , 91125 , USAD. A. KannInstituto de Astrofísica de Andalucía (IAA-CSIC) , Glorieta de la Astronomía , s/n , E-18008 , Granada , SpainM. BlazekInstituto de Astrofísica de Andalucía (IAA-CSIC) , Glorieta de la Astronomía , s/n , E-18008 , Granada , SpainA. S. PozanenkoSpace Research InstituteS. BelkinSchool of Physics & Astronomy , Monash University , Clayton VIC 3800 , AustraliaL. IzzoDARK , Niels Bohr Institute , University of Copenhagen , Jagtvej 155A , 2200 , Copenhagen N , DenmarkH. KumarPhysics Department , Indian Institute of Technology Bombay , Powai , 400 076 , IndiaA. de Ugarte PostigoA. RossiNational Institute for AstrophysicsG. C. AnupamaIndian Institute of Astrophysics , 2nd Block 100 Feet Rd , Koramangala Bangalore , 560 034 , IndiaV. BhaleraoPhysics Department , Indian Institute of Technology Bombay , Powai , 400 076 , IndiaD. BhattacharyaDepartment of Physics , Ashoka University , Sonipat , Haryana - 131029 , IndiaN. K. ChakradhariSchool of Studies in Physics and Astrophysics , Pandit Ravishankar Shukla University , Raipur , Chattisgarh 492010 , IndiaS. ChandraIndian Institute of Space Science and Technology , Trivandrum 695547 , Kerala , IndiaR. GuptaK. M. JayasuryaA. KumarDepartment of Physics , Royal Holloway , University of London , Egham , TW20 0EX , UKB. KumarSouth-Western Institute for Astronomy Research , Yunnan University , Kunming , Yunnan 650504 , People's Republic of ChinaT. S. KumarAryabhatta Research Institute of observational sciences , Manora Peak , Nainital 263 001 , IndiaА. С. МосквитинSpecial Astrophysical Observatory , Russian Academy of Sciences , Nizhnij Arkhyz , 369167 , RussiaS. B. PandeyAryabhatta Research Institute of observational sciences , Manora Peak , Nainital 263 001 , IndiaA. OmarIndian Institute of Technology , Kanpur , 208016 , IndiaA. R. RaoTata Institute of Fundamental Research , Homi Bhabha Road , Mumbai , India 400 005L. ResmiIndian Institute of Space Science and Technology , Trivandrum 695547 , Kerala , IndiaV. RumyantsevCrimean Astrophysical ObservatoryP. SanwalAryabhatta Research Institute of observational sciences , Manora Peak , Nainital 263 001 , IndiaA. VolnovaSpace Research InstituteA. NovichonokPetrozavodsk State University , Petrozavodsk , 185910 , RussiaM. KrugovFesenkov Astrophysical Institute , Almaty , 050020 , KazakhstanS. EhgamberdievUlugh Beg Astronomical Institute , Uzbekistan Academy of Sciences , Tashkent 100052 , UzbekistanA. E. VolvachCNRS , Artemis , 06304 Nice , France

2026

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Annotatsiya

We conducted a comprehensive multi-wavelength analysis of a high energetic long-duration ZTF20abbiixp / GRB~200524A detected by \textit{Fermi} Gamma Ray Burst Monitor (GBM). Our study combines extended high-energy observations from multiple space-based observatories including \textit{Fermi} with broadband afterglow data spanning X-ray to radio wavelengths, complemented by extensive photometric and spectroscopic follow-up from several ground-based optical facilities worldwide like 3.6-m Devasthal Optical Telescope (DOT). ZTF20abbiixp / GRB~200524A exhibits almost negligible spectral lag, likely arising from the presence of multiple overlapping emission episodes, a property uncommon among long-duration bursts. The burst additionally shows a clear intensity-tracking evolution of the prompt-emission spectral parameters. The broadband afterglow light curve best fits with a broken powerlaw with a break at $10^{5}$ s since the GBM trigger. The electron powerlaw index (p) calculated from the temporal and spectral slopes fail to distinguish between a interstellar medium and a wind environment. Our custom-developed afterglow model fits the panchromatic data well, combining forward shock (FS) and reverse shock (RS) emission. The RS contribution required to fit the early time optical data. The inferred afterglow model parameters suggest that ZTF20abbiixp / GRB~200524A is a high energetic burst expanding into a dense ISM environment, with a relatively large value of the fraction of energy going to accelerating electron and magnetic field ($ε_B$).

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DOI: 10.48550/arxiv.2608.09704

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