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XRF 241001A/SN 2024aiiq: A Faint Soft X-ray Transient Detected by SVOM with a Broad-Line Type Ic Supernova Revealed by JWST

Fuente: arXiv

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Hauptverfasser:	Schneider, B., Brunet, M., Gompertz, B. P., Turpin, D., Malesani, D. B., Godet, O., Levan, A. J., Daigne, F., Sarin, N., Rakotondrainibe, N. A., Martin-Carrillo, A., Palmerio, J. T., Thöne, C. C., Li, H. L., Saccardi, A., Postigo, A. de Ugarte, Antier, S., Buat, V., Ďurovčíková, D., Izzo, L., Leung, J. K., Mo, G., Qiu, Y. L., Vergani, S. D., Wang, J., Wei, J. Y., Xin, L. P., Mochkovitch, R., Zhang, B., Cai, H. B., Campana, S., Coleiro, A., Cordier, B., D'Avanzo, P., Dagoneau, N., D'Elia, V., Dong, Y. W., Götz, D., Guillot, S., Han, X. H., Hartmann, D. H., Huang, L., Huang, Y. F., Jakobsson, P., Klotz, A., Lachaud, C., Lu, X. M., Maggi, P., De Pasquale, M., Piron, F., Salvaterra, R., Schanne, S., Sollerman, J., Tanvir, N. R., Vidadi, Z., Wang, P., Wu, C., Xiong, S. L., Xu, Y., Zafar, T., Zhang, P. P., Zhang, S. N., Zheng, S. J.
Format:	Preprint
Veröffentlicht:	2026
Schlagworte:	High Energy Astrophysical Phenomena
Online-Zugang:	Acceder al recurso
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_version_	1866913053969219584
author	Schneider, B. Brunet, M. Gompertz, B. P. Turpin, D. Malesani, D. B. Godet, O. Levan, A. J. Daigne, F. Sarin, N. Rakotondrainibe, N. A. Martin-Carrillo, A. Palmerio, J. T. Thöne, C. C. Li, H. L. Saccardi, A. Postigo, A. de Ugarte Antier, S. Buat, V. Ďurovčíková, D. Izzo, L. Leung, J. K. Mo, G. Qiu, Y. L. Vergani, S. D. Wang, J. Wei, J. Y. Xin, L. P. Mochkovitch, R. Zhang, B. Cai, H. B. Campana, S. Coleiro, A. Cordier, B. D'Avanzo, P. Dagoneau, N. D'Elia, V. Dong, Y. W. Götz, D. Guillot, S. Han, X. H. Hartmann, D. H. Huang, L. Huang, Y. F. Jakobsson, P. Klotz, A. Lachaud, C. Lu, X. M. Maggi, P. De Pasquale, M. Piron, F. Salvaterra, R. Schanne, S. Sollerman, J. Tanvir, N. R. Vidadi, Z. Wang, P. Wu, C. Xiong, S. L. Xu, Y. Zafar, T. Zhang, P. P. Zhang, S. N. Zheng, S. J.
author_facet	Schneider, B. Brunet, M. Gompertz, B. P. Turpin, D. Malesani, D. B. Godet, O. Levan, A. J. Daigne, F. Sarin, N. Rakotondrainibe, N. A. Martin-Carrillo, A. Palmerio, J. T. Thöne, C. C. Li, H. L. Saccardi, A. Postigo, A. de Ugarte Antier, S. Buat, V. Ďurovčíková, D. Izzo, L. Leung, J. K. Mo, G. Qiu, Y. L. Vergani, S. D. Wang, J. Wei, J. Y. Xin, L. P. Mochkovitch, R. Zhang, B. Cai, H. B. Campana, S. Coleiro, A. Cordier, B. D'Avanzo, P. Dagoneau, N. D'Elia, V. Dong, Y. W. Götz, D. Guillot, S. Han, X. H. Hartmann, D. H. Huang, L. Huang, Y. F. Jakobsson, P. Klotz, A. Lachaud, C. Lu, X. M. Maggi, P. De Pasquale, M. Piron, F. Salvaterra, R. Schanne, S. Sollerman, J. Tanvir, N. R. Vidadi, Z. Wang, P. Wu, C. Xiong, S. L. Xu, Y. Zafar, T. Zhang, P. P. Zhang, S. N. Zheng, S. J.
contents	X-ray flashes (XRFs) are a type of gamma-ray bursts (GRBs) with prompt emission predominantly below 30 keV poorly detected by previous missions. The advent of the SVOM mission, with its wide-field instrument ECLAIRs, provides a new way to detect soft X-ray transients such as XRFs. We present photometric and spectroscopic observations of XRF 241001A detected by SVOM, a soft, sub-luminous, and low-energetic burst located in a poorly populated region of the Amati relation. We investigate the origin of its faint, soft high-energy emission to assess its connection to the long GRB population. We analyze the SVOM/ECLAIRs prompt emission and model its afterglow emission from X-ray to-radio. We present JWST/NIRSpec and SVOM/VT observations of the associated supernova (SN 2024aiiq), which we model with an Arnett radioactive decay component and compare its properties with previously detected GRB/SNe. XRF 241001A is located at z = 0.573 and has a prompt emission dominated by photons below 20 keV with a duration of T90 = 3.14 seconds. Its spectrum can be modeled by non-thermal or thermal models, all pointing towards a low Epeak < 10 keV and Eiso ~ 8x10^49 erg. The X-ray-to-radio afterglow modeling favors an origin from a relativistic jet viewed on-axis. In the optical, XRF 241001A exhibits an early blue emission, similar to that detected in some fast X-ray transients and inconsistent with synchrotron emission. The JWST/NIRSpec observations firmly established its collapsar origin by revealing a SN Type Ic with broad lines, comparable to SN 1998bw and SN 2025kg-like events. XRF 241001A is a soft, low-luminosity collapsar event produced by a weak relativistic jet observed on-axis, supporting the view that part of the XRF population forms the low-energy tail of the long GRB population. It demonstrates the potential of SVOM/ECLAIRs to probe the soft regime of the high-energy transient population.
format	Preprint
id	arxiv_https___arxiv_org_abs_2604_20346
institution	arXiv
publishDate	2026
record_format	arxiv
spellingShingle	XRF 241001A/SN 2024aiiq: A Faint Soft X-ray Transient Detected by SVOM with a Broad-Line Type Ic Supernova Revealed by JWST Schneider, B. Brunet, M. Gompertz, B. P. Turpin, D. Malesani, D. B. Godet, O. Levan, A. J. Daigne, F. Sarin, N. Rakotondrainibe, N. A. Martin-Carrillo, A. Palmerio, J. T. Thöne, C. C. Li, H. L. Saccardi, A. Postigo, A. de Ugarte Antier, S. Buat, V. Ďurovčíková, D. Izzo, L. Leung, J. K. Mo, G. Qiu, Y. L. Vergani, S. D. Wang, J. Wei, J. Y. Xin, L. P. Mochkovitch, R. Zhang, B. Cai, H. B. Campana, S. Coleiro, A. Cordier, B. D'Avanzo, P. Dagoneau, N. D'Elia, V. Dong, Y. W. Götz, D. Guillot, S. Han, X. H. Hartmann, D. H. Huang, L. Huang, Y. F. Jakobsson, P. Klotz, A. Lachaud, C. Lu, X. M. Maggi, P. De Pasquale, M. Piron, F. Salvaterra, R. Schanne, S. Sollerman, J. Tanvir, N. R. Vidadi, Z. Wang, P. Wu, C. Xiong, S. L. Xu, Y. Zafar, T. Zhang, P. P. Zhang, S. N. Zheng, S. J. High Energy Astrophysical Phenomena X-ray flashes (XRFs) are a type of gamma-ray bursts (GRBs) with prompt emission predominantly below 30 keV poorly detected by previous missions. The advent of the SVOM mission, with its wide-field instrument ECLAIRs, provides a new way to detect soft X-ray transients such as XRFs. We present photometric and spectroscopic observations of XRF 241001A detected by SVOM, a soft, sub-luminous, and low-energetic burst located in a poorly populated region of the Amati relation. We investigate the origin of its faint, soft high-energy emission to assess its connection to the long GRB population. We analyze the SVOM/ECLAIRs prompt emission and model its afterglow emission from X-ray to-radio. We present JWST/NIRSpec and SVOM/VT observations of the associated supernova (SN 2024aiiq), which we model with an Arnett radioactive decay component and compare its properties with previously detected GRB/SNe. XRF 241001A is located at z = 0.573 and has a prompt emission dominated by photons below 20 keV with a duration of T90 = 3.14 seconds. Its spectrum can be modeled by non-thermal or thermal models, all pointing towards a low Epeak < 10 keV and Eiso ~ 8x10^49 erg. The X-ray-to-radio afterglow modeling favors an origin from a relativistic jet viewed on-axis. In the optical, XRF 241001A exhibits an early blue emission, similar to that detected in some fast X-ray transients and inconsistent with synchrotron emission. The JWST/NIRSpec observations firmly established its collapsar origin by revealing a SN Type Ic with broad lines, comparable to SN 1998bw and SN 2025kg-like events. XRF 241001A is a soft, low-luminosity collapsar event produced by a weak relativistic jet observed on-axis, supporting the view that part of the XRF population forms the low-energy tail of the long GRB population. It demonstrates the potential of SVOM/ECLAIRs to probe the soft regime of the high-energy transient population.
title	XRF 241001A/SN 2024aiiq: A Faint Soft X-ray Transient Detected by SVOM with a Broad-Line Type Ic Supernova Revealed by JWST
topic	High Energy Astrophysical Phenomena
url	https://arxiv.org/abs/2604.20346