A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
A study in scarlet I. Photometric properties of a sample of intermediate-luminosity red transients
Alaotsikko: I. Photometric properties of a sample of intermediate-luminosity red transients
Tekijät: Valerin, G.; Pastorello, A.; Reguitti, A.; Benetti, S.; Cai, Y.-Z.; Chen, T.-W.; Eappachen, D.; Elias-Rosa, N.; Fraser, M.; Gangopadhyay, A.; Hsiao E., Y.; Howell D., A.; Inserra, C.; Izzo, L.; Jencson, J.; Kankare, E.; Kotak, R.; Mazzali P., A.; Misra, K.; Pignata, G.; Prentice S., J.; Sand D., J.; Smartt S., J.; Stritzinger M., D.; Tartaglia, L.; Valenti, S.; Anderson J., P.; Andrews J., E.; Amaro R., C.; Brennan, S.; Bufano, F.; Callis, E.; Cappellaro, E.; Dastidar, R.; Della Valle, M.; Fiore, A.; Fulton M., D.; Galbany, L.; Heikkilä, T.; Hiramatsu, D.; Karamehmetoglu, E.; Kuncarayakti, H.; Leloudas, G.; Lundquist, M.; McCully, C.; Müller-Bravo T., E.; Nicholl, M.; Ochner, P.; Padilla Gonzalez, E.; Paraskeva, E.; Pellegrino, C.; Rau, A.; Reichart D., E.; Reynolds T., M.; Roy, R.; Salmaso, I.; Singh, M.; Turatto, M.; Tomasella, L.; Wyatt, S.; Young D., R.
Kustantaja: EDP Sciences
Julkaisuvuosi: 2025
Journal: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: Astronomy & Astrophysics
Vuosikerta: 695
Aloitussivu: A42
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202451733
Verkko-osoite: https://doi.org/10.1051/0004-6361/202451733
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/492085269
Aims. We investigate the photometric characteristics of a sample of intermediate-luminosity red transients (ILRTs), a class of elusive objects with peak luminosity between that of classical novae and standard supernovae. Our goal is to provide a stepping stone in the path to reveal the physical origin of such events, thanks to the analysis of the datasets collected.
Methods. We present the multi-wavelength photometric follow-up of four ILRTs, namely NGC 300 2008OT-1, AT 2019abn, AT 2019ahd, and AT 2019udc. Through the analysis and modelling of their spectral energy distribution and bolometric light curves, we inferred the physical parameters associated with these transients.
Results. All four objects display a single-peaked light curve which ends in a linear decline in magnitudes at late phases. A flux excess with respect to a single blackbody emission is detected in the infrared domain for three objects in our sample, a few months after maximum. This feature, commonly found in ILRTs, is interpreted as a sign of dust formation. Mid-infrared monitoring of NGC 300 2008OT-1 761 days after maximum allowed us to infer the presence of ∼10−3–10−5 M⊙ of dust, depending on the chemical composition and the grain size adopted. The late-time decline of the bolometric light curves of the considered ILRTs is shallower than expected for 56Ni decay, hence requiring an additional powering mechanism. James Webb Space Telescope observations of AT 2019abn prove that the object has faded below its progenitor luminosity in the mid-infrared domain, five years after its peak. Together with the disappearance of NGC 300 2008OT-1 in Spitzer images seven years after its discovery, this supports the terminal explosion scenario for ILRTs. With a simple semi-analytical model we tried to reproduce the observed bolometric light curves in the context of a few solar masses ejected at few 103 km s−1 and enshrouded in an optically thick circumstellar medium.
Key words: circumstellar matter / supernovae: general / supernovae: individual: NGC 300 2008OT-1 / supernovae: individual: AT 2019abn / supernovae: individual: AT 2019ahd / supernovae: individual: AT 2019udc
Ladattava julkaisu This is an electronic reprint of the original article. |  |
Julkaisussa olevat rahoitustiedot:
Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de
los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Observations from the Nordic Optical Telescope were obtained through the NUTS2 collaboration which are supported in part by the Instrument Centre for Danish Astrophysics (IDA). The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA). This work makes use of data from the Las Cumbres Observatory
network. The LCO team is supported by NSF grants AST–1911225 and AST–1911151, and NASA SWIFT grant 80NSSC19K1639. Data were also obtained at the Liverpool Telescope, which is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos with financial support from the UK Science and Technology Facilities Council. Part of the observations were collected at Copernico and Schmidt
telescopes (Asiago, Italy) of the INAF – Osservatorio Astronomico di Padova. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. Time domain research by the University of Arizona team and D.J.S. is supported by NSF grants AST-1821987, 1813466, 1908972, & 2108032, and by the Heising-Simons Foundation under grant #20201864. G.V., N.E.R. and I.S.
acknowledge financial support from PRIN-INAF 2022 “Shedding light on the nature of gap transients: from the observations to the models”. N.E.R. also acknowledge support from the Spanish MICINN grant PID2019-108709GBI00 and FEDER funds, and from the program Unidad de Excelencia Maria de Maeztu CEX2020-001058-M. A.R. acknowledges financial support from the
GRAWITA Large Program Grant (PI P. D’Avanzo) and the PRIN-INAF 2022 “Shedding light on the nature of gap transients: from the observations to the models”. Y.-Z. Cai is supported by the National Natural Science Foundation of China (NSFC, Grant No. 12303054), the Yunnan Fundamental Research Projects (Grant No. 202401AU070063) and the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). T.E.M.B. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion (MCIN),
the Agencia Estatal de Investigacion (AEI) 10.13039/501100011033, and the European Union Next Generation EU/PRTR funds under the 2021 Juan de la Cierva program FJC2021-047124-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia
Maria de Maeztu CEX2020-001058-M. MF is supported by a Royal Society – Science Foundation Ireland University Research Fellowship. The Aarhus supernova group is funded by the Independent Research Fund Denmark (IRFD, grant numbers 8021-00170B, 10.46540/2032-00022B). L.G. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European
Social Fund (ESF). This work was funded by ANID, Millennium Science Initiative, ICN12_009 M.N. is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 948381). Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). H.K. was funded by the Academy of Finland projects 324504 and 328898. R.K. acknowledges support from the Research Council of Finland (340613).
