J/A+A/707/A80 Photometry of 6 SN 2009ip-like supernovae (Salmaso+, 2026)
SN 2024hpj: a perspective on SN 2009ip-like events.
Salmaso I., Pastorello A., Borsato E., Benetti S., Botticella M.T.,
Cai Y.-Z., Elias-Rosa N., Farina A., Fraser M., Galbany L.,
Gonzalez-Banuelos M., Gutierrez C.P., Huang M., Lundqvist P., Kangas T.,
Killestein T.L., Kravtsov T., Matilainen K., Morales-Garoffolo A., Mura A.,
Pignata G., Reguitti A., Reynolds T.M., Smartt S., Srivastav S.,
Tartaglia L., Valerin G., Wang Z.-Y.
<Astron. Astrophys. 707, A80 (2026)>
=2026A&A...707A..80S 2026A&A...707A..80S (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry ; Optical
Keywords: supernovae: general -
supernovae: individual: SN 2025csc -
supernovae: individual: SN 2024uzf -
supernovae: individual: SN 2024hpj -
supernovae: individual: SN 2022ytx -
supernovae: individual: SN 2022mop
Abstract:
Supernovae (SNe) IIn are terminal explosions of massive stars that
are surrounded by a dense circumstellar medium (CSM). Among SNe IIn, a
notable subset is the SNe 2009ip-like, which exhibit an initial,
fainter peak attributed to stellar variability in the late
evolutionary stages, followed by a brighter peak, interpreted as the
SN explosion itself. In this context, we analyse the
spectrophotometric evolution of SN 2024hpj, an object with a
triple-peaked light curve and spectra typical of a SN IIn but with a
complex line profile composed of broad P-Cygni features topped by
narrow emissions. Comparing it with other SNe 2009ip-like in the
literature, as well as other unpublished objects (SNe 2019mry,
2022ytx, 2024uzf, and 2025csc), we identify star-forming regions as
their preferred formation environment. On the other hand, the
diversity of spectrophotometric features within the sample suggests
that variations in CSM mass and distribution may influence the
observed characteristics. We identify four sub-classes based on the
luminosity and rapidity of the light curve evolution, which give
insights regarding possible differences in the progenitors, while a
statistical analysis on their observed rate indicates progenitor
masses around 25-31M☉ and lower.
Description:
Light curves of SN 2025csc, SN 2024uzf, SN 2024hpj, SN 2022ytx and
SN 2022mop.
Objects:
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RA (2000) DE Designation(s)
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17 48 47.759 +37 13 02.01 SN2024hpj
18 06 08.614 +23 28 00.48 SN2025csc
16 06 43.024 +48 43 28.25 SN2024uzf
23 00 46.550 +13 37 05.70 SN2022ytx
23 30 51.220 -02 56 33.90 SN2022mop
00 11 38.080 -68 34 18.10 SN2019mry
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
confront.dat 73 19 log of spectral observations
s2024hpj.dat 74 19 SN 2024hpj log of spectral observation
p2019mry.dat 100 137 SN 2019mry photometry (IV griz)
p2022mop.dat 107 794 SN 2022mop photometry
(BV ugriz gaia.G cyan orange PS1.w PS1.y)
p2022ytx.dat 108 332 SN 2022ytx photometry
(V ugriz gaia.G cyan orange PS1.w)
p2024hpj.dat 101 1235 SN 2024hpj photometry
(JHK ugri cyan orange PS1.w PS1.y)
p2024uzf.dat 108 114 SN 2024uzf photometry (ugri cyan orange)
p2025csc.dat 105 125 SN 2025csc photometry (griz cyan orange)
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Byte-by-byte Description of file: confront.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- SN Supernova name
9- 18 A10 "date" Date Observation date
20- 24 I5 d MJD Modified Julian Date
27- 29 I3 d Phase Phase from peak
31- 39 A9 --- Tel Telescope
41- 47 A7 --- Inst Instrument
49- 59 A11 --- Grism Grism
61- 69 A9 s ExpTime Exposure time
72- 73 I2 0.1nm Res Resolution
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Byte-by-byte Description of file: s2024hpj.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "date" Date Obsevation date
12- 16 I5 d MJD Modified Julian Date
19- 22 I4 d PhaseFromExplosion Phase from explosion
24- 27 I4 d PhaseFromPeak Phase from peak
29- 36 A8 --- Tel Telescope
38- 44 A7 --- Inst Instrument
46- 58 A13 --- Grism Grism
60- 68 A9 s ExpTime Exposure time
71- 74 F4.1 0.1nm Res Resolution
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Byte-by-byte Description of file: p*.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 "date" Date Observation date
25- 40 F16.10 d MJD Modified Julian Date
43- 48 A6 --- Band Band (1)
52- 55 A4 --- System [ab vega] Band system
60- 66 F7.4 mag mag Magnitude in Band
69- 74 F6.4 mag e_mag ?=0 Error on magnitude in Band
77 A1 --- Flag [PFU] Flag (P/F=reliable, U=upper limit)
83-108 A26 --- Tel Telescope
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Note (1): Bands could be ugriz, BVI, JHK, cyan, orange, gaia.G, PS1.w and PS1.y.
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Acknowledgements:
From Irene Salmaso, irene.salmaso(at)inaf.it
We thank the anonymous referee for the helpful comments,
S. Goto for providing the SN 2023vbg data, and S. Brennan for the
useful discussions. IS, AP, AR, GV, NER acknowledge financial support
from the PRIN-INAF 2022 "Shedding light on the nature of gap
transients: from the observations to the models". IS acknowledge
financial support from the SOXS project. YZC is supported by the
National Natural Science Foundation of China (NSFC, Grant No.
12303054), the National Key Research and Development Program of China
(Grant No. 2024YFA1611603), the Yunnan Fundamental Research Projects
(Grant Nos. 202401AU070063, 202501AS070078), and the International
Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). AR
acknowledges financial support from the GRAWITA Large Program Grant
(PI P. D'Avanzo). TLK acknowledges support via an Academy of Finland
grant (340613; P.I. R. Kotak), support from the Turku University
Foundation (grant no. 081810), and a Warwick Astrophysics prize
post-doctoral fellowship made possible thanks to a generous
philanthropic donation. MGB, CPG and NER acknowledge financial support
from the Spanish Ministerio de Ciencia e Innovacion (MCIN) and the
Agencia Estatal de Investigacion (AEI) 10.13039/501100011033 under
the PID2023-151307NB-I00 SNNEXT 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, and from the Departament de Recerca i Universitats
de la Generalitat de Catalunya through the 2021-SGR-01270 grant. CPG
acknowledges financial support from the Secretary of Universities and
Research (Government of Catalonia) and by the Horizon 2020 Research
and Innovation Programme of the European Union under the Marie
Sklodowska-Curie and the Beatriu de Pinos 2021 BP 00168 programme.
LG acknowledges financial support from AGAUR, CSIC, MCIN and AEI
10.13039/501100011033 under projects PID2023-151307NB-I00, PIE
20215AT016, CEX2020-001058- M, ILINK23001, COOPB2304, and
2021-SGR-01270. TK acknowledges support from the Research Council of
Finland project 360274. AMG acknowledges financial support from grant
PID2023-152609OA-I00, funded by the Spanish Ministerio de Ciencia,
Innovacion y Universidades (MICIU), the Agencia Estatal de
Investigacion (AEI, 10.13039/501100011033), and the European
Union's European Regional Development Fund (ERDF). Based on
observations collected at Copernico 1.82m telescope and Schmidt 67/92
telescope (Asiago Mount Ekar, Italy) INAF - Osservatorio Astronomico
di Padova. 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).
The Liverpool Telescope is operated on the island of La Palma by
Liverpool John Moores University in the Spanish Observatorio del Roque
de los Muchachos of the Instituto de Astrofisica de Canarias with
financial support from the UK Science and Technology Facilities
Council. This work was based in part on observations made with the
Italian Telescopio Nazionale Galileo (TNG), operated on the island of
La Palma by the Fundacion Galileo Galilei of the INAF (Istituto
Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias. Based on
observations made with the Gran Telescopio Canarias (GTC), (Programs
GTCMULTIPLE2B-24B (PI: Nancy Elias-Rosa), GTCMULTIPLE2G-24A (PI: Nancy
Elias-Rosa), GTCMULTIPLE2E-25A (PI: Antonia Morales-Garoffolo)
installed at the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofisica de Canarias, on the island of La Palma.
Based on observations collected at Centro Astronomico Hispano en
Andalucia (CAHA) at Calar Alto, operated jointly by Junta de
Andalucia and Consejo Superior de Investigaciones Cientificas
(IAACSIC). Based on observations obtained with the Samuel Oschin
Telescope 48- inch and the 60-inch Telescope at the Palomar
Observatory as part of the Zwicky Transient Facility project. ZTF is
supported by the National Science Foundation under Grant No.
AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann
Institute for Science, the Oskar Klein Center at Stockholm University,
the University of Maryland, Deutsches Elektronen-Synchrotron and
Humboldt University, the TANGO Consortium of Taiwan, the University of
Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore
National Laboratories, and IN2P3, France. Operations are conducted by
COO, IPAC, and UW. The Pan- STARRS1 Surveys (PS1) and the PS1 public
science archive have been made possible through contributions by the
Institute for Astronomy, the University of Hawaii, the Pan-STARRS
Project O ce, the Max-Planck Society and its participat
inginstitutes, the Max Planck Institute for Astronomy, Heidelberg and
the Max Planck Institute for Extraterrestrial Physics, Garching, The
Johns Hopkins University, Durham University, the University of
Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian
Center for Astrophysics, the Las Cumbres Observatory Global Telescope
Network Incorporated, the National Central University of Taiwan, the
Space Telescope Science Institute, the National Aeronautics and Space
Administration under Grant No. NNX08AR22G issued through the Planetary
Science Division of the NASA Science Mission Directorate, the National
Science Foundation Grant No. AST-1238877, the University of
Maryland, Eotvos Lorand University (ELTE), the Los Alamos National
Laboratory, and the Gordon and Betty Moore Foundation. This work has
made use of data from the Asteroid Terrestrial-impact Last Alert
System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert
System (ATLAS) project is primarily funded to search for near earth
asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and
80NSSC18K1575; byproducts of the NEO search include images and
catalogs from the survey area. This work was partially funded by
Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889, and STFC grants
ST/T000198/1 and ST/S006109/1. The ATLAS science products have been
made possible through the contributions of the University of Hawaii
Institute for Astronomy, the Queen's University Belfast, the Space
Telescope Science Institute, the South African Astronomical
Observatory, and The Millennium Institute of Astrophysics (MAS),
Chile. This work makes use of observations from the Las Cumbres
Observatory global telescope network (data from GSP telescope).
Based on observations made with the William Herschel Telescope
operated on the island of La Palma by the Isaac Newton Group of
Telescopes in the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofisica de Canarias. We acknowledge the usage of
the HyperLeda database (http://leda.univ-lyon1.fr). This research has
made use of the NASA/IPAC Extragalactic Database, which is funded by
the National Aeronautics and Space Administration and operated by the
California Institute of Technology.
(End) Patricia Vannier [CDS] 30-Dec-2025