J/A+A/706/A271 SN 2022ngb light curves (Zhao+, 2026)
SN 2022ngb: A faint, slow-evolving Type IIb supernova with a low-mass envelope.
Zhao J.-W., Benetti S., Cai Y.-Z., Pastorello A., Elias-Rosa N.,
Reguitti A., Valerin G., Wang Z.-Y., Cappellaro E., Feng G.-F., Fiore A.,
Fitzpatrick B., Fraser M., Isern J., Kankare E., Kravtsov T., Kumar B.,
Lundqvist P., Matilainen K., Mattila S., Mazzali P.A., Moran S., Ochner P.,
Peng Z.-H., Reynolds T.M., Salmaso I., Srivastav S., Stritzinger M.D.,
Taubenberger S., Tomasella L., Vinko J., Wheeler J.C., Williams S.,
Pei S.-P., Yang Y.-J., Liu X.-K., Liu X.-W., Yang Y.-P.
<Astron. Astrophys. 706, A271 (2026)>
=2026A&A...706A.271Z 2026A&A...706A.271Z (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry ; Optical ; Infrared
Keywords: supernovae: general - supernovae: individual: SN 2022ngb -
galaxies: individual: UGC 11380
Abstract:
Type IIb supernovae (SNe IIb) are stellar explosions whose spectra
show transitional features between hydrogen-rich (Type II) and
helium-rich (Type Ib) SNe. Their progenitors are massive stars that
were mostly stripped of their hydrogen envelope, most likely through
binary interaction and/or strong stellar winds, making them key tools
for studying the late stages of the evolution of massive stars. An
extensive photometric and spectroscopic follow-up campaign of the Type
IIb SN 2022ngb is presented in the article. Through detailed modeling
of this dataset, we aim to constrain the key physical parameters of
the explosion, infer the nature of the progenitor star and its
environment, and probe the dynamical properties of the ejecta. We
analyze photometric and spectroscopic data of SN 2022ngb. By
constructing and modeling the bolometric light curve with
semi-analytic models, we estimate the primary explosion parameters.
The spectroscopic data are compared with those of well- studied SNe
IIb and NLTE models to constrain the properties of the progenitor and
the structure of the resulting ejecta. SN 2022ngb is a low-luminosity
SN IIb with a peak bolometric luminosity of
LBol=7.76(+1.15/-1.00)x1041erg/s and a V-band rising time of
24.32±0.50 days. Light curve modeling indicates an ejecta mass of
∼2.9-3.2M☉, an explosion energy of ∼1.4x1051erg, and a low
synthesized 56Ni mass of ∼0.045M☉. Nebular phase spectra exhibit
asymmetric line profiles, pointing to a non-spherical explosion and an
anisotropic distribution of radioactive material. Our analysis reveals
a relatively compact stripped-envelope progenitor with a pre- SN mass
of approximately 4.7M☉ (corresponding to a 15-16M☉ ZAMS
star). Our analysis suggests that SN 2022ngb originated from the
explosion of a moderate-mass relatively compact, stripped-envelope
star in a binary system. The asymmetries inferred from the nebular
phase spectral line features suggest a non-spherical explosion.
Description:
The multi-band photometric data for SN 2022ngb.
Objects:
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RA (2000) DE Designation(s)
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18 56 51.47 +36 37 07.8 SN 2022ngb = ATLAS 22res
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
22ngb.dat 67 1342 Multi-band photometric data for SN 2022ngb
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Byte-by-byte Description of file: 22ngb.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "date" Date Observation date
12- 19 F8.2 d MJD MJD of the observation
21- 26 F6.3 mag mag Observed apparent magnitude
28- 32 F5.3 mag e_mag ?=0 Uncertainty of the magnitude
34- 39 A6 --- Band Photometric filter/band name (1)
41- 44 A4 --- System Photometric system (e.g. Vega, AB)
46 A1 --- Type [P/U] Type of observation
(U for upper limit magnitude)
48- 57 A10 --- Inst Name of the instrument for the observation
59- 67 A9 --- Tel Name of the telescope for the observation
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Note (1): Filters are BV JHK griz cyan orange.
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Acknowledgements:
From Jie-Wei Zhao, zhaojiewei(at)stu.ynu.edu.cn
We gratefully thank the anonymous referee for his/her insightful
comments and suggestions that improved the paper. We thank Luc Dessart
for kindly providing the light curve and spectral models for SNe IIb,
as well as for his valuable guidance and support in this work. We
thank L.-H. Li for helpful discussions and T. Nagao for some data
observations.
This work is supported by the National Key Research and Development
Program of China (Grant No. 2024YFA1611603), the National Natural
Science Foundation of China (NSFC, Grant Nos. 12303054, 12473047), the
Yunnan Fundamental Research Projects (Grant Nos. 202401AU070063,
202501AS070078), the Yunnan Key Laboratory of Survey Science (No.
202449CE340002), and the International Centre of Supernovae, Yunnan
Key Laboratory (No. 202302AN360001). AP, AR, SB, EC, NER, LT, GV and
IS acknowledge support from the PRIN-INAF 2022, "Shedding light on the
nature of gap transients: from the observations to the models". AR
also acknowledges financial support from the GRAWITA Large Program
Grant (PI P. D'Avanzo).
N.E.R. also acknowledges support from the Spanish Ministerio de
Ciencia e Innovacion (MCIN) and the Agencia Estatal de Investigacion
(AEI) 10.13039/501100011033 under the program Unidad de Excelencia
Maria de Maeztu CEX2020-001058-M. A. F. acknowledges funding by the
European Union - NextGenerationEU RFF M4C2 1.1 PRIN 2022 project
"2022RJLWHN URKA" and by INAF 2023 Theory Grant ObFu 1.05.23.06.06
"Understanding R-process & Kilonovae Aspects (URKA)". EC acknowledges
support from MIUR, PRIN 2020 (METE, grant 2020KB33TP). BK is supported
by the "Special Project for High-End Foreign Experts", Xingdian
Funding from Yunnan Province. S. Mattila acknowledges financial
support from the Research Council of Finland project 350458. A.F.
acknowledges the support by the State of Hesse within the Research
Cluster ELEMENTS (Project ID 500/10.006). S. Moran is funded by
Leverhulme Trust grant RPG-2023-240. M.D. Stritzinger is funded by the
Independent Research Fund Denmark (IRFD, grant number
10.46540/2032-00022B). T.K. acknowledges support from the Research
Council of Finland project 360274. JV is supported by NKFIH-OTKA Grant
K142534. S.-P. Pei is supported by the Science and Technology
Foundation of Guizhou Province (QKHJC-ZK[2023]442). T.M.R is part of
the Cosmic Dawn Center (DAWN), which is funded by the Danish National
Research Foundation under grant DNRF140. T.M.R acknowledges support
from the Research Council of Finland project 350458. M.D.S. is funded
by the Independent Research Fund Denmark (IRFD, grant number
10.46540/2032-00022B) and by an Aarhus University Research Foundation
Nova project (AUFF-E-2023-9-28). Y.-J. Yang is supported by the
National Natural Science Foundation of China (Grants No. 12305066).
S.M. acknowledges financial support from the Research Council of
Finland project 350458. We acknowledge the support of the staffs of
the various observatories at which data were obtained. Based on
observations made with the Nordic Optical Telescope (NOT), 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 NOT were obtained
through the NUTS2 collaboration which is supported in part by the
Instrument Centre for Danish Astrophysics (IDA), and the Finnish
Centre for Astronomy with ESO (FINCA) via Academy of Finland grant nr
306531. The data presented here were obtained in part with ALFOSC,
which is provided by the Instituto de Astrofisica de Andalucia (IAA)
under a joint agreement with the University of Copenhagen and NOTSA.
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. The Italian Telescopio Nazionale Galileo (TNG) is 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 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),
(Programs GTCMULTIPLE2A-22A and GTCMULTIPLE2G-22B; PI: Nancy
Elias-Rosa) installed at the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias, on the island
of La Palma. This work makes use of data from the Las Cumbres
Observatory (LCO) Network and the Global Supernova Project. The LCO
team is supported by U.S. NSF grants AST-1911225 and AST-1911151, and
NASA. Based on observations obtained with the Hobby-Eberly Telescope
(HET), which is a joint project of the University of Texas at Austin,
the Pennsylvania State University, Ludwig-Maximillians-Universitaet
Muenchen, and Georg-August Universitaet Goettingen. The HET is named
in honor of its principal benefactors, William P. Hobby and Robert E.
Eberly. The Low Resolution Spectrograph 2 (LRS2) was developed and
funded by the University of Texas at Austin McDonald Observatory and
Department of Astronomy, and by Pennsylvania State University. We
thank the Leibniz-Institut fur Astrophysik Potsdam (AIP) and the
Institut fur Astrophysik Goettingen (IAG) for their contributions to
the construction of the integral field units. We acknowledge the Texas
Advanced Computing Center (TACC) at The University of Texas at Austin
for providing high performance computing, visualization, and storage
resources that have contributed to the results reported within this
paper. 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. The Pan-STARRS2 Surveys (PS2) and the PS2
public science archive have been made possible through contributions
by the Institute for Astronomy, the University of Hawaii, the
Pan-STARRS Project Office, the Max-Planck Society and its
participating institutes, 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. The Zwicky Transient Facility (ZTF) is supported by
the National Science Foundation under Grants No. AST-1440341 and
AST-2034437 and involves a collaboration that includes current
partners such as Caltech, IPAC, the Oskar Klein Center at Stockholm
University, the University of Maryland, the University of California,
Berkeley, the University of Wisconsin-Milwaukee, the University of
Warwick, Ruhr University, Cornell University, Northwestern University,
and Drexel University. Operations are conducted by COO, IPAC, and UW.
(End) Patricia Vannier [CDS] 12-Dec-2025