J/A+A/678/A209 SN 2022xxf photometry and spectra (Kuncarayakti+, 2023)
The broad-lined Type-Ic supernova SN 2022xxf with extraordinary two-humped
light curves.
I. Signatures of H/He-free interaction in the first four months.
Kuncarayakti H., Sollerman J., Izzo L., Maeda K., Yang S., Schulze S.,
Angus C.R., Aubert M., Auchettl K., Della Valle M., Dessart L., Hinds K.,
Kankare E., Kawabata M., Lundqvist P., Nakaoka T., Perley D., Raimundo S.I.,
Strotjohann N.L., Taguchi K., Cai Y.-Z., Charalampopoulos P., Fang Q.,
Fraser M., Gutierrez C.P., Imazawa R., Kangas T., Kawabata K.S., Kotak R.,
Kravtsov T., Matilainen K., Mattila S., Moran S., Murata I., Salmaso I.,
Anderson J.P., Ashall C., Bellm E.C., Benetti S., Chambers K.C., Chen T.-W.,
Coughlin M., De Colle F., Fremling C., Galbany L., Gal-Yam A., Gromadzki M.,
Groom S.L., Hajela A., Inserra C., Kasliwal M.M., Mahabal A.A.,
Martin-Carrillo A., Moore T., Mueller-Bravo T.E., Nicholl M., Ragosta F.,
Riddle R.L., Sharma Y., Srivastav S., Stritzinger M.D., Wold A., Young D.R.
<Astron. Astrophys. 678, A209 (2023)>
=2023A&A...678A.209K 2023A&A...678A.209K (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, infrared ; Optical ; Spectroscopy
Keywords: supernovae: general - supernova: individual: SN2022xxf
Abstract:
We report on our study of supernova (SN) 2022xxf based on observations
obtained during the first four months of its evolution. The light
curves (LCs) display two humps of similar maximum brightness separated
by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN
IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705,
z=0.0037, at a distance of about 20Mpc). Optical and near-infrared
photometry and spectroscopy are used to identify the energy source
powering the LC. Nearly 50 epochs of high signal-to-noise-ratio
spectroscopy were obtained within 130 days, comprising an unparalleled
dataset for a SN IcBL, and one of the best-sampled SN datasets to
date. The global spectral appearance and evolution of SN 2022xxf
points to typical SN Ic/IcBL, with broad features (up to ∼14000km/s)
and a gradual transition from the photospheric to the nebular
phase. However, narrow emission lines (corresponding to
∼1000-2500km/s) are present in the spectra from the time of the second
rise, suggesting slower-moving circumstellar material (CSM). These
lines are subtle, in comparison to the typical strong narrow lines of
CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are
readily noticeable at late times such as in MgI λ5170 and [OI]
λ5577. Unusually, the near-infrared spectra show narrow line
peaks in a number of features formed by ions of O and Mg. We infer the
presence of CSM that is free of H and He. We propose that the
radiative energy from the ejecta-CSM interaction is a plausible
explanation for the second LC hump. This interaction scenario is
supported by the color evolution, which progresses to the blue as the
light curve evolves along the second hump, and the slow second rise
and subsequent rapid LC drop. SN 2022xxf may be related to an emerging
number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue
colors, and subtle CSM interaction lines. The progenitor stars of
these SNe likely experienced an episode of mass loss shortly prior to
explosion consisting of H/He-free material.
Description: The first observations of SN 2022xxf/ZTF22abnvurz with
the Zwicky Transient Facility, and the Palomar Schmidt 48-inch (P48)
Samuel Oschin telescope under the twilight survey, were made on
October 18, 2022 (MJDZTFFirstDerection=59870.53) in r-band, one
day after the discovery.
The first spectrum of SN 2022xxf was obtained using the Hiroshima
One-shot Wide-field Polarimeter (HOWPol) on the 1.5-m Kanata telescope
at the Higashi-Hiroshima Observatory, Hiroshima University.
Spectra and photometry data of SN 2022xxf.
Objects:
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RA (2000) DE Designation(s)
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11 30 05.94 +09 16 57.3 SN 2022xxf = SN 2022xxf
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
photnir.dat 38 12 NIR photometry (JHK)
photvis.dat 38 190 Visible photometry (ugriz)
bol.dat 66 47 Bolometric light curve of SN 2022xxf
bol-spln.dat 28 117 Calculated bolometric light curve
listsp.dat 70 47 List of spectra
sp/* . 47 Individual spectra
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Byte-by-byte Description of file: photnir.dat photvis.dat
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Bytes Format Units Label Explanations
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1- 10 F10.2 d JD Julian date of observation
12- 17 F6.3 mag mag Magnitude in Filter
19- 23 F5.3 mag e_mag Magnitude in Filter error
25- 29 F5.2 mag limmag Limiting magnitude in Filter
31 A1 --- Filt [JHKugriz] Filter
33- 38 A6 --- Inst Instrument
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Byte-by-byte Description of file: bol.dat
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Bytes Format Units Label Explanations
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1- 20 F20.16 d Phase Days from first maximum (MJD 59880.0)
22- 43 E22.17 10-7W Lbol Bolometric luminosity
45- 66 E22.17 10-7W e_Lbol Bolometric luminosity error
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Byte-by-byte Description of file: bol-spln.dat
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Bytes Format Units Label Explanations
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1- 5 F5.1 d Phase Days from first maximum (MJD 59880.0)
7- 28 E22.17 10-7W Lbol Bolometric luminosity
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Byte-by-byte Description of file: listsp.dat
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Bytes Format Units Label Explanations
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1- 31 A31 --- FileName Name of the spectrum file in subdirectory sp
35- 70 A36 --- Title Title of the file
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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1- 17 F17.11 0.1nm lambda Wavelength
19- 31 E13.7 10mW/m2 Flux Flux (in erg/s/cm2/Å))
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Acknowledgements:
Hanindyo Kuncarayakti, kuncarayakti(at)gmail.com
(End) Patricia Vannier [CDS] 11-Oct-2023