J/ApJ/949/33 LCs and spectra of Type Ia SN 2021hpr (Lim+, 2023)
The early light curve of the Type Ia supernova 2021hpr in NGC 3147: progenitor
constraints with the companion interaction model.
Lim G., Im M., Paek G.S.H., Yoon S.-C., Choi C., Kim S., Wheeler J.C.,
Thomas B.P., Vinko J., Kim D., Seo J., Kang W., Kim T., Sung H.-I.,
Kim Y., Yoon J.-N., Kim H., Kim J., Bae H., Ehgamberdiev S., Burhonov O.,
Mirzaqulov D.
<Astrophys. J., 949, 33 (2023)>
=2023ApJ...949...33L 2023ApJ...949...33L
ADC_Keywords: Supernovae; Photometry, UBVRI; Spectra, optical
Keywords: Type Ia supernovae ; White dwarf stars ; Supernovae ;
Astrophysical explosive burning ; Transient sources ;
Time domain astronomy
Abstract:
The progenitor system of Type Ia supernovae (SNe Ia) is expected to be
a close binary system consisting of a carbon/oxygen white dwarf (WD)
and a nondegenerate star or another WD. Here, we present results from
high-cadence monitoring observations of SN 2021hpr in a spiral galaxy,
NGC 3147, and constraints on the progenitor system based on its early
multicolor light-curve data. First, we classify SN 2021hpr as a normal
SN Ia from its long-term photometric and spectroscopic data. More
interestingly, we found a significant "early excess" in the light
curve over a simple power-law ∼t2 evolution. The early light curve
evolves from blue to red to blue during the first week. To explain
this, we fitted the early part of the BVRI-band light curves with a
two-component model consisting of ejecta-companion interaction and a
simple power-law model. The early excess and its color can be
explained by shock-cooling emission due to a companion star having a
radius of 8.84±0.58R☉. We also examined Hubble Space Telescope
preexplosion images, finding no detection of a progenitor candidate,
consistent with the above result. However, we could not detect signs
of a significant amount of stripped mass from a nondegenerate
companion star (≲0.003M☉ for Hα emission). The early
excess light in the multiband light curve supports a nondegenerate
companion in the progenitor system of SN 2021hpr. At the same time,
the nondetection of emission lines opens the door for other methods to
explain this event.
Description:
SN 2021hpr was discovered on 2021 April 2.45 UT. Here, we report our
Intensive Monitoring Survey of Nearby Galaxies (IMSNG;
Im+ 2019JKAS...52...11I 2019JKAS...52...11I) imaging observations and the data reduction
procedures. In addition, we also used the data in the literature such
as those taken at Caucasian Mountain Observatory (CMO;
Tsvetkov+ 2021ATel14541....1T 2021ATel14541....1T) and by the Zwicky Transient Facility
(ZTF; Bellm+ 2019PASP..131a8002B 2019PASP..131a8002B).
NGC 3147 has been monitored by IMSNG since 2014 in the B and R bands.
In our data, SN 2021hpr was first identified in B- and R-band images
taken on 2021 April 1.29 (UT) with the 1m telescope of the Mt. Lemmon
Optical Astronomy Observatory (LOAO), located in the USA, after the
last nondetection on 2021 March 31.18.
In addition to the LOAO 1.0m telescope, we used the 0.6m telescope at
the Mt. Sobaek Optical Astronomy Observatory (SOAO), the 1.0m
telescope at the Seoul National University Astronomical Observatory
(SAO), the 0.6m telescope at the Chungbuk National University
Observatory (CBNUO), the 1.0m telescope at the Deokheung Optical
Astronomy Observatory (DOAO) in Korea, and SNUCAM of the 1.5m
telescope at the Maidanak Astronomical Observatory in Uzbekistan
(MAO). Only BVR-band data were obtained at CBNUO and MAO.
We performed long-slit spectroscopy on 2021 April 6, 14, and May 2 at
SAO. We used the Shelyak LISA spectrograph. See Section 2.2.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
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10 16 38.61 +73 24 01.8 SN 2021hpr = SN 2021hpr
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 38 710 Optical light curve of SN 2021hpr
fig7.dat 19 2860 SAO/LISA spectra of SN 2021hpr
fig10.dat 47 4719 HET/LRS2-B spectrum of SN 2021hpr at the nebular
phase of +243 days since the explosion
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See also:
J/ApJ/645/488 : SN type Ia luminosities (Wang+, 2006)
J/ApJ/659/122 : Improved distances to type Ia supernovae (Jha+, 2007)
J/ApJ/686/749 : Improved cosmological constraints from SNe (Kowalski+, 2008)
J/MNRAS/389/1577 : UBVRI absolute magnitudes of Type Ia SNe (Takanashi+, 2008)
J/ApJ/700/331 : Light curves of type Ia supernovae (CfA3) (Hicken+, 2009)
J/ApJ/716/712 : HST light curves of six SNe and Union2 (Amanullah+, 2010)
J/ApJS/190/166 : Optical catalog of AKARI NEP-wide survey (Jeon+, 2010)
J/ApJ/750/99 : The Pan-STARRS1 photometric system (Tonry+, 2012)
J/A+A/554/A27 : 2011fe spectrophotometric time series (Pereira+, 2013)
J/AJ/146/86 : Cosmicflows-2 catalog (Tully+, 2013)
J/AJ/148/1 : Optical and ultraviolet phot. of SN 2012fr (Zhang+, 2014)
J/ApJ/813/30 : UV-Opt. light curves of the SNIa iPTF14bdn (Smitka+, 2015)
J/A+A/609/A114 : Local Group AGB stars & red supergiants (Groenewegen+, 2018)
J/ApJ/893/143 : UBVRIJHK & spec. obs. of type Ia SN2019ein (Kawabata+, 2020)
J/ApJ/933/L45 : LCs and spectra of type Ia SN 2021aefx (Hosseinzadeh+, 2022)
J/ApJ/924/35 : Optical spectra of type Ia SN 2015bq (Li+, 2022)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.2 d MJD [59256.85/59578.77] Epoch in Modified Julian date
10- 15 F6.2 d Phase [-65.01/256.91] Days after B-band maximum where
Phase=t-59321.856
17- 21 A5 --- Filt Observed band
23- 27 F5.2 mag mag [14.12/23.07] AB magnitude in Filter (2)
29- 34 F6.2 mag e_mag [0.01/0.9]?=-99 The 1-sigma uncertainty in mag
36 I1 --- Tel [1/8] Telescope used for the observation (3)
38 I1 --- Det [0/1] Detection code (1=detected; or 0=3-sigma
detection limit)
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Note (2): Without reddening and mag offset (telescope) corrections.
Note (3): Telescope as follows:
1 = Mt. Lemmon Optical Astronomy Observatory 1m telescope (LOAO;
372 occurrences)
2 = Seoul National University Astronomical Observatory 1m telescope (SAO;
35 occurrences)
3 = Deokheung Optical Astronomy Observatory 1m telescope (DOAO;
113 occurrences)
4 = Mt. Sobaek Optical Astronomy Observatory 0.6m telescope (SOAO;
29 occurrences)
5 = Chungbuk National University Observatory 0.6m telescope (CBNUO;
55 occurrences)
6 = Maidanak Astronomical Observatory 1.5m telescope (MAO; 71 occurrences)
7 = Caucasian Mountain Observatory (CMO; 25 occurrences)
8 = Zwicky Transient Facility (ZTF; 10 occurrences)
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Byte-by-byte Description of file: fig7.dat
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Bytes Format Units Label Explanations
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1 A1 --- SpID Spectrum identifier (1)
3- 9 F7.2 0.1nm lambda [4600.6/8997] Observed wavelength; Angstroms
11- 19 E9.3 mW/nm/m2 Flux [-3.7e-14/2.5e-13] Observed flux density;
erg/cm2/s/Angstrom
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Note (1): Spectrum identifier as follows:
A = April 6.61, 2021 (-11.2d)
B = April 14.58, 2021 (-3.3d)
C = May 2.55, 2021 (+14.7d)
With (Phase) relative to the epoch of B-band maximum (59321.864 MJD).
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Byte-by-byte Description of file: fig10.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm lambda [3640/6950.3] Observed wavelength; Angstroms
9- 17 E9.3 mW/nm/m2 Flux [-5.5e-16/1e-15] Observed flux density;
erg/cm2/s/Angstrom
19- 26 E8.3 mW/nm/m2 e_Flux [0/1.6e-15] 1-sigma uncertainty in Flux
28- 35 E8.3 mW/nm/m2 Back [0/4.5e-14] Flux density of the background;
erg/cm2/s/Angstrom
37- 41 F5.3 --- Apcor [0.75/0.94] Aperture correction value
43- 47 F5.3 --- Telcor [0/1.1] Telluric correction value
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-May-2025