J/ApJ/957/100 Long-term sp. obs. of SN IIb/Ib 2022crv (Gangopadhyay+, 2023)
Bridging between Type IIb and Ib Supernovae: SN IIb 2022crv with a very thin
hydrogen envelope.
Gangopadhyay A., Maeda K., Singh A., N. A J, Nakaoka T., Kawabata K.S.,
Taguchi K., Singh M., Chandra P., Ryder S.D., Dastidar R., Yamanaka M.,
Kawabata M., Alsaberi R.Z.E., Dukiya N., Teja R.S., Ailawadhi B.,
Dutta A., Sahu D.K., Moriya T.J., Misra K., Tanaka M., Chevalier R.,
Tominaga N., Uno K., Imazawa R., Hamada T., Hori T., Isogai K.
<Astrophys. J., 957, 100 (2023)>
=2023ApJ...957..100G 2023ApJ...957..100G
ADC_Keywords: Spectra, optical; Supernovae
Keywords: Photometry ; Spectroscopy ; Supernovae ; Type Ib supernovae ;
Radio astronomy
Abstract:
We present optical, near-infrared, and radio observations of supernova
(SN) SN IIb 2022crv. We show that it retained a very thin H envelope
and transitioned from an SN IIb to an SN Ib; prominent Hα seen
in the pre-maximum phase diminishes toward the post-maximum phase,
while HeI lines show increasing strength. SYNAPPS modeling of the
early spectra of SN 2022crv suggests that the absorption feature at
6200Å is explained by a substantial contribution of Hα
together with SiII, as is also supported by the velocity evolution of
Hα. The light-curve evolution is consistent with the canonical
stripped-envelope SN subclass but among the slowest. The light curve
lacks the initial cooling phase and shows a bright main peak (peak
MV=-17.82±0.17mag), mostly driven by radioactive decay of
56Ni. The light-curve analysis suggests a thin outer H envelope
(Menv∼0.05M☉) and a compact progenitor (Renv∼3R☉). An
interaction-powered synchrotron self-absorption model can reproduce
the radio light curves with a mean shock velocity of 0.1c. The
mass-loss rate is estimated to be in the range of
(1.9-2.8)x10-5M☉/yr for an assumed wind velocity of 1000km/s,
which is on the high end in comparison with other compact SNe IIb/Ib.
SN 2022crv fills a previously unoccupied parameter space of a very
compact progenitor, representing a beautiful continuity between the
compact and extended progenitor scenario of SNe IIb/Ib.
Description:
We estimated the explosion time t0 of SN 2022crv to be
JD=2459627.75±0.5. See Section 2.1.
Adopting H0=73km/s/Mpc, Ωmatter=0.27 and Ωvacuum=0.73,
we obtain a distance of 34.4±2.4Mpc, corrected for Virgo, Shapley,
and Great Attractor, to the host galaxy NGC 3054 (with a redshift of
z=0.008091). See Section 2.2.
We observed SN 2022crv with the BgVriRI filters from ~-8 to 86 days
with respect to the V-band maximum. The imaging observations were
carried out using the 1.5m Kanata telescope (KT) of Hiroshima
University, 3.8m Seimei Telescope of Kyoto University at Okayama
observatory, 1m Sampurnanand Telescope (ST), 1.3m Devasthal Fast
Optical Telescope (DFOT), Aryabhatta Research Institute of
observational sciencES (ARIES), India and 2m Himalayan Chandra
Telescope (HCT), Indian Institute of Astrophysics (IIA), India.
The NIR data of SN 2022crv were obtained with the HONIR instrument of KT.
The spectroscopic observations were carried out using the Himalayan
Faint Object Spectrograph and Camera (HFOSC) mounted on the HCT,
KOOLS-IFU on the Seimei Telescope, and Aries Faint Object Spectrograph
and Camera (ADFOSC) mounted on the 3.6m Devasthal Optical Telescope
(DOT), ARIES, India. Our spectral coverage spans from -10 to +33days.
We included the publicly available Gemini-N/GMOS spectrum taken on
-15 days in our analysis (Andrews+ 2022TNSCR.454....1A 2022TNSCR.454....1A).
See Section 2.3.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
09 54 25.90 -25 42 11.1 SN 2022crv = ATLAS 22gdi
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table8.dat 82 11 Log of spectroscopic observations of SN 2022crv
sp/* . 11 Individual spectra in ASCII format
(data behind Figure 1)
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See also:
J/A+AS/135/391 : VI CCD photometry of NGC 6553 (Sagar+ 1999)
J/MNRAS/389/955 : u'BVg'r'i'z' light curves of SN 2008ax (Pastorello+, 2008)
J/MNRAS/383/1485 : BVRI light curves of SN 2003jd (Valenti+, 2008)
J/ApJ/702/226 : Swift/UVOT panchromatic obs. of SN 2008D (Modjaz+, 2009)
J/ApJ/741/97 : Light curves of Ibc supernovae (Drout+, 2011)
J/MNRAS/416/3138 : SN 2009jf light curves (Valenti+, 2011)
J/MNRAS/431/308 : SN 2011fu BVRI light curves (Kumar+, 2013)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/ApJ/908/75 : Radio fluxes of type Ib/c & II SNe (Bietenholz+, 2021)
J/ApJ/927/61 : Spectroscopic follow-up of Type Ib SN 2017iro (Kumar+, 2022)
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 F5.1 d Phase [-15.3/33.3] Phase measured with respect to
the V-band maximum (JD 2459644.19)
7- 18 A12 --- Tel Telescope (Seimei, HCT, DOT or Gemini-North)
20- 28 A9 --- Inst Instrument
30- 33 I4 0.1nm lam1 [3400/4100] Lower range of wavelength in Angstrom
34 A1 --- --- [-]
35- 38 I4 0.1nm lam2 [6840/9500] Upper range of wavelength in Angstrom
40- 49 A10 --- Date Observation date (UT)
51- 82 A32 --- File Filename; see subdirectory "sp"
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Byte-by-byte Description of file: sp/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
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1- 16 F16.11 0.1nm lambda [3652/9244] Rest Wavelength, Angstroms
18- 39 E22.7 mW/m2 Flux ?=0 Flux, erg/s/cm2
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Jan-2026