J/A+A/660/A138 SN2020qmp light curves (Srinivasaragavan+, 2022)
PGIR 20eid (SN 2020qmp): A Type II-P Supernova at 15.6 Mpc discovered by the
Palomar Gattini-IR survey.
Srinivasaragavan G.P., Sfaradi I., Jencson J., De K., Horesh A.,
Kasliwal M.M., Tinyanont S., Hankins M., Schulze S., Ashley M.C.B.,
Graham M.J., Karambelkar V., Lau R., Mahabal A.A., Moore A.M., Ofek E.O.,
Sharma Y., Sollerman J., Soon J., Soria R., Travouillon T., Walters R.
<Astron. Astrophys. 660, A138 (2022)>
=2022A&A...660A.138S 2022A&A...660A.138S (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, CCD
Keywords: supernovae: individual: SN2020qmp - shock waves
Abstract:
We present a detailed analysis of SN 2020qmp, a nearby Type IIP
core-collapse supernova (CCSN), discovered by the Palomar Gattini-IR
(PGIR) survey in the galaxy UGC07125 (distance of ∼15.6±4Mpc). We
illustrate how the multiwavelength study of this event helps our
general understanding of stellar progenitors and circumstellar medium
(CSM) interactions in CCSNe. We highlight the importance of
near-infrared (NIR) surveys for detections of SNe in dusty
environments.
We analyze data from observations in various bands: radio, NIR,
optical and X-rays. We use optical and NIR data for a spectroscopic
and spectropolarimetric study of the SN, and to model its lightcurve
(LC). We obtain an estimate of the ZAMS progenitor mass from the
luminosity of the [OI] doublet lines (λλ6300,6364)
normalized to the decay power of 56Co. We also independently
estimate the explosion energy and zero-age main sequence (ZAMS)
progenitor mass through hydrodynamical LC modeling. From radio and
X-ray observations, we derive the mass loss rate and microphysical
parameters of the progenitor star, and investigate possible deviations
from energy equipartition of magnetic fields and electrons in a
standard CSM interaction model. Finally, we simulate a sample of CCSNe
with plausible distributions of brightness and extinction, within
40Mpc, and test what fraction of the sample is detectable at peak
light by NIR surveys versus optical surveys.
SN 2020qmp displays characteristic hydrogen lines in its optical
spectra, as well as a plateau in its optical LC, hallmarks of a Type
IIP SN. We do not detect linear polarization during the plateau phase,
with a 3σ upper limit of 0.78%. Through hydrodynamical LC
modeling and an analysis of its nebular spectra, we estimate a
zero-age main-sequence progenitor mass of around 11.0M☉, and an
explosion energy of around 0.8x1051erg. We find that the spectral
energy distribution cannot be explained by a simple CSM interaction
model, assuming a constant shock velocity and steady mass-loss rate.
In particular, the excess X-ray luminosity compared with the
synchrotron radio luminosity suggests deviations from equipartition.
Finally, we demonstrate the advantages of NIR surveys over optical
surveys for the detection of dust-obscured CCSNe in the local
universe. Specifically, our simulations show that the Wide-Field
Infrared Transient Explorer (WINTER) will detect up to 14 more CCSNe
out of 75 expected in its footprint within 40Mpc, over five years
than an optical survey equivalent to the Zwicky Transient Facility
(ZTF) would detect.
We have determined or constrained the main properties of SN 2020qmp
and of its progenitor, highlighting the value of multiwavelength
follow up observations of nearby CCSNe. We have shown that forthcoming
NIR surveys will enable us to improve constraints on the local CCSN
rate by detecting obscured SNe that would be missed by optical
searches.
Description:
Photometric measurements obtained of SN 2020qmp, from the PGIR survey
(De et al., 2020PASP..132b5001D 2020PASP..132b5001D; J band), Zwicky Transient Facility
(Bellm et al. 2019PASP..131a8002B 2019PASP..131a8002B; g, r and i bands), and the Neils
Gehrels Swift Ultra-Violet Optical Telescope (Roming et al.
2005SSRv..120...95R 2005SSRv..120...95R; UVW2, UVM2, UVW1, u, b, and V bands).
Measurements begin from the latest non-detection made by PGIR.
Objects:
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RA (2000) DE Designation(s)
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12 08 44.43 +36 48 19.4 SN 2020qmp = SN 2020qmp
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 68 315 Photometric data of SN 2020qmp
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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3- 13 F11.3 d JD Julian date of observation
18- 27 A10 --- Inst Instrument measurement was taken with
32- 35 A4 --- Filter Photometric filter measurement was taken with (1)
42- 46 F5.2 mag magpsf ?=99 Magnitude in Filter (AB)
52- 56 F5.2 mag e_magpsf ?=99 Magnitude error in Filter )AB)
64- 68 F5.2 mag limmag Magnitude in Filter of limiting measurement (AB)
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Note (1): Filters are U, B, J, ugri, UVM2, UVW1 and UVW2.
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Acknowledgements:
Gokul Srinivasaragavan, gsriniv2(at)umd.edu
References:
De et al., 2020PASP..132b5001D 2020PASP..132b5001D, Palomar Gattini-IR: Survey Overview,
Data Processing System, On-sky Performance and First Result
Bellm et al., 2019PASP..131a8002B 2019PASP..131a8002B, The Zwicky Transient Facility:
System Overview, Performance, and First Results
Roming et al., 2005SSRv..120...95R 2005SSRv..120...95R, The Swift Ultra-Violet/Optical Telescope
(End) Patricia Vannier [CDS] 18-Feb-2022