J/ApJ/893/132 Optical follow-up of SNIc ZTF18aaqjovh (Ho+, 2020)
The broad-lined Ic supernova ZTF18aaqjovh (SN 2018bvw): an optically discovered
engine-driven supernova candidate with luminous radio emission.
Ho A.Y.Q., Corsi A., Cenko S.B., Taddia F., Kulkarni S.R., Adams S., De K.,
Dekany R., Frederiks D.D., Fremling C., Golkhou V.Z., Graham M.J., Hung T.,
Kupfer T., Laher R.R., Mahabal A., Masci F.J., Miller A.A., Neill J.D.,
Reiley D., Riddle R., Ridnaia A., Rusholme B., Sharma Y., Sollerman J.,
Soumagnac M.T., Svinkin D.S., Shupe D.L.
<Astrophys. J., 893, 132-132 (2020)>
=2020ApJ...893..132H 2020ApJ...893..132H (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae; Photometry; Spectra, optical
Keywords: Core-collapse supernovae; Type Ic supernovae; Supernovae; Hypernovae
Radio transient sources; Transient sources; High energy astrophysics
Time domain astronomy; Sky surveys
Abstract:
We present ZTF18aaqjovh (SN 2018bvw), a high-velocity ("broad-lined")
stripped-envelope (Type Ic) supernova (Ic-BL SN) discovered in the
Zwicky Transient Facility one-day cadence survey. ZTF18aaqjovh shares
a number of features in common with engine-driven explosions: the
photospheric velocity and the shape of the optical light curve are
very similar to those of the Type Ic-BL SN 1998bw, which was
associated with a low-luminosity gamma-ray burst (LLGRB) and had
relativistic ejecta. However, the radio luminosity of ZTF18aaqjovh is
almost two orders of magnitude fainter than that of SN 1998bw at the
same velocity phase, and the shock velocity is at most mildly
relativistic (v=0.06-0.4c). A search of high-energy catalogs reveals
no compelling gamma-ray burst (GRB) counterpart to ZTF18aaqjovh, and
the limit on the prompt GRB luminosity of Lγ,iso∼1.6x1048erg/s
excludes a classical GRB but not an LLGRB. Altogether, ZTF18aaqjovh
represents another transition event between engine-driven SNe
associated with GRBs and "ordinary" Ic-BL SNe.
Description:
ZTF18aaqjovh was discovered in an image obtained on 2018 May 5 UT as
part of the ZTF one-day cadence survey. The full light curve,
corrected for Milky Way extinction, is provided in Table 1. The P48
measurements come from forced photometry (Yao+ 2019, J/ApJ/886/152).
The g-band reference image was constructed from data taken between
2018 April 22 and 2018 May 16, so we had to subtract a baseline flux
to account for SN light in the reference. See Section 2.1.
On 2018 May 9 UT we obtained a spectrum of ZTF18aaqjovh using the
P60/SEDM. On 2018 May 14 UT, we observed ZTF18aaqjovh using the Low
Resolution Imaging Spectrometer (LRIS) on the Keck I 10m telescope.
The next day, we observed the source using the Andalusia Faint Object
Spectrograph and Camera (ALFOSC) on the Nordic Optical Telescope (NOT).
We obtained another spectrum on 2018 June 8 UT using the Double Beam
Spectrograph (DBSP) on the 200 inch Hale telescope at the Palomar
Observatory.
Objects:
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RA (ICRS) DE Designation(s)
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11 52 43.62 +25 40 30.1 ZTF18aaqjovh = SN 2018bvw
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 35 74 Optical light curve of ZTF18aaqjovh from
forced photometry on P48 images
fig3.dat 37 16702 Optical spectra of ZTF18aaqjovh
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See also:
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
J/ApJS/126/19 : BATSE gamma-ray burst spectral cat. I. (Preece+, 2000)
J/MNRAS/383/1485 : BVRI light curves of SN 2003jd (Valenti+, 2008)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/other/Nat/463.513 : Radio observations of SN 2009bb (Soderberg+, 2010)
J/AJ/141/163 : Ultimate LC of SN 1998bw/GRB 980425 (Clocchiatti+, 2011)
J/ApJ/782/42 : Panchromatic observations of PTF11qcj (Corsi+, 2014)
J/A+A/593/A68 : PTF12os & iPTF13bvn spectra and LCs (Fremling+, 2016)
J/ApJ/832/108 : Spectral data of Type Ic & Ic-bl SNe (Modjaz+, 2016)
J/ApJ/880/7 : Census of the Local Universe survey. I. CLU-Ha (Cook+, 2019)
J/ApJ/886/152 : ZTF early observations of Type Ia SNe. I. LCs (Yao+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 F12.6 --- MJD [58243.17/58284.22] Observation date
14- 18 F5.2 --- Delt [9.99/51.04] Time interval Δt
20- 22 A3 --- Inst Instrument (P48 or P60)
24 A1 --- Filt Filter (g or r)
26- 30 F5.2 --- mag [18.17/20.85] AB magnitude in Filt
32- 35 F4.2 --- e_mag [0.02/0.29] mag uncertainty
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Byte-by-byte Description of file: fig3.dat
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Bytes Format Units Label Explanations
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1 I1 --- Code [1/5] Observation code (1)
3- 12 F10.4 0.1nm lambda [3077.4/10500.4] Wavelength;
in Angstrom units
14- 25 E12.5 cW/m2/nm Flux [-5.7e-16/8.5e-16] Observed flux;
in erg/s/cm2/Å units
27- 37 E11.5 cW/m2/nm e_Flux [1.8e-19/4e-17]? Uncertainty in Flux
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Note (1): Observational detail of spectra from Table 2:
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Date Δt Tel+Inst. Exp Time Vph
(MJD) (d) (s) (104km/s)
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1 = 58247.359 14 P60+SEDM 1800 2.12±0.46
2 = 58252.322 19 KeckI+LRIS 920 1.74±0.28
3 = 58253.977 20 NOT+ALFOSC 2400 1.84±0.54
4 = 58277.253 44 P200+DBSP 2700 1.12±0.33
5 = 58338.249 105 KeckI+LRIS 1720 N/A
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 08-Sep-2021