J/ApJ/938/19 Optical phot. and sp. monitoring of SN 2019esa (Andrews+, 2022)
High-cadence TESS and ground-based data of SN 2019esa, the less energetic
sibling of SN 2006gy.
Andrews J.E., Pearson J., Lundquist M.J., Sand D.J., Jencson J.E.,
Bostroem K.A., Hosseinzadeh G., Valenti S., Smith N., Amaro R.C., Dong Y.,
Janzen D., Meza N., Wyatt S., Burke J., Hiramatsu D., Howell D.A.,
McCully C., Pellegrino C.
<Astrophys. J., 938, 19 (2022)>
=2022ApJ...938...19A 2022ApJ...938...19A
ADC_Keywords: Supernovae; Photometry; Spectra, optical
Keywords: Supernovae ; Massive stars ; Circumstellar matter ; Stellar mass loss
Abstract:
We present photometric and spectroscopic observations of the nearby
(D∼28Mpc) interacting supernova (SN) 2019esa, discovered within hours
of explosion and serendipitously observed by the Transiting Exoplanet
Survey Satellite (TESS). Early, high-cadence light curves from both
TESS and the DLT40 survey tightly constrain the time of explosion, and
show a 30 day rise to maximum light followed by a near-constant linear
decline in luminosity. Optical spectroscopy over the first 40 days
revealed a reddened object with narrow Balmer emission lines seen in
Type IIn SNe. The slow rise to maximum in the optical light curve
combined with the lack of broad Hα emission suggest the presence
of very optically thick and close circumstellar material (CSM) that
quickly decelerated the SN ejecta. This CSM was likely created from a
massive star progenitor with an dM/dt∼0.2M☉/yr lost in a
previous eruptive episode 3-4yr before eruption, similar to giant
eruptions of luminous blue variable stars. At late times, strong
intermediate-width CaII, FeI, and FeII lines are seen in the optical
spectra, identical to those seen in the superluminous interacting SN
2006gy. The strong CSM interaction masks the underlying explosion
mechanism in SN 2019esa, but the combination of the luminosity,
strength of the Hα lines, and mass-loss rate of the progenitor
seem to be inconsistent with a Type Ia CSM model and instead point to
a core-collapse origin.
Description:
Continuous photometric monitoring of SN 2019esa was done by the two
discovery telescopes of the DLT40 survey, the PROMPT5 0.4m telescope
at Cerro Tololo International Observatory (CTIO), and the PROMPT-MO
0.4m telescope at Meckering Observatory in Australia, operated by the
Skynet telescope network. The PROMPT5 telescope has no filter ("Open")
while the PROMPT-MO telescope has a broadband "Clear" filter, both of
which we calibrate to the Sloan Digital Sky Survey r band.
The last nondetection from DLT40 was two days before discovery, on
2019-May-04 (JD2458607.58), or 31hr before the estimated explosion to
a limiting magnitude of 19.2, and the first DLT40 detection was
roughly 17hr after explosion.
A high-cadence photometric campaign by the Las Cumbres Observatory
(LCO) telescope network began immediately after discovery, in the
UBVgri bands with the Sinistro cameras on the 1m telescopes, through
the Global Supernova Project. UBV-band data were calibrated to Vega
magnitudes. gri-band data were calibrated to AB magnitudes using the
Sloan Digital Sky Survey.
SN 2019esa was also observed by TESS during Sector 11, 12, and 13
operations of the mission, from 2019-Apr-23 07:02:56.026 to
2019-Jul-17 20:01:19.027 UTC. The TESS light curve of SN 2019esa was
previously published in Vallely+ (2021MNRAS.500.5639V 2021MNRAS.500.5639V), and we present
it here as well. See Section 2.1.
The majority of optical spectra were taken with the robotic FLOYDS
spectrograph on the 2m Faulkes Telescope South in Siding Springs,
Australia, through the Global Supernova Project.
One late-time spectrum (2020-Nov-26) was obtained with the Low
Dispersion Survey Spectrograph 3 (LDSS-3) on the 6.5m Magellan Clay
telescope at Las Campanas Observatory in Chile.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
07 55 00.88 -76 24 43.1 SN 2019esa = DLT 19c
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
fig2.dat 25 546 Optical photometry of SN 2019esa
table1.dat 47 9 Optical spectroscopy of SN 2019esa
fig4.dat 30 30357 Optical spectroscopic evolution of SN 2019esa
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See also:
J/A+A/419/215 : em. lines of strontium filament near eta Car (Hartman+, 2004)
J/ApJ/756/173 : Phot. of type IIn SNe 2005ip and 2006jd (Stritzinger+, 2012)
J/MNRAS/433/1312 : SN2009ip UBVRI, UVOT and JHK light curves (Fraser+, 2013)
J/A+A/555/A10 : Light curves of 5 type IIn supernovae (Taddia+, 2013)
J/ApJ/787/163 : Photometric data for SN 2009ip (Graham+, 2014)
J/MNRAS/438/L101 : First month on SN 2013ej (Valenti+, 2014)
J/MNRAS/446/3895 : The rising light curves of Type Ia supernovae (Firth+, 2015)
J/MNRAS/449/1876 : Photometric observations of SN PTF11iqb (Smith+, 2015)
J/AJ/152/50 : Cosmicflows-3 catalog (CF3) (Tully+, 2016)
J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)
J/AJ/154/211 : The CSP (DR3): photometry of low-z SNe Ia (Krisciunas+, 2017)
J/ApJ/853/62 : Optical & NIR spectra and LCs of SN2016ija (Tartaglia+, 2018)
J/A+A/630/A75 : Six luminous red novae photometry (Pastorello+, 2019)
J/MNRAS/483/628 : SNIa properties using bolometric light curves (Scalzo+, 2019)
J/A+A/637/A73 : Type IIn supernova photometry (Nyholm+, 2020)
J/A+A/635/A39 : Photometry of SN 2015da (Tartaglia+, 2020)
J/A+A/637/A20 : AT 2019abn: multi-wavelength observations (Williams+, 2020)
Byte-by-byte Description of file: fig2.dat
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Bytes Format Units Label Explanations
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1- 9 F9.3 d MJD [58609.15/59003.45] Modified Julian Date
11- 12 A2 --- Filt Filter (UBV, r, gp,rp,ip) (1)
14- 19 F6.3 mag mag [14.26/20.3] Apparent magnitude in Filt
21- 25 F5.3 mag e_mag [0.01/0.1] Uncertainty in mag
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Note (1): The r band data is from the DLT40 survey telescopes. The other
data was obtained the Las 187 Cumbres Observatory telescope network.
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "Y/M/D" Date Observation date (UT)
12- 19 F8.2 d MJD [58609.38/59180.3] Modified Julian Date
21- 23 I3 d Phase [1/572] Days after explosion
(MJD58608.44, 2019 May 5.94)
25- 38 A14 --- Tel Telescope and Instrument
40- 42 I3 --- R [400/750] Resolution (λ/Δλ)
44- 47 I4 s Exp [1500/3600] Exposure time
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Byte-by-byte Description of file: fig4.dat
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Bytes Format Units Label Explanations
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1 A1 --- Obs [AB] Observation code (1)
3- 12 A10 "Y/M/D" Date Observation date (UT)
14- 20 F7.1 0.1nm lambda [3499.1/10000.5] Wavelength; Angstroms
22- 30 E9.2 mW/m2 Flux [-3.5e-16/1.7e-14] Flux density (2)
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Note (1): Observation code as follows:
A = FTS+FLOYDS
B = Magellan+LDSS3
Note (2): The FTS spectra are calibrated to the photometry. The Magellan
spectrum is not as there is no photometry at this epoch.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Aug-2024