J/MNRAS/461/2003 SN 2013ej light curves 1 to 450d after explosion (Yuan+, 2016)
450 d of Type II SN 2013ej in optical and near-infrared.
Yuan F., Jerkstrand A., Valenti S., Sollerman J., Seitenzahl I.R.,
Pastorello A., Schulze S., Chen T.-W., Childress M.J., Fraser M.,
Fremling C., Kotak R., Ruiter A.J., Schmidt B.P., Smartt S.J., Taddia F.,
Terreran G., Tucker B.E., Barbarino C., Benetti S., Elias-Rosa N.,
Gal-Yam A., Howell D.A., Inserra C., Kankare E., Lee M.Y., Li K.L.,
Maguire K., Margheim S., Mehner A., Ochner P., Sullivan M., Tomasella L.,
Young D.R.
<Mon. Not. R. Astron. Soc., 461, 2003-2018 (2016)>
=2016MNRAS.461.2003Y 2016MNRAS.461.2003Y (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, UBVRI ; Photometry, infrared ;
Photometry, SDSS
Keywords: supernovae: general - supernovae: individual: SN 2013ej
Abstract:
We present optical and near-infrared photometric and spectroscopic
observations of SN 2013ej, in galaxy M74, from 1 to 450 d after the
explosion. SN 2013ej is a hydrogen-rich supernova, classified as a
Type IIL due to its relatively fast decline following the initial
peak. It has a relatively high peak luminosity (absolute magnitude
MV=-17.6) but a small 56Ni production of ∼0.023M☉. Its
photospheric evolution is similar to other Type II SNe, with shallow
absorption in the Hα profile typical for a Type IIL. During
transition to the radioactive decay tail at ∼100d, we find the SN to
grow bluer in B-V colour, in contrast to some other Type II
supernovae. At late times, the bolometric light curve declined faster
than expected from 56Co decay and we observed unusually broad and
asymmetric nebular emission lines. Based on comparison of nebular
emission lines most sensitive to the progenitor core mass, we find our
observations are best matched to synthesized spectral models with a
MZAMS=12-15 M☉ progenitor. The derived mass range is similar
to but not higher than the mass estimated for Type IIP progenitors.
This is against the idea that Type IIL are from more massive stars.
Observations are consistent with the SN having a progenitor with a
relatively low-mass envelope.
Description:
The LCOGT network started an extensive monitoring campaign of SN
2013ej a few days after its discovery (Valenti et al., 2014, Cat.
(J/MNRAS/438/L101). Multiband (UBVRIgriz) photometric observations
were carried out with nine 1-m telescopes.
Objects:
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RA (2000) DE Designation(s)
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01 36 48.16 +15 45 31.0 SN 2013ej = PSN J01364816+1545310
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 43 722 Optical and NIR photometric observations of
SN 2013ej
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See also:
J/MNRAS/438/L101 : First month on SN 2013ej (Valenti+, 2014)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "date" Obs.Date UT observation date
12- 20 F9.3 d JD Julian date (JD-2400000)
22- 26 F5.2 mag mag Magnitude in Filter
28- 31 F4.2 mag e_mag rms uncertainty on mag
33- 34 A2 --- Filt Filter (1)
36- 43 A8 --- Tel Telescope/Instrument (2)
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Note (1): Filtesr are UBVRIJHKs and ugriz.
Note (2): Optical telescopes and instruments as follows:
1m008 = LCOGT 1m at Mc-Donald observatory, USA
1m010 = LCOGT 1m at Sutherland, South Africa
1m012 = LCOGT 1m at Sutherland, South Africa
1m013 = LCOGT 1m at Sutherland, South Africa
1m004 = LCOGT 1m at Cerro Tololo, Cile
1m005 = LCOGT 1m at Cerro Tololo, Cile
1m009 = LCOGT 1m at Cerro Tololo, Cile
1m003 = LCOGT 1m at Siding Spring, Australia
1m011 = LCOGT 1m at Siding Spring, Australia
LOT = 1m at the Lulin Observatory in Taiwan
AFOSC = INAF 1.82 m + AFOSC
SBIG = INAF Schmidt 67/92 cm + SBIG
NTT = NTT + EFOSC2
VLT = X-shooter Acquisition and Guiding camera
See Section 2 for further details.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 27-Nov-2017