J/MNRAS/448/2608 UV and optical photometric data for SN 2013by (Valenti+, 2015)
Supernova 2013by: a Type IIL supernova with a IIP-like light-curve drop.
Valenti S., Sand D., Stritzinger M., Howell D.A., Arcavi I., McCully C.,
Childress M.J., Hsiao E.Y., Contreras C., Morrell N., Phillips M.M.,
Gromadzki M., Kirshner R.P., Marion G.H.
<Mon. Not. R. Astron. Soc., 448, 2608-2616 (2015)>
=2015MNRAS.448.2608V 2015MNRAS.448.2608V (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, ultraviolet ; Photometry, UBV ;
Photometry, ugriz
Keywords: supernovae: general - supernovae: individual: SN 2013by
Abstract:
We present multiband ultraviolet and optical light curves, as well as
visual-wavelength and near-infrared spectroscopy of the Type II linear
(IIL) supernova (SN) 2013by. We show that SN 2013by and other SNe IIL
in the literature, after their linear decline phase that start after
maximum, have a sharp light-curve decline similar to that seen in SNe IIP.
This light-curve feature has rarely been observed in other SNe IIL due
to their relative rarity and the intrinsic faintness of this
particular phase of the light curve. We suggest that the presence of
this drop could be used as a physical parameter to distinguish between
subclasses of SNe II, rather than their light-curve decline rate
shortly after peak. Close inspection of the spectra of SN 2013by
indicate asymmetric line profiles and signatures of high-velocity
hydrogen. Late (∼90d after explosion) near-infrared spectra of SN 2013by
exhibit oxygen lines, indicating significant mixing within the ejecta.
From the late-time light curve, we estimate that 0.029 M☉ of 56Ni
was synthesized during the explosion. It is also shown that the V-band
light-curve slope is responsible for part of the scatter in the luminosity
(V magnitude 50d after explosion) versus 56Ni relation. Our observations
of SN 2013by and other SNe IIL through the onset of the nebular phase
indicate that their progenitors are similar to those of SNe IIP.
Description:
Photometric monitoring in BVgri of SN 2013by with the LCOGT 1 m
telescope network began on 2013 April 24 (UT), and continued every two
to three nights (52 epochs of data were collected) for more than
150 d, well after the light curve settled on to the 56Co decay tail.
Additional imaging was obtained from Swift and the CSP. The CSP
obtained 17 epochs of science images using the SITe3 CCD camera along
with a set of ugriBV filters attached to the Swope 1 m telescope
located at Las Campanas Observatory (LCO).
Objects:
---------------------------------------------------------------
RA (ICRS) DE Designation(s)
---------------------------------------------------------------
16 59 02.43 -60 11 41.8 SN 2013by = PSN J16590243-6011418
---------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea2.dat 46 394 Photometric data
--------------------------------------------------------------------------------
See also:
II/339 : Swift/UVOT Serendipitous Source Catalog (Yershov, 2015)
J/MNRAS/442/844 : Type II-P supernovae BVRI light curves (Faran+, 2014)
J/ApJ/799/208 : Type IIP supernovae from Pan-STARRS1 (Sanders+, 2015)
Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "date" Date Date of the observation
12- 22 F11.3 d JD Julian Date
24- 29 F6.3 mag mag Magnitude in Filter (1)
31- 35 F5.3 mag e_mag Uncertainty in mag
37- 39 A3 --- Filter Filter (2)
41- 46 A6 --- Tel Telescope identifier (3)
--------------------------------------------------------------------------------
Note (1): Data have not been corrected for extinction.
Note (2): Filter are: UBV, ugri, um2, uw1 and uw2.
Note (3): Telescope as follows:
Swift = Swift telescope;
CSP = Las Campanas, Chile;
1m0-08 = McDonald observatory, USA;
1m0-10, 1m0-12, 1m0-13 = Sutherland, South Africa;
1m0-04, 1m0-05, 1m0-09 = Cerro Tololo, Chile;
1m0-03, 1m0-11 = Siding Spring, Australia.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 22-Nov-2017