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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 (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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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