J/ApJ/820/33 R-band light curves of type II supernovae (Rubin+, 2016)
Type II supernova energetics and comparison of light curves to shock-cooling
models.
Rubin A., Gal-Yam A., De Cia A., Horesh A., Khazov D., Ofek E.O.,
Kulkarni S.R., Arcavi I., Manulis I., Yaron O., Vreeswijk P.,
Kasliwal M.M., Ben-Ami S., Perley D.A., Cao Y., Cenko S.B.,
Rebbapragada U.D., Wozniak P.R., Filippenko A.V., Clubb K.I., Nugent P.E.,
Pan Y.-C., Badenes C., Howell D.A., Valenti S., Sand D., Sollerman J.,
Johansson J., Leonard D.C., Horst J.C., Armen S.F., Fedrow J.M.,
Quimby R.M., Mazzali P., Pian E., Sternberg A., Matheson T., Sullivan M.,
Maguire K., Lazarevic S.
<Astrophys. J., 820, 33 (2016)>
=2016ApJ...820...33R 2016ApJ...820...33R (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, RI ; Redshifts
Keywords: supernovae: general
Abstract:
During the first few days after explosion, Type II supernovae (SNe)
are dominated by relatively simple physics. Theoretical predictions
regarding early-time SN light curves in the ultraviolet (UV) and
optical bands are thus quite robust. We present, for the first time, a
sample of 57 R-band SN II light curves that are well-monitored during
their rise, with >5 detections during the first 10 days after
discovery, and a well-constrained time of explosion to within 1-3
days. We show that the energy per unit mass (E/M) can be deduced to
roughly a factor of five by comparing early-time optical data to the
2011 model of Rabinak & Waxman, while the progenitor radius cannot be
determined based on R-band data alone. We find that SN II explosion
energies span a range of E/M=(0.2-20)x1051erg/(10M_☉), and have
a mean energy per unit mass of <E/M≥0.85x1051erg/(10M_☉),
corrected for Malmquist bias. Assuming a small spread in progenitor
masses, this indicates a large intrinsic diversity in explosion
energy. Moreover, E/M is positively correlated with the amount of
56Ni produced in the explosion, as predicted by some recent models
of core-collapse SNe. We further present several empirical
correlations. The peak magnitude is correlated with the decline rate
(Δm15), the decline rate is weakly correlated with the rise
time, and the rise time is not significantly correlated with the peak
magnitude. Faster declining SNe are more luminous and have longer rise
times. This limits the possible power sources for such events.
Description:
Our sample consists of 57 SNe from the PTF (Law et al.
2009PASP..121.1395L 2009PASP..121.1395L; Rau et al. 2009PASP..121.1334R 2009PASP..121.1334R) and the
intermediate Palomar Transient Factory (iPTF; Kulkarni
2013ATel.4807....1K 2013ATel.4807....1K) surveys. Data were routinely collected by the
Palomar 48-inch survey telescope in the Mould R-band. Follow-up
observations were conducted mainly with the robotic 60-inch telescope
using an SDSS r-band filter, with additional telescopes providing
supplementary photometry and spectroscopy (see Gal-Yam et al. 2011,
J/ApJ/736/159).
The full list of SNe, their coordinates, and classification spectra
are presented in Table 1. Most of the spectra were obtained with the
Double Spectrograph on the 5m Hale telescope at Palomar Observatory,
the Kast spectrograph on the Shane 3m telescope at Lick Observatory,
the Low Resolution Imaging Spectrometer (LRIS) on the Keck I 10m
telescope, and the DEep Imaging Multi-Object Spectrograph (DEIMOS) on
the Keck II 10m telescope.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 96 57 List of supernovae included in this study
table2.dat 44 7171 Photometry
--------------------------------------------------------------------------------
See also:
II/313 : Palomar Transient Factory (PTF) photometric catalog 1.0 (Ofek+, 2012)
J/ApJ/799/215 : 26 type II-Plateau supernovae parameters (Pejcha+, 2015)
J/ApJ/799/208 : Type IIP supernovae from Pan-STARRS1 (Sanders+, 2015)
J/MNRAS/442/844 : BVRI light curves of type II-P supernovae (Faran+, 2014)
J/MNRAS/438/L101 : First month on SN 2013ej (Valenti+, 2014)
J/other/NewA/20.30 : BVRI light curves of 3 SN (Munari+, 2013)
J/A+A/555/A142 : Spectra of 5 Type II supernovae (Inserra+, 2013)
J/ApJ/736/159 : Photometry monitoring of the SN PTF10vdl (Gal-Yam+, 2011)
J/A+A/537/A141 : UBVRI light curves of SN 2009E (Pastorello+, 2012)
J/ApJ/708/661 : SDSS-II SN Survey: SNe II-P (D'Andrea+, 2010)
J/MNRAS/395/1409 : Type II-P SN progenitor constraints (Smartt+, 2009)
J/MNRAS/394/2266 : SN 2005cs one-year photometry (Pastorello+, 2009)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- SN Supernova identifier (PTFYYaaaa or iPTFYYaaa) (1)
12 A1 --- f_SN [cde] Flag on SN (2)
14- 15 I2 h RAh Hour of Right Ascension (J2000)
17- 18 I2 min RAm Minute of Right Ascension (J2000)
20- 25 F6.3 s RAs Second of Right Ascension (J2000)
27 A1 --- DE- Sign of the Declination (J2000)
28- 29 I2 deg DEd Degree of Declination (J2000)
31- 32 I2 arcmin DEm Arcminute of Declination (J2000)
34- 38 F5.2 arcsec DEs Arcsecond of Declination (J2000)
40- 46 F7.5 --- z [0.002/0.1] Spectroscopic redshift
48- 52 F5.2 mag DM [30.2/38.2] Distance modulus (3)
54- 57 F4.2 mag AR [0.02/0.4] The R band extinction (4)
59- 62 F4.2 mag Ar [0.02/0.4] The r band extinction (4)
64- 73 A10 "Y/M/D" Date UT Date of the observation
75- 88 A14 --- Tel Telescope identifier of the classification
spectrum (5)
90- 96 A7 --- Inst Instrument identifier of the classification
spectrum
--------------------------------------------------------------------------------
Note (1): iPTF13kg in table 1 of the original version is a misprint
for iPTF13akg; corrected at CDS.
Note (2): Flag as follows:
c = The spectrum of this SN has a reddened continuum and Na D
absorption lines; it likely suffers from host-galaxy extinction.
d = The spectrum of this SN has a reddened continuum, but no Na D
absorption lines; it may suffer from host-galaxy extinction.
e = The spectrum of this SN has a blue continuum, but also Na D
absorption lines; it could possibly suffer from host-galaxy extinction.
Note (3): Derived using the lum_dist routine in MATLAB with the
cosmological parameters given in Section 3.
Note (4): Derived using the sky_ebv routine in MATLAB, using RV=3.08.
Note (5): Telescopes are: APO 3.5m, Keck-1, Keck-2, LCOGT, Lick-3m,
Magellan-Baade, Mayall, P200, TNG and WHT-4.2m.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- SN Supernova identifier (PTFYYaaaa or iPTFYYaaa)
11- 19 F9.3 d MJD Modified Julian Date of observation
21- 25 F5.2 mag mag [13.2/22.6]? Observed apparent magnitude in Filt
27- 30 F4.2 mag e_mag [0/0.5]? Error in mag
32- 36 F5.2 mag Limit [17.4/22.7]? Detection limit in Filter
38- 42 A5 --- Tel Telescope (1)
44 A1 --- Filt Filter (R or r)
--------------------------------------------------------------------------------
Note (1): Telescope as follows:
PTF48 = Palomar Transient Factory 48-inch Oschin Schmidt telescope;
PTF60 = Palomar Transient Factory 60-inch telescope;
MLO = Mount Laguna Observatory 40-inch telescope;
LCOGT = Las Cumbres Observatory Global Telescope Network.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-May-2016