J/ApJ/835/58 PTF 12dam & iPTF 13dcc follow-up (Vreeswijk+, 2017)
On the early-time excess emission in hydrogen-poor superluminous supernovae.
Vreeswijk P.M., Leloudas G., Gal-Yam A., De Cia A., Perley D.A.,
Quimby R.M., Waldman R., Sullivan M., Yan L., Ofek E.O., Fremling C.,
Taddia F., Sollerman J., Valenti S., Arcavi I., Howell D.A.,
Filippenko A.V., Cenko S.B., Yaron O., Kasliwal M.M., Cao Y., Ben-Ami S.,
Horesh A., Rubin A., Lunnan R., Nugent P.E., Laher R., Rebbapragada U.D.,
Wozniak P., Kulkarni S.R.
<Astrophys. J., 835, 58-58 (2017)>
=2017ApJ...835...58V 2017ApJ...835...58V (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, UBVRI ; Spectroscopy
Keywords: supernovae: general; supernovae: individual: (PTF 12dam, iPTF 13dcc)
Abstract:
We present the light curves of the hydrogen-poor superluminous
supernovae (SLSNe I) PTF 12dam and iPTF 13dcc, discovered by the
(intermediate) Palomar Transient Factory. Both show excess emission at
early times and a slowly declining light curve at late times. The
early bump in PTF 12dam is very similar in duration (∼10days) and
brightness relative to the main peak (2-3mag fainter) compared to that
observed in other SLSNe I. In contrast, the long-duration (>30days)
early excess emission in iPTF 13dcc, whose brightness competes with
that of the main peak, appears to be of a different nature. We
construct bolometric light curves for both targets, and fit a variety
of light-curve models to both the early bump and main peak in an
attempt to understand the nature of these explosions. Even though the
slope of the late-time decline in the light curves of both SLSNe is
suggestively close to that expected from the radioactive decay of
56Ni and 56Co, the amount of nickel required to power the full
light curves is too large considering the estimated ejecta mass. The
magnetar model including an increasing escape fraction provides a
reasonable description of the PTF 12dam observations. However, neither
the basic nor the double-peaked magnetar model is capable of
reproducing the light curve of iPTF 13dcc. A model combining a shock
breakout in an extended envelope with late-time magnetar energy
injection provides a reasonable fit to the iPTF 13dcc observations.
Finally, we find that the light curves of both PTF 12dam and iPTF
13dcc can be adequately fit with the model involving interaction with
the circumstellar medium.
Description:
Spectroscopic follow-up observations of PTF 12dam were performed with
the Kast Spectrograph at the Lick 3m Shane telescope, and the Low
Resolution Imaging Spectrograph (LRIS) at the Keck-I 10m telescope (on
Mauna Kea, Hawaii) on 2012 May 20, 21, and 22. The full spectroscopic
sequence of PTF 12dam will be presented by R. M. Quimby et al. (2016,
in preparation).
PTF 12dam was imaged with the Palomar Oschin 48 inch (P48) (i)PTF
survey telescope in the Mould R filter, the Palomar 60 inch (P60) and
CCD camera in Johnson B and Sloan Digital Sky Survey (SDSS) gri, the
Las Cumbres Observatory Global Telescope Network (LCOGT) in SDSS r,
and LRIS mounted on the 10m Keck-I telescope in Rs.
iPTF 13dcc has not had any exposure in the literature yet. It was
flagged as a transient source on 2013 August 29. Spectroscopic
follow-up observations spanning 2013 Nov 26 to 2014 Jan 16 were
performed with the Double Spectrograph (DBSP) at the Palomar 200 inch
(P200), LRIS at Keck-I, and the Inamori-Magellan Areal Camera &
Spectrograph (IMACS) at the Magellan Baade telescope, showing iPTF
13dcc to be an SLSN at z=0.4305.
iPTF 13dcc was imaged with the P48 Oschin (i)PTF survey telescope in
the Mould R filter, the P60 in SDSS gri, the 4.3m Discovery Channel
Telescope (DCT, at Lowell Observatory, Arizona) with the Large
Monolithic Imager (LMI) in SDSS ri, and finally with the Hubble Space
Telescope (HST) Advanced Camera for Surveys (ACS) Wide-Field Camera
using filter F625W (under program GO-13858; P.I. A. De Cia).
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
14 24 46.20 +46 13 48.3 PTF 12dam = PTF 12dam
02 57 02.50 -00 18 44.0 iPTF 13dcc = iPTF 13dcc
----------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table10.dat 37 271 Log of observations of PTF 12dam
table11.dat 36 181 Log of observations of iPTF 13dcc
fig5.dat 34 24156 Time series of spectra of iPTF13dcc
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/ApJ/690/1358 : Spectra of unusual optical transient SCP 06F6 (Barbary+, 2009)
J/ApJ/696/870 : Catalina Real-time Transient Survey (CRTS) (Drake+, 2009)
J/ApJ/788/154 : Palomar Transient Factory SNe IIn photometry (Ofek+, 2014)
J/ApJ/795/142 : Defining photometric peculiar SNe Ia (Gonzalez-Gaitan+, 2014)
J/ApJ/830/13 : Host-galaxy NUV-NIR data of superluminous SNe (Perley+, 2016)
Byte-by-byte Description of file: table10.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.2 d MJD Modified Julian Date of the observation
10- 15 F6.2 d Phase Supernova rest-frame phase (1)
17- 22 A6 --- Tel Telescope used in the observation (P60, P48,
LCOGT or Keck 1;
see the section "Description" above)
24 A1 --- Filt [BRgri] Filter used in the observation (BRgri)
26 A1 --- l_mag Limit flag on mag
28- 32 F5.2 mag mag [16.7/22.5] Apparent AB magnitude in Filt (2)
34- 37 F4.2 mag e_mag [0.01/0.4]? Uncertainty in mag
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Note (1): Calculated using MJDr,peak=56096.7 and z=0.107.
Note (2): The magnitudes have not been corrected for Galactic extinction.
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.2 d MJD Modified Julian Date of the observation
10- 15 F6.2 d Phase Supernova rest-frame phase (1)
17- 19 A3 --- Tel Telescope used in the observation (P48, P60, DCT
or HST; see the section "Description" above)
21- 25 A5 --- Filt Filter used in the observation (Rgri and F625W)
27- 31 F5.2 mag mag [19/25] Apparent AB magnitude in Filt (2)
33- 36 F4.2 mag e_mag [0.03/0.3]? Uncertainty in mag
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Note (1): Calculated using MJDr,peak=56618.3 and z=0.431.
Note (2): The magnitudes have not been corrected for Galactic extinction.
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Byte-by-byte Description of file: fig5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "Y/M/D" Date UT date of the observation
12- 16 A5 --- Inst Instrument used in the observation (1)
18- 24 F7.2 0.1nm lambda [3250/10000] Wavelength in Angstroms
26- 34 E9.2 cW/m2/nm Flux Observed flux density; erg/s/cm2/Angstroms (2)
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Note (1): Instrument as follows:
DBSP = Double Spectrograph (DBSP) at the Palomar 200 inch (8219 measures;
coverage: 3400-10400Å) on 2013 Nov 26 (resolution 9.3Å) and
2014 Jan 6 (resolution 8.5Å)
IMACS = Inamori-Magellan Areal Camera & Spectrograph (IMACS) at the
Magellan Baade telescope (3365 measures; coverage: 3700-9700Å)
on 2013 Dec 31 (resolution 6.1Å)
LRIS = Low Resolution Imaging Spectrograph (LRIS) at the Keck-I 10m
telescope (12572 measures; coverage: 3140-10240Å) on
2013 Dec 3 (resolution: 6Å) and 2013 Dec 4 (resolution 5.8Å).
See Table 1 for the full observational details for these spectra.
Note (2): The spectra were corrected for Galactic extinction (Schlafly &
Finkbeiner 2011ApJ...737..103S 2011ApJ...737..103S) and scaled to the polynomial
fit to the r-band photometry depicted in Figure 4 to ensure a
proper absolute calibration.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-Aug-2017