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 (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:
FileName Lrecl Records Explanations
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
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
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
Note (1): Calculated using MJDr,peak=56096.7 and z=0.107. Note (2): The magnitudes have not been corrected for Galactic extinction.
Byte-by-byte Description of file: table11.dat
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
Note (1): Calculated using MJDr,peak=56618.3 and z=0.431. Note (2): The magnitudes have not been corrected for Galactic extinction.
Byte-by-byte Description of file: fig5.dat
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)
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) and scaled to the polynomial fit to the r-band photometry depicted in Figure 4 to ensure a proper absolute calibration.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-Aug-2017
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