J/MNRAS/437/656 SN PS1-11ap light curves (McCrum+, 2014)
The superluminous supernova PS1-11ap:
bridging the gap between low and high redshift.
McCrum M., Smartt S.J., Kotak R., Rest A., Jerkstrand A., Inserra C.,
Rodney S.A., Chen T.-W., Howell D.A., Huber M.E., Pastorello A.,
Tonry J.L., Bresolin F., Kudritzki R.-P., Chornock R., Berger E., Smith K.,
Botticella M.T., Foley R.J., Fraser M., Milisavljevic D., Nicholl M.,
Riess A.G., Stubbs C.W., Valenti S., Wood-Vasey W.M., Wright D.,
Young D.R., Drout M., Czekala I., Burgett W.S., Chambers K.C., Draper P.,
Flewelling H., Hodapp K.W., Kaiser N., Magnier E.A., Metcalfe N.,
Price P.A., Sweeney W., Wainscoat R.J.
<Mon. Not. R. Astron. Soc., 437, 656-674 (2014)>
=2014MNRAS.437..656M 2014MNRAS.437..656M (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, SDSS
Keywords: supernovae: general - supernovae: individual: PS1-11ap
Abstract:
We present optical photometric and spectroscopic coverage of the
superluminous supernova (SLSN) PS1-11ap, discovered with the
Pan-STARRS1 Medium Deep Survey at z=0.524. This intrinsically blue
transient rose slowly to reach a peak magnitude of Mu=-21.4mag and
bolometric luminosity of 8x1043erg/s before settling on to a
relatively shallow gradient of decline. The observed decline is
significantly slower than those of the SLSNe-Ic which have been the
focus of much recent attention. Spectroscopic similarities with the
lower redshift SN2007bi and a decline rate similar to 56Co decay
time-scale initially indicated that this transient could be a
candidate for a pair instability supernova (PISN) explosion. Overall
the transient appears quite similar to SN2007bi and the lower redshift
object PTF12dam. The extensive data set, from 30d before peak to 230d
after, allows a detailed and quantitative comparison with published
models of PISN explosions. We find that the PS1-11ap data do not match
these model explosion parameters well, supporting the recent claim
that these SNe are not pair instability explosions. We show that
PS1-11ap has many features in common with the faster declining
SLSNe-Ic, and the light-curve evolution can also be quantitatively
explained by the magnetar spin-down model. At a redshift of z=0.524,
the observer-frame optical coverage provides comprehensive rest-frame
UV data and allows us to compare it with the SLSNe recently found at
high redshifts between z=2 and 4. While these high-z explosions are
still plausible PISN candidates, they match the photometric evolution
of PS1-11ap and hence could be counterparts to this lower redshift
transient.
Description:
The PS1 system is a high-etendue wide-field imaging system, designed
for dedicated survey observations. The system is installed on the peak
of Haleakala on the island of Maui in the Hawaiian island chain. The
telescope has a 1.8m diameter primary mirror, and the gigapixel
camera (GPC1) located at the f/4.4 Cassegrain focus consists of sixty
4800x4800-pixel detectors (pixel scale 0.258-arcsec) giving a
field of view of 3.3° diameter.
The PS1 observations are obtained through a set of five broad-band
filters, which are designated as gP1, rP1, iP1, zP1 and yP1.
The PS1 photometric system and its response are covered in detail in
Tonry et al. (2012ApJ...750...99T 2012ApJ...750...99T, Cat. J/ApJ/750/99).
Objects:
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RA (2000) DE Designation(s)
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10 48 27.7 +57 09 09.2 PS1-11ap = PS1-11ap
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 55 240 Observed photometry of PS1-11ap,
without K-corrections.
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See also:
J/ApJ/750/99 : The Pan-STARRS1 photometric system (Tonry+, 2012)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "date" Obs.date Observation date
12- 19 F8.2 d MJD Modified Julian date of observation
21- 23 F3.2 d e_MJD ? rms uncertainty on MJD (1)
26- 31 F6.2 d Phase Phase (days since explosion)
33- 35 F3.2 d e_Phase ? rms uncertainty on Phase (1)
37 A1 --- l_mag Limit flag on mag
38- 42 F5.2 mag mag LT magnitude in Filter (2)
44- 47 F4.2 mag e_mag ? rms uncertainty on mag
49- 51 A3 --- Filt [grizy P1] Filter (3)
53- 55 A3 --- Tel [LT PS1] Telescope
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Note (1): The MJD and phase of any observations from 2011 December onwards
represent the mid-points of the co-added frames, hence the uncertainties given.
Note (2): The LT magnitudes (Filters GRIZ) have been converted to the PS1
system as discussed in Section 2.2.
Note (3): LT filters: g, r, i and z.
PS1 filters: gP1, rP1, iP1, zP1 and yP1.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 10-Mar-2015