J/MNRAS/433/1312 SN2009ip UBVRI, UVOT and JHK light curves (Fraser+, 2013)
SN 2009ip a la PESSTO: no evidence for core collapse yet.
Fraser M., Inserra C., Jerkstrand A., Kotak R., Pignata G., Benetti S.,
Botticella M.-T., Bufano F., Childress M., Mattila S., Pastorello A.,
Smartt S.J., Turatto M., Yuan F., Anderson J.P., Bayliss D.D.R.,
Bauer F.E., Chen T.-W., Forster Buron F., Gal-yam A., Haislip J.B.,
Knapic C., Le Guillou L., Marchi S., Mazzali P., Molinaro M., Moore J.P.,
Reichart D., Smareglia R., Smith K.W., Sternberg A., Sullivan M.,
Takats K., Tucker B.E., Valenti S., Yaron O., Young D.R., Zhou G.
<Mon. Not. R. Astron. Soc., 433, 1312-1337 (2013)>
=2013MNRAS.433.1312F 2013MNRAS.433.1312F
ADC_Keywords: Supernovae ; Photometry, UBVRI ; Photometry, infrared ;
Photometry, ultraviolet
Keywords: stars: massive - stars: mass-loss - supernovae: general -
supernovae: individual: SN 2009ip
Abstract:
We present ultraviolet, optical and near-infrared observations of the
interacting transient SN 2009ip, covering the period from the start of
the outburst in 2012 October until the end of the 2012 observing
season. The transient reached a peak magnitude of MV=-17.7mag, with
a total integrated luminosity of 1.9x1049erg over the period of 2012
August-December. The light curve fades rapidly, dropping by 4.5mag
from the V-band peak in 100d. The optical and near-infrared spectra
are dominated by narrow emission lines with broad electron scattering
wings, signalling a dense circumstellar environment, together with
multiple components of broad emission and absorption in H and He at
velocities in the range 0.5-1.2x104km/s. We see no evidence for
nucleosynthesized material in SN 2009ip, even in late-time
pseudo-nebular spectra. We set a limit of <0.02M☉ on the mass of
any possible synthesized 56Ni from the late-time light curve. A simple
model for the narrow Balmer lines is presented and used to derive
number densities for the circumstellar medium in the range
∼109-1010cm-3. Our near-infrared data do not show any excess at
longer wavelengths, and we see no other signs of dust formation. Our
last data, taken in 2012 December, show that SN 2009ip has
spectroscopically evolved to something quite similar to its appearance
in late 2009, albeit with higher velocities. It is possible that
neither of the eruptive and high-luminosity events of SN 2009ip were
induced by a core collapse. We show that the peak and total integrated
luminosity can be due to the efficient conversion of kinetic energy
from colliding ejecta, and that around 0.05-0.1M☉ of material
moving at 0.5-1x104km/s could comfortably produce the observed
luminosity. We discuss the possibility that these shells were ejected
by the pulsational pair instability mechanism, in which case the
progenitor star may still exist, and will be observed after the
current outburst fades. The long-term monitoring of SN 2009ip, due to
its proximity, has given the most extensive data set yet gathered of a
high-luminosity interacting transient and its progenitor. It is
possible that some purported Type IIn supernovae are in fact analogues
of the 2012b event and that pre-explosion outbursts have gone
undetected.
Description:
Optical spectroscopic follow-up of SN 2009ip was chiefly obtained with
the New Technology Telescope (NTT) + ESO Faint Object Spectrograph and
Camera 2 (EFOSC2), as part of the Public European Southern Observatory
(ESO) Spectroscopic Survey of Transient Objects (PESSTO). The PESSTO
data were supplemented with data from the Telescopio Nazionale Galileo
(TNG) + Device Optimized for the LOw RESolution (DOLORES), and the
Australian National University (ANU) 2.3m telescope + Wide Field
Spectrograph (WiFeS).
Objects:
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RA (2000) DE Designation(s)
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22 23 08.26 -28 56 52.4 SN 2009ip = SN 2009ip
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 84 78 Optical UBVRI photometry of SN 2009ip
in the Landolt system
tableb2.dat 52 33 UV photometry of SN 2009ip from Swift+UVOT
tableb3.dat 60 11 NIR photometry of SN 2009ip in the 2MASS system
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "date" Date Observation date
12- 19 F8.2 d MJD Modified Julian date
21- 26 F6.3 mag Umag ?=- Landolt U magnitude
28- 31 F4.2 mag e_Umag ? rms uncertainty on Umag
34 A1 --- l_Bmag Limit flag on Bmag
35- 39 F5.2 mag Bmag ?=- Landolt B magnitude
41- 44 F4.2 mag e_Bmag ? rms uncertainty on Bmag
46- 50 F5.2 mag Vmag ?=- Landolt V magnitude
52- 55 F4.2 mag e_Vmag ? rms uncertainty on Vmag
57- 61 F5.2 mag Rmag ?=- Landolt R magnitude
63- 66 F4.2 mag e_Rmag ? rms uncertainty on Rmag
68- 72 F5.2 mag Imag ?=- Landolt I magnitude
74- 77 F4.2 mag e_Imag ? rms uncertainty on Imag
79- 84 A6 --- Inst Instrument
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "date" Date Observation date
12- 19 F8.2 d MJD Modified Julian date
21- 25 F5.2 mag UVW2 ?=- UVOT UVW2 magnitude
27- 30 F4.2 mag e_UVW2 ? rms uncertainty on UVW2
32- 36 F5.2 mag UVM2 ?=- UVOT UVM2 magnitude
38- 41 F4.2 mag e_UVM2 ? rms uncertainty on UVM2
43- 47 F5.2 mag UVW1 ?=- UVOT UVW1 magnitude
49- 52 F4.2 mag e_UVW1 ? rms uncertainty on UVW1
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Byte-by-byte Description of file: tableb3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "date" Date Observation date
12- 19 F8.2 d MJD Modified Julian date
21- 25 F5.2 mag Jmag ?=- 2MASS J magnitude
27- 30 F4.2 mag e_Jmag ? rms uncertainty on Jmag
32- 36 F5.2 mag Hmag ?=- 2MASS H magnitude
38- 41 F4.2 mag e_Hmag ? rms uncertainty on Hmag
43- 47 F5.2 mag Kmag ?=- 2MASS Ks magnitude
49- 52 F4.2 mag e_Kmag ? rms uncertainty on Kmag
54- 60 A7 --- Inst Instrument
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 17-Nov-2014