J/AJ/144/131 Photometry and spectroscopy of SN 2010jl (Zhang+, 2012)
Type IIn supernova SN 2010jl: optical observations for over 500 days after
explosion.
Zhang T., Wang X., Wu C., Chen J., Chen J., Liu Q., Huang F., Liang J.,
Zhao X., Lin L., Wang M., Dennefeld M., Zhang J., Zhai M., Wu H., Fan Z.,
Zou H., Zhou X., Ma J.
<Astron. J., 144, 131 (2012)>
=2012AJ....144..131Z 2012AJ....144..131Z
ADC_Keywords: Supernovae ; Photometry, UBVRI ; Equivalent widths ; Mass loss ;
Spectroscopy
Keywords: supernovae: general - supernovae: individual (SN 2010jl)
Abstract:
We present extensive optical observations of a Type IIn supernova (SN
IIn) 2010jl for the first 1.5years after its discovery. The UBVRI
light curves demonstrated an interesting two-stage evolution during
the nebular phase, which almost flatten out after about 90days from
the optical maximum. SN 2010jl has one of the highest intrinsic
Hα luminosities ever recorded for an SN IIn, especially at late
phase, suggesting a strong interaction of SN ejecta with the dense
circumstellar material (CSM) ejected by the progenitor. This is also
indicated by the remarkably strong Balmer lines persisting in the
optical spectra. One interesting spectral evolution about SN 2010jl is
the appearance of asymmetry of the Balmer lines. These lines can be
well decomposed into a narrow component and an intermediate-width
component. The intermediate-width component showed a steady increase
in both strength and blueshift with time until t∼400days after
maximum, but it became less blueshifted at t∼500days, when the line
profile appeared relatively symmetric again. Owing to the fact that a
pure reddening effect will lead to a sudden decline of the light
curves and a progressive blueshift of the spectral lines, we therefore
propose that the asymmetric profiles of H lines seen in SN 2010jl are
unlikely due to the extinction by newly formed dust inside the ejecta,
contrary to the explanation by some early studies. Based on a simple
CSM-interaction model, we speculate that the progenitor of SN 2010jl
may suffer a gigantic mass loss (∼30-50M☉) a few decades before
explosion. Considering a slow-moving stellar wind (e.g.,∼28km/s)
inferred for the preexisting, dense CSM shell and the extremely high
mass-loss rate (1-2M☉/yr), we suggest that the progenitor of SN
2010jl might have experienced a red supergiant stage and may explode
finally as a post-red supergiant star with an initial mass above
30-40M☉.
Description:
The photometry of SN 2010jl was obtained by the 0.8m Tsinghua-NAOC
reflecting Telescope (TNT; this telescope is co-operated by Tsinghua
University and the National Astronomical Observatories of China, NAOC)
located at NAOC Xinglong Observatory. This telescope is equipped with
a CCD. Our observation of SN 2010jl started on 2010 November 8, about
6 days after the discovery, and extended out to about 500 days after
that. The aperture photometry was performed to obtain the instrumental
magnitudes of the SN. We transform the instrumental magnitudes to the
standard Johnson UBV and Kron-Cousins RI systems.
Low-resolution optical spectra of SN 2010jl were obtained with the
Cassegrain spectrograph and BAO Faint Object Spectrograph & Camera
(BFOSC) mounted on the 2.16m telescope at NAOC Xinglong Observatory.
Two late-time spectra taken at 86 days and 392 days after maximum
light were, respectively, obtained with the Carelec spectrograph on
the 1.93m telescope at Haute-Provence Observatory (OHP) France and the
Yunnan Astronomical Observatory Faint Object Spectrograph & Camera
(YFOSC) on the 2.4m telescope at Lijiang Observatory. A journal of
spectroscopic observations is listed below:
UT Date | JD | Phase | Range |Resolution| Instrument
|-2450000 |(in days)|(in Å)|(in Å) |
|(in days)| (a) | | (b) |
---------------------------------------------------------------------------
2010 Nov 11| 5512.4 | 24.4 |3500-8500| 4 | BAO 2.16 m Cassegrain
2010 Nov 27| 5528.4 | 40.4 |3000-9000| 3-5 | BAO 2.16 m BFOSC
2010 Dec 2 | 5533.4 | 45.4 |3500-7800| 4 | BAO 2.16 m Cassegrain
2011 Jan 10| 5572.4 | 84.4 |3500-8200| 4 | BAO 2.16 m Cassegrain
2011 Jan 12| 5574.1 | 86.1 |3600-7300| 7 | OHP 1.93 m Carelec
2011 Feb 11| 5604.1 | 116.1 |3600-8800| 4 | BAO 2.16 m Cassegrain
2011 Mar 25| 5646.1 | 158.1 |3600-8800| 4 | BAO 2.16 m Cassegrain
2011 Apr 04| 5656.1 | 168.1 |5500-8000| 2 | BAO 2.16 m Cassegrain
2011 May 13| 5704.0 | 216.0 |4200-8700| 4 | BAO 2.16 m BFOSC
2011 Nov 13| 5880.4 | 392.4 |3800-9000| 3 | YNAO 2.4 m YFOSC
2011 Dec 23| 5919.2 | 431.2 |3800-9000| 4 | BAO 2.16 m Cassegrain
2012 Mar 16| 6003.0 | 515.0 |4300-8700| 4 | BAO 2.16 m Cassegrain
---------------------------------------------------------------------------
a = Relative to the V-band maximum (JD=2455488; Stoll et al.,
2011ApJ...730...34S 2011ApJ...730...34S).
b = Approximate spectral resolution (FWHM intensity).
---------------------------------------------------------------------------
Objects:
----------------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------------
09 42 53.33 +09 29 41.8 SN 2010jl = PTF 10aaxf
----------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 91 51 UBVRI magnitudes of SN 2010jl from
Tsinghua-NAOC reflecting Telescope (TNT)
table4.dat 54 9 Spectroscopic parameters of SN 2010jl
table5.dat 28 9 Some physical properties derived for SN 2010jl
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/A+A/555/A10 : Light curves of 5 type IIn supernovae (Taddia+, 2013)
J/A+A/538/A120 : A unified supernova catalogue (Lennarz+, 2012)
J/A+A/544/A81 : Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)
J/PASP/122/1 : BVRI light curves of SN 2007gi (Zhang+, 2010)
J/AJ/131/2245 : BATC photometry of SN2004dj (Zhang+, 2006)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 "Y:M:D" Date UT date of observation
13- 19 F7.2 d JD Julian Date of observation; JD-2450000
21- 26 F6.2 d Phase Phase relative to the V-band maximum
(JD=2455488; Stoll et al., 2011ApJ...730...34S 2011ApJ...730...34S)
28 A1 --- u_Umag [~] Uncertainty flag on Umag
30- 35 F6.3 mag Umag ? Johnson U-band magnitude
37- 39 I3 mmag e_Umag ? 1σ uncertainty in Umag (1)
41 A1 --- u_Bmag [~] Uncertainty flag on Bmag
43- 48 F6.3 mag Bmag Johnson B-band magnitude
50- 52 I3 mmag e_Bmag ? 1σ uncertainty in Bmag (1)
54 A1 --- u_Vmag [~] Uncertainty flag on Vmag
56- 61 F6.3 mag Vmag Johnson V-band magnitude
63- 65 I3 mmag e_Vmag ? 1σ uncertainty in Vmag (1)
67 A1 --- u_Rmag [~] Uncertainty flag on Rmag
69- 74 F6.3 mag Rmag Kron-Cousins R-band magnitude
76- 78 I3 mmag e_Rmag ? 1σ uncertainty in Rmag (1)
80 A1 --- u_Imag [~] Uncertainty flag on Imag
82- 87 F6.3 mag Imag ? Kron-Cousins I-band magnitude
89- 91 I3 mmag e_Imag ? 1σ uncertainty in Imag (1)
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Note (1): includes both the uncertainty in the calibration of the local
standard stars and the uncertainty of the instrumental magnitudes.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 F5.1 d Phase Phase relative to the V-band maximum
(JD=2455488; Stoll et al., 2011ApJ...730...34S 2011ApJ...730...34S)
7- 11 I5 0.1nm EWHa Hα equivalent width
13- 16 I4 0.1nm EWHb Hβ equivalent width
18- 21 I4 km/s FHa Full Width Half Maximum (FHWM) velocity of
Hα (1)
23- 25 I3 km/s e_FHa Uncertainty in FHa (1)
27- 30 I4 km/s FHb Full Width Half Maximum (FHWM) velocity of
Hβ (1)
32- 34 I3 km/s e_FHb Uncertainty in FHb (1)
36- 39 I4 km/s BHa Hα blueshift (1)
41- 42 I2 km/s e_BHa Uncertainty in BHa (1)
44- 47 I4 km/s BHb Hβ blueshift (1)
49- 50 I2 km/s e_BHb Uncertainty in BHb (1)
52- 54 F3.1 --- Ha/Hb Flux ratio Hα/Hβ
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Note (1): The parameters measured for the intermediate-width component.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 d Ph1 Phase relative to the V-band maximum
(JD=2455488; Stoll et al., 2011ApJ...730...34S 2011ApJ...730...34S)
5- 7 F3.1 10+9Lsun Lbol Bolometric luminosity
9 A1 --- u_T [~] Uncertainty flag on T
10- 13 I4 K T Blackbody temperature
15- 17 F3.1 Msun/yr dM/dt Progenitor mass-loss rate of the circumstellar
material (CSM) shell (2)
19- 21 F3.1 Msun/yr e_dM/dt Uncertainty in dM/dt
23- 28 F6.1 yr tau Timescale of the stellar wind flow (3)
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Note (2): Calculated using the expression (e.g., Wood-Vasey et al.,
2004ApJ...616..339W 2004ApJ...616..339W): dM/dt=2L[vw/(α(vs3))], where
L is the observed bolometric luminosity, and α represents the
conversion term from kinetic energy to optical luminosity. vw is
the velocity of the pre-explosion stellar wind, which is adopted as
-28km/s inferred from an absorption minimum of the narrow component
of Hα (Smith et al., 2011ApJ...732...63S 2011ApJ...732...63S). vs is the velocity
of the post-shock shell, assuming as the FWHM velocity of the
intermediate-width component of Hα lines.
Note (3): Estimated with the mass-loss rate, the timescale of the stellar
wind flow is the number of years prior to explosion when the
progenitor of SN 2010jl had such a mass-loss rate. tau = Rs/vw,
where Rs is the radius of the circumstellar material (CSM) shell
expanding approximately at an average speed of about 2750km/s, and
vw represents the velocity of the pre-explosion stellar wind, which
is adopted as -28km/s inferred from an absorption minimum of the
narrow component of Hα (Smith et al., 2011ApJ...732...63S 2011ApJ...732...63S).
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History:
From electronic version of the journal
(End) Sylvain Guehenneux [CDS] 26-Nov-2013