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J/MNRAS/410/585     SN 2009dc BVRI light curves              (Silverman+, 2011)

Fourteen months of observations of the possible super-Chandrasekhar mass type Ia supernova 2009dc. Silverman J.M., Ganeshalingam M., Li W., Filippenko A.V., Miller A.A., Poznanski D. <Mon. Not. R. Astron. Soc., 410, 585-611 (2011)> =2011MNRAS.410..585S
ADC_Keywords: Supernovae ; Photometry Keywords: supernovae: general - supernovae: individual: SN 2009dc - supernovae: individual: SN 2007if - supernovae: individual: SN 2003fg - supernovae: individual: SN 2006gz Abstract: In this paper, we present and analyse optical photometry and spectra of the extremely luminous and slowly evolving Type Ia supernova (SN Ia) 2009dc, and offer evidence that it is a super-Chandrasekhar mass (SC) SN Ia and thus has a SC white dwarf (WD) progenitor. Optical spectra of SN 2007if, a similar object, are also shown. SN 2009dc had one of the most slowly evolving light curves ever observed for a SN Ia, with a rise time of ∼23d and {DELTA}m15(B)=0.72mag. We calculate a lower limit to the peak bolometric luminosity of ∼2.4x1043erg/s, though the actual value is likely almost 40 per cent larger. Optical spectra of SN 2009dc and SN 2007if obtained near maximum brightness exhibit strong CII features (indicative of a significant amount of unburned material), and the post-maximum spectra are dominated by iron-group elements (IGEs). All of our spectra of SN 2009dc and SN 2007if also show low expansion velocities. However, we see no strong evidence in SN 2009dc for a velocity `plateau' near maximum light like the one seen in SN 2007if. The high luminosity and low expansion velocities of SN 2009dc lead us to derive a possible WD progenitor mass of more than 2M and a 56Ni mass of about 1.4-1.7M. Description: Observations of SN 2009dc began on 2009 Apr. 17, about one week before maximum B-band brightness, in BVRI filters using the 0.76-m Katzman Automatic Imaging Telescope (KAIT) and the 1-m Nickel telescope, both at Lick Observatory. We continued to follow SN 2009dc for over 5 months until 2009 Sept. 26, when it reached the western limit of both telescopes in the early evening. We obtained late-time gVRI images of SN 2009dc using the dual-arm Low-Resolution Imaging Spectrometer (LRIS) with the 10-m Keck I telescope on 2010 Feb. 6 (281d past maximum), BRI images using the DEIMOS spectrograph (Faber et al. 2003) mounted on the 10-m Keck II telescope on 2010 Jun. 12 (403d past maximum) and V-band images again using LRIS on 2010 Jun. 13. Our optical photometry is complemented with data taken from the UltraViolet Optical Telescope (UVOT) on the Swift Observatory in the U, B, V, UVW1, UVM2 and UVW2 filters. We downloaded seven epochs of observations from the Swift archives. Objects: ---------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------- 15 51 12.1 +25 42 28 SN 2009dc = SN 2009dc ---------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 65 66 Early-time BVRI photometry of SN 2009dc table4.dat 28 34 UVOT (aboard Swift) photometry of SN 2009dc
See also: B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 10 F10.2 d JD Julian date 12- 17 F6.3 mag Bmag ?=- Johnson B magnitude 19- 22 F4.3 mag e_Bmag ?=- rms uncertainty on Bmag 24- 29 F6.3 mag Vmag ?=- Johnson V magnitude 31- 34 F4.3 mag e_Vmag ?=- rms uncertainty on Vmag 36- 41 F6.3 mag Rcmag ?=- Cousins R magnitude 43- 46 F4.3 mag e_Rcmag ?=- rms uncertainty on Rcmag 48- 53 F6.3 mag Icmag ?=- Cousins I magnitude 55- 58 F4.3 mag e_Icmag ?=- rms uncertainty on Icmag 60- 65 A6 --- Tel Telescope used
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 10 F10.2 d JD Julian date 12- 15 A4 --- Filt [UVM2 UVW1 UVW2 UBV] Filter (1) 17- 22 F6.3 mag mag Magnitude in Filter 24- 28 F5.3 mag e_mag rms uncertainty on mag
Note (1): UBV in Johnson-Cousins system; the UV filters central wavelength (c) and FWHM (w) are, in nm (see Poole et al. 2008MNRAS.383..627P): ----------------- (F) (c) (w) ----------------- UVW1 260.0 69.3 UVM2 224.6 49.8 UVW2 192.8 65.7 -----------------
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Aug-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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