J/MNRAS/449/1921 UV/optical/NIR photometry for Type Ibn SNe (Pastorello+, 2015)
Massive stars exploding in a He-rich circumstellar medium - IV. Transitional Type Ibn supernovae. Pastorello A., Benetti S., Brown P.J., Tsvetkov D.Y., Inserra C., Taubenberger S., Tomasella L., Fraser M., Rich D.J., Botticella M.T., Bufano F., Cappellaro E., Ergon M., Gorbovskoy E.S., Harutyunyan A., Huang F., Kotak R., Lipunov V.M., Magill L., Miluzio M., Morrell N., Ochner P., Smartt S.J., Sollerman J., Spiro S., Stritzinger M.D., Turatto M., Valenti S., Wang X., Wright D.E., Yurkov V.V., Zampieri L., Zhang T. <Mon. Not. R. Astron. Soc., 449, 1921-1940 (2015)> =2015MNRAS.449.1921P (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, UBVRI ; Photometry, infrared ; Photometry, ultraviolet Keywords: supernovae: general - supernovae: individual: SN 2010al - supernovae: individual: SN 2011hw - supernovae: individual: SN 2006jc - supernovae: individual: SN 2005la - supernovae: individual: SN 2000er Abstract: We present ultraviolet, optical and near-infrared data of the Type Ibn supernovae (SNe) 2010al and 2011hw. SN 2010al reaches an absolute magnitude at peak of MR=-18.86±0.21. Its early light curve shows similarities with normal SNe Ib, with a rise to maximum slower than most SNe Ibn. The spectra are dominated by a blue continuum at early stages, with narrow P-Cygni HeI lines indicating the presence of a slow-moving, He-rich circumstellar medium. At later epochs, the spectra well match those of the prototypical SN Ibn 2006jc, although the broader lines suggest that a significant amount of He was still present in the stellar envelope at the time of the explosion. SN 2011hw is somewhat different. It was discovered after the first maximum, but the light curve shows a double peak. The absolute magnitude at discovery is similar to that of the second peak (MR=-18.59±0.25), and slightly fainter than the average of SNe Ibn. Though the spectra of SN 2011hw are similar to those of SN 2006jc, coronal lines and narrow Balmer lines are clearly detected. This indicates substantial interaction of the SN ejecta with He-rich, but not H-free, circumstellar material. The spectra of SN 2011hw suggest that it is a transitional SN Ibn/IIn event similar to SN 2005la. While for SN 2010al the spectrophotometric evolution favours a H-deprived Wolf-Rayet progenitor (of WN-type), we agree with the conclusion of Smith et al. that the precursor of SN 2011hw was likely in transition from a luminous blue variable to an early Wolf-Rayet (Ofpe/WN9) stage. Description: We started our optical and near-infrared (NIR) observational campaigns soon after the classification announcements of the two SNe, using the instruments available to our collaboration (see Tables A3 and A4). Additional photometry with small-size telescopes was kindly provided by amateur astronomers. Both SNe 2010al and 2011hw were visible for only 60-70 d after their discoveries, then they disappeared behind the Sun. We tried to recover SN 2010al at very late phases, but it was only visible in NIR observations obtained with the 8.4-m Large Binocular Telescope (Mt. Graham, Arizona; USA) equipped with Lucifer. Additional space observations of SNe 2010al and 2011hw in the ultra-violet (UV) and optical bands were obtained with the Swift satellite and its Ultraviolet/Optical Telescope (UVOT). These data were useful to constrain the large energy contribution of the UV domain in the early phases of the evolution of the two SNe. Objects: --------------------------------------------------------------- RA (ICRS) DE Designation(s) --------------------------------------------------------------- 08 14 15.91 +18 26 18.2 SN 2010al = SN 2010al 22 26 14.54 +34 12 59.1 SN 2011hw = PSN J22261454+3412591 --------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea3.dat 119 54 Calibrated multiband photometry of SN 2010al tablea4.dat 119 33 Calibrated multiband photometry of SN 2011hw tablea5.dat 93 25 Swift/UVOT band photometry of SNe 2010al and SN 2011hw
See also: II/339 : Swift/UVOT Serendipitous Source Catalog (Yershov, 2015) J/AJ/137/4517 : UVOT light curves of supernovae (Brown+, 2009) Byte-by-byte Description of file: tablea3.dat tablea4.dat
Bytes Format Units Label Explanations
1- 11 A11 "date" Date Observation date 12 A1 --- n_Date [*D] Note on Date (1) 14- 20 F7.2 d JD Julian Date (JD-2455000) 22 A1 --- l_Umag [>] Limit flag on Umag 23- 27 F5.2 mag Umag ? U-band magnitude 29- 32 F4.2 mag e_Umag ? Uncertainty in Umag (2) 34 A1 --- l_Bmag [>] Limit flag on Bmag 35- 39 F5.2 mag Bmag ? B-band magnitude 41- 44 F4.2 mag e_Bmag ? Uncertainty in Bmag (2) 46 A1 --- l_Vmag [>] Limit flag on Vmag 47- 51 F5.2 mag Vmag ? V-band magnitude (3) 53- 56 F4.2 mag e_Vmag ? Uncertainty in Vmag (2) (3) 58 A1 --- l_Rmag [>] Limit flag on Rmag 59- 63 F5.2 mag Rmag ? R-band magnitude (3) 65- 68 F4.2 mag e_Rmag ? Uncertainty in Rmag (2) (3) 70 A1 --- l_Imag [>] Limit flag on Imag 71- 75 F5.2 mag Imag ? I-band magnitude 77- 80 F4.2 mag e_Imag ? Uncertainty in Imag (2) 82 A1 --- l_Jmag [>] Limit flag on Jmag 83- 87 F5.2 mag Jmag ? J-band magnitude 89- 92 F4.2 mag e_Jmag ? Uncertainty in Jmag (2) 94 A1 --- l_Hmag [>] Limit flag on Hmag 95- 99 F5.2 mag Hmag ? H-band magnitude 101-104 F4.2 mag e_Hmag ? Uncertainty in Hmag (2) 106 A1 --- l_Kmag [>] Limit flag on Kmag 107-111 F5.2 mag Kmag ? K-band magnitude 113-116 F4.2 mag e_Kmag ? Uncertainty in Kmag (2) 118-119 I2 --- Inst [1/19] Instrument identification (4)
Note (1): Note as follows: * = Marks unfiltered data rescaled to the R-band magnitudes. These have been obtained by computing zero-points using the R-band magnitudes of the stellar sequence in the SN field, and assuming negligible colour correction; D = Indicates luminance filter measurements reported to V-band magnitudes. Note (2): The errors are obtained by combining in quadrature the errors in the photometric calibration and instrumental PSF measurement errors. Note (3): Standard Johnson-Cousins V- and R-band magnitudes from amateur astronomers have been obtained by computing instrumental zero-points using the V and R magnitudes of the local sequence stars reported in Table A1, and adopting no colour correction. Note (4): The numbers identify the instrumental configurations. Source as follows: 1 = Meade 16" Reflector + SBIG ST-9XE Dual CCD camera (Rich Observatory, Hampden, Maine, USA; obs. D.R.); 2 = 0.4-m MASTER telescope + Apogee Alta U16M CCD (Kislovodsk, Caucasian region Russia); 3 = 0.36-m Schmidt-Cassegrain + Apogee ALTA U47 CCD camera (New Millennium Observatory, Mozzate, Italy; obs. E. Cozzi); 4 = 12.5-inch RCOS Telescope + SBIG STL6303 CCD camera (Macedon Ranges Observatory, Melbourne, Australia; obs. J. Brimacombe); 5 = 0.4-m MASTER Telescope + Apogee Alta U16M CCD (Blagoveschensk; Far East region, Russia); 6 = 0.80-m Tsinghua-NAOC Telescope + Princeton Instruments VersArray:1300B CCD (Xinglong Observatory, Yanshan mountains, Hebei, China); 7 = 2.0-m Liverpool Telescope + SupIRCam (La Palma, Canary Islands, Spain); 8 = 8.2-m Very Large Ttelescope (UT2) + XShooter (spectrophotometry; European Southern Observatory; Cerro Paranal, Chile); 9 = 280-mm Celestron 11 + Atik 16HR with Sony chip ICX285AL (Posadas Observatory; Cordoba, Spain; obs. R. Benavides); 10 = 1.82-m Copernico Telescope + AFOSC (Mt. Ekar, Asiago, Italy); 11 = 3.58-m New Technology Telescope + EFOSC2 (European Southern Observatory; La Silla, Chile); 12 = 3.58-m New Technology Telescope + SOFI (European Southern Observatory; La Silla, Chile); 13 = 3.58-m Telescopio Nazionale Galileo + Dolores (La Palma, Canary Islands, Spain); 14 = 2.2-m Calar Alto Telescope + CAFOS (Calar Alto Observatory, Almeria, Spain); 15 = 2 OE 8.4-m Large Binocular Telescope + Lucifer (Mt. Graham International Observatory, Arizona, USA); 16 = 67/92-cm Schmidt Telescope + SCAM (Mt. Ekar, Asiago, Italy); 17 = 2.0-m Faulkes Telescope North + EM03 (Haleakala, Hawaii Isl., USA); 18 = 2.0-m Liverpool Telescope + RATCam (La Palma, Canary Isl., Spain); 19 = 4.2-m William Herschel Telescope + ACAM (La Palma, Canary Isl., Spain).
Byte-by-byte Description of file: tablea5.dat
Bytes Format Units Label Explanations
1 A1 --- SN [AB] SN designation (1) 3- 13 A11 "date" Date Observation date 15- 21 F7.2 d JD Julian Date (JD-2455000) 23 A1 --- l_uvw2 [>] Limit flag on uvw2 24- 28 F5.2 mag uvw2 Swift/UVOT uvw2 magnitude 30- 33 F4.2 mag e_uvw2 ? Uncertainty in uvw2 35 A1 --- l_uvm2 [>] Limit flag on uvm2 36- 40 F5.2 mag uvm2 Swift/UVOT uvm2 magnitude 42- 45 F4.2 mag e_uvm2 ? Uncertainty in uvm2 47 A1 --- l_uvw1 [>] Limit flag on uvw1 48- 52 F5.2 mag uvw1 Swift/UVOT uvw1 magnitude 54- 57 F4.2 mag e_uvw1 ? Uncertainty in uvw1 59 A1 --- l_umag [>] Limit flag on umag 60- 64 F5.2 mag umag ? Swift/UVOT u-band magnitude (2) 66- 69 F4.2 mag e_umag ? Uncertainty in umag (2) 71 A1 --- l_bmag [>] Limit flag on bmag 72- 76 F5.2 mag bmag ? Swift/UVOT b-band magnitude (2) 78- 81 F4.2 mag e_bmag ? Uncertainty in bmag (2) 83 A1 --- l_vmag [>] Limit flag on vmag 84- 88 F5.2 mag vmag ? Swift/UVOT v-band magnitude (2) 90- 93 F4.2 mag e_vmag ? Uncertainty in vmag (2)
Note (1): SN as follows: A = SN 2010al; B = SN 2011hw. Note (2): Original u, b, v UVOT magnitudes have been converted to those in the Johnson-Cousins photometric system using the magnitudes of the stellar sequences reported in Table A1.
History: From electronic version of the journal References: Pastorello et al. Paper I. 2008MNRAS.389..113P Pastorello et al. Paper II. 2008MNRAS.389..131P Mattila et al. Paper III. 2008MNRAS.389..141M Pastorello et al. Paper V. 2015MNRAS.449.1941P Pastorello et al. Paper VI. 2015MNRAS.449.1954P Pastorello et al. Paper VII. 2015MNRAS.453.3649P Pastorello et al. Paper VIII. 2015MNRAS.454.4293P Pastorello et al. Paper IX. 2016MNRAS.456..853P
(End) Tiphaine Pouvreau [CDS] 04-Dec-2017
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