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Optical and IR Observations of SN 2002Dj: Some Possible Common Mon. Not. R. Astron. Soc. 000, 1–?? (2008) Printed 26 October 2018 (MN LATEX style file v2.2) Optical and IR observations of SN 2002dj: some possible common properties of fast expanding SNe Ia G. Pignata,1,2⋆ S. Benetti,3 P. A. Mazzali,4,5 R. Kotak,6 F. Patat,7 P. Meikle,8 M. Stehle,4 B. Leibundgut,7 N. B. Suntzeff,9 L. M. Buson,3 E. Cappellaro,3 A. Clocchiatti,2 M. Hamuy,1 J. Maza,1 J. Mendez,10 P. Ruiz-Lapuente,10 M. Salvo,11 B. P. Schmidt,11 M. Turatto3 and W. Hillebrandt4 1 Departamento de Astronom´ıa, Universidad de Chile, Casilla 36-D, Santiago, Chile 2 Departamento de Astronom´ıa y Astrof´ısica, Pontificia Universidad Cat´olica de Chile, Casilla 306, Santiago 22, Chile 3 INAF Osservatorio Astronomico di Padova, Vicolo dell Osservatorio 5, I-35122 Padova, Italy 4 Max-Planck-Institut f¨ur Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching bei M¨unchen, Germany 5 Osservatorio Astronomico di Trieste, Via Tiepolo 11, I-34131 Trieste, Italy 6 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, United Kingdom 7 European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei M¨unchen, Germany 8 Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2BW, United Kingdom 9 Department of Physics, Texas A&M University, College Station, TX 77843-4242 10 Department of Astronomy, University of Barcelona, Marti i Franques 1, E-08028 Barcelona, Spain 11 Research School of Astronomy and Astrophysics, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia Accepted ...... Received .......; in original form ....... ABSTRACT As part of the European Supernova Collaboration we obtained extensive photome- try and spectroscopy of the type Ia SN 2002dj covering epochs from 11 days before to nearly two years after maximum. Detailed optical and near-infrared observations show that this object belongs to the class of the high-velocity gradient events as indi- cated by Si, S and Ca lines. The light curve shape and velocity evolution of SN 2002dj appear to be nearly identical to SN 2002bo. The only significant difference is observed in the optical to near-IR colours and a reduced spectral emission beyond 6500 A.˚ For high-velocity gradient Type Ia supernovae, we tentatively identify a faster rise to max- imum, a more pronounced inflection in the V and R light curves after maximum and a brighter, slower declining late-time B light curve as common photometric properties arXiv:0805.1089v2 [astro-ph] 11 Jun 2008 of this class of objects. They also seem to be characterized by a different colour and colour evolution with respect to “normal” SNe Ia. The usual light curve shape param- eters do not distinguish these events. Stronger, more blueshifted absorption features of intermediate-mass elements and lower temperatures are the most prominent spec- troscopic features of Type Ia supernovae displaying high velocity gradients. It appears that these events burn more intermediate-mass elements in the outer layers. Possible connections to the metallicity of the progenitor star are explored. Key words: supernovae: general - supernovae: individual: SN 2002dj 1 INTRODUCTION 2007) and SNLS (Astier et al. 2006) use the relation be- tween the shape of the light curve and its peak lumi- In the last decade type Ia Supernovae (SNe Ia) have nosity (Phillips 1993; Phillips et al. 1999; Hamuy et al. been extensively used for cosmology yielding evidence 1996; Riess, Press & Kirshner 1996; Goldhaber et al. 2001; that we live in an accelerating Universe (Riess et al. Guy et al. 2005; Prieto, Rest & Suntzeff 2006) to constrain 1998; Perlmutter et al. 1999). Ongoing surveys such the equation-of-state parameter for dark energy. An impor- as ESSENCE (Miknaitis et al. 2007; Wood-Vasey et al. tant caveat is that those relations assume that SNe Ia are a one parameter family. ⋆ E-mail: [email protected] However, in recent years there has been growing evi- c 2008 RAS 2 G. Pignata dence for the observational diversity among SN Ia and this Table 3. Magnitudes for the local IR photometric sequence in the is of prime interest in their application as distance indica- field of SN 2002dj (Fig. 1 right panel). The data were obtained tors. Subtle but unequivocal differences between events with during three photometric nights with SofI. large wavelength coverage and dense temporal sampling are evident in light curve shapes, colour evolutions, luminosities, id J H Ks evolution of spectral lines and expansion velocities derived 2 12.23 ± 0.03 11.75 ± 0.03 11.63 ± 0.03 from the line shifts. The search for accurate correlations be- 2 IR 14.80 ± 0.03 14.18 ± 0.03 13.95 ± 0.04 tween photometric and spectroscopic properties could im- 7 13.63 ± 0.04 13.42 ± 0.04 13.38 ± 0.04 prove the luminosity calibration and help to shed light on 11 14.32 ± 0.04 13.89 ± 0.04 13.76 ± 0.04 the explosion mechanisms and progenitor system. Recently, Benetti et al. (2005) have identified three classes of SNe Ia based on their spectroscopic features. A similar classification is also reported in Branch et al. (2006). Interestingly, two of these classes are nearly indistinguishable in some of their photometric parameters (e.g. ∆m15, Phillips et al. 1993); • yet they show clear spectroscopic differences. High velocity 0.9m telescope located at Cerro Tololo Inter-American gradient (HVG) SNe are characterized by a fast decrease Observatory (CTIO) equipped with a CCD camera × −1 in their expansion velocity over time as measured from the (2048 2048, pixel size = 0.40 arcsec pixel ) and UBVRI minimum of the Si II (6355 A)˚ absorption line. On the other Johnsons, Kron-Cousin standard filters. • hand in the low velocity gradient (LVG) SNe group, which 1.0m telescope located at CTIO equipped with A Novel represents the majority of SN Ia, the evolution of the Si II Double-Imaging CAMera (ANDICAM; Hawaii HgCdTe × −1 (6355 A)˚ velocity is smooth, the ejecta expansion is slower 1024 1024, pixel size = 0.137 arcsec pixel ) and JHKs than in HVG SNe. These spectroscopic differences may or standard filters. may not affect the relations used to calibrate the luminosi- • European Southern Observatory (ESO) New Technol- ties of SNe Ia. Subtle differences in colour may exist among ogy Telescope (NTT) located at La Silla Observatory and the different classes and lead to significant bias in redden- equipped with the ESO Multi Mode Instrument (EMMI) in RILD mode (2×MIT/LL CCD 2048×4096, pixel size = ing estimates. The existence of spectroscopic families sug- −1 gests possible differences in the progenitor channels and/or 0.167 arcsec pixel ) and BVRI standard filters with ESO explosion mechanisms. Branch & van den Bergh (1993) for identification numbers 605, 606, 608 and 610, respectively. example reported that SNe characterized by high expansion • ESO-NTT equipped with the Son of ISAAC camera velocities, tend to explode in late type galaxies, pointing to (SofI; Hawaii HgCdTe 1024×1024, pixel size = 0.29 arcsec −1 progenitors arising from a young population. pixel ) and JHKs standard filters. In this paper we present the observations of the HVG • Danish 1.54m telescope located at La Silla Observatory SN 2002dj carried out by the European Supernova Col- equipped with the Danish Faint Object Spectrograph and laboration (ESC). SN 2002dj (α = 13h13m00s.34, δ = Camera (DFOSC; MAT/EEV CCD 44-82 2048×2048, pixel −1 −19◦31′08′′.7, J2000) was discovered in NGC 5018 on June size = 0.39 arcsec pixel ) and UBVRI standard filters with 12.2 UT (IAUC 7918, Hutchings & Li 2002) and classified by ESO identification numbers 632, 450, 451, 452 and 425, re- ESC members as a Type Ia event on June 14.15 UT (IAUC spectively. 7919, Riello et al. 2002). The layout of the manuscript is as • ESO-Kueyen Very Large Telescope (VLT) located at follows. Observations and data reduction are presented in Paranal Observatory equipped with the FOcal Reducer and Sect. 2. We describe the reddening estimate in Sect. 3. In low dispersion Spectrograph (FORS1; 2×E2V 2048×4096 −1 Sect. 4 we analyze the SN 2002dj optical and IR photometry pixel size = 0.2 arcsec pixel ) and BVRI standard filters comparing its properties with those of its kinematical twin, with ESO identification numbers +34, +35, +36 and +37, SN 2002bo. We also investigate whether they are representa- respectively. tive of the HVG SNe group. Sect. 5 contains the determina- • Nordic Optical Telescope (NOT) located at Roque de tion of the SN 2002dj absolute luminosity and a character- los Muchachos Observatory equipped with the Andaluc´ıa ization of the properties of its host galaxy. The optical and Faint Object Spectrograph and Camera (ALFOSC; E2V −1 IR spectroscopy is analyzed in Sect. 6 and Sect. 7, respec- 2048×2048, pixel size = 0.19 arcsec pixel ) and UBVR tively. The expansion velocities are discussed in Sect. 8 and standard filters with NOT identification numbers 7, 74, 75 models of the early and late spectra in Sect 9. We conclude and 76, respectively, and an interference i filter with number in Sect. 10 by examining possible physical conditions in the 12. HGV SNe ejecta that could explain part of their spectro- • Isaac Newton Group (ING) Jacobus Kapteyn Telescope scopic and photometric behavior. (JKT) located at Roque de los Muchachos Observatory equipped with a CCD camera (SITe2 2048×2048, pixel size = 0.33 arcsec pixel−1) and UBVRI standard filters with ING identification numbers 3, 27, 30, 37 and 44, respectively. 2 OBSERVATIONS AND DATA REDUCTION • ING-Isaac Newton Telescope (INT) located at Roque de los Muchachos Observatory equipped with the Wide Field 2.1 Instrument settings Camera (WFC; 4 thinned EEV 2048×4096, pixel size = 0.33 −1 SN 2002dj was observed with seven different instruments in arcsec pixel ) and UBVRi(sloan) standard filters with ING the optical and two facilities in the near infrared.
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