Early Observations and Analysis of the Type Ia SN 2014J in M82
| Autor: | Marion, G. H., Sand, D. J., Hsiao, E. Y., Banerjee, D. P. K., Valenti, S., Stritzinger, M. D., Vinkó, J., Joshi, V., Venkataraman, V., Ashok, N. M., Amanullah, R., Binzel, R. P., Bochanski, J. J., Bryngelson, G. L., Burns, C. R., Drozdov, D., Fieber-Beyer, S. K., Graham, M. L., Howell, D. A., Johansson, J., Kirshner, R. P., Milne, P. A., Parrent, J., Silverman, J. M., Vervack, R. J., Wheeler, J. C. |
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| Rok vydání: | 2014 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1088/0004-637X/798/1/39 |
| Popis: | We present optical and near infrared (NIR) observations of the nearby Type Ia SN 2014J. Seventeen optical and twenty-three NIR spectra were obtained from 10 days before ($-$10d) to 10 days after (+10d) the time of maximum $B$-band brightness. The relative strengths of absorption features and their patterns of development can be compared at one day intervals throughout most of this period. Carbon is not detected in the optical spectra, but we identify CI $\lambda$ 1.0693 in the NIR spectra. We find that MgII lines with high oscillator strengths have higher initial velocities than other MgII lines. We show that the velocity differences can be explained by differences in optical depths due to oscillator strengths. The spectra of SN 2014J show it is a normal SN Ia, but many parameters are near the boundaries between normal and high-velocity subclasses. The velocities for OI, MgII, SiII, SII, CaII and FeII suggest that SN 2014J has a layered structure with little or no mixing. That result is consistent with the delayed detonation explosion models. We also report photometric observations, obtained from $-$10d to +29d, in the $UBVRIJH$ and $K_s$ bands. SN 2014J is about 3 magnitudes fainter than a normal SN Ia at the distance of M82, which we attribute to extinction in the host. The template fitting package SNooPy is used to interpret the light curves and to derive photometric parameters. Using $R_V$ = 1.46, which is consistent with previous studies, SNooPy finds that $A_V = 1.80$ for $E(B-V)_{host}=1.23 \pm 0.01$ mag. The maximum $B$-band brightness of $-19.19 \pm 0.10$ mag was reached on February 1.74 UT $ \pm 0.13$ days and the supernova had a decline parameter of $\Delta m_{15}=1.11 \pm 0.02$ mag. Comment: 6 figures, 6 tables, submitted to the ApJ |
| Databáze: | arXiv |
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