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OPTICAL OBSERVATIONS OF THE TYPE IA SUPERNOVA SN 2011fe IN M101 FOR NEARLY 500 DAYS

Kaicheng ZhangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaXiaofeng WangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaJujia ZhangKey Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, ChinaTianmeng ZhangNational Astronomical Observatory of China, Chinese Academy of Sciences, Beijing, 100012, ChinaM. GaneshalingamDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAWeidong LiDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAA. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAXulin ZhaoPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaWeiKang ZhengDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USABai, JinmingKey Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, ChinaJia ChenPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaJun-Cheng ChenPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaFang HuangAstronomy Department, Beijing Normal University, Beijing, 100875, ChinaJun MoPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaLiming RuiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaHao SongPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaHanna SaiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaWenxiong LiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, ChinaLifan WangPhysics and Astronomy Department, Texas A&M University, College Station, TX 77843, USAChao WuNational Astronomical Observatory of China, Chinese Academy of Sciences, Beijing, 100012, China

2019en

ABI

Annotatsiya

We present well-sampled optical observations of the bright Type Ia supernova (SN~Ia) SN 2011fe in M101. Our data, starting from $\sim16$ days before maximum light and extending to $\sim463$ days after maximum, provide an unprecedented time series of spectra and photometry for a normal SN~Ia. Fitting the early-time rising light curve, we find that the luminosity evolution of SN 2011fe follows a $t^n$ law, with the index $n$ being close to 2.0 in the $VRI$ bands but slightly larger in the $U$ and $B$ bands. Combining the published ultraviolet (UV) and near-infrared (NIR) photometry, we derive the contribution of UV/NIR emission relative to the optical. SN 2011fe is found to have stronger UV emission and reaches its UV peak a few days earlier than other SNe~Ia with similar $\Delta m_{15}(B)$, suggestive of less trapping of high-energy photons in the ejecta. Moreover, the $U$-band light curve shows a notably faster decline at late phases ($t\approx 100$--300 days), which also suggests that the ejecta may be relatively transparent to UV photons. These results favor the notion that SN 2011fe might have a progenitor system with relatively lower metallicity. On the other hand, the early-phase spectra exhibit prominent high-velocity features (HVFs) of O~I $\lambda$7773 and the Ca~II~NIR triplet, but only barely detectable in Si~II~6355. This difference can be caused either by an ionization/temperature effect or an abundance enhancement scenario for the formation of HVFs; it suggests that the photospheric temperature of SN 2011fe is intrinsically low, perhaps owing to incomplete burning during the explosion of the white dwarf.

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