Maqola

Optical and near-infrared observations of SN 2023ixf for over 600 days after the explosion

G.-C. LiDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaX. WangDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaA. PastorelloINAF -Osservatorio Astronomico di Padova , Vicolo dell'Osservatorio 5 , 35122 Padova , ItalyA. ReguittiINAF -Osservatorio Astronomico di Padova , Vicolo dell'Osservatorio 5 , 35122 Padova , ItalyG. ValerinINAF -Osservatorio Astronomico di Padova , Vicolo dell'Osservatorio 5 , 35122 Padova , ItalyP. OchnerDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyT. IijimaINAF -Osservatorio Astronomico di Padova , Vicolo dell'Osservatorio 5 , 35122 Padova , ItalyU. MunariINAF -Osservatorio Astronomico di Padova , Vicolo dell'Osservatorio 5 , 35122 Padova , ItalyI. SalmasoINAF-Osservatorio Astronomico di Capodimonte , Salita Moiariello 16 , 80131 Napoli , ItalyA. FarinaDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyR. CazzolaDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyN. TrabacchinCISAS G. Colombo , University of Padova , Via Venezia 15 , 35131 Padova , ItalyS. FiscaleINAF , Osservatorio Astronomico di Capodimonte , Salita Moiariello , 16 , Naples I-80131 , ItalyS. CiroiDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyA. MuraDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyA. SivieroINAF -Osservatorio Astronomico di Padova , Vicolo dell'Osservatorio 5 , 35122 Padova , ItalyF. CabrasDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyM. PabstDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyS. TaubenbergerMax-Planck-Institut fur Astrophysik , Karl-Schwarzschild Straße 1 , 85748 Garching , GermanyC. VoglMax-Planck-Institut fur Astrophysik , Karl-Schwarzschild Straße 1 , 85748 Garching , GermanyC. FiorinDipartimento di Fisica e Astronomia , Università Degli Studi di Padova , 35121 Padova , PD , ItalyJ. LiuDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaL. ChenDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaD. XiangJ. MoDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaLi LiZ.-Y. WangJ. ZhangQ. ZhaiKey Laboratory for the Structure and Evolution of Celestial Objects , Chinese Academy of Sciences , Kunming 650216 , ChinaD. O. MirzaqulovS. A. EhgamberdievUlugh Beg Astronomical Institute , Astronomy Street 33 , Tashkent 100052 , UzbekistanA. V. FilippenkoDepartment of Astronomy , University of California , Berkeley , CA 94720-3411 , USAS. YanDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaM. HuDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaX.-R. MaDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaQ. XiaDepartment of Physics , Tsinghua University , Beijing 100084 , ChinaX. GaoXingming Observatory , Urumqi 830000 , ChinaW. LiNational Astronomical Observatories , Chinese Academy of Sci- ences , Beijing 100101 , PR China

2025en

Ochiq kirishYashil

ABI

Annotatsiya

Context. We present a comprehensive photometric and spectroscopic study of the nearby Type II supernova (SN) 2023ixf; our extensive observations span the phases from ∼3 to over 600 days after the first light. Aims. The aim of this study is to obtain key information on the explosion properties of SN 2023ixf and the nature of its progenitor. Methods. The observational properties of SN 2023ixf were compared with those of a representative sample of Type IIP and IIL SNe to investigate commonalities and diversities. We conducted a detailed analysis of the temporal evolution of major spectral features observed throughout different phases of the SN 2023ixf explosion. Several key interpretations are addressed through a comparison between the data and the model spectra predicted by nonlocal thermodynamic equilibrium (non-LTE) radiative-transfer calculations for progenitor stars within a range of zero-age main sequence (ZAMS) masses. Results. Our observations indicate that SN 2023ixf is a transitional SN that bridges the gap between the Type IIP and IIL subclasses of H-rich SNe; it is characterized by a relatively short plateau (≲70 d) in the light curve. It shows a rather prompt spectroscopic evolution toward the nebular phase; emission lines of Na, O, H, and Ca in nebular spectra all exhibit multi-peak profiles, which might be due to a bipolar distribution of the ejecta. In particular, the Hα profile can be separated into two central peaked components (with velocities of about 1500 km s−1) that are likely due to nickel-powered ejecta and two outer box components (with velocities of up to ∼8000 km s−1) that can arise from interactions of the outermost ejecta with a circumstellar shell at a distance of ∼6.2 × 1015 cm. The nebular-phase spectra of SN 2023ixf show good agreement with those predicted by a non-LTE radiative-transfer code for progenitor stars with ZAMS masses ranging from 15 to 19 M⊙. A distance of $ 6.35^{+0.31}_{-0.39} $ Mpc is estimated for M101 based on the expanding photosphere method.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1051/0004-6361/202555030/pdf

Iqtiboslar va manbalar

0 ta iqtibos0 ta foydalanilgan manba