SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova

被引：41

作者：

Jacobson-Galan, W. V. ^{[1
]}

Dessart, L. ^{[2
]}

Margutti, R. ^{[1
,3
]}

Chornock, R. ^{[1
]}

Foley, R. J. ^{[4
]}

Kilpatrick, C. D. ^{[5
]}

Jones, D. O. ^{[6
,7
]}

Taggart, K. ^{[4
]}

Angus, C. R. ^{[8
]}

Bhattacharjee, S. ^{[9
]}

Braff, L. A. ^{[4
]}

Brethauer, D. ^{[1
]}

Burgasser, A. J. ^{[10
]}

Cao, F. ^{[11
]}

Carlile, C. M. ^{[12
]}

Chambers, K. C. ^{[13
]}

Coulter, D. A. ^{[4
]}

Dominguez-Ruiz, E. ^{[4
]}

Dickinson, C. B. ^{[4
]}

de Boer, T. ^{[13
]}

Gagliano, A. ^{[14
,15
]}

Gall, C. ^{[8
]}

Gao, H. ^{[13
]}

Gates, E. L. ^{[16
]}

Gomez, S. ^{[17
]}

Guolo, M. ^{[18
]}

Halford, M. R. J. ^{[19
]}

Hjorth, J. ^{[8
]}

Huber, M. E. ^{[13
]}

Johnson, M. N. ^{[20
]}

Karpoor, P. R. ^{[12
]}

Laskar, T. ^{[21
]}

Lebaron, N. ^{[1
]}

Li, Z. ^{[22
]}

Lin, Y. ^{[23
]}

Loch, S. D. ^{[19
]}

Lynam, P. D. ^{[16
]}

Magnier, E. A. ^{[13
]}

Maloney, P. ^{[4
]}

Matthews, D. J. ^{[1
]}

Mcdonald, M. ^{[23
]}

Miao, H. -y. ^{[9
]}

Milisavljevic, D. ^{[24
]}

Pan, Y. -c. ^{[9
]}

Pradyumna, S. ^{[23
]}

Ransome, C. L. ^{[25
]}

Rees, J. M. ^{[16
]}

Rest, A. ^{[17
,18
]}

Rojas-Bravo, C. ^{[4
]}

Sandford, N. R. ^{[1
]}

机构：

[1] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[2] Sorbonne Univ, Inst Astrophys Paris, CNRS, 98 bis Blvd Arago, F-75014 Paris, France

[3] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[4] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[5] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys CIE, Evanston, IL 60208 USA

[6] Gemini Observ, NSFs NOIRLab, 670 N Aohoku Pl, Hilo, HI 96720 USA

[7] Univ Copenhagen, Niels Bohr Inst, DARK, Jagtvej 128, Copenhagen, Denmark

[8] Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Zhongli 32001, Taoyuan, Taiwan

[9] Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Zhongli 32001, Taoyuan, Taiwan

[10] Univ Calif Riverside, UC San Didept Stat, Riverside, CA 92521 USA

[11] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA

[12] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

[13] Univ Illinois, Dept Astron, 1002 W Green St, Champaign, IL 61801 USA

[14] Ctr Astrophys Surveys, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA

[15] Univ Calif Observ, Lick Observ, Mt Hamilton, CA 95140 USA

[16] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[17] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[18] Auburn Univ, Dept Phys, 380 Duncan Dr, Auburn, AL 36849 USA

[19] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA

[20] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA

[21] Univ Calif Riverside, Dept Earth & Planetary Sci, Riverside, CA 92521 USA

[22] Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA USA

[23] Purdue Univ, Dept Phys & Astron, 525 Northwestern Ave, W Lafayette, IN 47907 USA

[24] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[25] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[26] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, North Ireland

[27] Univ Oxford, Dept Phys, Keble Rd, Oxford, England

[28] Penn State Univ, Inst Computat & Data Sci, University Pk, PA USA

[29] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2023年 / 954卷 / 02期

关键词：

MASS-LOSS; PAN-STARRS; EMISSION-LINES; LOCAL VALUE; PROGENITOR; DRIVEN; WINDS; SPECTROSCOPY; EXPLOSION; TELESCOPE;

D O I：

10.3847/2041-8213/acf2ec

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present UV and/or optical observations and models of SN 2023ixf, a type II supernova (SN) located in Messier 101 at 6.9 Mpc. Early time (flash) spectroscopy of SN 2023ixf, obtained primarily at Lick Observatory, reveals emission lines of H i, He i/ii, C iv, and N iii/iv/v with a narrow core and broad, symmetric wings arising from the photoionization of dense, close-in circumstellar material (CSM) located around the progenitor star prior to shock breakout. These electron-scattering broadened line profiles persist for similar to 8 days with respect to first light, at which time Doppler broadened the features from the fastest SN ejecta form, suggesting a reduction in CSM density at r greater than or similar to 10(15) cm. The early time light curve of SN 2023ixf shows peak absolute magnitudes (e.g., M-u = -18.6 mag, M-g = -18.4 mag) that are greater than or similar to 2 mag brighter than typical type II SNe, this photometric boost also being consistent with the shock power supplied from CSM interaction. Comparison of SN 2023ixf to a grid of light-curve and multiepoch spectral models from the non-LTE radiative transfer code CMFGEN and the radiation-hydrodynamics code HERACLES suggests dense, solar-metallicity CSM confined to r = (0.5-1) <bold>x</bold> 10(15) cm, and a progenitor mass-loss rate of M-center dot=10(-2 )M(circle dot) yr(-1). For the assumed progenitor wind velocity of v(w) = 50 km s(-1), this corresponds to enhanced mass loss (i.e., superwind phase) during the last similar to 3-6 yr before explosion.

引用

页数：15

共 10 条

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