Circumstellar Interaction Signatures in the Low-luminosity Type II SN 2021gmj

被引：3

作者：

Meza-Retamal, Nicolas ^{[1
]}

Dong, Yize ^{[1
]}

Bostroem, K. Azalee ^{[2
]}

Valenti, Stefano ^{[1
]}

Galbany, Lluis ^{[3
,4
]}

Pearson, Jeniveve ^{[2
]}

Hosseinzadeh, Griffin ^{[2
]}

Andrews, Jennifer E. ^{[5
]}

Sand, David J. ^{[2
]}

Jencson, Jacob E. ^{[2
]}

Janzen, Daryl ^{[6
]}

Lundquist, Michael J. ^{[7
]}

Hoang, Emily T. ^{[1
]}

Wyatt, Samuel ^{[8
]}

Brown, Peter J. ^{[9
]}

Howell, D. Andrew ^{[10
,11
]}

Newsome, Megan ^{[10
,11
]}

Gonzalez, Estefania Padilla ^{[10
,11
]}

Pellegrino, Craig ^{[10
,11
]}

Terreran, Giacomo ^{[10
,11
]}

Kouprianov, Vladimir ^{[12
]}

Hiramatsu, Daichi ^{[13
,14
]}

Jha, Saurabh W. ^{[15
]}

Smith, Nathan ^{[2
]}

Haislip, Joshua ^{[12
]}

Reichart, Daniel E. ^{[12
]}

Shrestha, Manisha ^{[2
]}

Rosales-Ortega, F. Fabian ^{[16
]}

Brink, Thomas G. ^{[17
]}

Filippenko, Alexei V. ^{[17
]}

Zheng, Weikang ^{[17
]}

Yang, Yi ^{[17
,18
,19
]}

机构：

[1] Univ Calif Davis, Dept Phys & Astron, 1 Shields Ave, Davis, CA 95616 USA

[2] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA

[3] Inst Space Sci ICE, CSIC, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[4] Inst Estudis Espacials Catalunya, Gran Capita 2-4 Edif Nexus,Desp 201, E-08034 Barcelona, Spain

[5] Gemini Observ, 670 North Aohoku Pl, Hilo, HI 96720 USA

[6] Univ Saskatchewan, Dept Phys & Engn Phys, 116 Sci Pl, Saskatoon, SK S7N 5E2, Canada

[7] WM Keck Observ, 65-1120 Mamalahoa Highway, Kamuela, HI 96743 USA

[8] Univ Washington, Dept Astron, 3910 15th Ave NE, Seattle, WA 98195 USA

[9] Texas A&M Univ, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA

[10] Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA

[11] Univ Calif, Dept Phys, Santa Barbara, CA 93106 USA

[12] Univ N Carolina, Dept Phys & Astron, 120 East Cameron Ave, Chapel Hill, NC 27599 USA

[13] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[14] NSF AI Inst Artificial Intelligence & Fundamental, Cambridge, MA USA

[15] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA

[16] Inst Nacl Astrofis Opt & Elect INAOE CONACyT, Luis E Erro 1, Puebla 72840, Mexico

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

[18] Tsinghua Univ, Phys Dept, Beijing 100084, Peoples R China

[19] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2024年 / 971卷 / 02期

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

CORE-COLLAPSE SUPERNOVAE; FOLLOW-UP OBSERVATIONS; LIGHT-CURVES; MASS-LOSS; SHOCK BREAKOUT; HYDROGEN-RICH; DISTANCE DETERMINATION; UV/OPTICAL EMISSION; PLATEAU SUPERNOVAE; NEBULAR SPECTRA;

D O I：

10.3847/1538-4357/ad4d55

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present comprehensive optical observations of SN 2021gmj, a Type II supernova (SN II) discovered within a day of explosion by the Distance Less Than 40 Mpc survey. Follow-up observations show that SN 2021gmj is a low-luminosity SN II (LL SN II), with a peak magnitude M-V = -15.45 and an Fe ii velocity of similar to 1800 km s(-1) at 50 days past explosion. Using the expanding photosphere method, we derive a distance of 17.8-0.4+0.6 Mpc. From the tail of the light curve we obtain a radioactive nickel mass of (MNi)-Ni-56 = 0.014 +/- 0.001 M-circle dot. The presence of circumstellar material (CSM) is suggested by the early-time light curve, early spectra, and high-velocity H alpha in absorption. Analytical shock-cooling models of the light curve cannot reproduce the fast rise, supporting the idea that the early-time emission is partially powered by the interaction of the SN ejecta and CSM. The inferred low CSM mass of 0.025 M-circle dot in our hydrodynamic-modeling light-curve analysis is also consistent with our spectroscopy. We observe a broad feature near 4600 angstrom, which may be high-ionization lines of C, N, or/and He II. This feature is reproduced by radiation-hydrodynamic simulations of red supergiants with extended atmospheres. Several LL SNe II show similar spectral features, implying that high-density material around the progenitor may be common among them.

引用

页数：20

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