在Pan-STARRS1 Medium Deep Survey中發現的類SN 1991T型超新星

以作者查詢圖書館館藏

、以作者查詢臺灣博碩士

、以作者查詢全國書目

、勘誤回報

、線上人數：119

、訪客IP：3.133.123.162

姓名

王品涵(Pin-Han Wang) 查詢紙本館藏

畢業系所

天文研究所

論文名稱

在Pan-STARRS1 Medium Deep Survey中發現的類SN 1991T型超新星
(The 1991T-like Type Ia Supernovae Discovered in Pan-STARRS1 Medium Deep Survey)

相關論文

★ LSST時代的資料處理──自動化的瞬變天體數據處理流水線

★ 透過噴發物速度探討 Ia 型超新星之演化

檔案

[Endnote RIS 格式]

[Bibtex 格式]

[相關文章]

[文章引用]

[完整記錄]

[館藏目錄]

[檢視]

[下載]

本電子論文使用權限為同意立即開放。
已達開放權限電子全文僅授權使用者為學術研究之目的，進行個人非營利性質之檢索、閱讀、列印。
請遵守中華民國著作權法之相關規定，切勿任意重製、散佈、改作、轉貼、播送，以免觸法。

摘要(中)

Ia型超新星中包含了典型的Ia型超新星和特殊的超新星，典型Ia型超新星是測量宇宙膨脹的可標準化燭光。而特殊的Ia型超新星中，91T-like超新星比起典型的Ia型超新星來得亮，也更容易在高紅移的宇宙中被發現，所以我們想找出並研究在高紅移的巡天計畫中所發現的91T-like超新星。我們的母樣本為約400顆來自Pan-STARRS1 Medium Deep Survey (PS1-MDS)的高紅移超新星，而我們使用了其光譜分類出16顆91T-like超新星，並進一步探討其特性。我們主要發現91T-like超新星的光度曲線下降率平均來說比起正常的Ia型超新星來得慢，這也與其較亮的光度一致，且其Hubble Residual傾向為負值。而91T-like超新星的顏色和其他類別的超新星相比並沒有明顯的差異，可能是受到星系裡塵埃的影響。再來是宿主星系的質量、恆星形成率和特定的恆星形成率，我們發現91T-like超新星的宿主星系質量和其他類別相比沒有明顯的差異，而91T-like超新星傾向出現在高恆星形成率和較高的特定恆星形成率的星系，較不會出現在很老或接近死亡的星系中。這些結果顯示高紅移的91T-like超新星與先前低紅移研究中的91T-like超新星有著一致的特性。

摘要(英)

Type Ia supernovae (SNe Ia) can be classified into many sub-types, including normal SNe Ia and several peculiar types such as 91-like and 91bg-like SNe Ia. Normal SNe~Ia are widely used as standardized candles for measuring the expansion of the universe. Among the peculiar types of SNe Ia, 91T-like SN Ia represents the brightest class. It is easier to detect in the high-redshift Universe. In this work, we aim to identify and study 91T-like SNe discovered from high-redshift surveys. Our sample consists of approximately 400 high-redshift SNe~Ia from the Pan-STARRS1 Medium Deep Survey (PS1-MDS). We spectroscopically classified 16 91T-like SN candidates, further exploring their characteristics. We found that the decline rates of the light curves of 91T-like SNe tend to be slower than those of normal SNe Ia, consistent with their brighter luminosities. Their Hubble residuals also tend to be negative compared to that predicted from the cosmological model. The colors of 91T-like SNe do not show significant differences compared to normal SNe Ia, possibly due to the influence of dust in the galaxies. Regarding the host-galaxy mass, star formation rate, and specific star formation rate, we found that the host-galaxy mass of 91T-like SNe is not significantly different from that of normal SNe Ia. However, 91T-like SNe tend to appear in galaxies with higher star formation rates and specific star formation rates. Our results indicate that the high-redshift 91T-like SNe generally exhibit consistent properties with those from lower-redshift studies.

關鍵字(中)

★ 類1991T型超新星
★ 巡天計畫
★ 高紅移91T-like超新星

關鍵字(英)

★ SN 1991T-like
★ Pan-STARRS1 Medium Deep Survey(PS1-MDS)

論文目次

電子論文授權書
指導教授推薦書
口試委員審定書
中文摘要 i
英文摘要 ii
List of Figures v
List of Tables vii
第一章緒論 1
1.1 la型超新星 2
1.2 SN 1991T-like超新星3
第二章目標篩選 7
2.1 Pan-STARRS 7
2.2 目標篩選 8
2.2.1 SN 1991T-like的光譜特色 9
2.2.2 DASH (Deep Automated Supernova and Host classifier) 10
2.2.3 Pseudo-equivalent widths (pEW) 12
第三章篩選結果與比較 15
3.1 篩選結果 15
3.2 各特性的比較 16
3.2.1 光度曲線下降率 17
3.2.2 顔色 18
3.2.3 Hubble Residual 22
3.2.4 宿主星系的質量 22
3.2.5 宿主星系的恆星形成率 25
3.2.6 宿主星系的specific恆星形成率 25
第四章討論 29
4.1 各特性的討論 29
4.1.1 光度曲線下降率 29
4.1.2 顏色 30
4.1.3 Hubble Residual 30
4.1.4 宿主星系的質量 30
4.1.5 宿主星系的恆星形成率以及specific恆星形成率 31
第五章結論 33
參考文獻 35
附錄一 37
附錄二 43

參考文獻

參考文獻
Blondin S., Tonry J. L., 2007, The Astrophysical Journal, 666, 1024
Branch D., Baron E., Jeffery D. J., 2001, Optical Spectra of Supernovae
(arXiv:astro-ph/0111573)
Colgate S. A., McKee C., 1969, ApJ, 157, 623
Filippenko A. V., 1997, ARA&A, 35, 309
Hakobyan A. A., Barkhudaryan L. V., Karapetyan A. G., Gevorgyan M. H., Mamon G. A., Kunth D., Adibekyan V., Turatto M., 2020, Monthly Notices of the Royal Astronomical Society, 499, 1424-1440
Hamuy M., Trager S. C., Pinto P. A., Phillips M. M., Schommer R. A., Ivanov V., Suntzeff N. B., 2000, The Astronomical Journal, 120, 1479
Howell D. A., 2001, The Astrophysical Journal, 554, L193-L196
Huterer D., Turner M. S., 1999, Phys. Rev. D, 60, 081301
Kessler R., et al., 2009, The Astrophysical Journal Supplement Series, 185, 32
Li W., Filippenko A. V., Treffers R. R., Riess A. G., Hu J., Qiu Y., 2001, The Astrophysical Journal, 546, 734
Liu Y., Modjaz M., 2015, SuperNova IDentification spectral templates of 70 stripped-envelope core-collapse supernovae (arXiv: 1405. 1437)
Liu Y.-Q., Modjaz M., Bianco F. B., Graur O., 2016, The Astrophysical Journal, 827, 90
Minkowski R., 1941, PASP, 53, 224
Muthukrishna D., Parkinson D., Tucker B. E., 2019, The Astrophysical Journal, 885, 85
O′Brien J. T., et al., 2024, ApJ, 964, 137
Phillips M. M., 1993, ApJ, 413, L105
Phillips M. M., et al., 2022, ApJ, 938, 47
Riess A. G., et al., 1998, The Astronomical Journal, 116, 1009
Riess A. G., et al., 2007, The Astrophysical Journal, 659, 98
Scolnic D. M., et al., 2018b, The Astrophysical Journal, 859, 101
Scolnic D. M., et al., 2018a, ApJ, 859, 101
Silverman J. M., et al., 2012, Monthly Notices of the Royal Astronomical Society, 425, 1789
Spyromilio J., Meikle W. P. S., Allen D. A., Graham J. R., 1992, MNRAS, 258, 53P
Vink J., 2004. https://api.semanticscholar.org/CorpusID:118388878
Wheeler J. C., Harkness R. P., 1990, Reports on Progress in Physics, 53, 1467
Yang J., et al., 2022, The Astrophysical Journal, 938, 83
Zeng et al P., 2024

指導教授

潘彥丞(Yen-Chen Pan)

審核日期

2024-5-17

推文