資料載入中.....
|
請使用永久網址來引用或連結此文件:
https://ir.lib.ncu.edu.tw/handle/987654321/101432
|
| 題名: | The host galaxy and late-time evolution of the superluminous supernova PTF12dam |
| 作者: | 陳婷琬;Chen, T.-W.;Smartt, S. J.;Jerkstrand, A.;Nicholl, M.;Bresolin, F.;Kotak, R.;Polshaw, J.;Rest, A.;Kudritzki, R.;Zheng, Z.;Elias-Rosa, N.;Smith, K.;Inserra, C.;Wright, D.;Kankare, E.;Kangas, T.;Fraser, M. |
| 貢獻者: | 理學院天文研究所 |
| 關鍵詞: | Dwarf galaxies;Dwarf stars;Fading;Gamma ray astronomy;Light curve;Luminosity;Metallicity;Photometry;Spectrum analysis;Star & galaxy formation;Supernovae;Supernovas;Symbols |
| 日期: | 2015-02-11 |
| 上傳時間: | 2026-04-21 14:33:49 (UTC+8) |
| 出版者: | Oxford University Press;London: Oxford University Press (OUP) |
| 摘要: | 摘要： Superluminous supernovae (SLSNe) of Type Ic have a tendency to occur in faint host galaxies which are likely to have low mass and low metallicity. PTF12dam is one of the closest and best-studied superluminous explosions that has a broad and slowly fading light curve similar to SN 2007bi. Here we present new photometry and spectroscopy for PTF12dam from 200–500 d (rest frame) after peak and a detailed analysis of the host galaxy (SDSS J142446.21+461348.6 at z = 0.107). Using deep templates and image subtraction we show that the light curve can be fit with a magnetar model if escape of high-energy gamma rays is taken into account. The full bolometric light curve from −53 to +399 d (with respect to peak) cannot be fit satisfactorily with the pair-instability models. An alternative model of interaction with a dense circumstellar material (CSM) produces a good fit to the data although this requires a very large mass (∼13 M⊙) of hydrogen-free CSM. The host galaxy is a compact dwarf (physical size ∼1.9 kpc) and with M g = −19.33 ± 0.10, it is the brightest nearby SLSN Ic host discovered so far. The host is a low-mass system (2.8 × 108 M⊙) with a star formation rate (5.0 M⊙ yr−1), which implies a very high specific star formation rate (17.9 Gyr−1). The remarkably strong nebular emission provide detections of the [O iii] λ4363 and [O ii] λλ7320, 7330auroral lines and an accurate oxygen abundance of 12 + log (O/H) = 8.05 ± 0.09. We show here that they are at the extreme end of the metallicity distribution of dwarf galaxies and propose that low metallicity is a requirement to produce these rare and peculiar SNe.
出版者： London: Oxford University Press (OUP)
出版日期： 2015-09-11
出處： Monthly Notices of the Royal Astronomical Society, 2015-09, Vol.452 (2), p.1567-1586
資源來源： Alma/SFX Local Collection
版權： 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2015
版權： Copyright Oxford University Press, UK Sep 11, 2015
識別號： ISSN: 0035-8711
識別號： ISSN: 1365-8711
識別號： ISSN: 1365-2966
識別號： EISSN: 1365-2966
識別號： DOI: 10.1093/mnras/stv1360 |
| 顯示於類別: | [天文研究所] 期刊論文
|
文件中的檔案:
| 檔案 |
描述 |
大小 | 格式 | 瀏覽次數 |
|---|
| index.html | | 0Kb | HTML | 28 | 檢視/開啟 |
|
在NCUIR中所有的資料項目都受到原著作權保護.
|
