SN 2012ec: mass of the progenitor from PESSTO follow-up of the photospheric phase
SN 2012ec: mass of the progenitor from PESSTO follow-up of the photospheric phase
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DOI：
10.1093/mnras/stv106
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发表时间：
2014-10
影响因子：
4.8
通讯作者：
C. Barbarino;M. Dall’ora;M. Botticella;M. Valle;L. Zampieri;J. Maund;M. L. Pumo;A. Jerkstrand;S. Benetti;N. Elias-Rosa;M. Fraser;A. Gal-yam;M. Hamuy;M. Hamuy;C. Inserra;C. Knapic;A. Lacluyze;M. Molinaro;P. Ochner;A. Pastorello;G. Pignata;D. Reichart;C. Ries;A. Riffeser;B. Schmidt;M. Schmidt;R. Smareglia;S. Smartt;K. Smith;J. Sollerman;M. Sullivan;L. Tomasella;M. Turatto;S. Valenti;O. Yaron;D. Young
中科院分区：
文献类型：
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作者：
C. Barbarino;M. Dall’ora;M. Botticella;M. Valle;L. Zampieri;J. Maund;M. L. Pumo;A. Jerkstrand;S. Benetti;N. Elias-Rosa;M. Fraser;A. Gal-yam;M. Hamuy;M. Hamuy;C. Inserra;C. Knapic;A. Lacluyze;M. Molinaro;P. Ochner;A. Pastorello;G. Pignata;D. Reichart;C. Ries;A. Riffeser;B. Schmidt;M. Schmidt;R. Smareglia;S. Smartt;K. Smith;J. Sollerman;M. Sullivan;L. Tomasella;M. Turatto;S. Valenti;O. Yaron;D. Young
我们提出了SN 2012 ec的光度和光谱监测活动的结果，它在螺旋星系NGC 1084中爆炸，在光球阶段。光度光变曲线呈现出一个光度L = 0.9 × 1042 erg s−1的平台，持续时间约为90 d，比标准的II-P型超新星（SNe）稍短。根据光变曲线放射性尾开始时的光度，我们估计镍的质量M（56 Ni）= 0.040 ± 0.015 M <$。SN 2012 ec的爆炸参数估计的比较测辐射热的光变曲线和观测到的温度和速度演变的喷出物与流体动力学模型的预测。我们导出了包封质量为12.6M·cm-1，初始母源半径为1.6 × 10 ~（13）cm，爆炸能量为1.2foe。这些估计与一项独立的研究一致，该研究对爆炸前图像中发现的原始星星进行了研究，确定其初始质量为M = 14-22 M。我们对另外两个II-P型SNe（SNe 2012 aw和2012 A）进行了同样的分析，并与本文推导的SN 2012 ec的性质进行了比较。我们发现一个合理的协议从爆炸前的图像和来自流体动力学模型的群众的祖细胞之间的群众。我们用标准蜡烛法（SCM）估计了SN 2012 ec的距离，并将其与基于其他主要和次要指标的其他估计进行了比较。SNe 2012 A、2012 aw和2012 ec都遵循SCM的标准关系，使用II-P型SNe作为距离指示器。
We present the results of a photometric and spectroscopic monitoring campaign of SN 2012ec, which exploded in the spiral galaxy NGC 1084, during the photospheric phase. The photometric light curve exhibits a plateau with luminosity L = 0.9 × 1042 erg s−1 and duration ∼90 d, which is somewhat shorter than standard Type II-P supernovae (SNe). We estimate the nickel mass M(56Ni) = 0.040 ± 0.015 M⊙ from the luminosity at the beginning of the radioactive tail of the light curve. The explosion parameters of SN 2012ec were estimated from the comparison of the bolometric light curve and the observed temperature and velocity evolution of the ejecta with predictions from hydrodynamical models. We derived an envelope mass of 12.6 M⊙, an initial progenitor radius of 1.6 × 1013 cm and an explosion energy of 1.2 foe. These estimates agree with an independent study of the progenitor star identified in pre-explosion images, for which an initial mass of M = 14-22 M⊙ was determined. We have applied the same analysis to two other Type II-P SNe (SNe 2012aw and 2012A), and carried out a comparison with the properties of SN 2012ec derived in this paper. We find a reasonable agreement between the masses of the progenitors obtained from pre-explosion images and masses derived from hydrodynamical models. We estimate the distance to SN 2012ec with the standardized candle method (SCM) and compare it with other estimates based on other primary and secondary indicators. SNe 2012A, 2012aw and 2012ec all follow the standard relations for the SCM for the use of Type II-P SNe as distance indicators.