超新星宿主星系的星族分析
发布时间：2018-08-09 16:47
【摘要】：超新星爆发是宇宙最激烈的天体物理现象之一，是某些恒星演化到生命的最后阶段的爆发性的终结，释放出大量的物质和极高的能量。超新星依据其光谱中有无氢线，分为II型和I型，没有氢线的I型又分为Ia、Ib和Ic。超新星的宿主星系，也就是超新星的爆发环境，对超新星的爆发有重要的影响，已经有很多工作研究了不同金属丰度、不同年龄的宿主星系中超新星爆发的类型及特征等。 PrantzosBoissier（2003）和BoissierPrantzos（2009）曾研究发现超新星Ibc与II的数目比值随宿主星系金属丰度的增加而增大，并认为其结果与有旋转的大质量星的演化模型相一致； Preito et al.（2008）通过直接测定超新星宿主星系整体的金属丰度，发现超新星Ibc的宿主星系比Ia和II的显示出更高的金属丰度；Hammuy etal.（1996）发现内禀暗的事件发生在早型星系中，而亮的事件发生在晚型的宿主星系中； Gallagher et al.（2008）认为发生在年龄较老星系中的超新星Ia的峰值光度比更年轻星系中的超新星Ia暗约一个星等，即更暗的超新星Ia发生在更老星族的星系中；Sullivan et al.（2006）Aubourg et al.（2008）发现超新星Ia宿主星系中短寿命前身星星族的证据，对超新星Ia的前身星质量范围给出了一定的限制。虽然已经有这些研究结果，但他们基于的样本一般都比较小，特别是还没有对SN Ia、II、Ib/c几种不同类型超新星宿主星系的星族进行详细比较的工作，而星族是表征超新星爆发环境的一个非常重要的直接参量，因此我们将SDSS主星系表与Asiago超新星表进行交叉，选出234个不同类型超新星及其宿主星系，详细分析了他们的星族成分。 我们利用30arcsec的交叉半径，对SDSS主星系表和Asiago超新星表中宿主星系的坐标进行了交叉，将得到的1201个样本，随后又以light-fraction0.15为衡量标准进一步取了一个次样本，其3角秒的fiber观测光谱能较好的表征星系整体光的性质。之后更进一步检查了样本的图像和光谱观测，最终得到234个星系，分为两类进行研究分析：137个发射线星系和97个吸收线星系。 对这两类星系，我们用STARLIGHT拟合了连续谱和吸收线，得到了他们不同年龄和不同金属丰度的星族成分，并从MPA/JHU数据库中得到Dn (4000)、H A、恒星质量、恒星形成率等特征参量，对超新星Ia、II、Ib/c三种类型超新星宿主星系的特征结果进行了比较分析。然后，对于137个发射线星系，又利用MPA/JHU团组提供的H和H的等值宽度，计算了星系中年轻星族的年龄。通过分析我们发现： 对于发射线星系样本，1）SN II宿主星系的年轻星族成分贡献最大，表明他们比SN Ia和Ib/c宿主星系更年轻，SN Ia宿主星系比SN Ib/c宿主星系稍微年轻一点；2）SN II宿主星系的富金属星族成分贡献最少，SN Ib/c宿主星系的富金属星族成分贡献最大，SN Ia位于二者之间，，表明SN Ib/c比SN II爆发在相对更加富金属的环境中；3）通过Hα和Hβ发射线等值宽度估计出的宿主星系年轻星族的年龄，给出了超新星爆发环境的年龄下限；4）SN Ia倾向于爆发在大质量的星系内，SN II爆发在大质量和中小质量的星系内。 对于吸收线星系样本，1）SN Ia宿主星系的年轻星族成分贡献最小，老年星族成分贡献最大，表明他们比SN Ib/c和II宿主星系更年老；2）SN Ia宿主星系的富金属星族成分贡献最大，表明其爆发在相对富金属的环境中。 对比发射线星系和吸收线星系，1）对同种类型超新星，发射线宿主星系的年轻星族成分更多，比吸收线宿主星系更年轻；2）对同种类型超新星，吸收线宿主星系比发射线宿主星系更加富金属；3）吸收线宿主星系的恒星质量相对较大，恒星形成率相对较低。
[Abstract]:The supernova eruption is one of the most intense astrophysical phenomena in the universe. It is the explosive end of the last stage of the evolution of some stars to life. It releases a lot of material and high energy. Supernova is divided into II and I based on its hydrogen free line in its spectrum. The I type without hydrogen line is also divided into host galaxies of Ia, Ib and Ic. supernova, too. The outbreak of supernova has an important impact on the outbreaks of supernovae. Many work has been done to study the types and characteristics of supernova eruptions in host galaxies of different metallicity and age.
PrantzosBoissier (2003) and BoissierPrantzos (2009) have found that the ratio of the number of supernova Ibc to II increases with the increase in the metallicity of the host star system, and considers that the result is in accordance with the evolution model of the large mass star with rotation; Preito et al. (2008) detected the metallicity of the whole supernova host galaxy by direct connection. The host galaxies of supernova Ibc showed higher metallicity than Ia and II; Hammuy etal. (1996) found that the intrinsic dark events occurred in the early type galaxies, and the bright events occurred in the late type host galaxy; Gallagher et al. (2008) believed that the peak luminosity of the supernova Ia in the older stars was younger than the younger galaxy. The supernova Ia is dark about one star, that is, the darker supernova Ia occurs in the older star galaxy; Sullivan et al. (2006) Aubourg et al. (2008) finds the evidence of the short life precursor star in the supernova Ia host galaxy, which limits the mass range of supernova Ia's precursor. Although these results have been found, However, the samples they are based on are generally relatively small, especially for the SN Ia, II, Ib/c and different types of supernova host galaxies in detail, and the star family is a very important direct parameter to characterize the supernova environment, so we cross the SDSS star table with the Asiago supernova table. Two hundred and thirty-four different types of supernovae and their host galaxies were analyzed in detail.
Using the cross radius of 30arcsec, we cross the coordinates of the host galaxy table of SDSS and the host galaxy in the Asiago supernova table. 1201 samples are obtained, and then a sub sample is taken by light-fraction0.15 as a measure. The fiber view spectrum of the 3 corner seconds can better characterize the properties of the whole galaxy light. Further examination of the image and spectral observations of the samples, and finally get 234 galaxies, divided into two types of research and analysis: 137 emitter galaxies and 97 absorption line galaxies.
For these two types of galaxies, we use STARLIGHT to fit the continuous spectrum and absorption line, get their different age and different metallicity, and get Dn (4000), H A, stellar mass and star formation rate from the MPA/JHU database, and carry out the characteristics of the supernova Ia, II, Ib/c, three types of supernova host galaxies. Then, for 137 emission line galaxies, we use the equivalent widths of H and H provided by the group of MPA/JHU groups to calculate the age of the middle age light stars in the galaxy.
For the emission line Galaxy samples, 1) the young star composition of the SN II host galaxy contributes the most, indicating that they are younger than the SN Ia and Ib/c host stars, and the SN Ia host galaxy is a little younger than the SN Ib/c host star system; and the SN II host galaxy has the least contribution to the rich metallic star component, and the rich metallic star component of the SN main star system contributes the most. Large, SN Ia is between two, indicating that SN Ib/c outbreaks in a relatively more metal rich environment than SN II; 3) the age of the young star family of the host galaxy estimated by the H alpha and H beta emission line equal width, gives the age limit of the supernova explosion environment; 4) SN Ia tends to explode in mass galaxies, SN II erupts in mass and Small and medium galaxies.
For the sample of the absorption line galaxies, 1) the young star composition of the SN Ia host galaxy has the smallest contribution to the young star family component, and the older star composition contributes most, indicating that they are older than the SN Ib/c and the II host galaxies; 2) the rich metallic star component of the SN Ia host galaxy contributes the most, indicating that its eruption is in the relatively metal rich environment.
Compared with the emitter and absorption line galaxies, 1) for the same type supernova, the young star family of the host galaxy is more, younger than the absorption line host star system; 2) for the same type supernova, the absorption line host star system is more metal than the ray host galaxy; 3) the star mass of the absorption line host galaxy is relatively large, and the star is relatively large. The formation rate is relatively low.
【学位授予单位】：河北师范大学
【学位级别】：硕士
【学位授予年份】：2012
【分类号】：P152
[Abstract]:The supernova eruption is one of the most intense astrophysical phenomena in the universe. It is the explosive end of the last stage of the evolution of some stars to life. It releases a lot of material and high energy. Supernova is divided into II and I based on its hydrogen free line in its spectrum. The I type without hydrogen line is also divided into host galaxies of Ia, Ib and Ic. supernova, too. The outbreak of supernova has an important impact on the outbreaks of supernovae. Many work has been done to study the types and characteristics of supernova eruptions in host galaxies of different metallicity and age.
PrantzosBoissier (2003) and BoissierPrantzos (2009) have found that the ratio of the number of supernova Ibc to II increases with the increase in the metallicity of the host star system, and considers that the result is in accordance with the evolution model of the large mass star with rotation; Preito et al. (2008) detected the metallicity of the whole supernova host galaxy by direct connection. The host galaxies of supernova Ibc showed higher metallicity than Ia and II; Hammuy etal. (1996) found that the intrinsic dark events occurred in the early type galaxies, and the bright events occurred in the late type host galaxy; Gallagher et al. (2008) believed that the peak luminosity of the supernova Ia in the older stars was younger than the younger galaxy. The supernova Ia is dark about one star, that is, the darker supernova Ia occurs in the older star galaxy; Sullivan et al. (2006) Aubourg et al. (2008) finds the evidence of the short life precursor star in the supernova Ia host galaxy, which limits the mass range of supernova Ia's precursor. Although these results have been found, However, the samples they are based on are generally relatively small, especially for the SN Ia, II, Ib/c and different types of supernova host galaxies in detail, and the star family is a very important direct parameter to characterize the supernova environment, so we cross the SDSS star table with the Asiago supernova table. Two hundred and thirty-four different types of supernovae and their host galaxies were analyzed in detail.
Using the cross radius of 30arcsec, we cross the coordinates of the host galaxy table of SDSS and the host galaxy in the Asiago supernova table. 1201 samples are obtained, and then a sub sample is taken by light-fraction0.15 as a measure. The fiber view spectrum of the 3 corner seconds can better characterize the properties of the whole galaxy light. Further examination of the image and spectral observations of the samples, and finally get 234 galaxies, divided into two types of research and analysis: 137 emitter galaxies and 97 absorption line galaxies.
For these two types of galaxies, we use STARLIGHT to fit the continuous spectrum and absorption line, get their different age and different metallicity, and get Dn (4000), H A, stellar mass and star formation rate from the MPA/JHU database, and carry out the characteristics of the supernova Ia, II, Ib/c, three types of supernova host galaxies. Then, for 137 emission line galaxies, we use the equivalent widths of H and H provided by the group of MPA/JHU groups to calculate the age of the middle age light stars in the galaxy.
For the emission line Galaxy samples, 1) the young star composition of the SN II host galaxy contributes the most, indicating that they are younger than the SN Ia and Ib/c host stars, and the SN Ia host galaxy is a little younger than the SN Ib/c host star system; and the SN II host galaxy has the least contribution to the rich metallic star component, and the rich metallic star component of the SN main star system contributes the most. Large, SN Ia is between two, indicating that SN Ib/c outbreaks in a relatively more metal rich environment than SN II; 3) the age of the young star family of the host galaxy estimated by the H alpha and H beta emission line equal width, gives the age limit of the supernova explosion environment; 4) SN Ia tends to explode in mass galaxies, SN II erupts in mass and Small and medium galaxies.
For the sample of the absorption line galaxies, 1) the young star composition of the SN Ia host galaxy has the smallest contribution to the young star family component, and the older star composition contributes most, indicating that they are older than the SN Ib/c and the II host galaxies; 2) the rich metallic star component of the SN Ia host galaxy contributes the most, indicating that its eruption is in the relatively metal rich environment.
Compared with the emitter and absorption line galaxies, 1) for the same type supernova, the young star family of the host galaxy is more, younger than the absorption line host star system; 2) for the same type supernova, the absorption line host star system is more metal than the ray host galaxy; 3) the star mass of the absorption line host galaxy is relatively large, and the star is relatively large. The formation rate is relatively low.
【学位授予单位】：河北师范大学
【学位级别】：硕士
【学位授予年份】：2012
【分类号】：P152
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