Title: Nearby supernova host galaxies from the CALIFA Survey: I. Sample, data analysis, and correlation to star-forming regions Show Chinese title

Title: 来自CALIFA巡天的近邻超新星宿主星系：I. 样本、数据分析以及与恒星形成区域的相关性

Abstract: [Abridged] We use optical IFS of nearby SN host galaxies provided by the CALIFA Survey with the goal of finding correlations in the environmental parameters at the location of different SN types. We recover the sequence in association of different SN types to the star-forming regions by using several indicators of the ongoing and recent SF related to both the ionized gas and the stellar populations. While the total ongoing SF is on average the same for the three SN types, SNe Ibc/IIb tend to happen closer to star-forming regions and occur in higher SF density locations compared to SNe II and SNe~Ia, the latter showing the weakest correlation. SNe~Ia host galaxies have on average masses that are $\sim$0.3-0.8~dex higher than CC SNe hosts due to a larger fraction of old stellar populations in the SNe~Ia hosts. Using the recent SN~Ia delay-time distribution and the SFHs of the galaxies, we show that the SN~Ia hosts in our sample should presently produce a factor 2 more SNe~Ia than the CC~SN hosts. Since both types are in hosts with similar SF rate and hence similar CC~SN rate, this can explain the mass difference between the SN~Ia and CC~SN hosts, and reinforce the finding that at least part of SNe~Ia should originate from very old progenitors. Comparing the mean SFH of the eight least massive galaxies to that of the massive SF SN~Ia hosts we find that the low-mass galaxies formed their stars over more extended time than the massive SN~Ia hosts. We estimate that the low-mass galaxies should produce by a factor of 10 less SNe~Ia, and a factor of 3 less CC~SNe than the high-mass group. Therefore the ratio between the number of CC~SNe and SNe~Ia is expected to increase with decreasing the galaxy mass. CC~SNe tend to explode at positions with younger stellar populations than the galaxy average, but the galaxy properties at SNe~Ia locations are one average the same as the global ones. Show Chinese abstract

Abstract: [摘要] 我们利用 CALIFA 巡天提供的附近超新星（SN）宿主星系的光学积分场单元光谱（IFS），旨在寻找不同超新星类型所在位置环境参数的相关性。通过使用与电离气体和恒星群体相关的多个当前及近期恒星形成（SF）指标，我们恢复了不同类型超新星与恒星形成区域之间的关联序列。 虽然三种超新星类型的总当前恒星形成率大致相同，但 Ibc/IIb 型超新星倾向于发生在更靠近恒星形成区域的位置，并且出现在更高的恒星形成密度区域，而 II 型和 Ia 型超新星则表现出较弱的相关性，其中 Ia 型超新星显示出了最弱的关联。 由于 Ia 型超新星宿主星系中老年恒星群体的比例更大，因此其平均质量比核心坍缩（CC）超新星宿主星系高出$\sim$0.3-0.8 dex。结合最新的 Ia 型超新星延迟时间分布和星系的恒星形成历史（SFH），我们表明样本中的 Ia 型超新星宿主星系目前产生的 Ia 型超新星数量应是 CC 型超新星宿主星系的两倍。由于两种类型超新星均位于具有相似恒星形成率的宿主星系中，这可以解释 Ia 型与 CC 型超新星宿主星系的质量差异，并进一步支持至少部分 Ia 型超新星应源自非常古老的前身星的观点。 将八颗最低质量星系的平均恒星形成历史与高质星 Ia 型超新星宿主星系进行比较后发现，低质量星系的恒星形成时间跨度大于高质星 Ia 型超新星宿主星系。我们估计低质量星系产生的 Ia 型超新星数量比高质星组少 10 倍，CC 型超新星数量少 3 倍。因此，随着星系质量的降低，CC 型与 Ia 型超新星的数量比预计会增加。 CC 型超新星倾向于在比星系平均年龄更年轻的恒星群体位置爆炸，但 Ia 型超新星所在位置的星系属性总体上与全局属性一致。