局域HRS星系样本的二元光度和质量函数。恒星、尘埃、气体的质量
The bivariate luminosity and mass functions of the local HRS galaxy sample. The stellar, dust, gas mass functions
摘要：
通过计算Herschel参考巡天（HRS）的二元K波段光度函数（BLF）和二元K波段质量函数（BMF），讨论了K波段与恒星质量、远红外光度、恒星形成率、尘埃和邻近星系气体质量之间的关系。我们推导出的BLF和BMF的K-波段和恒星质量，远红外光度，恒星形成率，尘埃和气体质量的累积分布，使用copula方法，详细概述。使用考虑上限的双变量计算使我们能够在更坚实的统计基础上推导出观测到的物理量之间的关系。分析表明，形态（光学选择）子样本的行为是完全不同的。只有从K波段与恒星质量的关系中才能得到对整个HRS样本有统计意义的结果，而对于其余的物理量（尘埃和气体质量、远红外光度和恒星形成率），晚型星系（LT）和早型星系（ETG）的分析是不同的。然而，ETG的数量很少，无法进行稳健的统计分析，并且在大多数情况下，仅讨论了LTG子样本的结果。LTG的亮度和质量函数（LFs，MFs）通常依赖于K带，并详细讨论了各种依赖关系。我们能够推导出相应的LF和MF，并将其与其他样本计算的LF和MF进行比较。我们的统计分析使我们能够重新计算HRS，虽然非均匀选择和部分偏向于低红外光度，可以被认为是当地LT星系人口的代表。
英文摘要：
We discuss the results of the relationships between the K-band and stellar mass, far-infrared luminosities, star formation rate, dust and gas masses of nearby galaxies computing the bivariate K-band Luminosity Function (BLF) and bivariate K-band Mass Function (BMF) of the Herschel Reference Survey (HRS), a volume-limited sample with full wavelength coverage. We derive the BLFs and BMFs from the K-band and stellar mass, far-infrared luminosities, star formation rate, dust and gas masses cumulative distributions using a copula method which is outlined in detail. The use of the bivariate computed taking into account the upper limits allows us to derive on a more solid statistical ground the relationship between the observed physical quantities. The analysis shows that the behaviour of the morphological (optically selected) subsamples is quite different. A statistically meaningful result can be obtained over the whole HRS sample only from the relationship between the K-band and the stellar mass, while for the remaining physical quantities (dust and gas masses, far-IR luminosity and star formation rate), the analysis is distinct for late-type (LT) and early-type galaxies (ETG). However, the number of ETGs is small to perform a robust statistical analysis, and in most of the case results are discussed only for the LTG subsample. The Luminosity and Mass Functions (LFs, MFs) of LTGs are generally dependent on the K-band and the various dependencies are discussed in detail. We are able to derive the corresponding LFs and MFs and compare them with those computed with other samples. Our statistical analysis allows us to characterise the HRS, that, although non homogeneously selected and partially biased towards low IR luminosities, may be considered as representative of the local LT galaxy population.
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