来自普朗克巡天的（亚）毫米波波段星系的局部光度函数
Local luminosity functions of galaxies at (sub)millimeter wavelengths from Planck surveys
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中文总结 AI 辅助
该研究利用第二代普朗克致密源目录数据，通过经典1/Vmax和非参数核密度估计方法，重新估计（亚）毫米波波段星系的局部光度函数，获得多个波段的函数及总红外光度函数、尘埃质量函数，发现与早期估计有显著差异。
中文摘要 AI 辅助
普朗克全天空（亚）毫米波巡天使我们能够精确确定直至最高光度的相应局部光度函数。探测到的星系严格局限于本地，因此在这些波长下已知特别强烈的演化效应不是问题。然而，此前研究仅依赖普朗克早期发布致密源目录（ERCSC）。相较于早期估计的另一重要改进是有数百兆秒差距内星系的全天空完整目录，其为附近物体提供与红移无关的距离，因为红移并非可靠的距离估计器。本文利用第二代普朗克致密源目录数据重新估计（亚）毫米波局部光度函数，该目录取代了之前使用的ERCSC，包含更多源和更精确测光。我们用经典的1/Vmax和非参数核密度估计（KDE）方法计算光度函数，KDE实现采用1/Vmax加权以考虑巡天选择效应。我们获得了基于普朗克的857、545、353和217GHz的局部光度函数，以及总红外光度函数和尘埃质量函数。我们发现与早期估计有显著差异并讨论了其可能来源。
英文摘要
The Planck all-sky surveys at (sub)millimeter wavelengths enable us to accurately determine the corresponding local luminosity functions up to the highest luminosities. The detected galaxies are strictly local, so evolutionary effects, which are known to be particularly strong at these wavelengths, are not a problem. However, previous studies have so far relied only on the Planck Early Release Compact Source Catalog (ERCSC) for this purpose. Another important improvement over earlier estimates is the availability of complete all-sky catalogs of galaxies within hundreds of megaparsecs, with redshift-independent distances for nearby objects, for which redshifts are not reliable distance estimators. In this paper we re-estimate the (sub)millimeter local luminosity functions using data from the Second Planck Catalog of Compact Sources, which supersedes the previously used ERCSC and contains far more sources and more accurate photometry. We computed the luminosity functions using both the classical $1/V_{\rm max}$ and the nonparametric kernel density estimation (KDE) method, which overcomes limitations of binning techniques. Our implementation of the KDE uses the $1/V_{\max}$ weighting to account for survey selection effects. We obtain Planck-based local luminosity functions at 857, 545, 353, and 217 GHz, as well as the total IR luminosity function and the dust mass function. We find significant differences from earlier estimates and discuss their possible origins.
