DustPedia: A Definitive Study of Cosmic Dust in the Local Universe
DustPedia: A Definitive Study of Cosmic Dust in the Local Universe
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DOI：
10.1088/1538-3873/129/974/044102
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发表时间：
2016-09
影响因子：
3.5
通讯作者：
J. Davies;M. Baes;S. Bianchi;A. Jones;S. Madden;M. Xilouris;M. Bocchio-;V. Casasola;L. Cassara';C. Clark;I. D. Looze;R. Evans;J. Fritz;M. Galametz;F. Galliano;S. Lianou;A. Mosenkov;M. Smith;S. Verstocken;S. Viaene;M. Vika;G. Wagle;N. Ysard
中科院分区：
文献类型：
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作者：
J. Davies;M. Baes;S. Bianchi;A. Jones;S. Madden;M. Xilouris;M. Bocchio-;V. Casasola;L. Cassara';C. Clark;I. D. Looze;R. Evans;J. Fritz;M. Galametz;F. Galliano;S. Lianou;A. Mosenkov;M. Smith;S. Verstocken;S. Viaene;M. Vika;G. Wagle;N. Ysard
欧洲航天局在两个基石任务上投入了大量资金：赫歇尔和普朗克。这些任务的遗留数据为研究星系中的宇宙尘埃提供了前所未有的机会，例如，我们可以回答有关化学元素的起源、星际介质中的物理过程、星际介质对恒星辐射的影响、星际介质与星星形成的关系以及星际介质与宇宙远红外背景的关系等基本问题。在本文中，我们描述了DustPedia项目，该项目使我们能够开发工具和计算机模型，帮助我们将观测到的宇宙尘埃排放与其物理性质（化学成分，尺寸分布和温度），其起源（演化的恒星，超新星和ISM中的生长）以及摧毁它的过程（高能碰撞和冲击加热气体）联系起来。为了进行这项研究，我们将联合收割机的赫歇尔/普朗克数据与来自其他数据源的数据相结合，并在光谱能量分布上提供许多波长（≤ 41）的观测结果，从而创建了DustPedia数据库。为了最大限度地提高我们的空间分辨率和对宇宙尘埃的敏感度，我们将我们的分析限制在4231个通过近红外光度（恒星质量）选择的本地星系（v < 3000 km s−1）。为了帮助我们解释这些数据，我们开发了一种新的尘埃物理模型（THEMIS），一种新的贝叶斯拟合和解释光谱能量分布的方法（HerBIE）和一种最先进的蒙特卡罗光子跟踪辐射传输模型（SKIRT）。在这篇DustPedia论文的第一篇中，我们描述了项目目标，使用的数据集，并提供了对我们计划实施的新科学方法的见解。
The European Space Agency has invested heavily in two cornerstones missions: Herschel and Planck. The legacy data from these missions provides an unprecedented opportunity to study cosmic dust in galaxies so that we can, for example, answer fundamental questions about the origin of the chemical elements, physical processes in the interstellar medium (ISM), its effect on stellar radiation, its relation to star formation and how this relates to the cosmic far-infrared background. In this paper we describe the DustPedia project, which enables us to develop tools and computer models that will help us relate observed cosmic dust emission to its physical properties (chemical composition, size distribution, and temperature), its origins (evolved stars, supernovae, and growth in the ISM), and the processes that destroy it (high-energy collisions and shock heated gas). To carry out this research, we combine the Herschel/Planck data with that from other sources of data, and provide observations at numerous wavelengths ( ≤ 41 ) across the spectral energy distribution, thus creating the DustPedia database. To maximize our spatial resolution and sensitivity to cosmic dust, we limit our analysis to 4231 local galaxies ( v < 3000 km s−1) selected via their near-infrared luminosity (stellar mass). To help us interpret this data, we developed a new physical model for dust (THEMIS), a new Bayesian method of fitting and interpreting spectral energy distributions (HerBIE) and a state-of-the-art Monte Carlo photon-tracing radiative transfer model (SKIRT). In this, the first of the DustPedia papers, we describe the project objectives, data sets used, and provide an insight into the new scientific methods we plan to implement.