标题： 佩加索斯.3：一个用于模拟星系从紫外到红外/亚毫米波段光谱和化学演化的尘埃代码 显示英文标题

标题： Pégase.3: A code for modeling the UV-to-IR/submm spectral and chemical evolution of galaxies with dust

摘要： 需要一个能够一致地计算恒星、气体和尘埃演化及其辐射能量的代码，以便通过拟合合成的 SED 到多波段观测来可靠地推导星系的历史。 本文介绍的新代码 Pégase.3 将先前版本提供的 UV 至近红外建模扩展到了远红外/亚毫米波段。 它首先计算不同金属丰度下单个恒星群体的属性。 然后跟踪星系恒星光度和星际介质中主要金属元素丰度随时间的变化，假设某种质量组装和恒星形成情景。 同时使用考虑散射的蒙特卡洛模拟预先计算的辐射传输网格，计算各种颗粒族的质量、星系的光学深度以及旋涡和球状星系中弥散星际介质对 SED 的吸收。 该代码确定平均辐射场和随机加热单颗颗粒的温度概率分布。 然后将其光谱相加，以得出弥散星际介质中的尘埃整体发射。 还计算星系的星云发射，并实现了一个简单的模型来描述尘埃对恒星形成区域 SED 的影响。 主要输出包括从星系诞生到 20 Gyr 的 UV 至亚毫米波段 SED、颜色、星系组分质量、星际介质中金属元素和尘埃物种的丰度以及超新星率。 单颗颗粒的温度和光谱也可用。 本文讨论了这一代表性银河系螺旋结构场景的一些这些输出。 Pégase.3 完全有文档记录，其 Fortran 95 源文件公开。 该代码对于宇宙学模拟和解释未来的中远红外数据（无论是 JWST、LSST、Euclid 还是 e-ELT 获得的）应该会特别有用。 显示英文摘要

摘要： A code computing consistently the evolution of stars, gas and dust, as well as the energy they radiate, is required to derive reliably the history of galaxies by fitting synthetic SEDs to multiwavelength observations. The new code P\'egase.3 described in this paper extends to the far-IR/submm the UV-to-near-IR modeling provided by previous versions of P\'egase. It first computes the properties of single stellar populations at various metallicities. It then follows the evolution of the stellar light of a galaxy and the abundances of the main metals in the ISM, assuming some scenario of mass assembly and star formation. It simultaneously calculates the masses of the various grain families, the optical depth of the galaxy and the attenuation of the SED through the diffuse ISM in spiral and spheroidal galaxies, using grids of radiative transfer precomputed with Monte Carlo simulations taking scattering into account. The code determines the mean radiation field and the temperature probability distribution of stochastically heated individual grains. It then sums up their spectra to yield the overall emission by dust in the diffuse ISM. The nebular emission of the galaxy is also computed, and a simple modeling of the effects of dust on the SED of star-forming regions is implemented. The main outputs are UV-to-submm SEDs of galaxies from their birth up to 20 Gyr, colors, masses of galactic components, ISM abundances of metallic elements and dust species, supernova rates. The temperatures and spectra of individual grains are also available. The paper discusses several of these outputs for a scenario representative of Milky Way-like spirals. P\'egase.3 is fully documented and its Fortran 95 source files are public. The code should be especially useful for cosmological simulations and to interpret future mid- and far-IR data, whether obtained by JWST, LSST, Euclid or e-ELT.