论文标题
对局部超湿红外星系的新看：其复杂物理的地图集和辐射转移模型
A new look at local ultraluminous infrared galaxies: the atlas and radiative transfer models of their complex physics
论文作者
论文摘要
我们将Herschel Ultra Puminous红外星系调查（HERUS）样本的紫外线介绍到亚毫米光谱能量分布（SED），这些样本是42个本地超浮标的红外星系（ULIRGS），并使用Markov Chain Monte Carlo（MCMC）使用Cyprus模型（cyprus cynus）cyperrus radectriative starriat radectriative starriat ractriative starriative starriative starriative starriative starriative starriat radective cypliative cyplrus（MCMC）细胞核（AGN）Tori和宿主星系。 Spitzer IRS光谱数据包含在拟合中。我们的贝叶斯SED拟合方法与流行的能量平衡方法相当，但它具有更大的动力和多功能性。所有Herus星系都具有恒星形成的高速率，但我们也发现样品的所有星系中都具有横杆化显着的AGN。我们估计，由于圆环的各向异性发射，ulirgs中AGN的亮度校正了，发现几乎边缘的Tori可能会达到$ \ sim10 $。我们将结果与Fritz等人的平滑圆环模型进行了比较。以及Siebenmorgen等人的两相模型。和Skirtor。我们发现，与所有其他模型相比，Cygnus AGN圆环模型明显更好地拟合样品的SED。我们没有发现证据表明强大的AGN出现在Starburst发作的开始或结束时，或者Starburst和AGN相互影响。 IRAS 01003-2238和MRK 1014在其SED拟合中显示了双重AGN的证据，表明样品中最小双重AGN分数。
We present the ultraviolet to submillimetre spectral energy distributions (SEDs) of the HERschel Ultra Luminous Infrared Galaxy Survey (HERUS) sample of 42 local ultraluminous infrared galaxies (ULIRGs) and fit them with a Markov chain Monte Carlo (MCMC) code using the CYprus models for Galaxies and their NUclear Spectra (CYGNUS) radiative transfer models for starbursts, active galactic nucleus (AGN) tori and host galaxy. The Spitzer IRS spectroscopy data are included in the fitting. Our bayesian SED fitting method takes comparable time to popular energy balance methods but it is more physically motivated and versatile. All HERUS galaxies harbor high rates of star formation but we also find bolometrically significant AGN in all of the galaxies of the sample. We estimate the correction of the luminosities of the AGN in the ULIRGs due to the anisotropic emission of the torus and find that it could be up to a factor of $\sim10$ for nearly edge-on tori. We present a comparison of our results with the smooth torus model of Fritz et al. and the two-phase models of Siebenmorgen et al. and SKIRTOR. We find that the CYGNUS AGN torus models fit significantly better the SEDs of our sample compared to all other models. We find no evidence that strong AGN appear either at the beginning or end of a starburst episode or that starbursts and AGN affect each other. IRAS 01003-2238 and Mrk 1014 show evidence for dual AGN in their SED fits suggesting a minimum dual AGN fraction in the sample of 5%.
