Fitting AGN/galaxy X-ray-to-radio SEDs with CIGALE and improvement of the code
Guang Yang, Médéric Boquien, William N. Brandt, Véronique Buat, Denis Burgarella, Laure Ciesla, Bret D. Lehmer, Katarzyna E. Małek, George Mountrichas, Casey Pa… 展开作者
Guang Yang, Médéric Boquien, William N. Brandt, Véronique Buat, Denis Burgarella, Laure Ciesla, Bret D. Lehmer, Katarzyna E. Małek, George Mountrichas, Casey Papovich, Estelle Pons, Marko Stalevski, Patrice Theulé, Shifu Zhu
Modern and future surveys effectively provide a panchromatic view for large numbers of extragalactic objects. Consistently modeling these multiwavelength survey data is a critical but challenging task for extragalactic studies. The Code Investigating GALaxy Emission (CIGALE) is an efficient PYTHON code for spectral energy distribution (SED) fitting of galaxies and active galactic nuclei (AGNs). Recently, a major extension of CIGALE (named X-CIGALE) has been developed to account for AGN/galaxy X-ray emission and improve AGN modeling at UV-to-IR wavelengths. Here, we apply X-CIGALE to different samples, including COSMOS spectroscopic type 2 AGNs, CDF-S X-ray detected normal galaxies, SDSS quasars, and COSMOS radio objects. From these tests, we identify several weaknesses of X-CIGALE and improve the code accordingly. These improvements are mainly related to AGN intrinsic X-ray anisotropy, X-ray binary emission, AGN accretion-disk SED shape, and AGN radio emission. These updates improve the fit quality and allow new interpretation of the results, based on which we discuss physical implications. For example, we find that AGN intrinsic X-ray anisotropy is moderate, and can be modeled as $L_X(θ) \propto 1+\cos θ$, where $θ$ is the viewing angle measured from the AGN axis. We merge the new code into the major branch of CIGALE, and publicly release this new version as CIGALE v2022.0 on https://cigale.lam.fr
AGNBoost: A Machine Learning Approach to AGN Identification with JWST/NIRCam+MIRI Colors and Photometry
University of Kansas（堪萨斯大学）；Rochester Institute of Technology（罗切斯特理工学院）；Colby College（科尔比学院）；Space Telescope Science Institute（太空望远镜科学研究所）；NASA-Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Texas A&M University（得克萨斯农工大学）
We present analyses of host galaxy properties of type 1 and type 2 X-ray selected AGNs in the XMM-XXL field, which have available optical spectroscopic classification. We model their optical to far-infrared spectral energy distributions (SEDs) using the X-CIGALE code. X-CIGALE allows the fitting of X-ray flux and accounts for the viewing angle of dusty torus and the attenuation from polar dust. By selecting matched type 1 and 2 subsamples in the X-ray luminosity and redshift parameter space, we find that both types live in galaxies with similar star formation. However, type 2 AGN tend to resid…
The sensitivity and angular resolution of photometric surveys executed by the Hubble Space Telescope (HST) enable studies of individual star clusters in galaxies out to a few tens of megaparsecs. The fitting of spectral energy distributions (SEDs) of star clusters is essential for measuring their physical properties and studying their evolution. We report on the use of the publicly available Code Investigating GALaxy Emission (CIGALE) SED fitting package to derive ages, stellar masses, and reddenings for star clusters identified in the Physics at High Angular resolution in Nearby GalaxieS-HST …
Obscured AGN at z < 1.5: X-ray to Far-Infrared SEDs and Host Galaxy Morphologies in the GOODS Fields
University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；University of Wisconsin - Madison（威斯康星大学麦迪逊分校）；Eureka Scientific（尤里卡科学公司）；Institute for Astronomy, University of Hawai‘i（夏威夷大学天体物理研究所）；Wuhan University（武汉大学）；Northwestern University（西北大学）；Yale Center for Astronomy and Astrophysics（耶鲁天文学与天体物理学中心）；Physics Department and Yale Center for Astronomy and Astrophysics（耶鲁大学物理系及天文学与天体物理学中心）；Yale University（耶鲁大学）；DiRAC Institute and the Department of Astronomy, University of Washington（华盛顿大学DiRAC研究所及天文学系）
Polar dust has been found to play an important role in the mid-infrared emission of nearby Seyfert nuclei. If and how often polar dust exists among the quasar population is unknown due to the lack of spatially-resolved observations. In this Letter, we report correlations between the prominence of AGN forbidden line emission (commonly associated with the narrow line region) and the dust mid-IR energy output among the archetypal Palomar-Green quasar sample and other bright type-1 AGNs drawn from the SDSS, Spitzer and WISE archives. The AGN mid-IR color differences traced by WISE W2 ($\sim4.6 μm$…
Compton-induced HE -- VHE $γ$-rays from pair cascade emissions in the SEDs of radio galaxies: NGC 1275
University of Johannesburg（约翰内斯堡大学）；The George Washington University（乔治华盛顿大学）；National Institute for Theoretical and Computational Sciences（国家理论与计算科学研究所）
Exploring the mid-infrared SEDs of six AGN dusty torus models I: synthetic spectra
在远离活动星系核（AGN）的地方，环境温度低于1500-1800 K，尘埃能够存活。因此，有可能存在一个围绕活动星系核的大尘埃结构。这是两篇论文中的第一篇，旨在比较六个尘埃环面模型与可用的SED，即Fritz et al.（2006），Nenkova et al.（2008 B），Hoenig & Kishimoto（2010），Siebenmorgen et al.（2015），Stalevski et al.（2016）和Hoenig & Kishimoto（2017）。在这第一篇论文中，我们使用合成光谱来探索这些模型之间的区别，在何种情况下，他们允许限制环面参数，而我们的第二篇论文分析了最好的模型来描述中红外光谱数据。我们已经产生了合成光谱，从目前的仪器：GTC/CanariCam和斯皮策/IRS和未来的JWST/MIRI和JWST/NIRSpec仪器。我们发现，对于一个合理的亮度（F12 um> 100 mJy），我们实际上可以区分模型之间，除了两对父模型。我们表明，这些模型可以区分的基础上的连续斜率和强度的硅酸盐功能。此外，对于除Hoenig & Kishimoto（2017）之外的所有模型，无论使用何种仪器，其参数都可以限制在15%的误差范围内。然而，当超过50%的环核贡献者被包括在内时，参数估计被破坏。因此，未来的高空间分辨率光谱，如那些预期从JWST将提供足够的覆盖…
We describe a complete, flux-density-limited sample of galaxies at redshift $0.8 < z < 1.3$ selected at 16 micron. At the selection wavelength near 8 micron rest, the observed emission comes both from dust heated by intense star formation and from active galactic nuclei (AGNs). Fitting the spectral energy distributions (SEDs) of the sample galaxies to local-galaxy templates reveals that more than half the galaxies have SEDs dominated by star formation. About one sixth of the galaxy SEDs are dominated by an AGN, and nearly all the rest of the SEDs are composite. Comparison with X-ray and far-in…
Far-infrared (far-IR)/sub-mm emission linked to AGN-heated dust has been a topic of contention for many years. Results have been diverse and various views have been presented. The empirical AGN SED derived by Symeonidis et al. (2016, hereafter S16) has more far-IR/sub-mm emission than other SEDs in the literature, and thus it is contested by other works which argue that its luminosity in that part of the spectrum is overestimated. Here, I investigate this topic and the concerns raised over the S16 AGN SED. I also examine the differences between the S16 AGN SED and other commonly-used empirical…
Feedback in Extragalactic Star Clusters (FEAST): Spectral Energy Distributions and the Physical Properties of Star Clusters in NGC 628 with CIGALE
University of Arizona（亚利桑那大学）；Stockholm University（斯德哥尔摩大学）；University of Massachusetts Amherst（马萨诸塞大学阿默斯特分校）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；University of Virginia（弗吉尼亚大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；Australian National University（澳大利亚国立大学）；Cardiff University（卡迪夫大学）
The JWST MIRI instrument will revolutionize extragalactic astronomy with unprecedented sensitivity and angular resolution in mid-IR. Here, we assess the potential of MIRI photometry to constrain galaxy properties in the Cosmic Evolution Early Release Science (CEERS) survey. We derive estimated MIRI fluxes from the spectral energy distributions (SEDs) of real sources that fall in a planned MIRI pointing. We also obtain MIRI fluxes for hypothetical AGN-galaxy mixed models varying the AGN fractional contribution to the total IR luminosity ($\rm frac_{AGN}$). Based on these model fluxes, we simula…
Star-forming galaxies are rich reservoirs of dust, both warm and cold. But the cold dust emission is faint alongside the relatively bright and ubiquitous warm dust emission. Recently, evidence for a very cold dust component has also been revealed via millimeter/submillimeter photometry of some galaxies. This component, despite being the most massive of the three dust components in star-forming galaxies, is by virtue of its very low temperature, faint and hard to detect together with the relatively bright emission from warmer dust. Here we analyze the dust content of a carefully selected sample…
ReveaLLAGN 1: JWST Emission-Line Spectra Reveal Low-Luminosity AGN with UV-Deficient SEDs and Warm Molecular Gas
University of Utah（犹他大学）；Vanderbilt University（范德堡大学）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理研究中心）；European Space Agency（欧洲空间局）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；The Pennsylvania State University（宾夕法尼亚州立大学）；Istituto di Astrofisica e Planetologia Spaziali (INAF–IAPS)（国家天体物理学和行星学研究所）
A Spectroscopic Survey of WISE-selected Obscured Quasars with the Southern African Large Telescope
我们提出了一个样本的40个候选人的遮蔽类星体的光谱调查的结果确定的基础上，他们的中红外发射探测的宽视场红外巡天探测器（WISE）。这次巡天的光谱是用南部非洲大望远镜上的罗伯特·斯托比摄谱仪获得的。我们的样品被选择与智慧的颜色特征的活动星系核，以及红色的光学中红外的颜色，表明光学/紫外活动星系核连续被尘埃遮蔽。我们获得安全的红移的对象，包括我们的样本（35/40）的大多数，并发现，在WISE W 4（22 $μ$ m）带明亮的源通常是在中等红移（<z>= 0.35 $) while sources fainter in W4 are at higher redshifts (<z> = 0.73$）。大多数的源有窄的发射线，与我们的WISE选择的源的光学颜色和发射线比是一致的活动星系核的轨迹上的休息框架$g-z$颜色与[NeIII] $λ$ 3869 / [OII] $λλ$ 3726+3729线比诊断图。我们还使用经验AGN和星系模板来模拟我们样本中的物体的光谱能量分布（SED），并发现虽然这些物体的观测SED存在显着变化，但大多数都需要强大的AGN组件。最后，我们使用我们的光谱和SED的分析结果，比较我们的选择标准，在文献中提出的替代标准。这些结果验证了基于它们的WISE颜色选择发光遮蔽活动星系核的有效性。
We study the host galaxy properties of active galactic nuclei (AGN) that have been detected in X-rays in the nearby Universe ($\rm z<0.2$). For that purpose, we use the catalogue provided by the ROSAT-2RXS in the 0.1-2.4\,keV energy band, one of the largest X-ray datasets with spectroscopic observations. Our sample consists of $\sim 900$ X-ray AGN. The catalogue provides classification of the sources into type 1 and 2, based on optical spectra. $\sim 25\%$ of the AGN are type 2. We use the available optical, near-IR and mid-IR photometry to construct SEDs. We measure the stellar mass ($M_*$) a…
A long-standing question in active galactic nucleus (AGN) research is how the corona is heated up to produce X-ray radiation much stronger than that arising from the viscous heating within the corona. In this paper, we carry out detailed investigations of magnetic-reconnection heating to the corona, specifically, studying how the disc and corona are self-consistently coupled with the magnetic field, and how the emergent spectra depend on the fundamental parameters of AGN. It is shown that diverse spectral shapes and luminosities over a broad bandpass from optical to X-ray can be produced from …
