From the far-ultraviolet to the far-infrared -- galaxy emission at $0\le z \le 10$ in the Shark semi-analytic model
Claudia del P. Lagos, Aaron S. G. Robotham, James W. Trayford, Rodrigo Tobar, Matías Bravo, Sabine Bellstedt, Luke J. M. Davies, Simon P. Driver, Pascal J. Elah… 展开作者
Claudia del P. Lagos, Aaron S. G. Robotham, James W. Trayford, Rodrigo Tobar, Matías Bravo, Sabine Bellstedt, Luke J. M. Davies, Simon P. Driver, Pascal J. Elahi, Danail Obreschkow, Chris Power
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Accepted for publication in MNRAS after minor corrections (22 pages, 21 figures)
We combine the Shark semi-analytic model of galaxy formation with the ProSpect software tool for spectral energy distribution (SED) generation to study the multi-wavelength emission of galaxies from the far-ultraviolet (FUV) to the far-infrared (FIR) at $0\le z\le 10$. We produce a physical model for the attenuation of galaxies across cosmic time by combining a local Universe empirical relation to compute the dust mass of galaxies from their gas metallicity and mass, attenuation curves derived from radiative transfer calculations of galaxies in the EAGLE hydrodynamic simulation suite, and the properties of Shark galaxies. We are able to produce a wide range of galaxies, from the $z=8$ star-forming galaxies with almost no extinction, $z=2$ submillimeter galaxies, down to the normal star-forming and red sequence galaxies at $z=0$. Quantitatively, we find that Shark reproduces the observed (i) the $z=0$ FUV-to-FIR, (ii) $0\le z\le 3$ rest-frame $K$-band, and (iii) $0\le z\le 10$ rest-frame FUV luminosity functions, (iv) $z\le 8$ UV slopes, (v) the FUV-to-FIR number counts (including the widely disputed 850$μ$m), (vi) redshift distribution of bright $850μ$m galaxies and (vii) the integrated cosmic SED from $z=0$ to $z=1$ to an unprecedented level. This is achieved without the need to invoke changes in the stellar initial mass function, dust-to-metal mass ratio, or metal enrichment timescales. Our model predicts star formation in galaxy disks to dominate in the FUV-to-optical, while bulges dominate at the NIR at all redshifts. The FIR sees a strong evolution in which disks dominate at $z\le 1$ and starbursts (triggered by both galaxy mergers and disk instabilities, in an even mix) dominate at higher redshifts, even out to $z=10$.
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）
Radio-only and Radio-to-far-ultraviolet Spectral Energy Distribution Modeling of 14 ULIRGs: Insights into the Global Properties of Infrared Bright Galaxies
The rest ultraviolet to infrared spectral energy distributions of heavily reddened quasars are "V-shaped" and hot-dust poor
School of Physics and Astronomy, University of Southampton（南安普顿大学物理与天文学学院）；Centre for Extragalactic Astronomy, Department of Physics, Durham University（杜伦大学物理系河外天文中心）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）
The Spitzer Data Fusion - A Far-Ultraviolet to Far-Infrared Multi-Wavelength Database in Spitzer Extragalactic Survey Fields
Inter-University Institute for Data Intensive Astronomy (IDIA), Department of Astronomy, University of Cape Town（开普敦大学数据密集型天文学校际研究所）；University of the Western Cape（西开普大学）；INAF - Istituto di Radioastronomia（意大利国家天体物理研究所射电天文台）
Prescriptions for Correcting Ultraviolet-Based Redshifts for Luminous Quasars at High Redshift
高红移类星体的红移通常是由静止坐标系的紫外线（UV）发射线决定的。然而，这些线，更具体地说，突出的C IV $λ1549$发射线，通常是蓝移产生高度不确定的红移估计相比，从静止帧光发射线确定的红移。我们目前的近红外光谱的18个发光类星体在$2.15 < z < 3.70$，使我们能够获得可靠的系统红移这些来源。再加上近红外光谱的44个类星体具有可比的光度和红移的档案样本，我们提供了纠正紫外红移的处方。我们的处方减少速度偏移相对于系统的红移由$\sim140$公里的$^{-1}$和减少的不确定性的紫外线为基础的红移由$\sim25\%$相对于目前用于确定这些值的最佳方法。我们还发现，从斯隆数字巡天管道为我们的来源确定的红移遭受显着的不确定性，这是不容易减轻。我们讨论了我们的处方，以提高基于紫外线的红移校正的潜在的一个更大的样本的高红移类星体与近红外光谱。
RCSED - A Value-Added Reference Catalog of Spectral Energy Distributions of 800,299 Galaxies in 11 Ultraviolet, Optical, and Near-Infrared Bands: Morphologies, Colors, Ionized Gas and Stellar Populations Properties
