Discovery of the Most-Distant Double-Peaked Emitter at z=1.369
B. Luo, W. N. Brandt, J. D. Silverman, I. V. Strateva, F. E. Bauer, P. Capak, J. Kartaltepe, B. D. Lehmer, V. Mainieri, M. Salvato, G. Szokoly, D. P. Schneider, C. Vignali
We report the discovery of the most-distant double-peaked emitter, CXOECDFS J033115.0-275518, at z=1.369. A Keck/DEIMOS spectrum shows a clearly double-peaked broad Mg II $\lambda2799$ emission line, with FWHM 11000 km/s for the line complex. The line profile can be well fit by an elliptical relativistic Keplerian disk model. This is one of a handful of double-peaked emitters known to be a luminous quasar, with excellent multiwavelength coverage and a high-quality X-ray spectrum. CXOECDFS J033115.0-275518 is a radio-loud quasar with two radio lobes (FR II morphology) and a radio loudness of f_{5 GHz}/f_{4400 Å}~429. The X-ray spectrum can be modeled by a power law with photon index 1.72 and no intrinsic absorption; the rest-frame 0.5-8.0 keV luminosity is $5.0\times10^{44}$ erg/s. The spectral energy distribution (SED) of CXOECDFS J033115.0-275518 has a shape typical for radio-loud quasars and double-peaked emitters at lower redshift. The local viscous energy released from the line-emitting region of the accretion disk is probably insufficient to power the observed line flux, and external illumination of the disk appears to be required. The presence of a big blue bump in the SED along with the unexceptional X-ray spectrum suggest that the illumination cannot arise from a radiatively inefficient accretion flow.
A Census of Double-Peaked Lyman-alpha Emitters in MAGPI: Classification, Global Characteristics, and Spatially Resolved Properties
Macquarie University（麦考瑞大学）；Swinburne University of Technology（斯威本科技大学）；Observatori Astronòmic de la Universitat de València（瓦伦西亚大学天文台）；International Centre for Radio Astronomy Research (ICRAR), Curtin University（伊萨研究中心（ICRAR），科廷大学）；Sydney Institute for Astronomy, School of Physics, University of Sydney（悉尼大学物理学院悉尼天体物理学研究所）；International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia（伊萨研究中心（ICRAR），西澳大学）
Predicting emission line fluxes and number counts of distant galaxies for cosmological surveys
我们结合光度学和光谱学估计了高红移线发射体的数目及其随宇宙时间的演化。我们预测的H $α$，H $β$，[OII]和[OIII]线通量超过$35,000$星系下降到恒星质量的$\sim10^9$ $M_{\odot}$在COSMOS和GOODS-S领域，应用标准转换和利用光谱覆盖的FMOS-COSMOS调查在$z\sim1.55$校准的预测。在FMOS-COSMOS巡天覆盖的范围$1.4 < z < 1.8$内，我们计算了H $α$、[OII]和[OIII]发射体的数量计数，直到$1\times10^{-17}$ erg cm $^{-2}$ s $^{-1}$的通量。我们模拟的差分和累积H $α$计数的时间演变，急剧下降，在最亮的通量。我们期望$\sim9,300-9,700$和$\sim2,300-2,900$星系deg $^{-2}$的流量$\geq1\times10^{-16}$和$\geq2\times10^{-16}$ erg cm $^{-2}$ s $^{-1}$在$0.9<z<1.8$范围内。我们发现，观测到的星系红移的主要序列的演变是足够的再现观测到的计数变化$0.2<z<2.5$。我们用通量$\geq2\times10^{-16}$ erg cm $^{-2}$ s $^{-1}$来表征H $α$辐射体的物理性质，包括它们的恒星质量、紫外线大小、[NII]/H…
Double-Peaked Ly$α$ Emission during Reionization Requires Nearby Voids and a Favorable Local Ionizing Background
Institute for Basic Science（韩国基础科学研究院）；Center for Computational Sciences（计算科学中心）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；Chungbuk National University（忠北国立大学）；Observatoire Astronomique de Strasbourg, Université de Strasbourg, CNRS UMR 7550（斯特拉斯堡天文台，斯特拉斯堡大学，法国国家科学研究中心）；Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris VI（巴黎天体物理学研究所，法国国家科学研究中心，巴黎第六大学）；The University of Nottingham（诺丁汉大学）；University of Texas, Austin（德克萨斯大学奥斯汀分校）；University of Sussex（萨塞克斯大学）
