Optically-faint massive Balmer Break Galaxies at z>3 in the CANDELS/GOODS fields
Belén Alcalde Pampliega, Pablo G. Pérez-González, Guillermo Barro, Helena Domínguez Sánchez, M. Carmen Eliche-Moral, Nicolás Cardiel, Antonio Hernán-Caballero, … 展开作者
Belén Alcalde Pampliega, Pablo G. Pérez-González, Guillermo Barro, Helena Domínguez Sánchez, M. Carmen Eliche-Moral, Nicolás Cardiel, Antonio Hernán-Caballero, Lucía Rodriguez-Muñoz, Patricia Sánchez Blázquez, Pilar Esquej
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38 pages, 18 figures, Accepted for publication in The Astrophysical Journal 26/03/2019
We present a sample of 33 Balmer Break Galaxies (BBGs) selected as HST/F160W dropouts in the deepest CANDELS/GOODS fields ($H\gtrsim27.3$~mag) but relatively bright in {\it Spitzer}/IRAC ($[3.6],[4.5]<24.5$~mag), implying red colors (median and quartiles: $\langle H-[3.6]\rangle=3.1^{3.4}_{2.8}$\,mag). Half of these BBGs are newly identified sources. Our BBGs are massive ($\langle \log(\rm{M}/\rm{M}_\odot)\rangle=10.8$) high redshift ($\langle z\rangle=4.8$) dusty ($\langle \rm{A(V)}\rangle=2.0$~mag) galaxies. The SEDs of half of our sample indicate that they are star-forming galaxies with typical specific SFRs 0.5-1.0~Gyr$^{-1}$, qualifying them as main sequence (MS) galaxies at $3<z<6$. One third of those SEDs indicates the presence of prominent emission lines (H$β$+$[OIII]$, H$α$$+$[NII]) boosting the IRAC fluxes and red colors. Approximately 20\% of the BBGs are very dusty ($\rm{A(V)}\sim2.5$~mag) starbursts with strong mid-to-far infrared detections and extreme SFRs ($\rm{SFR}>10^{3}\,\rm{M}_\odot/yr$) that place them above the MS. The rest, 30\%, are post-starbursts or quiescent galaxies located $>2σ$ below the MS with mass-weighted ages older than 700~Myr. Only 2 of the 33 galaxies are X-ray detected AGN with optical/near-infrared SEDs dominated by stellar emission, but the presence of obscured AGN in the rest of sources cannot be discarded. Our sample accounts for 8\% of the total number density of $\log(\rm{M}/\rm{M}_\odot)>10$ galaxies at $z>3$, but it is a significant contributor (30\%) to the general population of red $\log(\rm{M}/\rm{M}_\odot)>11$ galaxies at $4<z<6$. Finally, our results point out that 1 of every 30 massive $\log(\rm{M}/\rm{M}_\odot)>11$ galaxies in the local Universe was assembled in the first 1.5~Gyr after the Big Bang, a fraction that is not reproduced by state-of-the-art galaxy formation simulations.
S-CANDELS: The Spitzer-Cosmic Assembly Near-Infrared Deep Extragalactic Survey. Survey Design, Photometry, and Deep IRAC Source Counts
斯皮策宇宙大会深近红外河外遗产调查（S-CANDELS; PI G。Fazio）是一个第8周期的探索计划，旨在探测非常高红移（z > 5）的星系。为了减轻宇宙变化的影响，并利用哈勃空间望远镜多周期财政计划CANDELS在多个波段的深度同延覆盖，S-CANDELS在五个相距甚远的河外区域进行：UKIDSS超深巡天、扩展钱德拉深场南、COSMOS、HST深场北和扩展格罗斯带。S-CANDELS建立在斯皮策扩展深度调查（SEDS）现有的这些领域的覆盖范围之上，将积分时间从12小时增加到总共50小时，但在较小的区域内，0.16平方度。额外的深度显著增加了微弱星等下的勘测完整性。本文介绍了S-CANDELS调查的设计、处理和公开提供的数据产品。我们目前的IRAC双波段3.6+4.5微米目录达到26.5 AB MAG的深度。深IRAC计数的大约135,000个星系检测的S-CANDELS是一致的模型的基础上已知的星系种群。比早期斯皮策/IRAC调查更深的深度增加并没有揭示离散源对弥漫的宇宙红外背景（CIB）的显着额外贡献。因此，它仍然是正确的，只有大约一半的估计CIB通量从COBE/DIRBE解决。
Extending the evolution of the stellar mass-size relation at $z \leq 2$ to low stellar mass galaxies from HFF and CANDELS
我们可靠地扩展恒星的质量-尺寸关系$0.2\leq z \leq2$低恒星质量的星系相结合的深度哈勃前沿场（HFF）的大体积覆盖的坎德尔。使用MegaMorph项目开发的工具，在多个波段中同时对Galerkin进行建模，从而允许稳健的尺寸（即，半光半径）的估计，即使是小，微弱，高红移星系。我们表明，以上10 $^7$ M $_\odot$，恒星形成的星系是很好地代表了一个单一的权力法律上的质量大小的平面在我们的整个红移范围。相反，恒星质量为$\geq 10^{10.3}$ M $_\odot$的静止星系和质量较低的恒星，无论静止星系是根据恒星形成活动、静止坐标系颜色还是结构特征来选择的，恒星质量-尺寸关系都是陡峭的。在$z\leq1$的$\sim1$ kpc的大小下发生这种平坦化。因此，一个双幂定律是首选的恒星质量大小的关系，静止星系，至少在10 $^7$ M $_\odot$。我们没有发现强烈的红移依赖于恒星形成星系以及高质量的静止星系的关系的斜率。我们还表明，恒星质量$\geq$ 10 $^{9.5}$ M $_\odot$和恒星质量$\geq10^{10.3}$ M $_\odot$的恒星形成星系经历了显着的大小增长，因为$z\sim2$，正如预期的那样，但是，低质量的星系没有。最后，我们补充我们的数据，主要是静止的矮星系从天炉座星系团的核心，表明恒星的质量-尺寸关系是连续的…
The gradual decline of Ly$α$ visibility in the CANDELS fields: evidence for the combined effects of galaxy evolution and reionization
INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Scuola Normale Superiore（比萨高等师范学院）；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学红外天文研究实验室）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校宇宙前沿中心）；Armagh Observatory and Planetarium（阿马赫天文馆与天文台）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Astrophysics Science Division, NASA Goddard Space Flight Center（NASA戈达德太空飞行中心天体物理学部）；Center for Space Sciences and Technology, UMBC（马里兰大学巴尔的摩分校空间科学与技术中心）
MIDIS: The identification of deep MIRI-red sources as candidates for extreme Balmer-break and line emitting galaxies at high-z
Cosmic Dawn Center (DAWN)（宇宙黎明中心）；DTU-Space, Technical University of Denmark（丹麦技术大学空间科学部）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Department of Astronomy, Oskar Klein Centre, Stockholm University（斯德哥尔摩大学奥斯卡·克莱因中心天文学系）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；Centro de Astrobiología (CAB), CSIC-INTA（CSIC-INTA天体生物学中心）；Space Telescope Science Institute（太空望远镜科学研究所）
Early Results from GLASS-JWST. XXVI. Spatially Resolved Star Formation and Balmer Decrements at $1.1<z<2.3$ from NIRISS Slitless Spectroscopy
School of Astronomy and Space Science, University of Chinese Academy of Sciences (UCAS)（中国科学院大学天文与空间科学学院）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学天文与前沿科学研究院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Department of Physics and Astronomy, University of California Davis（加州大学戴维斯分校物理与天文学系）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）；Department of Physics and Astronomy, University of California, Los Angeles（加州大学洛杉矶分校物理与天文学系）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）
JWST Spectroscopic Census of ALMA Faint Submillimeter Galaxies in the Hubble Ultra Deep Field
The Graduate University for Advanced Studies, SOKENDAI（日本高级研究院）；National Astronomical Observatory of Japan（日本国立天文台）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学 Kavli 宇宙物理数学研究所）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学大卫·邓普天文学与天体物理学系）；Dunlap Institute for Astronomy and Astrophysics（邓普天文学与天体物理学研究所）
Probing the Star Formation Main Sequence down to 10$^{7} M_\odot$ at $1 < z < 9$
Saint Mary’s University（圣玛丽大学）；Columbia University（哥伦比亚大学）；Space Telescope Science Institute（太空望远镜科学研究所）；National Research Council of Canada, Herzberg Astronomy & Astrophysics Research Centre（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究中心）；University of California Davis（加州大学戴维斯分校）；University of Groningen（格罗宁根大学）；York University（约克大学）
本研究通过结合多源数据，探测1 < z < 9范围内10^7 M_太阳的恒星形成主序列，揭示了不同质量范围内的恒星形成历史及演化特征。
GLIMPSE: An ultra-faint $\simeq$ 10$^{5}$ $M_{\odot}$ Pop III Galaxy Candidate and First Constraints on the Pop III UV Luminosity Function at $z\simeq6-7$
