A Two-Dimensional Spectroscopic Study of Emission Line Galaxies in the Faint Infrared Grism Survey (FIGS) I: Detection Method and Catalog
Norbert Pirzkal, Barry Rothberg, Russell E. Ryan, Sangeeta Malhotra, James Rhoads, Norman Grogin, Emma Curtis-Lake, Jacopo Chevallard, Stephane Charlot, Steven … 展开作者
Norbert Pirzkal, Barry Rothberg, Russell E. Ryan, Sangeeta Malhotra, James Rhoads, Norman Grogin, Emma Curtis-Lake, Jacopo Chevallard, Stephane Charlot, Steven L. Finkelstein, Anton M. Koekemoer, Parviz Ghavamian, Myriam Rodrigues, François Hammer, Mathieu Puech, Rebecca L. Larson, Lise Christensen, Andrea Cimatti, Ignacio Ferreras, Jonathan P. Gardner, Caryl Gronwall, Nimish P. Hathi, Bhavin Joshi, Harald Kuntschner, Gerhardt R. Meurer, Robert W. O'Connell, Goeran Oestlin, Anna Pasquali, John Pharo, Amber N. Straughn, Jeremy R. Walsh, Darach Watson, Rogier A. Windhorst, Nadia L Zakamsk
We present the results from the application of a two-dimensional emission line detection method, EMission-line two-Dimensional (EM2D), to the near-infrared G102 grism observations obtained with the Wide-Field Camera 3 (WFC3) as part of the Cycle 22 {\em Hubble Space Telescope} Treasury Program: the Faint Infrared Grism Survey (FIGS). Using the EM2D method, we have assembled a catalog of emission line galaxies (ELGs) with resolved star formation from each of the four FIGS fields. Not only can one better assess the global properties of ELGs, but the EM2D method allows for the analysis and an improved study of the individual emission-line region {\it within} each galaxy. This paper includes a description of the methodology, advantages, and the first results of the EM2D method applied to ELGs in FIGS. The advantage of 2D emission line measurements includes significant improvement of galaxy redshift measurements, approaching the level of accuracy seen in high-spectral-resolution data, but with greater efficiency; and the ability to identify and measure the properties of multiple sites of star-formation and over scales of $\sim$ 1 kpc within individual galaxies out to z $\sim$ 4. The EM2D method also significantly improves the reliability of high-redshift ($z\sim7$) Lyman-$α$ detections. Coupled with the wide field of view and high efficiency of space-based grism observations, EM2D provides a noteworthy improvement on the physical parameters that can be extracted from grism observations.
FIGS: Spectral fitting constraints on the star formation history of massive galaxies since Cosmic Noon
利用HST的ACS和WFC 3星系的双标架光学和近红外无缝光谱，对52个质量对数Ms>10.5的大质量星系样本的恒星星族性质进行了约束，得到了红移范围为0.5<z<2的恒星族分布。深度曝光（~100 ks）使我们能够将大质量星系的单个光谱定位到F160 W =22.5AB。我们的光谱拟合方法使用一组六个基础模型，适应每个观测的红移和光谱分辨率，并通过MCMC方法拟合基础模型的权重，包括潜在的尘埃衰减。我们的样本包括静止星系（19）和恒星形成星系（33）的混合分布。我们量化的年龄分布（Dt）的宽度，发现占主导地位的检索参数的方差根据主成分分析。人口参数遵循预期的趋势，随着质量的增加，年龄较大，和DT似乎弱反相关恒星质量，这表明一个更有效的恒星形成在大规模的结束。正如预期的那样，静态样本中相对恒星年龄（以宇宙源的年龄为单位测量）的红移依赖性拒绝了单一爆发（又名整体坍缩）的假设。每个星系内的径向颜色梯度也进行了探索，发现一个更广泛的分散在恒星形成的子样本，但没有决定性的趋势相对于人口参数。
Medium-band Astrophysics with the Grism of NIRCam In Frontier fields (MAGNIF): Spectroscopic Census of H$α$ Luminosity Functions and Cosmic Star Formation at $z\sim 4.5$ and 6.3
Lyman-$α$ Visibility During the Epoch of Reionization: Combining JWST FRESCO Grism Data with Keck Archival Spectroscopy
Anton Pannekoek Institute for Astronomy（安顿·潘内科克天文学研究所）；Institute of High-Energy Physics（高能物理研究所）；University of Amsterdam（阿姆斯特丹大学）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究所）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；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）；Institute of Science and Technology Austria (ISTA)（奥地利科学与技术研究所）
The Grism Lens-Amplified Survey from Space (GLASS). IV. Mass reconstruction of the lensing cluster Abell 2744 from frontier field imaging and GLASS spectroscopy
SAPPHIRES: Extremely Metal-Poor Galaxy Candidates with $12+{\rm log(O/H)}<7.0$ at $z\sim5-7$ from Deep JWST/NIRCam Grism Observations
Space Telescope Science Institute (STScI)（太空望远镜科学研究所）；The Johns Hopkins University（约翰斯·霍普金斯大学）；Association of Universities for Research in Astronomy (AURA), Inc.（大学天文研究协会）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；Ben-Gurion University of the Negev（内盖夫本-古里安大学）；University of Groningen（格罗宁根大学）；University of Cambridge（剑桥大学）；University College London（伦敦大学学院）；University of Arizona（亚利桑那大学）；Tsinghua University（清华大学）；Chiba University（千叶大学）；The University of Tokyo（东京大学）；National Astronomical Observatory of Japan（日本国立天文台）；SOKENDAI (The Graduate University for Advanced Studies)（综合研究大学院大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；University of Copenhagen（哥本哈根大学）；University of Oxford（牛津大学）；Westlake University（西湖大学）；University of Michigan（密歇根大学）
Hubble Space Telescope Grism Spectroscopy of Extreme Starbursts Across Cosmic Time: The Role of Dwarf Galaxies in the Star Formation History of the Universe
The Luminosity Function and Clustering of H$α$ Emitting Galaxies at $z\approx4-6$ from a Complete NIRCam Grism Redshift Survey
Tsinghua University（清华大学）；University of Arizona（亚利桑那大学）；University of Michigan（密歇根大学）；University of Oxford（牛津大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Cambridge（剑桥大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
Abundant Population of Broad H$α$ Emitters in the GOODS-N Field Revealed by CONGRESS, FRESCO, and JADES
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Astronomy, Tsinghua University（清华大学天文系）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics, University of Oxford（牛津大学物理系）；European Space Agency (ESA), European Space Astronomy Centre (ESAC)（欧洲空间局（ESA）欧洲空间天文中心（ESAC））；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文与天体物理系）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）
A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Spectroscopically Complete Census of Obscured Cosmic Star Formation Rate Density at $z=4-6$
Emission-line galaxies at $z\sim1$ from near-IR HST Slitless Spectroscopy: metallicities, star formation rates and redshift confirmations from VLT/FORS2 spectroscopy
