PEARLS: Low Stellar Density Galaxies in the El Gordo Cluster Observed with JWST
Timothy Carleton, Seth H. Cohen, Brenda Frye, Alex Pigarelli, Jiashuo Zhang, Rogier A. Windhorst, Jose M. Diego, Christopher J. Conselice, Cheng Cheng, Simon P.… 展开作者
Timothy Carleton, Seth H. Cohen, Brenda Frye, Alex Pigarelli, Jiashuo Zhang, Rogier A. Windhorst, Jose M. Diego, Christopher J. Conselice, Cheng Cheng, Simon P. Driver, Nicholas Foo, Rachana A. Bhatawdekar, Patrick Kamieneski, Rolf A. Jansen, Haojing Yan, Jake Summers, Aaron Robotham, Christopher N. A. Willmer, Anton Koekemoer, Scott Tompkins, Dan Coe, Norman Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Russell E. Ryan
A full understanding of how unusually large "Ultra Diffuse Galaxies" (UDGs) fit into our conventional understanding of dwarf galaxies remains elusive, despite the large number of objects identified locally. A natural extension of UDG research is the study of similar galaxies at higher redshift to establish how their properties may evolve over time. However, this has been a challenging task given how severely systematic effects and cosmological surface brightness dimming inhibit our ability to study low-surface brightness galaxies at high-$z$. Here, we present an identification of low stellar surface density galaxies (LDGs), likely the progenitors of local UDGs, at moderate redshift with deep near-IR observations of the El Gordo cluster at $z = 0.87$ with JWST. By stacking 8 NIRCAM filters, we are able to achieve an apparent surface brightness sensitivity of $24.59$ mag arcsec$^{-2}$, faint enough to be complete to the bright end of the LDG population. Our analysis identifies significant differences between this population and local UDGs, such as their color and size distributions, which suggest that UDG progenitors are bluer and more extended at high-$z$ than at $z = 0$. This suggests that multiple mechanisms are responsible for UDG formation and that prolonged transformation of cluster dwarfs is not a primary UDG formation mechanism at high-$z$. Furthermore, we find a slight overabundance of LDGs in El Gordo, and, in contrast to findings in local clusters, our analysis does not show a deficit of LDGs in the center of El Gordo, implying that tidal destruction of LDGs is significant between $z = 0.87$ and $z = 0$.
Galaxy-scale lens search in the PEARLS NEP TDF and CEERS JWST fields
University of Melbourne（墨尔本大学）；ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D)（三维全天空天体物理学卓越研究中心）；Arizona State University（亚利桑那州立大学）；Instituto de Fisica de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）；Space Telescope Science Institute（太空望远镜科学研究所）
JWST's PEARLS: A clumpy ring galaxy at $z = 4.0148$
University of Illinois（伊利诺伊大学）；Durham University（杜伦大学）；Arizona State University（亚利桑那州立大学）；Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS（中国科学院南天文中心，国家天文台，中科院）；Jodrell Bank Centre for Astrophysics, University of Manchester（曼彻斯特大学乔德雷尔银行天体物理学中心）；Instituto de Fisica de Cantabria (CSIC-UC)（坎塔布里亚物理研究所（西班牙科学理事会-坎塔布里亚大学））；University of Arizona（亚利桑那大学）；Space Telescope Science Institute（太空望远镜科学研究所）
JWSTs PEARLS: NIRCam imaging and NIRISS spectroscopy of a $z=3.6$ star-forming galaxy lensed into a near-Einstein Ring by a $z=1.258$ massive elliptical galaxy
EPOCHS Paper II: The Ultraviolet Luminosity Function from $7.5<z<13.5$ using 180 square arcminutes of deep, blank-fields from the PEARLS Survey and Public JWST data
PEARLS: JWST Counterparts of Micro-Jy Radio Sources in the NEP Time Domain Field. II. All Four Spokes
Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼学会）；Eureka Scientific（尤里卡科学）；INAF––Istituto di Astrofisica Spaziale e Fisica Cosmica Milano（意大利国家天体物理研究所米兰空间天体物理与宇宙物理研究所）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Space Telescope Science Institute（太空望远镜科学研究所）
JWST's PEARLS: 119 multiply imaged galaxies behind MACS0416, lensing properties of caustic crossing galaxies, and the relation between halo mass and number of globular clusters at $z=0.4$
JWST's PEARLS: A Candidate Massive Binary Star System in a Lensed Galaxy at Redshift 0.94
University of Minnesota（明尼苏达大学）；Arizona State University（亚利桑那州立大学）；FORTH（希腊研究所）；University of Manchester（曼彻斯特大学）；University of California, Berkeley（加州大学伯克利分校）；University of Arizona（亚利桑那大学）；University of Louisville（路易斯维尔大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Ben-Gurion University of the Negev（内盖夫本-古里安大学）；University of Maryland（马里兰大学）；New York University Abu Dhabi（纽约大学阿布扎比分校）；University of Missouri - Columbia（密苏里大学哥伦比亚分校）
JWST's PEARLS: Temperatures of Nine Highly Magnified Stars in a Galaxy at Redshift 0.94 and Simulated Stellar Population Dependence on Stellar Metallicity and the Initial Mass Function
University of Minnesota（明尼苏达大学）；Arizona State University（亚利桑那州立大学）；University of California, Berkeley（加州大学伯克利分校）；The University of Hong Kong（香港大学）；Donostia International Physics Center, DIPC（圣塞巴斯蒂安国际物理中心）；University of Basque Country UPV/EHU（巴斯克国立大学）；Oklahoma State University（俄克拉荷马州立大学）；University of Manchester（曼彻斯特大学）；University of Louisville（路易斯维尔大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Ben-Gurion University of the Negev（内盖夫本-古里安大学）；University of Maryland, College Park（马里兰大学帕克分校）；University of Missouri - Columbia（密苏里大学哥伦比亚分校）
PEARLS: NuSTAR and XMM-Newton Extragalactic Survey of the JWST North Ecliptic Pole Time Domain Field VI: Multiwavelength SED Analysis
Arizona State University（亚利桑那州立大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼学会）；University of Utah（犹他大学）
PEARLS: 21 Transients Found in the Three-Epoch NIRCam Observations in the Continuous Viewing Zone of the James Webb Space Telescope
University of Missouri（密苏里大学）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Texas A. & M. University（德克萨斯农工大学）；University of Arizona（亚利桑那大学）；Oklahoma State University（俄克拉荷马州立大学）；Space Telescope Science Institute（太空望远镜科学研究所）；The Ohio State University（俄亥俄州立大学）
PEARLS: Two Distinct Populations of AGN Hosts Moving Between Star Formation and Quiescence
School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森天体物理中心）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
Free-form lens model and mass estimation of the high redshift galaxy cluster ACT-CL J0102-4915, "El Gordo"
我们研究了大规模的碰撞集群埃尔戈多，在高红移最大的集群之一。我们使用自由形式的透镜重建方法，避免了对质量分布的假设。我们使用的数据，从MANUICS计划，并确定新的多透镜系统的候选人。新的约束条件和自由形式的方法提供了一个新的独立的质量估计这个有趣的碰撞集群。我们的结果被发现是与早期的参数模型，间接证实了在早期的工作中所作的假设是一致的。通过将双gNFW轮廓拟合到透镜模型，并外推到维里半径，我们推断出$M_{200c}=(1.08^{+0.65}_{-0.12})\times10^{15}$ M $_{\odot}$簇的总质量。我们估计的质量的不确定性，由于测光红移的误差，并讨论了不确定性，由于推断的维里质量从透镜模型的外推。我们还发现，在我们的镜头地图对应的大彗星尾部的热气体，加强其解释为一个大的潮汐功能预测的流体动力学模拟，模仿埃尔戈多质量过密。最后，我们讨论了所观察到的等离子体和质量图之间的关系，发现在投影质量图的峰值可能与一个大的浓度较冷的气体，表现出可能的恒星形成。El Gordo是JWST观测到的首批星系团之一，预计将在这个有趣的星系团周围发现新的高红移透镜星系，并对其质量提供更准确的估计。
