Resolved UV and optical color gradients reveal environmental influence on galaxy evolution at redshift z$\sim$1.6
William J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. S… 展开作者
William J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
The changes in colors across a galaxy are intimately connected to the galaxy's formation, growth, quenching history, and dust content. A particularly important epoch in the growth of galaxies is near $z \sim 2$ often referred to as `cosmic noon', where galaxies on average reach the peak of their star formation. We study a population of 125 cluster galaxies at $z \sim 1.6$ in three Hubble Space Telescope (HST) filters, F475W, F625W, and F160W, roughly corresponding to the rest-frame FUV, NUV, and r band, respectively. By comparing to a control sample of 200 field galaxies at similar redshift, we reveal clear, statistically significant differences in the overall spatially resolved colors and color gradients in galaxies across these two different environments. On average, cluster galaxies have redder UV colors in both the inner and outer regions bounded by $r_{\mathrm{50}}$, as well as an overall wider dispersion of outside-in color gradients. The presence of these observed differences, along with evidence from ancillary data from previous studies, strongly suggests that the environment drives these population-level color differences, by affecting the stellar populations and/or dust content.
Rhodes University（罗德斯大学）；Queen’s University（女王大学）；Arthur B. McDonald Canadian Astroparticle Physics Research Institute, Queen’s University（亚瑟·B·麦克唐纳加拿大高能粒子物理研究所，女王大学）；IFPU – Institute for Fundamental Physics of the Universe（宇宙基础物理研究所 (IFPU)）；Seoul National University（首尔大学）；The University of Western Australia（西澳大学）
The GOGREEN Survey: AI Powered Deconvolution Lifts The Veil on Outside-in Environmental Quenching at z > 1
University of California, Merced（加利福尼亚大学默塞德分校）；The University of Kansas（堪萨斯大学）；Ecole Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；University of Waterloo（滑铁卢大学）；University of California, Davis（加利福尼亚大学戴维斯分校）；York University（约克大学）；University of Colorado（科罗拉多大学）
Environmental dependence of AGN activity. I.: the effects of host galaxy
利用SDSS DR 5中选取的大样本（144，940个）（-17.5< Mr <-22，0.025 < z <0.107），我们在匹配的光度、速度色散、颜色、颜色梯度或浓度指数下比较了活动星系核宿主星系和非活动星系核星系，以研究活动星系核活动与星系性质的关系。活动星系核样品是由窄发射线通量比大于6的II型活动星系核组成。我们发现，活动星系核所占的比例（f_AGN）强烈地依赖于星系的形态和颜色，而与宿主星系的光度和速度色散关系很弱。特别是在色固定的情况下，早型星系活动星系核的f_AGN几乎不受光度和速度色散的影响。活动星系核对早型宿主星系的偏好色为u-r ~2.0，对晚型宿主星系的偏好色为u-r=2.0-2.4。这一趋势表明，活动星系核主要由中等质量的晚型星系承载。我们还研究了吸积功率如何随星系性质而变化。虽然爱丁顿比（[OIII]线亮度归一化的黑洞质量）的范围超过三个数量级的形态类型，晚型星系是所有活动星系核功率的主导主机。在晚型星系中，蓝颜色的星系拥有更高功率的活动星系核。这些结果与一种假设是一致的，即更大质量和更红的星系更难容纳AGN，因为这些星系已经消耗了中心的气体，或者没有足够的气体供应来喂养黑洞。相比之下，中等质量、中等颜色和更集中的晚型星系更有可能拥有活动星系核，这意味着可能有一部分低质量、蓝色和不太集中的晚型星系可能没有大质量黑洞，或者可能拥有非常低功率的活动星系核。
Spider-Webb: Spatially-Resolved Evidence of Inside-Out Quenching in the Spiderweb Protocluster at $z \sim 2$
National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies（高级研究院）；Tohoku University（东北大学）；Waseda University（早稻田大学）
GMP-selected dual and lensed AGNs: selection function and classification based on near-IR colors and resolved spectra from VLT/ERIS, KECK/OSIRIS, and LBT/LUCI
Environmental dependence of galaxy properties in the southern GAMA regions
Indian Space Research Organisation（印度空间研究组织）；National Centre for Nuclear Research（国家核研究中心）；University of the Witwatersrand（威特沃特斯兰德大学）；The University of Western Australia（西澳大利亚大学）；Jagiellonian University（雅盖隆大学）；University of KwaZulu-Natal（夸祖鲁-纳塔尔大学）
The miniJPAS survey: Dissecting galaxy properties across environments with spatially resolved photometry
Universidade Federal de Santa Catarina（圣卡塔琳娜联邦大学）；University of Heidelberg（海德堡大学）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）；Unidad Asociada “Grupo de Astrofísica Extragaláctica y Cosmología”, IFCA-CSIC/Universitat de València（IFCA-CSIC/瓦伦西亚大学联合单位“河外天体物理学与宇宙学组”）；Instituto de Física, Universidade de São Paulo（圣保罗大学物理研究所）；Observatório Nacional – MCTI (ON)（国家天文台）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克尔巴斯克，巴斯克科学基金会）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理学研究中心）
Environmental Regulation of Dust and Star Formation Unveiled by Subaru Dual Narrow-band Imaging: Degree-scale Balmer Decrement Mapping across a z = 0.9 Supercluster
Tohoku University（东北大学）；Gemini Observatory, NSF NOIRLab（吉米天文台，美国国家光学红外天文实验室）；University of California, Davis（加州大学戴维斯分校）；Kwansei Gakuin University（关西学院大学）；The Graduate University for Advanced Studies（日本高等研究院）；National Astronomical Observatory of Japan（日本国立天文台）；Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences（昴星望远镜，日本国立天文台，日本国立自然科学研究所）；Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency（宇宙科学研究所，日本宇宙航空研究开发机构）；University of Hawai’i（夏威夷大学）；The University of Tokyo（东京大学）
Large-scale and local environmental drivers of quenching: tracing H$α$ concentration in X-ray and optical galaxy groups
The University of Sydney（悉尼大学）；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）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Beijing Normal University（北京师范大学）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）
Special Astrophysical Observatory of the Russian Academy of Sciences（俄罗斯科学院特别天文台）；Saint Petersburg State University（圣彼得堡国立大学）；Institute for Astronomy, University of Hawaii（夏威夷大学天体物理研究所）；Space Telescope Science Institute（太空望远镜科学研究所）
