Imaging with the James Webb Space Telescope (JWST) will allow for observing the bulk of distant galaxies at the epoch of reionisation. The recovery of their properties, such as age, color excess E(B-V), specific star formation rate (sSFR) and stellar mass, will mostly rely on spectral energy distribution fitting, based on the data provided by JWST's two imager cameras, namely the Near Infrared Camera (NIRCam) and the Mid Infrared Imager (MIRI). In this work we analyze the effect of choosing different combinations of NIRCam and MIRI broad-band filters, from 0.6 μm to 7.7 μm, on the recovery of these galaxy properties. We performed our tests on a sample of 1542 simulated galaxies, with known input properties, at z=7-10. We found that, with only 8 NIRCam broad-bands, we can recover the galaxy age within 0.1 Gyr and the color excess within 0.06 mag for 70% of the galaxies. Besides, the stellar masses and sSFR are recovered within 0.2 and 0.3 dex, respectively, at z=7-9. Instead, at z=10, no NIRCam band traces purely the λ> 4000 Å regime and the percentage of outliers in stellar mass (sSFR) increases by > 20% (> 90%), in comparison to z=9. The MIRI F560W and F770W bands are crucial to improve the stellar mass and the sSFR estimation at z=10. When nebular emission lines are present, deriving correct galaxy properties is challenging, at any redshift and with any band combination. In particular, the stellar mass is systematically overestimated in up to 0.3 dex on average with NIRCam data alone and including MIRI observations improves only marginally the estimation.
Estimating Photometric Distances to Ultracool Dwarfs in Next Generation Space-based Infrared Surveys: Synthetic Photometry and New Absolute Magnitude Versus Spectral Type Relations for JWST, Euclid, and Roman Filters
JWST MIRI color classification of mid-infrared selected galaxies: MIRI color classification toward cosmic noon
Department of Astronomy and Space Sciences, Science Faculty, İstanbul University（伊斯坦布尔大学理学院天文学与空间科学系）；Institute of Astronomy, National Tsing Hua University（国立清华大学天文研究所）；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）；Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies)（日本综合研究大学院大学天文学科学系）；National Astronomical Observatory of Japan（日本国立天文台）；Department of Physics, National Chung Hsing University（国立中兴大学物理系）；Research School of Astronomy and Astrophysics, The Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Sabancı University, Faculty of Engineering and Natural Sciences（萨班哲大学工程与自然科学学院）
The Stellar Populations and Rest-Frame Colors of Star-Forming Galaxies at $z \approx 8$: Exploring the Impact of Filter Choice and Star Formation History Assumption with JADES
The TRGB-SBF Project. IV. A Color Calibration of the TRGB in the JWST F090W+F150W Filters
Special Astrophysical Observatory of the Russian Academy of Sciences（俄罗斯科学院特别天文台）；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）；NSF’s NOIRLab（美国国家科学基金会NOIR实验室）；Utah Valley University（犹他谷大学）
Observing the host galaxies of high-redshift quasars with JWST: predictions from the BlueTides simulation
高红移类星体发出的明亮辐射在静止坐标系的紫外/光学波段完全掩盖了它们的宿主星系，甚至哈勃太空望远镜（HST）也无法利用详细的点扩散函数（PSF）建模技术来探测这些波长的宿主星系。在这项研究中，我们产生模拟图像的样本z=7类星体提取的BlueTides模拟，并应用马尔可夫链蒙特卡洛为基础的PSF建模，以确定其宿主星系的可探测性与詹姆斯韦伯太空望远镜（JWST）。虽然没有统计学意义的检测与HST，我们预测，在相同的波长和曝光时间JWST近红外相机成像将检测到约50%的类星体宿主星系。我们研究了各种观测策略，发现长波长滤波器中的NIRCam宽带成像导致成功探测类星体宿主的比例最高，在5 ks的曝光时间内探测到>80%的明亮类星体宿主。在NIRCam宽波段滤波器中，需要约5 k s的曝光时间来探测大多数宿主星系，然而，即使用MIRI进行10 k s的曝光，也会导致<30%的宿主星系探测成功。我们发现星系的属性和它们的可探测性之间没有显着的趋势。PSF模型可以准确地恢复主机的大小，半径和空间分布的大规模的发射，占中央核心被污染的残余类星体通量。在解释使用PSF建模测量的主机属性时应小心。
JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: NIRCam Imaging in GOODS-S and GOODS-N
Department of Astronomy and Astrophysics, University of California, Santa Cruz（加州大学圣克鲁兹分校天文与天体物理系）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
JWST Whirlpool Galaxy Treasury: Mid-Infrared Emission in M51 and its Relation to Gas Column and Star Formation
University of California, San Diego（加州大学圣地亚哥分校）；University of Wyoming（怀俄明大学）；The Ohio State University（俄亥俄州立大学）；National Radio Astronomy Observatory（国家射电天文台）；Stockholm University（斯德哥尔摩大学）；Whitman College（惠特曼学院）；European Space Agency（欧洲空间局）；Space Telescope Science Institute（太空望远镜科学研究所）
The JWST Resolved Stellar Populations Early Release Science Program. IX. The RR Lyrae Population in WLM with HST and JWST
Minnesota Institute for Astrophysics, University of Minnesota（明尼苏达大学天体物理研究所）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics and Astronomy, Rutgers, the State University of New Jersey（新泽西州立大学罗格斯大学物理与天文系）
Disk-like galaxies at 4 < z < 7.7 : JWST/NIRCam morphologies revealed by denoising VAE-GCNN classification
Center for Cosmology and Astrophysics, Alikhanyan National Laboratory（阿利哈尼扬国家实验室宇宙学与天体物理中心）；Yerevan State University（埃里温国立大学）；SIA, Sapienza University of Rome（罗马智慧大学天体物理研究所）
研究利用去噪VAE-GCNN分类方法分析JWST/NIRCam多滤光片切片，确定红移4 < z < 7.7范围内盘状星系占比为0.34，揭示高红移星系中盘状结构的重要性。
JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: Catalogs of inferred morphological properties of galaxies from JWST/NIRCam imaging in GOODS-N and GOODS-S
University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of Cambridge（剑桥大学）；University of Arizona（亚利桑那大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；University of Hertfordshire（赫特福德大学）；The Johns Hopkins University（约翰斯·霍普金斯大学）；University College London（伦敦大学学院）；Space Telescope Science Institute（太空望远镜科学研究所）；NSF National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）
Black Holes in the Shadow: The Missing High-Ionization Lines in the Earliest JWST AGNs
Università degli Studi di Milano-Bicocca（米兰比可卡大学）；Stockholm University（斯德哥尔摩大学）；University of Cambridge（剑桥大学）；University College London（伦敦大学学院）；University of California Santa Cruz（加州大学圣克鲁兹分校）
A New Window on the Hα Luminosity Function and Star Formation Rate Density from 1.2 < z < 6.6 from JWST Medium-Band Photometry
University of Ljubljana（卢布尔雅那大学）；NRC Herzberg（国家研究委员会赫茨伯格研究所）；University of Toronto（多伦多大学）；University of California Davis（加州大学戴维斯分校）；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）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）
