Life beyond 30: probing the -20<M_UV<-17 luminosity function at 8<z<13 with the NIRCam parallel field of the MIRI Deep Survey
Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Noorgaard-Nielsen… 展开作者
Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Noorgaard-Nielsen, Thomas Greve, Göran Ostlin, Gillian Wright, Almudena Alonso-Herrero, Javier Álvarez-Márquez, Karina I. Caputi, Andreas Eckart, Olivier Le Fèvre, Álvaro Labiano, Macarena García-Marín, Jens Hjorth, Sarah Kendrew, John P. Pye, Tuomo Tikkanen, Paul van der Werf, Fabian Walter, Martin Ward, Arjan Bik, Leindert Boogaard, Sarah E. I. Bosman, Alejandro Crespo Gómez, Steven Gillman, Edoardo Iani, Iris Jermann, Jens Melinder, Romain A. Meyer, Thibaud Moutard, Ewine van Dishoek, Thomas Henning, Pierre-Olivier Lagage, Manuel Guedel, Florian Peissker, Tom Ray, Bart Vandenbussche, Ángela García-Argumánez, Rosa María Mérida
备注：
Accepted for publication in ApJL, in memoriam Hans Ulrik Noorgaard-Nielsen and Olivier Le Fèvre
We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at $8<z<13$ derived from deep NIRCam observations taken in parallel with the MIRI Deep Survey (MDS) of the Hubble Ultra Deep Field (HUDF), NIRCam covering the parallel field 2 (HUDF-P2). Our deep (40 hours) NIRCam observations reach a F277W magnitude of 30.8 ($5σ$), more than 2 magnitudes deeper than JWST public datasets already analyzed to find high redshift galaxies. We select a sample of 44 $z>8$ galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at $z>8$, good fits based on $χ^2$ calculations, and predominant solutions compared to $z<8$ alternatives. We find mild evolution in the luminosity function from $z\sim13$ to $z\sim8$, i.e., only a small increase in the average number density of $\sim$0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values $α=-2.2\pm0.1$ and $M^*=-20.8\pm0.2$ mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses $\sim10^8$ M$_\odot$ during the first 350 Myr of the Universe, $z\sim12$, with models matching better the luminosity density observational estimations $\sim$150 Myr later, by $z\sim9$.
The determination of galaxy redshifts in James Webb Space Telescope (JWST)'s blank-field surveys will mostly rely on photometric estimates, based on the data provided by JWST's Near-Infrared Camera (NIRCam) at 0.6-5.0 μm and Mid Infrared Instrument (MIRI) at λ>5.0 μm. In this work we analyse the impact of choosing different combinations of NIRCam and MIRI broad-band filters (F070W to F770W), as well as having ancillary data at λ<0.6 μm, on the derived photometric redshifts (zphot) of a total of 5921 real and simulated galaxies, with known input redshifts z=0-10. We found that observations at λ…
AGNBoost: A Machine Learning Approach to AGN Identification with JWST/NIRCam+MIRI Colors and Photometry
University of Kansas（堪萨斯大学）；Rochester Institute of Technology（罗切斯特理工学院）；Colby College（科尔比学院）；Space Telescope Science Institute（太空望远镜科学研究所）；NASA-Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Texas A&M University（得克萨斯农工大学）
We make use of \textit{JWST} medium and broad-band NIRCam imaging, along with ultra-deep MIRI $5.6 \rm μm$ imaging, in the Hubble eXtreme Deep Field (XDF) to identify prominent line emitters at $z\simeq 7-8$. Out of a total of 58 galaxies at $z\simeq 7-8$, we find 18 robust candidates ($\simeq$31\%) for (H$β$ + [OIII]) emitters, based on their enhanced fluxes in the F430M and F444W filters, with EW$_{0}$(H$β$ +[OIII]) $\simeq 87 - 2100$ Å. Among these emitters, 16 lie in the MIRI coverage area and 12 exhibit a clear flux excess at $5.6 \, \rm μm$, indicating the simultaneous presence of a prom…
No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam
University of Nottingham（诺丁汉大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Edinburgh（爱丁堡大学）；University of St Andrews（圣安德鲁斯大学）
We present James Webb Space Telescope (JWST) imaging of NGC 7469 with the Near-Infrared Camera (NIRCam) and the Mid-InfraRed Instrument (MIRI). NGC 7469 is a nearby, $z=0.01627$, luminous infrared galaxy (LIRG) that hosts both a Seyfert Type-1.5 nucleus and a circumnuclear starburst ring with a radius of $\sim$0.5 kpc. The new near-infrared (NIR) JWST imaging reveals 66 star-forming regions, 37 of which were not detected by HST observations. Twenty-eight of the 37 sources have very red NIR colors that indicate obscurations up to A$_{\rm{v}}\sim7$ and a contribution of at least 25$\%$ from hot …
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 …
JWST NIRCam and MIRI Reveal the Dust-Producing AGB Population of NGC 6822
Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；UK Astronomy Technology Centre, Royal Observatory（英国天文技术中心，皇家天文台）；IPAC, California Institute of Technology（加州理工学院IPAC）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Department of Physics & Engineering Physics, Morgan State University（摩根州立大学物理与工程物理系）；Department of Physics, Maynooth University（梅努斯大学物理系）；Space Telescope Science Institute（太空望远镜科学研究所）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；SETI Institute（搜寻地外文明研究所）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, College Lane Campus, University of Hertfordshire（赫特福德大学College Lane校区物理、天文与数学系天体物理研究中心）
Multi-wavelength morphology and dust emission in low-redshift dwarf galaxies in COSMOS-Web with HST and JWST
University of Hertfordshire（赫特福德大学）；Rochester Institute of Technology（罗切斯特理工学院）；University of Manchester（曼彻斯特大学）；University of Nottingham（诺丁汉大学）；University of Cambridge（剑桥大学）
The Mid-Infrared Instrument (MIRI) for the {\em James Webb Space Telescope} (JWST) will revolutionize our understanding of infrared stellar populations in the Local Volume. Using the rich {\em Spitzer}-IRS spectroscopic data-set and spectral classifications from the Surveying the Agents of Galaxy Evolution (SAGE)-Spectroscopic survey of over a thousand objects in the Magellanic Clouds, the Grid of Red supergiant and Asymptotic giant branch star ModelS ({\sc grams}), and the grid of YSO models by Robitaille et al. (2006), we calculate the expected flux-densities and colors in the MIRI broadband…
To high redshift and low mass: exploring the emergence of quenched galaxies and their environments at $3<z<6$ in the ultra-deep JADES MIRI F770W parallel
We present a new analysis of the potential power of deep, near-infrared, imaging surveys with the James Webb Space Telescope (JWST) to improve our knowledge of galaxy evolution. In this work we properly simulate what can be achieved with realistic survey strategies, and utilise rigorous signal:noise calculations to calculate the resulting posterior constraints on the physical properties of galaxies. We explore a broad range of assumed input galaxy types (>20,000 models, including extremely dusty objects) across a wide redshift range (out to z~12), while at the same time considering a realistic…
Ages of the resolved stellar populations inside the JWST/MIRI bubbles in NGC 628
Instituto Nacional de Astrofísica, Óptica y Electrónica（墨西哥国家天体物理学、光学和电子学研究所）；SISSA（国际高等研究学院）；Osservatorio Astronomico di Padova—INAF（帕多瓦天文台-意大利国家天体物理研究所）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Instituto de Astrofísica de Andalucía – Consejo Superior de Investigaciones Científicas (IAA-CSIC)（安达卢西亚天体物理研究所-西班牙最高科学研究委员会）；Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文研究所）
Modeling the JWST MIRI Counts, Insights Into the Source Properties and Role of Dust-Obscured AGN
Tufts University（塔夫茨大学）；Université de Strasbourg, CNRS, Observatoire Astronomique de Strasbourg（斯特拉斯堡大学、法国国家科学研究中心、斯特拉斯堡天文台）；Winona State University（威诺纳州立大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）
The Stellar Population of NGC 346 in the Small Magellanic Cloud with JWST
Maynooth University（梅努斯大学）；Dublin Institute for Advanced Studies（都柏林高等研究院）；European Space Research and Technology Centre（欧洲空间研究与技术中心）；University of Edinburgh（爱丁堡大学）；Royal Observatory（皇家天文台）；California Institute of Technology（加州理工学院）；AURA for the European Space Agency, ESA Office, STScI（美国大学研究协会（代表欧洲航天局，ESA办公室，STScI））；Space Telescope Science Institute（太空望远镜科学研究所）；Morgan State University（摩根州立大学）；INAF, Astronomical Observatory of Rome（意大利国家天体物理研究所，罗马天文台）
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 MIRI Early Obscured-AGN Wide Survey (MEOW): A Population of Hidden AGN at $z \gtrsim 5$ Revealed by JWST/MIRI Imaging
MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理与空间研究所）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；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）；University of the Pacific（太平洋大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家研究委员会-国家航空航天技术研究所）
We present predictions for the outcome of deep galaxy surveys with the $James$ $Webb$ $Space$ $Telescope$ ($JWST$) obtained from a physical model of galaxy formation in $Λ$CDM. We use the latest version of the GALFORM model, embedded within a new ($800$ Mpc)$^{3}$ dark matter only simulation with a halo mass resolution of $M_{\rm halo}>2\times10^{9}$ $h^{-1}$ M$_{\odot}$. For computing full UV-to-mm galaxy spectral energy distributions, including the absorption and emission of radiation by dust, we use the spectrophotometric radiative transfer code GRASIL. The model is calibrated to reproduce …
A census of quiescent galaxies across $0.5 < z < 8$ with JWST/MIRI: Mass-dependent number density evolution of quiescent galaxies in the early Universe
Nanjing University（南京大学）；Tianjin Normal University（天津师范大学）
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）
JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: MIRI Coordinated Parallels in GOODS-S and GOODS-N
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；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）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文学和数学系天体物理研究中心）；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）；Department of Physics and Astronomy, The Johns Hopkins University（约翰斯·霍普金斯大学物理与天文学系）；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文与天体物理学系）
Probing Direct Contributions of Galaxies and AGN to Cosmic Reionization in a Quasar Field J0226+0302 with JWST NIRCam and NIRSpec
University of Michigan（密歇根大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所黎明中心）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学宇宙起源研究核心理论研究中心）；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学宇宙起源研究核心理论中心数据驱动发现中心）；Department of Physics & Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）
An Archival Calibration of JWST/MIRI Prism Wide-Field Slitless Spectroscopy: Methodology, Performance, and a Mid-Infrared Spectral Atlas of Galaxies at $z=0-4$ in the GOODS-N/S Fields
Westlake University（西湖大学）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所与高等科学研究中心天体生物学中心）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Astronomy and Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文学与天体物理学系）；Tsinghua University（清华大学）
Probing the IMF in the Early Universe -- Direct measurements in the Boötes I UFD with JWST/NIRCam
University of Maryland, College Park（马里兰大学帕克分校）；Space Telescope Science Institute（太空望远镜科学研究所）；INAF – Osservatorio Astronomico di Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；INFN – Sezione di Pisa, Universita’ di Pisa（意大利国家核物理研究所比萨分部，比萨大学）
通过JWST/NIRCam对Boötes I UFD中低质量IMF进行研究，结合机器学习和统计方法，发现单幂律IMF无法再现观测到的光度函数，而分段幂律和对数正态IMF参数与银河系一致，表明低金属度下恒星形成遵循相似IMF。
University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；National Center for Supercomputing Applications, University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校国家超级计算应用中心）；University of Pennsylvania（宾夕法尼亚大学）；UC San Diego（加州大学圣地亚哥分校）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Princeton University（普林斯顿大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
Detection of new galaxy candidates at z > 11 in the JADES field using JWST NIRCam
Department of Physics, University of Arkansas（阿肯色大学物理系）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究研究所）；Stony Brook University（石溪大学）
CHAMPS: The COSMOS High-Redshift ALMA-MIRI Population Survey - A New Census of the Dusty Early Universe
California Institute of Technology（加州理工学院）；Rochester Institute of Technology（罗切斯特理工学院）；Universidad Diego Portales（迭戈帕托莱斯大学）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；The University of Tokyo（东京大学）
