JWST/MIRI Simulated Imaging: Insights into Obscured Star-Formation and AGN for Distant Galaxies in Deep Surveys
Guang Yang, Casey Papovich, Micaela B. Bagley, Veronique Buat, Denis Burgarella, Mark E. Dickinson, David Elbaz, Steven L. Finkelstein, Adriano Fontana, Norman … 展开作者
Guang Yang, Casey Papovich, Micaela B. Bagley, Veronique Buat, Denis Burgarella, Mark E. Dickinson, David Elbaz, Steven L. Finkelstein, Adriano Fontana, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Allison Kirkpatrick, Pablo G. Pérez-González, Norbert Pirzkal, L. Y. Aaron Yung
备注：
31 pages, 24 figures, 3 tables. Re-submitted to ApJS after revision
The JWST MIRI instrument will revolutionize extragalactic astronomy with unprecedented sensitivity and angular resolution in mid-IR. Here, we assess the potential of MIRI photometry to constrain galaxy properties in the Cosmic Evolution Early Release Science (CEERS) survey. We derive estimated MIRI fluxes from the spectral energy distributions (SEDs) of real sources that fall in a planned MIRI pointing. We also obtain MIRI fluxes for hypothetical AGN-galaxy mixed models varying the AGN fractional contribution to the total IR luminosity ($\rm frac_{AGN}$). Based on these model fluxes, we simulate CEERS imaging (3.6-hour exposure) in 6 bands from F770W to F2100W using MIRISIM, and reduce these data using JWST PIPELINE. We perform PSF-matched photometry with TPHOT, and fit the source SEDs with X-CIGALE, simultaneously modeling photometric redshift and other physical properties. Adding the MIRI data, the accuracy of both redshift and $\rm frac_{AGN}$ is generally improved by factors of $\gtrsim 2$ for all sources at $z\lesssim 3$. Notably, for pure-galaxy inputs ($\rm frac_{AGN}=0$), the accuracy of $\rm frac_{AGN}$ is improved by $\sim 100$ times thanks to MIRI. The simulated CEERS MIRI data are slightly more sensitive to AGN detections than the deepest X-ray survey, based on the empirical $L_{\rm X}$-$L_{\rm 6μm}$ relation. Like X-ray observations, MIRI can also be used to constrain the AGN accretion power (accuracy $\approx 0.3$ dex). Our work demonstrates that MIRI will be able to place strong constraints on the mid-IR luminosities from star formation and AGN, and thereby facilitate studies of the galaxy/AGN co-evolution.
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）
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…
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）
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）
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）
Compact Obscured Nuclei (CONs) potentially hide extreme supermassive black hole (SMBH) growth behind large column densities of gas/dust. We present a spectroscopic analysis of the heavily obscured nucleus and the surrounding environment of the eastern region of the nearby ($z = 0.02007$) interacting galaxy VV 114 with the JWST Mid-InfraRed Instrument (MIRI). We model the spectrum from 4.9 - 28 $μ$m to extract Polycyclic Aromatic Hydrocarbon (PAH) emission and the underlying obscured continuum. We find that the NE nucleus (A) is highly obscured where the low PAH equivalent width (EW) ratio, EW(…
Until now, our knowledge of the extragalactic Universe at mid-IR wavelengths (> 5 microns) was limited to rare active galactic nuclei (AGN) and the brightest normal galaxies up to z~3. The advent of the JWST with its Mid-Infrared Instrument (MIRI) will revolutionise the ability of the mid-IR regime as a key wavelength domain to probe the high-z Universe. In this work we present a first study of JWST MIRI 7.7 micron sources selected with > 3 sigma significance from the lensing cluster field SMACS J0723.3-7327. We model their spectral energy distribution fitting with 13 JWST and HST broad bands,…
MEOW: The increase in the obscured AGN fraction in mid-infrared from 0 < z < 6 with JWST MIRI
Massachusetts Institute of Technology（麻省理工学院）；Kavli Institute for Astrophysics and Space Research（卡弗里天体物理学与空间研究所）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家航空航天技术研究所/西班牙高等科学研究理事会）；Department of Physics, University of the Pacific（太平洋大学物理系）；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）
利用JWST MIRI数据，研究发现0 < z < 6范围内 obscured AGN 分数随红移增加而显著上升，揭示了光学/紫外波段无法检测到的大量被尘埃遮蔽的AGN。
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）
JWST MIRI-MRS observations of the Red Rectangle: AIB class transformation in the outer nebula
The University of Western Ontario（韦仕敦大学）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内克天文研究所）；University of Nottingham（诺丁汉大学）；University of Toledo（托莱多大学）；KU Leuven（荷语鲁汶大学）
A Characterization of JWST MIRI Detector Persistence and Implications for High-Contrast Imaging
University of Michigan（密歇根大学）；Massachusetts Institute of Technology（麻省理工学院）；Eureka Scientific Inc.（尤里卡科学公司）；JHU Applied Physics Laboratory（约翰霍普金斯大学应用物理实验室）
The origin of complex organic molecules (COMs) in young Class 0 protostars has been one of the major questions in astrochemistry and star formation. While COMs are thought to form on icy dust grains via gas-grain chemistry, observational constraints on their formation pathways have been limited to gas-phase detection. Sensitive mid-infrared spectroscopy with JWST enables unprecedented investigation of COM formation by measuring their ice absorption features. We present an overview of JWST/MIRI MRS spectroscopy and imaging of a young Class 0 protostar, IRAS 15398-3359, and identify several majo…
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 …
The bulk of the stellar growth over cosmic time is dominated by IR luminous galaxies at cosmic noon (z=1-2), many of which harbor a hidden active galactic nucleus (AGN). We use state of the art infrared color diagnostics, combining Spitzer and Herschel observations, to separate dust-obscured AGN from dusty star forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24 micron counts of SFGs, AGN/star forming "Composites", and AGN. AGN and Composites dominate the counts above 0.8 mJy at 24 micron, and Composites form at least 25% of an IR sample even to faint detection limits. W…
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…
PDRs4All XXIII. JWST-MIRI template spectra of PAHs in the Orion Bar obtained with blind signal separation
Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, Centre National de la Recherche Scientifique (CNRS), Centre National d’Etudes Spatiales（天体物理学与行星学研究所，图卢兹大学，法国国家科学研究中心，法国国家空间研究中心）；NASA Ames Research Center（美国宇航局艾姆斯研究中心）；Centro de Astrobiología (CAB), INTA-CSIC（航空天文学中心（CAB），西班牙国家航空航天技术研究所-西班牙国家研究委员会）；Instituto de Física Fundamental (CSIC)（基础物理研究所（CSIC））；Institut d’Astrophysique Spatiale, Université Paris-Saclay, CNRS（天体物理研究所，巴黎萨克雷大学，法国国家科学研究中心）；Department of Astronomy, Graduate School of Science, The University of Tokyo（东京大学理学研究科天文学系）
The Mid-Infrared Instrument (MIRI) on-board JWST will provide imaging, coronagraphy, low-resolution spectroscopy and medium-resolution spectroscopy at unprecedented sensitivity levels in the mid-infrared wavelength range. The Medium-Resolution Spectrometer (MRS) of MIRI is an integral field spectrograph that provides diffraction-limited spectroscopy between 4.9 and 28.3 um, within a FOV varying from 13 to 56" square. From ground testing, we calculate the physical parameters essential to general observers and calibrating the wavelength solution and resolving power of the MRS is critical for max…
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）
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）
Silicate emission in a type-2 quasar: JWST/MIRI constraints on torus geometry and radiative feedback
Instituto de Astrofísica de Canarias（加那利天体物理学研究所）；Universidad de La Laguna（拉古纳大学）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家研究委员会-国家航空航天技术研究所天体生物学中心）；University of South Carolina（南卡罗来纳大学）；Stanford University（斯坦福大学）；University of Southampton（南安普顿大学）；Observatorio Astronómico Nacional (OAN-IGN（国家天文台（ IGN））
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）
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）
Using MIRI on-board JWST we present mid-infrared sub-arcsec imaging (MIRIM) and spectroscopy (MRS) of the hyperluminous infrared system SPT0311-58 at z=6.9. MIRI observations are compared with existing ALMA far-infrared continuum and [CII]158$μ$m imaging. Even though the ALMA observations suggests very high star formation rates (SFR) in the eastern (E) and western (W) galaxies of the system, the H$α$ line is not detected. This, together with the detection of the Pa$α$ line, implies very high optical nebular extinction with lower limits of 4.2 (E) and 3.9 mag (W), and even larger 5.6 (E) and 10…
JWST reveals the diversity of nuclear obscuring dust in nearby AGN: nuclear isolation of MIRI/MRS datacubes and continuum spectral fitting
Instituto de Radioastrononomía y Astrofísica (IRyA), Universidad Nacional Autónoma de México（墨西哥国立自治大学射电天文学与天体物理研究所）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所/西班牙高等科学研究理事会天体生物学中心）；Department of Physics & Astronomy, University of South Carolina（南卡罗来纳大学物理与天文系）；Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；Instituto de Astrofśica de Canarias（加那利群岛天体物理研究所）；Departamento de Astrofísica, Universidad de La Laguna（拉帕尔马大学天体物理学系）
The James Webb Space Telescope's Medium Resolution Spectrometer (MRS), will offer nearly 2 orders of magnitude improvement in sensitivity and >3X improvement in spectral resolution over our previous space-based mid-IR spectrometer, the Spitzer IRS. In this paper, we make predictions for spectroscopic pointed observations and serendipitous detections with the MRS. Specifically, pointed observations of Herschel sources require only a few minutes on source integration for detections of several star-forming and active galactic nucleus lines, out to z$=$3 and beyond. But the same data will also inc…
JWST Observations of Starbursts: The motion of dust - PAH kinematics of M82 and NGC 253 with JWST/MIRI spectroscopy
University of California San Diego（加州大学圣地亚哥分校）；University of Maryland（马里兰大学）；Joint Space-Science Institute（空间科学联合研究所）；Princeton University（普林斯顿大学）；University of Toledo（托莱多大学）；Universität Heidelberg（海德堡大学）；University of Kansas（堪萨斯大学）；University of Pittsburgh（匹兹堡大学）
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 …
