PHANGS-JWST First Results: Stellar Feedback-Driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, Eric Emsellem, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glo… 展开作者
Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, Eric Emsellem, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley. T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
备注：
19 pages, 7 figures and 2 tables in total (12 pages and 6 figures in main text). Accepted as part of a PHANGS-JWST Focus Issue to appear in ApJL
We compare embedded young massive star clusters (YMCs) to (sub-)millimeter line observations tracing the excitation and dissociation of molecular gas in the starburst ring of NGC 1365. This galaxy hosts one of the strongest nuclear starbursts and richest populations of YMCs within 20 Mpc. Here we combine near-/mid-IR PHANGS-JWST imaging with new ALMA multi-J CO (1-0, 2-1 and 4-3) and [CI](1-0) mapping, which we use to trace CO excitation via R42 = I_CO(4-3)/I_CO(2-1) and R21 = I_CO(2-1)/I_CO(1-0) and dissociation via RCICO = I_[CI](1-0)/I_CO(2-1) at 330 pc resolution. We find that the gas flowing into the starburst ring from northeast to southwest appears strongly affected by stellar feedback, showing decreased excitation (lower R42) and increased signatures of dissociation (higher RCICO) in the downstream regions. There, radiative transfer modeling suggests that the molecular gas density decreases and temperature and [CI/CO] abundance ratio increase. We compare R42 and RCICO with local conditions across the regions and find that both correlate with near-IR 2 um emission tracing the YMCs and with both PAH (11.3 um) and dust continuum (21 um) emission. In general, RCICO exhibits ~ 0.1 dex tighter correlations than R42, suggesting CI to be a more sensitive tracer of changing physical conditions in the NGC 1365 starburst than CO (4-3). Our results are consistent with a scenario where gas flows into the two arm regions along the bar, becomes condensed/shocked, forms YMCs, and then these YMCs heat and dissociate the gas.
JWST/MIRI imaging of the nearby galaxies IC 5332, NGC 628, NGC 1365 and NGC 7496 from PHANGS reveals a richness of gas structures that in each case form a quasi-regular network of interconnected filaments, shells and voids. We examine whether this multi-scale network of structure is consistent with the fragmentation of the gas disk through gravitational instability. We use FilFinder to detect the web of filamentary features in each galaxy and determine their characteristic radial and azimuthal spacings. These spacings are then compared to estimates of the most Toomre-unstable length (a few kpc…
Polycyclic aromatic hydrocarbons (PAHs) play a critical role in the reprocessing of stellar radiation and in balancing the heating and cooling processes in the interstellar medium (ISM), but appear to be destroyed in HII regions. However, the mechanisms driving their destruction are still not completely understood. Using PHANGS-JWST and PHANGS-MUSE observations, we investigate how the PAH fraction changes in about 1500 HII regions across four nearby star-forming galaxies (NGC 628, NGC 1365, NGC 7496, IC 5332). We find a strong anti-correlation between the PAH fraction and the ionization parame…
The earliest stages of star formation occur enshrouded in dust and are not observable in the optical. Here we leverage the extraordinary new high-resolution infrared imaging from JWST to begin the study of dust-embedded star clusters in nearby galaxies throughout the local volume. We present a technique for identifying dust-embedded clusters in NGC 7496 (18.7 Mpc), the first galaxy to be observed by the PHANGS-JWST Cycle 1 Treasury Survey. We select sources that have strong 3.3$μ$m PAH emission based on a $\rm F300M-F335M$ color excess, and identify 67 candidate embedded clusters. Only eight o…
Tracing the earliest stages of star and cluster formation in 19 nearby galaxies with PHANGS-JWST and HST: compact 3.3 $μ$m PAH emitters and their relation to the optical census of star clusters
We present a comparison of theoretical predictions of dust continuum and polycyclic aromatic hydrocarbon (PAH) emission with new JWST observations in three nearby galaxies: NGC 628, NGC 1365, and NGC 7496. Our analysis focuses on a total of 1063 compact stellar clusters and 2654 stellar associations previously characterized by HST in the three galaxies. We find that the distributions and trends in the observed PAH-focused infrared colors generally agree with theoretical expectations, and that the bulk of the observations is more aligned with models of larger, ionized PAHs. These JWST data ushe…
The PHANGS collaboration has been building a reference dataset for the multi-scale, multi-phase study of star formation and the interstellar medium in nearby galaxies. With the successful launch and commissioning of JWST, we can now obtain high-resolution infrared imaging to probe the youngest stellar populations and dust emission on the scales of star clusters and molecular clouds ($\sim$5-50 pc). In Cycle 1, PHANGS is conducting an 8-band imaging survey from 2-21$μ$m of 19 nearby spiral galaxies. CO(2-1) mapping, optical integral field spectroscopy, and UV-optical imaging for all 19 galaxies…
We use PHANGS-JWST data to identify and classify 1271 compact 21 $μ$m sources in four nearby galaxies using MIRI F2100W data. We identify sources using a dendrogram-based algorithm, and we measure the background-subtracted flux densities for JWST bands from 2 $μ$m to 21 $μ$m. Using the SED in JWST as well as HST bands, plus ALMA and MUSE/VLT observations, we classify the sources by eye. Then we use this classification to define regions in color-color space, and so establish a quantitative framework for classifying sources. We identify 1085 sources as belonging to the ISM of the target galaxies…
JWST observations of polycyclic aromatic hydrocarbon (PAH) emission provide some of the deepest and highest resolution views of the cold interstellar medium (ISM) in nearby galaxies. If PAHs are well mixed with the atomic and molecular gas and illuminated by the average diffuse interstellar radiation field, PAH emission may provide an approximately linear, high resolution, high sensitivity tracer of diffuse gas surface density. We present a pilot study that explores using PAH emission in this way based on MIRI observations of IC 5332, NGC 628, NGC 1365, and NGC 7496 from the PHANGS-JWST Treasu…
PHANGS-JWST mid-infrared (MIR) imaging of nearby spiral galaxies has revealed ubiquitous filaments of dust emission in intricate detail. We present a pilot study to systematically map the dust filament network (DFN) at multiple scales between 25-400 pc in NGC 628. MIRI images at 7.7, 10, 11.3 and 21$μ$m of NGC 628 are used to generate maps of the filaments in emission, while PHANGS-HST B-band imaging yields maps of dust attenuation features. We quantify the correspondence between filaments traced by MIR thermal continuum / polycyclic aromatic hydrocarbon (PAH) emission and filaments detected v…
The first JWST observations of nearby galaxies have unveiled a rich population of bubbles that trace the stellar feedback mechanisms responsible for their creation. Studying these bubbles therefore allows us to chart the interaction between stellar feedback and the interstellar medium, and the larger galactic flows needed to regulate star formation processes globally. We present the first catalog of bubbles in NGC628, visually identified using MIRI F770W PHANGS-JWST observations, and use them to statistically evaluate bubble characteristics. We classify 1694 structures as bubbles with radii be…
Ratios of polycyclic aromatic hydrocarbon (PAH) vibrational bands are a promising tool for measuring the properties of the PAH population and their effect on star formation. The photometric bands of the MIRI and NIRCam instruments on JWST provide the opportunity to measure PAH emission features across entire galaxy disks at unprecedented resolution and sensitivity. Here we present the first results of this analysis in a sample of three nearby galaxies: NGC 628, NGC 1365, and NGC 7496. Based on the variations observed in the 3.3, 7.7, and 11.3 $μ$m features, we infer changes to the average PAH …
We explore the relationship between mid-infrared (mid-IR) and CO rotational line emission from massive star-forming galaxies, which is one of the tightest scalings in the local universe. We assemble a large set of unresolved and moderately ($\sim 1$ kpc) spatially resolved measurements of CO (1-0) and CO (2-1) intensity, $I_{\rm CO}$, and mid-IR intensity, $I_{\rm MIR}$, at 8, 12, 22, and 24$μ$m. The $I_{\rm CO}$ vs. $I_{\rm MIR}$ relationship is reasonably described by a power law with slopes $0.7{-}1.2$ and normalization $I_{\rm CO} \sim 1$ K km s$^{-1}$ at $I_{\rm MIR} \sim 1$ MJy sr$^{-1}$…
We combine archival HST and new JWST imaging data, covering the ultraviolet to mid-infrared regime, to morphologically analyze the nuclear star cluster (NSC) of NGC 628, a grand-design spiral galaxy. The cluster is located in a 200 pc x 400 pc cavity, lacking both dust and gas. We find roughly constant values for the effective radius (r_eff ~ 5 pc) and ellipticity (ε ~ 0.05), while the Sérsic index (n) and position angle (PA) drop from n ~ 3 to ~ 2 and PA ~ 130° to 90°, respectively. In the mid-infrared, r_eff ~ 12pc, ε ~ 0.4, and n ~ 1-1.5, with the same PA ~ 90°. The NSC has a stellar mass o…
A primary new capability of JWST is the ability to penetrate the dust in star forming galaxies to identify and study the properties of young star clusters that remain embedded in dust and gas. In this paper we combine new infrared images taken with JWST with our optical HST images of the star-bursting barred (Seyfert2) spiral galaxy NGC 1365. We find that this galaxy has the richest population of massive young clusters of any known galaxy within 30 Mpc, with $\sim$ 30 star clusters that are more massive than 10$^6$ Msolar and younger than 10 Myr. Sixteen of these clusters are newly discovered …
Time-scales of polycyclic aromatic hydrocarbon and dust continuum emission from gas clouds compared to molecular gas cloud lifetimes in PHANGS-JWST galaxies
The earliest stages of star formation, when young stars are still deeply embedded in their natal clouds, represent a critical phase in the matter cycle between gas clouds and young stellar regions. Until now, the high-resolution infrared observations required for characterizing this heavily obscured phase (during which massive stars have formed, but optical emission is not detected) could only be obtained for a handful of the most nearby galaxies. One of the main hurdles has been the limited angular resolution of the Spitzer Space Telescope. With the revolutionary capabilities of the JWST, it …
Localized Deviations from the CO-PAH Relation in PHANGS-JWST Galaxies: Faint PAH Emission or Elevated CO Emissivity?
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）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Center for Cosmology and Astroparticle Physics (CCAPP)（宇宙学与高能物理中心）；Department of Astronomy & Astrophysics, University of California, San Diego（加州大学圣地亚哥分校天文与天体物理系）；Sterrenkundig Observatorium, Universiteit Gent（根特大学天文台）；Department of Astronomy, University of Maryland（马里兰大学天文学系）；Observatorio Astronómico Nacional (IGN)（国家天文台（西班牙国家地理研究所））；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Department of Physics, Stanford University（斯坦福大学物理系）
We present maps of the 3.3 micron polycyclic aromatic hydrocarbon (PAH) emission feature in NGC 628, NGC 1365, and NGC 7496 as observed with the Near-Infrared Camera (NIRCam) imager on JWST from the PHANGS-JWST Cycle 1 Treasury project. We create maps that isolate the 3.3 micron PAH feature in the F335M filter (F335M$_{\rm PAH}$) using combinations of the F300M and F360M filters for removal of starlight continuum. This continuum removal is complicated by contamination of the F360M by PAH emission and variations in the stellar spectral energy distribution slopes between 3.0 and 3.6 micron. We m…
We combine JWST observations with ALMA CO and VLT-MUSE H$α$ data to examine off-spiral arm star formation in the face-on, grand-design spiral galaxy NGC 628. We focus on the northern spiral arm, around a galactocentric radius of 3-4 kpc, and study two spurs. These form an interesting contrast, as one is CO-rich and one CO-poor, and they have a maximum azimuthal offset in MIRI 21$μ$m and MUSE H$α$ of around 40$^\circ$ (CO-rich) and 55$^\circ$ (CO-poor) from the spiral arm. The star formation rate is higher in the regions of the spurs near to spiral arms, but the star formation efficiency appear…
We present maps tracing the fraction of dust in the form of polycyclic aromatic hydrocarbons (PAHs) in IC 5332, NGC 628, NGC 1365, and NGC 7496 from JWST/MIRI observations. We trace the PAH fraction by combining the F770W ($7.7~μ$m) and F1130W ($11.3~μ$m) filters to track ionized and neutral PAH emission, respectively, and comparing the PAH emission to F2100W which traces small, hot dust grains. We find average $R{\rm_{PAH} = (F770W+F1130W)/F2100W}$ values of 3.3, 4.7, 5.1, and 3.6 in IC 5332, NGC 628, NGC 1365, and NGC 7496, respectively. We find that H II regions traced by MUSE H$α$ show a s…
We present a high-resolution view of bubbles within The Phantom Galaxy (NGC 628); a nearby (~10Mpc), star-forming (~2Msun/yr), face-on (i~9deg) grand-design spiral galaxy. With new data obtained as part of the PHANGS-JWST treasury program, we perform a detailed case-study of two regions of interest, one of which contains the largest and most prominent bubble in the galaxy (The Phantom Void; over 1kpc in diameter), and the other being a smaller region that may be the precursor to such a large bubble (The Precursor Phantom Void). When comparing to matched resolution Halpha observations from the …
PHANGS-JWST: the largest extragalactic molecular cloud catalog traced by polycyclic aromatic hydrocarbon emission
University of Bonn（波恩大学）；Ohio State University（俄亥俄州立大学）；Center for Cosmology and Astroparticle Physics（宇宙学与基本粒子物理中心）；University of Alberta（阿尔伯塔大学）；University of California, San Diego（加利福尼亚大学圣地亚哥分校）；Cardiff University（卡迪夫大学）；Stockholm University（斯德哥尔摩大学）；Universität zu Köln（科隆大学）；Universiteit Gent（根特大学）
We compare mid-infrared (mid-IR), extinction-corrected H$α$, and CO (2-1) emission at 70--160 pc resolution in the first four PHANGS-JWST targets. We report correlation strengths, intensity ratios, and power law fits relating emission in JWST's F770W, F1000W, F1130W, and F2100W bands to CO and H$α$. At these scales, CO and H$α$ each correlate strongly with mid-IR emission, and these correlations are each stronger than the one relating CO to H$α$ emission. This reflects that mid-IR emission simultaneously acts as a dust column density tracer, leading to the good match with the molecular gas-tra…
Large-scale bars can fuel galaxy centers with molecular gas, often leading to the development of dense ring-like structures where intense star formation occurs, forming a very different environment compared to galactic disks. We pair ~0.3" (30pc) resolution new JWST/MIRI imaging with archival ALMA CO(2-1) mapping of the central ~5kpc of the nearby barred spiral galaxy NGC1365, to investigate the physical mechanisms responsible for this extreme star formation. The molecular gas morphology is resolved into two well-known bright bar lanes that surround a smooth dynamically cold gas disk (R_gal ~ …
Duration and properties of the embedded phase of star formation in 37 nearby galaxies from PHANGS-JWST
Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文中心）；Cosmic Origins Of Life (COOL) Research DAO（生命宇宙起源（COOL）研究DAO）；Kavli Institute for Particle Astrophysics & Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；INAF — Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；European Southern Observatory（欧洲南方天文台）；Department of Physics, University of Arkansas（阿肯色大学物理系）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学、蔚蓝海岸天文台、法国国家科学研究中心拉格朗日实验室）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）
A steep mass transition for bar-driven ISM structuring revealed by PHANGS-JWST
European Southern Observatory（欧洲南方天文台）；Univ Lyon, Univ Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574（里昂大学、里昂第一大学、巴黎高等师范学校里昂分校、法国国家科学研究中心、里昂天体物理研究中心）；Whitman College（惠特曼学院）；Algoma University（阿尔戈马大学）；Ohio State University（俄亥俄州立大学）；Center for Cosmology and Astroparticle Physics（宇宙学与高能物理中心）；California Institute of Technology（加州理工学院）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；The University of Manchester（曼彻斯特大学）；University of California, San Diego（加利福尼亚大学圣地亚哥分校）
The Hidden Life of Stars: Embedded Beginnings to AGB Endings in the PHANGS-JWST Sample. I. Catalog of Mid-IR Sources
University of Alberta（阿尔伯塔大学）；The Ohio State University（俄亥俄州立大学）；Center for Cosmology and Astroparticle Physics (CCAPP)（宇宙学与亚原子物理中心）；UCSD（加州大学圣地亚哥分校）；Université Côte d’Azur（蔚蓝海岸大学）；Observatoire de la Côte d’Azur（蔚蓝海岸天文台）；CNRS, Laboratoire Lagrange（法国国家科学研究中心，拉格朗日实验室）；The 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）；European Southern Observatory（欧洲南方天文台）；Max-Planck-Institut für Extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）
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）
Dust-Embedded Star Formation: Bridging Magellanic Cloud Studies of Massive Young Stellar Objects to Nearby Spiral Galaxies
Space Telescope Science Institute（太空望远镜科学研究所）；Instituto de Astrofísica de La Plata, CONICET–UNLP（拉普拉塔天体物理研究所，阿根廷国家科学研究委员会-拉普拉塔国立大学）；University of Virginia Astronomy Department（弗吉尼亚大学天文系）；National Radio Astronomy Observatory（美国国家射电天文台）；Department of Physics and Astronomy, The Johns Hopkins University（约翰斯·霍普金斯大学物理与天文系）；Department of Physics, University of Alberta（阿尔伯塔大学物理系）；UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester（英国ALMA区域中心节点，曼彻斯特大学天体物理学中心约德尔银行天体物理学部，物理与天文系）
Resolving dense photodissociation regions: the structure of photochemical fronts in three-dimensional gas distributions
Faculty of Physics, University of Duisburg-Essen（杜伊斯堡-埃森大学物理学院）；Research Center for Computational Earth and Space Science, Zhejiang Lab（浙江实验室计算地球与空间科学研究中心）
JWST observations of photodissociation regions: II. Warm molecular Hydrogen spectroscopy in the Horsehead nebula
Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale（巴黎萨克雷大学）；Sorbonne Université, CNRS, Institut d’Astrophysique de Paris（索邦大学）；Space Telescope Science Institute（太空望远镜科学研究所）；LUX, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（巴黎天文台）；Université Paris-Cité（巴黎西岱大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Physics & Astronomy, The University of Western Ontario（韦仕敦大学物理与天文学系）；Ritter Astrophysical Research Center, University of Toledo（托莱多大学里特天体物理研究中心）
Massive stars disrupt their natal molecular cloud material through radiative and mechanical feedback processes. These processes have profound effects on the evolution of interstellar matter in our Galaxy and throughout the Universe, from the era of vigorous star formation at redshifts of 1-3 to the present day. The dominant feedback processes can be probed by observations of the Photo-Dissociation Regions (PDRs) where the far-ultraviolet photons of massive stars create warm regions of gas and dust in the neutral atomic and molecular gas. PDR emission provides a unique tool to study in detail t…
H II region filling factors in NGC 628: Luminosity-size relation and connection with polycyclic aromatic hydrocarbon emission
Universidad de Granada（格拉纳达大学）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理研究所）；Instituto Universitario Carlos I de Física Teórica y Computacional, Universidad de Granada（格拉纳达大学卡洛斯一世理论与计算物理研究所）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学戴维·A·邓普天文学与天体物理学系）；Dunlap Institute for Astronomy and Astrophysics（邓普普天文学与天体物理研究所）；Département de Physique, de Génie Physique et d’Optique, Université Laval（拉瓦尔大学物理、物理工程与光学系）；Centre de Recherche en Astrophysique du Québec (CRAQ)（魁北克天体物理研究中心）；Department of Physics and Astronomy, University of Hawaii at Hilo（夏威夷大学希洛分校物理与天文学系）；Laboratoire d’Astrophysique de Marseille, CNRS, CNES, Aix Marseille University（马赛天体物理实验室）；Department of Physics and Astronomy, Texas A&M University（德克萨斯农工大学物理与天文学系）
JWST observations of photodissociation regions. IV. Carbonaceous emission band sub-components in NGC 7023 have distinct spatial distributions
The University of Western Ontario（韦仕敦大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Institut d’Astrophysique Spatiale, Université Paris-Saclay, CNRS（巴黎萨克雷大学国家科学研究中心天体物理学研究所）；Sterrenkundig Observatorium, Universiteit Gent（根特大学天文台）；Ritter Astrophysical Research Center, University of Toledo（托莱多大学里特天体物理研究中心）；Sorbonne Université, CNRS, Institut d’Astrophysique de Paris（索邦大学国家科学研究中心巴黎天体物理研究所）；United Kingdom Astronomy Technology Centre（英国天文学技术中心）
Feedback in Extragalactic Star Clusters (FEAST): Spectral Energy Distributions and the Physical Properties of Star Clusters in NGC 628 with CIGALE
University of Arizona（亚利桑那大学）；Stockholm University（斯德哥尔摩大学）；University of Massachusetts Amherst（马萨诸塞大学阿默斯特分校）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；University of Virginia（弗吉尼亚大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；Australian National University（澳大利亚国立大学）；Cardiff University（卡迪夫大学）
PDRs4All XVII: Formation and excitation of HD in photodissociation regions. Application to the Orion Bar
Institut d’Astrophysique Spatiale, Université Paris-Saclay, CNRS（空间天体物理研究所，巴黎萨克雷大学，法国国家科学研究中心）；LUX, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（LUX，巴黎天文台，巴黎文理研究大学，索邦大学，法国国家科学研究中心）；Université Paris-Cité（巴黎西岱大学）；Department of Physics, College of Science, United Arab Emirates University (UAEU)（阿拉伯联合酋长国大学理学院物理学系）；Instituto de Física Fundamental (CSIC)（基础物理研究所（西班牙国家研究委员会））；Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory（查尔姆斯理工大学空间、地球与环境系，翁萨拉空间观测站）
