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Currie T, Brandt GM, Brandt TD, Lacy B, Burrows A, Guyon O, Tamura M, Liu RY, Sagynbayeva S, Tobin T, Chilcote J, Groff T, Marois C, Thompson W, Murphy SJ, Kuzuhara M, Lawson K, Lozi J, Deo V, Vievard S, Skaf N, Uyama T, Jovanovic N, Martinache F, Kasdin NJ, Kudo T, McElwain M, Janson M, Wisniewski J, Hodapp K, Nishikawa J, Hełminiak K, Kwon J, Hayashi M. Direct imaging and astrometric detection of a gas giant planet orbiting an accelerating star. Science 2023; 380:198-203. [PMID: 37053312 DOI: 10.1126/science.abo6192] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 04/15/2023]
Abstract
Direct imaging of gas giant exoplanets provides information on their atmospheres and the architectures of planetary systems. However, few planets have been detected in blind surveys with direct imaging. Using astrometry from the Gaia and Hipparcos spacecraft, we identified dynamical evidence for a gas giant planet around the nearby star HIP 99770. We confirmed the detection of this planet with direct imaging using the Subaru Coronagraphic Extreme Adaptive Optics instrument. The planet, HIP 99770 b, orbits 17 astronomical units from its host star, receiving an amount of light similar to that reaching Jupiter. Its dynamical mass is 13.9 to 16.1 Jupiter masses. The planet-to-star mass ratio [(7 to 8) × 10-3] is similar to that of other directly imaged planets. The planet's atmospheric spectrum indicates an older, less cloudy analog of the previously imaged exoplanets around HR 8799.
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Affiliation(s)
- Thayne Currie
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA
- University of Texas-San Antonio, San Antonio, TX 78006, USA
- Eureka Scientific, Oakland, CA 94602, USA
| | - G Mirek Brandt
- Department of Physics, University of California, Santa Barbara, Santa Barbara, CA 93106, USA
| | - Timothy D Brandt
- Department of Physics, University of California, Santa Barbara, Santa Barbara, CA 93106, USA
| | - Brianna Lacy
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
- Department of Astronomy, University of Texas-Austin, Austin, TX 78712, USA
| | - Adam Burrows
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | - Olivier Guyon
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA
- Astrobiology Center, Osawa, Mitaka, Tokyo 181-8588, Japan
- Steward Observatory, The University of Arizona, Tucson, AZ 85721, USA
| | - Motohide Tamura
- Astrobiology Center, Osawa, Mitaka, Tokyo 181-8588, Japan
- National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan
- Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Ranger Y Liu
- Department of Astronomy, Columbia University, New York, NY 10027, USA
| | - Sabina Sagynbayeva
- Department of Physics and Astronomy, State University of New York-Stony Brook, Stony Brook, NY 11790, USA
| | - Taylor Tobin
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA
| | - Jeffrey Chilcote
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA
| | - Tyler Groff
- NASA-Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Christian Marois
- National Research Council-Herzberg, Victoria, BC V9E 2E7, Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8W 2Y2, Canada
| | - William Thompson
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8W 2Y2, Canada
| | - Simon J Murphy
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, Australia
- Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD 4350, Australia
| | - Masayuki Kuzuhara
- Astrobiology Center, Osawa, Mitaka, Tokyo 181-8588, Japan
- National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Kellen Lawson
- NASA-Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Julien Lozi
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA
| | - Vincent Deo
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA
| | - Sebastien Vievard
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA
| | - Nour Skaf
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA
| | - Taichi Uyama
- National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan
- Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
| | - Nemanja Jovanovic
- Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - Frantz Martinache
- Universite Cote d'Azur, Observatoire de la Cote d'Azur, Laboratoire Lagrange, Nice 06000, France
| | - N Jeremy Kasdin
- Department of Mechanical Engineering, Princeton University, Princeton, NJ 08544, USA
| | - Tomoyuki Kudo
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720, USA
| | | | - Markus Janson
- Department of Astronomy, Stockholm University, Stockholm 114 19, Sweden
| | - John Wisniewski
- Department of Physics and Astronomy, George Mason University, Fairfax, VA 22030, USA
| | - Klaus Hodapp
- Institute for Astronomy, University of Hawai'i, Hilo, HI 96720, USA
| | - Jun Nishikawa
- National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan
- Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Krzysztof Hełminiak
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Torun 87-100, Poland
| | - Jungmi Kwon
- Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Masahiko Hayashi
- National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan
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Kühn JG, Patapis P. Active focal-plane coronagraphy with liquid-crystal spatial-light modulators: broadband contrast performance in the visible. APPLIED OPTICS 2022; 61:9000-9009. [PMID: 36607029 DOI: 10.1364/ao.467802] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/20/2022] [Accepted: 09/28/2022] [Indexed: 06/17/2023]
Abstract
The technological progress in spatial-light modulator (SLM) technology has made it possible to use those devices as programmable active focal-plane phase coronagraphic masks, opening the door to novel versatile and adaptive high-contrast imaging observation strategies. However, the scalar nature of the SLM-induced phase response is a potential hurdle when applying the approach to wideband light, as is typical in astronomical imaging. For the first time, to our knowledge, we present laboratory results with broadband light (up to ∼12% bandwidth) for two commercially available SLM devices used as active focal-plane phase masks in the visible regime (640 nm). It is shown that under ideal or realistic telescope aperture conditions, the contrast performance is negligibly affected in this bandwidth regime, reaching a sufficient level for ground-based high-contrast imaging, which is typically dominated by atmospheric residuals.
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Giant planet imaged orbiting two massive stars. Nature 2021; 600:227-228. [PMID: 34880431 DOI: 10.1038/d41586-021-03607-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Martinod MA, Tuthill P, Gross S, Norris B, Sweeney D, Withford MJ. Achromatic photonic tricouplers for application in nulling interferometry. APPLIED OPTICS 2021; 60:D100-D107. [PMID: 34263832 DOI: 10.1364/ao.423541] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/01/2021] [Accepted: 05/27/2021] [Indexed: 06/13/2023]
Abstract
Integrated-optic components are being increasingly used in astrophysics, mainly where accuracy and precision are paramount. One such emerging technology is nulling interferometry that targets high contrast and high angular resolution. Two of the most critical limitations encountered by nullers are rapid phase fluctuations in the incoming light causing instability in the interference and chromaticity of the directional couplers that prevent a deep broadband interferometric null. We explore the use of a tricoupler designed by ultrafast laser inscription that solves both issues. Simulations of a tricoupler, incorporated into a nuller, result in an order of a magnitude improvement in null depth.
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Martinod MA, Norris B, Tuthill P, Lagadec T, Jovanovic N, Cvetojevic N, Gross S, Arriola A, Gretzinger T, Withford MJ, Guyon O, Lozi J, Vievard S, Deo V, Lawrence JS, Leon-Saval S. Scalable photonic-based nulling interferometry with the dispersed multi-baseline GLINT instrument. Nat Commun 2021; 12:2465. [PMID: 33927206 PMCID: PMC8084960 DOI: 10.1038/s41467-021-22769-x] [Citation(s) in RCA: 8] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/16/2020] [Accepted: 03/29/2021] [Indexed: 11/09/2022] Open
Abstract
Characterisation of exoplanets is key to understanding their formation, composition and potential for life. Nulling interferometry, combined with extreme adaptive optics, is among the most promising techniques to advance this goal. We present an integrated-optic nuller whose design is directly scalable to future science-ready interferometric nullers: the Guided-Light Interferometric Nulling Technology, deployed at the Subaru Telescope. It combines four beams and delivers spatial and spectral information. We demonstrate the capability of the instrument, achieving a null depth better than 10-3 with a precision of 10-4 for all baselines, in laboratory conditions with simulated seeing applied. On sky, the instrument delivered angular diameter measurements of stars that were 2.5 times smaller than the diffraction limit of the telescope. These successes pave the way for future design enhancements: scaling to more baselines, improved photonic component and handling low-order atmospheric aberration within the instrument, all of which will contribute to enhance sensitivity and precision.
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Affiliation(s)
- Marc-Antoine Martinod
- Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW, Australia.
- Sydney Astrophotonic Instrumentation Laboratories, Physics Road, University of Sydney, Sydney, NSW, Australia.
- AAO-USyd, School of Physics, University of Sydney, Sydney, NSW, Australia.
| | - Barnaby Norris
- Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW, Australia
- Sydney Astrophotonic Instrumentation Laboratories, Physics Road, University of Sydney, Sydney, NSW, Australia
- AAO-USyd, School of Physics, University of Sydney, Sydney, NSW, Australia
| | - Peter Tuthill
- Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW, Australia
- Sydney Astrophotonic Instrumentation Laboratories, Physics Road, University of Sydney, Sydney, NSW, Australia
- AAO-USyd, School of Physics, University of Sydney, Sydney, NSW, Australia
| | - Tiphaine Lagadec
- Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT, Australia
| | | | - Nick Cvetojevic
- Laboratoire Lagrange, Observatoire de la Côte d'Azur, Université Côte d'Azur, Nice, France
| | - Simon Gross
- MQ Photonics Research Centre, Macquarie University, Sydney, Australia
| | - Alexander Arriola
- MQ Photonics Research Centre, Macquarie University, Sydney, Australia
| | - Thomas Gretzinger
- MQ Photonics Research Centre, Macquarie University, Sydney, Australia
| | | | - Olivier Guyon
- Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Hilo, HI, USA
- Steward Observatory, University of Arizona, Tucson, AZ, USA
- Astrobiology Center, National Institutes of Natural Sciences, Mitaka, Tokyo, Japan
- James C. Wyant College of Optical Sciences, University of Arizona, Tucson, AZ, USA
| | - Julien Lozi
- Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Hilo, HI, USA
| | - Sébastien Vievard
- Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Hilo, HI, USA
- Astrobiology Center, National Institutes of Natural Sciences, Mitaka, Tokyo, Japan
| | - Vincent Deo
- Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Hilo, HI, USA
| | - Jon S Lawrence
- Australian Astronomical Optics - Macquarie, Macquarie University, Sydney, NSW, Australia
| | - Sergio Leon-Saval
- Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW, Australia
- Sydney Astrophotonic Instrumentation Laboratories, Physics Road, University of Sydney, Sydney, NSW, Australia
- Institute of Photonics and Optical Science, School of Physics, University of Sydney, Sydney, NSW, Australia
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Imaging low-mass planets within the habitable zone of α Centauri. Nat Commun 2021; 12:922. [PMID: 33568657 PMCID: PMC7876126 DOI: 10.1038/s41467-021-21176-6] [Citation(s) in RCA: 17] [Impact Index Per Article: 5.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/06/2020] [Accepted: 01/13/2021] [Indexed: 01/30/2023] Open
Abstract
Giant exoplanets on wide orbits have been directly imaged around young stars. If the thermal background in the mid-infrared can be mitigated, then exoplanets with lower masses can also be imaged. Here we present a ground-based mid-infrared observing approach that enables imaging low-mass temperate exoplanets around nearby stars, and in particular within the closest stellar system, α Centauri. Based on 75-80% of the best quality images from 100 h of cumulative observations, we demonstrate sensitivity to warm sub-Neptune-sized planets throughout much of the habitable zone of α Centauri A. This is an order of magnitude more sensitive than state-of-the-art exoplanet imaging mass detection limits. We also discuss a possible exoplanet or exozodiacal disk detection around α Centauri A. However, an instrumental artifact of unknown origin cannot be ruled out. These results demonstrate the feasibility of imaging rocky habitable-zone exoplanets with current and upcoming telescopes.
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Abstract
Adaptive optics (AO) is a technique that corrects for optical aberrations. It was originally proposed to correct for the blurring effect of atmospheric turbulence on images in ground-based telescopes and was instrumental in the work that resulted in the Nobel prize-winning discovery of a supermassive compact object at the centre of our galaxy. When AO is used to correct for the eye's imperfect optics, retinal changes at the cellular level can be detected, allowing us to study the operation of the visual system and to assess ocular health in the microscopic domain. By correcting for sample-induced blur in microscopy, AO has pushed the boundaries of imaging in thick tissue specimens, such as when observing neuronal processes in the brain. In this primer, we focus on the application of AO for high-resolution imaging in astronomy, vision science and microscopy. We begin with an overview of the general principles of AO and its main components, which include methods to measure the aberrations, devices for aberration correction, and how these components are linked in operation. We present results and applications from each field along with reproducibility considerations and limitations. Finally, we discuss future directions.
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New HST data and modeling reveal a massive planetesimal collision around Fomalhaut. Proc Natl Acad Sci U S A 2020; 117:9712-9722. [PMID: 32312810 DOI: 10.1073/pnas.1912506117] [Citation(s) in RCA: 18] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The apparent detection of an exoplanet orbiting Fomalhaut was announced in 2008. However, subsequent observations of Fomalhaut b raised questions about its status: Unlike other exoplanets, it is bright in the optical and nondetected in the infrared, and its orbit appears to cross the debris ring around the star without the expected gravitational perturbations. We revisit previously published data and analyze additional Hubble Space Telescope (HST) data, finding that the source is likely on a radial trajectory and has faded and become extended. Dynamical and collisional modeling of a recently produced dust cloud yields results consistent with the observations. Fomalhaut b appears to be a directly imaged catastrophic collision between two large planetesimals in an extrasolar planetary system. Similar events should be very rare in quiescent planetary systems of the age of Fomalhaut, suggesting that we are possibly witnessing the effects of gravitational stirring due to the orbital evolution of hypothetical planet(s) around the star.
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Population-level Eccentricity Distributions of Imaged Exoplanets and Brown Dwarf Companions: Dynamical Evidence for Distinct Formation Channels. ACTA ACUST UNITED AC 2020. [DOI: 10.3847/1538-3881/ab5b11] [Citation(s) in RCA: 47] [Impact Index Per Article: 11.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-3881/ab16e9] [Citation(s) in RCA: 178] [Impact Index Per Article: 35.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/aaf389] [Citation(s) in RCA: 37] [Impact Index Per Article: 7.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Detecting Water in the Atmosphere of HR 8799 c with L-band High-dispersion Spectroscopy Aided by Adaptive Optics. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-3881/aae47b] [Citation(s) in RCA: 22] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? GEOSCIENCES 2018. [DOI: 10.3390/geosciences8100362] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
“Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST.
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Fujii Y, Angerhausen D, Deitrick R, Domagal-Goldman S, Grenfell JL, Hori Y, Kane SR, Pallé E, Rauer H, Siegler N, Stapelfeldt K, Stevenson KB. Exoplanet Biosignatures: Observational Prospects. ASTROBIOLOGY 2018; 18:739-778. [PMID: 29938537 PMCID: PMC6016572 DOI: 10.1089/ast.2017.1733] [Citation(s) in RCA: 20] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/03/2017] [Accepted: 03/13/2018] [Indexed: 05/04/2023]
Abstract
Exoplanet hunting efforts have revealed the prevalence of exotic worlds with diverse properties, including Earth-sized bodies, which has fueled our endeavor to search for life beyond the Solar System. Accumulating experiences in astrophysical, chemical, and climatological characterization of uninhabitable planets are paving the way to characterization of potentially habitable planets. In this paper, we review our possibilities and limitations in characterizing temperate terrestrial planets with future observational capabilities through the 2030s and beyond, as a basis of a broad range of discussions on how to advance "astrobiology" with exoplanets. We discuss the observability of not only the proposed biosignature candidates themselves but also of more general planetary properties that provide circumstantial evidence, since the evaluation of any biosignature candidate relies on its context. Characterization of temperate Earth-sized planets in the coming years will focus on those around nearby late-type stars. The James Webb Space Telescope (JWST) and later 30-meter-class ground-based telescopes will empower their chemical investigations. Spectroscopic studies of potentially habitable planets around solar-type stars will likely require a designated spacecraft mission for direct imaging, leveraging technologies that are already being developed and tested as part of the Wide Field InfraRed Survey Telescope (WFIRST) mission. Successful initial characterization of a few nearby targets will be an important touchstone toward a more detailed scrutiny and a larger survey that are envisioned beyond 2030. The broad outlook this paper presents may help develop new observational techniques to detect relevant features as well as frameworks to diagnose planets based on the observables. Key Words: Exoplanets-Biosignatures-Characterization-Planetary atmospheres-Planetary surfaces. Astrobiology 18, 739-778.
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Affiliation(s)
- Yuka Fujii
- NASA Goddard Institute for Space Studies, New York, New York, USA
- Earth-Life Science Institute, Tokyo Institute of Technology, Ookayama, Meguro, Tokyo, Japan
| | - Daniel Angerhausen
- CSH Fellow for Exoplanetary Astronomy, Center for Space and Habitability (CSH), Universität Bern, Bern, Switzerland
- Blue Marble Space Institute of Science, Seattle, Washington, USA
| | - Russell Deitrick
- Department of Astronomy, University of Washington, Seattle, Washington, USA
- NASA Astrobiology Institute's Virtual Planetary Laboratory
| | - Shawn Domagal-Goldman
- NASA Astrobiology Institute's Virtual Planetary Laboratory
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - John Lee Grenfell
- Department of Extrasolar Planets and Atmospheres (EPA), Institute of Planetary Research, German Aerospace Centre (DLR), Berlin, Germany
| | - Yasunori Hori
- Astrobiology Center, National Institutes of Natural Sciences (NINS), Mitaka, Tokyo, Japan
| | - Stephen R. Kane
- Department of Earth Sciences, University of California, Riverside, California, USA
| | - Enric Pallé
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
- Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain
| | - Heike Rauer
- Department of Extrasolar Planets and Atmospheres (EPA), Institute of Planetary Research, German Aerospace Centre (DLR), Berlin, Germany
- Center for Astronomy and Astrophysics, Berlin Institute of Technology, Berlin, Germany
| | - Nicholas Siegler
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
- NASA Exoplanet Exploration Office
| | - Karl Stapelfeldt
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
- NASA Exoplanet Exploration Office
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2MASS J13243553+6358281 Is an Early T-type Planetary-mass Object in the AB Doradus Moving Group. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/2041-8213/aaacfd] [Citation(s) in RCA: 19] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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HELIOS–RETRIEVAL:An Open-source, Nested Sampling Atmospheric Retrieval Code; Application to the HR 8799 Exoplanets and Inferred Constraints for Planet Formation. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-3881/aa7ed8] [Citation(s) in RCA: 83] [Impact Index Per Article: 11.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Kenchington Goldsmith HD, Ireland M, Ma P, Cvetojevic N, Madden S. Improving the extinction bandwidth of MMI chalcogenide photonic chip based MIR nulling interferometers. OPTICS EXPRESS 2017; 25:16813-16824. [PMID: 28789181 DOI: 10.1364/oe.25.016813] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/02/2017] [Accepted: 06/22/2017] [Indexed: 06/07/2023]
Abstract
Research into planets beyond our own star system has until recently relied on indirect imaging methods. Direct imaging methods are now establishing a foothold in the hunt for alien planets and habitable worlds. Nulling interferometry is a promising approach for suppressing the host star brightness and resolving surrounding planets. A key requirement in this method is the interference of light from multiple telescopes/baselines and free space optical devices have already rendered images of other worlds. Photonic chip based systems are also becoming accepted as means of accomplishing this but require, in particular, wide bandwidth, high precision on chip beam splitters. In this paper a design improvement is outlined to one of the most fabrication tolerant integrated beam splitter components that significantly increases its coupling bandwidth and therefore its bandwidth at high extinction. Preliminary experimental results from a fabricated device are also shown. The predicted bandwidth spans 3.8 - 4.1 μm at an extinction of ∼50 dB but at the expense of increasing the loss to 0.6 dB in transmission.
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Goldsmith HDK, Cvetojevic N, Ireland M, Madden S. Fabrication tolerant chalcogenide mid-infrared multimode interference coupler design with applications for Bracewell nulling interferometry. OPTICS EXPRESS 2017; 25:3038-3051. [PMID: 28241521 DOI: 10.1364/oe.25.003038] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
Understanding exoplanet formation and finding potentially habitable exoplanets is vital to an enhanced understanding of the universe. The use of nulling interferometry to strongly attenuate the central star's light provides the opportunity to see objects closer to the star than ever before. Given that exoplanets are usually warm, the 4 µm Mid-Infrared region is advantageous for such observations. The key performance parameters for a nulling interferometer are the extinction ratio it can attain and how well that is maintained across the operational bandwidth. Both parameters depend on the design and fabrication accuracy of the subcomponents and their wavelength dependence. Via detailed simulation it is shown in this paper that a planar chalcogenide photonic chip, consisting of three highly fabrication tolerant multimode interference couplers, can exceed an extinction ratio of 60 dB in double nulling operation and up to 40 dB for a single nulling operation across a wavelength window of 3.9 to 4.2 µm. This provides a beam combiner with sufficient performance, in theory, to image exoplanets.
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THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/832/1/41] [Citation(s) in RCA: 189] [Impact Index Per Article: 23.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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THE TRENDS HIGH-CONTRAST IMAGING SURVEY. VI. DISCOVERY OF A MASS, AGE, AND METALLICITY BENCHMARK BROWN DWARF. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/831/2/136] [Citation(s) in RCA: 30] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Moses JI, Marley MS, Zahnle K, Line MR, Fortney JJ, Barman TS, Visscher C, Lewis NK, Wolff MJ. ON THE COMPOSITION OF YOUNG, DIRECTLY IMAGED GIANT PLANETS. THE ASTROPHYSICAL JOURNAL 2016; 829:66. [PMID: 31171882 PMCID: PMC6547835 DOI: 10.3847/0004-637x/829/2/66] [Citation(s) in RCA: 53] [Impact Index Per Article: 6.6] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
The past decade has seen significant progress on the direct detection and characterization of young, self-luminous giant planets at wide orbital separations from their host stars. Some of these planets show evidence for disequilibrium processes like transport-induced quenching in their atmospheres; photochemistry may also be important, despite the large orbital distances. These disequilibrium chemical processes can alter the expected composition, spectral behavior, thermal structure, and cooling history of the planets, and can potentially confuse determinations of bulk elemental ratios, which provide important insights into planet-formation mechanisms. Using a thermo/photochemical kinetics and transport model, we investigate the extent to which disequilibrium chemistry affects the composition and spectra of directly imaged giant exoplanets. Results for specific "young Jupiters" such as HR 8799 b and 51 Eri b are presented, as are general trends as a function of planetary effective temperature, surface gravity, incident ultraviolet flux, and strength of deep atmospheric convection. We find that quenching is very important on young Jupiters, leading to CO/CH4 and N2/NH3 ratios much greater than, and H2O mixing ratios a factor of a few less than, chemical-equilibrium predictions. Photochemistry can also be important on such planets, with CO2 and HCN being key photochemical products. Carbon dioxide becomes a major constituent when stratospheric temperatures are low and recycling of water via the H2 + OH reaction becomes kinetically stifled. Young Jupiters with effective temperatures ≲700 K are in a particularly interesting photochemical regime that differs from both transiting hot Jupiters and our own solar-system giant planets.
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Affiliation(s)
- J I Moses
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
| | - M S Marley
- NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - K Zahnle
- NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - M R Line
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - J J Fortney
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - T S Barman
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - C Visscher
- Dordt College, Sioux Center, IA 51250, USA and Space Science Institute, Boulder, CO 80301, USA
| | - N K Lewis
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | - M J Wolff
- Space Science Institute, Boulder, CO 80301, USA
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Rice K. Detecting structure in a protostellar disk. Science 2016; 353:1492-1493. [DOI: 10.1126/science.aag2855] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Spiral structure may provide clues about the early stages of star and planet formation
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Affiliation(s)
- Ken Rice
- Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UK
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ASTROMETRIC MONITORING OF THE HR 8799 PLANETS: ORBIT CONSTRAINTS FROM SELF-CONSISTENT MEASUREMENTS. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-6256/152/2/28] [Citation(s) in RCA: 44] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Sengupta S, Marley MS. DETECTING EXOMOONS AROUND SELF-LUMINOUS GIANT EXOPLANETS THROUGH POLARIZATION. THE ASTROPHYSICAL JOURNAL 2016; 824:76. [PMID: 29430024 PMCID: PMC5805157 DOI: 10.3847/0004-637x/824/2/76] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
Many of the directly imaged self-luminous gas giant exoplanets have been found to have cloudy atmospheres. Scattering of the emergent thermal radiation from these planets by the dust grains in their atmospheres should locally give rise to significant linear polarization of the emitted radiation. However, the observable disk averaged polarization should be zero if the planet is spherically symmetric. Rotation-induced oblateness may yield a net non-zero disk averaged polarization if the planets have sufficiently high spin rotation velocity. On the other hand, when a large natural satellite or exomoon transits a planet with cloudy atmosphere along the line of sight, the asymmetry induced during the transit should give rise to a net non-zero, time resolved linear polarization signal. The peak amplitude of such time dependent polarization may be detectable even for slowly rotating exoplanets. Therefore, we suggest that large exomoons around directly imaged self-luminous exoplanets may be detectable through time resolved imaging polarimetry. Adopting detailed atmospheric models for several values of effective temperature and surface gravity which are appropriate for self-luminous exoplanets, we present the polarization profiles of these objects in the infrared during transit phase and estimate the peak amplitude of polarization that occurs during the inner contacts of the transit ingress/egress phase. The peak polarization is predicted to range between 0.1 and 0.3 % in the infrared.
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Affiliation(s)
- Sujan Sengupta
- Indian Institute of Astrophysics, Koramangala 2nd Block, Bangalore 560 034, India
| | - Mark S Marley
- NASA Ames Research Center, MS-245-3, Moffett Field, CA 94035, U.S.A
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Borucki WJ. KEPLER Mission: development and overview. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2016; 79:036901. [PMID: 26863223 DOI: 10.1088/0034-4885/79/3/036901] [Citation(s) in RCA: 12] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/05/2023]
Abstract
The Kepler Mission is a space observatory launched in 2009 by NASA to monitor 170,000 stars over a period of four years to determine the frequency of Earth-size and larger planets in and near the habitable zone of Sun-like stars, the size and orbital distributions of these planets, and the types of stars they orbit. Kepler is the tenth in the series of NASA Discovery Program missions that are competitively-selected, PI-directed, medium-cost missions. The Mission concept and various instrument prototypes were developed at the Ames Research Center over a period of 18 years starting in 1983. The development of techniques to do the 10 ppm photometry required for Mission success took years of experimentation, several workshops, and the exploration of many 'blind alleys' before the construction of the flight instrument. Beginning in 1992 at the start of the NASA Discovery Program, the Kepler Mission concept was proposed five times before its acceptance for mission development in 2001. During that period, the concept evolved from a photometer in an L2 orbit that monitored 6000 stars in a 50 sq deg field-of-view (FOV) to one that was in a heliocentric orbit that simultaneously monitored 170,000 stars with a 105 sq deg FOV. Analysis of the data to date has detected over 4600 planetary candidates which include several hundred Earth-size planetary candidates, over a thousand confirmed planets, and Earth-size planets in the habitable zone (HZ). These discoveries provide the information required for estimates of the frequency of planets in our galaxy. The Mission results show that most stars have planets, many of these planets are similar in size to the Earth, and that systems with several planets are common. Although planets in the HZ are common, many are substantially larger than Earth.
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Affiliation(s)
- William J Borucki
- Science Directorate, NASA Ames Research Center, Moffett Field, CA 94035, USA
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Dalba PA, Muirhead PS, Fortney JJ, Hedman MM, Nicholson PD, Veyette MJ. THE TRANSIT TRANSMISSION SPECTRUM OF A COLD GAS GIANT PLANET. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/814/2/154] [Citation(s) in RCA: 47] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Currie T, Cloutier R, Brittain S, Grady C, Burrows A, Muto T, Kenyon SJ, Kuchner MJ. RESOLVING THE HD 100546 PROTOPLANETARY SYSTEM WITH THE GEMINI PLANET IMAGER: EVIDENCE FOR MULTIPLE FORMING, ACCRETING PLANETS. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/2041-8205/814/2/l27] [Citation(s) in RCA: 113] [Impact Index Per Article: 12.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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41
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Accreting protoplanets in the LkCa 15 transition disk. Nature 2015; 527:342-4. [PMID: 26581290 DOI: 10.1038/nature15761] [Citation(s) in RCA: 225] [Impact Index Per Article: 25.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/16/2015] [Accepted: 09/10/2015] [Indexed: 11/08/2022]
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Macintosh B, Graham JR, Barman T, De Rosa RJ, Konopacky Q, Marley MS, Marois C, Nielsen EL, Pueyo L, Rajan A, Rameau J, Saumon D, Wang JJ, Patience J, Ammons M, Arriaga P, Artigau E, Beckwith S, Brewster J, Bruzzone S, Bulger J, Burningham B, Burrows AS, Chen C, Chiang E, Chilcote JK, Dawson RI, Dong R, Doyon R, Draper ZH, Duchêne G, Esposito TM, Fabrycky D, Fitzgerald MP, Follette KB, Fortney JJ, Gerard B, Goodsell S, Greenbaum AZ, Hibon P, Hinkley S, Cotten TH, Hung LW, Ingraham P, Johnson-Groh M, Kalas P, Lafreniere D, Larkin JE, Lee J, Line M, Long D, Maire J, Marchis F, Matthews BC, Max CE, Metchev S, Millar-Blanchaer MA, Mittal T, Morley CV, Morzinski KM, Murray-Clay R, Oppenheimer R, Palmer DW, Patel R, Perrin MD, Poyneer LA, Rafikov RR, Rantakyrö FT, Rice EL, Rojo P, Rudy AR, Ruffio JB, Ruiz MT, Sadakuni N, Saddlemyer L, Salama M, Savransky D, Schneider AC, Sivaramakrishnan A, Song I, Soummer R, Thomas S, Vasisht G, Wallace JK, Ward-Duong K, Wiktorowicz SJ, Wolff SG, Zuckerman B. Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager. Science 2015; 350:64-7. [DOI: 10.1126/science.aac5891] [Citation(s) in RCA: 391] [Impact Index Per Article: 43.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/17/2015] [Accepted: 08/03/2015] [Indexed: 11/02/2022]
Affiliation(s)
- B. Macintosh
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
- Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94040, USA
| | - J. R. Graham
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - T. Barman
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - R. J. De Rosa
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - Q. Konopacky
- Center for Astrophysics and Space Sciences, University of California–San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA
| | - M. S. Marley
- NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035, USA
| | - C. Marois
- National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, Canada
- Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria, British Columbia V8P 5C2, Canada
| | - E. L. Nielsen
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
- Search for Extraterrestrial Intelligence Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA
| | - L. Pueyo
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - A. Rajan
- School of Earth and Space Exploration, Arizona State University, Post Office Box 871404, Tempe, AZ 85287, USA
| | - J. Rameau
- Institut de Recherche sur les Exoplanètes, Départment de Physique, Université de Montréal, Montréal, Québec H3C 3J7, Canada
| | - D. Saumon
- Los Alamos National Laboratory, Post Office Box 1663, MS F663, Los Alamos, NM 87545, USA
| | - J. J. Wang
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - J. Patience
- School of Earth and Space Exploration, Arizona State University, Post Office Box 871404, Tempe, AZ 85287, USA
| | - M. Ammons
- Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94040, USA
| | - P. Arriaga
- Department of Physics and Astronomy, University of California–Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
| | - E. Artigau
- Institut de Recherche sur les Exoplanètes, Départment de Physique, Université de Montréal, Montréal, Québec H3C 3J7, Canada
| | - S. Beckwith
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - J. Brewster
- Search for Extraterrestrial Intelligence Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA
| | - S. Bruzzone
- Department of Physics and Astronomy, Centre for Planetary Science and Exploration, The University of Western Ontario, London, Ontario N6A 3K7, Canada
| | - J. Bulger
- School of Earth and Space Exploration, Arizona State University, Post Office Box 871404, Tempe, AZ 85287, USA
- Subaru Telescope, 650 North A'ohoku Place, Hilo, HI 96720, USA
| | - B. Burningham
- NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035, USA
- Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB, UK
| | - A. S. Burrows
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | - C. Chen
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - E. Chiang
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - J. K. Chilcote
- Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada
| | - R. I. Dawson
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - R. Dong
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - R. Doyon
- Institut de Recherche sur les Exoplanètes, Départment de Physique, Université de Montréal, Montréal, Québec H3C 3J7, Canada
| | - Z. H. Draper
- National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, Canada
- Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria, British Columbia V8P 5C2, Canada
| | - G. Duchêne
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
- Institut de Planétologie et d’Astrophysique de Grenoble, Université Grenoble Alpes, Centre National de la Recherche Scientifique, 38000 Grenoble, France
| | - T. M. Esposito
- Department of Physics and Astronomy, University of California–Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
| | - D. Fabrycky
- Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA
| | - M. P. Fitzgerald
- Department of Physics and Astronomy, University of California–Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
| | - K. B. Follette
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - J. J. Fortney
- Department of Astronomy and Astrophysics, University of California–Santa Cruz, Santa Cruz, CA 95064, USA
| | - B. Gerard
- National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, Canada
- Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria, British Columbia V8P 5C2, Canada
| | - S. Goodsell
- Department of Physics, Durham University, Stockton Road, Durham DH1, UK
- Gemini Observatory, Casilla 603, La Serena, Chile
| | - A. Z. Greenbaum
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- Department of Physics and Astronomy, Johns Hopkins University, 3600 North Charles Street, Baltimore, MD 21218, USA
| | - P. Hibon
- Gemini Observatory, Casilla 603, La Serena, Chile
| | - S. Hinkley
- University of Exeter, Astrophysics Group, Physics Building, Stocker Road, Exeter EX4 4QL, UK
| | - T. H. Cotten
- Department of Physics and Astronomy, University of Georgia, Athens, GA 30602, USA
| | - L.-W. Hung
- Department of Physics and Astronomy, University of California–Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
| | - P. Ingraham
- Large Synoptic Survey Telescope, 950 North Cherry Avenue, Tucson, AZ 85719, USA
| | - M. Johnson-Groh
- National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, Canada
- Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria, British Columbia V8P 5C2, Canada
| | - P. Kalas
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
- Search for Extraterrestrial Intelligence Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA
| | - D. Lafreniere
- Institut de Recherche sur les Exoplanètes, Départment de Physique, Université de Montréal, Montréal, Québec H3C 3J7, Canada
| | - J. E. Larkin
- Department of Physics and Astronomy, University of California–Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
| | - J. Lee
- Department of Physics and Astronomy, University of Georgia, Athens, GA 30602, USA
| | - M. Line
- Department of Astronomy and Astrophysics, University of California–Santa Cruz, Santa Cruz, CA 95064, USA
| | - D. Long
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - J. Maire
- Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada
| | - F. Marchis
- Search for Extraterrestrial Intelligence Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA
| | - B. C. Matthews
- National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, Canada
- Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria, British Columbia V8P 5C2, Canada
| | - C. E. Max
- Department of Astronomy and Astrophysics, University of California–Santa Cruz, Santa Cruz, CA 95064, USA
| | - S. Metchev
- Department of Physics and Astronomy, Centre for Planetary Science and Exploration, The University of Western Ontario, London, Ontario N6A 3K7, Canada
- Department of Physics and Astronomy, Stony Brook University, 100 Nicolls Road, Stony Brook, NY 11794-3800, USA
| | - M. A. Millar-Blanchaer
- Department of Astronomy and Astrophysics, University of Toronto, Toronto, Ontario M5S 3H4, Canada
| | - T. Mittal
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - C. V. Morley
- Department of Astronomy and Astrophysics, University of California–Santa Cruz, Santa Cruz, CA 95064, USA
| | - K. M. Morzinski
- Steward Observatory, 933 North Cherry Avenue, University of Arizona, Tucson, AZ 85721, USA
| | - R. Murray-Clay
- Department of Physics, University of California–Santa Barbara, Broida Hall, Santa Barbara, CA 93106-9530, USA
| | - R. Oppenheimer
- Department of Astrophysics, American Museum of Natural History, New York, NY 10024, USA
| | - D. W. Palmer
- Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94040, USA
| | - R. Patel
- Department of Physics and Astronomy, Stony Brook University, 100 Nicolls Road, Stony Brook, NY 11794-3800, USA
| | - M. D. Perrin
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - L. A. Poyneer
- Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94040, USA
| | - R. R. Rafikov
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | | | - E. L. Rice
- Department of Astrophysics, American Museum of Natural History, New York, NY 10024, USA
- Department of Engineering Science and Physics, College of Staten Island, City University of New York, Staten Island, NY 10314, USA
| | - P. Rojo
- Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Casilla 36-D, Las Condes, Santiago, Chile
| | - A. R. Rudy
- Department of Astronomy and Astrophysics, University of California–Santa Cruz, Santa Cruz, CA 95064, USA
| | - J.-B. Ruffio
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
- Search for Extraterrestrial Intelligence Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA
| | - M. T. Ruiz
- Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Casilla 36-D, Las Condes, Santiago, Chile
| | - N. Sadakuni
- Gemini Observatory, Casilla 603, La Serena, Chile
- Stratospheric Observatory for Infrared Astronomy, Universities Space Research Association, NASA Armstrong Flight Research Center, 2825 East Avenue P, Palmdale, CA 93550, USA
| | - L. Saddlemyer
- National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, Canada
| | - M. Salama
- Department of Astronomy, University of California–Berkeley, Berkeley, CA 94720, USA
| | - D. Savransky
- Sibley School of Mechanical and Aerospace Engineering, Cornell University, Ithaca, NY 14853, USA
| | - A. C. Schneider
- Physics and Astronomy, University of Toledo, 2801 West Bancroft Street, Toledo, OH 43606, USA
| | - A. Sivaramakrishnan
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - I. Song
- Department of Physics and Astronomy, University of Georgia, Athens, GA 30602, USA
| | - R. Soummer
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - S. Thomas
- Large Synoptic Survey Telescope, 950 North Cherry Avenue, Tucson, AZ 85719, USA
| | - G. Vasisht
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - J. K. Wallace
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - K. Ward-Duong
- School of Earth and Space Exploration, Arizona State University, Post Office Box 871404, Tempe, AZ 85287, USA
| | - S. J. Wiktorowicz
- Department of Astronomy and Astrophysics, University of California–Santa Cruz, Santa Cruz, CA 95064, USA
| | - S. G. Wolff
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- Department of Physics and Astronomy, Johns Hopkins University, 3600 North Charles Street, Baltimore, MD 21218, USA
| | - B. Zuckerman
- Department of Physics and Astronomy, University of California–Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
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Mawet D. Eyeing up a Jupiter-like exoplanet. Science 2015; 350:39-40. [DOI: 10.1126/science.aad0904] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Extreme adaptive optics systems enable the direct imaging of exoplanetary systems
[Also see Report by
Macintosh
et al.
]
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Affiliation(s)
- Dimitri Mawet
- Department of Astronomy, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91125, USA
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Gagné J, Faherty JK, Cruz KL, Lafreniére D, Doyon R, Malo L, Burgasser AJ, Naud ME, Artigau É, Bouchard S, Gizis JE, Albert L. BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0067-0049/219/2/33] [Citation(s) in RCA: 136] [Impact Index Per Article: 15.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Quanz SP, Amara A, Meyer MR, Girard JH, Kenworthy MA, Kasper M. CONFIRMATION AND CHARACTERIZATION OF THE PROTOPLANET HD 100546 b—DIRECT EVIDENCE FOR GAS GIANT PLANET FORMATION AT 50 AU. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/807/1/64] [Citation(s) in RCA: 109] [Impact Index Per Article: 12.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Bowler BP, Shkolnik EL, Liu MC, Schlieder JE, Mann AW, Dupuy TJ, Hinkley S, Crepp JR, Johnson JA, Howard AW, Flagg L, Weinberger AJ, Aller KM, Allers KN, Best WMJ, Kotson MC, Montet BT, Herczeg GJ, Baranec C, Riddle R, Law NM, Nielsen EL, Wahhaj Z, Biller BA, Hayward TL. PLANETS AROUND LOW-MASS STARS (PALMS). V. AGE-DATING LOW-MASS COMPANIONS TO MEMBERS AND INTERLOPERS OF YOUNG MOVING GROUPS. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/806/1/62] [Citation(s) in RCA: 21] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Contro B, Wittenmyer RA, Horner J, Marshall JP. The Dynamical Structure of HR 8799's Inner Debris Disk. ORIGINS LIFE EVOL B 2015; 45:41-9. [PMID: 25862330 DOI: 10.1007/s11084-015-9405-x] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/21/2014] [Accepted: 11/09/2014] [Indexed: 10/23/2022]
Abstract
The HR 8799 system, with its four giant planets and two debris belts, has an architecture closely mirroring that of our Solar system where the inner, warm asteroid belt and outer, cool Edgeworth-Kuiper belt bracket the giant planets. As such, it is a valuable laboratory for examining exoplanetary dynamics and debris disk-exoplanet interactions. Whilst the outer debris belt of HR 8799 has been well resolved by previous observations, the spatial extent of the inner disk remains unknown. This leaves a significant question mark over both the location of the planetesimals responsible for producing the belt's visible dust and the physical properties of those grains. We have performed the most extensive simulations to date of the inner, unresolved debris belt around HR 8799, using UNSW Australia's Katana supercomputing facility to follow the dynamical evolution of a model inner disk comprising 300,298 particles for a period of 60 Ma. These simulations have enabled the characterisation of the extent and structure of the inner disk in detail, and will in future allow us to provide a first estimate of the small-body impact rate and water delivery prospects for possible (as-yet undetected) terrestrial planet (s) in the inner system.
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Affiliation(s)
- B Contro
- School of Physics, UNSW Australia, Sydney, NSW, 2052, Australia,
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Gauza B, Béjar VJS, Pérez-Garrido A, Osorio MRZ, Lodieu N, Rebolo R, Pallé E, Nowak G. DISCOVERY OF A YOUNG PLANETARY MASS COMPANION TO THE NEARBY M DWARF VHS J125601.92-125723.9. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/804/2/96] [Citation(s) in RCA: 120] [Impact Index Per Article: 13.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Barman TS, Konopacky QM, Macintosh B, Marois C. SIMULTANEOUS DETECTION OF WATER, METHANE, AND CARBON MONOXIDE IN THE ATMOSPHERE OF EXOPLANET HR 8799 b. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/804/1/61] [Citation(s) in RCA: 143] [Impact Index Per Article: 15.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Seager S, Bains W. The search for signs of life on exoplanets at the interface of chemistry and planetary science. SCIENCE ADVANCES 2015; 1:e1500047. [PMID: 26601153 PMCID: PMC4643826 DOI: 10.1126/sciadv.1500047] [Citation(s) in RCA: 12] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/14/2015] [Accepted: 02/05/2015] [Indexed: 05/04/2023]
Abstract
The discovery of thousands of exoplanets in the last two decades that are so different from planets in our own solar system challenges many areas of traditional planetary science. However, ideas for how to detect signs of life in this mélange of planetary possibilities have lagged, and only in the last few years has modeling how signs of life might appear on genuinely alien worlds begun in earnest. Recent results have shown that the exciting frontier for biosignature gas ideas is not in the study of biology itself, which is inevitably rooted in Earth's geochemical and evolutionary specifics, but in the interface of chemistry and planetary physics.
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Affiliation(s)
- Sara Seager
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - William Bains
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- Rufus Scientific, Herts SG8 6ED, UK
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