DOCSLIB.ORG

The LICK OBSERVER AUTOMATED PLANET FINDER (APF) BAGS FIRST SUCCESSFUL FIRST LIGHT for SHANE ADAPTIVE PLANETS by Steven S

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The LICK OBSERVER AUTOMATED PLANET FINDER (APF) BAGS FIRST SUCCESSFUL FIRST LIGHT for SHANE ADAPTIVE PLANETS by Steven S Volume 2 Spring 2014 Number 2 University of California Observatories Lick Observatory Est. 1888 The LICK OBSERVER AUTOMATED PLANET FINDER (APF) BAGS FIRST SUCCESSFUL FIRST LIGHT FOR SHANE ADAPTIVE PLANETS By Steven S. Vogt • UCSC Astronomer OPTICS! By Don Gavel (PI) and the ShaneAO Team • UCO The first planets Earth, Mars, and Jupiter overlaid for discovered using data from reference. ShaneAO off ShaneAO on the Automated Planet With its three gas giant planets Finder (APF) Telescope orbiting at distances similar to the are described in a paper, terrestrial planets of our own solar recently accepted for system, and an outer 4th gas giant in publication, that was authored by the an orbit similar to our own Jupiter, Lick-Carnegie Exoplanet Team, co-led this system is fundamentally alien. Yet, it is also typical of the sorts of planetary systems found around ~10% of F, G, and K stars. HD 141399 was long suspected of hosting planets from data gathered by HIRES on Keck, but there was insufficient cadence and precision to characterize the multiple orbits securely. APF's ability to get high precision with high After years of hard work from the capability for Lick astronomers and by cadence quickly clinched all the orbits, ShaneAO team (including 3 PhD providing technology proof for the characterizing each with high graduate students and one undergrad), next generation of Keck AO accuracy. Indeed, the quality of the high-performance AO correction was instruments. APF measurements shows that APF achieved within the first hour of on-sky is functioning fully as expected, and commissioning on April 12, 2014. has, since July 2013, been delivering Special thanks are due for the intensive state-of-the-art radial velocity and expert help from the entire staff by Steve Vogt of UCSC and R. Paul precision.✯ on Mt. Hamilton. Butler of Carnegie. The left frame shows the new data of The first catch was a 4-planet system M92, a famous and well-studied cluster orbiting the slightly evolved K-type star HELP SAVE LICK of stars, with no AO correction. The HD 141399, about 118 light-years right shows the same field with the new away. This system features four gas Click here to see the latest AO system turned on. The three stars Renate Kupke in the control room during giant planets in orbits with periods of news, letters, and articles in the circle are 0.42 and 0.58 arc- ShaneAO first light. 94d, 202d, 2.9y, and 10.1y, as shown in about Lick, or to become seconds apart. ShaneAO represents a ShaneAO is made possible through an top view (red lines) in the figure. This a donor or Friend of Lick leap forward for UC astronomical NSF Major Research Instrumentation figure also shows (dashed lines) the Observatory. instrumentation, with its advanced grant, #0923585. ✯ orbits of our own Mercury, Venus, LICK’S STORM PROVIDES NEW MAPS OF GAS A GLIMMER OF LIGHT FROM POLARIZED WORLDS By Sloane Wiktorowicz • Sagan Fellow at UCO SWIRLING AROUND SUPER-MASSIVE BLACK HOLES By Liuyi Pei • PhD Student at UC Irvine Forty years ago, of 0.61 in UV and blue light. However, the detection of HST photometry during stellar The Space Telescope and polarized, occultation of the planet allowed Evans Optical Reverberation scattered light et al. (2013, ApJ, 772, L16) to measure a Mapping (STORM) from Venus blue albedo of only 0.23. POLISH2 program is an international revealed the data are inconsistent with the 0.61 campaign to obtain the presence of albedo model but are possibly first-ever detailed map of the broad- Sloane with his POLISH2 s u l f u r i c a c i d line region (BLR) of a nearby active instrument at the Shane 3-meter Telescope. droplets in the galactic nucleus (AGN). Doppler- atmosphere. A broadened emission lines of the BLR 100-fold improvement in instrument are emitted by gas orbiting within sensitivity, required to obtain similar several light-days around a black hole. "is plot shows the spectral region around the H- results on distant exoplanets, is now The BLR is irradiated by the central beta emission line in NGC 5548 on two di#erent possible. Ground-based polarimetry black hole accretion disk seen as the nights. "e broad H-beta emission comes from now rivals the sensitivity of the recently spectral continuum. Reverberation ionized gas in rapid rotation around the black hole, defunct Kepler Mission (Wiktorowicz, POLISH2 linear polarimetry of the HD 189733 mapping uses the time lags between the while the narrow [O III] (doubly ionized oxygen) star+planet vs. the planet’s orbit, where 0 is changes in the continuum and emission emission lines come from a much larger region in 2009, ApJ, 696, 1116) at a fraction of during mid-transit and 0.5 is during the host galaxy. the cost ($40k). Since 2011, the occultation of the exoplanet by the host star. lines to characterize the size, structure, POLISH2 instrument (Wiktorowicz & Blue POLISH2 data are inconsistent with the and dynamics of the BLR. securing optical spectra from the Kast Matthews, 2008, PASP, 120, 1282) has black 0.61 albedo curve (original claim) but STORM’s target is the Seyfert 1 Spectrograph on the 3-m Shane monitored a handful of known possibly match the red 0.23 one (from HST). galaxy NGC 5548, which will be telescope. For each dark run from exoplanets with the Lick 3-m Shane consistent with the 0.23 one. Ongoing monitored photometrically and February to July of 2014, each group Telescope to search for polarized efforts with POLISH2 are soon to be spectroscopically for six months. UV of regularly-scheduled Kast observers scattering in blue light (B band). finished that will significantly improve spectra from an 180-orbit HST is taking two observations of NGC A reported detection of scattered light the accuracy of nightly measurements. program will monitor carbon IV lines 5548 each night. This interrupt-mode from the transiting hot Jupiter HD Therefore, the first, reliable isolation of from the inner BLR. Over the same of observing gives Lick Observatory 189733b (Berdyugina et al., 2011, ApJ, scattered light from a distant exoplanet six-month span, Lick will monitor the the unique ability to provide 728, L6 [B11a]) requires nearly the will soon be another scientific triumph changes in the hydrogen-beta line observations for a long monitoring maximum possible reflectivity (albedo) from the historic Lick 3-m telescope. ✯ which comes from the outer BLR by (Continued on page 2) The LICK OBSERVER The LICK OBSERVER Spring 2014 Page 2 LICK OBSERVATORY NEWS (Black Holes from page 1) period with only minimal interruptions to the IRISH MINISTER OF STATE VISITS observing time of other research groups using Shane. LICK OBSERVATORY Meanwhile, Lick’s robotic KAIT telescope contributes For St Patrick's day, world landmarks turn green, regular photometry from optical images. Irish Ministers of state disperse across the globe, and My thesis contribution to STORM is analyzing while presenting a bowl of shamrock, the Taoiseach optical spectra of NGC 5548 from the Lick 3-m as (Irish Prime Minister) has the ear of the US well the MDM 1.3-m and APO 3.5-m telescopes. My President. This year, Minister of Arts, Culture and job is to construct light curves to track the time lags the Gaeltacht (Gaelic Affairs) James Deenihan toured between the changing broad-lines (see Figure) and the Bay Area, which has links with Ireland through continuum. Combining data into standardized the twinning of San Jose with Dublin and San parameters and quality from different telescopes is Francisco with Cork. On March 18, the Minister was challenging and requires communication and coordination across multiple campuses and observatories, as well as the willing cooperation of fellow observers. Special times at Lick Observatory's public The results from this collaboration will be the first programs. (Image Credit: E. Gates) of its kind, and Lick Observatory’s participation in STORM has brought together observers across 2014 PUBLIC PROGRAMS AT multiple UC campuses in a combined effort to further our understanding of the structure of AGNs and LICK OBSERVATORY their role in the co-evolution of galaxies and super- massive black holes through cosmic time. ✯ In the 126 years since its inauguration, Lick Observatory has continued to offer the public opportunities to visit, observe through its telescopes, REPORT FROM LICK and share an understanding of our wondrous Universe. Thus, in addition to its pedigree as an OBSERVATORY COUNCIL active centre of forefront research and development, In March, Mr. Adam Kablanian became the newest Lick is a pioneer of science outreach. member of the Lick Observatory Council (LOC). This summer will see those traditions continue as Mr. Kablanian is currently the Executive Chairman the public programs of this iconic San Francisco Bay UCO Director Sandy Faber with Bob Kibrick present James Deenihan with a souvenir of his visit to Lick. (Image Credit: M. Bolte).) of PlasmaSi, a startup company focused on sentinel welcome thousands of participants to its becoming the leader in thin film barrier technology beautiful mountaintop setting. welcomed (in Gaelic) to Mount Hamilton, and learned of Lick's history, Irish connections, and the for OLED displays, and a board member of Cortex Summer Visitors Program TARA project (http://www.bco.ie/tara/), an initative MCP, a startup company developing a new foundational platform for the future of Mobile Every second weekend between Memorial Day and of Blackrock Castle Observatory in Cork. TARA seeks to stimulate interest in science, technology, Commerce. Mr. Kablanian has numerous inventions, Labor Day, renowned astronomers will speak about 14 patents granted in the area of micro-chip design, astronomical discoveries, ancient, modern and those engineering, math, culture, and cooperation among thousands of students in Ireland, California, and and he is the author and co-author of over 15 yet to be made.
Load more

Recommended publications
  • Evergreen • East Hills Vision Strategy Project San José, California
    DRAFT EIR for the EVERGREEN • EAST HILLS VISION STRATEGY PROJECT SAN JOSÉ, CALIFORNIA State Clearinghouse Number: 2005102007 City of San José File Numbers: GP05-08-01A and PDC05-050 GP05-08-01B and PDC05-051 GP05-08-01C and PDC05-048 GP05-08-01D and PDC05-049 GP05-08-01E and PDC05-052 GP05-08-01F and PDC05-053 CITY OF SAN JOSÉ FEBRUARY 2006 TABLE OF CONTENTS SECTION 1. INTRODUCTION, BACKGROUND, & PROJECT OBJECTIVES .........1 1.1 Introduction .........................................................1 1.2 Project Location .....................................................1 1.3 Background .........................................................1 1.4 Project Objectives ...................................................10 1.5 Uses of the EIR .....................................................12 1.5.1 Lead and Responsible CEQA Agencies ............................12 1.5.2 Level of Environmental Review Provided by this EIR ................12 SECTION 2. DESCRIPTION OF THE PROPOSED PROJECT ......................28 2.1 Land Use Development Scenarios ......................................28 2.1.1 Introduction and Overview ......................................28 2.1.2 Development Scenarios for the Arcadia Property ....................33 2.1.3 Development Scenarios for the Pleasant Hills Golf Course Property .....38 2.1.4 Development Scenarios for the Berg/IDS Property ...................42 2.1.5 Development Scenarios for the Legacy Partners Property ..............48 2.1.6 Development Scenarios for the Evergreen Valley College Property ......51 2.1.7 Other General Plan Amendments .................................55 2.2 Transportation and Community Amenity Projects ..........................56 2.2.1 Operational Improvements on U.S. 101 ............................61 2.2.2 Reconfigure White Road between Ocala Avenue and Aborn Road ......63 2.2.3 Reconfigure Ocala Avenue between Capitol Expwy and White Road ....63 2.2.4 Improvements along Capitol Expwy between Quimby Rd.
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • Five-Year Review of the UC Observatories (UCO)
    UNIVERSITY OF CALIFORNIA, ACADEMIC SENATE BERKELEY • DAVIS • IRVINE • LOS ANGELES • MERCED • RIVERSIDE • SAN DIEGO • SAN FRANCISCO SANTA BARBARA • SANTA CRUZ Kum-Kum Bhavnani Chair of the Assembly of the Academic Senate Telephone: (510) 987-9303 Faculty Representative to the Regents Email:[email protected] University of California 1111 Franklin Street, 12th Floor Oakland, California 94607-5200 July 1, 2020 THERESA MALDONADO, VICE PRESIDENT RESEARCH AND INNOVATION Re: Five-Year Review of the UC Observatories (UCO) Dear Theresa, At its June 24, 2020 meeting, the Academic Council approved the attached Five-Year Review of the UC Observatories (UCO) Multicampus Research Unit (MRU). Following procedures outlined in the Compendium, the review was performed by a Joint Senate Review Committee, led by the University Committee on Research Policy (UCORP) with input from the University Committee on Planning and Budget (UCPB) and the Coordinating Committee on Graduate Affairs (CCGA). The Review Committee recommends renewing the UCO as an MRU unit for five years, and also makes recommendations for strengthening the UCO in the areas of budget and administrative transparency, governance, student participation in research, and education and outreach. We request that that you forward the report to the UCO director. The Academic Council appreciates the significant time and effort the Review Committee spent in preparing and writing this report. In particular, I want to recognize the substantial contributions and outstanding leadership of UCORP Chair Andrew Baird. Please do not hesitate to contact me if you have additional questions. Sincerely, Kum-Kum Bhavnani, Chair Academic Council cc: Academic Council UCORP Senate Directors Review of University of California Observatories (UCO) ________________________________________________________________ University Committee on Research Policy (UCORP) (Lead Committee) University Committee on Planning and Budget (UCPB) Coordinating Committee on Graduate Affairs (CCGA) May 19, 2020 l.
    [Show full text]
  • Pre-Vetted False Positives for TESS
    Swarthmore College Works Physics & Astronomy Faculty Works Physics & Astronomy 11-1-2018 The KELT Follow-Up Network And Transit False-Positive Catalog: Pre-Vetted False Positives For TESS K. A. Collins K. I. Collins FJ.ollow Pepper this and additional works at: https://works.swarthmore.edu/fac-physics J. Labadie-Bar Part of the Astrtz ophysics and Astronomy Commons Let us know how access to these works benefits ouy K. G. Stassun See next page for additional authors Recommended Citation K. A. Collins, K. I. Collins, J. Pepper, J. Labadie-Bartz, K. G. Stassun, B. S. Gaudi, D. Bayliss, J. Bento, K. D. Colón, D. Feliz, D. James, M. C. Johnson, R. B. Kuhn, M. B. Lund, M. T. Penny, J. E. Rodriguez, R. J. Siverd, D. J. Stevens, X. Yao, G. Zhou, M. Akshay, G. F. Aldi, C. Ashcraft, S. Awiphan, Ö. Baştürk, D. Baker, T. G. Beatty, P. Benni, P. Berlind, G. B. Berriman, Z. Berta-Thompson, A. Bieryla, V. Bozza, S. C. Novati, M. L. Calkins, J. M. Cann, D. R. Ciardi, W. D. Cochran, David H. Cohen, D. Conti, J. R. Crepp, I. A. Curtis, G. D'Ago, K. A. Diazeguigure, C. D. Dressing, F. Dubois, E. Ellington, T. G. Ellis, G. A. Esquerdo, P. Evans, A. Friedli, A. Fukui, B. J. Fulton, E. J. Gonzales, J. C. Good, J. Gregorio, T. Gumusayak, D. A. Hancock, C. K. Harada, R. Hart, E. G. Hintz, H. Jang-Condell, E. J. Jeffery, Eric L.N. Jensen, E. Jofré, M. D. Joner, A. Kar, D. H. Kasper, B. Keten, J.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • Ghost Imaging of Space Objects
    Ghost Imaging of Space Objects Dmitry V. Strekalov, Baris I. Erkmen, Igor Kulikov, and Nan Yu Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109-8099 USA NIAC Final Report September 2014 Contents I. The proposed research 1 A. Origins and motivation of this research 1 B. Proposed approach in a nutshell 3 C. Proposed approach in the context of modern astronomy 7 D. Perceived benefits and perspectives 12 II. Phase I goals and accomplishments 18 A. Introducing the theoretical model 19 B. A Gaussian absorber 28 C. Unbalanced arms configuration 32 D. Phase I summary 34 III. Phase II goals and accomplishments 37 A. Advanced theoretical analysis 38 B. On observability of a shadow gradient 47 C. Signal-to-noise ratio 49 D. From detection to imaging 59 E. Experimental demonstration 72 F. On observation of phase objects 86 IV. Dissemination and outreach 90 V. Conclusion 92 References 95 1 I. THE PROPOSED RESEARCH The NIAC Ghost Imaging of Space Objects research program has been carried out at the Jet Propulsion Laboratory, Caltech. The program consisted of Phase I (October 2011 to September 2012) and Phase II (October 2012 to September 2014). The research team consisted of Drs. Dmitry Strekalov (PI), Baris Erkmen, Igor Kulikov and Nan Yu. The team members acknowledge stimulating discussions with Drs. Leonidas Moustakas, Andrew Shapiro-Scharlotta, Victor Vilnrotter, Michael Werner and Paul Goldsmith of JPL; Maria Chekhova and Timur Iskhakov of Max Plank Institute for Physics of Light, Erlangen; Paul Nu˜nez of Coll`ege de France & Observatoire de la Cˆote d’Azur; and technical support from Victor White and Pierre Echternach of JPL.
    [Show full text]
  • City Manager's Update July 11, 2019
    July 11, 2019 Department of Public Safety Hosts Third Youth Leadership Academy The Department of Public Safety (DPS) hosted its third annual Youth Leadership Academy from June 17 to 27. Twenty-seven students entering grades 7 through 9 participated in the two-week program. Participants learned valuable skills in communication, conflict resolution, character building, decision making, and goal setting. They also received information about cyber-safety, bullying, and lifetime fitness. This program was funded by a grant from the Bureau of State and Community Corrections. For information about the Youth Leadership Academy, contact Elaine Ketell at 408-730-7234 or [email protected]. Water Quality Information Available Online The City of Sunnyvale’s Water Quality Report (Consumer Confidence Report), is now available. Our goal is to provide residents with high- quality, safe, reliable drinking water that meets every federal and state water requirement. Sunnyvale analyzes more than 20,000 water samples annually. The report lets customers know where the drinking water comes from, how it is treated to make it safe, the results of water quality monitoring and other important information about water quality. This information is provided in compliance with requirements established by the U.S. Environmental Protection Agency and the California Department of Health Services. If you have any questions or need further information, please contact Kevin Woodworth, Water Distribution Supervisor at 408-730-7900 or [email protected]. Update Sunnyvale 7/11/19 Sunnyvale DPS Deploys UAV in Search for a Missing Person On Monday, June 24, Sunnyvale DPS utilized its newly formed Unmanned Aerial Vehicle (UAV) unit on its maiden deployment.
    [Show full text]
  • Exoplanet Community Report
    JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probe­class missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2
    [Show full text]
  • AMD-Stability and the Classification of Planetary Systems
    A&A 605, A72 (2017) DOI: 10.1051/0004-6361/201630022 Astronomy c ESO 2017 Astrophysics& AMD-stability and the classification of planetary systems? J. Laskar and A. C. Petit ASD/IMCCE, CNRS-UMR 8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 7 November 2016 / Accepted 23 January 2017 ABSTRACT We present here in full detail the evolution of the angular momentum deficit (AMD) during collisions as it was described in Laskar (2000, Phys. Rev. Lett., 84, 3240). Since then, the AMD has been revealed to be a key parameter for the understanding of the outcome of planetary formation models. We define here the AMD-stability criterion that can be easily verified on a newly discovered planetary system. We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit the planetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require some additional dynamical studies to conclude on their stability. The AMD-stability classification is applied to the 131 multiplanet systems from The Extrasolar Planet Encyclopaedia database for which the orbital elements are sufficiently well known. Key words. chaos – celestial mechanics – planets and satellites: dynamical evolution and stability – planets and satellites: formation – planets and satellites: general 1. Introduction motion resonances (MMR, Wisdom 1980; Deck et al. 2013; Ramos et al. 2015) could justify the Hill-type criteria, but the The increasing number of planetary systems has made it nec- results on the overlap of the MMR island are valid only for close essary to search for a possible classification of these planetary orbits and for short-term stability.
    [Show full text]
  • Nasa and the Search for Technosignatures
    NASA AND THE SEARCH FOR TECHNOSIGNATURES A Report from the NASA Technosignatures Workshop NOVEMBER 28, 2018 NASA TECHNOSIGNATURES WORKSHOP REPORT CONTENTS 1 INTRODUCTION .................................................................................................................................................................... 1 What are Technosignatures? .................................................................................................................................... 2 What Are Good Technosignatures to Look For? ....................................................................................................... 2 Maturity of the Field ................................................................................................................................................... 5 Breadth of the Field ................................................................................................................................................... 5 Limitations of This Document .................................................................................................................................... 6 Authors of This Document ......................................................................................................................................... 6 2 EXISTING UPPER LIMITS ON TECHNOSIGNATURES ....................................................................................................... 9 Limits and the Limitations of Limits ...........................................................................................................................
    [Show full text]
  • Lick Observatory Records: Photographs UA.036.Ser.07
    http://oac.cdlib.org/findaid/ark:/13030/c81z4932 Online items available Lick Observatory Records: Photographs UA.036.Ser.07 Kate Dundon, Alix Norton, Maureen Carey, Christine Turk, Alex Moore University of California, Santa Cruz 2016 1156 High Street Santa Cruz 95064 [email protected] URL: http://guides.library.ucsc.edu/speccoll Lick Observatory Records: UA.036.Ser.07 1 Photographs UA.036.Ser.07 Contributing Institution: University of California, Santa Cruz Title: Lick Observatory Records: Photographs Creator: Lick Observatory Identifier/Call Number: UA.036.Ser.07 Physical Description: 101.62 Linear Feet127 boxes Date (inclusive): circa 1870-2002 Language of Material: English . https://n2t.net/ark:/38305/f19c6wg4 Conditions Governing Access Collection is open for research. Conditions Governing Use Property rights for this collection reside with the University of California. Literary rights, including copyright, are retained by the creators and their heirs. The publication or use of any work protected by copyright beyond that allowed by fair use for research or educational purposes requires written permission from the copyright owner. Responsibility for obtaining permissions, and for any use rests exclusively with the user. Preferred Citation Lick Observatory Records: Photographs. UA36 Ser.7. Special Collections and Archives, University Library, University of California, Santa Cruz. Alternative Format Available Images from this collection are available through UCSC Library Digital Collections. Historical note These photographs were produced or collected by Lick observatory staff and faculty, as well as UCSC Library personnel. Many of the early photographs of the major instruments and Observatory buildings were taken by Henry E. Matthews, who served as secretary to the Lick Trust during the planning and construction of the Observatory.
    [Show full text]
  • Introduction (PDF)
    Section Name –YUDHIJIT BHATTACHARJEE AND DANIEL CLERY In 1992, astronomers announced that a whirling neutron star our sun, but others are truly alien: hot Jupiters, mini-Neptunes, called a millisecond pulsar harbored the fi rst known planets outside super-Earths. our solar system: extrasolar planets, or exoplanets. Two decades on, To help readers navigate the bewildering variety of new worlds exoplanets are practically an astronomical commodity. Nearly 900 and their discoverers, Science presents this guide for the perplexed: of them have been confi rmed, and hundreds of fresh candidates are an overview of planet-hunting techniques and representative efforts, turning up every month. Some resemble the familiar orbs circling followed by an informal glossary of popular exo-objects. Radial velocity measurement is the mother of exoplanet search techniques. Michel Mayor and Didier Queloz of the Observa- tory of Geneva in Switzerland used it in 1995 to make the fi rst confi rmed detection of an exoplanet around a sunlike star, and it’s still going strong. As a planet orbits a star, its gravity causes the star to move around their com- mon center of gravity, usually inside the star. If we view such a system edge-on, the star would appear to be wobbling from side to side. Current telescopes can’t on May 4, 2013 detect such tiny movements, but they can spot a wobble back and forth along the line of sight because such changes in radial velocity raise and lower the frequency of the star’s light. To spot exoplanets this way, astronomers don’t need a huge telescope or one in S space—just an extremely sensitive spectrometer and lots of time.
    [Show full text]