Exploration of the Kuiper Belt by Stellar occultations
|
|
- Everett Cooper
- 6 years ago
- Views:
Transcription
1 Exploration of the Kuiper Belt by Stellar occultations Françoise Roques Y. Boissel, A. Doressoundiram, B. Sicardy, T. Widemann LESIA, Observatoire de Paris the occultation projects of the Paris team serendipitous occultations : a strategy of research the large telescopes research campaign results about the Kuiper Belt instrumental projects
2
3 Sicardy et al. 2003
4 Varuna : 6-7 december - Namibia: Hess - Hakos: clouded out - Brazil:Pico dos Dias: clear weather,star acquired with **high SNR**, no event seen - Belo Horizonte:light curve is obtained, still awaiting processing - Uruguay: Los Molinos: very low SNR signal obtained - Aigua: no observation possible due to very low elevation - Salto: no observation due to very low elevation - UK: Elliott's place. Star easily recorded, till ice prevented any observation - Germany:Munich: clouded out - France:St-Sulpice, star observed, no event detected - Meudon: clouded out - Pic du Midi: clouded out - Spain CalarAlto : no observation
5 stellar occultations :a diffracting phenomenon What? detection of the diffraction shadow of KBOs to scan invisible small and far populations Why? : small KBO are detectable the diffraction pattern is instructive How? fast photometry large telescope Where? : target stars with small angular size
6 Occultations : the future of the Kuiper Belt? T!h!e!!o!b!s!e!r!v!e!d!!s!l!o!p!e!!o!f!!t!h!e!!l!u!m!i!n!o!s!i!t!y!!f!u!n!c!t!i!o!n!!i!m!p!l!i!e!s!!t!h!a!t!! t!h!e!!s!i!z!e!!d!i!s!t!r!i!b!u!t!i!o!n!!o!f!!t!h!e!!k!u!i!p!e!r!!b!e!l!t! i!s!!c!o!n!s!i!s!t!e!n!t!!w!i!t!h!!a!!p!o!w!e!r!-!l!a!w!!w!i!t!h!!s!l!o!p!e!!q!!=!!4!.!2!5!!±!!0!.!2!5!!f!o!r!!o!b!j!e!c!t!s!!w!i!t!h!!d!i!a!m!e!t!e!r!s!!l!a!r!g!e!r!!t!h!a!n!!d! ~!5!0!!k!m!.! Fraser et al., 2008 From the luminosity function,we have inferred the underlying size distribution and find that it is consistent with a large object power-law slope q 1 ~ 4.8 that breaks to a slope q 2 ~1.9 at object diameter D ~ 60 km assuming 6% albedos. Fraser et al., 2008 Our results have demonstrated that the size distribution of the Kuiper belt can be described by three size distribution parameters, q1, q2, and D, and that, to accurately measure the break-slope q2 requires that the radial distribution be accounted for in a way which removes the ambiguity between source brightness and source size. We have found that q1 ~ 4, q2 ~ -1, and D ~ 40 km. Fraser et al., 2008
7 Distance of the occultors Roques et Moncuquet, 2000
8 The Fresnel scale F = (λ.r/2), : λ wavelength, R: distance of the occultor R = 3 AU, F = 245 m R = 40 AU, F = 1.1 km R = 10 5 AU, F = 55 km The Fresnel scale is a scaling factor of the occultation df/f = 10% => r = 0.2 Roques et Moncuquet, 2000
9 stellar occultations : a diffracting phenomenon r< 100 meters at 50 AU : ~ 50 stars per degrees-square for a 2-m telescope
10 The t2m/photometers campaign Observations on Bernard Lyot Telescope with multi-objects photometers field : 2 targets + 1 reference star 20 Hz 15h with S/N = 55 strategy : search for dips in the ligthcurve => first constraint on the size Distribution :q < 4.5 one potential event (r=150m) Roques et al., 2003
11 The large telescopes campaign The instrument : ULTRACAM an ultra-fast, triple-beam CCD camera (u : 0.36 µm, g :0.48 µm and i :0.77 µm) V. Dhillon, T. Marsh pulsars, X-ray binaries stars
12 The choice of the star
13 The data analysis : examples of false events Electronic problems Atmospheric effect
14 The data analysis 0.48 µm 0.77 µm a synthetic event: a 200 m radius object at 40 AU standard deviation (i) standard deviation (g)
15 The WHT-Ultracam results 5.6 σ 7.2 σ 5.3 σ
16 The WHT-Ultracam results Several cheks have been run to asses the validity of the detections : Comparison star The color signature Check the star position Chech the sky glitches Search in randomized data Search for events in the ligthcurve of a large star (occultations by Uranus and Neptune of stars with radius larger than 10 km at 40 AU)
17 The VLT-Ultracam results Search on intervals SNR > h Doressoundiram et al., submitted
18 The VLT-Ultracam results 200m at 50 AU 2000m at 5000 AU Doressoundiram et al., submitted
19 The Ultracam campaign result : I - an object of 110m at 9-19 AU Several isolated events in the occultation lightcurves announced during the 80 s (exploration of the Uranus-Neptune systems). After, lack of fast photometric instrumentation on large telescopes For exemple: 22 avril 1982 : during an occultation par Uranus, an event has been observed simultaneously with two nearby telescopes. compatible with a 1.4 km diameter object More dark matter around Uranus and Neptune?, Sicardy et al., Nature august 1980 : Isolated events detected during occultation : figure 5 The 15 august 1980 Occultation by the Uranian System : Structure of the Rings and Temperature of the Upper Atmosphere, Sicardy et al., Icarus, 52,
20 The VLT-Ultracam results II - no object in the Kuiper Belt AU v. dt 3 Fsu 200 meters objects are detectable Diffracting occultation scan a surface of : ds = 10-9 R -1.5 (AU) d 2. dt(h) R=40 AU No detections in 35 h => N(200 m) < at 40 AU
21 The VLT-Ultracam results III object farther than 100AU AU A cold extented disk composed of small objects? N(200m) : (0.5 earth mass) NB : serendipitous occultations is a statistical method, The verity will come from numbers Roques et al., AJ, in press
22 Bickerton et al Doressoundiram et al., submitted
23 Then, we need more observations more observations more observations
24 ULTRACAM : an ultra-fast, triple-beam CCD camera (V. Dhillon and T. Marsh) William Herschel Telescope VLT 5 - u : 0.36 µm, g :0.48 µm and i :0.77 µm) - two fields : one target + one reference
25 G. Georgevits, M. Aschley, W. Saunders (UNSW)
26 6df/UKST Difficult data analysis : Vibrations Fibers transmission factor scintillation Georgevits et al., 2006
27
28 UltraPhot :the science case : Compact pulsators in clusters : pulsating subdwarf B (sdb) stars, that are extreme horizontal branch objects with very high effective temperatures of about 30,000 K and pulsating white dwarfs belonging to the three known instability strips: DAVs or ZZ Ceti stars, DBVs and PNNV-DOVs with or without planetary nebula. periods between ~2 min and 1-2 hours Compact binaries in clusters : mapping of clusters- Cross correlation with X-ray sources : -white dwarfs, neutron stars and stellar mass black holes (time scale from second to milliseconds. On timescales of a tenth of a second, echo-tomography allow to determine the accretion geometry of cataclysmic variable and X-ray binaries (with ASTROSAT). Young Stellar Objects : UltraPhot will allow long-term monitoring of the irregular variability and survey of the variation with timescales shorter than a few hours. New database to improve our understanding of the nature of accretion processes.
29 UltraPhot la science : Exoplanets : Transit timing is a relativity new concept and few instruments exist to efficiently utilize the effect. One key desideratum for precise timing measurements is a very fast read-out from the CCD camera and today the best read-out possible is just under 1 second from the RISE instrument on the 2m Liverpool Telescope. Ultraphot offers an opportunity for two orders of magnitude better read-out frequency and therefore is ideally placed to fully exploit the transit timing effect. For Ultraphot, the timing accuracy should be at least 6 seconds per epoch, implying a resonant perturbing body could be detected in a system with 3-day period transiting hot-jupiter down to M, or 5.4 Lunar masses In addition, the potential moons of exoplanets may be also detected through timing mesurements. For example, a 1M around GJ436b would cause a 13.7 second rms amplitude and due to a linear scaling, 6 second accuracy corresponds to a 0.44 M exomoon sensitivity.
30 Stellar occultations Kuiper belt + Oort Cloud (!)
31 The VLT-Ultracam results II - no object in the Kuiper Belt AU Doressoundiram et al., submitted
32 The multi-fiber photometry concept : The first step is to upgrade MEFOS, a 29 fibers spectrograph formely at the ESO 3.6-m telescope. The project is to design a new fiber link and replace the spectrograph by a fast camera mounted on the 1.93m telescope of the Observatoire de Haute Provence (OHP, France).
33
34 UltraPhot concept Ultraphot instrument is composed : A multi-object fibres link A photometer composed of : - Structure Assembly : (Bench, Interface Support ) - Slit Entrance Assembly (slits, Back Illumination, Motion Tx&Ty.) - Optics Assembly : (Relays, Mirrors, Lenses, Dichroics ) - CCD-Camera Assembly
35 Analyse UltraCam r=2.4 Sky = 15-19
36
37
38 UltraPhot Full Frame CCD => No dead time one cycle = integration : 8.7 ms transfert+binning+reading : 1.3 ms
39 UltraPhot :scientific specifications nm spreaded in 3 colors acquisition frequency >= 100 Hz number of targets >= 100 photometric precision transmission factor > 20% input aperture on the sky >5arcsec diameter temporal and relative stability of the fibres
40 UltraPhot team Scientific PI Tecnical PI Scientific involvement Technical involvement Financial involvement Paris O.-LESIA X X X X Paris O.-GEPI X X X NTHU (Taiwan) X X X Napoli O. (Italia) X Paris O.-Luth X IAP X AAO (TBC) X Paris observatory - LESIA : F. Roques, A. Doressoundiram, Y. Boissel, B. Sicardy, J-T. Buey, M. Marteaud Paris Observatory - GEPI : I. Guinouard, D. Horville National Tsing Hua University - Department of Physics : H.-K. Chang, A. Kong, S.-P. Lai, C.-C. Hsieh Naples Observatory - INAF : D. de Martino, R. Silvotti Institut d Astrophysique de Paris : J.P. Beaulieu Paris Observatory LUTH:J. Schneider Anglo-Australian Observatory : T. Farrell, K. Shortridge ANR-NSC : 2.8 FTE
41 Budget Fibre link 50 K Mechanical 45 K Optical 30 K Camera 70K Others 15K?focal plate? Total 210 K ANR (french research agency) : 140k NSC (taiwanese research agency): 70k Planning T0 : T0 + 9 months : end of the design T0 +21 months : end of the manufacturing T months : end of integration
42 in conclusion, we need to do more observations use various telescope size - various technics - ground/space collaborate to convince of the interest of the occultation method and of fast photometry thanks very much for this workshop
UltraPhot, a photometric mode for FLAMES. Françoise Roques LESIA Observatoire de Paris
UltraPhot, a photometric mode for FLAMES Françoise Roques LESIA Observatoire de Paris UltraPhot Science : Variable Objects, Transits, Occultations Temporal resolution is a relatively unexplored region
More informationFast photometry at the Paris observatory: portable cameras and multi-fibre instruments
Fast photometry at the Paris observatory: portable cameras and multi-fibre instruments F. Roques 1,a, Y. Boissel a, H.-K. Chang b, A. Doressoundiram a, I-C. Shih a, B. Sicardy a, T. Widemann a a LESIA,
More informationThe Kuiper Belt Explored by Serendipitous Stellar Occultations
Roques et al.: Exploration by Serendipitous Stellar Occultations 545 The Kuiper Belt Explored by Serendipitous Stellar Occultations F. Roques Paris Observatory G. Georgevits University of New South Wales
More informationA Detection Method for Small Kuiper Belt Objects: The Search for Stellar Occultations
Icarus 147, 530 544 (2000) doi:10.1006/icar.2000.6452, available online at http://www.idealibrary.com on A Detection Method for Small Kuiper Belt Objects: The Search for Stellar Occultations Françoise
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationActuality of Exoplanets Search. François Bouchy OHP - IAP
Actuality of Exoplanets Search François Bouchy OHP - IAP How detect extrasolar planets? Two main difficulties : 1 A tiny angular separation 0.75 arcsec Sun Jupiter at 4 light years 4 Sun Jupiter at 100
More informationDesign Reference Mission. DRM approach
Design Reference Mission The Design Reference Mission (DRM) is a set of observing programs which together provide a tool to assist with tradeoff decisions in the design of the E-ELT (examples of observing
More informationThe Transneptunian Automated Occultation Survey (TAOS II) Matthew Lehner ASIAA
The Transneptunian Automated Occultation Survey (TAOS II) Matthew Lehner ASIAA Academia Sinica Institute of Astronomy and Astrophysics Universidad Nacional Autónoma de México Harvard-Smithsonian Center
More informationExploration of the Kuiper Belt by High-Precision Photometric Stellar Occultations: First Results
Exploration of the Kuiper Belt by High-Precision Photometric Stellar Occultations: First Results F. Roques, A. Doressoundiram, V. Dhillon, T. Marsh, S. Bickerton, J. J. Kavelaars, M. Moncuquet, M. Auvergne,
More informationUniverse Now. 2. Astronomical observations
Universe Now 2. Astronomical observations 2. Introduction to observations Astronomical observations are made in all wavelengths of light. Absorption and emission can reveal different things on different
More informationMichaël Gillon (Université de Liège, Belgium)
12th Meeting of the FNRS Contact Group Astronomie & Astrophysique 17 May 2011 Planetarium, Brussels Michaël Gillon (Université de Liège, Belgium) michael.gillon@ulg.ac.be ~1% pour Soleil + Jupiter Brown
More informationSmallest Kuiper Belt Object Ever Detected
National Aeronautics and Space Administration Smallest Kuiper Belt Object Ever Detected Taken from: Hubble 2009: Science Year in Review Produced by NASA Goddard Space Flight Center and the Space Telescope
More informationTelescope Arrays & Related Topics Bruce Holenstein, Rich Mitchell, and Dylan Holenstein
Telescope Arrays & Related Topics Bruce Holenstein, Rich Mitchell, and Dylan Holenstein Gravic Labs Workshop October 8, 2011 www.gravic.com 1 Topics The case for telescope arrays: SNR Gravic s array plans
More informationIntroduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical
Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical Trigonometry p. 9 The Earth p. 12 The Celestial Sphere p. 14 The
More informationPlanets around evolved stellar systems. Tom Marsh, Department of Physics, University of Warwick
Planets around evolved stellar systems Tom Marsh Department of Physics, University of Warwick Tom Marsh, Department of Physics, University of Warwick Slide 1 / 35 Tom Marsh, Department of Physics, University
More informationAPHRODITE. Ground-Based Observing Team -1-
APHRODITE Ground-Based Observing Team -1- Science Goals 1) Detecting Earth-like planets in the habitable zone of solar-type stars Earth around a G2V star @ 1 AU cm/s -2- Science Goals 1) Detecting Earth-like
More informationScience Olympiad Astronomy C Division Event National Exam
Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)
More informationExoplanet Search Techniques: Overview. PHY 688, Lecture 28 April 3, 2009
Exoplanet Search Techniques: Overview PHY 688, Lecture 28 April 3, 2009 Course administration final presentations Outline see me for paper recommendations 2 3 weeks before talk see me with draft of presentation
More informationCASE/ARIEL & FINESSE Briefing
CASE/ARIEL & FINESSE Briefing Presentation to NRC Committee for Exoplanet Science Strategy including material from the ARIEL consortium Mark Swain - JPL 19 April 2019 2018 California Institute of Technology.
More informationCecilia Fariña - ING Support Astronomer
Cecilia Fariña - ING Support Astronomer Introduction: WHT William Herschel Telescope 2 Introduction: WHT WHT located in La Palma, Canary Islands, Spain William Herschel Telescope l 2 3 Introduction: WHT
More informationSearch for Transiting Planets around Nearby M Dwarfs. Norio Narita (NAOJ)
Search for Transiting Planets around Nearby M Dwarfs Norio Narita (NAOJ) Outline Introduction of Current Status of Exoplanet Studies Motivation for Transiting Planets around Nearby M Dwarfs Roadmap and
More informationUsing Spitzer to Observe the Solar System
Using Spitzer to Observe the Solar System Sean Carey Spitzer Science Center 47 th DPS meeting 09 November 2015 SJC - 1 Spitzer Space Telescope NASA s Infrared Great Observatory Launched on 25 August 2003
More informationThe 14-Nov-2003 Titan Occultation. Eliot F. Young Angela Zalucha
The 14-Nov-2003 Titan Occultation Eliot F. Young Angela Zalucha Occultations: background For solar system bodies, stellar occultations occur when an object s parallactic motion intersects a star. Velocity
More informationMeter-Class Telescope Array Science
Meter-Class Telescope Array Science Bruce Holenstein and Russ Genet Second Phoenix Astro-Solar Workshop October 13, 2012 Talk adapted from presentation given at Alt-Az Initiative Portland VI Workshop,
More informationAstronomy C UT Regional, Spring 2018 Contact: Dhruva Karkada,
Astronomy C UT Regional, Spring 2018 Contact: Dhruva Karkada, dkarkada@gmail.com Competitors: School Name: Team Number: This test contains 5 sections, cumulatively worth 150 points. As always, you ll have
More informationHD Transits HST/STIS First Transiting Exo-Planet. Exoplanet Discovery Methods. Paper Due Tue, Feb 23. (4) Transits. Transits.
Paper Due Tue, Feb 23 Exoplanet Discovery Methods (1) Direct imaging (2) Astrometry position (3) Radial velocity velocity Seager & Mallen-Ornelas 2003 ApJ 585, 1038. "A Unique Solution of Planet and Star
More information2014 Uranus storm activity observations by amateur astronomers
2014 Uranus storm activity observations by amateur astronomers October 1 st, 2015, Nantes, France ( delcroix.marc@free.fr ), Planetary Observations section, French Astronomical Society (SAF) Station de
More informationSynergies between E-ELT and space instrumentation for extrasolar planet science
Synergies between E-ELT and space instrumentation for extrasolar planet science Raffaele Gratton and Mariangela Bonavita INAF Osservatorio Astronomico di Padova - ITALY Main topics in exo-planetary science
More informationarxiv: v1 [astro-ph] 12 May 2008
Mon. Not. R. Astron. Soc. 000, 1 6 (2008) Printed 29 August 2017 (MN LATEX style file v2.2) Millisecond dip events in the 2007 RXTE/PCA data of Sco X-1 and the TNO size distribution arxiv:0805.1579v1 [astro-ph]
More informationWhipple: Exploring the Solar System Beyond Neptune Using a Survey for Occultations of Bright Stars
Whipple: Exploring the Solar System Beyond Neptune Using a Survey for Occultations of Bright Stars Charles Alcock 1, Matthew Holman 1, Matthew Lehner 2,3,1, Stephen Murray 1, Pavlos Protopapas 1,4 and
More informationUseful Formulas and Values
Name Test 1 Planetary and Stellar Astronomy 2017 (Last, First) The exam has 20 multiple choice questions (3 points each) and 8 short answer questions (5 points each). This is a closed-book, closed-notes
More informationAstronomy 104: Second Exam
Astronomy 104: Second Exam Stephen Lepp October 29, 2014 Each question is worth 2 points. Write your name on this exam and on the scantron. Short Answer A The Sun is powered by converting hydrogen to what?
More informationToday. Next time. Emission & Absorption lines measuring elemental abundances. Doppler Effect. Telescopes technology to measure with
Today Emission & Absorption lines measuring elemental abundances Doppler Effect measuring motion Telescopes technology to measure with Solar System Overview what s out there? Next time Homework 3 Due Chemical
More informationLecture 8. October 25, 2017 Lab 5
Lecture 8 October 25, 2017 Lab 5 News Lab 2 & 3 Handed back next week (I hope). Lab 4 Due today Lab 5 (Transiting Exoplanets) Handed out and observing will start Friday. Due November 8 (or later) Stellar
More informationLecture Outlines. Chapter 15. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 15 Astronomy Today 7th Edition Chaisson/McMillan Chapter 15 The Formation of Planetary Systems Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Terrestrial and Jovian Planets
More informationSearching for extrasolar planets with SPHERE. Mesa Dino, Raffaele Gratton, Silvano Desidera, Riccardo Claudi (INAF OAPD)
Searching for extrasolar planets with SPHERE Mesa Dino, Raffaele Gratton, Silvano Desidera, Riccardo Claudi (INAF OAPD) The field of extrasolar planets today At the moment 2017 planets have been discovered.
More informationWide and Fast: A new Era of EMCCD and CMOS?
Wide and Fast: A new Era of EMCCD and CMOS? ZTF PTF?????? Gregg Hallinan California Institute of Technology gh@astro.caltech.edu Negligible 1 sec Transient Phase Space: Mansi Kasliwal Conventional CCDs
More informationFundamental Astronomy
H. Karttunen P. Kroger H. Oja M.Poutanen K.J. Donner (Eds.) Fundamental Astronomy Fifth Edition With 449 Illustrations Including 34 Colour Plates and 75 Exercises with Solutions < J Springer VII 1. Introduction
More informationChapter 5. Telescopes. Copyright (c) The McGraw-Hill Companies, Inc. Permission required for reproduction or display.
Chapter 5 Telescopes Copyright (c) The McGraw-Hill Companies, Inc. Permission required for reproduction or display. Why do we need Telescopes? Large collection area for photons than the eye long integration
More informationDetection and characterization of exoplanets from space
Detection and characterization of exoplanets from space Heike Rauer 1,2, 1:Institute for Planetary Research, DLR, Berlin 2:Center for Astronomy and Astrophysics, TU Berlin Exoplanet Space Missions and
More information1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO?
Astronomy 418/518 final practice exam 1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO? b. Describe the visibility vs. baseline for a two element,
More informationTerrestrial Planet (and Life) Finder. AST 309 part 2: Extraterrestrial Life
Terrestrial Planet (and Life) Finder AST 309 part 2: Extraterrestrial Life The Drake Equation: N = N * f pl n hab f L f C f T L/T Stars? Planets? Habitable Origin Complex Intelligence, Lifetime planets?
More informationThe MAORY Multi-Conjugate Adaptive Optics module Emiliano Diolaiti Istituto Nazionale di Astrofisica
The MAORY Multi-Conjugate Adaptive Optics module Emiliano Diolaiti Istituto Nazionale di Astrofisica On behalf of the MAORY module Consortium Shaping E-ELT Science and Instrumentation workshop, ESO, 25
More informationChapter 5. Telescopes. Copyright (c) The McGraw-Hill Companies, Inc. Permission required for reproduction or display.
Chapter 5 Telescopes Copyright (c) The McGraw-Hill Companies, Inc. Permission required for reproduction or display. Tools of the Trade: Telescopes The Powers of a Telescope Collecting Power Bigger telescope,
More informationAstronomy 1140 Quiz 4 Review
Astronomy 1140 Quiz 4 Review Anil Pradhan December 6, 2016 I The Outer Planets in General 1. How do the sizes, masses and densities of the outer planets compare with the inner planets? The outer planets
More informationAstronomy 405 Solar System and ISM
Astronomy 405 Solar System and ISM Lecture 18 Planetary System Formation and Evolution February 25, 2013 grav collapse opposed by turbulence, B field, thermal Cartoon of Star Formation isolated, quasi-static,
More informationAy 1 Midterm. Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA
Ay 1 Midterm Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA You have THREE HOURS to complete the exam, but it is about two hours long. The
More informationDelaware Asteroseismic Research Center. Asteroseismology with the Whole Earth Telescope (and More!)
Delaware Asteroseismic Research Center Asteroseismology with the Whole Earth Telescope (and More!) Asteroseismology Study of interior stellar structure as revealed by global oscillations. Important- -
More informationHubble Science Briefing: 25 Years of Seeing Stars with the Hubble Space Telescope. March 5, 2015 Dr. Rachel Osten Dr. Alex Fullerton Dr.
Hubble Science Briefing: 25 Years of Seeing Stars with the Hubble Space Telescope March 5, 2015 Dr. Rachel Osten Dr. Alex Fullerton Dr. Jay Anderson Hubble s Insight into the Lives of Stars Comes From:
More informationCurrently, the largest optical telescope mirrors have a diameter of A) 1 m. B) 2 m. C) 5 m. D) 10 m. E) 100 m.
If a material is highly opaque, then it reflects most light. absorbs most light. transmits most light. scatters most light. emits most light. When light reflects off an object, what is the relation between
More informationAST 101 INTRODUCTION TO ASTRONOMY SPRING MIDTERM EXAM 2 TEST VERSION 1 ANSWERS
AST 101 INTRODUCTION TO ASTRONOMY SPRING 2008 - MIDTERM EXAM 2 TEST VERSION 1 ANSWERS Multiple Choice. In the blanks provided before each question write the letter for the phrase that best answers the
More informationATINER's Conference Paper Series PHY
ATINER CONFERENCE PAPER SERIES No: LNG2014-1176 Athens Institute for Education and Research ATINER ATINER's Conference Paper Series PHY2014-1253 On Direct Measurements of the Angular Sizes of Stars by
More informationTrES Exoplanets and False Positives: Finding the Needle in the Haystack
Transiting Extrasolar Planets Workshop ASP Conference Series, Vol. 366, 2007 C. Afonso, D. Weldrake and Th. Henning TrES Exoplanets and False Positives: Finding the Needle in the Haystack F. T. O Donovan
More informationASTR STELLAR PULSATION COMPONENT. Peter Wood Research School of Astronomy & Astrophysics
ASTR 3007 - STELLAR PULSATION COMPONENT Peter Wood Research School of Astronomy & Astrophysics TOPICS COVERED Main types of variable stars Linear adiabatic pulsation theory => periods of pulsation Linear
More informationMULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Homework Ch 7, 8, 9 Name MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) Our most detailed knowledge of Uranus and Neptune comes from 1) A) the
More informationSearching for Other Worlds
Searching for Other Worlds Lecture 32 1 In-Class Question What is the Greenhouse effect? a) Optical light from the Sun is reflected into space while infrared light passes through the atmosphere and heats
More informationTransiting Extrasolar Planets
Transiting Extrasolar Planets Recent Progress, XO Survey, and the Future Christopher J. Burke Solar System Has Predominately Circular Orbits Top View Side View Planet Formation NASA/JPL-Caltech/R. Hurt
More information29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A
29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A There are 20 questions (Note: There will be 32 on the real thing). Read each question and all of the choices before choosing.
More informationASTR Midterm 2 Phil Armitage, Bruce Ferguson
ASTR 1120-001 Midterm 2 Phil Armitage, Bruce Ferguson SECOND MID-TERM EXAM MARCH 21 st 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.
More informationFrom the VLT to ALMA and to the E-ELT
From the VLT to ALMA and to the E-ELT Mission Develop and operate world-class observing facilities for astronomical research Organize collaborations in astronomy Intergovernmental treaty-level organization
More informationOne of a kind: A radio pulsing white dwarf binary star
One of a kind: A radio pulsing white dwarf binary star Dr. F.-J. (Josch) Hambsch VVS, BAV, AAVSO, GEOS Introduction White dwarfs are compact stars, similar in size to Earth but 200000 times more massive
More informationIndirect Methods: gravitational perturbation of the stellar motion. Exoplanets Doppler method
Indirect Methods: gravitational perturbation of the stellar motion Exoplanets The reflex motion of the star is proportional to M p /M * This introduces an observational bias that favours the detection
More informationAST 2010: Descriptive Astronomy EXAM 2 March 3, 2014
AST 2010: Descriptive Astronomy EXAM 2 March 3, 2014 DO NOT open the exam until instructed to. Please read through the instructions below and fill out your details on the Scantron form. Instructions 1.
More informationANSWER KEY. Stars, Galaxies, and the Universe. Telescopes Guided Reading and Study. Characteristics of Stars Guided Reading and Study
Stars, Galaxies, a the Universe Stars, Galaxies, and the Universe Telescopes Use Target Reading Skills Check student definitions for accuracy. 1. Electromagneticradiationisenergythatcan travel through
More informationPLATO-2.0 Follow-up. Questions addressed. PLATO Follow-up activities. Mass distribution Spectroscopy. Small mass planets are numerous => huge work
PLATO-20 Follow-up PLATO Follow-up activities Context'and'organisaon S Udry University of Geneva Overall PSPM structure The prime science product of PLATO = sample of fully characterized planets (various
More informationPLATO Follow-up. Questions addressed. Importance of the follow-up. Importance of the follow-up. Organisa(on*&*Progress*Report
PLATO Follow-up Organisa(on*&*Progress*Report Questions addressed A next generation transit mission will be efficient only with ground-based help S. Udry University of Geneva (Geneva Observatory) Needs
More informationCyclic variations in the periods of RR Lyr stars arxiv: v1 [astro-ph.sr] 29 Jan 2018
Cyclic variations in the periods of RR Lyr stars arxiv:1801.09702v1 [astro-ph.sr] 29 Jan 2018 Ennio Poretti 1 2 3, Jean-Francois Le Borgne 4 5 3, Alain Klotz 4 5 3, Monica Rainer 1 6 and Mercedes Correa
More informationUniverse Now. 12. Revision and highlights
Universe Now 12. Revision and highlights Practical issues about the exam The exam is on Monday 6.5. (12.00-16.00), lecture hall B121 (Exactum). Paper will be provided. You have 4 hours to finish the exam,
More informationASTB01 Exoplanets Lab
ASTB01 Exoplanets Lab Author: Anders Johansen Revision date: $Date: 2015/08/28 14:55:59 $ Planets orbiting stars other than the Sun are called exoplanets. Stellar light reflected off
More informationAstro 1010 Planetary Astronomy Sample Questions for Exam 3
Astro 1010 Planetary Astronomy Sample Questions for Exam 3 Chapter 6 1. Which of the following statements is false? a) Refraction is the bending of light when it passes from one medium to another. b) Mirrors
More information4. Direct imaging of extrasolar planets. 4.1 Expected properties of extrasolar planets. Sizes of gas giants, brown dwarfs & low-mass stars
4. Direct imaging of extrasolar planets Reminder: Direct imaging is challenging: The proximity to its host star: 1 AU at 1 for alpha Cen 0.15 for the 10th most nearby solar-type star The low ratio of planet
More informationNatural History of the Heavens in the Eighteenth Century
Natural History of the Heavens in the Eighteenth Century Last time Newtonian astronomy in the 18c The tasks The tools Measure planetary motions Explain motions with Newton s laws Prove long-term stability
More informationPhase-Referencing and the Atmosphere
Phase-Referencing and the Atmosphere Francoise Delplancke Outline: Basic principle of phase-referencing Atmospheric / astrophysical limitations Phase-referencing requirements: Practical problems: dispersion
More informationUranus & Neptune: The Ice Giants. Discovery of Uranus. Bode s Law. Discovery of Neptune
Uranus & Neptune: The Ice Giants Discovery of Uranus Discovery of Uranus & Neptune Properties Density & Composition Internal Heat Source Magnetic fields Rings Uranus Rotational Axis by William Herschel
More informationTransiting Hot Jupiters near the Galactic Center
National Aeronautics and Space Administration Transiting Hot Jupiters near the Galactic Center Kailash C. Sahu Taken from: Hubble 2006 Science Year in Review The full contents of this book include more
More informationAstronomy. Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes
Astronomy Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes are hot, compact stars whose mass is comparable to the Sun's and size to the Earth's. A. White dwarfs B. Neutron stars
More informationTHE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES DAVID F. GRAY University of Western Ontario, London, Ontario, Canada CAMBRIDGE UNIVERSITY PRESS Contents Preface to the first edition Preface to the
More informationThe Austrian contribution to the European Extremely Large Telescope
The Austrian contribution to the European Extremely Large Telescope Werner W. Zeilinger consortium Evolution of Telescope Size Scientific American 2015 14/15.Dec.2015 From Ground to Space 2 Discoveries
More information(1,2), E. (1), T. (3), P. (1,4), P. (5), C. (6), T. (7), M. (8), E. (3), D. (1), J.
TNOs are Cool: A survey of the trans-neptunian region. Results from the combined Herschel PACS and SPIRE observations of 9 bright targets at 70-500 μm. S. Fornasier (1,2), E. Lellouch (1), T. Müller (3),
More informationScience Update SBAG July, Andrew Cheng (JHU/APL) Karl Hibbitts (JHU/APL) Eliot Young (SwRI)
Science Update SBAG July, 2014 Andrew Cheng (JHU/APL) Karl Hibbitts (JHU/APL) Eliot Young (SwRI) Overview BOPPS science objectives BIRC calibration results UVVis update Science operations 4/23/14 2 BOPPS
More informationImproving Precision in Exoplanet Transit Detection. Aimée Hall Institute of Astronomy, Cambridge Supervisor: Simon Hodgkin
Improving Precision in Exoplanet Transit Detection Supervisor: Simon Hodgkin SuperWASP Two observatories: SuperWASP-North (Roque de los Muchachos, La Palma) SuperWASP-South (South African Astronomical
More informationAST 101 Intro to Astronomy: Stars & Galaxies
AST 101 Intro to Astronomy: Stars & Galaxies Telescopes Mauna Kea Observatories, Big Island, HI Imaging with our Eyes pupil allows light to enter the eye lens focuses light to create an image retina detects
More informationFinding habitable earths around white dwarfs with a robotic telescope transit survey
Finding habitable earths around white dwarfs with a robotic telescope transit survey Eric Agol Associate Professor Department of Astronomy University of Washington (UW) Feb 16, 2011 1 Evolution of a Sun-Like
More informationField Tests of elongated Sodium LGS wave-front sensing for the E-ELT
Florence, Italy. May 2013 ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13437 Field Tests of elongated Sodium LGS wave-front sensing for the E-ELT Gérard Rousset 1a, Damien Gratadour 1, TIm J. Morris 2,
More informationGemini Planet Imager. Raphaël Galicher from presentations provided by James Graham and Marshall Perrin
Gemini Planet Imager from presentations provided by James Graham and Marshall Perrin Outline Ojectives The instrument Three examples of observations The GPI Exoplanet Survey 2 Objectives Radial velocity
More informationA library of stellar light variations due to extra-solar comets
ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 140, 15 20 (1999) NOVEMBER II 1999, PAGE15 A library of stellar light variations due to extra-solar comets A. Lecavelier des Etangs
More informationAstronomy 1504 Section 10 Final Exam Version 1 May 6, 1999
Astronomy 1504 Section 10 Final Exam Version 1 May 6, 1999 Reminder: When I write these questions, I believe that there is one one correct answer. The questions consist of all parts a e. Read the entire
More informationTaiwanese American Occultation Survey: Products: dim KBO
Taiwanese American Occultation Survey: Products: dim KBO & by-products: Gamma Ray Bursters, Exo-planets, Flare stars by Typhoon Lee (phys1970) of AsiaA at Astrophysics Inst. NTHU on 4/9/2008 TAOS Collaborators
More informationFCAT Review Space Science
FCAT Review Space Science The Law of Universal Gravitation The law of universal gravitation states that ALL matter in the universe attracts each other. Gravity is greatly impacted by both mass and distance
More informationGravitational microlensing. Exoplanets Microlensing and Transit methods
Gravitational microlensing Exoplanets Microlensing and s Planets and Astrobiology (2016-2017) G. Vladilo May take place when a star-planet system crosses the visual of a background star, as a result of
More informationThoughts on Astrophysics with nano/6u cubesats
18 July 2012 Thoughts on Astrophysics with nano/6u cubesats Harvey Butcher Stars & Planets Interstellar medium Transients Other ideas Recall: Space platforms can provide: Access to γ-ray, x-ray, UV, IR,
More informationAstronomy 405 Solar System and ISM
Astronomy 405 Solar System and ISM Lecture 17 Planetary System Formation and Evolution February 22, 2013 grav collapse opposed by turbulence, B field, thermal Cartoon of Star Formation isolated, quasi-static,
More informationThere are 4 x stars in the Galaxy
ExtraSolar Planets Our solar system consists of 1 Star 4 Jovian planets (+ icy moons) 4 Terrestrial planets The asteroid belt (minor planets) The Kuiper belt (dwarf planets, plutinos and TNOs) The Oort
More informationEarth, Uranus, Neptune & Pluto
14a. Uranus, Neptune & Pluto The discovery of Uranus & Neptune Uranus is oddly tilted & nearly featureless Neptune is cold & blue Uranus & Neptune are like yet dislike Jupiter The magnetic fields of Uranus
More informationHigh contrast imaging at 3-5 microns. Philip M. Hinz University of Arizona Matt Kenworthy, Ari Heinze, John Codona, Roger Angel
High contrast imaging at 3-5 microns Philip M. Hinz University of Arizona Matt Kenworthy, Ari Heinze, John Codona, Roger Angel University of Arizona ABSTRACT The 6.5 m MMT with its integrated deformable
More informationSERENA Meeting. Visby Interplanetary Space Physics Institute (IFSI) Roma, Italy
SERENA Meeting Visby 2010 Na EXOSPHERE GROUND--BASED GROUND OBSERVATIONS: past and future Valeria Mangano Interplanetary Space Physics Institute (IFSI) Roma, Italy Outline Italian campaign at TNG in 2002-2009
More informationPolarimetry and spectral imaging of mature Jupiter and super Earth SEE COAST
Polarimetry and spectral imaging of mature Jupiter and super Earth SEE COAST Jean Schneider, A. Boccaletti, P. Baudoz, G. Tinetti, D. Stam, R. Gratton,... Eth Zurich Univ. of Leiden Univ. Amsterdam CSL
More informationCHARACTERIZING EXOPLANETS SATELLITE
JWST Transit Workshop Pasadena CHARACTERIZING EXOPLANETS SATELLITE David Ehrenreich! CHEOPS Mission Scientist s first small-class mission Mass-radius diagram Apparent continuity of masses for exoplanets
More informationCompact Evolved Binaries with exoplanets
Low-mass companion M-dwarf/brown dwarf/white dwarf White dwarf Accretion disk Compact Evolved Binaries with exoplanets Puji Irawati Hot spot Credit: Stuart Littlefair 1 Overview of the project Main goal:
More information