GAIA Science and Mission

Save this PDF as:
 WORD  PNG  TXT  JPG

Size: px
Start display at page:

Download "GAIA Science and Mission"

Transcription

1 GAIA Science and Mission Nicholas Walton Institute of Astronomy The University of Cambridge p1

2 Outline Gaia high level science drivers Example science objectives Gaia mission overview Gaia data analysis and processing Gaia Science Team Gaia and the UK dimension Thanks to Gerry Gilmore and Floor van Leeuwen at the IoA for input to these slides. p2

3 What's driving Gaia? Towards a more precise understanding of the current structure and history of our galaxy: Distributions of mass, energy and angular momentum Signatures of mergers Missing mass, dark matter? Dwarf galaxies within the local group History of star formation and enrichment of the interstellar dust and gas In a nutshell map the Galaxy and Local Universe a billion stars, μ arcsec astrometry, to V= mag one μarcsec : 'resolve a finger nail on the moon!' p3

4 What's required for this mapping? Accurate positions and velocities of stars over a large volume of space Complete survey down to a limiting magnitude size of the galaxy implies a Radius ~10 to kpc (dist.mod: 15.0 to 16.5) Approximately th magnitude, 109 objects Complementary data required to 'sort' the objects effective temperature surface gravity metallicity luminosity p4

5 Gaia: Design Considerations Astrometry (V < ): completeness to th mag (with on-board detection) : 109 stars accuracy: 1025 μarcsec at 15th mag (c.f. Hipparcos: 1 milliarcsec at 9th mag) scanning satellite, two viewing directions global accuracy, with optimal use of observing time principles: global astrometric reduction (as for Hipparcos) Photometry (V < ): astrophysical diagnostics (low-dispersion photometry)/ chromaticity Teff ~ 0 K, log g, [Fe/H] to 0.2 dex, extinction Radial velocity (V < 1617): application: third component of space motion, perspective acceleration dynamics, population studies, binaries spectra: chemistry, rotation principles: slitless spectroscopy using Ca triplet ( nm) p5

6 Gaia: Complete, Faint, Accurate Hipparcos Gaia Magnitude limit Completeness Bright limit Number of objects Effective distance limit Quasars Galaxies Accuracy 1 kpc None None 1 milliarcsec Photometry photometry Radial velocity Observing programme 2-colour (B and V) None Pre-selected mag mag 6 mag 26 million to V = million to V = million to V = 1 Mpc 5 x µarcsec at V = µarcsec at V = µarcsec at V = Low-res. spectra to V = 15 km/s to V = Complete and unbiased source: ESA p6

7 Main Performances and Capabilities Two orders of magnitude improvement over current best precision First large-area high-spatial resolution survey Unbiased sample of 1% of Galactic stars Every one of these stars in the Galaxy and LG will have its movement observed A major resource for astronomy p7

8 GAIA: Some Science Objectives Structure and kinematics of our Galaxy: Stellar populations: shape and rotation of bulge, disk and halo internal motions of star forming regions, clusters, etc nature of spiral arms and the stellar warp space motions of all Galactic satellite systems physical characteristics of all Galactic components initial mass function, binaries, chemical evolution star formation histories Tests of galaxy formation: dynamical determination of dark matter distribution reconstruction of merger and accretion history p8

9 10 as = 10% distances at 10 kpc equiv 1AU at 100 kpc N A Walton: GAIA Science GSD08 17 KIAA Mar,: 08 2 Dec, 08 p9 10 as/yr = 1 km/sec at kpc Printed: p9 02/12/08

10 Astrometric Accuracy Massive leap from Hipparcos to Gaia: accuracy: 2 orders of magnitude (1 milliarcsec to 7 microarcsec) limiting sensitivity: 4 orders of magnitude (~10 mag to mag) number of stars: 4 orders of magnitude (105 to 109) Measurement principles identical: two viewing directions (absolute parallaxes) sky scanning over 5 years parallaxes and proper motions Instrument improvement: larger primary mirror: 0.3x0.3 m2 1.45x0.50 m2, D-(3/2) improved detector (IDT, CCD): QE, bandpass, multiplexing Control of all associated error sources: aberrations, chromaticity, solar system ephemerides, attitude control p10

11 Astrometric Accuracy Numbers due to Jos de Bruijne p11

12 % Parallax horizon for K5III stars 10 AV = 5 mag 10 kpc AV = LAMOST: R=00 to 17.5 kpc (V=16) 2 p12 5 Figure courtesy of Lennart Lindegren %

13 GAIA: Science Objectives... cont.. Solar System studies Extra Solar Planets masses (down to 10Mearth at 10pc) for nearby sample great for more detailed followup Stellar AstroPhysics distances to 1% for ~2x10^7 stars at 2.5Kpc and to 10% for ~2x10^8 stars to 25kpc calibration of distance indicators (Cepheids/ RRLyrae/ MCs) light deflection, PPN asteroids, kuiper belt objects, trojans orbits, masses and near earth objects Fundamental Physics... and lots more... p13

14 Exo-Planets: Expected Discoveries Astrometric survey: monitoring hundreds of thousands of FGK stars to ~0 pc detection limits: ~1MJ and P < 10 years complete census of all stellar types, P = 29 years masses, rather than lower limits (m sin i) multiple systems measurable, giving relative inclinations Results expected: 10,000 exo-planets (~10 per day) displacement for 47 UMa = 360 μas orbits for ~5000 systems masses down to 10 MEarth to 10 pc Planet: ρ=100 mas, P=18 mths Δδ('') Photometric transits: ~5000? Δαcos δ('') Figure courtesy François Mignard p14

15 Field of Streams: Insights on Assembly p15

16 The Local Group & Gaia Large scale kinematic/ chemical surveys from e.g. Gaia allow for better characterisation of Local Group features e.g. further detail on the dwarf galaxies recently discovered from SDSS star counts e.g. Leo T (Irwin et al, 07, ApJ, 656, L13) identification of disrupted satellites LG orbits [Sawa+Fujimoto 05] Orbits of the dwarf spheroidal galaxies (Dsph) Draco and Sagittarius projected onto the LGG plane. They started from the formation site in similar directions, spiraled along the orbit of the Galaxy and reached their present positions, respectively. p16

17 Chemistry of the Galaxy / LG [Renzini+Fusi Pecci (1988)] For our galaxy insights on the formation of the bulge the thick/ thin disk formation and the halo Gaia allows for a better selection of volume complete samples p17

18 GAIA and complementary missions Gaia is a unique mission but can benefit from: radial velocity programmes for faint stars VISTA / IR surveys (dust models) LSST and Pan Starrs will complement Gaia SDSS and extensions radial velocities for stars with V > 17 Impact of LAMOST for wide field spectroscopic pre or followup observations of Gaia objects Time to define and prepare focused programmes in preparation for the 'age of Gaia' p18

19 Schedule: not so far away now! now Proposal source: ESA Concept & Technology Study Mission Selection Re-Assessment Study Phase B1 Definition Selection of Prime Contractor (EADS Astrium) Phase B2 Phase C/D Implementation Launch 11-Dec-01 Scientific operation Operation Studies Software Development Data Processing Mission Data Processing Intermediate Mission Products p19 Final

20 Gaia by the numbers Primary mirrors: 1.45 m x 0.5 m Focal length: 35 m Pixel: 59 x 177 mas (10 µas ~1/6000 pixel) 1 µas: rotation M1 < 10 picometers at the edge Focal plane: 4 x 850 mm 106 CCDs, ~1 Gpixel Star on CCD: mean: 150, peak: (magnitude ) Stellar flux: 000 V=15, 0 V= Sample datation accuracy: 50 ns Tore (3 m diameter) thermal stability required ~some tens of µk Rate measurement error < 0.9 mas/s Rate pointing error < 5 mas Attitude High Frequency Disturbance < 3.4 µas S/C launch mass 2.1 tons Solar Array capability 1.9 kw Mass memory capability 1 Tb S/C Height 3 m Deployed Sunshield ø = 10 m source: Moisson EADS Astrium p

21 Satellite and System ESA-only mission Launch date: late 11 Lifetime: 5 years (+ possible 1 year) Launcher: SoyuzFregat from CSG Orbit: L2 Ground station: New Norcia and/or Cebreros Downlink rate: 48 Mbps Mass: 30 kg (payload 690 kg) Power: 17 W (payload 830 W) Figures courtesy EADS-Astrium p21

22 p22

23 Payload and Telescope Two SiC primary mirrors 1.45 ξ 0.50 m2 at Basic angle monitoring system Rotation axis (6 h) SiC toroidal structure (optical bench) Superposition of two Fields of View (FoV) Figure courtesy EADS-Astrium p23 Combined focal plane (CCDs)

24 Figure courtesy Alex Short Focal Plane cm 42.35cm Wave Front Sensor Red Photometer CCDs Blue Photometer CCDs Wave Front Sensor Radial-Velocity Spectrometer CCDs Basic Angle Monitor Basic Angle Monitor Star motion in 10 s Sky Mapper CCDs Astrometric Field CCDs Total field: - active area: 0.75 deg2 - CCDs: x 1966 pixels (TDI) - pixel size = 10 µm x 30 µm = 59 mas x 177 mas Photometry: Sky mapper: - detects all objects to mag - rejects cosmic-ray events - FoV discrimination Astrometry: - total detection noise: 6 e- p24 - two-channel photometer - blue and red CCDs Spectroscopy: - high-resolution spectra - red CCDs

25 Downlink Using Cebreros (35M) 3-8Mb/s downlink ~ 30GB/day -> ~100TB so download 'windows' around objects occasionally New Norcia depends on encoding which depends on weather! during Galactic plane scans data accumulated onboard downlinked later Data is compressed encoded and requires a lot of processing (~10^21 FLOP) p25

26 On-Board Object Detection Requirements: unbiased sky sampling (mag, colour, resolution) no all-sky catalogue at Gaia resolution (0.1 arcsec) to V~ Solution: on-board detection: no input catalogue or observing programme good detection efficiency to V~21 mag low false-detection rate, even at high star densities Will therefore detect: variable stars (eclipsing binaries, Cepheids, etc.) supernovae:,000 microlensing events: ~1000 photometric; ~100 astrometric Solar System objects, including NEOs and KBOs p26

27 Sky Scanning Principle 45o Spin axis Scan rate: Spin period: Figure courtesy Karen O Flaherty p27 45o to Sun 60 arcsec/s 6 hours

28 p28

29 p29

30 Photometry Measurement Concept (1/2) Blue photometer: nm Red photometer: nm Figures courtesy EADS-Astrium p30

31 Photometry Measurement Concept (2/2) Blue photometer wavelength (nm) wavelength (nm) spectral dispersion per pixel (nm) Red photometer AL pixels spectral dispe AL pixels RP spectrum of M dwarf (V=17.3) Red box: data sent to ground White contour: sky-background level Colour coding: signal intensity Figures courtesy Anthony Brown p31

32 Radial Velocity Measurement Concept Spectroscopy: nm (resolution 11,500) Figures courtesy EADS-Astrium p32

33 Radial Velocity Measurement Concept Field of view RVS spectrograph CCD detectors RVS spectra of F3 giant (V=16) S/N = 7 (single measurement) S/N = 130 (summed over mission) Figures courtesy David Katz p33

34 Data Reduction Principles Scan width: 0.7 Figure courtesy Michael Perryman Sky scans (highest accuracy along scan) 1. Object matching in successive scans 2. Attitude and calibrations are updated 3. Objects positions etc. are solved 4. Higher terms are solved 5. More scans are added 6. System is iterated p34

35 slide: wil o'mullane Astrometric GIS What? Calculate parameters describing observed (proper) directions to a subset of "well-behaved" (primary) sources attitude of the instrument as function of time transformation from field angles to pixel coordinates This will directly give: astrometric parameters for the primary sources attitude parameters (for the relevant time intervals) geometric calibration parameters (for the relevant detectors) if desired, any other parameter entering the calculation of proper directions (e.g. paramaterised post newtonian (PPN) ) and indirectly: approximate astrometric parameters for all other (secondary) sources (except solar system sources) p35

36 Large Computers... at least for AGIS As a courtesy of Barcelona Supercomputing Center p36

37 Gaia Scientific Organisation Gaia Science Team (GST): 7 members + DPAC Executive Chair + ESA Project Scientist Direct scientific community participation: organised in Data Processing and Analysis Consortium (DPAC) ~350 scientists active at some level Community is active and productive: regular science team/dpac meetings growing archive of scientific reports advance of simulations, algorithms, accuracy models, etc. Data distribution policy: Intermediate data releases final catalogue ~19 no proprietary data rights p37

38 Gaia Data Processing and Analysis Consortium: To prepare, test, implement and execute all the software required to process all the science and auxiliary data produced by the Gaia satellite, to such level that the reduced data is ready for further astrophysical exploration p38

39 DPAC coordination units CU1: System Architecture CU2: Data Simulations CU3: Core Processing CU4: Object Processing CU5: Photometric Processing CU6: Spectroscopic Processing CU7: Variability Processing CU8: Astrophysical Parameters CU9: Catalogue Access p39 ESA areas of Contribution

40 The Participating Institutes Graphic : Francois Mignard - DPAC p40

41 DPAC: Data Processing Centres DPCs underpin and support CUs Software support and production Operation of processing system(s) ESAC BPC CNES ISDC IoA OATO (CU1,3) (CU2,3) (CU4,6,8) (CU7) (CU5) (CU3) Madrid Barcelona Toulouse Geneva Cambridge Torino p41

42 GAIA DPAC in the UK Gaia Data Flow System project UK DPAC Multi institute consortium IoA, Cambridge MSSL Leicester Edinburgh RAL OU Provides leadership of CU5 (photometry) and major partner on CU6 (spectroscopy) DPC at IoA during operation/ exploitation phase p42

43 Gaia: Timescales & Data Final astrometry dependent on global iterative solution of entire mission data Intermediate data releases final catalogues to be released ~ one or more during the course of the mission Science alerts Synergies with new and existing instruments e.g. Star-formation: Herschel/ ALMA most GAIA sources can be followed up with existing 24-8m class ground based telescopes p43

44 Gaia and the Virtual Observatory ESA/ DPAC create the required software infrastructure to process and generate intermediate and final data products Scientific & Cost effective delivery of these projects will be facilitated by use of the Euro-VO/AstroGrid Virtual Observatory infrastructure reduces cost of development: no bespoke interfaces p44

45 Hipparcos via AstroGrid in 4 clicks p45

46 GREAT: Gaia Research for European Astronomy Training ESA Project/ Science Team/ DPACE sponsored initiative to build community awareness of science opportunities from Gaia Funding proposal to ESF Research Network Prog Involved 70+ groups from ~ countries representing ~600 European researchers To fund 'science of Gaia' activities over Workshops, training events, exchanges, conferences, information First co-i meeting ~Easter 09 Options for Chinese involvement p46

47 p47

The Gaia Archive. Center Forum, Heidelberg, June 10-11, 2013. Stefan Jordan. The Gaia Archive, COSADIE Astronomical Data

The Gaia Archive. Center Forum, Heidelberg, June 10-11, 2013. Stefan Jordan. The Gaia Archive, COSADIE Astronomical Data The Gaia Archive Astronomisches Rechen-Institut am Zentrum für Astronomie der Universität Heidelberg http://www.stefan-jordan.de 1 2 Gaia 2013-2018 and beyond Progress with Gaia 3 HIPPARCOS Gaia accuracy

More information

DU640 Radial Velocity Zero-Point Software Requirement Specifications

DU640 Radial Velocity Zero-Point Software Requirement Specifications DU640 Radial Velocity Zero-Point Software Requirement Specifications prepared by: approved by: reference: issue: 4 revision: 1 date: 28-03-2008 status: Issued G. Jasniewicz, F. Crifo, D. Hestroffer, A.

More information

Science@ESA vodcast series. Script for Episode 6 Charting the Galaxy - from Hipparcos to Gaia

Science@ESA vodcast series. Script for Episode 6 Charting the Galaxy - from Hipparcos to Gaia Science@ESA vodcast series Script for Episode 6 Charting the Galaxy - from Hipparcos to Gaia Available to download from http://sci.esa.int/gaia/vodcast Hello, I m Rebecca Barnes and welcome to the Science@ESA

More information

Lecture 6: distribution of stars in. elliptical galaxies

Lecture 6: distribution of stars in. elliptical galaxies Lecture 6: distribution of stars in topics: elliptical galaxies examples of elliptical galaxies different classes of ellipticals equation for distribution of light actual distributions and more complex

More information

Gaia: Solar System observations

Gaia: Solar System observations Gaia: Solar System observations Paolo Tanga Observatoire de la Côte d Azur (France) Gaia will also observe Asteroids (~250.000 most known) Comets Mainly Main Belt Asteroids (MBA) Several NEOs Other populations

More information

Towards the Detection and Characterization of Smaller Transiting Planets

Towards the Detection and Characterization of Smaller Transiting Planets Towards the Detection and Characterization of Smaller Transiting Planets David W. Latham 27 July 2007 Kepler MISSION CONCEPT Kepler Mission is optimized for finding habitable planets ( 10 to 0.5 M )

More information

Explorations of the Outer Solar System. B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics

Explorations of the Outer Solar System. B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics Explorations of the Outer Solar System B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics The Known Solar System How big is the solar system? a tidal R 0 M Sun M Galaxy 1/3 200,000AU How big is

More information

165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars

165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching

More information

Class 2 Solar System Characteristics Formation Exosolar Planets

Class 2 Solar System Characteristics Formation Exosolar Planets Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System

More information

Chemical tagging with. Ricardo Schiavon

Chemical tagging with. Ricardo Schiavon Chemical tagging with Ricardo Schiavon Stellar Populations Newton Meeting São Paulo, November 30, 2015 Chemical tagging with Discovery of a new stellar population in the Galactic bulge Astrophysics Research

More information

Observing the Universe

Observing the Universe Observing the Universe Stars & Galaxies Telescopes Any questions for next Monday? Light Doppler effect Doppler shift Doppler shift Spectra Doppler effect Spectra Stars Star and planet formation Sun Low-mass

More information

MODULE P7: FURTHER PHYSICS OBSERVING THE UNIVERSE OVERVIEW

MODULE P7: FURTHER PHYSICS OBSERVING THE UNIVERSE OVERVIEW OVERVIEW More than ever before, Physics in the Twenty First Century has become an example of international cooperation, particularly in the areas of astronomy and cosmology. Astronomers work in a number

More information

TRANSITING EXOPLANETS

TRANSITING EXOPLANETS TRANSITING EXOPLANETS Introduction 11 Chapter 1 Our Solar System from afar 13 Introduction 13 1.1 Direct imaging 20 1.1.1 Coronagraphy 24 1.1.2 Angular difference imaging 25 1.2 Astrometry 26 1.3 Radial

More information

The Milky Way Galaxy is Heading for a Major Cosmic Collision

The Milky Way Galaxy is Heading for a Major Cosmic Collision The Milky Way Galaxy is Heading for a Major Cosmic Collision Roeland van der Marel (STScI) [based on work with a team of collaborators reported in the Astrophysical Journal July 2012] Hubble Science Briefing

More information

CAUP s Astronomical Instrumentation and Surveys

CAUP s Astronomical Instrumentation and Surveys CAUP s Astronomical Instrumentation and Surveys CENTRO DE ASTROFÍSICA DA UNIVERSIDADE DO PORTO www.astro.up.pt Sérgio A. G. Sousa Team presentation sousasag@astro.up.pt CAUP's Astronomical Instrumentation

More information

and the VO-Science Francisco Jiménez Esteban Suffolk University

and the VO-Science Francisco Jiménez Esteban Suffolk University The Spanish-VO and the VO-Science Francisco Jiménez Esteban CAB / SVO (INTA-CSIC) Suffolk University The Spanish-VO (SVO) IVOA was created in June 2002 with the mission to facilitate the international

More information

Giant Molecular Clouds

Giant Molecular Clouds Giant Molecular Clouds http://www.astro.ncu.edu.tw/irlab/projects/project.htm Galactic Open Clusters Galactic Structure GMCs The Solar System and its Place in the Galaxy In Encyclopedia of the Solar System

More information

Virtual Observatory tools for the detection of T dwarfs. Enrique Solano, LAEFF / SVO Eduardo Martín, J.A. Caballero, IAC

Virtual Observatory tools for the detection of T dwarfs. Enrique Solano, LAEFF / SVO Eduardo Martín, J.A. Caballero, IAC Virtual Observatory tools for the detection of T dwarfs Enrique Solano, LAEFF / SVO Eduardo Martín, J.A. Caballero, IAC T dwarfs Low-mass (60-13 MJup), low-temperature (< 1300-1500 K), low-luminosity brown

More information

Software challenges in the implementation of large surveys: the case of J-PAS

Software challenges in the implementation of large surveys: the case of J-PAS Software challenges in the implementation of large surveys: the case of J-PAS 1/21 Paulo Penteado - IAG/USP pp.penteado@gmail.com http://www.ppenteado.net/ast/pp_lsst_201204.pdf (K. Taylor) (A. Fernández-Soto)

More information

In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.

In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The

More information

12-3. Spherical groups of millions of stars found in the Milky Way are called: a) novas b) globular clusters X c) open clusters d) galactic clusters

12-3. Spherical groups of millions of stars found in the Milky Way are called: a) novas b) globular clusters X c) open clusters d) galactic clusters Chapter 12 Quiz, Nov. 28, 2012, Astro 162, Section 4 12-1. Where in our Galaxy has a supermassive (or galactic) black hole been observed? a) at the outer edge of the nuclear bulge b) in the nucleus X c)

More information

Planet Detection Techniques and Results (outline of lectures)

Planet Detection Techniques and Results (outline of lectures) Planet Detection Techniques and Results (outline of lectures) These notes are meant to be read in conjunction with the lecture presentation. A pdf of the powerpoint presentation containing all the illustrations

More information

Debris disks at high resolution. Mark Wyatt Rachel Smith Institute of Astronomy, Cambridge

Debris disks at high resolution. Mark Wyatt Rachel Smith Institute of Astronomy, Cambridge Debris disks at high resolution Mark Wyatt Rachel Smith Institute of Astronomy, Cambridge Debris disk overview Debris disks are remnants of planet formation, planetesimals which failed to grow into planets;

More information

(Long-Baseline) Interferometric Measurements of Binary Stars

(Long-Baseline) Interferometric Measurements of Binary Stars (Long-Baseline) Interferometric Measurements of Binary Stars A. Boden MSC/Caltech & GSU C. Hummel USNO/ESO G. Torres & D. Latham CfA H. McAlister CHARA/GSU Outline Introduction: Why study binary stars

More information

Are We Alone?! Exoplanet Characterization and Direct Imaging!

Are We Alone?! Exoplanet Characterization and Direct Imaging! From Cosmic Birth to Living Earths A Vision for Space Astronomy in the 2020s and Beyond Are We Alone?! Exoplanet Characterization and Direct Imaging! A Study Commissioned by the Associated Universities

More information

NASA s Future Missions in X-ray Astronomy

NASA s Future Missions in X-ray Astronomy NASA s Future Missions in X-ray Astronomy Nicholas E. White NASA s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, MD 20771 USA nwhite@lheapop.gsfc.nasa.gov Abstract The

More information

Big Data, Cloud & Virtualization

Big Data, Cloud & Virtualization Big Data, Cloud & Virtualization Tokyo, 2014 Vik Nagjee Product Manager, Database Platforms Big Data 1 What s Big about {Big} Data? The 3 V s Volume Variety Velocity The {Big} Data Challenge Image credit:

More information

arxiv:0806.2575v2 [astro-ph] 8 Sep 2013

arxiv:0806.2575v2 [astro-ph] 8 Sep 2013 The Galaxy disk in a cosmological context Proceedings IAU Symposium No. 254, 2009 c 2009 International Astronomical Union DOI: 00.0000/X000000000000000X What will Gaia tell us about the Galactic disk?

More information

This paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00

This paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00 Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June

More information

Cosmic Variability Study in Taiwan

Cosmic Variability Study in Taiwan Cosmic Variability Study in Taiwan Wen-Ping Chen Institute of Astronomy National Central University, Taiwan 2010 November 16@Jena/YETI Advantages in Taiwan: - Many high mountains - Western Pacific longitude

More information

Other Planetary Systems

Other Planetary Systems Other Planetary Systems Other Planetary Systems Learning goals How do we detect planets around other stars? What have other planetary systems taught us about our own? Extrasolar planet search

More information

The Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun

The Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun The Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun P.C. Frisch and A.J. Hanson Department of Astronomy and Astrophysics University of Chicago and Computer Science

More information

Adaptive Optics (AO) TMT Partner Institutions Collaborating Institution Acknowledgements

Adaptive Optics (AO) TMT Partner Institutions Collaborating Institution Acknowledgements THIRTY METER TELESCOPE The past century of astronomy research has yielded remarkable insights into the nature and origin of the Universe. This scientific advancement has been fueled by progressively larger

More information

Indiana University Science with the WIYN One Degree Imager

Indiana University Science with the WIYN One Degree Imager Indiana University Science with the WIYN One Degree Imager Katherine Rhode (Indiana University, WIYN SAC member) Indiana University Department of Astronomy Nine faculty members, plus active emeritus faculty

More information

Evolution of Close Binary Systems

Evolution of Close Binary Systems Evolution of Close Binary Systems Before going on to the evolution of massive stars and supernovae II, we ll think about the evolution of close binary systems. There are many multiple star systems in the

More information

SIERRA COLLEGE OBSERVATIONAL ASTRONOMY LABORATORY EXERCISE NUMBER III.F.a. TITLE: ASTEROID ASTROMETRY: BLINK IDENTIFICATION

SIERRA COLLEGE OBSERVATIONAL ASTRONOMY LABORATORY EXERCISE NUMBER III.F.a. TITLE: ASTEROID ASTROMETRY: BLINK IDENTIFICATION SIERRA COLLEGE OBSERVATIONAL ASTRONOMY LABORATORY EXERCISE NUMBER III.F.a. TITLE: ASTEROID ASTROMETRY: BLINK IDENTIFICATION DATE- PRINT NAME/S AND INITIAL BELOW: GROUP DAY- LOCATION OBJECTIVE: Use CCD

More information

Class #14/15 14/16 October 2008

Class #14/15 14/16 October 2008 Class #14/15 14/16 October 2008 Thursday, Oct 23 in class You ll be given equations and constants Bring a calculator, paper Closed book/notes Topics Stellar evolution/hr-diagram/manipulate the IMF ISM

More information

Many areas of science will be addressed by the Gaia mission as indicated in this schematic figure.

Many areas of science will be addressed by the Gaia mission as indicated in this schematic figure. Overall Science Goals Many areas of science will be addressed by the Gaia mission as indicated in this schematic figure. Gaia will measure the positions, distances, space motions, and many physical characteristics

More information

Detecting and measuring faint point sources with a CCD

Detecting and measuring faint point sources with a CCD Detecting and measuring faint point sources with a CCD Herbert Raab a,b a Astronomical ociety of Linz, ternwarteweg 5, A-400 Linz, Austria b Herbert Raab, chönbergstr. 3/1, A-400 Linz, Austria; herbert.raab@utanet.at

More information

Astronomy of extrasolar planetary systems. Methods and results of searches for planets around other stars

Astronomy of extrasolar planetary systems. Methods and results of searches for planets around other stars Astronomy of extrasolar planetary systems Methods and results of searches for planets around other stars Course layout - methods Introduction and history of searches for planets Doppler spectroscopy and

More information

SCIENCE 101 DISTANCES IN ASTRONOMY LECTURE NOTES

SCIENCE 101 DISTANCES IN ASTRONOMY LECTURE NOTES SCIENCE 0 DISTANCES IN ASTRONOMY LECTURE NOTES Distances in the Solar System Distance to Venus can be obtained using radar ranging Send signal, determine how long it takes to return Radio waves move at

More information

A Preliminary Summary of The VLA Sky Survey

A Preliminary Summary of The VLA Sky Survey A Preliminary Summary of The VLA Sky Survey Eric J. Murphy and Stefi Baum (On behalf of the entire Science Survey Group) 1 Executive Summary After months of critical deliberation, the Survey Science Group

More information

Science Standard 4 Earth in Space Grade Level Expectations

Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal

More information

8.1 Radio Emission from Solar System objects

8.1 Radio Emission from Solar System objects 8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio

More information

The challenges of the Gaia mission

The challenges of the Gaia mission gaia ESA s billion-pixel camera The challenges of the Gaia mission Philippe Gare, Giuseppe Sarri & Rudolf Schmidt Directorate of Science and Robotic Exploration, ESTEC, Noordwijk, The Netherlands Gaia

More information

First Discoveries. Asteroids

First Discoveries. Asteroids First Discoveries The Sloan Digital Sky Survey began operating on June 8, 1998. Since that time, SDSS scientists have been hard at work analyzing data and drawing conclusions. This page describes seven

More information

Ellipticals. Elliptical galaxies: Elliptical galaxies: Some ellipticals are not so simple M89 E0

Ellipticals. Elliptical galaxies: Elliptical galaxies: Some ellipticals are not so simple M89 E0 Elliptical galaxies: Ellipticals Old view (ellipticals are boring, simple systems)! Ellipticals contain no gas & dust! Ellipticals are composed of old stars! Ellipticals formed in a monolithic collapse,

More information

Top 10 Discoveries by ESO Telescopes

Top 10 Discoveries by ESO Telescopes Top 10 Discoveries by ESO Telescopes European Southern Observatory reaching new heights in astronomy Exploring the Universe from the Atacama Desert, in Chile since 1964 ESO is the most productive astronomical

More information

15.6 Planets Beyond the Solar System

15.6 Planets Beyond the Solar System 15.6 Planets Beyond the Solar System Planets orbiting other stars are called extrasolar planets. Until 1995, whether or not extrasolar planets existed was unknown. Since then more than 300 have been discovered.

More information

Einstein Rings: Nature s Gravitational Lenses

Einstein Rings: Nature s Gravitational Lenses National Aeronautics and Space Administration Einstein Rings: Nature s Gravitational Lenses Leonidas Moustakas and Adam Bolton Taken from: Hubble 2006 Science Year in Review The full contents of this book

More information

Origins of the Cosmos Summer 2016. Pre-course assessment

Origins of the Cosmos Summer 2016. Pre-course assessment Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of

More information

Rough subdivision. Characteristic values for E s (Schneider 2006). Elliptical galaxies. Elliptical galaxies

Rough subdivision. Characteristic values for E s (Schneider 2006). Elliptical galaxies. Elliptical galaxies Rough subdivision Normal ellipticals. Giant ellipticals (ge s), intermediate luminosity (E s), and compact ellipticals (ce s), covering a range of luminosities from M B 23 m to M B 15 m. Dwarf ellipticals

More information

The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor)

The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor) The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor) Didier BARRET on behalf of the SVOM collaboration didier.barret@cesr.fr Outline SVOM background

More information

16 th IOCCG Committee annual meeting. Plymouth, UK 15 17 February 2011. mission: Present status and near future

16 th IOCCG Committee annual meeting. Plymouth, UK 15 17 February 2011. mission: Present status and near future 16 th IOCCG Committee annual meeting Plymouth, UK 15 17 February 2011 The Meteor 3M Mt satellite mission: Present status and near future plans MISSION AIMS Satellites of the series METEOR M M are purposed

More information

The Gaia-ESO Survey. Sofia Randich INAF-Osservatorio di Arcetri

The Gaia-ESO Survey. Sofia Randich INAF-Osservatorio di Arcetri The Gaia-ESO Survey Sofia Randich INAF-Osservatorio di Arcetri Survey Co-PIs: Gerry Gilmore & Sofia Randich 300++ CoIs (mostly from Europe, but not only) 90++ institutes, about 50 CoIs from INAF Gaia-ESO

More information

The Sun and the Solar System

The Sun and the Solar System ASTR 371, Fall 2016 Lecture 1 The Sun and the Solar System Introduction and Overview Homework Due September 7, Wed. FK Chap 1, Questions 3, 16, 24, 38 A1: (a) use data of the diameter and average distance

More information

Modeling Galaxy Formation

Modeling Galaxy Formation Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages

More information

Name: Class: Date: ID: A

Name: Class: Date: ID: A Name: Class: _ Date: _ Practice Quiz 4 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. What is the wavelength of the longest wavelength light that can

More information

The M-dwarfs in Multiples (MinMs) Survey - Stellar Multiplicity within 15 pc

The M-dwarfs in Multiples (MinMs) Survey - Stellar Multiplicity within 15 pc The M-dwarfs in Multiples (MinMs) Survey - Stellar Multiplicity within 15 pc K. Ward-Duong 1, J. Patience 1, R. J. De Rosa 1, J. Bulger 1, A. Rajan 1, D. McCarthy 2, C. Kulesa 2, S. Goodwin 3, R. Parker

More information

Populations and Components of the Milky Way

Populations and Components of the Milky Way Chapter 2 Populations and Components of the Milky Way Our perspective from within the Milky Way gives us an opportunity to study a disk galaxy in detail. At the same time, it s not always easy to relate

More information

Big Data, Big Challenges and new Paradigm for the Gaia Archive

Big Data, Big Challenges and new Paradigm for the Gaia Archive Big Data, Big Challenges and new Paradigm for the Gaia Archive Christophe Arviset Head of ESAC Science Data Centre 15/03/2016 Issue/Revision: 1.0 Reference: Gaia Archive's big data challenges Status: Issued

More information

Astronomy 100 Exam 2

Astronomy 100 Exam 2 1 Prof. Mo Exam Version A Astronomy 100 Exam 2 INSTRUCTIONS: Write your name and ID number on BOTH this sheet and the computer grading form. Use a #2 Pencil on the computer grading form. Be careful to

More information

Faber-Jackson relation: Fundamental Plane: Faber-Jackson Relation

Faber-Jackson relation: Fundamental Plane: Faber-Jackson Relation Faber-Jackson relation: Faber-Jackson Relation In 1976, Faber & Jackson found that: Roughly, L! " 4 More luminous galaxies have deeper potentials Can show that this follows from the Virial Theorem Why

More information

The Formation of Planetary Systems. Astronomy 1-1 Lecture 20-1

The Formation of Planetary Systems. Astronomy 1-1 Lecture 20-1 The Formation of Planetary Systems Astronomy 1-1 Lecture 20-1 Modeling Planet Formation Any model for solar system and planet formation must explain 1. Planets are relatively isolated in space 2. Planetary

More information

The Chemical Composition of a Molecular Cloud at the Outer Edge of the Galaxy

The Chemical Composition of a Molecular Cloud at the Outer Edge of the Galaxy Carnegie Observatories Astrophysics Series, Vol. 4: Origin and Evolution of the Elements, 2003 ed. A. McWilliam and M. Rauch (Pasadena: Carnegie Observatories, http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html)

More information

Monday 24 June 2013 Morning

Monday 24 June 2013 Morning THIS IS A NEW SPECIFICATION H Monday 24 June 2013 Morning GCSE TWENTY FIRST CENTURY SCIENCE PHYSICS A A183/02 Module P7 (Higher Tier) * A 1 3 7 3 1 0 6 1 3 * Candidates answer on the Question Paper. A

More information

Astro 130, Fall 2011, Homework, Chapter 17, Due Sep 29, 2011 Name: Date:

Astro 130, Fall 2011, Homework, Chapter 17, Due Sep 29, 2011 Name: Date: Astro 130, Fall 2011, Homework, Chapter 17, Due Sep 29, 2011 Name: Date: 1. If stellar parallax can be measured to a precision of about 0.01 arcsec using telescopes on Earth to observe stars, to what distance

More information

What is the Sloan Digital Sky Survey?

What is the Sloan Digital Sky Survey? What is the Sloan Digital Sky Survey? Simply put, the Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining

More information

The Moon. Nicola Loaring, SAAO

The Moon. Nicola Loaring, SAAO The Moon Nicola Loaring, SAAO Vital Statistics Mean distance from Earth Orbital Period Rotational Period Diameter 384,400 km 27.322 days 27.322 days 3476 km (0.272 x Earth) Mass 7.3477 10 22 kg (0.0123

More information

Chapter 1: Our Place in the Universe. 2005 Pearson Education Inc., publishing as Addison-Wesley

Chapter 1: Our Place in the Universe. 2005 Pearson Education Inc., publishing as Addison-Wesley Chapter 1: Our Place in the Universe Topics Our modern view of the universe The scale of the universe Cinema graphic tour of the local universe Spaceship earth 1.1 A Modern View of the Universe Our goals

More information

LSST Data Management System Applications Layer Simulated Data Needs Description: Simulation Needs for DC3

LSST Data Management System Applications Layer Simulated Data Needs Description: Simulation Needs for DC3 LSST Data Management System Applications Layer Simulated Data Needs Description: Simulation Needs for DC3 Draft 25 September 2008 A joint document from the LSST Data Management Team and Image Simulation

More information

CBERS Program Update Jacie 2011. Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com

CBERS Program Update Jacie 2011. Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com CBERS Program Update Jacie 2011 Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com Overview CBERS 3 and 4 characteristics Differences from previous CBERS satellites (CBERS 1/2/2B) Geometric

More information

astronomy 2008 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times.

astronomy 2008 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. 5. If the distance between the Earth and the Sun were increased,

More information

New results on HE 0107 5240 and future surveys for metal-poor stars

New results on HE 0107 5240 and future surveys for metal-poor stars New results on HE 0107 5240 and future surveys for metal-poor stars Norbert Christlieb Department of Astronomy and Space Physics, Uppsala University HE 0107 5240 [Fe I/H] NLTE = 5.3 The most heavy-element

More information

The Hidden Lives of Galaxies. Jim Lochner, USRA & NASA/GSFC

The Hidden Lives of Galaxies. Jim Lochner, USRA & NASA/GSFC The Hidden Lives of Galaxies Jim Lochner, USRA & NASA/GSFC What is a Galaxy? Solar System Distance from Earth to Sun = 93,000,000 miles = 8 light-minutes Size of Solar System = 5.5 light-hours What is

More information

Elliptical Galaxies. Houjun Mo. April 19, 2004. Basic properties of elliptical galaxies. Formation of elliptical galaxies

Elliptical Galaxies. Houjun Mo. April 19, 2004. Basic properties of elliptical galaxies. Formation of elliptical galaxies Elliptical Galaxies Houjun Mo April 19, 2004 Basic properties of elliptical galaxies Formation of elliptical galaxies Photometric Properties Isophotes of elliptical galaxies are usually fitted by ellipses:

More information

Development of the Extreme Ultraviolet Spectrometer: EXCEED

Development of the Extreme Ultraviolet Spectrometer: EXCEED Development of the Extreme Ultraviolet Spectrometer: EXCEED Go Murakami*, Kazuo Yoshioka, Atsushi Yamazaki, Tomoki Kimura Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency

More information

United Nations - Nations Unies. COSPAR Symposium. Measuring the Universe. Looking Back in Time with Modern Astronomy. Monday, 2nd February 2015

United Nations - Nations Unies. COSPAR Symposium. Measuring the Universe. Looking Back in Time with Modern Astronomy. Monday, 2nd February 2015 United Nations - Nations Unies COSPAR Symposium Measuring the Universe Looking Back in Time with Modern Astronomy Monday, 2nd February 2015 15:00 18:00 Conference Rooms M1, Building M, Vienna International

More information

Ay 20 - Fall Lecture 17. Stellar Luminosity and Mass Functions * * * * * History and Formation of Our Galaxy

Ay 20 - Fall Lecture 17. Stellar Luminosity and Mass Functions * * * * * History and Formation of Our Galaxy Ay 20 - Fall 2004 - Lecture 17 Stellar Luminosity and Mass Functions * * * * * History and Formation of Our Galaxy Stellar Luminosity and Mass Functions Basic statistical descriptors of stellar populations:

More information

Invisible Galaxies. University of Nebraska, October Beth Willman (Haverford College)

Invisible Galaxies. University of Nebraska, October Beth Willman (Haverford College) Invisible Galaxies University of Nebraska, October 2013 Beth Willman (Haverford College) Invisible Galaxies Finding and studying invisible galaxies The connection with dark matter Contributions of Haverford

More information

Inside the Zodiac A 10-minute planetarium mini-show by Alan Gould 1, Toshi Komatsu 1, Jeff Nee 1, and Dr. Steve Howell 2

Inside the Zodiac A 10-minute planetarium mini-show by Alan Gould 1, Toshi Komatsu 1, Jeff Nee 1, and Dr. Steve Howell 2 Inside the Zodiac A 10-minute planetarium mini-show by Alan Gould 1, Toshi Komatsu 1, Jeff Nee 1, and Dr. Steve Howell 2 About this show In one Word... In one Sentence... In one Paragraph... Storyboard

More information

Chapter 15.3 Galaxy Evolution

Chapter 15.3 Galaxy Evolution Chapter 15.3 Galaxy Evolution Elliptical Galaxies Spiral Galaxies Irregular Galaxies Are there any connections between the three types of galaxies? How do galaxies form? How do galaxies evolve? P.S. You

More information

CU9 Science Enabling Applications Development Work Package Software Requirements Specification (WP970)

CU9 Science Enabling Applications Development Work Package Software Requirements Specification (WP970) Science Enabling Applications Development Work Package Software Requirements Specification (WP970) prepared by: approved by: reference: issue: revision: 1 X. Luri, P.M. Marrese, F.Julbe, H. Enke, N. Walton,

More information

Monday 23 June 2014 Morning

Monday 23 June 2014 Morning H Monday 23 June 2014 Morning GCSE TWENTY FIRST CENTURY SCIENCE PHYSICS A/FURTHER ADDITIONAL SCIENCE A A183/02 Module P7 (Higher Tier) *3173662729* Candidates answer on the Question Paper. A calculator

More information

White Dwarf Properties and the Degenerate Electron Gas

White Dwarf Properties and the Degenerate Electron Gas White Dwarf Properties and the Degenerate Electron Gas Nicholas Rowell April 10, 2008 Contents 1 Introduction 2 1.1 Discovery....................................... 2 1.2 Survey Techniques..................................

More information

Lecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula

Lecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula Origin of the Solar System Lecture 7 Formation of the Solar System Reading: Chapter 9 Quiz#2 Today: Lecture 60 minutes, then quiz 20 minutes. Homework#1 will be returned on Thursday. Our theory must explain

More information

Report on ESA Gaia activities & VLDB 2010

Report on ESA Gaia activities & VLDB 2010 Report on ESA Gaia activities & VLDB 2010 Pilar de Teodoro Gaia Science Operations database administrator European Space Astronomy Centre (ESAC) Madrid Spain The Milky Way Our Sun Gaia s main aim: unravel

More information

Chapter 13 Other Planetary Systems: The New Science of Distant Worlds

Chapter 13 Other Planetary Systems: The New Science of Distant Worlds Chapter 13 Other Planetary Systems: The New Science of Distant Worlds 13.1 Detecting Extrasolar Planets Our goals for learning: Why is it so difficult to detect planets around other stars? How do we detect

More information

1) The final phase of a star s evolution is determined by the star s a. Age b. Gravitational pull c. Density d. Mass

1) The final phase of a star s evolution is determined by the star s a. Age b. Gravitational pull c. Density d. Mass Science Olympiad Astronomy Multiple Choice: Choose the best answer for each question. Each question is worth one point. In the event of a tie, there will be a tie-breaking word problem. 1) The final phase

More information

Lecture Outlines. Chapter 15. Astronomy Today 7th Edition Chaisson/McMillan. 2011 Pearson Education, Inc.

Lecture Outlines. Chapter 15. Astronomy Today 7th Edition Chaisson/McMillan. 2011 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 information

Study Guide: Solar System

Study Guide: Solar System Study Guide: Solar System 1. How many planets are there in the solar system? 2. What is the correct order of all the planets in the solar system? 3. Where can a comet be located in the solar system? 4.

More information

M01/430/H(3) Name PHYSICS HIGHER LEVEL PAPER 3. Number. Wednesday 16 May 2001 (morning) 1 hour 15 minutes INSTRUCTIONS TO CANDIDATES

M01/430/H(3) Name PHYSICS HIGHER LEVEL PAPER 3. Number. Wednesday 16 May 2001 (morning) 1 hour 15 minutes INSTRUCTIONS TO CANDIDATES INTERNATIONAL BACCALAUREATE BACCALAURÉAT INTERNATIONAL BACHILLERATO INTERNACIONAL M01/430/H(3) PHYSICS HIGHER LEVEL PAPER 3 Wednesday 16 May 2001 (morning) Name Number 1 hour 15 minutes INSTRUCTIONS TO

More information

GAIA Unravelling the Origin and Evolution of Our Galaxy

GAIA Unravelling the Origin and Evolution of Our Galaxy r bulletin 103 august 2000 GAIA Unravelling the Origin and Evolution of Our Galaxy M.A.C. Perryman Space Science Department, ESA Directorate of Scientific Programmes, ESTEC, Noordwijk, The Netherlands

More information

DTUsat II An Asteroseismic CubeSat

DTUsat II An Asteroseismic CubeSat DTUsat II An Asteroseismic CubeSat Christoffer Karoff, Morten Stejner Sand Pedersen, and Henrik Robenhagen Jensen Department of Physics and Astronomy, University of Aarhus. Ny Munkegade, Bld. 1520 DK-8000

More information

The Origin of the Solar System and Other Planetary Systems

The Origin of the Solar System and Other Planetary Systems The Origin of the Solar System and Other Planetary Systems Modeling Planet Formation Boundary Conditions Nebular Hypothesis Fixing Problems Role of Catastrophes Planets of Other Stars Modeling Planet Formation

More information

Spectrophotometry of Ap Stars

Spectrophotometry of Ap Stars Spectrophotometry of Ap Stars ASTRA Status Report Barry Smalley Astrophysics Group Keele University Staffordshire United Kingdom bs@astro.keele.ac.uk What is Spectrophotometry? Spectroscopy through a wide

More information

RS platforms. Fabio Dell Acqua - Gruppo di Telerilevamento

RS platforms. Fabio Dell Acqua - Gruppo di Telerilevamento RS platforms Platform vs. instrument Sensor Platform Instrument The remote sensor can be ideally represented as an instrument carried by a platform Platforms Remote Sensing: Ground-based air-borne space-borne

More information

Carol and Charles see their pencils fall exactly straight down.

Carol and Charles see their pencils fall exactly straight down. Section 24-1 1. Carol is in a railroad car on a train moving west along a straight stretch of track at a constant speed of 120 km/h, and Charles is in a railroad car on a train at rest on a siding along

More information

PRESENTATION SPACE MISSIONS

PRESENTATION SPACE MISSIONS GENERAL PRESENTATION SPACE MISSIONS CONTENTS 1. Who we are 2. What we do 3. Space main areas 4. Space missions Page 2 WHO WE ARE GENERAL Multinational conglomerate founded in 1984 Private capital Offices

More information

Section 2.2. Contents of the Tycho Catalogue

Section 2.2. Contents of the Tycho Catalogue Section 2.2 Contents of the Tycho Catalogue 141 2.2. Contents of the Tycho Catalogue Overview of the Tycho Catalogue: The Tycho Catalogue provides astrometry (positions, parallaxes and proper motions)

More information