1 / 34

3671: Multi-wavelength Astronomy

3671: Multi-wavelength Astronomy. Dr. Matthew Burleigh. www.star.le.ac.uk/~mbu. The Electro-magnetic Spectrum. 100MeV 100keV 0.1keV 1000A 5000A 1micron 1cm 100m. Gamma Ray Xray EUV UV Optical IR Micro-wave Radio.

cappsd
Download Presentation

3671: Multi-wavelength Astronomy

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 3671: Multi-wavelength Astronomy Dr. Matthew Burleigh www.star.le.ac.uk/~mbu

  2. The Electro-magnetic Spectrum 100MeV 100keV 0.1keV 1000A 5000A 1micron 1cm 100m Gamma Ray Xray EUV UV Optical IR Micro-wave Radio http://imagine.gsfc.nasa.gov/docs/science/know_l1/emspectrum.html

  3. Multi-wavelength Astronomy

  4. Wavelength scales • Rather annoyingly, astronomers use a variety of wavelength scales depending on the waveband involved (see diagram on last slide) • Radio astronomers use m and cm • Infra-red astronomers use microns • Optical and UV astronomers use Angstroms or nano-meters • X-ray and gamma ray observers switch to an energy scale, i.e. in electron-Volts

  5. Conversion factors • E = hn = hc/l in Joules • 1eV = 1.6x10-19J • Wavelength l in Angstroms -> Energy in keV • keV = 12.4/l • 1Angstrom = 10-10m • 1 nm = 10-9m • 1mm (micron) = 10-6m = 10,000A • Point at which optical becomes infra-red!

  6. What is multi-wavelength astronomy? • Astronomers used to think of themselves as either ‘optical’, ‘radio’, ‘IR’ or ‘Xray’ • But modern astrophysics requires studying an object across the whole EM spectrum • Different physical processes can be studied at different wavelengths • Xray, gamma ray and radio astronomers need to identify their sources with optical counterparts http://imagine.gsfc.nasa.gov/docs/science/know_l1/multiwavelength.html

  7. The Milky Way: Optical Stars, Dust lanes

  8. The Milky Way: IR See through dust

  9. The Milky Way: Xray Hot gas

  10. Andromeda (M31): Optical

  11. Andromeda (M31): IR Star forming regions in spiral arms

  12. Andromeda (M31): UV Young, hot stars in spiral arms

  13. Andromeda (M31): Xray Xray binaries, supernova remnants, hot gas

  14. Orion in the optical and xrays Optical Xrays

  15. Multi-wavelength study of Xray sources

  16. Binary stars: Sirius A & B Chandra: Xrays Optical photograph

  17. Binary white dwarfs revealed in the ultra-violet HST Optical UV: white dwarf companion (star Ab)

  18. Brown dwarfs & extra-solar planets in the infra-red HST IR image Gl 229: Red dwarf + brown dwarf companion

  19. Brown dwarfs & extra-solar planets in the infra-red J band (IR) image from Gemini North of a nearby white dwarf Estimate a 10Mjup planet would have a magnitude of J~20.5

  20. Effect of atmosphere

  21. Effect of atmosphere

  22. Types of observation • Photometry – the brightness of an object in a certain waveband • Time-resolved photometry -

  23. Types of observation • Spectroscopy - http://imagine.gsfc.nasa.gov/docs/science/how_l1/analysis.html

  24. Course Outline • Overview: Today • The electro-magnetic spectrum • What is multi-wavelength astronomy? • Observing at different wavelengths

  25. Course Outline • Basic physical processes: Tomorrow • Attenuation of radiation by matter • (important to IR, UV and X-ray) • BB radiation • (how to decide which waveband to observe in) • Emission processes

  26. Optical astronomy • Telescopes • Modern telescope design • Diffraction limit, resolution • Seeing • Adaptive optics • Detectors • CCDs

  27. Optical astronomy • Techniques • Spectroscopy: grating equation, resolution • Imaging: magnitude system, filters, colour

  28. Infra-red Astronomy • Infra-red • Absorption by and emission from dust • Interstellar reddening • Detectors, telescopes and satellite missions

  29. Ultraviolet Astronomy • Ultraviolet • Satellite Missions • Interstellar absorption • Curve of growth

  30. Radio Astronomy • Radio astronomy • Differences between optical and radio • The radio telescope • Interferometers • Examples: Pulsars, radio galaxies, neutral H

  31. The High-Energy Universe • X-ray astronomy • History • X-ray detectors • Absorption processes • X-ray emitting objects • Accretion onto compact objects • Black holes and the Eddington luminosity

  32. Complimentary courses • 4326 Interaction radiation/matter – Wynn • 3611.2 Galaxies – O’Brien • 3611.1 Active Galaxies – Stewart • 3631.2 Interstellar Medium - Jameson • 3631.1 Binary stars – Wynn • 3677 Life in the Universe – Raine/Sims/Burleigh • 4424 High Energy Astrophysics – Ward/Watson

  33. Thursdays 10.30am LRB Fridays 1.30pm LRB Lecture timetable 3rd Yr Support course TBD

  34. Books • Modern Astrophysics – Carroll & Ostlie • High Energy Astrophysics – Longair (Cambridge University Press) ISBN 0-521-38873-6 • Active Galactic Nuclei – Robson (Wiley)ISBN 0-471-96050-0 • Active Galactic Nuclei – Peterson (Cambridge University Press) ISBN 0-521-47911-8 • Observational Astronomy - Kitchin

More Related