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Phys 1830: Lecture 34

Phys 1830: Lecture 34. More astro courses! Want to become an astronomer?. Image-making workshop tonight at 5:30pm Allen 536. Previous Classes: galaxies This Class galaxies interacting galaxies cosmology Upcoming class quiz cosmology. Also Check out the other courses:.

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Phys 1830: Lecture 34

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  1. Phys 1830: Lecture 34 More astro courses! Want to become an astronomer? Image-making workshop tonight at 5:30pm Allen 536 • Previous Classes: • galaxies • This Class • galaxies • interacting galaxies • cosmology • Upcoming class • quiz • cosmology

  2. Also Check out the other courses: • Physics 1810 – A survey course • Physics 1820 – More mathematical • In the upper years there are courses on stars, on galaxies, and a thesis project.

  3. Becoming an astronomer • Consider science, for example. An astronomer can make $102,250 but a biological scientist has an average salary of $69,430. The difference could be due in part to supply and demand. • http://superscholar.org/highest-paying-jobs/

  4. Engineering vs Astrophysics http://www.livingin-canada.com/salaries-for-electrical-electronics-engineers-canada.html Engineer starting salary in Winnipeg $38,000 – $7,100 taxes = $30,900 – there are other deductibles too! Graduate students - NO TAX DEDUCTED: MSc with scholarships $28,000 PhD with scholarships $28,000 to $53,000 And travel to conferences and research is paid. • http://www.salaryexplorer.com/ • Physicist: $6,667 per month • Engineer: $5,542 per month (Mechanical )

  5. Career Course: • Examples of fields of study: • computational astrophysics • astrobiology Internship Specialization • Bachelor of Science • Masters of Science if in Canada • typically a 2 yr project • at UM can transfer after 1 year to PhD • PhD • up to 5 yr but can do it in less time • Post-doctoral Fellowship Astronomer • typically two contracts of 2 or 3 years each • Professional Research Astronomer • for a government institute (help run an observatory) • in academia (professor)

  6. Prospects: Square Kilometre Array in South Africa and Australia is currently being commissioned – aim for full operations in 2020. James Webb Space Telescope launch expected 2018.

  7. Galaxies: Hubble Tuning Fork Diagram • Main types are • Elliptical (E) • Spiral (S or SB, if they have a bar.) • Irregular (Irr)

  8. Galaxies: Elliptical • 20% of observed galaxies (not including faint, distant dwarf ellipticals). • Population II and old Population I stars (i.e. old stars). • Mass: 10**5 to 10**13 solar masses • Luminosity: 3 * 10**5 to 10**11 solar L • Stars in orbit but orbits are at random orientations.

  9. Galaxies: Elliptical • Leo I: A low surface brightness dwarf galaxy with a spheroidal shape.

  10. Galaxies: Spirals • 77% of observed galaxies • Note the dust lanes and the pink HII regions. • Arms are bluish  young Pop I stars. • Nucleus and throughout disk are yellowish like an elliptical  Pop II and old Pop I stars.

  11. Galaxies: Spirals • Mass: 10**9 to 4* 10**11 solar masses. • Luminosity: 10**8 to 2 x 10**10 • Most of the stars, gas and dust orbit in a plane. • Stars in the bulge and halo orbit in random orientations, like stars do in an elliptical.

  12. Try this at home: • How long for our sun to orbit the centre of the Milky Way? The distance from the Galactic centre is 8.5 kpc and the sun orbits at 220 km/s. There are 3.09 * 10**13 km per kpc. • on order of thousands of years • on order of millions of years • on order of billions of years • It doesn’t orbit in circle so one can’t calculate this.

  13. In an E galaxy all the stars orbit in the same direction around the centre of the galaxy. This causes the ones that are spinning faster to have a flattened appearance. • True • False

  14. Galaxies: Hubble Tuning Fork Diagram • The appearance of gaps of empty space between arms is a misrepresentation. • The apparent gaps are actually dust lanes.

  15. Spirals: No gaps in disk of galaxy. HST • I-band image. • Dusting of stars throughout the disk. • Pop II and older Pop I stars. (Recall low mass stars live longer and are red on the MS.)

  16. Spirals: No gaps in disk of galaxy. HST • B-band image. • Dust absorbs UV and B radiation, obscuring stars. • Recall on MS massive stars are blue.

  17. Spirals: No gaps in disk of galaxy. HST • F435W(B), F555W(V), F814W(I) • Note that it is missing H_alpha filter so we don’t see pink HII regions.

  18. Spiral Disk Galaxies: Canada-France-Hawaii Telescope: Jean-Charles Cuillandre • Disk galaxies can have a spiral arm pattern of dust and hot young stars superimposed on the disk. • The disk rotates. Stars and gas orbit around the centre.

  19. Galaxies: Spirals – examples and inclination. • Flocculent (like a sheep)

  20. Galaxies: Spirals – examples and inclination. • Almost face-on inclination. • Grand Design Spirals have well-defined arms

  21. Galaxies: Spirals – examples and inclination. • Barred galaxy.

  22. Galaxies: Spirals – examples and inclination. • Edge-on. • Note the dust lane in midplane of galaxy and dust filaments rising into the halo.

  23. Galaxies: Spirals – examples and inclination. • Edge-on. • Large bulge (spherical component). • Note the nucleus in the centre of the bulge.

  24. Galaxies: Irregular • Appearance of irregular shape is often due to the distribution of regions of star formation. • Mostly Population I stars.

  25. Review Which of these does not have young population I stars? A) elliptical galaxies B) non-barred spirals C) Irregular galaxies D) barred spirals

  26. Galaxies: HI distribution compared to stellar distribution • Optical image of M 33.

  27. Galaxies: HI distribution compared to stellar distribution • Radio 21 cm image of M 33. • Notice the gas is more extended in distribution than the stars.

  28. Galaxies: Evolution with time Atoms for Peace galaxy (NGC 7252) Hibbard & van Gorkom (1996) HCG 31 HST English, Charlton et al. • Interacting spiral galaxies – lectures on tidal effects. • Eventually they merge together to form elliptical galaxies. • Material around merger remnant (on right) would fall towards the central region forming elliptical orbits.

  29. Galaxies: Evolution with Time. • Spiral metamorphosis at Gravitas website. • http://www.galaxydynamics.org/spiral_metamorphosis.html • Watch for tidal tails left behind & bridges between interacting galaxies.

  30. Interactions and Mergers John Dubinski (U. of Toronto) • Note tails and bridges • Outstanding Questions: • If E form from mergers, why do E and S/SBs both co-exist at early times in the universe? • How do disk galaxies get spiral arms?

  31. Galaxies: You can participate in research • Galaxy Zoo http://www.galaxyzoo.org/ • “In order to understand how these galaxies — and our own — formed, we need your help to classify them according to their shapes — a task at which your brain is better than even the fastest computer.” • “Based on the basic input parameters that we provide, a Java applet running in your browser will simulate some possible collision scenarios. Computers don’t do a good job comparing simulations and real astronomical images, so we need your help to find out which simulations are the most similar to the real galaxy collision.”

  32. It is likely that • E galaxies fragment to become SB galaxies. • Irr galaxies are the last stage of merging galaxies. • Galaxies formed out of gas clouds at the beginning of time and remained the same since. They will never change shape. • S and SB galaxies interact, merging together to form E galaxies.

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