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Galaxy Mass

Galaxy Mass. Star Number/Density Counting stars in a given volume Use volume of galaxy to estimate mass Good idea?. Rotation Curve Best for spirals (s for ellipticals) Based on Kepler ’ s Third Law Mass(R) = R v 2 /G Mass(R) = mass within radius R For Sun V=220 km/s R=7.5 kpc

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Galaxy Mass

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  1. Galaxy Mass • Star Number/Density • Counting stars in a given volume • Use volume of galaxy to estimate mass • Good idea?

  2. Rotation Curve • Best for spirals (s for ellipticals) • Based on Kepler’s Third Law Mass(R) = R v2/G Mass(R) = mass within radius R For Sun • V=220 km/s • R=7.5 kpc • M ≈ 1011 M • Velocity – Mass • M/L values • Sa/Sb > Sc/Sd

  3. Binary Galaxies • Greater uncertainty • M/L = 20-80 • Galaxy Clusters • Even greater uncertainty • M/L up to 1000!

  4. Dark Matter • Evidence • Spiral Rotation Curves • Large mass halo • 2-10 x disk mass • Gravitational Lensing • Amount of mass found by degree of lensing • Mass of clusters > Luminosity of clusters • 90% total mass of Universe!

  5. WIMPs Weakly Interacting Massive Particles Massive neutrinos Fast moving “Hot” Dark Matter (HDM) Detection: Very difficult MACHOs Massive Compact Halo Objects Stars, planets, black holes Slow moving “Cold” Dark Matter (CDM) Detection: Microlensing WIMPs vs MACHOs

  6. Microlensing • Massive object distorts light • Observe many stars, look for brightening • MACHO surveys • MACHO • EROS • OGLE • And many more…. • Results?

  7. Many MACHOs detected – but not enough Other benefits from surveys

  8. Evolution of Galaxies • Depends upon the evolution of its stars • Low Mass stars • More common • Slower • More complex than Pop I, Pop II • [Fe/H] variations between galaxies • [Fe/H] variations within galaxies (gradient) • Why?

  9. [Fe/H] • Comes from supernovae • Which come from massive stars • Which come from large areas of star formation • Which come from large gas/dust clouds • Which are found mainly in disks (mid-plane) • So…. • [Fe/H] gradient (in R, z) linked to all of the above

  10. Halo Objects – Very low [Fe/H] • Formation independent of disk • Globulars formed before disk

  11. What triggered the formation of galaxies? • Early Universe not smooth • Fluctuations ~ 30 million pc • Density Enhancements needed

  12. Gravity versus Gas Pressure • Jean’s Length m=hydrogen • Jean’s Mass Minimum mass that forms ~ 100,000 M

  13. Further evolution information • Star formation/evolution – colors of galaxies • Consistency of surface brightness laws • Contraction leads to galaxy type? • Angular momentum • Magnetic fields • Turbulence • Chemical composition • Current observations of galaxy formation • Deep surveys (HUDF)

  14. Fully formed large galaxies seen at great distance – implications?

  15. Or are they still forming at this distance? • Ellipticals first, spirals later? • Or galaxy building blocks first? • Depends upon form of dark matter

  16. 1996 2002 Galaxy formation – star formation, when did it start? Are we sure?

  17. Other galaxy evolution problems • Bars • Few seen at great distance • Later evolutionary effect? Tidal effect? • Influences later evolution • Gas motion inward/outward • Alters [Fe/H] gradient (big bar – shallow gradient) • Enhances star formation • Bulge structure • Alters galaxy type?

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