# ASTC22 - Lecture 7 Milky Way's kinematics and structure - PowerPoint PPT Presentation

ASTC22 - Lecture 7 Milky Way's kinematics and structure

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ASTC22 - Lecture 7 Milky Way's kinematics and structure

## ASTC22 - Lecture 7 Milky Way's kinematics and structure

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1. ASTC22 - Lecture 7 Milky Way's kinematics and structure Parallax Luminosity and mass functions - a few basic facts Kinematics of the solar neighborhood Asymmetric drift Thin disk, thick disk Open and globular clusters - metallicity, age, distribution, motion Infrared view Galactic bulge and center Differential rotation

2. Step number one: measure the parallax (Hipparcos satellite, 1989-1993) measure the apparent magnitude m. This could be done for0.12 mln bright stars, with positional accuracy ~milliarcsec (1 milliarcsec = 1/1000 seeing disk) Step number two: derive distance from (d/ 1pc) = (1” / parallax) derive the absolute magnitude from distance modulus m - M = 5 log (d/ 10pc) = 5 log (0.1” / parallax) This gave accurate distances to ~few*100 pc.

3. Luminosity function --> initial luminosity function --> ---> initial mass function.

4. The most numerous stars in the Galaxy are small, 0.3-0.5 Msun M*(Salpeter IMF) Brown dwarfs Frequency of stars with different masses = a power-law with exponent (index) -2.35

5. Thin and thick disks of the Galaxy

6. Vertical velocity w.r.t. sun (W) as a function of stellar age: stars are born in a thin disk with small W; old stars are in a thick disk. -10 km/s

7. The Bottlinger diagram for 200 main-sequence star from the solar neighborhood U = radial velocity difference w.r.t. the sun V = tangential velocity diff. - pop I objects similar to the sun U=U* - Usun V=V* - Vsun gc = Galactic center in general (U,V,W) V <0 U>0 or <0 Retrograde prograde orbits orbits gc V* Vsun

8. Open clusters - e.g., Pleiades, Hyades (Pop I) 16 Myr 100 Myr Foreground gas nebulae

9. 47 Tucanae is the second brightest globular cluster. It contains ~1 mln star. It can only be seen from the Southern Hemisphere. This image is 34 arcmin across, ~ 0.56 degrees (comparable with Moon, Sun). The infrared colors of all these stars are very similar.

10. Globular clusters - e.g. omega Centauri, 47 Tucanae (Pop II) spherical system thick disk Connection between kinematics and geometry: thick disk of high-metallicity globular clusters (left-hand panel) is made of objects on low-inclination, nearly-circular orbits <=> the system has some prograde rotation. Spherical system (right panel) has completely disorganized motions, no rotation on average; some clusters have prograge, some retrograde motion, Orbits are highly inclined.

11. Age, distance, metallicity are varied in models until the predicted H-R diagram (below) matches the observations (above). For instance, 47 Tuc has [Fe/H] = -0.83 and age ~12 Gyr M30 has [Fe/H] = -2.31 and age ~14 Gyr One also uses RR Lyr variables (pulsating low-mass stars with L~50 Lsun) as standard candles

12. INFRARED & RADIO VIEW of our GALAXY SPECTRAL REGION WAVELENGTH TEMPERATURE (microns) (Kelvin) WHAT WE SEE Near-Infrared 0.8 to 5 740 to 5200 Cooler red stars, Red giants, Dust is transparent Mid-Infrared 5 to 2590 to 750 Planets, comets, asteroids Dust warmed by starlight Protoplanetary disks Far-Infrared 25 to 350 10 to 100 Cold dust Central regions of galaxies Very cold molecular clouds …………………………………………………………………………………………… Sub-mm and mm 850-2000 10 to 30 Larger (~mm), cold dust grains Radio e.g., 21 cm HI line Global structure of the Galaxy, hydrogen clouds

13. Infrared view of the center of the Galaxy: optical view 2MASS (2 micron all-sky) survey Picture made from star counts (not a direct image) total of 250 mln stars measured in 2MASS.

14. Infrared view of the Galaxy hR = 2 to 4 kpc, both for the thin (hz ~ 0.3 kpc) and the thick disk (hz ~ 1.5 kpc) Beyond R=15 kpc, the disk density is rapidly declining. The brightness distributions of other galaxies show similar downturns.

15. Infrared view of the Galaxy: 2MASS (2 micron all-sky) survey 20% of Galaxy’s light from the bulge, R~1 kpc Stars: few Gyr old, metal-rich unlike the metal-poor stars of the galactic halo, the inner halo is also more round and does not show rotation (bulge rotates in the prograde sense, like the sun, but slower: <Vc> ~ 100 km/s) A slight asymmetry of the bulge and additional kinematic data show that the Milky Way has a central bar extending to R=2-3 kpc. It is a Sbc galaxy or SABbc( r) - there can be no perfect agreement when looking at multiwavelength data! The center of the Galaxy (nucleus) is a very exotic place, with the Sagittarius A* radio source, surrounded by a torus (R=7 pc) of molecular gas, which flows in at a rate of 0.001-0.01 Msun/yr and formed dozens of massive stars within the last 3-7 Myr. Nucleus (right panel, showing gas) is much smaller than the black dot in the background picture. A fairly dark and inactive, ‘starved’ black hole (m= 2-3e6 Msun) lurks in the center of Galactic Nucleus (white dot). Bulge Galactic Nucleus .

16. Differential rotation of the Galaxy: rotation with shear, similar to Kepler’s laws Differential rotation of the Galaxy was discovered by Jan Oort in 1927 using proper motions of stars at different galactic longitudes l, because it varied as Vt ~ const + cos 2 l, (which was actually known in 1900).

17. The position and velocity of the “Local Standard of Rest” (solar neighb.) Ro = sun-Galaxy center dist. Ro = 8.5 kpc (IAU), 8 kpc (recent) Vo= 220 km/s (IAU), 200 km/s (recent) IAU=International Astron. Union Rotation of the Galaxy Assuming circular motions of S and P,

18. Rotation of the Galaxy Errata (CUP,on-line)!

19. A B Jan Oort (1900-1992)

20. This section of the book shows you how A,B, Ro, Vo, are fitted to the observed radial velocity measurements..read it ! (other parts too!)

21. Distribution of H and H2 in our Galaxy

22. Rotation curve of Milky Way is approximately flat: