the milky way - physics and astronomy at...
TRANSCRIPT
The Milky Way
Cerro Tololo Inter-American Observatory
Large Magellanic Cloud
K. Don, NOAO/AURA/NSFSaturday, January 5, 2013
Panoramic Picture of Milky Way taken from Death Valley, CA, Dan Duriscoe, US National Park Service
Saturday, January 5, 2013
Milky Way Galaxy
Our Galaxy is a collection of stars and interstellar matter - stars, gas, dust, neutron stars, black holes -
held together by gravity
Composite near-IR (2 micron) Image from the Two Micron All Sky Survey (IPAC/Caltech/UMass)
Saturday, January 5, 2013
Historical Models of the Milky Way Galaxy
Greeks: Γαλαξίας κύκλος Galaxias Kyklos "Milky Circle".
Roman: Via Lactea (Milky Way).
East Asia: “Silvery River” of Heaven (Chinese: 銀河; Korean: eunha; Japanese: Ginga)
Finno-Ugric (Finns, Estonians): “Pathway of the Birds”. Birds follow path for migrations... some evidence this is true.
Austrailian Aboriginal: Wodliparri (house-river).
Galileo first suggested the Milky Way is a vast collection of individual stars.
Saturday, January 5, 2013
Historical Models of the Milky Way Galaxy
In 1780 William Herschel produced the map below by counting stars in different directions. He concluded that the Sun is near the center of the Galaxy, and that the
dimensions along the plane were five times greater than the vertical thickness.
Herschel assumed (1) all stars have same luminosity (Absolute Magnitude), (2) Number density in space is roughly constant, and (3) there is nothing in space to obscure the Stars
(fainter stars are farther away)
Sun
In mid-1700s, Immanuel Kant (1724-1804) and Thomas Wright (1711-1786) proposed the Galaxy must be a disk of stars to
explain the circular distribution in the sky. They went further and suggested our Sun is one component in the Milky Way.
William Herschel (1738-1822)
Saturday, January 5, 2013
Historical Models of the Milky Way Galaxy
Jacobus Kapteyn (1851-1922)
Jacobus Kapteyn (1851-1922) used star counting to confirm the Herschel model, but with much-improved methods. Now
called the Kapteyn Universe.
Galaxy consists of a flattened Spheroidal system with a decreasing stellar density with increasing distance from the center. His published self-titled “attempt” to describe the “Stellar system” (=Milky Way) appear in the year he died
(Kapteyn 1922, ApJ, 55, 302):
Saturday, January 5, 2013
Historical Models of the Milky Way Galaxy
Harlow Shapley (1885-1972)
From 1915-1919, Harlow Shapley estimated the distances to 93 globular clusters using RR Lyrae and W Virginis variable stars
(like Cepheids). Shapley found they are not uniformly distributed in the Galaxy, but are concentrated in the
constellation Sagittarius (where the center of Galaxy is). He determined these were 15,000 pc (15 kpc) away.
The most distant clusters he could measure were 70 kpc away. Shapley argued our Galaxy has a diameter of 100 kpc, close to 10x that of Kapteyn. Also as important, Shapley put
our Sun far from the center of the Galaxy. Kapteyn had the Sun near the center.
Saturday, January 5, 2013
Historical Models of the Milky Way Galaxy
Who was right, Kapteyn or Shapley ?
Saturday, January 5, 2013
Historical Models of the Milky Way Galaxy
Who was right, Kapteyn or Shapley ?
Neither ! They are both wrong, but for the same reason. They both ignored the effects of dust, which causes the extinction of light.
Kapteyn missed stars he could not see, could not see the most distant regions of the Milky Way.
Shapley’s variable stars were more luminous then he thought because their apparent magnitudes were extincted.
Similar to being on a boat and trying to see land through fog.
Saturday, January 5, 2013
The Morphology of the Galaxy
The solar Galactocentric distance, R0, is still debated. In 1985 the International Astronomical Union (IAU) adopted R0 = 8.5 kpc. Recent studies
find R0 = 8 kpc (Eisenhauer 2003). Your book uses this latter value.
The Galaxy is composed of a bulge, a thin and thick disk, and a halo.
Most stars are in disk components. Disk contains lots of gas and dust.
Halo has low density and it contains many globular clusters.
Saturday, January 5, 2013
The Morphology of the Galaxy
Structure of Thin and Thick Disks
We define the size of the components using the scale height. (We don’t have a way of defining the “edge” of the galaxy or its components ? )
If n is the number density of stars in the disk, and z is the vertical distance above the Galactic midplane, then the number density scale height is
1/Hn = -(1/n) (dn/dz)
Take Hn to be a constant (OK assumption) then we can solve for n using differential equations:
n = n0 exp( -z/Hn )
If Hn = z then n = n0 e-1, so H is the point where the number density has dropped by a factor of e.
Saturday, January 5, 2013
The Morphology of the Galaxy
Structure of Thin and Thick Disks
Galactic Disk has two major components, the thin disk, and the thick disk.
Thin disk: composed of young stars, dust, and gas, with Hnthin = 350 pc (youngest stars found with scale height of 35-90 pc).
Thick disk: older stars with a scale height of Hnthick = 1000 pc. The number density of stars in the thick disk is ~8.5% that of the thin disk.
Our Sun is a member of the thin disk, and lies about 30 pc above the midplane.
Saturday, January 5, 2013
The Morphology of the Galaxy
Age-Metallicity Relation
Thin and thick disks have different scale heights, stellar densities, and metal fractions and ages !
Recall that stars have different metal fractions, different Populations.
Population I: high metal fractions, Z~0.02.
Population II: low metal fractions, Z~0.001.
Population III: zero metal fraction, Z~0. (hypothesized).
Astronomers commonly use the ratio of Iron (Fe) to Hydrogen (H) relative to that in the Sun to quantify the metal fraction. We call this the metallicity:
Stars with [Fe/H] > 0 have a higher metal fraction than the Sun. Stars with [Fe/H] < 0 have a lower metal fraction.
Saturday, January 5, 2013
The Morphology of the Galaxy
Age-Metallicity Relation
Stars with [Fe/H] > 0 have a higher metal fraction than the Sun. Stars with [Fe/H] < 0 have a lower metal fraction.
extremely metal-poor stars (Population II) have [Fe/H] ~ -5.4. Highest values are [Fe/H] ~ 0.6.
Studying Globular Cluster “turn-off” masses, younger clusters have high [Fe/H] then older clusters, which have low [Fe/H]. This is the
age-metallicity relation.
Saturday, January 5, 2013
The Morphology of the GalaxyAge-Metallicity Relation
Rana 1991, ARAA, 29, 129
Time since formation of disk (Age - td, where td = 12 Gyr)
Solar Value
Saturday, January 5, 2013
The Morphology of the Galaxy
Thin Disk: typical iron-hydrogen ratios are -0.5 < [Fe/H] < 0.3.
Thick Disk: typical iron-hydrogen ratios are -0.6 < [Fe/H] < -0.4 (some as low as -1.6?!)
Which contains older stars ? Which “formed” first ?
Saturday, January 5, 2013
The Morphology of the Galaxy
Thin Disk: typical iron-hydrogen ratios are -0.5 < [Fe/H] < 0.3.
Thick Disk: typical iron-hydrogen ratios are -0.6 < [Fe/H] < -0.4 (some as low as -1.6?!)
Which contains older stars ? Which “formed” first ?
Appears that star formation began in thin disk about 8 Gyr ago, and is continuing today. This is supported by the cooling times of white
dwarfs in the thin disk.
Thick disk predated most of that of the thin disk by 2-3 Gyr, probably during the period 10-11 Gyr ago.
Saturday, January 5, 2013
from Digital Sky LLC
http://www.youtube.com/watch?v=Suugn-p5C1M
Saturday, January 5, 2013
from Digital Sky LLC
http://www.youtube.com/watch?v=Suugn-p5C1M
Saturday, January 5, 2013
Milky Way Galaxy
The Galactic Bulge
COBE Satellite image of Milky Way at 1.2-3.5 micron.
Saturday, January 5, 2013
The Galactic Bulge
Galactic Bulge: Independent component from disk. Mass of the bulge is believed to be ~1010 M⊙. Scale Height is ~100 to 500 pc, depending on whether younger stars are used (smaller scale heights) than older stars (higher scale heights).
Surface brightness (units of L⊙ pc-2 ) follows the “r1/4 law” distribution, discovered by Gerard de Vaucouleurs (1918-1995), also called the de
Vaucouleurs profile.
Our Bulge has an effective radius, re = ~0.7 kpc.
The Bulge is very difficult to observe because it is so centrally concentrated and there is a lot of dust and gas in the Galactic center. Must look in “windows”
with lower extinction (one is the so-called “Baade’s window”).
Stars in the bulge have -2 < [Fe/H] < 0.5. Possibly multiple metallicity groupings in bulge. One group is <200 Myr old, one is as old as 7-10 Gyr.
Saturday, January 5, 2013
The Galactic HaloGalactic (“Stellar”) Halo is composed of globular clusters (GCs) and field stars.
Older, metal-poor globular clusters have [Fe/H] < -0.8, spherical distribution.
These metal-poor GCs range from 500 pc to 120 kilo-pc ! Youngest is about 11 Gyr old and oldest are about 13 Gyr old.
Zinn 1985, ApJ, 293, 424
Saturday, January 5, 2013
The Components of the Galaxy
Neutral Gas Thin Disk Thick Disk Bulge Halo
Mass (1010 M⊙) 0.5 6 0.2-0.4 1 0.3
LB (1010 L⊙) 0 1.8 0.02 0.3 0.1
M/LB - 3 ~10 3 ~1-3
Radius (kpc) 25 25 25 4 >100
Scale Height (kpc)
<0.1 0.35 1 0.1-0.5 3
[Fe/H] >+0.1 -0.5 to +0.3 -2.2 to -0.5 -2 to 0.5 < -5.4 to -0.5
Age [Gyr] <~ 10 8 10 <0.2 to 10 11 to 13
Saturday, January 5, 2013
The Galactic Center
Challenging to observe because of all the dust/gas !
But, in 15 million years, the Sun will be 85 pc above the Galactic midplane, we would presumably have a much better view then !
Saturday, January 5, 2013
The Galactic Center
Astronomers use high angular resolution images in the near-IR (~2 micron) to help see through the dust. This is helpful because
there are large number of K and M giant stars (T ~ 4000 K) in the central part of the galaxy, and
these are brightest in at 2-micron.
Note that the nearest star to the Sun is ~1 pc away. The density of
stars is much higher in the Galactic Center !
From Schödel et al. 2002Saturday, January 5, 2013
The Galactic Center
Astronomers use high angular resolution images in the near-IR (~2 micron) to help see through the dust. This is helpful because there are large
number of K and M giant stars (T ~ 4000 K) in the central part of the galaxy, and these are brightest in at 2-micron.
Astronomer group led by Rainer Schödel and Reinhard Genzel followed the orbits of K-giants near the Galactic center.
One star, S2, has a period of 15.2 yr with eccentricity e=0.87 and perigalacticon distance of 1.8 x 1013 m = 120 AU (a few times bigger than
Pluto’s orbit).
You can work out from Kepler’s laws that the mass interior to S2’s orbit is ~3.5 x 106 solar masses.
Saturday, January 5, 2013
The Galactic CenterProf. Andrea Ghez’s UCLA group.
Saturday, January 5, 2013