ASTR 1040: Stars & Galaxies

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1 ASTR 1040: Stars & Galaxies Our wide world (universe) of Galaxies Expanding universe: Hubble s discovery #2 Challenge of measuring s in universe review methods used Subtle concept of Lookback time Active galaxies: radio jets and quasars Prof. Juri Toomre TA: Ryan Orvedahl Lecture 25 Tues 15 Apr 2014 zeus.colorado.edu/astr1040-toomre Our Schedule Mid-Term Exam 3 on Thurs in class review tomorrow (Wed) 5pm-7pm here Observatory Night #9 (spectroscopy) last night (report), plus lunar eclipse Solar Day (optional) this Fri 2:30-4:30pm Homework #11 due today, new HW #12 The Big Picture: Universe is filled with network of galaxies in groups and clusters ~100 billion galaxies! Finish reading Chap 21 Galaxy Evolution, and 21.3 Quasars and active galactic nuclei in detail Pattern of galaxies (3 million+),15 o portion of sky Brighter = more galaxies Hubble: next showed universe appeared to be expanding! Vesto Slipher (1912) reported that most galaxies showed Doppler redshifts Edwin Hubble, using new 100 telescope, started busily measuring galaxy redshifts Hubble (1929) announced that redshifts of galaxies appear to increase with from us This was startling: suggests an EXPANDING UNIVERSE! 1

2 Hubble and recession of galaxies: measured many redshifts Further away, greater redshift! Hubble guessed their s by size and brightness -- underestimated by factor 10! Hubble showed universe appears to be expanding! Hubble's Law: Hubble's (1929) original: Velocity of Recession (Doppler Shift) (km/sec) v = H o d Hubble's Constant (km/sec/mpc) Distance (Mpc) Scatter here from random velocities of nearby galaxies, unreliable estimates Clicker Question From Hubble's original plot, what is the Hubble Constant? Velocity (km/s) A. 100 km/s B. 500 km/s C. 500 km/s/mpc D km/s E km/s/mpc 1000km/s 500km/s 0 km/s 0 Mpc Distance (parsecs) 1 Mpc 2 Mpc Answer (today) is ~71 km/s/mpc Best current values for expansion H o = 71 +/- 4 km/s/mpc HUBBLE CONSTANT velocity Hubble (1929) plot extended only to 2 Mpc, H o was ~500! Universe expands like raisin bread! On an expanding balloon, no galaxy is at the center of expansion; no edge Expansion happens into a higher dimension (2-D surface into a 3-D space) Balloon analogy for expanding universe Is our 3-D space expanding through a 4 th dimension? 2

3 Clicker -- reading on galaxies How might you classify this galaxy? A. Sa B. SBb C. E D. SO B. Mapping the universe: need s to galaxies! Identify (and calibrate) properties of galaxies that could serve as STANDARD CANDLES -- beyond direct measure by trigonometric parallax 1. Make some measure of an object which identifies its luminosity (like period in Cepheid) 2. Use this luminosity and measure apparent brightness to infer to it ESTIMATE 1 Start with cluster A (upper) whose known via parallax Main-Sequence Fitting A Main Sequence Fitting often compared to nearby Hyades Cluster (M45) Only 151 ly away Compare with other cluster B (lower) Get to B from brightness difference B Distances up to ~200,000 light years Close enough to get measuremen ts through parallax ESTIMATE 2 Cepheid variable stars ESTIMATE 2 Cepheids variables as standard candles Period - Luminosity relation brighter Cepheids have longer periods 1. Measure period of variability 2. From periodluminosity relation, infer the luminosity 3. Compare with apparent brightness and thus determine Cepheid variable in M100 (HST) 3

4 Number of Fuzzier Distance Estimators A. Apparent brightness of (resolved) red and blue supergiants Distance ladder to measure universe B. Size and brightness of H II regions (emission nebulae) or starbirth regions C. Intercompare s so deduced for specific galaxies (overlapping rungs in ` ladder ) Different standard candles are useful for different s Overlap is important! Measuring big s to galaxies STANDARD CANDLES -- important ones in ` ladder 0. Parallax 1. Main-sequence fitting 2. Cepheid variables 3. Tully-Fisher relation 4. White dwarf supernovae Brightness ~ Luminosity / (Distance) 2 ESTIMATE 3 Fast rotation speeds in spiral galaxies à more mass in galaxy à higher luminosity Measure rotation speeds to infer luminosity Need bright edge-on spirals, estimate tilt Tully-Fisher Relation ESTIMATE 4 Even brighter: White dwarf supernovae Bright enough to be seen halfway across observable universe Standard explosion = fusion of 1.4 solar masses of material Nearly the same amount of energy released Useful for mapping the universe to the largest s 4

5 Supernovae in very distant galaxies BEFORE White dwarf supernovae Carbon fusion explosion: mass transfer in binary takes white dwarf `over the edge Roughly same amount of energy released (calibrate) ESTIMATE 4 brighter SN dim more slowly! calibrated Distance ladder Overlapping standard candles REVIEW VELOCITY = H o x recession velocity DEMO HUBBLE CONSTANT H o = 71 +/- 4 km / sec / Mpc ESTIMATE 5 Use Hubble s Law itself to estimate vast s D Measure velocity, then: D = v / H o Example: using H o = 70 km/sec/mpc, and finding that v = 700 km/sec D = 700 km/sec / 70 km/sec/mpc = 10 Mpc = 32 million light years Quasars Quasi-stellar Radio Source (QSOs) Nuclei so bright that the rest of the galaxy is not easily seen First discovered as radio sources - then found to have high redshifts! (far, far away?) 5

6 Cosmological (Big) Redshifts (from expansion of universe) Alternative definition of redshift : Quasar 3C 273 spectrum Z = redshift = change in wavelength/ normal wavelength 1 + Z = observed wavelength / normal wavelength redshifts always have Z > 0 (redder light has larger wavelengths) Tricky to identify hydrogen emission lines. very big red shift Model for active galaxies Accretion disk, supermassive BH, beams on axis Central Engine -- artist s conception Accretion disk around supermassive black hole Disk itself may or may not be obscured by dust If bright nucleus is visible, looks like a quasar, if not, then a radio galaxy Flying toward supermassive black hole Radio galaxies Central elliptical galaxy, huge lobes of emission, compact central source Synchrotron radiation 6

7 Remains of spiral galaxy as dust lane? Prototypical radio galaxy Cen A Giant elliptical galaxy NGC 5128 with dust lane (from spiral galaxy?) + Centaurus A (Cen A) radio source (color lobes) HST Clicker Question Cen A dust lane + nucleus Hubble s Law shows that: IR zoom-in VISIBLE - HST REVIEW VELOCITY = Ho x A. The further away we look in the universe, the faster things are moving B. The further away we look in the universe, the slower things are moving C. Everything in the universe is moving away from us at the same speed D. Everything in the universe is staying still, we re just the ones moving E. We must be the center of the Universe Synchrotron radiation from particles moving outward recession velocity JET HUBBLE CONSTANT Ho = 71 +/- 4 km / sec / Mpc Spinning accretion disk drags along magnetic fields 7

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