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Home , 3C 279, Granat, NGC 3079, NGC 4151

Index

0957+561, 107, 109, 110, 114, 115, 117, Cerenkov radiation, 50 118, 132, 206 Chandra X-ray Observatory, 35, 49, 64, 3C 279, 40, 41 66, 187, 188, 202 Chandrasekhar limit, 75, 76, 232 Aaronson, Marc, 220 Chandrasekhar, Subrahmanyan, 75, 76, , 141, 143, 147 181 Abell 2218, 138, 141, 144 Cl 0024+1654, 140, 142 aberration, 13, 67, 68, 124 clusters of , 137, 140–145, 147, Adams, Walter S., 73, 76, 77 149, 159, 185 adaptive optics, 194, 195 Compton -Ray Observatory, Alvan Clark and Sons, 73 44–47, 49, 62 Anglo-Australian (AAT), 53, Cosmic Background Explorer (COBE), 59 230, 231 Arp, Halton, 153, 154, 156, 222 cosmic rays, 90–93, 95 cosmological constant, 205, 211, 235 B1359+154, 124, 126 Couderc, Paul, 15 Baade, Walter, 79, 80, 82 Crab , 64–66, 82, 84, 85, 94, 96 Barnard, F.A.P., 72, 74 Curtis, H.D., 35, 118, 208 Barnothy Forro, Madeleine, 106, 121 Cygnus X-1, 186, 187 Barnothy, Jeno, 106, 111, 121, 155 Bell, Jocelyn, 81 dark matter, 148, 149, 152, 153, 230, 235 BeppoSAX, 46 de Sitter, Willem, 206 Berks, Robert, 1 de Vaucouleurs, Gerard, 112, 219, 221 Bethe, Hans, 6, 168 degeneracy, 75, 82 black holes, 48, 57, 85, 112, 179, 181–187, Doppler boosting, 31, 40, 48, 51, 63 189, 191–193, 195, 196, 198–203, Doppler shift, 59, 63, 67, 68, 151, 202, 232 206, 212, 220 blackbody radiation, 22, 78, 85, 229 DuBois, W.E.B., 241 blazars, 49, 51 dust, 17, 122, 159, 217, 219, 221 Bohr, Niels, 23 Bradley, James, 13 , Arthur Stanley, 6, 76, 100, Burbidge, Geoffrey, 111, 175 104, 165, 167 Burbidge, Margaret, 175 Einstein Cross, 129–132 Einstein ring, 130, 133, 134, 156, 160 Canada––Hawaii Telescope, 138, Einstein, Albert, 1, 3, 7, 14, 58, 97–99, 140, 142, 200 102, 104–106, 134, 148, 149, 152, Carswell, R.F., 108, 110, 111 155, 180, 181, 205, 211, 213, 235, Cepheids, 165, 210, 216, 217, 219, 223, 237, 241 225, 228, 229 Ellis, Richard, 146 244 Index

European Southern Observatory, 139, 133, 140–146, 148, 158–162, 175, 140, 145, 154, 195 200–202, 217, 222, 225 Hubble’s Variable Nebula, 20, 21 Fath, E.A., 165, 196 Hubble, Edwin, 7, 206, 208, 209, 211–214, Fermi, Enrico, 92 225, 234 Fisher, Rick, 220 Huchra, John, 220 Fishman, Jerry, 45 Humason, Milton, 211, 212 Fowler, Willy, 175, 176 frame dragging, 238 Infrared Astronomical Satellite (IRAS), Freedman, Wendy, 223 125–127, 192 Freundlich, Erwin, 100 infrared astronomy, 189, 193, 220 International Ultraviolet Explorer (IUE), Friedmann, Alexander, 206 27, 29–32 Frost, E.B., 105 FSC 10214+4724, 125, 129, 130 jets, 31, 35–37, 41, 42, 48, 51, 52, 57, fusion, 7, 168, 174, 176 59–61, 63, 65, 95, 198, 199 Jodrell Bank, 107–109 Galactic Center, 158, 189–193, 195, 197 , 12 Keck Observatory, 146, 195–197, 227 gamma rays, 42, 48–50 Kennicutt, Rob, 222, 223 gamma-ray bursts, 42, 43, 45–48 Kirchhoff, Gustav, 24 general relativity, 1, 71, 78, 97, 104, Kitt Peak, 84, 85, 108, 110, 111, 114, 137, 179–181, 205, 218, 235, 238–240 139, 151, 175, 214, 221, 223, 224, Giacconi, Riccardo, 184, 202 226, 233 globular clusters, 224, 226, 227 Kuiper Airborne Observatory, 192, 193 gold, 71, 72, 177 Large Magellanic Cloud, 15, 43, 44, 83, Granat, 62, 63 157, 187, 209, 210, 219, 232 gravitational deflection, 97–99, 101, 102 Leavitt, Henrietta, 209, 210 gravitational lens, 8, 105, 115, 131, 132 Lemaˆıtre, Georges, 206 gravitational lensing, 102–104, 106, 107, Lick Observatory, 35, 54, 56–58, 73, 84, 110, 111, 113, 118, 121, 124, 133, 111, 114, 117, 140, 154, 174, 206, 135, 147–149, 153, 156, 159, 162, 208, 214, 234 182 light echo, 14–20 gravitational radiation, 238–240 Lorentz factor, 32, 33, 37, 58, 88, 93, 96 gravitational , 76–78, 80 Lorentz, Hendrik, 32, 33 Gravity Probe-B (GP-B), 238, 239 Lowell Observatory, 151, 206, 207 Green Bank, 107–109, 122, 220 Lynds, Roger, 138, 139

Hardie, Robert, 73 M33, 210 Hawking, Stephen, 181–183 M81, 200 Herschel, John, 14, 165 M87, 35–37, 40, 96, 199, 200 Hertzsprung–Russell diagram, 172 MACHOs, 152, 153, 155, 157, 158 Hess, Victor, 90 Mandl, R.W., 103, 104 Hewish, Anthony, 81 Margon, Bruce, 54–57 Hoag, Arthur, 137, 139 Mauna Kea, 111–113, 130, 140, 147, 195, Hoyle, Fred, 175–177 196, 200 Hubble constant, 131, 132, 215–217, 219, Maxwell, James Clerk, 23 221, 222, 226, 231, 234 microlensing, 148, 153, 155, 156, 158–162 Hubble , 30, 35, 36, , 60–63, 95 44, 59, 64, 78, 79, 85, 91, 93, 95, microwave background, 227, 229, 232 115, 117, 118, 122–126, 129–131, Milgrom, Mordehai, 57, 152 Index 245

Milky Way, 6, 149, 155, 176, 187, 189, Rubin, Vera, 151, 152 195, 206–208, 210, 217, 219, 232 Russell, Henry Norris, 165, 166, 172 Mould, Jeremy, 220, 223 Ryle, Martin, 38 MS1512-cB58, 141, 145, 146 Mt. Wilson Observatory, 73, 76, 153, 175, Sandage, Allan, 211, 214–217, 219, 221, 194, 208, 209, 211, 213, 214, 216, 222, 225, 231 222, 223 Schwarzschild, Karl, 180 SETI, 162 National Academy of Sciences, 1, 208 Seyfert galaxies, 26, 32, 123, 153, 196, neutrinos, 172, 173 198 neutron , 43, 48, 71, 78, 80, 82, 83, Shklovsky, Iosif, 94 85, 187, 192, 232 Sirius B, 72–74, 76–79 Newton, Isaac, 1, 6, 97, 152, 182, 205, Slipher, V.M., 206, 207 237 Sloan Digital Sky Survey, 122, 123, 148, NGC 1068, 196 155, 202 NGC 2261, 20, 21 eclipse, 99–101 NGC 3079, 107, 109, 118 Soucail, Genevi`eve, 138, 140 NGC 3115, 200 special relativity, 31, 40, 67, 79, 83 NGC 3314, 159–162 , 21–26 NGC 4151, 27, 28 , 94, 146 NGC 4321, 228 SS 433, 55–61, 152 NGC 5548, 30, 32 starbow, 67, 68 NGC 5746, 151 strong nuclear force, 169 NGC 6822, 210 , 41, 51 nuclear tests, 91, 92, 170, 176 superluminal motions, 40 Supernova 1987A, 15–18, 83, 232 Palomar Observatory, 108, 112, 113, 118, supernovae, 15, 16, 44, 48, 49, 53, 59, 79, 122, 153, 199, 214, 216 80, 82, 85, 95, 105, 177, 185, 189, Payne-Gaposchkin, Cecilia, 6 209, 223, 225, 231, 232, 234 Penrose–Terrell rotation, 34, 36 surface-brightness fluctuations, 225 PG 1115+080, 119 synchrotron radiation, 86–89, 93–96 photoelectric effect, 1, 7, 21 time dilation, 63, 93 , Max, 22 Tinsley, Beatrice, 221 planetary nebulae, 223, 224 Tolman, Richard, 211, 218 polarization, 94, 96 pulsars, 80–82, 84, 85, 239 , 184, 186, 188 quantum theory, 23 V838 Monocerotis, 17, 19 quasars, 26, 28, 35, 39–41, 49, 95, Van Allen belts, 91 109–111, 114, 115, 117, 121, 123, Very Large Array, 39, 60, 62, 88, 113, 131, 148, 153, 154, 156, 179, 198 116, 122 very-long-baseline interferometry (VLBI), radio astronomy, 37, 85 40, 42 radio galaxies, 40, 87, 88, 95, 123, 198, cluster, 199, 220, 221, 223, 225, 229 199 von Weizs¨acker, Carl, 6, 168 radioactivity, 6, 166 redshift, 14, 47, 77, 153, 179, 211, 212, W50, 53, 59, 60 215, 218, 220, 229, 230 Walsh, Dennis, 107, 108, 110, 111, 118 Rees, Martin, 57, 199 weak nuclear force, 169, 172 Refsdal, Sjur, 105, 116, 131, 149 Wells, H.G., 241 246 Index

Weymann, Ray, 110, 111, 115, 119 X-ray astronomy, 8, 184 white dwarfs, 71–78, 82, 177 XMM/Newton, 187 Wilkinson Microwave Anisotropy Probe (WMAP), 231, 232 Yerkes Observatory, 73, 105, 106 Telescope, 127, 128, Young, Peter, 112, 133, 199, 200 132 WIMPs, 152 Zwicky, Fritz, 79, 80, 82, 102–105, 119, Wright, Thomas, 207 121, 141, 149 Colour Tables Chapter 2

3C 279 Superluminal Motion

1992.0

1993.0

1994.0

1995.0 5 milliarcseconds

Fig. 2.13. The quasar 3C 279, showing superluminal motion in its jet. Pseudocolor intensity coding has been used to make subtle features more apparent. The prominent outer knots to the right are moving outward with a projected speed of 4c.Atthis quasar’s distance of 5 billion light-years, the scale bar of 5 milliarcseconds corresponds to a length of 100 light-years. The bright knot to the right moves almost 20 light-years in 4.5 years, as viewed in our reference frame. These observations, at a radio wavelength of 1.3 cm, were carried out initially with an ad hoc network of radio telescope, and starting in 1994, with the Very Long Baseline Array of the National Radio Astronomy Observatory, a dedicated network of stretching from the Virgin Islands to Hawaii. (Images courtesy Ann Wehrle and Steve Unwin.) This figure also appears in color as Plate 1. ^ VLA HST UIT EUVE ROSAT EGRET Cerenkov

Optical UV X−rays γ rays + + +++ Infrared ++ + ++++ −10 Radio + + 10 − + + + + + +− second + + flaring + + 2 +++++++ + +++++++ + + +++++ ++ +++ +

+ faint ), erg/cm ),

ν +

F ν 10−12 − + − +++ + ++ Markarian 421 − broad−band spectrum Flux per decade ( decade per Flux ++

10−14 10 15 20 25 log frequency (Hertz)

Fig. 2.17. The blazar Markarian 421 as seen across the . This montage shows the relative energy received from this blazar in various spectral regions, both when it is quiet and when it is in a bright flare such as may accompany the appearance of new jet material. The inset images show its appearance to various instruments used for these observations. The distinct gamma-ray peak is evidence that its lower-energy radiation is being scattered and Doppler-boosted in a jet directed nearly toward us. (Data provided by T. Weekes, the NRAO FIRST radio survey, and the NASA archives from the Hubble, Compton, ROSAT, UIT,andExtreme Ultraviolet Explorer missions.) This figure appears in color as Plate 2. Fig. 2.27. Simulations of the starbow as seen looking forward from the bridge of a starship in the vicinity of , heading toward . Each shows a full hemisphere’s view. One image is at rest (that is, our actual view), while the others represent forward velocities of 0.5, 0.9, and 0.99c. As the velocity toward Orion increases, aberration bunches the stars forward at high velocities, and Doppler shifting changes their colors and relative brightness, depending on the broad shape of each ’s spectrum. At yet higher speeds, infrared emission from interstellar dust shifts into the visible band straight ahead. (Images courtesy of Jun Fukue of Osaka Kyoiku University, originally produced for the 1991 Japanese-language book Visual Relativity 2.) This figure appears as color plate 3. Chapter 4

Fig. 4.9. The gravitationally-lensed quasar Q0957+561 in a color-composite Hubble image. The quasar images, 6 arcseconds apart in our sky, appear blue, with the redder light of the primary lensing almost in front of the southern image. Additional galaxies are part of a surrounding cluster, at redshift z =0.39 or a distance of about 4 billion light-years. Data from the NASA/ESA archive, orig- inally obtained with G. Rhee as principal investigator. This figure appears as color plate 4. Chapter 5

+

Fig. 5.8. Simulated images of a galaxy (Messier 83, in this case) as it would appear gravitationally lensed by a point mass (such as an intervening ). These three images depict the situation as the lens moves from left to right across the galaxy, eventually forming a ring image of its bright core. This and Fig. 5.9 use screen shots created with Peter J. Kernan’s “Lens an Astrophysicist” applet. (For clarity, I have removed superfluous images inside the Einstein ring, created by the applet’s assumption of periodic tiling of the sky with the same pattern outside the image region.) This figure appears in color as Plate 5. Fig. 5.9. Simulated images of the galaxy Messier 83 as it would appear lensed by foreground point masses, now varying the lens mass between images. The lens mass doubles for each step downward in the figure. As in Fig. 5.8, I have removed superfluous images inside the Einstein ring. This figure appears in color as Plate 6. Fig. 5.12. The spectacular lensed galaxy in the cluster Cl 0024+1654, in a color composite Hubble image. The cluster generates five images of a single blue background galaxy, distinguished by its distinct “theta” shape; in this case, the lensing effect is visually obvious. (W. Colley, Princeton University, and NASA). This figure appears in color as Plate 7. Chapter 8

Fig. 8.13. An all-sky map of fluctuations in the cosmic microwave background, the product of the first year of measurements by the Wilkinson Microwave Anisotropy Probe (WMAP). Pseudocolor mapping is used to make these subtle patterns stand out more clearly. This map has been processed to remove the signatures of foreground dust and gas in the as well as more distant radio sources. (NASA/WMAP Science Team.) This figure appears in color as Plate 8.