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Cambridge University Press 978-0-521-82048-6 - The de Vaucouleurs Atlas of Galaxies Ronald J. Buta, Harold G. Corwin and Stephen C. Odewahn Index More information Index 2MASS, see Two Micron All-Sky BCD, see blue compact dwarfs DDO dwarfs, 54 Survey Birr Castle, 6, 7 de Vaucouleurs classification system Block, A., 83 classification volume, 13, 15, 17, 53 accretion rings, 80 Block, D. L., 8 edge-on galaxies, 7, 19, 33, 35, 38, active galactic nuclei, 49 blue compact dwarfs, 70–73, 270, 296 40, 135, 272 Amorphous irregular galaxies, 12, 16, Burton, C. E., 6 revisions to the VRHS system, 84 84, 266, 268, 271, 296 stages, 13, 15, 16, 19, 23, 24, 54, 61, asymmetry, 16, 17, 19, 22, 33, 130, Canberra, Australia, 2 87, 259 164, 172, 178, 184, 189, 194, 197, Canes Venatici I Cloud, 262 underline notation, 15, 16, 86, 131, 203, 212, 227, 233, 250, 252, 255, carbon stars, 246 148, 163, 167, 180, 184, 187, 256, 259–264, 286–288, 299, 309 Carnegie Atlas, 1, 2, 13, 24, 81, 193, 223, 229, 245, 246 Atlas Units, 39, 47, 55, 57, 73, 82–85 179, 264 de Vaucouleurs, A., 311 atmospheric seeing, 83 Cartwheel, 77, 78, 300 de Vaucouleurs, G., 1, 311 atomic hydrogen, 5 Catalogues digital images, 2, 3, 81–83 Australian National University, 311 CSRG, 3, 44, 66, 86, 147, 152 disky ellipticals, 57 distribution of bar strengths, 306, 307 Baade, W., 1 GC, 6 double-barred galaxies, 50, 51 Ball, R. S., 6 IC, 6 Dreyer, J. L. E., 6 bar-driven resonance rings, 80 NGC, 6, 52, 260 dust ring, 122, 123, 144, 158, 174, 176, bar–spiral separation, 61 RC1, 3 177, 179, 183, 275 Barnard, E. E., 6 RC2, 3, 51, 72, 81, 134 dust-lane ellipticals, 56, 57, 122 barred spirals, 1, 7, 10, 12, 13, 16, 50, RC3, 3, 16, 19, 20, 22–24, 27, 63, 64, dust-penetrated classification, 65 59, 60, 137, 183, 186, 198, 208, 71, 72, 76, 77, 80–82, 86, 87, near-IR pitch angle classes, 58 213, 249, 250, 304, 306, 99, 113, 122, 148, 149, 153, dwarf ellipticals, 53, 54 plumes, 45, 164, 168, 171, 213 158, 174, 175, 192, 199, 215, nucleated, 53, 220, 296 bars 219, 287, 294, 296 dwarf galaxies, 16, 27, 52, 76, 269 ansae, 36, 37, 108, 112, 116–120, SGC, 3, 27 dwarf irregulars, 53, 54, 70, 266 122, 128, 129, 135, 137, 144, CCD, see charge-coupled device dwarf spheroidal galaxies, 83 146–148, 171, 175, 176, 194, Cepheids, 247, 253 Dwingeloo 1, 67, 245 282, 294 charge-coupled device, 3, 30, 81–83 ellipticity, 60, 306, 307 clumpy irregular galaxy, 270 fast, 38, 39, 41, 128 collisional ring galaxies, 299 early-type galaxies, 8, 36, 87, 138, 304 formation, 67, 302, 304, 305 compact galaxy, 75 edge-on barred galaxies Lagrangian points, 37, 45, 164 Copeland, R., 6 box/peanut bulges, 33, 36, 111 ovals, 15, 37, 41, 120, 217, 301 Corotation Resonance, 38, 39, 41, 42, observational diagnostics, 33 pattern speed, 35, 38, 39, 41, 44, 45, 44, 45, 47, 78, 79, 163, 304 edge-on spirals, 24, 36 47, 51, 65, 66, 79, 108, 112, counter-rotation, 80, 139 elliptical galaxies, 1, 7, 54, 56, 57, 74, 119, 128, 133, 151, 163, 192, CR, see Corotation Resonance 76, 80, 99, 106, 201, 294, 309, 311 302, 305–307 Curtis, H. D., 6 boxy, 56 periodic orbits, 33, 37, 38, 41–44, 48, cylindrical rotation, 33 disky, 56 135, 305, 307 isophote twists, 57 quadrupole moment, 47 DDO 50, 269 epicyclic approximation, 132 relative frequency, 59, 305 DDO 155, 270 epicyclic frequency, 41 slow, 38, 41, 43, 56, 66, 77, 302, 304 DDO 165, 270 ESO 34−11, 299 strength, 13, 15, 38, 60–65, 69, 79, DDO 180, 261 ESO 111−22, 121, 202 188, 306, 307 DDO 216, 288 ESO 153−20, 181 © Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-82048-6 - The de Vaucouleurs Atlas of Galaxies Ronald J. Buta, Harold G. Corwin and Stephen C. Odewahn Index More information 338 Index ESO 198−13, 153, 162 galaxy morphology Hubble sequence, 7, 8, 11, 22, 24, 56, ESO 235–58, 77, 78, 298 dash–dot in brackets, 18 287, 301–304, 307–309 ESO 236−29, 152 distinct components, 69, 70 Hubble Space Telescope, 25, 30, 35, 37, ESO 239−4, 160 visual, 6, 7, 22, 80 49–51, 76, 77, 83, 103, 132, 141, ESO 245−1, 160 galaxy morphology, effects of 148, 152, 174, 196, 208, 299 ESO 286−10, 159 distance, 4, 126, 152, 175, 262, 269, Hubble tuning fork, 1, 10, 11, 53 ESO 294−16, 160 270, 312 Hubble, E. P., 1 ESO 297–27, 30, 38 environment, 5, 49, 68, 80, 117, 140, Hubble–Sandage classification ESO 325−28, 45, 64, 67, 204 220, 240, 247, 306, 308 system, 2 ESO 350−40, 300 evolution, 5, 6, 37, 38, 44, 48, 50, 51, Hunter, S., 6, 7 ESO 365−35, 136 66, 80, 301, 304, 305, 307, 309 ESO 426−2, 136 Galactic extinction, 23, 24, 67, 71, I0 galaxies, 16, 71, 266, 271, 290, 291, ESO 437−67, 181 72, 117 293, 296–298 ESO 509−98, 37, 45, 52, 147 inclination, 23, 27, 30, 35, 118, 126, IC 10, 71, 269 ESO 526−7, 195 164, 169, 171, 191, 192, IC 1613, 31, 269 ESO 565−11, 49, 50, 66, 71, 151, 176, 199–201, 207, 210, 219, 228, 228 230, 239, 257, 278, 284, 285, IC 1179, 295 ESO 566−24, 164, 186, 189 287 IC 1181, 295 ESO 575−47, 181 luminosity, 5, 11, 16, 21, 22, 24, 27, IC 1993, 182, 197 ESO-B Sky Survey, 81 29, 51–55, 57, 63, 76, 84, 99, IC 1438, 137, 150 extraplanar dust, 281, 282 106, 113, 175, 265, 266, 270, IC 1459, 102 274, 288, 292, 300, 306, 308, IC 1805, 103 311 IC 2006, 134 faint fuzzies, 108 redshift, 5, 22, 75, 152, 165, 186, IC 2036, 181 Fourier bar, 59, 142 273, 305, 307–309 IC 2163, 73, 294 fundamental plane, 56 total mass, 5, 304, 301 IC 2233, 287 wavelength, 4, 5, 33, 49, 58, 83, 84, IC 2574, 265 87, 200, 309 IC 3328, 53 galaxy classification giant elliptical galaxies, 99, 106 IC 3370, 57 CAS system, 309 giant low surface brightness galaxies, 54 IC 342, 67, 103, 245, 247, 266, 288 cells, 13, 19, 69, 87 globular clusters, 49, 54, 76, 103, 108, IC 3583, 173 continuity, 13, 15, 16, 28, 39, 62, 254, 299 IC 4182, 259, 262 105, 128 GOLDMine, 81 IC 4290, 137, 141 family, 14, 15, 22, 43, 61, 64, 85, 86, Gould, S. J., 1 IC 4444, 225 125, 135, 140, 278, 284, gravitational torque method, 60, 61, 64, IC 5052, 288 305 188, 306, 307 IC 5169, 121 stage, 2, 15, 17–20, 22–24, 27, 36, GTM, see gravitational torque method IC 5240, 18, 35, 40, 64, 66, 78, 137, 44, 55, 63, 64, 107, 124, 137, 138 162, 164, 182, 206, 226, 232, IC 5325, 225 235, 243, 246, 247, 252, 254, Handbuch der Physik,2,3 IC 879, 159, 280 259, 260, 273, 275, 292, Harvard Boyden Station, 2 ILR, see Inner Lindblad Resonance 302 hermeneutical circularity, 301 image processing type correlations, 19, 22 Herschel, J., 6 background subtraction, 83 variety, 11, 14, 15, 18, 19, 22, 24, 25, Herschel, W., 6 bad columns, 83, 84 52, 129, 147, 153, 166, 208, HII regions, 54, 66, 69, 70, 72, charge overflow, 83 209, 214, 215, 219, 222, 226, 125–127, 135, 138, 142, 152, 163, CI map, 84 228, 231, 249, 250, 256, 263, 165, 170, 172, 196, 201 cosmic ray event removal, 83 264, 277, 278, 282, 284, Holmberg II, 269 FITS, 83, 84 307 HST, see Hubble Space Telescope Fourier analysis, 30, 33, 155 Galaxy Evolution Explorer Hubble Atlas, 1, 2, 10–12, 15, 18, 51, surface brightness map, 82, 84 (GALEX), 309 84, 130, 141, 167, 228 unsharp masking, 33 galaxy formation, 3, 301–303 Hubble Heritage, 83 zero point, 82, 84, 312 © Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-82048-6 - The de Vaucouleurs Atlas of Galaxies Ronald J. Buta, Harold G. Corwin and Stephen C. Odewahn Index More information Index 339 Image Reduction and Analysis leading dust lanes, 126, 127, 132, 133, NGC 53, 65, 66, 165 Facility, 83, 84 138, 141, 145, 148, 149, 151, 156, NGC 128, 33, 39 COSMICRAY, 83 166, 167, 168, 169, 170, 172, 184, NGC 147, 54 IMEDIT, 83 185, 188–191, 193, 194, 207, 208, NGC 150, 188 IMSURFIT, 83 210, 211, 213, 231, 232, 236, 244 NGC 151, 206, 223 XIMTOOL, 84 LEDA, 87 NGC 157, 235 Infrared Array Camera (IRAC), 309 lens, 8, 11, 15, 37, 38, 45, 51, 52, 69, NGC 210, 15, 182, 195 inner lens, 52, 111, 112, 114, 119, 125, 85, 99, 105, 107–116, 119, 123, NGC 221, 9, 106 136, 147, 149, 153, 155 125, 129, 136, 141, 145, 147, 149, NGC 224, 201 Inner 4 : 1 Ultraharmonic Resonance, 153, 155, 156, 177, 258, 274, NGC 244, 270 41, 44–47, 79, 132, 163 294, 296 NGC 247, 253 Inner Lindblad Resonance, 41, 43, 45, lenticulars, 8, 16, 19 NGC 253, 230, 237, 238 51, 79, 132, 141, 178, 180, 192, Leo I dwarf spheroidal galaxy, 83 NGC 266, 162, 168 213, 220, 305 Leo II dwarf spheroidal galaxy, 53, 83 NGC 278, 196 vertical, 36 Lindblad precession frequencies, 41 NGC 289, 221 inner pseudoring, 68, 86, 119, 127, 130, LINER, 191 NGC 300, 253 131, 139, 141–145, 151, 152, 154, low surface brightness galaxies, 54 NGC 309, 13, 14, 226, 228 158, 166–169, 171, 172, 176, 185, luminous asymmetric objects, 309 NGC 428, 263 187, 189–191, 193–198, 200, 203, luminous diffuse objects, 309 NGC 578, 31, 251 210, 211, 214, 218, 219, 221, 227, NGC 584, 109 228, 233–236, 239, 240, 244, 245, M31, 6, 54, 106, 201 NGC 598, 31, 243, 246 247–251, 257, 258, 261, 264, 292, M51, 6, 28, 290, 291 NGC 613, 34, 211 294 M61, 8, 15 NGC 619, 176 inner ring, 11, 13, 15, 18, 30, 35, M81 Group, 270 NGC 625, 268 44–46, 48, 50, 54, 64–66, 69, 71, M82, 12, 178, 296 NGC 628, 28, 232 78, 79, 112, 114, 116–122, 124, M83, 8, 15, 17, 231 NGC 678, 277 126–136, 138, 141, 145, 146, M101, 245 NGC 680, 277 148–154, 156–158, 163–172, 174, Maffei 1, 67, 68, 71, 103 NGC 685, 248 175, 179, 180, 183–187, 189–191, Maffei 2, 67, 72, 222 NGC 718, 142 192–197, 200, 202, 207–209, 211, Magellanic Clouds, 8, 15, 16, 54, 311 NGC 720, 102 212, 214, 216, 217, 219, 223, 224, characteristic asymmetry, 16 NGC 779, 203 228–230, 232, 233, 235, 247, 258, Magellanic spirals and irregulars, 16 NGC 799, 155 273, 278, 284, 290, 292 Malin 1, 54, 55 NGC 864, 241 interstellar dust mean radial force, 60 NGC 891, 281 composition, 227 merger, 33, 49, 73, 75, 106, 153, 157, NGC 908, 238 IRAF, see Image Reduction and 196, 209, 227, 235, 271, 275, 292, NGC 925, 258 Analysis Facility 295, 297, 298, 301, 304 NGC 936, 107, 119 Irr I galaxies, 9, 12 Messier, C., 6 NGC 1003, 256 Irr II galaxies, 9, 12 misaligned bar–ring galaxies, 176, 228 NGC 1022, 158 irregular galaxies, 54 Mitchell, R.
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  • ASTRONOMY and ASTROPHYSICS the Elliptical Galaxy Formerly Known As the Local Group: Merging the Globular Cluster Systems

    ASTRONOMY and ASTROPHYSICS the Elliptical Galaxy Formerly Known As the Local Group: Merging the Globular Cluster Systems

    Astron. Astrophys. 358, 471–480 (2000) ASTRONOMY AND ASTROPHYSICS The elliptical galaxy formerly known as the Local Group: merging the globular cluster systems Duncan A. Forbes1,2, Karen L. Masters1, Dante Minniti3, and Pauline Barmby4 1 University of Birmingham, School of Physics and Astronomy, Edgbaston, Birmingham B15 2TT, UK 2 Swinburne University of Technology, Astrophysics and Supercomputing, Hawthorn, Victoria 3122, Australia 3 P. Universidad Catolica,´ Departamento de Astronom´ıa y Astrof´ısica, Casilla 104, Santiago 22, Chile 4 Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA Received 5 November 1999 / Accepted 27 January 2000 Abstract. Prompted by a new catalogue of M31 globular clus- al. 1995; Minniti et al. 1996). Furthermore Hubble Space Tele- ters, we have collected together individual metallicity values for scope studies of merging disk galaxies reveal evidence for the globular clusters in the Local Group. Although we briefly de- GC systems of the progenitor galaxies (e.g. Forbes & Hau 1999; scribe the globular cluster systems of the individual Local Group Whitmore et al. 1999). Thus GCs should survive the merger of galaxies, the main thrust of our paper is to examine the collec- their parent galaxies, and will form a new GC system around tive properties. In this way we are simulating the dissipationless the newly formed elliptical galaxy. merger of the Local Group, into presumably an elliptical galaxy. The globular clusters of the Local Group are the best studied Such a merger is dominated by the Milky Way and M31, which and offer a unique opportunity to examine their collective prop- appear to be fairly typical examples of globular cluster systems erties (reviews of LG star clusters can be found in Brodie 1993 of spiral galaxies.
  • Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei Davide Lena

    Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei Davide Lena

    Rochester Institute of Technology RIT Scholar Works Theses Thesis/Dissertation Collections 4-2015 Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei Davide Lena Follow this and additional works at: http://scholarworks.rit.edu/theses Recommended Citation Lena, Davide, "Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei" (2015). Thesis. Rochester Institute of Technology. Accessed from This Dissertation is brought to you for free and open access by the Thesis/Dissertation Collections at RIT Scholar Works. It has been accepted for inclusion in Theses by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei A Search for Recoiling Supermassive Black Holes Gas Kinematics in the Circumnuclear Region of Two Seyfert Galaxies Davide Lena A dissertation submitted in partial fulfillment of the requirements for the degree of Ph.D. in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Rochester Institute of Technology © D. Lena April, 2015 Cover image: flux map for the [NII]λ6583 emission line in the nuclear region of the Seyfert galaxy NGC 1386. The map was derived from integral field observations performed with the Gemini Multi Object Spectrograph on the Gemini-South Observatory. Certificate of Approval Astrophysical Sciences and Technologies R·I·T College of Science Rochester, NY, USA The Ph.D. Dissertation of DAVIDE LENA has been approved by the undersigned members of the dissertation committee as satisfactory for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology.
  • Long Delayed Echo: New Approach to the Problem

    Long Delayed Echo: New Approach to the Problem

    Geometrical joke(r?)s for SETI. R. T. Faizullin OmSTU, Omsk, Russia Since the beginning of radio era long delayed echoes (LDE) were traced. They are the most likely candidates for extraterrestrial communication, the so-called "paradox of Stormer" or "world echo". By LDE we mean a radio signal with a very long delay time and abnormally low energy loss. Unlike the well-known echoes of the delay in 1/7 seconds, the mechanism of which have long been resolved, the delay of radio signals in a second, ten seconds or even minutes is one of the most ancient and intriguing mysteries of physics of the ionosphere. Nowadays it is difficult to imagine that at the beginning of the century any registered echo signal was treated as extraterrestrial communication: “Notable changes occurred at a fixed time and the analogy among the changes and numbers was so clear, that I could not provide any plausible explanation. I'm familiar with natural electrical interference caused by the activity of the Sun, northern lights and telluric currents, but I was sure, as it is possible to be sure in anything, that the interference was not caused by any of common reason. Only after a while it came to me, that the observed interference may occur as the result of conscious activities. I'm overwhelmed by the the feeling, that I may be the first men to hear greetings transmitted from one planet to the other... Despite the signal being weak and unclear it made me certain that soon people, as one, will direct their eyes full of hope and affection towards the sky, overwhelmed by good news: People! We got the message from an unknown and distant planet.