DOCSLIB.ORG

2MASS, See Two Micron All-Sky Survey Accretion Rings, 80 Active

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
2MASS, See Two Micron All-Sky Survey Accretion Rings, 80 Active 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.
Load more

Recommended publications
  • Arxiv:1312.6769V2
    Infall of nearby galaxies into the Virgo cluster as traced with HST1 Igor. D. Karachentsev Special Astrophysical Observatory RAS, Nizhnij Arkhyz, Karachai-Cherkessian Republic, Russia 369167 [email protected] R. Brent Tully Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA Po-Feng Wu Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA Edward J. Shaya Department of Astronomy, University of Maryland, College Park, MD 20742, USA Andrew E. Dolphin Raytheon Company, 1151 East Hermans Road, Tucson, AZ 85756, USA Received ; accepted arXiv:1312.6769v2 [astro-ph.GA] 13 Jan 2014 –2– ABSTRACT We measured the Tip of the Red Giant Branch distances to nine galaxies in the direction to the Virgo cluster using the Advanced Camera for Surveys on the Hubble Space Telescope. These distances put seven galaxies: GR 34, UGC 7512, NGC 4517, IC 3583, NGC 4600, VCC 2037 and KDG 215 in front of the Virgo, and two galaxies: IC 3023, KDG 177 likely inside the cluster. Distances and radial velocities of the galaxies situated between us and the Virgo core clearly exhibit the infall phenomenon toward the cluster. In the case of spherically symmetric radial infall we estimate the radius of the “zero-velocity surface” to be (7.2±0.7) 14 Mpc that yields the total mass of the Virgo cluster to be (8.0 ± 2.3) × 10 M⊙ in good agreement with its virial mass estimates. We conclude that the Virgo outskirts does not contain significant amounts of dark matter beyond its virial radius. 1. Introduction In the standard ΛCDM cosmological model groups and clusters are built from the merging of already formed galaxies embedded in massive dark haloes (White & Rees, 1978).
    [Show full text]
  • CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
    Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1,
    [Show full text]
  • Li Abundances in F Stars: Planets, Rotation, and Galactic Evolution,
    A&A 576, A69 (2015) Astronomy DOI: 10.1051/0004-6361/201425433 & c ESO 2015 Astrophysics Li abundances in F stars: planets, rotation, and Galactic evolution, E. Delgado Mena1,2, S. Bertrán de Lis3,4, V. Zh. Adibekyan1,2,S.G.Sousa1,2,P.Figueira1,2, A. Mortier6, J. I. González Hernández3,4,M.Tsantaki1,2,3, G. Israelian3,4, and N. C. Santos1,2,5 1 Centro de Astrofisica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal 3 Instituto de Astrofísica de Canarias, C/via Lactea, s/n, 38200 La Laguna, Tenerife, Spain 4 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 5 Departamento de Física e Astronomía, Faculdade de Ciências, Universidade do Porto, Portugal 6 SUPA, School of Physics and Astronomy, University of St. Andrews, St. Andrews KY16 9SS, UK Received 28 November 2014 / Accepted 14 December 2014 ABSTRACT Aims. We aim, on the one hand, to study the possible differences of Li abundances between planet hosts and stars without detected planets at effective temperatures hotter than the Sun, and on the other hand, to explore the Li dip and the evolution of Li at high metallicities. Methods. We present lithium abundances for 353 main sequence stars with and without planets in the Teff range 5900–7200 K. We observed 265 stars of our sample with HARPS spectrograph during different planets search programs. We observed the remaining targets with a variety of high-resolution spectrographs.
    [Show full text]
  • Guide Du Ciel Profond
    Guide du ciel profond Olivier PETIT 8 mai 2004 2 Introduction hjjdfhgf ghjfghfd fg hdfjgdf gfdhfdk dfkgfd fghfkg fdkg fhdkg fkg kfghfhk Table des mati`eres I Objets par constellation 21 1 Androm`ede (And) Andromeda 23 1.1 Messier 31 (La grande Galaxie d'Androm`ede) . 25 1.2 Messier 32 . 27 1.3 Messier 110 . 29 1.4 NGC 404 . 31 1.5 NGC 752 . 33 1.6 NGC 891 . 35 1.7 NGC 7640 . 37 1.8 NGC 7662 (La boule de neige bleue) . 39 2 La Machine pneumatique (Ant) Antlia 41 2.1 NGC 2997 . 43 3 le Verseau (Aqr) Aquarius 45 3.1 Messier 2 . 47 3.2 Messier 72 . 49 3.3 Messier 73 . 51 3.4 NGC 7009 (La n¶ebuleuse Saturne) . 53 3.5 NGC 7293 (La n¶ebuleuse de l'h¶elice) . 56 3.6 NGC 7492 . 58 3.7 NGC 7606 . 60 3.8 Cederblad 211 (N¶ebuleuse de R Aquarii) . 62 4 l'Aigle (Aql) Aquila 63 4.1 NGC 6709 . 65 4.2 NGC 6741 . 67 4.3 NGC 6751 (La n¶ebuleuse de l’œil flou) . 69 4.4 NGC 6760 . 71 4.5 NGC 6781 (Le nid de l'Aigle ) . 73 TABLE DES MATIERES` 5 4.6 NGC 6790 . 75 4.7 NGC 6804 . 77 4.8 Barnard 142-143 (La tani`ere noire) . 79 5 le B¶elier (Ari) Aries 81 5.1 NGC 772 . 83 6 le Cocher (Aur) Auriga 85 6.1 Messier 36 . 87 6.2 Messier 37 . 89 6.3 Messier 38 .
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • Report of Contributions
    Mapping the X-ray Sky with SRG: First Results from eROSITA and ART-XC Report of Contributions https://events.mpe.mpg.de/e/SRG2020 Mapping the X- … / Report of Contributions eROSITA discovery of a new AGN … Contribution ID : 4 Type : Oral Presentation eROSITA discovery of a new AGN state in 1H0707-495 Tuesday, 17 March 2020 17:45 (15) One of the most prominent AGNs, the ultrasoft Narrow-Line Seyfert 1 Galaxy 1H0707-495, has been observed with eROSITA as one of the first CAL/PV observations on October 13, 2019 for about 60.000 seconds. 1H 0707-495 is a highly variable AGN, with a complex, steep X-ray spectrum, which has been the subject of intense study with XMM-Newton in the past. 1H0707-495 entered an historical low hard flux state, first detected with eROSITA, never seen before in the 20 years of XMM-Newton observations. In addition ultra-soft emission with a variability factor of about 100 has been detected for the first time in the eROSITA light curves. We discuss fast spectral transitions between the cool and a hot phase of the accretion flow in the very strong GR regime as a physical model for 1H0707-495, and provide tests on previously discussed models. Presenter status Senior eROSITA consortium member Primary author(s) : Prof. BOLLER, Thomas (MPE); Prof. NANDRA, Kirpal (MPE Garching); Dr LIU, Teng (MPE Garching); MERLONI, Andrea; Dr DAUSER, Thomas (FAU Nürnberg); Dr RAU, Arne (MPE Garching); Dr BUCHNER, Johannes (MPE); Dr FREYBERG, Michael (MPE) Presenter(s) : Prof. BOLLER, Thomas (MPE) Session Classification : AGN physics, variability, clustering October 3, 2021 Page 1 Mapping the X- … / Report of Contributions X-ray emission from warm-hot int … Contribution ID : 9 Type : Poster X-ray emission from warm-hot intergalactic medium: the role of resonantly scattered cosmic X-ray background We revisit calculations of the X-ray emission from warm-hot intergalactic medium (WHIM) with particular focus on contribution from the resonantly scattered cosmic X-ray background (CXB).
    [Show full text]
  • National Observatories
    Sidney C Wolff NOAO/DIR NATIONAL OPTICAL ASTRONOMY OBSERVATORIES NATIONAL OPTICAL ASTRONOMY OBSERVATORIES Cerro Tololo Inter-American Observatory Kitt Peak National Observatory National Solar Observatory La Serena, Chile Tucson, Arizona 85726 Sunspot, New Mexico 88349 ANNUAL REPORT October 1996 - September 1997 October 30,1997 TABLE OF CONTENTS L INTRODUCTION IL AURA BOARD m. SCffiNTDJIC PROGRAM A. Cerro Tololo Inter-American Observatory (CTIO) 1. The Search for High Z Supernovae 2. Nearby Stars and Planets 2 B. Kitt Peak National Observatory (KPNO) 3 1. The History of Star Formation in Distant Galaxies 3 2. Oxygen Abundance and the Age of the Universe 4 3. The Age of Elliptical Galaxies - Is There Enough Time? 5 C. National Solar Observatory (NSO) 5 1. Results from GONG 5 2. High-Resolution Images of Solar Magnetic Fields 6 3. Active Optics Control Loop Closed at the Sac Peak Vacuum Tower Telescope 7 IV. DIVISION OPERATIONS 7 A. CTIO 7 Telescope Upgrades and Instrumentation 7 1. 4-m Upgrades 8 2. Major Instrumentation Efforts 9 3. SOAR 4-m Telescope Project 9 4. CCD Implementation and ARCON Controller Development 10 5. Existing Small General-User Telescopes on Cerro Tololo 10 6. New "Tenant" Installations and Upgrades 10 7. Other 11 B. KPNO 12 1. Image Quality Improvements 12 2. WTYN Queue Observing Experiment 12 3. WTYN 13 4. KPNO Instrumentation Improvements 14 5. Burrell-Schmidt 14 C. NSO 15 1. Kitt Peak 15 2. Sacramento Peak 17 3. Digital Library Development 21 D. USGP/ScOpe 21 E. NOAO Instrumentation 25 1. CCD Mosaic Imager 26 2.
    [Show full text]
  • A Spectroscopic Study of the Giant Low Surface Brightness Galaxy Malin 1
    1 BlueMUSE Science workshop A spectroscopic study of the giant low surface brightness galaxy Malin 1 Junais Samuel Boissier Collaborators : Philippe Amram Benoit Epinat Alessandro Boselli Barry Madore Jin Koda Armando Gil de Paz J.C Muñoz-Mateos Laurent Chemin 10 November 2020 2 Low Surface Brightness Galaxies (LSBs) • Historical definition of LSBs based on disk central surface brightness (Freeman 1970): Bothun et al. (1997) 3 Low Surface Brightness Galaxies (LSBs) • Historical definition of LSBs based on disk central surface brightness (Freeman 1970): • LSBs may account up to 50% of all the galaxies in the universe (Impey & Bothun 1997, Martin et al. 2019) Bothun et al. (1997) 4 Low Surface Brightness Galaxies (LSBs) • In recent years, with powerful instruments (e.g. MUSE, Megacam, Dragonfly), there is a new interest in these sources. • LSBs also similar to galaxies with eXtended UV disk (XUV) (Thilker et al. 2007) • Ideal laboratories for the study of Star Formation activities in low density regime • Important to study this large population of galaxies • Their properties may redefine our knowledge of galaxy formation & evolution M83 with an XUV Disk 5 Low Surface Brightness Definitions • « Historical definition » (Freeman 1970) Diffuse galaxies Disk central surface brightness LSB • « Diffuse galaxies » (Sprayberry+1995) • « Ultra Diffuse Galaxies » (Koda+ 2015) UDG Hagen et al. (2016) 6 Low Surface Brightness Definitions • « Historical definition » (Freeman 1970) Diffuse galaxies Disk central surface brightness LSB • « Diffuse galaxies » (Sprayberry+1995) • « Ultra Diffuse Galaxies » (Koda+ 2015) UDG Malin 1 Hagen et al. (2016) MALIN 1 77 An extreme case of LSB !! Malin 1 image credits : NGVS u, g, i MALIN 1 88 Bothun et al.
    [Show full text]
  • The Extragalactic Distance Scale
    The Extragalactic Distance Scale Published in "Stellar astrophysics for the local group" : VIII Canary Islands Winter School of Astrophysics. Edited by A. Aparicio, A. Herrero, and F. Sanchez. Cambridge ; New York : Cambridge University Press, 1998 Calibration of the Extragalactic Distance Scale By BARRY F. MADORE1, WENDY L. FREEDMAN2 1NASA/IPAC Extragalactic Database, Infrared Processing & Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA 2Observatories, Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena CA 91101, USA The calibration and use of Cepheids as primary distance indicators is reviewed in the context of the extragalactic distance scale. Comparison is made with the independently calibrated Population II distance scale and found to be consistent at the 10% level. The combined use of ground-based facilities and the Hubble Space Telescope now allow for the application of the Cepheid Period-Luminosity relation out to distances in excess of 20 Mpc. Calibration of secondary distance indicators and the direct determination of distances to galaxies in the field as well as in the Virgo and Fornax clusters allows for multiple paths to the determination of the absolute rate of the expansion of the Universe parameterized by the Hubble constant. At this point in the reduction and analysis of Key Project galaxies H0 = 72km/ sec/Mpc ± 2 (random) ± 12 [systematic]. Table of Contents INTRODUCTION TO THE LECTURES CEPHEIDS BRIEF SUMMARY OF THE OBSERVED PROPERTIES OF CEPHEID
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]