DOCSLIB.ORG

Index of Objects

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Cambridge University Press 978-1-107-00054-4 - Dynamics of Galaxies: Second Edition Giuseppe Bertin Index More information Index of objects Galaxies NGC 3198, 31, 36, 175–6, 178, 255, 276, 283, NGC 221 (= M32), 20, 321, 350 285, 287, 293 NGC 224 (= M31), 4–5, 48, 80, 282–3, 289, NGC 3344, 264 321, 350, 381 NGC 3377, 321 NGC 309, 258, 265, 288 NGC 3379, 32–3, 314, 342, 344, 347, 371, 373, NGC 598 (= M33), 223–4, 381 376, 379, 385–6 NGC 628 (= M74), 23, 174, 259, 261, 265 NGC 3521, 36 NGC 720, 375, 377 NGC 3741, 259 NGC 801, 36, 284 NGC 3923, 386 NGC 821, 379 NGC 3938, 264 NGC 3998, 159 NGC 891, 24, 177, 180, 182 NGC 4013, 276 NGC 936, 264 NGC 4038, 75 NGC 1035, 284 NGC 4039, 75 NGC 1058, 259 NGC 4244, 27 NGC 1068, 445–6 NGC 4254 (= M99), 223–4, 256, 258, 261, 264 NGC 1300, 13, 225, 254, 256 NGC 4258 (= M106), 294, 321–2, 350, 445 NGC 1316, 386 NGC 4278, 378 NGC 1344, 387 NGC 4321 (= M100), 23, 224, 254, 264–5 NGC 1365, 225 NGC 4374, 33, 373, 387, 405–6 NGC 1379, 410–1 NGC 4406, 386 NGC 1399, 351, 373, 376, 379, 385–6, NGC 4472 (= M49), 347, 349–50, 370–3, 375–6, 405–6 379, 385–6, 405–6 NGC 1404, 373, 405–6 NGC 4486 (= M87), 5, 8, 20, 72, 80, 321, 350–1, NGC 1407, 388 376, 379, 385–6 NGC 1549, 22 NGC 4494, 379 NGC 1566, 21 NGC 4550, 37 NGC 1637, 265, 288 NGC 4552, 33, 410–1 NGC 2300, 382 NGC 4559, 177 NGC 2403, 28, 31, 177 NGC 4565, 27 = NGC 2599 ( UGC 4458), 36 NGC 4594 (= M104), 321 NGC 2663, 37 NGC 4596, 264 NGC 2683, 36 NGC 4622, 223, 254, 256–7, 288 NGC 2685, 159 NGC 4636, 5, 373, 375, 379, 385–6, 405–6 NGC 2841, 22 NGC 4649 (= M60), 379, 386 NGC 2859, 253 NGC 4650, 159 NGC 2903,174, 293 NGC 4725, 174 NGC 2915, 259, 261 NGC 4762, 27 NGC 2974, 378 NGC 5018, 37 NGC 2997, 23, 224, 258, 264–5 NGC 5044, 382 NGC 3031 (= M81), 17–8, 22–3, 163, 186, 249, NGC 5055 (= M63), 267 252, 257, 262–4 NGC 5077, 380 NGC 3079, 445–6, 449 NGC 5128 (= Cen A), 352, 379, 386–7 NGC 3108, 379 NGC 5194 (= M51), 12, 27, 224, 252, 255–6, 263–4 NGC 3115, 49, 321 NGC 5195, 224 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-00054-4 - Dynamics of Galaxies: Second Edition Giuseppe Bertin Index More information 456 Index of objects NGC 5236 (= M83), 21, 264 ESO 510-G13, 23 NGC 5266, 379 ESO 603-G21, 159 NGC 5364, 21 NGC 5371, 174 II Zw 73, 159 NGC 5457 (= M101), 23–4, 264–5 Globular clusters NGC 5907, 24, 27, 47 NGC 104 (= 47 Tuc), 336–7, 351 NGC 6946, 23–4, 27, 259–60, NGC 2419, 331, 341 264–5 NGC 5139 (= ω Cen), 337, 351 NGC 7079, 264 NGC 6341 (= M92), 331 NGC 7796, 372, 374 NGC 7078 (= M15), 337 UGC 463, 264, 294 Clusters of galaxies UGC 2259, 292 UGC 2885, 36, 284, 292 Abell 370 (A370), 425 UGC 7321, 177 Abell 496 (A496), 388 UGC 7576, 159 Abell 520 (A520), 296 Abell 1758 (A1758), 434 UGC 12591, 36, 49 Abell 2218 (A2218), 5 Bullet, 15, 296, 375, 384, IC 342, 264 388, 427 IC 2006, 378 Coma, 51, 383, 388, 431 Ring, 296, 388 ESO 199-IG12, 159 Ursa Major, 8, 32, 40–1, 296 ESO 474-G26, 159 Virgo, 5, 8, 10, 20, 23, 46 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-00054-4 - Dynamics of Galaxies: Second Edition Giuseppe Bertin Index More information Index Abel inversion, 166, 316–7 stationary phase, 123, 245 accretion, 14, 24, 177, 392, 403, 405–6 steepest descent, 123 accretion disks, 63, 103, 109, 403, 435–49 two-scale analysis, 165 active disk, 442 atomic deuterium, 16 advection-dominated, 439 atomic hydrogen, 9–10, 12, 16–7, 24, 35, 40, 47, 159, α-disks, 438 177–80, 447 external irradiation, 438, 442, 444–5 21-cm line, 9, 11, 16, 34, 282, 317 and flat rotation curves, 441–2, 445–7 in elliptical galaxies, 55, 104, 377–9, 386, 435, 447 line profiles, 445, 447, 449 and Jeans instability, 12 luminosity, 437 and modeling of the basic state, 86, 162, 173–4, 218 optically thin, 438, 442 and rotation curves, 9, 34–6, 49, 167, 280, 282–3, 285 role of self-gravity, 439–47 in tests of density-wave theory, 17, 257 self-regulated, 439–47 and warps, 24, 266–7, 276 spectral energy distribution, 442–4 atomic nuclei, α decay of, 246 steady-state, 439–47 thickness, 438–9, 441 ballerina effect, 275 transition regions, 441 Balmer lines, 14 action and angle variables, 145, 152, 186, 301 barred spiral structure, 27, 223, 228, 240–1, 249, 288. See active disk, 174, 188, 216, 232, 288 also modes, global: bar active galactic nuclei, 7, 12–4, 18, 403, 435, 438, 445, in the near infrared, 27, 223, 228 adiabatic growth, 72, 290, 402 basic state, 54, 56, 82, 95, 99, 101–2, 113–4, 131–8, linearized equations, 324 162–83 models, 321–5 for disks, 88, 103 adiabatic invariant, 143, 154–5, 157, 223 for elliptical galaxies, 104 adiabatic response, 138, 357 evolution of, 180, 219, 229–30, 243–4, 248, 250, 261, age gradients, 252, 261 280, 287, 305, 313–5, 323–4, 355, 364–7, 391–6, Airy functions, 124 402, 413 Alfv´en resonance, 81, 276 reference, for disk stability analyses, 172–4 Alfv´en velocity, 275 reference, for the problem of dark halos, 175–7 amplitude modulation of spiral arms, 223, 228, 240, BBGKY hierarchy, 85 253, 256 bending waves, 61, 101, 119, 157–8, 184, 265–79 amplitude of spiral structure. See arm-interarm contrast action conservation, 269, 289 (or arm strength) analogy with a flag flapping in the wind, 270, 278, 289 angular-diameter distance, 412, 420, 429 angular-momentum density, 269 anisotropic harmonic oscillator, 304–5, 312 on a current sheet (in the heliosphere), 273–6 anisotropy radius, 339 and disk-halo interaction, 270–2, 278 arm-interarm contrast (or arm strength), 23, 224, 228, group velocity, 269 243, 258, 261, 285 homogeneous slab model, 269–72 asymptotic methods (or analysis), 62, 90–2, 94, 121, 124, inhomogeneous disk, 272–3 190–1, 234, 236, 344, 441 wave packets, 267, 270–1 Laplace integration, 340 wave trains, 269 matched asymptotic expansions (or matching), 91–2, Bessel functions, 170, 189, 193, 221, 237–9 121, 186, 207, 231, 237, 239, 276, 333 Big Bang, 4, 45, 57 ordering, 46, 91–2, 188, 190–1, 207, 219, 232–3, 344 Bohr-Sommerfeld quantum condition, 239 phase-integral, 94, 237 Boltzmann entropy. See entropy functional © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-00054-4 - Dynamics of Galaxies: Second Edition Giuseppe Bertin Index More information 458 Index bounce frequency, 137–8, 164 and statistical mechanics, 394–401 bounce orbit and violent relaxation, 77–8 average, 324, 359 color gradients, 30 expansion, 138 across spiral arms, 252, 261–2 boundary conditions, 62–3, 65, 82, 90–2, 98, 177, 182, comoving coordinates. See Lagrangian coordinates 292, 320, 327, 333, 340–1 (description) for bending modes, 273 compact ellipticals, 20 for bending waves on a current sheet, 276 concordance cosmological model, 10, 46–7, 57 and dispersive waves, 122, 126–8 conspiracy, 35–6, 40–1, 286–7, 348, 408 for global spiral modes, 186–7, 189, 201, 204, 231–3 continuum limit, 58, 64, 72, 84–5, 143, 394 for modes in spherical systems, 360–1, 394 controlled thermonuclear research, 65 for selection of quasi-spherical models, 339–40 convective amplification and damping, 270–1 for a steady cooling flow, 404 cooling flows, 402–8 in two-turning point problem, 234–5, 238, 246 fit for a set of x-ray bright galaxies, 406 boundary layer, 91–2, 437 core radius, 320, 330 Boussinesq equation, 128 Coriolis force, 64, 134 box orbits, 306, 309, 311 corotation boxiness, 21, 33, 38, 335, 344 circle or radius, 149–52, 155, 185, 189, 197–9, 203–6, boxlets, 311 216, 221, 260, 269 Boyle law, 392–3 empirical determination, 252, 256–7, 262–4 bremsstrahlung (free-free emission), 11, 383, 403, 442 for normal and barred modes, 240–2, 248, 253–4 bulge, 7, 21, 23, 29–32, 36, 38, 48, 57, 74, 87–8, 90, 103, resonance, 149–50, 189, 222–3 157–8, 162–3, 167–8, 171–80, 200, 249, 254, 267, turning point, 238–9 283–4, 286, 300, 322, 352 zone or region, 64, 157, 186, 203–6, 231, 235 Burgers equation, 121 corrugations, 23, 266, 276, 355. See also warps cosmic acceleration equation, 46 capture of satellites, 71–4, 365 cosmic age or time, 46, 414 cat’s eyes, 156–7 cosmic background radiation, 9–10, 45–6, 57, 429 causality condition, 128, 135 cosmic chemical composition, 404 cD galaxies, 7, 20, 38, 74, 406 cosmic ether, 45 Cepheid variables, 10, 46 cosmic expansion equation, 46 Cerenkovˇ cone, 129 cosmic rays, 16, 18, 62, 274 Chebyshev polynomials, 305 cosmic shear, 429–30, 433. See also gravitational lensing chemical evolution of galaxies, 14 cosmological constant (). See parameter: cosmological circular velocity, 34, 36, 168, 346, 349, 372, 409, 425, dark energy () circularity function, 317 Coulomb logarithm, 68, 71, 79, 85 circularization of orbits, 71–2, 379 counterrotation, 37, 39, 168 classification of galaxies coupling dynamical, 54, 253–5 of disk and halo, 271 luminosity, 21 of modes, 258 morphology (Hubble), 19–20, 26, 103, 248–9, 254, 391 cross correlation technique, 49 regularity, 22 current sheet, 61 clusters of galaxies, 4–7, 9–10, 15–16, 20, 32, 37–8, in a plasma slab (Harris pinch), 97–9 40–4, 46, 49–51, 56, 74, 104, 280–1, 294, 296, 375, in the heliosphere, 273–6, 279 380–5, 388, 402–8, 418–9, 425–32 cusps coexistence, 27, 243, 249, 251, 254, 257, 262.
Recommended publications
  • Observing Galaxies in Lynx 01 October 2015 22:25

    Observing Galaxies in Lynx 01 October 2015 22:25

    Observing galaxies in Lynx 01 October 2015 22:25 Context As you look towards Lynx you are looking above the galactic plane above the Perseus spiral arm of our galaxy which itself is about 7,000 light years away. The constellation contains a number of brighter galaxies 30 - 50 million light years away and is also relatively rich in galaxies which spread out in to the distance out to over 300 million light years away. The constellation is well placed from early winter to early summer. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 2683 This is a very edge on bright galaxy which I can see in my 100mm binoculars. It is a galaxy which does not seem to be part of a group. NGC 2549 By constellation Page 1 A smaller fainter version of NGC 2683. It was still easy to see with direct vision in my 10 inch reflector. NGC 2537 Near a group of three stars in a row. Quite large looking but with a low surface brightness in my 10 inch scope. NGC 2273 By constellation Page 2 Nice circular galaxy in my 14 inch scope. I could only see the bright core in the above image. NGC 2832 This was a lovely looking galaxy in my 14 inch Dark star scope. As you can see this galaxy is the central galaxy of a group.
  • Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies

    Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies

    The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al.
  • NGC-2683 (The UFO Galaxy) Edge-On Galaxy in Lynx Introduction the Purpose of the Observer’S Challenge Is to Encourage the Pursuit of Visual Observing

    NGC-2683 (The UFO Galaxy) Edge-On Galaxy in Lynx Introduction the Purpose of the Observer’S Challenge Is to Encourage the Pursuit of Visual Observing

    MONTHLY OBSERVER’S CHALLENGE Las Vegas Astronomical Society Compiled by: Roger Ivester, Boiling Springs, North Carolina & Fred Rayworth, Las Vegas, Nevada With special assistance from: Rob Lambert, Las Vegas, Nevada MARCH 2015 NGC-2683 (The UFO Galaxy) Edge-On Galaxy In Lynx Introduction The purpose of the Observer’s Challenge is to encourage the pursuit of visual observing. It’s open to everyone that’s interested, and if you’re able to contribute notes, and/or drawings, we’ll be happy to include them in our monthly summary. We also accept digital imaging. Visual astronomy depends on what’s seen through the eyepiece. Not only does it satisfy an innate curiosity, but it allows the visual observer to discover the beauty and the wonderment of the night sky. Before photography, all observations depended on what the astronomer saw in the eyepiece, and how they recorded their observations. This was done through notes and drawings, and that’s the tradition we’re stressing in the Observers Challenge. We’re not excluding those with an interest in astrophotography, either. Your images and notes are just as welcome. The hope is that you’ll read through these reports and become inspired to take more time at the eyepiece, study each object, and look for those subtle details that you might never have noticed before. NGC-2683 Almost Edge-On Galaxy In Lynx NGC-2683 is also called “The UFO Galaxy.” It was discovered by William Herschel on February 5, 1788. He gave it the designation H-200-1. It lies about 16 to 25 million light-years away and is almost edge-on from our point of view, giving it that narrow, but fat almost streak- like appearance.
  • Magnificent Spiral Galaxy Is Being Stretched by Passing Neighbor 27 May 2021, by Ray Villard

    Magnificent Spiral Galaxy Is Being Stretched by Passing Neighbor 27 May 2021, by Ray Villard

    Magnificent spiral galaxy is being stretched by passing neighbor 27 May 2021, by Ray Villard animals—the gingham dog and calico cat—who got into a spat and ate each other. It's not so dramatic in this case. The galaxies are only getting a little chewed up because of their close proximity. The magnificent spiral galaxy NGC 2276 looks a bit lopsided in this Hubble Space Telescope snapshot. A bright hub of older yellowish stars normally lies directly in the center of most spiral galaxies. But the bulge in NGC 2276 looks offset to the upper left. What's going on? In reality, a neighboring galaxy to the right of NGC 2276 (NGC 2300, not seen here) is gravitationally tugging on its disk of blue stars, pulling the stars on one side of the galaxy outward to distort the galaxy's normal fried-egg appearance. This sort of "tug of war" between galaxies that pass close enough to feel each other's gravitational pull is not uncommon in the universe. But, like Credit: NASA, ESA, STScI, Paul Sell (University of snowflakes, no two close encounters look exactly Florida) alike. In addition, newborn and short-lived massive stars form a bright, blue arm along the upper left edge of The myriad spiral galaxies in our universe almost NGC 2276. They trace out a lane of intense star all look like fried eggs. A central bulge of aging formation. This may have been triggered by a prior stars is like the egg yolk, surrounded by a disk of collision with a dwarf galaxy.
  • THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B

    THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B

    The Astronomical Journal, 128:16–46, 2004 July A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 1000 BRIGHTEST HIPASS GALAXIES: H i PROPERTIES B. S. Koribalski,1 L. Staveley-Smith,1 V. A. Kilborn,1, 2 S. D. Ryder,3 R. C. Kraan-Korteweg,4 E. V. Ryan-Weber,1, 5 R. D. Ekers,1 H. Jerjen,6 P. A. Henning,7 M. E. Putman,8 M. A. Zwaan,5, 9 W. J. G. de Blok,1,10 M. R. Calabretta,1 M. J. Disney,10 R. F. Minchin,10 R. Bhathal,11 P. J. Boyce,10 M. J. Drinkwater,12 K. C. Freeman,6 B. K. Gibson,2 A. J. Green,13 R. F. Haynes,1 S. Juraszek,13 M. J. Kesteven,1 P. M. Knezek,14 S. Mader,1 M. Marquarding,1 M. Meyer,5 J. R. Mould,15 T. Oosterloo,16 J. O’Brien,1,6 R. M. Price,7 E. M. Sadler,13 A. Schro¨der,17 I. M. Stewart,17 F. Stootman,11 M. Waugh,1, 5 B. E. Warren,1, 6 R. L. Webster,5 and A. E. Wright1 Received 2002 October 30; accepted 2004 April 7 ABSTRACT We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 H i brightest galaxies in the southern sky as obtained from the H i Parkes All-Sky Survey (HIPASS). The selection of the brightest sources is basedontheirHi peak flux density (Speak k116 mJy) as measured from the spatially integrated HIPASS spectrum. 7 ; 10 The derived H i masses range from 10 to 4 10 M .
  • Southern Arp - AM # Order

    Southern Arp - AM # Order

    Southern Arp - AM # Order A B C D E F G H I J 1 AM # Constellation Object Name RA DEC Mag. Size Uranom. Uranom. Millenium 2 1st Ed. 2nd Ed. 3 AM 0003-414 Phoenix ESO 293-G034 00h06m19.9s -41d30m00s 13.7 3.2 x 1.0 386 177 430 Vol I 4 AM 0006-340 Sculptor NGC 10 00h08m34.5s -33d51m30s 13.3 2.4 x 1.2 350 159 410 Vol I 5 AM 0007-251 Sculptor NGC 24 00h09m56.5s -24d57m47s 12.4 5.8 x 1.3 305 141 366 Vol I 6 AM 0011-232 Cetus NGC 45 00h14m04.0s -23d10m55s 11.6 8.5 x 5.9 305 141 366 Vol I 7 AM 0027-333 Sculptor NGC 134 00h30m22.0s -33d14m39s 11.4 8.5 x 2.0 351 159 409 Vol I 8 AM 0029-643 Tucana ESO 079- G003 00h32m02.2s -64d15m12s 12.6 2.7 x 0.4 440 204 409 Vol I 9 AM 0031-280B Sculptor NGC 150 00h34m15.5s -27d48m13s 12 3.9 x 1.9 306 141 387 Vol I 10 AM 0031-320 Sculptor NGC 148 00h34m15.5s -31d47m10s 13.3 2 x 0.8 351 159 387 Vol I 11 AM 0033-253 Sculptor IC 1558 00h35m47.1s -25d22m28s 12.6 3.4 x 2.5 306 141 365 Vol I 12 AM 0041-502 Phoenix NGC 238 00h43m25.7s -50d10m58s 13.1 1.9 x 1.6 417 177 449 Vol I 13 AM 0045-314 Sculptor NGC 254 00h47m27.6s -31d25m18s 12.6 2.5 x 1.5 351 176 386 Vol I 14 AM 0050-312 Sculptor NGC 289 00h52m42.3s -31d12m21s 11.7 5.1 x 3.6 351 176 386 Vol I 15 AM 0052-375 Sculptor NGC 300 00h54m53.5s -37d41m04s 9 22 x 16 351 176 408 Vol I 16 AM 0106-803 Hydrus ESO 013- G012 01h07m02.2s -80d18m28s 13.6 2.8 x 0.9 460 214 509 Vol I 17 AM 0105-471 Phoenix IC 1625 01h07m42.6s -46d54m27s 12.9 1.7 x 1.2 387 191 448 Vol I 18 AM 0108-302 Sculptor NGC 418 01h10m35.6s -30d13m17s 13.1 2 x 1.7 352 176 385 Vol I 19 AM 0110-583 Hydrus NGC
  • Spiral Galaxy HI Models, Rotation Curves and Kinematic Classifications

    Spiral Galaxy HI Models, Rotation Curves and Kinematic Classifications

    Spiral galaxy HI models, rotation curves and kinematic classifications Theresa B. V. Wiegert A thesis submitted to the Faculty of Graduate Studies of The University of Manitoba in partial fulfillment of the requirements of the degree of Doctor of Philosophy Department of Physics & Astronomy University of Manitoba Winnipeg, Canada 2010 Copyright (c) 2010 by Theresa B. V. Wiegert Abstract Although galaxy interactions cause dramatic changes, galaxies also continue to form stars and evolve when they are isolated. The dark matter (DM) halo may influence this evolu- tion since it generates the rotational behaviour of galactic disks which could affect local conditions in the gas. Therefore we study neutral hydrogen kinematics of non-interacting, nearby spiral galaxies, characterising their rotation curves (RC) which probe the DM halo; delineating kinematic classes of galaxies; and investigating relations between these classes and galaxy properties such as disk size and star formation rate (SFR). To generate the RCs, we use GalAPAGOS (by J. Fiege). My role was to test and help drive the development of this software, which employs a powerful genetic algorithm, con- straining 23 parameters while using the full 3D data cube as input. The RC is here simply described by a tanh-based function which adequately traces the global RC behaviour. Ex- tensive testing on artificial galaxies show that the kinematic properties of galaxies with inclination > 40 ◦, including edge-on galaxies, are found reliably. Using a hierarchical clustering algorithm on parametrised RCs from 79 galaxies culled from literature generates a preliminary scheme consisting of five classes. These are based on three parameters: maximum rotational velocity, turnover radius and outer slope of the RC.
  • April Constellations of the Month

    April Constellations of the Month

    April Constellations of the Month Leo Small Scope Objects: Name R.A. Decl. Details M65! A large, bright Sa/Sb spiral galaxy. 7.8 x 1.6 arc minutes, magnitude 10.2. Very 11hr 18.9m +13° 05’ (NGC 3623) high surface brighness showing good detail in medium sized ‘scopes. M66! Another bright Sb galaxy, only 21 arc minutes from M65. Slightly brighter at mag. 11hr 20.2m +12° 59’ (NGC 3627) 9.7, measuring 8.0 x 2.5 arc minutes. M95 An easy SBb barred spiral, 4 x 3 arc minutes in size. Magnitude 10.5, with 10hr 44.0m +11° 42’ a bright central core. The bar and outer ring of material will require larger (NGC 3351) aperature and dark skies. M96 Another bright Sb spiral, about 42 arc minutes east of M95, but larger and 10hr 46.8m +11° 49’ (NGC 3368) brighter. 6 x 4 arc minutes, magnitude 10.1. Located about 48 arc minutes NNE of M96. This small elliptical galaxy measures M105 only 2 x 2.1 arc minutes, but at mag. 10.3 has very high surface brightness. 10hr 47.8m +12° 35’ (NGC 3379) Look for NGC 3384! (110NGC) and NGC 3389 (mag 11.0 and 12.2) which form a small triangle with M105. NGC 3384! 10hr 48.3m +12° 38’ See comment for M105. The brightest galaxy in Leo, this Sb/Sc spiral galaxy shines at mag. 9.5. Look for NGC 2903!! 09hr 32.2m +21° 30’ a hazy patch 11 x 4.7 arc minutes in size 1.5° south of l Leonis.
  • The Skyscraper 2009 04.Indd

    The Skyscraper 2009 04.Indd

    A Better Galaxy Guide: Early Spring M67: One of the most ancient open clusters known and Craig Cortis is a great novelty in this regard. Located 1.7° due W of mag NGC 2419: 3.25° SE of mag 6.2 66 Aurigae. Hard to find 4.3 Alpha Cancri. and see; at E end of short row of two mag 7.5 stars. Highly NGC 2775: Located 3.7° ENE of mag 3.1 Zeta Hydrae. significant and worth the effort —may be approximately (Look for “Head of Hydra” first.) 300,000 light years distant and qualify as an extragalactic NGC 2903: Easily found at 1.5° due S of mag 4.3 Lambda cluster. Named the Intergalactic Wanderer. Leonis. NGC 2683: Marks NW “crook” of coathanger-type triangle M95: One of three bright galaxies forming a compact with easy double star mag 4.2 Iota Cancri (which is SSW by triangle, along with M96 and M105. All three can be seen 4.8°) and mag 3.1 Alpha Lyncis (at 6° to the ENE). together in a low power, wide field view. M105 is at the NE tip of triangle, midway between stars 52 and 53 Leonis, mag Object Type R.A. Dec. Mag. Size 5.5 and 5.3 respectively —M95 is at W tip. Lynx NGC 3521: Located 0.5° due E of mag 6.0 62 Leonis. M65: One of a pair of bright galaxies that can be seen in NGC 2419 GC 07h 38.1m +38° 53’ 10.3 4.2’ a wide field view along with M66, which lies just E.
  • Arxiv:2009.04090V2 [Astro-Ph.GA] 14 Sep 2020

    Arxiv:2009.04090V2 [Astro-Ph.GA] 14 Sep 2020

    Research in Astronomy and Astrophysics manuscript no. (LATEX: tikhonov˙Dorado.tex; printed on September 15, 2020; 1:01) Distance to the Dorado galaxy group N.A. Tikhonov1, O.A. Galazutdinova1 Special Astrophysical Observatory, Nizhnij Arkhyz, Karachai-Cherkessian Republic, Russia 369167; [email protected] Abstract Based on the archival images of the Hubble Space Telescope, stellar photometry of the brightest galaxies of the Dorado group:NGC 1433, NGC1533,NGC1566and NGC1672 was carried out. Red giants were found on the obtained CM diagrams and distances to the galaxies were measured using the TRGB method. The obtained values: 14.2±1.2, 15.1±0.9, 14.9 ± 1.0 and 15.9 ± 0.9 Mpc, show that all the named galaxies are located approximately at the same distances and form a scattered group with an average distance D = 15.0 Mpc. It was found that blue and red supergiants are visible in the hydrogen arm between the galaxies NGC1533 and IC2038, and form a ring structure in the lenticular galaxy NGC1533, at a distance of 3.6 kpc from the center. The high metallicity of these stars (Z = 0.02) indicates their origin from NGC1533 gas. Key words: groups of galaxies, Dorado group, stellar photometry of galaxies: TRGB- method, distances to galaxies, galaxies NGC1433, NGC 1533, NGC1566, NGC1672 1 INTRODUCTION arXiv:2009.04090v2 [astro-ph.GA] 14 Sep 2020 A concentration of galaxies of different types and luminosities can be observed in the southern constella- tion Dorado. Among them, Shobbrook (1966) identified 11 galaxies, which, in his opinion, constituted one group, which he called “Dorado”.
  • HST Imaging of the Globular Clusters in the Fornax Cluster: NGC 1379

    HST Imaging of the Globular Clusters in the Fornax Cluster: NGC 1379

    HST Imaging of the Globular Clusters in the Fornax Cluster: NGC 1379 Rebecca A. W. Elson Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK Electronic mail: [email protected] Carl J. Grillmair Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 USA Electronic mail: [email protected] Duncan A. Forbes School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK Electronic mail: [email protected] Mike Rabban Lick Observatory, University of California, Santa Cruz, CA 95064 USA Electronic mail: [email protected] Gerard. M. Williger Goddard Space Flight Center, Greenbelt, MD 20771 USA Electronic mail: [email protected] arXiv:astro-ph/9710041v1 3 Oct 1997 Jean P. Brodie Lick Observatory, University of California, Santa Cruz, CA 95064 USA Electronic mail: [email protected] Received ; accepted –2– ABSTRACT We present B and I photometry for ∼ 300 globular cluster candidates in NGC 1379, an E0 galaxy in the Fornax Cluster. Our data are from both Hubble Space Telescope (HST) and ground-based observations. The HST photometry (B only) is essentially complete and free of foreground/background contamination to ∼ 2 mag fainter than the peak of the globular cluster luminosity function. Fitting a Gaussian to the luminosity function we find hBi = 24.95 ± 0.30 and σB =1.55 ± 0.21. We estimate the total number of globular clusters to be 436 ± 30. To a radius of 70 arcsec we derive a moderate specific frequency, SN =3.5 ± 0.4. At radii r ∼ 3 − 6 kpc the surface density profile of the globular cluster system is indistinguishable from that of the underlying galaxy light.
  • Distances to PHANGS Galaxies: New Tip of the Red Giant Branch Measurements and Adopted Distances

    Distances to PHANGS Galaxies: New Tip of the Red Giant Branch Measurements and Adopted Distances

    MNRAS 501, 3621–3639 (2021) doi:10.1093/mnras/staa3668 Advance Access publication 2020 November 25 Distances to PHANGS galaxies: New tip of the red giant branch measurements and adopted distances Gagandeep S. Anand ,1,2‹† Janice C. Lee,1 Schuyler D. Van Dyk ,1 Adam K. Leroy,3 Erik Rosolowsky ,4 Eva Schinnerer,5 Kirsten Larson,1 Ehsan Kourkchi,2 Kathryn Kreckel ,6 Downloaded from https://academic.oup.com/mnras/article/501/3/3621/6006291 by California Institute of Technology user on 25 January 2021 Fabian Scheuermann,6 Luca Rizzi,7 David Thilker ,8 R. Brent Tully,2 Frank Bigiel,9 Guillermo A. Blanc,10,11 Med´ eric´ Boquien,12 Rupali Chandar,13 Daniel Dale,14 Eric Emsellem,15,16 Sinan Deger,1 Simon C. O. Glover ,17 Kathryn Grasha ,18 Brent Groves,18,19 Ralf S. Klessen ,17,20 J. M. Diederik Kruijssen ,21 Miguel Querejeta,22 Patricia Sanchez-Bl´ azquez,´ 23 Andreas Schruba,24 Jordan Turner ,14 Leonardo Ubeda,25 Thomas G. Williams 5 and Brad Whitmore25 Affiliations are listed at the end of the paper Accepted 2020 November 20. Received 2020 November 13; in original form 2020 August 24 ABSTRACT PHANGS-HST is an ultraviolet-optical imaging survey of 38 spiral galaxies within ∼20 Mpc. Combined with the PHANGS- ALMA, PHANGS-MUSE surveys and other multiwavelength data, the data set will provide an unprecedented look into the connections between young stars, H II regions, and cold molecular gas in these nearby star-forming galaxies. Accurate distances are needed to transform measured observables into physical parameters (e.g.