DOCSLIB.ORG

Fellows at ESO

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Fellows at ESO Other Astronomical News Fellows at ESO Rubina Kotak pher the physics of thermonuclear super- novae (SNe). Partly as a result of the Although I spent the first two years of my numerous side-projects that sprouted out life in the south-western corner of Tanza- of this, two of my current preoccupa- nia, I grew up near the equator, in Ken- tions are the characterisation and use of Photo: G. Dremel, ESO ya. Having obtained my Masters degree circumstellar matter surrounding SNe from Canterbury (Kent), I decided that to determine the nature of the progenitor it was time to venture somewhere a little star(s), and whether core-collapse SNe more exotic. Hence I moved north, to are able to produce significant quantities southern Sweden to start a PhD at Lund of dust at all redshifts. Observatory. I arrived at ESO-Garching less than a Here I worked on time-resolved spectros- year ago and am still negotiating my way copy of cool white dwarf pulsators with a around the intriguing maze of corridors, view to simultaneously tapping their as- doors, and dead ends, making navigation teroseismological potential and constrain- using images e.g. of the Horsehead ing the properties of the convection zone Nebula, a necessity! My duties at ESO in- Rubina Kotak in a novel way. Having (temporarily) ex- clude working in the PR department hausted all the targets that could be ob- which is both fun and stimulating. Being served in this way, using the largest at ESO gives that child-in-a-sweetshop come. My time at ESO is sadly coming (optical) telescope on the planet, it was feeling: lots of interesting talks, experts in to an end, but I’m looking forward to tak- time to move on. So I found myself at every field, and a general feeling of be- ing up a staff positon at Queen’s Uni- Imperial College London, working as part ing at the hub of events and decisions versity Belfast. Definitely time to invest in of a concerted European effort to deci- that will shape the future for decades to umbrellas! The Starburst Galaxy NGC 908. Im- age based on data obtained with FORS2 on the VLT, using B, V, and R filters. North is up and East is to the left. The data were extracted from the ESO Science Archive and further processed by Henri Boffin (ESO). More information can be found in ESO PR Photo 27a/06. Corrigendum The caption of the second photo in the re- port on the Walloon Space Days in the last issue of The Messenger mentioned Mme Simonet, Minister for Science, New Technolo- gies and External Relations of the Walloon Re- Photo: S. Tarquinio, AMOS gional Government, while the photo showed Dr. Monnik Desmeth, Belgian delegate and Vice President of the ESO Council. The picture here shows Mme Simonet at the press con- ference at AMOS. 58 The Messenger 125 – September 2006.
Load more

Recommended publications
  • Lopsided Spiral Galaxies: Evidence for Gas Accretion
    A&A 438, 507–520 (2005) Astronomy DOI: 10.1051/0004-6361:20052631 & c ESO 2005 Astrophysics Lopsided spiral galaxies: evidence for gas accretion F. Bournaud1, F. Combes1,C.J.Jog2, and I. Puerari3 1 Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France e-mail: [email protected] 2 Department of Physics, Indian Institute of Science, Bangalore 560012, India 3 Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1, 72840 Tonantzintla, Puebla, Mexico Received 3 January 2005 / Accepted 15 March 2005 Abstract. We quantify the degree of lopsidedness for a sample of 149 galaxies observed in the near-infrared from the OSUBGS sample, and try to explain the physical origin of the observed disk lopsidedness. We confirm previous studies, but for a larger sample, that a large fraction of galaxies have significant lopsidedness in their stellar disks, measured as the Fourier amplitude of the m = 1 component normalised to the average or m = 0 component in the surface density. Late-type galaxies are found to be more lopsided, while the presence of m = 2 spiral arms and bars is correlated with disk lopsidedness. We also show that the m = 1 amplitude is uncorrelated with the presence of companions. Numerical simulations were carried out to study the generation of m = 1viadifferent processes: galaxy tidal encounters, galaxy mergers, and external gas accretion with subsequent star formation. These simulations show that galaxy interactions and mergers can trigger strong lopsidedness, but do not explain several independent statistical properties of observed galaxies. To explain all the observational results, it is required that a large fraction of lopsidedness results from cosmological accretion of gas on galactic disks, which can create strongly lopsided disks when this accretion is asymmetrical enough.
    [Show full text]
  • Making a Sky Atlas
    Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it.
    [Show full text]
  • Ngc Catalogue Ngc Catalogue
    NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39
    [Show full text]
  • Constraining Dark Matter Halo Profiles and Galaxy Formation Models Using
    Draft version January 8, 2018 A Preprint typeset using LTEX style emulateapj v. 5/2/11 CONSTRAINING DARK MATTER HALO PROFILES AND GALAXY FORMATION MODELS USING SPIRAL ARM MORPHOLOGY. II. DARK AND STELLAR MASS CONCENTRATIONS FOR 13 NEARBY FACE-ON GALAXIES Marc S. Seigar1,2, Benjamin L. Davis3, Joel Berrier3,4,5, and Daniel Kennefick3,4 Draft version January 8, 2018 ABSTRACT We investigate the use of spiral arm pitch angles as a probe of disk galaxy mass profiles. We confirm our previous result that spiral arm pitch angles (P) are well correlated with the rate of shear (S) in disk galaxy rotation curves. We use this correlation to argue that imaging data alone can provide a powerful probe of galactic mass distributions out to large look-back times. We then use a sample of 13 galaxies, with Spitzer 3.6-µm imaging data and observed Hα rotation curves, to demonstrate how an inferred shear rate coupled with a bulge-disk decomposition model and a Tully-Fisher-derived velocity normalization can be used to place constraints on a galaxy’s baryon fraction and dark matter halo profile. Finally we show that there appears to be a trend (albeit a weak correlation) between spiral arm pitch angle and halo concentration. We discuss implications for the suggested link between supermassive black hole (SMBH) mass and dark halo concentration, using pitch angle as a proxy for SMBH mass. Subject headings: dark matter — galaxies: fundamental parameters — galaxies: halos — galaxies: kinematics and dynamics — galaxies: spiral — galaxies: structure 1. INTRODUCTION of most spiral density wave models (e.g.
    [Show full text]
  • A Classical Morphological Analysis of Galaxies in the Spitzer Survey Of
    Accepted for publication in the Astrophysical Journal Supplement Series A Preprint typeset using LTEX style emulateapj v. 03/07/07 A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Ronald J. Buta1, Kartik Sheth2, E. Athanassoula3, A. Bosma3, Johan H. Knapen4,5, Eija Laurikainen6,7, Heikki Salo6, Debra Elmegreen8, Luis C. Ho9,10,11, Dennis Zaritsky12, Helene Courtois13,14, Joannah L. Hinz12, Juan-Carlos Munoz-Mateos˜ 2,15, Taehyun Kim2,15,16, Michael W. Regan17, Dimitri A. Gadotti15, Armando Gil de Paz18, Jarkko Laine6, Kar´ın Menendez-Delmestre´ 19, Sebastien´ Comeron´ 6,7, Santiago Erroz Ferrer4,5, Mark Seibert20, Trisha Mizusawa2,21, Benne Holwerda22, Barry F. Madore20 Accepted for publication in the Astrophysical Journal Supplement Series ABSTRACT The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im.
    [Show full text]
  • Constraining Spiral Galaxy Mass Distributions with the Rss Imaging Spectroscopy Nearby Galaxy Survey
    CONSTRAINING SPIRAL GALAXY MASS DISTRIBUTIONS WITH THE RSS IMAGING SPECTROSCOPY NEARBY GALAXY SURVEY By CARL J. MITCHELL A dissertation submitted to the Graduate School|New Brunswick Rutgers, The State University of New Jersey in partial fulfillment of the requirements for the degree of Doctor of Philosophy Graduate Program in Physics and Astronomy written under the direction of J. A. Sellwood and approved by New Brunswick, New Jersey October, 2017 ABSTRACT OF THE DISSERTATION Constraining Spiral Galaxy Mass Distributions with the RSS Imaging Spectroscopy Nearby Galaxy Survey By CARL J. MITCHELL Dissertation Director: J. A. Sellwood Kinematic measurements of galaxies provide a way to trace their mass distributions. The RSS Imaging spectroscopy Nearby Galaxy Survey (RINGS) was designed to probe the mass distributions of 19 spiral galaxies on small spatial scales by obtaining a suite of multi-wavelength kinematic and photometric data. In this dissertation, I introduce the high-spatial-resolution, medium-spectral-resolution Hα kinematic portion of the survey, and detail the process which has been used to convert the raw Fabry-P´erotobservations into useful kinematic data and models. These Hα kinematic data were obtained with the Robert Stobie Spectrograph (RSS) at the Southern African Large Telescope (SALT). I then demon- strate how these Hα kinematic data can be combined with the other types of observations in RINGS, H I radio interferometry and broadband photometric imaging, to probe these galaxies' mass distributions. ii Acknowledgments This work would not have been possible without the contributions of a number of other people. First and foremost, I must thank Jerry Sellwood for providing me with his support and insight over the last several years.
    [Show full text]
  • Daily Relative Sunspot Numbers and Sunspot Areas
    DAILY RELATIVE SUNSPOT NUMBERS AND SUNSPOT AREAS JULY 2006 Relative-Numbers Sunspot Areas Drawing Day Gro. N.H. S.H. Sum N.H. S.H. Sum 1 2 11 15 26 6 323 329 2 - - - - - - - 3 - - - - - - - 4 2 9 16 24 557 4 561 5 2 0 21 21 448 69 517 6 2 0 27 27 0 498 498 7 2 0 25 25 0 316 316 8 2 0 28 28 0 392 392 9 2 0 21 21 0 302 302 10 1 0 10 10 0 17 17 11 1 0 10 10 0 13 13 12 1 0 13 13 0 13 13 13 1 0 10 10 0 7 7 14 4 0 33 33 0 17 17 15 1 0 10 10 0 6 6 16 1 0 11 11 0 10 10 17 1 0 15 15 0 17 17 18 1 0 18 18 0 21 21 19 1 0 19 19 0 33 33 20 - - - - - - - 21 1 0 10 10 0 6 6 22 1 8 0 8 30 0 30 23 1 11 0 11 43 0 43 24 - - - - - - - 25 1 16 0 16 78 0 78 26 1 20 0 20 65 0 65 27 1 21 0 21 58 0 58 28 1 20 0 20 44 0 44 29 2 21 9 30 42 2 44 30 2 17 8 25 19 12 31 31 4 27 19 46 19 17 36 Mean 6.7 12.9 19.6 52.2 77.6 129.8 1 DAILY SUNSPOT OBSERVATIONS JULY 2006 CMP Corre.
    [Show full text]
  • Dark and Luminous Matter in Bright Spiral Galaxies
    Dark and Luminous Matter in Bright Spiral Galaxies DISSERTATION Presented in Partial Ful¯llment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Susan Alice Joan Kassin ***** The Ohio State University 2004 Dissertation Committee: Approved by Professor Richard Pogge, Adviser Professor Bradley Peterson Adviser Astronomy Graduate Program Professor Christopher Kochanek Professor Jay Frogel ABSTRACT I present photometrically calibrated images and surface photometry in the B; V; R; J; H; and K-bands of 26, and in the g, r, and K-bands of 5 nearby bright o (BT < 12:5 mag) spiral galaxies with inclinations between 30{65 degrees spanning the Hubble Sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey, the Two Micron All Sky Survey, and the Sloan Digital Sky Survey Second Data Release. Radial surface brightness pro¯les are extracted, and integrated magnitudes are measured from the pro¯les. Axis ratios, position angles, and scale lengths are measured from the near-infrared. A 1-dimensional bulge/disk decomposition is performed on galaxies with a non-negligable bulge component. Radial stellar mass distributions are estimated by applying color-M=L relations derived from spectrophotometric spiral galaxy evolution models to the photometry. When available, radial gas masses are added to the radial stellar mass distributions to produce radial baryonic mass distributions. For each galaxy, a rotation curve due to its radial baryonic mass distribution is calculated, taking into account both the bulge and disk components when necessary. All of the galaxies have high-quality ii rotation curves available in the literature which allows us to calculate radial dark matter distributions for each galaxy by comparison with the baryonic mass rotation curves.
    [Show full text]
  • 2019 Gone Fishin’ – Observing List Notes
    The Eldorado Star Party 2019 Telescope Observing Club by Bill Flanagan Houston Astronomical Society Purpose and Rules Welcome to the Annual ESP Telescope Club! The main purpose of this club is to give you an opportunity to observe some of the showpiece objects of the fall season under the pristine skies of Southwest Texas. We have also included a few items on the observing lists that may challenge you to observe some fainter and more obscure objects that present themselves at their very best under the dark skies of the Eldorado Star Party. The rules are simple; just observe the required number of objects listed while you are at the Eldorado Star Party to receive a club badge. Gone Fishin’ West Texas may be known for its dry climate and dry river beds, but in the fall after the sun goes down, the night skies over X-Bar Ranch provide an excellent opportunity to go fishing. Pisces (the Fish) and Pisces Austrinus (the Southern Fish) can be reeled in during most of the night. Delphinus (the Dolphin) is high in the sky just after sunset. The constellation Eridanus (the River) winds its way through the southern portion of the sky, and Cetus (the Sea Monster) can be seen dipping his front flippers into this magnificent winding river. So given this great fall opportunity, the Telescope Observing Club program for the 2019 Eldorado Star Party is “Gone Fishin’.” The program is a list of 27 objects located in the five above mentioned constellations. You only have to reel in 22 of the 27 objects on the list with a telescope to qualify for the Telescope Observing Club badge.
    [Show full text]
  • Marketing Fragment 8.5 X 12.T65
    Cambridge University Press 978-0-521-85893-9 - Steve O’Meara’s Herschel 400 Observing Guide Steve O’Meara Index More information Index Ancient City Astronomy Club (ACAC), ix , Aquila NGC 5195 (H I-186), 194 4 , 5 specific objects in NGC 5273 (H I-98), 193 asterisms NGC 6755 (H VII-19), 248 Canis Major Coathanger, 252 NGC 6756 (H VII-62), 249 specific objects in Kemble’s Cascade, 35 , 36 NGC 6781 (H III-743), 249 NGC 2204 (H VII-13), 48 M73, 267 Aries NGC 2354 (H VII-16), 48 Astronomical League (AL), ix specific objects in NGC 2360 (H VII-12), 49 Herschel 400 certificates, ix NGC 772 (H I-112), 309 NGC 2362 (H VII-17), 49 Auriga Cassiopeia Barbuy, B., 240 specific objects in specific objects in Bayer, Johann NGC 1644 (H VIII-59), 22 NGC 129 (H VIII-79), 292 and Greek letters for stars, 10 NGC 1857 (H VII-33), 24 NGC 136 (H VI-35), 292 Bernoulli, J., 141 , 181 , 216 NGC 1907 (H VII-39), 24 NGC 185 (H II-707), 287 Bica, E., 240 NGC 1931 (H I-261), 25 NGC 225 (H VIII-78), 293 Blinking Planetary Nebula (see NGC 2126 (H VIII-68), 22 NGC 278 (H I-159), 288 NGC 6826) NGC 2281 (H VIII-71), 25 NGC 381 (H VIII-64), 293 Box Galaxy (see NGC 4449) Bootes NGC 436 (H VII-45), 295 bright nebulae specific objects in NGC 457 (H VII-42), 295 definition of, 5 NGC 5248 (H I-34), 197 NGC 559 (H VII-48), 296 specific objects NGC 5466 (H VI-9), 212 NGC 637 (H VII-49), 296 M8, 241 NGC 5557 (H I-99), 212 NGC 654 (H VII-46), 298 M27, 252 NGC 5676 (H I-189), 209 NGC 659 (H VIII-65), 297 NGC 1788 (H V-32), 30 NGC 5689 (H I-188), 209 NGC 663 (H VI-31), 298 NGC 1931
    [Show full text]
  • 2018 ANNUAL PROGRESS REPORT of the GEMINI OBSERVATORY Table of Contents
    2018 ANNUAL PROGRESS REPORT OF THE GEMINI OBSERVATORY Table of Contents 1 Introduction & Science Highlights ..................................................................................................... 1 1.1 Introduction .................................................................................................................................. 1 1.2 Science Highlights ......................................................................................................................... 2 1.3 Proposal and Publication Statistics ............................................................................................... 8 2 Finance & Staffing ............................................................................................................................. 9 2.1 Finance .......................................................................................................................................... 9 2.2 Budget ........................................................................................................................................... 9 2.2.1 Partner Contributions ........................................................................................................... 9 2.2.2 Financial Results for the Year 2018 ..................................................................................... 10 2.2.3 O&M 2018 Budget vs Actual Variance Analysis .................................................................. 11 2.3 Organization and Staffing ..........................................................................................................
    [Show full text]
  • Marketing Fragment 7.5 X 12.T65
    Cambridge University Press 978-0-521-83704-0 - Deep-Sky Companions: Hidden Treasures Stephen James O'Meara Index More information Index A View from a Distant Star,227 NGC6873 inNGC 1365, 100 Abell 779,238 SailofCorvus, 305 inNGC 2655,241 Acker, Agnes, 6 Astro-1, 126 inNGC 4699, 342 Aitken, Robert Grant, 321 Astro-2 Spacelab, 295 inNGC5746, 369 Albino Butterfly Nebula Astronomy with an Opera-Glass,85 inNGC6503, 424 (NGC 2440), 204 AsymptoticGiant Branch (AGB) Black Swallowtail ButterflyCluster Albuquerque AstronomicalSociety, Stars, 40, 516 (IC 4665), 414, 416 371 Aunt Margaret’sMirror (Hidden Blade and Pearl Galaxy (NGC5746), Alessi, Bruno, 533 Treasure 29), 146, 149 368 Alessi J23407 +0757 (O’Meara1), Auwers, Arthur, 184, 423,425 Block, Eugen, 95, 110 530–534 Avery, Captain, 197 Blue Oyster Nebula, 120 Alexander, P., 316 Avery’sIsland (NGC 2353), 197 Bok, Bart, 166 al-Firuzabadi, 84, 85, 147 Bok Globules, 28, 166 AlHalbah(Coma Berenices), 310 Bailey, Solon Irving,253,414, 459 Bond, GeorgePhillips, 541 Allen, D.A., 90 Balick, Bruce, 322, 419 Bond’sGalaxy (NGC 7793), 541 Allen, Richard H., 169, 500 Balloon and Gondola, 31 Bonn Observatory,89 Allen, Richard Hinckley, 5, 33, 106, Barnard 30, 148 Bonner Durchmusterung,89 223 Barnard 33, 171 Bower, Gary, 342, 369 Aller, Lawrence, 322, 391, 448, 490 Barnard 77, 404, 406 Box Nebula (NGC6445), 419,421 Alonso–Herrero, Almudena,258 Barnard 78(Pipe Nebula), 404 Brahe, Tycho, 310 Alpha Persei MovingCluster Barnard 86 Brakel, Albert, 254 (Melotte 20), 83,85, 131 Barnard 160, 523 Branchett, D., 19,23
    [Show full text]