April, 2005 Observer

Total Page:16

File Type:pdf, Size:1020Kb

April, 2005 Observer Fort Bend Astronomy Club P.O. Box 942 Stafford, TX 77497- 0942 The FBAC Observer Volume 19, Issue 4 April, 2005 The CCD Chronicles Wes Whiddon A while back there was considerable discus- Astronomy or Sky and Tel one day when I stumbled on sion on Netslyder and in personal conversations about in- the SBIG page featuring the ST-237A camera. As I sat dividuals using the club’s ST-7 camera outside the con- there on the throne (and most of you know which one I fines of the dome. Some of us seem to be for it and oth- mean), I realized I could buy a good CCD camera with ers against it. A great deal of talk against outside use color filter wheel for less than a king’s ransom. Remem- came from the notion that imaging is a difficult thing to ber, I was sitting on the throne at the time so I made, after do and operation of a CCD camera requires great perse- consulting the other half of the monarchy, a decision to verance and superior intellect to accomplish. Since I dis- buy one. In due course, I found myself standing in front agree with this assumption, (especially about the intellect of the counter at Land, Sea, and Sky, check book in hand, part because, after all, I can do it), I would like to offer, in purchasing an ST-237A complete with color filter wheel. a series of articles, my experience—limited as it is—as an While I was waiting for the tape to stop winding out of operator of a CCD camera. Notice I say operator, not the cash register and for the sales clerk to stop licking his imager, because, even though I’ve used several different lips, visions of astronomical objects in all their glory CCD and video cameras over the course of the last few floated before my eyes. Colorful images of Andromeda, years, I still can’t produce the kind of images you see the Whirlpool, and Orion floated in inky black space every month in the back of Sky and Telescope and As- filled with pinpoint stars. Darkness would fall, the heav- tronomy magazines or when you look at Randy Brewer’s ens were waiting, and I would be their master. I was soon web site. And by the way, I won’t even attempt to get to learn there is much disappointment to be found when you anywhere near the le vel of imaging that someone like darkness falls. Randy has reached. Imagers like him are in a league of Anticipation is one of our base human emotions. their own for reasons I will discuss la ter. But, laying all And since a lot of us have evolved, over the past few dec- that aside, I think I can dispel the idea that imaging is ades, into technocrats, we can’t wait to get our hands on a hard to do. So, lets get started. new gadget. I raced home with my camera, hurried First though, I give to you a warning and then a through the back door, slipped my penknife along the story. CCD imaging is not rocket science but, like any- tape securing the box, threw back the flaps on the box, thing worthwhile, it takes practice. Notice that in the and there it was in it’s neat little foam rubber cocoon, in- paragraph preceding this one, I did not completely deny ert now but soon to come to life and convert ancient and that it takes perseverance. Practice makes perfect and im- invisible photons into electrons and back into photons for aging is no exception. When I first started out, my efforts my viewing pleasure. were hit and miss because I didn’t develop a plan for I was anxious to get started so as soon as twilight practicing things like focusing, exposure control, learning came, I drug my Celestar 8 out into the backyard, found software, and other essentials that go with CCDing. To Polaris in the light polluted skies, polar aligned as best I heck with the preliminaries, I wanted to take pretty pic- could, set up the camera, and attached it to the back of the tures. It didn’t take long for me to realize that failure was scope. Seconds later I began to realize that the scope did- just around the corner. n’t like this much weight on its tail and it promptly began To this day I don’t remember exactly when and to sag backwards. I tightened up the declination bands on why I decided to begin electronic imaging. I tried using the scope and it seemed OK. By then I saw a sprinkling film a few times but light pollution doesn’t treat film of stars around the sky so I slewed over to a bright one, kindly, turning the sky a ghastly kind of green in most cranked up the camera, made my first exposure…and saw shots. So I put the old Nikon F body aside thinking I absolutely nothing. might take it up another day. (Continued next month) I suppose I may have been perusing the ads in PAGE 2 April 2005 Astro Calendar SUN MON TUE WED THU FRI SAT 1 Last quarter 2 Sirius reaches moon at 6:50 p.m. its highest point CST. Look for in the sky, due Luna in Sagitta- south, 1/2 hour rius. before sunset. THE FBACOBSERVER 3 Luna 8 degrees 4 Jupiter just past 5 Waning moon 6 Find mag 2 Al- 7 Neptune sits 8 New moon at 9 View an exqui- right of Mars at opposition, rising low in the east- phard in Hydra, the only 3 degrees to 3:32 p.m. CDT. site, thin crescent dawn in Capricor- within minutes of southeast just be- Water Snake. If the upper left of Partial solar moon early this nus. CDT begins. sunset. fore sunrise. you can find skies Mars. eclipse can be evening. that good here. seen from here. 10 Saturn in 11 Luna and the 12 Green laser night. 13 After posting 14 AOW Star 15 FBAC Club 16 First quarter quadrature today, Pleiades convene Shine your laser into bond, get out of Party, Faith Lu- Meeting. See moon at 9:37 a.m. 90 degrees from together. A beau- your neighbor’s win- jail and check out theran Church. Web Site, CDT. dow and see what the Sun. tiful site. happens. Arcturus near See web site, fbac.org Jupiter. fbac.org 17 Orion low in 18 Regulus and 19 Watch Mars 20 See the future. 21 Lyrid Meteor 22 See the moon 23 Speed over to the west soon to the Waxing near Gamma Cap Early risers can Shower before occult Jupiter. Move first mag Spica in be bid adieu. Moon. Nice title for the next few see August stars. dawn tomorrow. to South Africa to Virgo. Did you catch it. Or Antarc- for a book. mornings. Expected to be a tica, take your pick. know it’s a vari- flop. able? VOLUME 24 Full Moon at 25 The Moon is 26 Mercury 27 Take time off 28 Fort Bend 29 AOW Star 30 The Beehive 5:06 a.m. CDT. oblong tonight be- reaches greatest from observing. Wine and Food Party, Dickinson is buzzing. Look 19, Penumbral eclipse cause it’s one day elongation. Watch TV and Event, George Elementary for the Praesepe ISSUE in western part of after full. improve your Observatory School. See web in Cancer. 4 U.S. mind. site, fbac.org VOLUME 19, ISSUE 4 THE FBAC OBSERVER PAGE 3 was eventually able to detect an elongated, egg-shaped glow be- tween two stars. This planetary is very obscure, so if you do de- GOING DEEP tect it you can count yourself among a select group of people Keith Rivich who have ever seen it. Go back to 15 Mon and picture a point about ½ of the funny thought occurred to me the other night as I way to 12 Mon and just a tad south. Scan around a little until you was contemplating the sky and thinking about this find a little comet shaped nebula, a.k.a. Hubble’s Variable Ne b- article; it seems that once a constellation crosses the ula (NGC 2261). This most interesting object is fun to watch meridian I sort of lose interest in observing there. over time as the appearance of the nebula changes with irregular AMy thoughts seem to be on what’s rising in the east, not setting frequency. Once thought to be caused by the variability of the in the west! I suppose my attention is drawn to the “new” and illuminating star it has been determined that the changes are sort of pushes the “old” to another part of my mind, for it will be caused by huge clouds orbiting near the star and casting shadows “new” again in six months or so and I will be excited all over against the nebula. Way cool! again. But this shouldn’t be the case. For most of us observing While centered on NGC 2261 look near the SW edge of from the Houston area the SW sky is the darkest and should be your finder scope and you will see the odd shaped open cluster used the most for observing. NGC 2251. Instead of the being roundish, like its cousins, NGC For this article I will break my bad habit by playing 2251 is elongated and flattened on one end, similar in appear- around in the neighborhood of the “Christmas Tree” cluster in ance to the constellation Delphinus.
Recommended publications
  • 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.
    [Show full text]
  • GALEX Helix Nebula Poster
    National Aeronautics and Space Administration The Helix Nebula: What is it? The object shown on the front of this poster is the This “Mountains Helix Nebula. Although this object and others like it are of Creation” image called planetary nebulae (pronounced NEB-u-lee), they was captured by really have nothing to do with planets. They got their name the Spitzer Space ZKHQDVWURQRPHUV¿rst saw them through early telescopes, Telescope in infrared because they looked similar to planets with rings around light. It reveals them, like Saturn. billowing mountains of dust ablaze with A planetary nebula is the ¿res of active star really a shell of glowing gas formation. GALEX and plasma from a star at the can see the new stars end of its life. The star has forming, because they glow brightly in ultraviolet (UV) light. blown off much of its material However, the surrounding dust and gas clouds are cooler and and what is left is a very not so visible to GALEX. compact object called a white dwarf. For a while, the white dwarf is still hot and bright A Tug of War enough to make the material Planetary nebula JnEr1, A star is an amazing from the former star glow, as seen by GALEX. ! Ow! If not for balancing act between two ! * * gravity, my head and that is what we see as a * * would explode! beautiful nebula. Over 10,000 huge forces. On the one * years or so, the gas will drift away and the white dwarf will hand, the crushing force of the star’s own gravity Gravity Heat cool so much that we can no longer see the nebula.
    [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]
  • Poster Abstracts
    Aimée Hall • Institute of Astronomy, Cambridge, UK 1 Neptunes in the Noise: Improved Precision in Exoplanet Transit Detection SuperWASP is an established, highly successful ground-based survey that has already discovered over 80 exoplanets around bright stars. It is only with wide-field surveys such as this that we can find planets around the brightest stars, which are best suited for advancing our knowledge of exoplanetary atmospheres. However, complex instrumental systematics have so far limited SuperWASP to primarily finding hot Jupiters around stars fainter than 10th magnitude. By quantifying and accounting for these systematics up front, rather than in the post- processing stage, the photometric noise can be significantly reduced. In this paper, we present our methods and discuss preliminary results from our re-analysis. We show that the improved processing will enable us to find smaller planets around even brighter stars than was previously possible in the SuperWASP data. Such planets could prove invaluable to the community as they would potentially become ideal targets for the studies of exoplanet atmospheres. Alan Jackson • Arizona State University, USA 2 Stop Hitting Yourself: Did Most Terrestrial Impactors Originate from the Terrestrial Planets? Although the asteroid belt is the main source of impactors in the inner solar system today, it contains only 0.0006 Earth mass, or 0.05 Lunar mass. While the asteroid belt would have been much more massive when it formed, it is unlikely to have had greater than 0.5 Lunar mass since the formation of Jupiter and the dissipation of the solar nebula. By comparison, giant impacts onto the terrestrial planets typically release debris equal to several per cent of the planet’s mass.
    [Show full text]
  • Two Rings but No Fellowship: Lotr 1 and Its Relation to Planetary Nebulae
    Mon. Not. R. Astron. Soc. 000, 1–16 (2013) Printed 17 October 2018 (MN LATEX style file v2.2) Two rings but no fellowship: LoTr 1 and its relation to planetary nebulae possessing barium central stars. A.A. Tyndall1,2⋆, D. Jones2, H.M.J. Boffin2, B. Miszalski3,4, F. Faedi5, M. Lloyd1, J.A. L´opez6, S. Martell7, D. Pollacco5, and M. Santander-Garc´ıa8 1Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, M13 9PL, UK 2European Southern Observatory, Alonso de C´ordova 3107, Casilla 19001, Santiago, Chile 3South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa 4Southern African Large Telescope. PO Box 9, Observatory 7935, South Africa 5Department of Physics, University of Warwick, CV4 7AL, UK 6Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Ensenada, Baja California, C.P. 22800, Mexico 7Australian Astronomical Observatory, North Ryde, 2109 NSW, Australia 8Observatorio Astron´omico National, Madrid, and Centro de Astrobiolog´ıa, CSIC-INTA, Spain Accepted xxxx xxxxxxxx xx. Received xxxx xxxxxxxx xx; in original form xxxx xxxxxxxx xx ABSTRACT LoTr 1 is a planetary nebula thought to contain an intermediate-period binary central star system ( that is, a system with an orbital period, P, between 100 and, say, 1500 days). The system shows the signature of a K-type, rapidly rotating giant, and most likely constitutes an accretion-induced post-mass transfer system similar to other PNe such as LoTr 5, WeBo 1 and A70. Such systems represent rare opportunities to further the investigation into the formation of barium stars and intermediate period post-AGB systems – a formation process still far from being understood.
    [Show full text]
  • X-Ray Emission from a Merger Remnant, NGC 7252,The “Atoms-For-Peace” Galaxy
    X-ray emission from a merger remnant, NGC 7252,the \Atoms-for-Peace" galaxy Hisamitsu Awaki Department of Physics, Faculty of Science, Ehime University Hironori Matsumoto1 Department of Earth and Space Science, Osaka University, and Hiroshi Tomida Space Utilization Research Program, National Space Development Agency of Japan, ABSTRACT We observed a nearby merger remnant NGC 7252 with the X-ray satellite ASCA, 13 1 2 and detected X-ray emission with the X-ray flux of (1.8 0.3) 10− ergs s− cm− in ± × 40 1 the 0.5–10 keV band. This corresponds to the X-ray luminosity of 8.1 10 ergs s− . The X-ray emission is well described with a two-component model: a soft× component with kT =0:72 0.13 keV and a hard component with kT > 5:1 keV. Although NGC 7252 is referred± to as a dynamically young protoelliptical, the 0.5–4 keV luminosity of 40 1 the soft component is about 2 10 ergs s− , which is low for an early-type galaxy. The × ratio of LX=LFIR suggests that the soft component originated from the hot gas due to star formation. Its low luminosity can be explained by the gas ejection from the galaxy as galaxy winds. Our observation reveals the existence of hard X-ray emission with the 40 1 2–10 keV luminosity of 5.6 10 ergs s− . This may indicate the existence of nuclear activity or intermediate-mass× black hole in NGC 7252. Subject headings: galaxies: evolution — galaxies: individual (NGC 7252) — X-rays: galaxies 1Center for Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, NE80-6045, Cambridge, MA02139-4307, USA 1 1.
    [Show full text]
  • Instruction Manual Meade Instruments Corporation
    Instruction Manual 7" LX200 Maksutov-Cassegrain Telescope 8", 10", and 12" LX200 Schmidt-Cassegrain Telescopes Meade Instruments Corporation NOTE: Instructions for the use of optional accessories are not included in this manual. For details in this regard, see the Meade General Catalog. (2) (1) (1) (2) Ray (2) 1/2° Ray (1) 8.218" (2) 8.016" (1) 8.0" Secondary 8.0" Mirror Focal Plane Secondary Primary Baffle Tube Baffle Field Stops Correcting Primary Mirror Plate The Meade Schmidt-Cassegrain Optical System (Diagram not to scale) In the Schmidt-Cassegrain design of the Meade 8", 10", and 12" models, light enters from the right, passes through a thin lens with 2-sided aspheric correction (“correcting plate”), proceeds to a spherical primary mirror, and then to a convex aspheric secondary mirror. The convex secondary mirror multiplies the effective focal length of the primary mirror and results in a focus at the focal plane, with light passing through a central perforation in the primary mirror. The 8", 10", and 12" models include oversize 8.25", 10.375" and 12.375" primary mirrors, respectively, yielding fully illuminated fields- of-view significantly wider than is possible with standard-size primary mirrors. Note that light ray (2) in the figure would be lost entirely, except for the oversize primary. It is this phenomenon which results in Meade 8", 10", and 12" Schmidt-Cassegrains having off-axis field illuminations 10% greater, aperture-for-aperture, than other Schmidt-Cassegrains utilizing standard-size primary mirrors. The optical design of the 4" Model 2045D is almost identical but does not include an oversize primary, since the effect in this case is small.
    [Show full text]
  • Understanding the H2/HI Ratio in Galaxies 3
    Mon. Not. R. Astron. Soc. 394, 1857–1874 (2009) Printed 6 August 2021 (MN LATEX style file v2.2) Understanding the H2/HI Ratio in Galaxies D. Obreschkow and S. Rawlings Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK Accepted 2009 January 12 ABSTRACT galaxy We revisit the mass ratio Rmol between molecular hydrogen (H2) and atomic hydrogen (HI) in different galaxies from a phenomenological and theoretical viewpoint. First, the local H2- mass function (MF) is estimated from the local CO-luminosity function (LF) of the FCRAO Extragalactic CO-Survey, adopting a variable CO-to-H2 conversion fitted to nearby observa- 5 1 tions. This implies an average H2-density ΩH2 = (6.9 2.7) 10− h− and ΩH2 /ΩHI = 0.26 0.11 ± · galaxy ± in the local Universe. Second, we investigate the correlations between Rmol and global galaxy properties in a sample of 245 local galaxies. Based on these correlations we intro- galaxy duce four phenomenological models for Rmol , which we apply to estimate H2-masses for galaxy each HI-galaxy in the HIPASS catalog. The resulting H2-MFs (one for each model for Rmol ) are compared to the reference H2-MF derived from the CO-LF, thus allowing us to determine the Bayesian evidence of each model and to identify a clear best model, in which, for spi- galaxy ral galaxies, Rmol negatively correlates with both galaxy Hubble type and total gas mass. galaxy Third, we derive a theoretical model for Rmol for regular galaxies based on an expression for their axially symmetric pressure profile dictating the degree of molecularization.
    [Show full text]
  • Diffuse X-Ray Emission from the Planetary Nebula NGC 7009
    A&A 387, L1–L5 (2002) Astronomy DOI: 10.1051/0004-6361:20020330 & c ESO 2002 Astrophysics Diffuse X-ray emission from the planetary nebula NGC 7009? M. A. Guerrero, R. A. Gruendl, and Y.-H. Chu Astronomy Department, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA Received 7 February 2002 / Accepted 1 March 2002 Abstract. XMM-Newton EPIC observations of the planetary nebula (PN) NGC 7009, the Saturn Nebula, have detected extended X-ray emission in its central cavity. The diffuse X-ray emission must originate in the shocked fast stellar wind. The spectra show that the temperature of the hot gas is 1.8 × 106 K. The rms density derived from the volume emission measure is a few tens H-atom cm−3. The hot gas does not appear over-pressurized with respect to the nebular shell. NGC 7009 represents an evolutionary stage at which the influence of the hot gas in the PN interior starts to decline due to the diminishing strength of the fast stellar wind and the expansion of the central cavity. Key words. ISM: planetary nebulae: general – ISM: planetary nebulae: individual: NGC 7009 – stars: winds, outflows – X-rays: ISM 1. Introduction Chandra observations of the evolved PN NGC 7293 (the Helix Nebula), on the other hand, does not show any dif- It has been commonly accepted that the shell struc- fuse X-ray emission (Guerrero et al. 2001). These results ture of a planetary nebula (PN) is formed by the cur- suggest that the hot gas content of a PN diminishes as the rent fast stellar wind sweeping up the previous asymp- PN ages.
    [Show full text]
  • Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
    Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C.
    [Show full text]
  • Investigating the Relation Between CO (3-2) and Far Infrared Luminosities
    Publ. Astron. Soc. Japan (2014) 00(0), 1–16 1 doi: 10.1093/pasj/xxx000 Investigating the Relation between CO (3–2) and Far Infrared Luminosities for Nearby Merging Galaxies Using ASTE Tomonari MICHIYAMA,1,2 Daisuke IONO,1,2 Kouichiro NAKANISHI1,2 Junko UEDA,3 Toshiki SAITO,4,2 Misaki ANDO,1,2 Hiroyuki KANEKO,5,2 Takuji YAMASHITA,6 Yuichi MATSUDA,1,2 Bunyo HATSUKADE,2 Kenichi KIKUCHI,2 Shinya KOMUGI,7 and Takayuki MUTO7 1Department of Astronomical Science, SOKENDAI (The Graduate University of Advanced Studies), Mitaka, Tokyo 181-8588 2National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588 3Harvard-Smithsonian Center for Astrophysics, 60 Garden Street,Cambridge, MA 02138, USA 4Department of Astronomy, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 133-0033 5Nobeyama Radio Observatory, 462-2, Minamimaki, Minamisaku, Nagano, 384-1305 6Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210 7Division of Liberal Arts, Kogakuin University, 1-24-2, Nishi-Shinjuku, Shinjuku-ku, Tokyo 163-8677 ∗E-mail: [email protected] Received ; Accepted Abstract We present the new single dish CO (3–2) emission data obtained toward 19 early stage and 7 late stage nearby merging galaxies using the Atacama Submillimeter Telescope Experiment (ASTE). Combining with the single dish and interferometric data of galaxies observed in pre- ′ vious studies, we investigate the relation between the CO (3–2) luminosity (LCO(3−2)) and the far Infrared luminosity (LFIR) in a sample of 29 early stage and 31 late stage merging galaxies, and 28 nearby isolated spiral galaxies.
    [Show full text]
  • 7.5 X 11.5.Threelines.P65
    Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93,
    [Show full text]