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The HERACLES View of the H -To-HI Ratio in Galaxies
The HERACLES View of the H2-to-HI Ratio in Galaxies Adam Leroy (NRAO, Hubble Fellow) Fabian Walter, Frank Bigiel, the HERACLES and THINGS teams The Saturday Morning Summary • Star formation rate vs. gas relation on ~kpc scales breaks apart into: A relatively universal CO-SFR relation in nearby disks Systematic environmental scalings in the CO-to-HI ratio • The CO-to-HI ratio is a strong function of radius, total gas, and stellar surface density correlated with ISM properties: dust-to-gas ratio, pressure harder to link to dynamics: gravitational instability, arms • Interpretation: the CO-to-HI ratio traces the efficiency of GMC formation Density and dust can explain much of the observed behavior heracles Fabian Walter Erik Rosolowsky MPIA UBC Frank Bigiel Eva Schinnerer UC Berkeley THINGS plus… MPIA Elias Brinks Antonio Usero Gaelle Dumas U Hertfordshire OAN, Madrid MPIA Erwin de Blok Andreas Schruba Helmut Wiesemeyer U Cape Town IRAM … MPIA Rob Kennicutt Axel Weiss Karl Schuster Cambridge MPIfR IRAM Barry Madore Carsten Kramer Karin Sandstrom Carnegie IRAM MPIA Michele Thornley Daniela Calzetti Kelly Foyle Bucknell UMass MPIA Collaborators The HERA CO-Line Extragalactic Survey First maps Leroy et al. (2009) • IRAM 30m Large Program to map CO J = 2→1 line • Instrument: HERA receiver array operating at 230 GHz • 47 galaxies: dwarfs to starbursts and massive spirals -2 • Very wide-field (~ r25) and sensitive (σ ~ 1-2 Msun pc ) NGS The HI Nearby Galaxy Survey HI Walter et al. (2008), AJ Special Issue (2008) • VLA HI maps of 34 galaxies: -
Big Halpha Kinematical Sample of Barred Spiral Galaxies - I
BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle To cite this version: O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle. BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2005, 360 Issue 4, pp.1201. 10.1111/j.1365-2966.2005.09125.x. hal-00014446 HAL Id: hal-00014446 https://hal.archives-ouvertes.fr/hal-00014446 Submitted on 26 Jan 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 360, 1201–1230 (2005) doi:10.1111/j.1365-2966.2005.09125.x BHαBAR: big Hα kinematical sample of barred spiral galaxies – I. Fabry–Perot observations of 21 galaxies O. Hernandez,1,2 † C. Carignan,1 P. Amram,2 L. Chemin1 and O. Daigle1 1Observatoire du mont Megantic,´ LAE, Universitede´ Montreal,´ CP 6128 succ. centre ville, Montreal,´ Quebec,´ Canada H3C 3J7 2Observatoire Astronomique de Marseille Provence et LAM, 2 pl. -
MESSIER 13 RA(2000) : 16H 41M 42S DEC(2000): +36° 27'
MESSIER 13 RA(2000) : 16h 41m 42s DEC(2000): +36° 27’ 41” BASIC INFORMATION OBJECT TYPE: Globular Cluster CONSTELLATION: Hercules BEST VIEW: Late July DISCOVERY: Edmond Halley, 1714 DISTANCE: 25,100 ly DIAMETER: 145 ly APPARENT MAGNITUDE: +5.8 APPARENT DIMENSIONS: 20’ Starry Night FOV: 1.00 Lyra FOV: 60.00 Libra MESSIER 6 (Butterfly Cluster) RA(2000) : 17Ophiuchus h 40m 20s DEC(2000): -32° 15’ 12” M6 Sagitta Serpens Cauda Vulpecula Scutum Scorpius Aquila M6 FOV: 5.00 Telrad Delphinus Norma Sagittarius Corona Australis Ara Equuleus M6 Triangulum Australe BASIC INFORMATION OBJECT TYPE: Open Cluster Telescopium CONSTELLATION: Scorpius Capricornus BEST VIEW: August DISCOVERY: Giovanni Batista Hodierna, c. 1654 DISTANCE: 1600 ly MicroscopiumDIAMETER: 12 – 25 ly Pavo APPARENT MAGNITUDE: +4.2 APPARENT DIMENSIONS: 25’ – 54’ AGE: 50 – 100 million years Telrad Indus MESSIER 7 (Ptolemy’s Cluster) RA(2000) : 17h 53m 51s DEC(2000): -34° 47’ 36” BASIC INFORMATION OBJECT TYPE: Open Cluster CONSTELLATION: Scorpius BEST VIEW: August DISCOVERY: Claudius Ptolemy, 130 A.D. DISTANCE: 900 – 1000 ly DIAMETER: 20 – 25 ly APPARENT MAGNITUDE: +3.3 APPARENT DIMENSIONS: 80’ AGE: ~220 million years FOV:Starry 1.00Night FOV: 60.00 Hercules Libra MESSIER 8 (THE LAGOON NEBULA) RA(2000) : 18h 03m 37s DEC(2000): -24° 23’ 12” Lyra M8 Ophiuchus Serpens Cauda Cygnus Scorpius Sagitta M8 FOV: 5.00 Scutum Telrad Vulpecula Aquila Ara Corona Australis Sagittarius Delphinus M8 BASIC INFORMATION Telescopium OBJECT TYPE: Star Forming Region CONSTELLATION: Sagittarius Equuleus BEST -
1. Introduction
THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other. -
Age and Interstellar Absorption in Young Star-Formation Regions In
ISSN 1063-7729, Astronomy Reports, 2008, Vol. 52, No. 9, pp. 714–728. c Pleiades Publishing, Ltd., 2008. Original Russian Text c A.S. Gusev, V.I. Myakutin, A.E. Piskunov, F.K. Sakhibov, M.S. Khramtsova, 2008, published in Astronomicheski˘ı Zhurnal, 2008, Vol. 85, No. 9, pp. 794–809. Age and Interstellar Absorption in Young Star-Formation Regions in the Galaxies NGC 1068, NGC 4449, NGC 4490, NGC 4631, and NGC 4656/57 Derived from Multicolor Photometry A. S. Gusev1, V.I.Myakutin2, A.E.Piskunov2,F.K.Sakhibov3, 4,andM.S.Khramtsova5 1Sternberg Astronomical Institute, Universitetski ˘ı pr. 13, Moscow, 119991, Russia 2Institute of Astronomy, Russian Academy of Sciences, ul. Pyatnitskaya 48, Moscow, 109017 Russia 3Giessen–Friedberg University for Applied Studies, Friedberg, Germany 4Institute of Astrophysics, Academy of Sciences of Tajikistan, ul. Bukhoro 22, Dushanbe, 734670 Tajikistan 5Ural State University, pr. Lenina 51, Yekaterinburg, 620083 Received October 3, 2007; in final form, October, 26, 2007 Abstract—We have compared the results of multicolor UBVR and Hα photometry for 169 young star-formation complexes in five galaxies using a grid of evolutionary models for young star clusters. The ages and interstellar absorptions are estimated for 102 star-formation complexes with the standard m uncertainties σt =0.30 dex and σAV =0.45 . The accuracies of these parameters were verified using numerical simulations. PACS num b e r s : 98.52.Nr, 98.62.Ai, 97.10.Bt DOI: 10.1134/S1063772908090035 1. INTRODUCTION several evolutionary models, instead considering a set The evolution of galaxies depends on their history of models encompassing the entire interval of the of star formation, i.e., the history of variations of IMF and SFR. -
August 13 2016 7:00Pm at the Herrett Center for Arts & Science College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, August 13th 2016 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. Public Star Party Follows at the Colleagues, Centennial Observatory Club Officers It's that time of year: The City of Rocks Star Party. Set for Friday, Aug. 5th, and Saturday, Aug. 6th, the event is the gem of the MVAS year. As we've done every Robert Mayer, President year, we will hold solar viewing at the Smoky Mountain Campground, followed by a [email protected] potluck there at the campground. Again, MVAS will provide the main course and 208-312-1203 beverages. Paul McClain, Vice President After the potluck, the party moves over to the corral by the bunkhouse over at [email protected] Castle Rocks, with deep sky viewing beginning sometime after 9 p.m. This is a chance to dig into some of the darkest skies in the west. Gary Leavitt, Secretary [email protected] Some members have already reserved campsites, but for those who are thinking of 208-731-7476 dropping by at the last minute, we have room for you at the bunkhouse, and would love to have to come by. Jim Tubbs, Treasurer / ALCOR [email protected] The following Saturday will be the regular MVAS meeting. Please check E-mail or 208-404-2999 Facebook for updates on our guest speaker that day. David Olsen, Newsletter Editor Until then, clear views, [email protected] Robert Mayer Rick Widmer, Webmaster [email protected] Magic Valley Astronomical Society is a member of the Astronomical League M-51 imaged by Rick Widmer & Ken Thomason Herrett Telescope Shotwell Camera https://herrett.csi.edu/astronomy/observatory/City_of_Rocks_Star_Party_2016.asp Calendars for August Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 6 New Moon City Rocks City Rocks Lunation 1158 Castle Rocks Castle Rocks Star Party Star Party Almo, ID Almo, ID 7 8 9 10 11 12 13 MVAS General Mtg. -
X-Ray and Gamma-Ray Variability of NGC 1275
galaxies Article X-ray and Gamma-ray Variability of NGC 1275 Varsha Chitnis 1,*,† , Amit Shukla 2,*,† , K. P. Singh 3 , Jayashree Roy 4 , Sudip Bhattacharyya 5, Sunil Chandra 6 and Gordon Stewart 7 1 Department of High Energy Physics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India 2 Discipline of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore, Khandwa Road, Simrol, Indore 453552, India 3 Indian Institute of Science Education and Research Mohali, Knowledge City, Sector 81, SAS Nagar, Manauli 140306, India; [email protected] 4 Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune 411 007, India; [email protected] 5 Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India; [email protected] 6 Centre for Space Research, North-West University, Potchefstroom 2520, South Africa; [email protected] 7 Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, UK; [email protected] * Correspondence: [email protected] (V.C.); [email protected] (A.S.) † These authors contributed equally to this work. Received: 30 June 2020; Accepted: 24 August 2020; Published: 28 August 2020 Abstract: Gamma-ray emission from the bright radio source 3C 84, associated with the Perseus cluster, is ascribed to the radio galaxy NGC 1275 residing at the centre of the cluster. Study of the correlated X-ray/gamma-ray emission from this active galaxy, and investigation of the possible disk-jet connection, are hampered because the X-ray emission, particularly in the soft X-ray band (2–10 keV), is overwhelmed by the cluster emission. -
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. -
PUBLIC OBSERVING NIGHTS the William D. Mcdowell Observatory
THE WilliamPUBLIC D. OBSERVING mcDowell NIGHTS Observatory FREE PUBLIC OBSERVING NIGHTS WINTER Schedule 2019 December 2018 (7PM-10PM) 5th Mars, Uranus, Neptune, Almach (double star), Pleiades (M45), Andromeda Galaxy (M31), Oribion Nebula (M42), Beehive Cluster (M44), Double Cluster (NGC 869 & 884) 12th Mars, Uranus, Neptune, Almach (double star), Pleiades (M45), Andromeda Galaxy (M31), Oribion Nebula (M42), Beehive Cluster (M44), Double Cluster (NGC 869 & 884) 19th Moon, Mars, Uranus, Neptune, Almach (double star), Pleiades (M45), Andromeda Galaxy (M31), Oribion Nebula (M42), Beehive Cluster (M44), Double Cluster (NGC 869 & 884) 26th Moon, Mars, Uranus, Neptune, Almach (double star), Pleiades (M45), Andromeda Galaxy (M31), Oribion Nebula (M42), Beehive Cluster (M44), Double Cluster (NGC 869 & 884)? January 2019 (7PM-10PM) 2nd Moon, Mars, Uranus, Neptune, Sirius, Almach (double star), Pleiades (M45), Orion Nebula (M42), Open Cluster (M35) 9th Mars, Uranus, Neptune, Sirius, Almach (double star), Pleiades (M45), Orion Nebula (M42), Open Cluster (M35) 16 Mars, Uranus, Neptune, Sirius, Almach (double star), Pleiades (M45), Orion Nebula (M42), Open Cluster (M35) 23rd, Moon, Mars, Uranus, Neptune, Sirius, Almach (double star), Pleiades (M45), Andromeda Galaxy (M31), Orion Nebula (M42), Beehive Cluster (M44), Double Cluster (NGC 869 & 884) 30th Moon, Mars, Uranus, Neptune, Sirius, Almach (double star), Pleiades (M45), Andromeda Galaxy (M31), Orion Nebula (M42), Beehive Cluster (M44), Double Cluster (NGC 869 & 884) February 2019 (7PM-10PM) 6th -
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. -
Ghost Hunt Challenge 2020
Virtual Ghost Hunt Challenge 10/21 /2020 (Sorry we can meet in person this year or give out awards but try doing this challenge on your own.) Participant’s Name _________________________ Categories for the competition: Manual Telescope Electronically Aided Telescope Binocular Astrophotography (best photo) (if you expect to compete in more than one category please fill-out a sheet for each) ** There are four objects on this list that may be beyond the reach of beginning astronomers or basic telescopes. Therefore, we have marked these objects with an * and provided alternate replacements for you just below the designated entry. We will use the primary objects to break a tie if that’s needed. Page 1 TAS Ghost Hunt Challenge - Page 2 Time # Designation Type Con. RA Dec. Mag. Size Common Name Observed Facing West – 7:30 8:30 p.m. 1 M17 EN Sgr 18h21’ -16˚11’ 6.0 40’x30’ Omega Nebula 2 M16 EN Ser 18h19’ -13˚47 6.0 17’ by 14’ Ghost Puppet Nebula 3 M10 GC Oph 16h58’ -04˚08’ 6.6 20’ 4 M12 GC Oph 16h48’ -01˚59’ 6.7 16’ 5 M51 Gal CVn 13h30’ 47h05’’ 8.0 13.8’x11.8’ Whirlpool Facing West - 8:30 – 9:00 p.m. 6 M101 GAL UMa 14h03’ 54˚15’ 7.9 24x22.9’ 7 NGC 6572 PN Oph 18h12’ 06˚51’ 7.3 16”x13” Emerald Eye 8 NGC 6426 GC Oph 17h46’ 03˚10’ 11.0 4.2’ 9 NGC 6633 OC Oph 18h28’ 06˚31’ 4.6 20’ Tweedledum 10 IC 4756 OC Ser 18h40’ 05˚28” 4.6 39’ Tweedledee 11 M26 OC Sct 18h46’ -09˚22’ 8.0 7.0’ 12 NGC 6712 GC Sct 18h54’ -08˚41’ 8.1 9.8’ 13 M13 GC Her 16h42’ 36˚25’ 5.8 20’ Great Hercules Cluster 14 NGC 6709 OC Aql 18h52’ 10˚21’ 6.7 14’ Flying Unicorn 15 M71 GC Sge 19h55’ 18˚50’ 8.2 7’ 16 M27 PN Vul 20h00’ 22˚43’ 7.3 8’x6’ Dumbbell Nebula 17 M56 GC Lyr 19h17’ 30˚13 8.3 9’ 18 M57 PN Lyr 18h54’ 33˚03’ 8.8 1.4’x1.1’ Ring Nebula 19 M92 GC Her 17h18’ 43˚07’ 6.44 14’ 20 M72 GC Aqr 20h54’ -12˚32’ 9.2 6’ Facing West - 9 – 10 p.m. -
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.