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Arxiv:0804.4630V1 [Astro-Ph] 29 Apr 2008 I Ehnv20;Ficao 06) Ti Nti Oeas Role This in Is It 2006A)
DRAFT VERSION NOVEMBER 9, 2018 Preprint typeset using LATEX style emulateapj v. 05/04/06 OPEN CLUSTERS AS GALACTIC DISK TRACERS: I. PROJECT MOTIVATION, CLUSTER MEMBERSHIP AND BULK THREE-DIMENSIONAL KINEMATICS PETER M. FRINCHABOY1,2,3 AND STEVEN R. MAJEWSKI2 Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA Draft version November 9, 2018 ABSTRACT We have begun a survey of the chemical and dynamical properties of the Milky Way disk as traced by open star clusters. In this first contribution, the general goals of our survey are outlined and the strengths and limita- tions of using star clusters as a Galactic disk tracer sample are discussed. We also present medium resolution (R 15,0000) spectroscopy of open cluster stars obtained with the Hydra multi-object spectrographs on the Cerro∼ Tololo Inter-American Observatory 4-m and WIYN 3.5-m telescopes. Here we use these data to deter- mine the radial velocities of 3436 stars in the fields of open clusters within about 3 kpc, with specific attention to stars having proper motions in the Tycho-2 catalog. Additional radial velocity members (without Tycho-2 proper motions) that can be used for future studies of these clusters were also identified. The radial velocities, proper motions, and the angular distance of the stars from cluster center are used to derive cluster member- ship probabilities for stars in each cluster field using a non-parametric approach, and the cluster members so-identified are used, in turn, to derive the reliable bulk three-dimensional motion for 66 of 71 targeted open clusters. -
A Gaia DR2 View of the Open Cluster Population in the Milky Way T
Astronomy & Astrophysics manuscript no. manuscript˙arXiv2 © ESO 2018 July 13, 2018 A Gaia DR2 view of the Open Cluster population in the Milky Way T. Cantat-Gaudin1, C. Jordi1, A. Vallenari2, A. Bragaglia3, L. Balaguer-Nu´nez˜ 1, C. Soubiran4, D. Bossini2, A. Moitinho5, A. Castro-Ginard1, A. Krone-Martins5, L. Casamiquela4, R. Sordo2, and R. Carrera2 1 Institut de Ciencies` del Cosmos, Universitat de Barcelona (IEEC-UB), Mart´ı i Franques` 1, E-08028 Barcelona, Spain 2 INAF-Osservatorio Astronomico di Padova, vicolo Osservatorio 5, 35122 Padova, Italy 3 INAF-Osservatorio di Astrofisica e Scienza dello Spazio, via Gobetti 93/3, 40129 Bologna, Italy 4 Laboratoire dAstrophysique de Bordeaux, Univ. Bordeaux, CNRS, UMR 5804, 33615 Pessac, France 5 CENTRA, Faculdade de Ciencias,ˆ Universidade de Lisboa, Ed. C8, Campo Grande, P-1749-016 Lisboa, Portugal Received date / Accepted date ABSTRACT Context. Open clusters are convenient probes of the structure and history of the Galactic disk. They are also fundamental to stellar evolution studies. The second Gaia data release contains precise astrometry at the sub-milliarcsecond level and homogeneous pho- tometry at the mmag level, that can be used to characterise a large number of clusters over the entire sky. Aims. In this study we aim to establish a list of members and derive mean parameters, in particular distances, for as many clusters as possible, making use of Gaia data alone. Methods. We compile a list of thousands of known or putative clusters from the literature. We then apply an unsupervised membership assignment code, UPMASK, to the Gaia DR2 data contained within the fields of those clusters. -
Large-Scale Outflows in Edge-On Seyfert Galaxies. II. Kiloparsec
Large-Scale Outflows in Edge-on Seyfert Galaxies. II. Kiloparsec-Scale Radio Continuum Emission Edward J. M. Colbert1,2, Stefi A. Baum1, Jack F. Gallimore1,2, Christopher P. O’Dea1, Jennifer A. Christensen1 Received ; accepted arXiv:astro-ph/9604022v1 3 Apr 1996 1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 2 Department of Astronomy, University of Maryland, College Park, MD 20742 –2– ABSTRACT We present deep images of the kpc-scale radio continuum emission in 14 edge-on galaxies (ten Seyfert and four starburst galaxies). Observations were taken with the VLA at 4.9 GHz (6 cm). The Seyfert galaxies were selected from a distance-limited sample of 22 objects (defined in paper I). The starburst galaxies were selected to be well-matched to the Seyferts in radio power, recessional velocity and inclination angle. All four starburst galaxies have a very bright disk component and one (NGC 3044) has a radio halo that extends several kpc out of the galaxy plane. Six of the ten Seyferts observed have large-scale (radial extent >1 kpc) radio structures extending outward from the ∼ nuclear region, indicating that large-scale outflows are quite common in Seyferts. Large-scale radio sources in Seyferts are similar in radio power and radial extent to radio halos in edge-on starburst galaxies, but their morphologies do not resemble spherical halos observed in starburst galaxies. The sources have diffuse morphologies, but, in general, they are oriented at skewed angles with respect to the galaxy minor axes. This result is most easily understood if the outflows are AGN-driven jets that are somehow diverted away from the galaxy disk on scales >1 kpc. -
February 14, 2015 7:00Pm at the Herrett Center for Arts & Science Colleagues, College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, February 14, 2015 7:00pm at the Herrett Center for Arts & Science Colleagues, College of Southern Idaho. Public Star Party Follows at the It’s that time of year when obstacles appear in the sky. In particular, this year is Centennial Obs. loaded with fog. It got in the way of letting us see the dance of the Jovian moons late last month, and it’s hindered our views of other unique shows. Still, members Club Officers reported finding enough of a clear sky to let us see Comet Lovejoy, and some great photos by members are popping up on the Facebook page. Robert Mayer, President This month, however, is a great opportunity to see the benefit of something [email protected] getting in the way. Our own Chris Anderson of the Herrett Center has been using 208-312-1203 the Centennial Observatory’s scope to do work on occultation’s, particularly with asteroids. This month’s MVAS meeting on Feb. 14th will give him the stage to Terry Wofford, Vice President show us just how this all works. [email protected] The following weekend may also be the time the weather allows us to resume 208-308-1821 MVAS-only star parties. Feb. 21 is a great window for a possible star party; we’ll announce the location if the weather permits. However, if we don’t get that Gary Leavitt, Secretary window, we’ll fall back on what has become a MVAS tradition: Planetarium night [email protected] at the Herrett Center. -
Open Clusters in Gaia
Sede Amministrativa: Università degli Studi di Padova Dipartimento di Fisica e Astronomia “G. Galilei” Corso di Dottorato di Ricerca in Astronomia Ciclo XXX OPEN CLUSTERS IN GAIA ERA Coordinatore: Ch.mo Prof. Giampaolo Piotto Supervisore: Dr.ssa Antonella Vallenari Dottorando: Francesco Pensabene i Abstract Context. Open clusters (OCs) are optimal tracers of the Milky Way disc. They are observed at every distance from the Galactic center and their ages cover the entire lifespan of the disc. The actual OC census contain more than 3000 objects, but suffers of incom- pleteness out of the solar neighborhood and of large inhomogeneity in the parameter deter- minations present in literature. Both these aspects will be improved by the on-going space mission Gaia . In the next years Gaia will produce the most precise three-dimensional map of the Milky Way by surveying other than 1 billion of stars. For those stars Gaia will provide extremely precise measure- ment of proper motions, parallaxes and brightness. Aims. In this framework we plan to take advantage of the first Gaia data release, while preparing for the coming ones, to: i) move the first steps towards building a homogeneous data base of OCs with the high quality Gaia astrometry and photometry; ii) build, improve and test tools for the analysis of large sample of OCs; iii) use the OCs to explore the prop- erties of the disc in the solar neighborhood. Methods and Data. Using ESO archive data, we analyze the photometry and derive physical parameters, comparing data with synthetic populations and luminosity functions, of three clusters namely NGC 2225, NGC 6134 and NGC 2243. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Planetary Nebulae
Southern Planetaries 6/27/04 9:20 PM Observatory Tents Nebula Filters by Andover Ngc 60 Meade NGC60 Premier online astronomy For viewing emission and Find, compare and buy Refractor Telescope $181 shop has a selection of planetary nebulae. Telescopes! Simply Fast Free Shipping. Affiliate. observatory dome tents Narrowband and O-III types Savings www.amazon.com www.telescopes.net www.andcorp.com www.Shopping.com Observing Down Under: Part II - Planetary Nebulae by Steve Gottlieb Shapley 1 - AAO This is the second part in a series based on my trip to Australia last summer, covering observations of a few southern showpiece objects. The other parts in the series are: Southern Globular Clusters Southern Galaxies Two Southern Galaxy Groups During the stay at the Magellan Observatory I had full access to an 18" f/4.5 JMI NGT-18, an innovative split-ring truss- tube equatorial with a rotating upper cage assembly. The scope was housed in a 4.5 meter dome (which came in very handy on windy nights) and outfitted with DSC's and it could be converted to use with a bino-viewer. Because I was trying to survey the full gamut of DSO's mostly below -50° (I easily could have spent the entire time just on the Large Magellanic Cloud!), I generally stuck to eye-candy -- and there was plenty to feast on! - and was really loafing it with an 18" on these brighter planetaries (everything below was immediately visible once in the field). Some of these were reobservations for me but from northern California I never had a really good look. -
Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V
Astronomy Letters, Vol. 27, No. 4, 2001, pp. 207–212. Translated from Pis’ma v Astronomicheskiœ Zhurnal, Vol. 27, No. 4, 2001, pp. 243–249. Original Russian Text Copyright © 2001 by Dubrovich. Formation Mechanisms of “Negative”-Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V. K. Dubrovich* Special Astrophysical Observatory, Russian Academy of Sciences, pos. Nizhniœ Arkhyz, Stavropol kraœ, 357147 Russia Received June 2, 2000; in final form, October 2, 2000 Abstract—We consider the formation mechanisms of “negative”-intensity spots in the radio band for various astrophysical conditions. For wavelengths λ < 1.5 mm, the regions of reduced temperature (relative to the cos- mic microwave background radiation, CMBR) are shown to be produced only by high-redshift objects moving at peculiar velocities. The main processes are CMBR Thomson scattering and bremsstrahlung. We show that the effect δT/T can be ~ 10–5 in magnitude. We derive simple analytic expressions, which allow the redshifts, electron densities, and linear sizes of these regions to be estimated from observed spectral and spatial parame- ters. Additional observational methods for refining these parameters are outlined. © 2001 MAIK “Nauka/Inter- periodica”. Key words: theoretical and observational cosmology INTRODUCTION only two formation mechanisms of the “glow.” One of In the last 30 years, much attention has been given them is the Doppler distortion of external, equilibrium, to the search for and a detailed analysis of spatial fluc- and isotropic radiation (CMBR). For this to occur, the tuations in cosmic microwave background radiation object must have a peculiar velocity Vp and some non- zero opacity. -
The HST Key Project on the Extragalactic Distance Scale XIV
c The HST Key Project on the Extragalactic Distance Scale XIV. The Cepheids in NGC 1365' N. A. Silbermann,2 Paul Laura Ferrare~e,~Peter B. Stetson,5Barry F. Madore,' Robert C. Kennicutt, Jr.,3 Wendy L. ,Freedman,7.Jeremy R. i\/lould,' Fabio Bre~olin,~ HollandBrad E;. Gibson,' John A. Graham,"Mingsheng Han," John G. 'Based on observations with the NASA/ESA HubbleSpace Telescope obtained at the Space Telescope Science Institute, which is operated by AURA, Inc. under NASA Contract No. NAS5-265.55. 21nfrared Processing and Analysis Center, Jet Propulsion Laboratory, California Institute of Technology, MS 100-22, Pasadena, CA 91125 3Steward Observatory, University of Arizona, Tucson, A2 85721 4Hubble Fellow, California Institute of Technology, Pasadena, CA 91125 5Dominion Astrophysical Observatory, Victoria, British Columbia V8X 4M6 Canada 'NASA ExtragalacticDatabase, Infrared Processing and A4nalysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125 70bservatories of the Carnegie Institution of Washington, Pa,sadena CA 91101 'Mount Stromlo and Siding Spring Observatories, Institute of Advanced Studies, ANU, ACT 2611 Australia 'Johns Hopkins University and Space Telescope Science Institute, Baltimore, MD 21218 "Dept. of Terrestrial Magnetism, Carnegie Institution of \Va.shington, Washington D.C. 20015 "University of Wisconsin, Madison, Wisconsin 53706 -- .j ~ ABSTRACT We report the detection of Clepheicl variable stars in the barred spiral galaxy NGC 1365, located in the Fornax cluster, using the Hubble Space Telescope Wide Field and Planetary Camera 2. Twelve V (F555W) and four I (F814W) epochs of observation were obtained. The two photometry packages, ALLFRAME and DoPHOT, were separately used to obtain profile-fitting photometry of all the stars in the HST field. -
The Ara Ob1a Association: Stellar Population and Star Formation History
Astronomy & Astrophysics manuscript no. 15497 c ESO 2018 November 7, 2018 The Ara OB1a association Stellar population and star formation history G. Baume1,⋆, G. Carraro2,⋆⋆, F. Comeron3, and G. C. de El´ıa1 1 Facultad de Ciencias Astron´omicas y Geof´ısicas (UNLP), Instituto de Astrof´ısica de La Plata (CONICET, UNLP), Paseo del Bosque s/n, La Plata, Argentina e-mail: [email protected] e-mail: [email protected] 2 ESO, Alonso de Cordova 3107, Vitacura, Santiago de Chile, Chile e-mail: [email protected] 3 ESO, Karl-Schwarzschild-Strasse 2 85748 Garching bei Munchen Germany e-mail: [email protected] Received: June 10, 2010; Accepted: April 26, 2011 ABSTRACT Context. The Ara OB1a association is a nearby complex in the fourth Galactic quadrant where a number of young/embedded star clusters are projected close to more evolved, intermediate age clusters. It is also rich in interstellar matter, and contains evidence of the interplay between massive stars and their surrounding medium, such as the rim HII region NGC 6188. Aims. We provide robust estimates of the fundamental parameters (age and distance) of the two most prominent stellar clusters, NGC 6167 and NGC 6193, that may be used as a basis for studing the star formation history of the region. Methods. The study is based on a photometric optical survey (UBVIHα) of NGC 6167 and NGC 6193 and their nearby field, complemented with public data from 2MASS-VVV, UCAC3, and IRAC-Spitzer in this region. Results. We produce a uniform photometric catalogue and estimate more robustly the fundamental parameters of NGC 6167 and NGC 6193, in addition to the IRAS 16375-4854 source. -
Name Glxy Plan Glxy Mltg Glob Glob Open Glob Glxy Glxy Glxy Open
Name 評価 コメント DSO Type Mag. Size Type/ Type/Mag V(HB) RA/Dec (5~1) CenterStar/Mag 5が最高、 V(tip)/#Star 1が最低 NGC 7814 UGC 8 CGCG 456-24 MCG +3-1-20 PGC 218 Glxy 11.6b 6.3x 2.2' 135 SA(s)ab: sp RC3 00 03 15.1 +16 08 45 NGC 40 PK 120+9.1 PNG 120.0+9.8 Plan 10.7p 70.0x60.0" 11.5 3b+3 STE 00 13 00.9 +72 31 19 NGC 55 ESO 293-50 MCG -7-1-13 PGC 1014 Glxy 8.4b 32.3x 5.6' 108 SB(s)m: sp RC3 00 15 08.1 -39 12 53 NGC 70 IC 1539 UGC 174 CGCG 499-108 Arp 113 MCG +5-1-67 PGC 1194 MltG 14.2p 1.9x 1.2' 5 SA(rs)c RC3 00 18 22.6 +30 04 46 NGC 104 Glob 4 50.0' 11.7 14.1 BAA 00 24 05.2 -72 04 51 NGC 121 Glob 1.5' BAA 00 26 41.3 -71 31 24 NGC 136 Cr 4 Open 1.2' 20 13 II 1 p LYN 00 31 31.0 +61 30 36 G 1 Glob 13.7 0.5x 0.5' MAC 00 32 46.3 +39 34 41 NGC 147 UGC 326 CGCG 550-6 MCG +8-2-5 DDO 3 PGC 2004 Glxy 10.5b 13.2x 7.7' 28 E5 pec RC3 00 33 11.6 +48 30 28 NGC 185 UGC 396 CGCG 550-9 MCG +8-2-10 IRAS 362+4803 PGC 2329 Glxy 10.1b 11.9x10.1' 35 E3 pec RC3 00 38 57.7 +48 20 14 M 110 NGC 205 UGC 426 CGCG 535-14 MCG +7-2-14 IRAS PGC 2429 Glxy 8.9b 21.9x10.9' 170 E5 pec RC3 00 40 22.9 +41 41 22 NGC 231 Open 12 1.2x 1.2' 131 15 NGC 00 41 06.5 -73 21 02 M 32 NGC 221 UGC 452 CGCG 535-16 Arp 168 MCG +7-2-15 Arak 12 Glxy 9.0b 8.7x 6.4' 170 cE2 RC3 00 42 41.8 +40 51 56 M 31 NGC 224 UGC 454 CGCG 535-17 MCG +7-2-16 PGC 2557 Glxy 4.4b 192x62' 35 SA(s)b RC3 00 42 44.4 +41 16 NGC 246 PK 118- PNG 118.8- Plan 8.0p 4.1' 11.9 3b STE 00 47 03.6 -11 52 20 NGC 247 UGCA 11 ESO 540-22 MCG -4-3-5 IRAS 446- PGC 2758 Glxy 9.1v 21.4x 6.0' SAB(s)d RC3 00 47 08.7 -20 45 38 NGC 265 Kron 24 Lind -
A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques.