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WelcomeWelcome toto thethe SpaceSpace TelescopeTelescope ScienceScience InstituteInstitute’’ss PublicPublic LectureLecture SeriesSeries zz YourYour host:host: MaxMax MutchlerMutchler zz LithographsLithographs onon tabletable z PleasePlease taketake oneone perper personperson TONIGHT TransNeptunianTransNeptunian BinariesBinaries andand CollisionCollision Families:Families: ProbesProbes ofof OurOur LocalLocal DustDust DiskDisk SusanSusan BenecchiBenecchi MayMay 5,5, 20092009 88 PMPM STScISTScI AuditoriumAuditorium UpcomingUpcoming TalksTalks zz JuneJune 2,2, 20092009 –– JasonJason TumlinsonTumlinson,, TheThe InvisibleInvisible Galaxy:Galaxy: NewNew ViewsViews ofof thethe MilkyMilky WayWay zz JulyJuly 7,7, 20092009 –– DouglasDouglas Long,Long, TheThe MysteryMystery ofof thethe ‘‘BeBe’’ StarsStars WebWeb SiteSite && WebcastWebcast • Google “hubble lecture” • http://hubblesite.org/go/talks • List of upcoming speakers • Link to current webcast • Links to previous webcasts Scientific Symposium May 4-7 Public Lecture May 8 at 7:00 PM at the Maryland Science Center: Dr. Steven Squyers (Cornell): Roving Mars Hubble Servicing Mission 4 Launch currently set for May 11, 2009 Two Space Shuttles sitting on the launch pad Hubble was deployed and is serviced by the Space Shuttle 1990 1993 1997 1999 2002 2009 5 days of spacewalking! Hubble mission milestones as chronicled by it’s workhorse: Wide Field Planetary Camera 2 (WFPC2, to be replaced with WFC3) “Top 10 reasons why the Hubble telescope isn’t working…” WFPC2 installed during servicing mission 1 in December 1993 WFPC2 from 1993-2001: The camera that made Hubble famous Comet Shoemaker-Levy 9 impacts Jupiter… and Hubble’s comeback story begins! WF2 camera Eagle Nebula Hubble’s quirky WFPC2 images become icons PC1 camera WF3 camera WF4 camera Hubble Deep Field Advanced Camera installed during servicing mission 3B in March 2002… …and failed in January 2007! WFPC2 from 2007-2009: Back to the future, and finishing strong! NGC 2440 in January 2007 First image taken after ACS failure NGC 2074 in the Tarantula Nebula Hubble’s 100,000th orbit in August 2008 Arp 147 “perfect 10” merging galaxies Hubble is “back in business” after failure in Oct 2008 Arp 194 merging galaxies Hubble’s 19th Anniversary on April 24, 2009 OurOur FeaturedFeatured SpeakerSpeaker SusanSusan BenecchiBenecchi TransNeptunianTransNeptunian BinariesBinaries andand CollisionCollision Families:Families: ProbesProbes ofof OurOur LocalLocal DustDust DiskDisk.

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Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis,
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Download the 2016 Spring Deep-Sky Challenge
Deep-sky Challenge 2016 Spring Southern Star Party Explore the Local Group Bonnievale, South Africa Hello! And thanks for taking up the challenge at this SSP! The theme for this Challenge is Galaxies of the Local Group. I’ve written up some notes about galaxies & galaxy clusters (pp 3 & 4 of this document). Johan Brink Peter Harvey Late-October is prime time for galaxy viewing, and you’ll be exploring the James Smith best the sky has to offer. All the objects are visible in binoculars, just make sure you’re properly dark adapted to get the best view. Galaxy viewing starts right after sunset, when the centre of our own Milky Way is visible low in the west. The edge of our spiral disk is draped along the horizon, from Carina in the south to Cygnus in the north. As the night progresses the action turns north- and east-ward as Orion rises, drawing the Milky Way up with it. Before daybreak, the Milky Way spans from Perseus and Auriga in the north to Crux in the South. Meanwhile, the Large and Small Magellanic Clouds are in pole position for observing. The SMC is perfectly placed at the start of the evening (it culminates at 21:00 on November 30), while the LMC rises throughout the course of the night. Many hundreds of deep-sky objects are on display in the two Clouds, so come prepared! Soon after nightfall, the rich galactic fields of Sculptor and Grus are in view. Gems like Caroline’s Galaxy (NGC 253), the Black-Bottomed Galaxy (NGC 247), the Sculptor Pinwheel (NGC 300), and the String of Pearls (NGC 55) are keen to be viewed.
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Curriculum Vitae of You-Hua Chu
Curriculum Vitae of You-Hua Chu Address and Telephone Number: Institute of Astronomy and Astrophysics, Academia Sinica 11F of Astronomy-Mathematics Building, AS/NTU No.1, Sec. 4, Roosevelt Rd, Taipei 10617 Taiwan, R.O.C. Tel: (886) 02 2366 5300 E-mail address: [email protected] Academic Degrees, Granting Institutions, and Dates Granted: B.S. Physics Dept., National Taiwan University 1975 Ph.D. Astronomy Dept., University of California at Berkeley 1981 Professional Employment History: 2014 Sep - present Director, Institute of Astronomy and Astrophysics, Academia Sinica 2014 Jul - present Distinguished Research Fellow, Institute of Astronomy and Astrophysics, Academia Sinica 2014 Jul - present Professor Emerita, University of Illinois at Urbana-Champaign 2005 Aug - 2011 Jul Chair of Astronomy Dept., University of Illinois at Urbana-Champaign 1997 Aug - 2014 Jun Professor, University of Illinois at Urbana-Champaign 1992 Aug - 1997 Jul Research Associate Professor, University of Illinois at Urbana-Champaign 1987 Jan - 1992 Aug Research Assistant Professor, University of Illinois at Urbana-Champaign 1985 Feb - 1986 Dec Graduate College Scholar, University of Illinois at Urbana-Champaign 1984 Sep - 1985 Jan Lindheimer Fellow, Northwestern University 1982 May - 1984 Jun Postdoctoral Research Associate, University of Wisconsin at Madison 1981 Oct - 1982 May Postdoctoral Research Associate, University of Illinois at Urbana-Champaign 1981 Jun - 1981 Aug Postdoctoral Research Associate, University of California at Berkeley Committees Served:
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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
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The Changing Role of the 'Catts
Journal of Astronomical History and Heritage , 13(3), 235-254 (2010). THE CHANGING ROLE OF THE ‘CATTS TELESCOPE’: THE LIFE AND TIMES OF A NINETEENTH CENTURY 20-INCH GRUBB REFLECTOR Wayne Orchiston Centre for Astronomy, James Cook University, Townsville, Queensland 4811, Australia. [email protected] Abstract: An historic 20-in (50.8-cm) Grubb reflector originally owned by the London amateur astronomer, Henry Ellis, was transferred to Australia in 1928. After passing through a number of amateur owners the Catts Telescope— as it became known locally—was acquired by Mount Stromlo Observatory in 1952, and was then used for astrophysical research and for site-testing. In the mid-1960s the telescope was transferred to the University of Western Australia and was installed at Perth Observatory, but with other demands on the use of the dome it was removed in 1999 and placed in storage, thus ending a century of service to astronomy in England and Australia. Keywords: Catts Telescope, Henry Ellis, Walter Gale, Mount Stromlo Observatory, Mount Bingar field station, photoelectric photometry, spectrophotometry, Lawrence Aller, Bart Bok, Priscilla Bok, Olin Eggen, Don Faulkner, John Graham, Arthur Hogg, Gerald Kron, Pamela Kennedy, Antoni Przybylski, David Sher, Robert Shobbrook, Bengt Westerlund, John Whiteoak, Frank Bradshaw Wood. 1 INTRODUCTION what of other telescopes, like the 20-in (50.8-cm) ‘Catts Telescope’? After passing from amateur owner- One of the roles of the Historic Instruments Working ship to Mount Stromlo Observatory in 1952, this was Group of the IAU is to assemble national master lists used over the following twelve years to make a valu- of surviving historically-significant telescopes and able contribution to astrophysics and to provide data auxiliary instrumentation, and at the 2000 General for five different Ph.D.
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The Fraction of Stars That Form in Clusters in Different Galaxies
Draft version August 5, 2021 Typeset using LATEX preprint style in AASTeX62 The Fraction of Stars That Form in Clusters in Different Galaxies Rupali Chandar,1 S. Michael Fall,2 Bradley C. Whitmore,2 and Alexander J. Mulia1 1Department of Physics & Astronomy, University of Toledo, Toledo, OH 43606 2Space Telescope Science Institute, Baltimore, MD, 21218 USA ABSTRACT We estimate the fraction of stars that form in compact clusters (bound and unbound), ΓF , in a diverse sample of eight star-forming galaxies, including two irregulars, two dwarf starbursts, two spirals, and two mergers. The average value for our sample is ΓF ≈ 24 ± 9%. We also calculate the fraction of stars in clusters that survive to ages between τ1 and τ2, denoted by ΓS(τ1; τ2), and find ΓS(10; 100) = 4:6 ± 2:5% and ΓS(100; 400) = 2:4±1:1%, significantly lower than ΓF for the same galaxies. We do not find any systematic trends in ΓF or ΓS with the star formation rate (SFR), the SFR per unit area (ΣSF R), or the surface density of molecular gas (ΣH2 ) within the host galaxy. Our results are consistent with those found previously from the CMF=SFR statistic (where CMF is the cluster mass function), and with the quasi-universal model in which clusters in different galaxies form and disrupt in similar ways. Our results, however, contradict many previous claims that the fraction of stars in bound clusters increases strongly with ΣSF R and ΣH2 . We find that the previously reported trends are largely driven by comparisons that mixed ΓF ≈ ΓS(0; 10) and ΓS(10; 100), where ΓS(0; 10) was systematically used for galaxies with higher ΣSF R and ΣH2 , and ΓS(10; 100) for galaxies with lower ΣSF R and ΣH2 .
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Skytools Chart
33 Dorado - Carina SkyTools 3 / Skyhound.com NGC 2546 ν α - ζ 40° σ α δ Puppis η2 Collinder 173 τ β 2 γ Canopus γ1 1433 NGC 2547 Horologium Pictor γ δ IC 2395 γ NGC 2670 χ α 1566 -5 0° ζ 1553 1549 ο NGC 2669 1672 IC 2391 δ ε α β 1261 Carina NGC 2516 ε Dorado ι α δ 2 γ η 1559 δ 1978 1866 1818 1783 NGC 1955 1805 Reticulum IC 2488 θ 2867 2164 κ ι NGC 1962 Large Magellanic Cloud β δ 2210 PK 278-06.1 Volans NGC 1874 NGC 1965 β NGC 1770 Tarantula Nebula NGC 1876 IC 2501 2031 β γ2 1313 ε -60° 2808 α NGC 3114 ζ Mensa ζ α υ PK 285-09.1 IC 2448 ε 1 β 0 -70° h 3211 h 0 02 8 52° x 34° 6h γ h 0 δ 06h00m00.0s -60°00'00" (Skymark) Globular Cl. Dark Neb. Galaxy 8 7 6 5 4 3 2 1 Globule Planetary Open Cl. Nebula 33 Dorado - Carina GALASSIE Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 1313 Ret 03h 18m 15s -66° 29' 51" +9,70 9',5x7',2 SBcd 13,5 Mly --- --- --- NGC 1433 Hor 03h 42m 02s -47° 13' 19" +10,80 6',2x3',6 Sba 43,0 Mly --- --- --- NGC 1549 Dor 04h 15m 45s -55° 35' 32" +10,70 5',0x4',3 E 42,0 Mly --- --- --- NGC 1553 Dor 04h 16m 10s -55° 46' 51" +10,30 6',2x4',1 S0 28,0 Mly --- --- --- NGC 1559 Ret 04h 17m 36s -62° 47' 01" +11,00 4',2x2',1 SBc 34,0 Mly --- --- --- NGC 1566 Dor 04h 20m 04s +54° 56' 16" +10,30 8',1 4',8 34,0 Mly --- --- --- NGC 1672 Dor 04h 45m 43s -59° 14' 51" +10,30 6',6x5',4 Sb 270,0 Mly --- --- --- PGC 17223 Large Magellanic Cloud Dor 05h 23m 35s -69° 45' 22" +0,80 648',0x552',0 SBm 0,2 Mly --- --- --- AMMASSI APERTI Sigla Nome Cost.
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Article Published in Amateur Astronomy #64 On
Amateur Astronomy 6464 News for, by, and about Amateur Astronomers around the world! Winter 2009 Australian Skies - Deepest South Texas Star Safari by Charlie Warren On The Moon * Shooting At Centaurus * Solar Sketching - Scientific Art * Ripples in Elipticals * People in Astronomy * Searching For The Great Attractor * ATM Pipe Dreams * Deepest South Texas Star Safari * Their Little Tectron * Pine Mountain Observatory Workshop * Portland Alt / Az Workshop * Inexpensive, Fun & Functional Astro Trailer * Star Party Calendar * Shorts From Down Under * Astro Trivia * Deep Sky Treasures * Observing and Imaging Virtually Unknown Super Nova Remnants *Alternate Universe * Reader's Forum *Short Subjects *Star People DeepestDeepest SouthSouth TTexasexas SStartar SafariSafari Article & Photos by Charlie Warren Group photo of the DSTSS 2009 participants: Front Row (left to right) - Charlie Warren, David Moody, Anne Adkins, Gary Kopff Middle row (L to R):Fred Koch, Brad Young, John Bozeman, Mark Lyon, Beth Moody, Mai Tran, Joan Fry, John Bambury, William & Carol Warfield, Back row (L to R) Paul Winalski, Eliot Lyon, Lachlan MacDonald (on ladder), Robert Werkman, Becky & Bob Hill, Jason Fry, Tony Buckley, Mike Roos, Bruce Sayre, Andrew Murrell, Bob Douglas, Petra deRuyter & David Chandler he Deepest South Texas Star Safari is an event I can highly our Australian sky guides and scopes were Andrew Murrell, John Bambury, T recommend to all who can work (18”-30”) that were set up. The equip- Gary Kopff and Mai Tran of Argo T ment set up for our use included; a 30- out the costs and logistics. It probably Navis, and Peter Read of SDM tele- represents one of the best values in inch f/4.5 SDM dobsonian, two 25's, scopes.
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Near-Infrared Color Evolution of LMC Clusters
A&A 409, 479–484 (2003) Astronomy DOI: 10.1051/0004-6361:20031136 & c ESO 2003 Astrophysics Near-infrared color evolution of LMC clusters J.-M. Kyeong1, M.-J. Tseng2, and Y.-I. Byun3 1 Korea Astronomy Observatory, Taejon, 305-348, Korea 2 Institute of Astronomy, National Central University, Chung-Li, 32054, Taiwan, ROC 3 Yonsei University Observatory and Department of Astronomy, Yonsei University, Seoul, 120-749, Korea Received 5 May 2003 / Accepted 7 July 2003 Abstract. We present here the digital aperture photometry for 28 LMC clusters whose ages are between 5 Myr and 12 Gyr. This photometry is based on our imaging observations in JHK and contains integrated magnitudes and colors as a function of aperture radius. In contrast to optical colors, our near-infrared colors do not show any strong dependence on cluster ages. Key words. galaxies: photometry – galaxies: Magellanic Clouds – galaxies: star clusters – infrared: stars 1. Introduction Previous eﬀort in near-infrared includes Persson et al. (1983, hereafter Persson83) and Ferraro et al. (1995). Star clusters of the Large Magellanic Cloud (LMC) provide ex- Persson83 studied the integrated light of 84 clusters in the cellent templates for studies of stellar populations in external Large and Small Magellanic Clouds using a single cell pho- galaxies. The LMC is close enough that star clusters within the toelectric aperture photometry. In contrast to the UV and opti- galaxy can be resolved into individual stars by high spatial res- cal clusters colors which vary smoothly with age, their infrared olution imaging from both ground and space based telescopes. integrated colors display a large scatter among a given SWB Their CMDs can be used for detailed age calibration.
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Identifying Young Stellar Objects in Nine Large Magellanic Cloud Star-Forming Regions
A&A 542, A66 (2012) Astronomy DOI: 10.1051/0004-6361/201118627 & c ESO 2012 Astrophysics Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions L. R. Carlson1,M.Sewiło2, M. Meixner3,K.A.Romita4, and B. Lawton3 1 Leiden Observatory, Leiden, The Netherlands e-mail: [email protected] 2 Johns Hopkins University, Baltimore, 3400 N. Charles St., Baltimore, MD, USA 3 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, USA 4 University of Florida, Gainesville, FL, USA Received 12 December 2011 / Accepted 13 March 2012 ABSTRACT We introduce a new set of selection criteria for the identiﬁcation of infrared bright young stellar object (YSO) candidates and apply them to nine Hii regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, AJ, 132, 2268), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997, AJ, 114, 1002) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, PASJ, 59, 615). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention.
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Newsletter 2018-4 September 2018
Newsletter 2018-4 September 2018 www.variablestarssouth.org Freyberg High School student Joseph Chamberlain undertook a project to measure the period of the WASP-17b exoplanet under the guidance of Carl Knight, VSS’s new Education Liaision Officer. Contents From the Director - Mark Blackford .................................................................................................................................................................. 2 Ranald McIntosh (1933-2018) ................................................................................................................................................................................ 3 Correct placement of five Innes variables – Mati Morel ......................................................................................................... 4 A funny thing happened on the way to the observatory the other night – Mark Blackford .......... 9 Student project: give it a go! – Carl Knight ..........................................................................................................................................11 The mystery of WASP-17b – the story of an exercise in mentoring – Joseph Chamberlain ..... 15 T Sagittarii - what’s hidden in the light curve – Stan Walker ......................................................................................... 18 Re-interpretation of the published O-C diagrams of the delta Scuti Star ZZ Microscopii, and further personal DSLR photometric observations – Roy Axelsen ...........................................................
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Southern Objects Paging
Southern Objects in Turn Left at Orion , 5th edition (by page in the book) Page Name Constellation Type RA Dec. 210 NGC 220 Tucana Open Cluster 0 H 40.5 min. −73° 24' 210 NGC 222 Tucana Open Cluster 0 H 40.7 min. −73° 23' 210 NGC 231 Tucana Open Cluster 0 H 41.1 min. −73° 21' 210 NGC 249 Tucana Diffuse Nebula 0 H 45.5 min. −73° 5' 210 NGC 261 Tucana Diffuse Nebula 0 H 46.5 min. −73° 6' 210 NGC 265 Tucana Open Cluster 0 H 47.2 min. −73° 29' 210 NGC 330 Tucana Open Cluster 0 H 56.3 min. −72° 28' 210 NGC 346 Tucana Diffuse Nebula 0 H 59.1 min. −72° 11' 210 NGC 371 Tucana Open Cluster 1 H 3.4 min. −72° 4' 210 NGC 376 Tucana Open Cluster 1 H 3.9 min. −72° 49' 210 NGC 395 Tucana Open Cluster 1 H 5.1 min. −72° 0' 210 NGC 419 Tucana Globular Cluster 1 H 8.3 min −72° 53' 210 NGC 456 Tucana Diffuse Nebula 1 H 14.4 min. −73° 17' 210 NGC 458 Tucana Open Cluster 1 H 14.9 min. −71° 33' 210 NGC 460 Tucana Open Cluster 1 H 14.6 min. −73° 17' 210 NGC 465 Tucana Open Cluster 1 H 15.7 min. −73° 19' 210 Small Magellanic Cloud Tucana Galaxy 0 H 53.0 min −72° 50' 212 NGC 104, 47 Tucanae Tucana Globular Cluster 0 H 24.1 min −62° 58' 214 NGC 362 Tucana Globular Cluster 1 H 3.2 min −70° 51' 215 Beta Tucanae Tucana Double Star 0 H 31.5 min.
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