DOCSLIB.ORG

Skytools Chart

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Skytools Chart 36 Ara - Pavo SkyTools 3 / Skyhound.com 2 ζ 6541 NGC 6231 ζ NGC 6124 θ NGC 6322 η η 6496 ζ 1 6388 PK 345-04.1 -4 NGC 6259 NGC 6192 0° 1 ε NGC 6249 ι 1 δ α PK 342-04.1 β IC 4699 μ σ Mu Normae Cluster β2 NGC 6250 NGC 6178 NGC 6204 6352 ω NGC 6200 δ ζ λ θ α IC 4651 NGC 6193 ε ι PK 342-14.1 NGC 6134 6584 6326 NGC 6167 2 Ara γ η 6397 γ1 λ ε1 NGC 6152 α NGC 6208 1 ν μ β 5946 γ ζ NGC 6067 -50° ξ PK 331-05.1 κ 5927 PK 329-02.2 η ζ η NGC 6087 NGC 5999 NGC 5925 Pavo Globular δ 6221 ι1 ξ Collinder 292 α NGC 5822 ν λ 6300 NGC 5823 NGC 6025 π NGC 5749 6744 η PK 325-12.1 γ β β φ1 Pavo δ β NGC 5662 ρ 6362 κ ζ Circinus δ Triangulum Australe ε α Rigel Kentaurus ε 5844 2 -6 α 0 ° β NGC 5617 ζ ζ α Agena 6101 γ γ NGC 5316 ε Apus PK 315-13.1 -7 0° NGC 5281 2 1h h 5 52° x 34° 1 18h 18h00m00.0s -60°00'00" (Skymark) Globular Cl. Dark Neb. Galaxy 8 7 6 5 4 3 2 1 Globule Planetary Open Cl. Nebula 36 Ara - Pavo GALASSIE Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 6221 Ara 16h 52m 47s -59° 12' 59" +10,70 4',6x2',8 Sc 18,0 Mly --- --- --- NGC 6300 Ara 17h 16m 59s -62° 49' 11" +11,00 5',5x3',5 SBb 34,0 Mly --- --- --- NGC 6744 Pav 19h 09m 46s -63° 51' 28" +9,10 17',0x10',7 SABb 21,0 Mly --- --- --- AMMASSI APERTI Sigla Nome Cost. A.R. Dec. Mv. Dim. N° Æ Distanza 200/4 80/11,5 20x60 NGC 3114 Car 10h 02m 36s -60° 07' 12" +4,50 35',0 --- 3.000 ly --- --- --- NGC 3228 Vel 10h 21m 22s -51° 43' 42" +6,40 5',0 15 1.800 ly --- --- --- IC 2581 Car 10h 27m 29s -57° 37' 00" +5,30 5',0 --- 8.000 ly --- --- --- Cr 223 Car 10h 32m 16s -60° 01' 12" +9,40 18',0 --- 9.200 ly --- --- --- NGC 3293 Car 10h 35m 51s -58° 13' 48" +6,20 6',0 --- 7.600 ly --- --- --- NGC 3324 Car 10h 37m 20s -58° 38' 30" +6,70 12',0 --- 7.600 ly --- --- --- NGC 3330 Vel 10h 38m 46s -54° 07' 24" +8,40 4',0 30 2.900 ly --- --- --- IC 2602 Car 10h 42m 58s -64° 24' 00" +1,60 100',0 --- 520 ly --- --- --- Cr 230 Car 10h 43m 56s -59° 33' 00" +6,80 5',0 --- 8.100 ly --- --- --- Cr 228 Car 10h 44m 00s -60° 05' 12" +4,90 14',0 --- 7.200 ly --- --- --- Cr 232 Car 10h 44m 39s -59° 33' 36" +6,80 4',0 --- 7.500 ly --- --- --- Cr 231 Car 10h 44m 43s -59° 22' 00" +9,00 14',0 --- 6.000 ly --- --- --- Cr 233 Car 10h 45m 13s -59° 44' 47" +6,70 3',0 --- 13.000 ly --- --- --- Cr 235 Car 10h 56m 24s -59° 12' 00" +9,40 5',0 --- 7.500 ly --- --- --- Cr 236 Car 10h 56m 51s -61° 07' 00" +7,70 10',0 --- 2.500 ly --- --- --- NGC 3496 Car 10h 59m 36s -60° 20' 12" +9,20 8',0 60 3.200 ly --- --- --- NGC 3532 Car 11h 05m 39s -58° 45' 12" +3,40 50',0 150 1.600 ly --- --- --- NGC 3572 Car 11h 10m 23s -60° 14' 54" +4,50 5',0 35 6.500 ly --- --- --- Cr 241 Car 11h 11m 28s -60° 40' 00" +8,20 5',0 --- 4.400 ly --- --- --- Cr 240 Car 11h 11m 40s -60° 18' 35" +3,90 32',0 --- 5.100 ly --- --- --- NGC 3590 Car 11h 12m 59s -60° 47' 18" +6,80 3',0 25 5.400 ly --- --- --- NGC 3603 Car 11h 15m 07s -61° 15' 36" +9,20 4',0 30 12.000 ly --- --- --- IC 2714 Car 11h 17m 27s -62° 44' 00" +8,20 14',0 --- 4.000 ly --- --- --- Cr 246 Car 11h 19m 42s -63° 29' 00" +9,40 5',0 --- 7.200 ly --- --- --- NGC 3766 Cen 11h 36m 14s -61° 36' 30" +4,60 9',3 100 7.200 ly --- --- --- IC 2944 Cen 11h 38m 20s -63° 22' 22" +2,80 65',0 --- 5.800 ly --- --- --- NGC 3960 Cen 11h 50m 33s -55° 40' 24" +8,80 5',0 45 6.000 ly --- --- --- NGC 5281 Cen 13h 46m 35s -62° 55' 00" +8,20 7',0 40 3.600 ly --- --- --- NGC 5316 Cen 13h 53m 57s -61° 52' 06" +8,80 14',0 80 4.000 ly --- --- --- NGC 5617 Cen 14h 29m 44s -60° 42' 42" +8,50 10',0 80 6.500 ly --- --- --- NGC 5662 Cen 14h 35m 37s -56° 37' 06" +7,70 29',0 70 2.200 ly --- --- --- 1/3 36 Ara - Pavo AMMASSI APERTI Sigla Nome Cost. A.R. Dec. Mv. Dim. N° Æ Distanza 200/4 80/11,5 20x60 NGC 5749 Lup 14h 48m 53s -54° 29' 54" +8,80 10',0 30 3.400 ly --- --- --- NGC 5822 Lup 15h 04m 21s -54° 23' 48" +6,50 35',0 150 3.000 ly --- --- --- NGC 5823 Cir 15h 05m 30s -55° 36' 12" +8,60 12',0 100 3.900 ly --- --- --- NGC 5925 Nor 15h 27m 26s -54° 31' 42" +8,40 20',0 120 --- --- --- --- Cr 292 Nor 15h 50m 08s -57° 37' 00" +7,90 14',0 --- 5.400 ly --- --- --- NGC 5999 Nor 15h 52m 08s -56° 28' 24" +9,00 3',0 40 6.700 ly --- --- --- NGC 6025 TrA 16h 03m 17s -60° 25' 54" +6,00 14',0 60 2.500 ly --- --- --- NGC 6067 Nor 16h 13m 11s -54° 13' 06" +6,50 14',0 100 4.600 ly --- --- --- NGC 6087 Nor 16h 18m 50s -57° 56' 06" +6,00 14',0 40 2.900 ly --- --- --- NGC 6124 Sco 16h 25m 20s -40° 39' 12" +6,30 39',0 100 1.700 ly NGC 6134 Nor 16h 27m 46s -49° 09' 06" +8,80 6',0 --- 3.000 ly --- --- --- NGC 6152 Nor 16h 32m 45s -52° 38' 36" +8,10 25',0 70 3.400 ly --- --- --- NGC 6169 Mu Normae Cluster Nor 16h 34m 04s -44° 02' 42" +6,60 12',0 40 3.600 ly NGC 6167 Nor 16h 34m 34s -49° 46' 18" +6,60 7',0 --- 3.600 ly --- --- --- NGC 6178 Sco 16h 35m 47s -45° 38' 36" +7,20 5',0 12 3.300 ly NGC 6192 Sco 16h 40m 23s -43° 22' 00" +8,50 9',0 60 5.000 ly NGC 6193 Ara 16h 41m 20s -48° 45' 48" +5,40 14',0 --- 3.800 ly --- --- --- NGC 6200 Ara 16h 44m 07s -47° 27' 48" +8,00 14',0 40 6.700 ly NGC 6204 Ara 16h 46m 09s -47° 01' 00" +8,40 5',0 45 3.900 ly NGC 6208 Ara 16h 49m 28s -53° 43' 42" +9,50 18',0 60 3.100 ly --- --- --- NGC 6231 Sco 16h 54m 10s -41° 49' 30" +3,40 14',0 --- 4.100 ly --- --- --- MHC 6249 Sco 16h 57m 41s -44° 48' 42" +9,30 5',0 30 3.200 ly --- --- --- NGC 6259 Sco 17h 00m 45s -44° 39' 18" +8,60 14',0 120 3.400 ly --- --- --- NGC 6322 Sco 17h 18m 25s -42° 56' 00" +6,50 5',0 30 3.200 ly --- --- --- IC 4651 Ara 17h 24m 49s -49° 56' 00" +8,00 10',0 --- 2.900 ly --- --- --- AMMASSI GLOBULARI Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 5927 Lup 15h 28m 01s -50° 40' 24" +8,00 6',0 VIII 9.800 ly --- --- --- NGC 5946 Nor 15h 35m 29s -50° 39' 36" +8,40 3',0 IX 100.000 ly --- --- --- NGC 6101 Aps 16h 25m 49s -72° 12' 06" +9,20 5',0 X 68.000 ly --- --- --- NGC 6352 Ara 17h 25m 29s -48° 25' 24" +7,80 9',0 XI 64.000 ly --- --- --- NGC 6362 Ara 17h 31m 55s -67° 02' 54" +8,10 15',0 X 23.000 ly --- --- --- NGC 6388 Sco 17h 36m 17s -44° 44' 06" +6,80 10',4 III 42.000 ly --- --- --- NGC 6397 Ara 17h 40m 42s -53° 40' 24" +5,30 31',0 IX 6.500 ly --- --- --- NGC 6496 Sco 17h 59m 03s -44° 15' 48" +8,60 5',6 XII 78.000 ly --- --- --- NGC 6541 CrA 18h 08m 02s -43° 42' 54" +6,30 15',0 III 13.000 ly --- --- --- 2/3 36 Ara - Pavo AMMASSI GLOBULARI Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 6584 Tel 18h 18m 38s -52° 12' 54" +7,90 6',6 VIII 42.000 ly --- --- --- NGC 6752 Pavo Globular Pav 19h 10m 52s -59° 58' 54" +5,30 29',0 VI 20.000 ly --- --- --- NEBULOSE PLANETARIE Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 5844 TrA 15h 10m 41s -64° 40' 28" +12,00 60" --- 4.200 ly --- --- --- PK 315-13.1 Aps 15h 37m 11s -71° 54' 53" +11,80 4",9 --- 7.600 ly --- --- --- Pk 329-02.2 Nor 16h 14m 32s -54° 57' 04" +11,90 25" Ring 7.000 ly --- --- --- PK 331-05.1 Ara 16h 37m 43s -55° 42' 26" +11,90 5" Stellar Apparence < 23.000 ly --- --- --- PK 325-12.1 TrA 16h 54m 35s -64° 14' 28" +12,00 3" Stellar Apparence 12.000 ly --- --- --- PK 342-04.1 Ara 17h 19m 33s -45° 53' 17" +12,00 40" --- --- --- --- --- NGC 6326 Ara 17h 20m 46s -51° 45' 15" +12,00 15" Irregular Disk 9.400 ly --- --- --- PK 345-04.1 Sco 17h 26m 12s -44° 11' 25" +11,90 5" Stellar Apparence --- --- --- --- PK 342-14.1 Ara 18h 07m 16s -51° 01' 10" +11,90 36" --- 7.600 ly --- --- --- IC 4699 Tel 18h 18m 32s -45° 59' 02" +12,00 13" Stellar Apparence 18.000 ly --- --- --- 3/3.
Load more

Recommended publications
  • The Desert Sky Observer
    Desert Sky Observer Volume 32 Antelope Valley Astronomy Club Newsletter February 2012 Up-Coming Events February 10: Club Meeting* February 11: Moon Walk @ Prime Desert Woodlands February 13: Executive Board Meeting @ Don’s house February 18: Telescope Night and Star Party @ Devil's Punchbowl * Monthly meetings are held at the S.A.G.E. Planetarium on the Cactus School campus in Palmdale, the second Friday of each month. The meeting location is at the northeast corner of Avenue R and 20th Street East. Meetings start at 7 p.m. and are open to the public. Please note that food and drink are not allowed in the planetarium President Don Bryden Well I gave a star party and no one showed up! Not that I can blame them – it was raining and windy and cold – it even hailed! Still I dragged out the scope and got it ready to go. Briefly, between the clouds I looked at Jupiter and it was quite a treat. The Galilean moons were all tight to the planet either coming from just in front or behind. It gave a bejeweled look like a large ruby surrounded by four small diamonds. Even with the winds and clouds the sky was surprisingly steady and I went as high as 260x with ease, exposing the shadow of Europa transiting the planet. But soon more clouds came and inside we had a nice fire so I put the Artist's rendering DVD “400 Years of the Telescope” on and settled in for the night. My daughter had a few friends over after a skating party that afternoon and later when I went out for one more look they came out to see what was up.
    [Show full text]
  • Broad-Band X-Ray/Γ-Ray Spectra and Binary Parameters of GX 339
    Mon. Not. R. Astron. Soc. 000, 1–17 (1998) Printed 5 March 2018 (MN LATEX style file v1.4) Broad-band X-ray/γ-ray spectra and binary parameters of GX 339–4 and their astrophysical implications Andrzej A. Zdziarski1, Juri Poutanen2, Joanna Miko lajewska1, Marek Gierli´nski3,1, Ken Ebisawa4, and W. Neil Johnson5 1N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland 2Stockholm Observatory, S-133 36 Saltsj¨obaden, Sweden 3Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Cracow, Poland 4Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA 5E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC 20375, USA Accepted 1998 July 28. Received 1998 January 2 ABSTRACT We present X-ray/γ-ray spectra of the binary GX 339–4 observed in the hard state simultaneously by Ginga and CGRO OSSE during an outburst in 1991 September. The Ginga X-ray spectra are well represented by a power law with a photon spectral index of Γ ≃ 1.75 and a Compton reflection component with a fluorescent Fe Kα line corresponding to a solid angle of an optically-thick, ionized, medium of ∼ 0.4×2π. The OSSE data (> 50 keV) require a sharp high-energy cutoff in the power-law spectrum. The broad-band spectra are very well modelled by repeated Compton scattering in a thermal plasma with an optical depth of τ ∼ 1 and kT ≃ 50 keV. We also study the distance to the system and find it to be ∼> 3 kpc, ruling out earlier determinations of ∼ 1 kpc.
    [Show full text]
  • N6l0-Aistralian Observatory
    ^^—^^r N6L0-AISTRALIAN OBSERVATORY GAS DYNAMICS IN BARRED SPIRALS, II: NGC 7496 AND 289 V.D. Pence and C.P. BlackMn AAO PP 194 * Suonitted to: Mon.Not.R.astr.Soc. Distribution date: February, 1984 P.O. BOX 296. EPPING. N.S.W.. 2121 PHONE 868-1666. TELEX ASTRO 26230 „. *u~ - .*.SÄ._TNW. - Afto-<?(*-- ^M GAS DYNAMICS IN BARRED SPIRALS, II: NGC 7496 AND 289 W.D.Pence. Anglo-Australian Observatory. P.O. Box 296. Epplng. NSW. Australia. C.P.Blactanan. Department of Astronomy. Edinburgh University. Received t SUMMAKT - The gas velocity fields in the barred spiral galaxies NGC 7496 and 289 have been measured by means of long-slit spectra obtained with the Anglo-Australian Telescope. Pronounced deviations fro« circular motion of the type predicted by recent theoretical mooels are seen in NGC 74961 the isovelocity contours are distorted into a characteristic S-shaped pattern and there is a large velocity gradient across the bar. The velocity field is virtually identical to that of a previously observed barred spiral, NGC 5383 for which a number of models have been published. The nuclear [OUI] emission lines are very asymmetric with a wing extending to about 1000 km s-1 to the blue of the systemic velocity; this wing is only faintly seen in the Balmer lines. NGC 289 has a much smaller bar *nd consequently the noncircular motions are less pronounced. The most obvious effect is that the Xinematic major and minor axes are not perpendicular which is a signature of oval distortions. Both galaxies have a mass (within the 10 outermost velocity measurement) of 9 x iO M0 and M/Lß » 6.
    [Show full text]
  • 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.
    [Show full text]
  • The Gaia-ESO Survey: Membership Probabilities for Stars in 32 Open Clusters from 3D Kinematics
    MNRAS 496, 4701–4716 (2020) doi:10.1093/mnras/staa1749 Advance Access publication 2020 June 19 The Gaia-ESO Survey: membership probabilities for stars in 32 open clusters from 3D kinematics R. J. Jackson,1‹ R. D. Jeffries,1‹ N. J. Wright,1 S. Randich,2 G. Sacco,2 E. Pancino ,2 T. Cantat-Gaudin,3 G. Gilmore,4 A. Vallenari,5 T. Bensby,6 A. Bayo,7,10 M. T. Costado,8 E. Franciosini,2 A. Gonneau,4 A. Hourihane,4 J. Lewis,4 L. Monaco,9 L. Morbidelli2 and C. Worley4 Downloaded from https://academic.oup.com/mnras/article/496/4/4701/5859956 by Universidad Andres Bello user on 27 August 2021 1Astrophysics Group, Keele University, Keele, Staffordshire ST5 5BG, UK 2INAF – Osservatorio Astrofisco di Arcetri, Largo E. Fermi, 5, I-50125 Firenze, Italy 3Institut de Ciencies` del Cosmos, Universitat de Barcelona (IEEC-UB), Mart´ı i Franques` 1, E-08028 Barcelona, Spain 4Institute of Astronomy, Cambridge University, Madingley Road, Cambridge CB3 0H, UK 5INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy 6Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, SE-221 00 Lund, Sweden 7Instituto de F´ısica y Astronom´ıa, Facultad de Ciencias, Universidad de Valpara´ıso, Av. Gran Bretana˜ 1111, 5030 Casilla, Valpara´ıso, Chile 8Departamento de Didactica,´ Universidad de Cadiz,´ E-11519 Puerto Real, Cadiz,´ Spain 9Departamento de Ciencias Fisicas, Universidad Andres Bello, Fernandez Concha 700, Las Condes, Santiago, Chile 10Nucleo´ Milenio Formacion´ Planetaria - NPF, Universidad de Valpara´ı Avenida Errazuriz´ 1834, Valpara´ıso, Chile Accepted 2020 June 12.
    [Show full text]
  • A Photometric and Spectroscopic Study of the Southern Open Clusters Pismis 18, Pismis 19, Ngc 6005, and Ngc 6253 Andre S E
    THE ASTRONOMICAL JOURNAL, 116:801È812, 1998 August ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. A PHOTOMETRIC AND SPECTROSCOPIC STUDY OF THE SOUTHERN OPEN CLUSTERS PISMIS 18, PISMIS 19, NGC 6005, AND NGC 6253 ANDRE S E. PIATTI1,2 AND JUAN J. CLARIA 2 Observatorio Astrono mico, Universidad Nacional de Co rdoba, Laprida 854, 5000 Co rdoba, Argentina; andres=oac.uncor.edu, claria=oac.uncor.edu EDUARDO BICA2 Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, C.P. 15051, Porto Alegre, 91500-970, RS, Brazil; bica=if.ufrgs.br DOUG GEISLER Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732, Tucson, AZ 85726; doug=noao.edu AND DANTE MINNITI Lawrence Livermore National Laboratory, L-413, P.O. Box 808, Livermore, CA 94550; dminniti=igpp.llnl.gov Received 1997 October 3; revised 1998 April 24 ABSTRACT CCD observations in the B, V , and I passbands have been used to generate color-magnitude diagrams (CMDs) for the southern open cluster candidates Pismis 18, Pismis 19, and NGC 6005, as well as for the old open cluster NGC 6253. The sample consists of about 1550 stars reaching down to V D 19 mag. From analysis of the CMDs, the physical reality of the three cluster candidates is conÐrmed and their reddening, distance, and age are derived, as well as those of NGC 6253. In addition, integrated spectra for Pismis 18, Pismis 19, and NGC 6253 covering a range from 3500 to 9200A were obtained. The reddening, age, and metallicity of these three clusters were derived from Balmer and Ca II triplet equiva- lent widths by comparing the observed spectra with those of template clusters.
    [Show full text]
  • 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.
    [Show full text]
  • 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).
    [Show full text]
  • All Charts 2010.Pdf
    The Evening Sky in October 2020 Four planets light up the evening sky most of the month. Jupiter and Mars are the brightest 'stars' in the sky, so the first seen after sunset. Golden Jupiter is northwest of overhead. Orange Mars is low in the eastern sky. As the sky darkens Saturn appears to the right of Jupiter. Mercury is low in the southwest, looking like a lone bright star. It fades into the twilight after the 20th. Of the four, Jupiter and Saturn are the most interesting in telescopes. Even a small telescope shows Jupiter's disk. Larger 'scopes will show the parallel bands in Jupiter's clouds. Jupiter's four big moons are lined up on either side of the planet, swapping positions from night to night. Jupiter is 760 million km from us mid-month. Saturn appears as an oval in a low-powered telescope as the rings and planet merge. Larger telescopes show the rings and Saturn's biggest moon Titan four ring-diameters from the planet. Smaller moons are closer in. Saturn is 1480 million km away. The moon will be near Jupiter and Saturn on the 22nd and 23rd. Mars is at its closest to Earth mid-month, 63 million km away. In a telescope it is a small disk with some dusky markings. Mercury is catching up on us most of the month. It then passes between us and the sun on the 25th and moves into the dawn sky. The Moon will be near Mars on the 3rd, and near Mercury on the 18th.
    [Show full text]
  • On the Metallicity of Open Clusters III
    A&A 585, A150 (2016) Astronomy DOI: 10.1051/0004-6361/201526370 & c ESO 2016 Astrophysics On the metallicity of open clusters III. Homogenised sample M. Netopil1, E. Paunzen1, U. Heiter2, and C. Soubiran3 1 Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlárskᡠ2, 611 37 Brno, Czech Republic e-mail: [email protected] 2 Institutionen för fysik och astronomi, Uppsala universitet, Box 516, 751 20 Uppsala, Sweden 3 Université de Bordeaux − CNRS, LAB − UMR 5804, BP 89, 33270 Floirac, France Received 21 April 2015 / Accepted 20 November 2015 ABSTRACT Context. Open clusters are known as excellent tools for various topics in Galactic research. For example, they allow accurately tracing the chemical structure of the Galactic disc. However, the metallicity is known only for a rather low percentage of the open cluster population, and these values are based on a variety of methods and data. Therefore, a large and homogeneous sample is highly desirable. Aims. In the third part of our series we compile a large sample of homogenised open cluster metallicities using a wide variety of different sources. These data and a sample of Cepheids are used to investigate the radial metallicity gradient, age effects, and to test current models. Methods. We used photometric and spectroscopic data to derive cluster metallicities. The different sources were checked and tested for possible offsets and correlations. Results. In total, metallicities for 172 open cluster were derived. We used the spectroscopic data of 100 objects for a study of the radial metallicity distribution and the age-metallicity relation. We found a possible increase of metallicity with age, which, if confirmed, would provide observational evidence for radial migration.
    [Show full text]
  • 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.
    [Show full text]
  • Pulsating Stars in the ASAS-3 Database. I. Β Cephei Stars
    ACTA ASTRONOMICA Vol. 55 (2005) pp. 219–236 Pulsating Stars in the ASAS-3 Database. I. β Cephei Stars by A. Pigulski Astronomical Institute, Wrocław University, ul. Kopernika 11, 51-622 Wrocław, Poland e-mail: [email protected] Received May 30, 2005 ABSTRACT We present results of an analysis of the ASAS-3 data for short-period variables from the re- cently published catalog of over 38000 stars. Using the data available in the literature we verify the results of the automatic classification related to β Cep pulsators. In particular, we find that 14 stars in the catalog can be classified unambiguously as new β Cep stars. By means of periodogram analysis we derive the frequencies and amplitudes of the excited modes. The main modes in the new β Cep stars have large semi-amplitudes, between 35 and 80 mmag. Up to four modes were found in some stars. Two (maybe three) new β Cep stars are members of southern young open clusters: ASAS 164409−4719.1 belongs to NGC6200, ASAS164630−4701.2 is a member of Hogg22, and ASAS 164939−4431.7 could be a member of NGC6216. We also analyze the photometry of four known β Cep stars in the ASAS-3 catalog, namely ILVel, NSV24078, V1449Aql and SYEqu. Finally, we discuss the distribution of β Cep stars in the Galaxy. Key words: Stars: early type – Stars: oscillations – Stars: variables: other 1. Introduction The idea of monitoring the whole sky for variability with small wide-field cam- eras, initiated and popularized by Paczynski´ (1997, 2000, 2001), resulted in several successful projects of which the All Sky Automated Survey (ASAS) conducted by Dr.
    [Show full text]