DOCSLIB.ORG

The Flamsteed Collection

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

The Flamsteed Collection Compiled by Richard Dibon-Smith © 2001-2012 Richard Dibon-Smith all rights reserved Andromeda (I) AND HD HIP α δ B-V µ(α)″ µ(δ)″ µ″ Dir Spect. Var? α 358 677 00h08m23.2 s +29º05′26″ -0.038 0.1357 -0.1630 0.212 140º B9IV:pHgMn (ACV) β 6860 5447 01 09 43.9 +35 37 14 1.576 0.1756 -0.1122 0.208 123 M0IIIvar γ1 12533 9640A 02 03 53.9 +42 19 47 1.370 0.0431 -0.0509 0.067 140 K3IIb γ2B 12534 9640B 02 03 54.7 +42 19 51 0.030 0.0431 -0.0509 0.067 140 B9V γ2C 12534 9640C 02 03 54.7 +42 19 51 0.030 0.0431 -0.0509 0.067 140 A0V δ 3627 3092 00 39 19.6 +30 51 40 1.268 0.1154 -0.0831 0.142 126 K3III ε 3546 3031 00 38 33.3 +29 18 43 0.871 -0.2294 -0.2541 0.342 222 G5IIIcomp ζ 4502 3693 00 47 20.3 +24 16 02 1.100 -0.1012 -0.0819 0.130 231 K1II (EB/GS) η 5516 4463 00 57 12.4 +23 25 04 0.940 -0.0437 -0.0461 0.064 224 G8III-IV ϑ 1280 1366 00 17 05.4 +38 40 54 0.059 -0.0500 -0.0179 0.053 250 A2V ι 222173 116631 23 38 08.1 +43 16 05 -0.083 0.0277 -0.0012 0.028 92 B8V κ 222439 116805 23 40 24.4 +44 20 02 -0.071 0.0813 -0.0190 0.084 103 B9IVn λ 222107 116584 23 37 33.8 +46 27 30 0.984 0.1592 -0.4215 0.451 159 G8III-IV (RS) µ 5448 4436 00 56 45.1 +38 29 58 0.130 0.1528 0.0368 0.157 76 A5V ν 4727 3881 00 49 48.8 +41 04 44 -0.136 0.0227 -0.0181 0.029 129 B5V SB ξ 8207 6411 01 22 20.3 +45 31 44 1.077 0.0322 0.0087 0.033 75 K0III-IV οΑ 217675 113726A 23 01 55.2 +42 19 34 -0.099 0.0225 0.0002 0.022 89 B6IIIpe+A2p (GCAS) οΒ 217675 113726B 23 01 55.2 +42 19 34 -0.099 0.0225 0.0002 0.022 89 – π 3369 2912 00 36 52.8 +33 43 10 -0.123 0.0152 -0.0036 0.016 103 B5V ρ 1671 1686 00 21 07.2 +37 58 07 0.442 0.0583 -0.0397 0.071 124 F5III σ 1404 1473 00 18 19.6 +36 47 07 0.054 -0.0665 -0.0425 0.079 237 A2V τ 10205 7818 01 40 34.7 +40 34 37 -0.068 0.0167 -0.0235 0.029 145 B8III υ 9826 7513 01 36 47.8 +41 24 20 0.536 -0.1726 -0.3810 0.418 204 F8V ϕΑ 6811 5434A 01 09 30.1 +47 14 31 0.012 0.0038 -0.0130 0.014 164 B7III ϕΒ 6811 5434B 01 09 30.2 +47 14 30 0.012 0.0077 -0.0100 0.013 142 – χ 10072 7719 01 39 20.9 +44 23 10 0.883 -0.0205 0.0150 0.025 306 G8III ψ 223047 117221 23 46 02.0 +46 25 13 1.086 0.0091 -0.0063 0.011 125 G5Ib ω 8799 6813 01 27 39.2 +45 24 25 0.421 0.3570 -0.1093 0.373 107 F5IV 2AAnd 217782 113788A 23 02 36.2 +42 45 28 0.094 0.0557 -0.0048 0.056 95 A3Vn 2BAnd — 113788B 23 02 36.2 +42 45 29 0.094 0.0557 -0.0048 0.056 95 – 3 And 218031 113919 23 04 10.9 +50 03 08 1.058 0.1667 0.1673 0.236 45 K0III 4 And 218452 114200 23 07 39.2 +46 23 14 1.409 -0.0119 -0.0300 0.032 202 K5III 5 And 218470 114210 23 07 45.3 +49 17 45 0.449 0.1522 0.1321 0.201 49 F5V 6 And 218804 114430 23 10 27.1 +43 32 40 0.450 -0.2022 -0.2077 0.290 224 F5IV 7 And 219080 114570 23 12 32.9 +49 24 23 0.302 0.0898 0.0956 0.131 43 F0V 8 And 219734 115022 23 17 44.6 +49 00 55 1.668 0.0345 0.0067 0.035 79 M2III 9 And 219815 115065 23 18 23.4 +41 46 25 0.215 -0.0096 -0.0110 0.015 221 A7m AN(EB) 10 And 219981 115191 23 19 52.3 +42 04 41 1.512 0.0478 0.0043 0.048 85 M0III 11 And 219945 115152 23 19 29.7 +48 37 32 1.014 0.0230 0.0519 0.057 24 K0III 12 And 220117 115280 23 20 53.2 +38 10 56 0.468 0.1296 -0.0612 0.143 115 F5V 13 And 220885 115755 23 27 07.3 +42 54 43 -0.007 0.0874 0.0171 0.089 79 B9III 14 And 221345 116076 23 31 17.3 +39 14 11 1.029 0.2873 -0.0838 0.299 106 K0III 15 And 221756 116354 23 34 37.5 +40 14 12 0.096 -0.0177 -0.0458 0.049 201 A1III V340(DSCT) 18 And 222304 116709 23 39 08.3 +50 28 18 -0.061 -0.0167 -0.0019 0.017 264 B9V 22 And 571 841 00 10 19.2 +46 04 20 0.405 0.0045 0.0002 0.005 87 F2II 23 And 905 1086 00 13 30.8 +41 02 08 0.331 -0.1228 -0.1469 0.191 220 F0IV 26 And 1438 1501 00 18 42.1 +43 47 28 -0.074 0.0233 -0.0027 0.023 97 B8V 28 And 2628 2355 00 30 07.3 +29 45 06 0.271 0.0436 -0.0572 0.072 143 A7III GN(DSCT) 32 And 3817 3231 00 41 07.1 +39 27 31 0.891 -0.0144 -0.0030 0.015 258 G8III 36AAnd 5286 4288A 00 54 58.0 +23 37 42 1.012 0.1371 -0.0456 0.144 108 K1IV 2 Andromeda (I) AND m M π pc l.y. V RV L F mc Bin? ADS α 2.07 -0.30 0.0336″ 30 97 32 -12 104 21 H V 32 94 β 2.07 -1.86 0.0164 61 199 60 0 437 43 Barnard 949 γ1 2.33 -2.86 0.0092 109 355 36 -12 1092 57 2.10 Σ 205 1630AxBC γ2B 5.50 -0.16 0.0092 109 355 37 -14 91 57 5.02 ΟΣ 38 1630B γ2C 6.30 -0.16 0.0092 109 355 34 - 91 57 ΟΣ 38 1630C δ 3.27 0.81 0.0322 31 101 22 -7 37 31 β 491 548 ε 4.34 0.77 0.0193 52 169 119 -84 39 30 ζ 4.08 0.35 0.0180 56 181 42 -24 57 34 β η 4.40 0.04 0.0134 74 243 25 -10 76 38 Fox ϑ 4.61 0.16 0.0129 78 253 20 1 68 24 ι 4.29 -1.65 0.0065 154 502 20 0 359 17 κ 4.15 0.57 0.0192 52 170 22 -9 47 19 h 1898 16916 λ 3.81 1.75 0.0387 26 84 56 7 16 16 β pm µ 3.86 0.75 0.0239 42 136 32 8 39 37 h 1057 788 ν 4.53 -2.06 0.0048 208 679 37 -24 527 35 ξ 4.87 0.98 0.0167 60 195 15 -12 32 46 οΑ 3.73 -2.90 0.0047 212 692 27 -14 1143 1 3.62 bin:A οΒ 6.03 -0.61 0.0047 212 692 23 - 138 1 bin:B π 4.34 -2.18 0.0050 201 656 17 9 585 29 h 1030 513 ρ 5.16 1.71 0.0204 49 160 19 9 16 27 σ 4.51 1.33 0.0231 43 141 18 -8 23 25 τ 4.96 -1.64 0.0048 209 681 32 -14 356 53 β 1311 υ 4.10 3.45 0.0743 13.5 44 39 -28 3.3 50 β pm ϕΑ 4.52 -2.25 0.0044 226 736 15 0 624 42 4.26 ΟΣ 515 940A ϕΒ 5.81 -0.95 0.0044 226 736 13 - 190 42 ΟΣ 515 940B χ 5.01 0.66 0.0135 74 242 11 7 43 52 ψ 4.97 -3.05 0.0025 402 1309 33 -25 1305 20 β ω 4.83 2.57 0.0353 28 92 51 11 7.0 48 β 999 1152AB 2AAnd 5.26 0.11 0.0093 107 349 28 2 71 5.09 β 1147 16467A 2BAnd 7.43 2.28 0.0093 107 349 28 - 10 β 1147 16467B 3 And 4.64 0.94 0.0182 55 179 71 -35 33 4 And 5.30 0.20 0.0095 105 342 17 -6 66 h 1849 16526 5 And 5.68 3.02 0.0293 34 111 33 -2 4.9 6 And 5.91 3.65 0.0354 28 92 58 -43 2.7 7 And 4.53 2.58 0.0408 24 80 20 13 7.3 8 And 4.82 -1.69 0.0050 201 655 34 -8 375 β 717 16656 9 And 5.98 0.17 0.0069 145 472 11 -4 67 10 And 5.81 -0.30 0.0060 166 542 38 3 103 11 And 5.44 0.43 0.0100 101 328 29 11 53 12 And 5.77 2.63 0.0236 42 138 30 -9 7.0 β 13 And 5.75 0.97 0.0111 90 294 39 -9 32 14 And 5.22 0.80 0.0131 76 249 123 -59 38 15 And 5.55 1.28 0.0140 72 233 21 13 24 18 And 5.35 -0.04 0.0084 120 390 13 9 82 22 And 5.01 -2.44 0.0032 309 1006 8 -5 743 23 And 5.71 2.99 0.0286 35 114 43 -29 5.0 26 And 6.10 -0.53 0.0047 212 692 25 7 129 ΟΣ 5 254 28 And 5.20 1.43 0.0176 57 185 22 -10 21 β 1095 409AB 32 And 5.30 0.18 0.0095 106 344 9 -5 67 36AAnd 6.19 3.23 0.0257 39 127 27 2 4.0 5.67 Σ 73 755A 3 Andromeda (II) AND HD HIP α δ B-V µ(α)″ µ(δ)″ µ″ Dir Spect.
Recommended publications
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation

    Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation

    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
  • Where Are the Distant Worlds? Star Maps

    Where Are the Distant Worlds? Star Maps

    W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star.
  • Messier Objects

    Messier Objects

    Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun.
  • Explore the Universe Observing Certificate Second Edition

    Explore the Universe Observing Certificate Second Edition

    RASC Observing Committee Explore the Universe Observing Certificate Second Edition Explore the Universe Observing Certificate Welcome to the Explore the Universe Observing Certificate Program. This program is designed to provide the observer with a well-rounded introduction to the night sky visible from North America. Using this observing program is an excellent way to gain knowledge and experience in astronomy. Experienced observers find that a planned observing session results in a more satisfying and interesting experience. This program will help introduce you to amateur astronomy and prepare you for other more challenging certificate programs such as the Messier and Finest NGC. The program covers the full range of astronomical objects. Here is a summary: Observing Objective Requirement Available Constellations and Bright Stars 12 24 The Moon 16 32 Solar System 5 10 Deep Sky Objects 12 24 Double Stars 10 20 Total 55 110 In each category a choice of objects is provided so that you can begin the certificate at any time of the year. In order to receive your certificate you need to observe a total of 55 of the 110 objects available. Here is a summary of some of the abbreviations used in this program Instrument V – Visual (unaided eye) B – Binocular T – Telescope V/B - Visual/Binocular B/T - Binocular/Telescope Season Season when the object can be best seen in the evening sky between dusk. and midnight. Objects may also be seen in other seasons. Description Brief description of the target object, its common name and other details. Cons Constellation where object can be found (if applicable) BOG Ref Refers to corresponding references in the RASC’s The Beginner’s Observing Guide highlighting this object.
  • 100 Closest Stars Designation R.A

    100 Closest Stars Designation R.A

    100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79,
  • Naming the Extrasolar Planets

    Naming the Extrasolar Planets

    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
  • Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆

    Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆

    A&A 565, A15 (2014) Astronomy DOI: 10.1051/0004-6361/201323058 & c ESO 2014 Astrophysics Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel J. P. Marshall1,2, A. Moro-Martín3,4, C. Eiroa1, G. Kennedy5,A.Mora6, B. Sibthorpe7, J.-F. Lestrade8, J. Maldonado1,9, J. Sanz-Forcada10,M.C.Wyatt5,B.Matthews11,12,J.Horner2,13,14, B. Montesinos10,G.Bryden15, C. del Burgo16,J.S.Greaves17,R.J.Ivison18,19, G. Meeus1, G. Olofsson20, G. L. Pilbratt21, and G. J. White22,23 (Affiliations can be found after the references) Received 15 November 2013 / Accepted 6 March 2014 ABSTRACT Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 μm with the sensitiv- ity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system’s Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis.
  • Australian Sky & Telescope

    Australian Sky & Telescope

    TRANSIT MYSTERY Strange sights BINOCULAR TOUR Dive deep into SHOOT THE MOON Take amazing as Mercury crosses the Sun p28 Virgo’s endless pool of galaxies p56 lunar images with your smartphone p38 TEST REPORT Meade’s 25-cm LX600-ACF P62 THE ESSENTIAL MAGAZINE OF ASTRONOMY Lasers and advanced optics are transforming astronomy p20 HOW TO BUY THE RIGHT ASTRO CAMERA p32 p14 ISSUE 93 MAPPING THE BIG BANG’S COSMIC ECHOES $9.50 NZ$9.50 INC GST LPI-GLPI-G LUNAR,LUNAR, PLANETARYPLANETARY IMAGERIMAGER ANDAND GUIDERGUIDER ASTROPHOTOGRAPHY MADE EASY. Let the LPI-G unleash the inner astrophotographer in you. With our solar, lunar and planetary guide camera, experience the universe on a whole new level. 0Image Sensor:'+(* C O LOR 0 Pixel Size / &#*('+ 0Frames per second/Resolution• / • / 0 Image Format: #,+$)!&))'!,# .# 0 Shutter%,*('#(%%#'!"-,,* 0Interface: 0Driver: ASCOM compatible 0GuiderPort: 0Color or Monochrome Models (&#'!-,-&' FEATURED DEALERS: MeadeTelescopes Adelaide Optical Centre | www.adelaideoptical.com.au MeadeInstrument The Binocular and Telescope Shop | www.bintel.com.au MeadeInstruments www.meade.com Sirius Optics | www.sirius-optics.com.au The device to free you from your handbox. With the Stella adapter, you can wirelessly control your GoTo Meade telescope at a distance without being limited by cord length. Paired with our new planetarium app, *StellaAccess, astronomers now have a graphical interface for navigating the night sky. STELLA WI-FI ADAPTER / $#)'$!!+#!+ #$#)'#)$##)$#'&*' / (!-')-$*')!($%)$$+' "!!$#$)(,#%',).( StellaAccess app. Available for use on both phones and tablets. /'$+((()$!'%!#)'*")($'!$)##!'##"$'$*) stars, planets, celestial bodies and more /$,'-),',### -' ($),' /,,,$"$')*!!!()$$"%)!)!($%( STELLA is controlled with Meade’s planetarium app, StellaAccess. Available for purchase for both iOS S and Android systems.
  • M-53 Ngc – 5053

    M-53 Ngc – 5053

    MONTHLY OBSERVER’S CHALLENGE Las Vegas Astronomical Society Compiled by: Roger Ivester, Boiling Springs, North Carolina & Fred Rayworth, Las Vegas, Nevada With special assistance from: Rob Lambert, Las Vegas, Nevada JUNE 2014 Messier 53 (M53)/NGC-5053 – Globular Cluster Pair In Coma Berenices Introduction The purpose of the observer’s challenge is to encourage the pursuit of visual observing. It is open to everyone that is interested, and if you are able to contribute notes, drawings, or photographs, we will be happy to include them in our monthly summary. Observing is not only a pleasure, but an art. With the main focus of amateur astronomy on astrophotography, many times people tend to forget how it was in the days before cameras, clock drives, and GOTO. Astronomy depended on what was seen through the eyepiece. Not only did it satisfy an innate curiosity, but it allowed the first astronomers to discover the beauty and the wonderment of the night sky. Before photography, all observations depended on what the astronomer saw in the eyepiece, and how they recorded their observations. This was done through notes and drawings and that is the tradition we are stressing in the observers challenge. By combining our visual observations with our drawings, and sometimes, astrophotography (from those with the equipment and talent to do so), we get a unique understanding of what it is like to look through an eyepiece, and to see what is really there. The hope is that you will read through these notes and become inspired to take more time at the eyepiece studying each object, and looking for those subtle details that you might never have noticed before.
  • Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B

    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,
  • IAU Division C Working Group on Star Names 2019 Annual Report

    IAU Division C Working Group on Star Names 2019 Annual Report

    IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ ​ WGSN Email: [email protected] ​ The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. ​ ​ ​ WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the ​ internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials.
  • The CORALIE Survey for Southern Extrasolar Planets XVII

    The CORALIE Survey for Southern Extrasolar Planets XVII

    Astronomy & Astrophysics manuscript no. coralieXVII c ESO 2019 July 1, 2019 The CORALIE survey for southern extrasolar planets XVII. New and updated long period and massive planets ? ?? M. Marmier1, D. Segransan´ 1, S. Udry1, M. Mayor1, F. Pepe1, D. Queloz1, C. Lovis1, D. Naef1, N.C. Santos2;3;1, R. Alonso4;5;1, S. Alves8;1, S. Berthet1, B. Chazelas1, B-O. Demory9;1, X. Dumusque1, A. Eggenberger1, P. Figueira2;1, M. Gillon6;1, J. Hagelberg1, M. Lendl1, R. A. Mardling7;1, D. Megevand´ 1, M. Neveu1, J. Sahlmann1, D. Sosnowska1, M. Tewes10, and A. H.M.J. Triaud1 1 Observatoire astronomique de l’Universite´ de Geneve,` 51 ch. des Maillettes - Sauverny -, CH-1290 Versoix, Switzerland 2 Centro de Astrof´ısica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 3 Departamento de F´ısica e Astronomia, Faculdade de Ciencias,ˆ Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 4 Instituto de Astrof´ısica de Canarias, C/ V´ıa Lactea´ S/N, E-38200 La Laguna, Spain 5 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Spain 6 Universite´ de Liege,` Allee´ du 6 aoutˆ 17, Sart Tilman, Liege` 1, Belgium 7 School of Mathematical Sciences, Monash University, Victoria, 3800, Australia 8 Departamento de F´ısica, Universidade Federal do Rio Grande do Norte, 59072-970, Natal, RN., Brazil 9 Department of Earth, Atmospheric and Planetary Sciences, Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave., Cambridge, MA 02139, USA 10 Laboratoire d’astrophysique, Ecole Polytechnique Fed´ erale´ de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland Received month day, year; accepted month day, year ABSTRACT Context.