History & Future of Northmoor Observatory
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Messier Plus Marathon Text
Messier Plus Marathon Object List by Wally Brown & Bob Buckner with additional objects by Mike Roos Object Data - Saguaro Astronomy Club Score is most numbered objects in a single night. Tiebreaker is count of un-numbered objects Observer Name Date Address Marathon Obects __________ Tiebreaker Objects ________ SEQ OBJECT TYPE CON R.A. DEC. RISE TRANSIT SET MAG SIZE NOTES TIME M 53 GLOCL COM 1312.9 +1810 7:21 14:17 21:12 7.7 13.0' NGC 5024, !B,vC,iR,vvmbM,st 12.. NGC 5272, !!,eB,vL,vsmbM,st 11.., Lord Rosse-sev dark 1 M 3 GLOCL CVN 1342.2 +2822 7:11 14:46 22:20 6.3 18.0' marks within 5' of center 2 M 5 GLOCL SER 1518.5 +0205 10:17 16:22 22:27 5.7 23.0' NGC 5904, !!,vB,L,eCM,eRi, st mags 11...;superb cluster M 94 GALXY CVN 1250.9 +4107 5:12 13:55 22:37 8.1 14.4'x12.1' NGC 4736, vB,L,iR,vsvmbM,BN,r NGC 6121, Cl,8 or 10 B* in line,rrr, Look for central bar M 4 GLOCL SCO 1623.6 -2631 12:56 17:27 21:58 5.4 36.0' structure M 80 GLOCL SCO 1617.0 -2258 12:36 17:21 22:06 7.3 10.0' NGC 6093, st 14..., Extremely rich and compressed M 62 GLOCL OPH 1701.2 -3006 13:49 18:05 22:21 6.4 15.0' NGC 6266, vB,L,gmbM,rrr, Asymmetrical M 19 GLOCL OPH 1702.6 -2615 13:34 18:06 22:38 6.8 17.0' NGC 6273, vB,L,R,vCM,rrr, One of the most oblate GC 3 M 107 GLOCL OPH 1632.5 -1303 12:17 17:36 22:55 7.8 13.0' NGC 6171, L,vRi,vmC,R,rrr, H VI 40 M 106 GALXY CVN 1218.9 +4718 3:46 13:23 22:59 8.3 18.6'x7.2' NGC 4258, !,vB,vL,vmE0,sbMBN, H V 43 M 63 GALXY CVN 1315.8 +4201 5:31 14:19 23:08 8.5 12.6'x7.2' NGC 5055, BN, vsvB stell. -
Ghost Hunt Challenge 2020
Virtual Ghost Hunt Challenge 10/21 /2020 (Sorry we can meet in person this year or give out awards but try doing this challenge on your own.) Participant’s Name _________________________ Categories for the competition: Manual Telescope Electronically Aided Telescope Binocular Astrophotography (best photo) (if you expect to compete in more than one category please fill-out a sheet for each) ** There are four objects on this list that may be beyond the reach of beginning astronomers or basic telescopes. Therefore, we have marked these objects with an * and provided alternate replacements for you just below the designated entry. We will use the primary objects to break a tie if that’s needed. Page 1 TAS Ghost Hunt Challenge - Page 2 Time # Designation Type Con. RA Dec. Mag. Size Common Name Observed Facing West – 7:30 8:30 p.m. 1 M17 EN Sgr 18h21’ -16˚11’ 6.0 40’x30’ Omega Nebula 2 M16 EN Ser 18h19’ -13˚47 6.0 17’ by 14’ Ghost Puppet Nebula 3 M10 GC Oph 16h58’ -04˚08’ 6.6 20’ 4 M12 GC Oph 16h48’ -01˚59’ 6.7 16’ 5 M51 Gal CVn 13h30’ 47h05’’ 8.0 13.8’x11.8’ Whirlpool Facing West - 8:30 – 9:00 p.m. 6 M101 GAL UMa 14h03’ 54˚15’ 7.9 24x22.9’ 7 NGC 6572 PN Oph 18h12’ 06˚51’ 7.3 16”x13” Emerald Eye 8 NGC 6426 GC Oph 17h46’ 03˚10’ 11.0 4.2’ 9 NGC 6633 OC Oph 18h28’ 06˚31’ 4.6 20’ Tweedledum 10 IC 4756 OC Ser 18h40’ 05˚28” 4.6 39’ Tweedledee 11 M26 OC Sct 18h46’ -09˚22’ 8.0 7.0’ 12 NGC 6712 GC Sct 18h54’ -08˚41’ 8.1 9.8’ 13 M13 GC Her 16h42’ 36˚25’ 5.8 20’ Great Hercules Cluster 14 NGC 6709 OC Aql 18h52’ 10˚21’ 6.7 14’ Flying Unicorn 15 M71 GC Sge 19h55’ 18˚50’ 8.2 7’ 16 M27 PN Vul 20h00’ 22˚43’ 7.3 8’x6’ Dumbbell Nebula 17 M56 GC Lyr 19h17’ 30˚13 8.3 9’ 18 M57 PN Lyr 18h54’ 33˚03’ 8.8 1.4’x1.1’ Ring Nebula 19 M92 GC Her 17h18’ 43˚07’ 6.44 14’ 20 M72 GC Aqr 20h54’ -12˚32’ 9.2 6’ Facing West - 9 – 10 p.m. -
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). -
Global Fitting of Globular Cluster Age Indicators
A&A 456, 1085–1096 (2006) Astronomy DOI: 10.1051/0004-6361:20065133 & c ESO 2006 Astrophysics Global fitting of globular cluster age indicators F. Meissner1 and A. Weiss1 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany e-mail: [meissner;weiss]@mpa-garching.mpg.de Received 3 March 2006 / Accepted 12 June 2006 ABSTRACT Context. Stellar models and the methods for the age determinations of globular clusters are still in need of improvement. Aims. We attempt to obtain a more objective method of age determination based on cluster diagrams, avoiding the introduction of biases due to the preference of one single age indicator. Methods. We compute new stellar evolutionary tracks and derive the dependence of age indicating points along the tracks and isochrone – such as the turn-off or bump location – as a function of age and metallicity. The same critical points are identified in the colour-magnitude diagrams of globular clusters from a homogeneous database. Several age indicators are then fitted simultaneously, and the overall best-fitting isochrone is selected to determine the cluster age. We also determine the goodness-of-fit for different sets of indicators to estimate the confidence level of our results. Results. We find that our isochrones provide no acceptable fit for all age indicators. In particular, the location of the bump and the brightness of the tip of the red giant branch are problematic. On the other hand, the turn-off region is very well reproduced, and restricting the method to indicators depending on it results in trustworthy ages. Using an alternative set of isochrones improves the situation, but neither leads to an acceptable global fit. -
Seeing the Light: the Art and Science of Astronomy
Chapter 1 Seeing the Light: The Art and Science of Astronomy In This Chapter ▶ Understanding the observational nature of astronomy ▶ Focusing on astronomy’s language of light ▶ Weighing in on gravity ▶ Recognizing the movements of objects in space tep outside on a clear night and look at the sky. If you’re a city dweller Sor live in a cramped suburb, you see dozens, maybe hundreds, of twin- kling stars. Depending on the time of the month, you may also see a full Moon and up to five of the eight planets that revolve around the Sun. A shooting star or “meteor” may appear overhead. What you actually see is the flash of light from a tiny piece of comet dust streaking through the upper atmosphere. Another pinpoint of light moves slowly and steadily across the sky. Is it a space satellite, such as the Hubble Space Telescope, or just a high-altitude airliner? If you have a pair of binoculars, you may be able to see the difference. Most air- liners have running lights, and their shapes may be perceptible. If you liveCOPYRIGHTED in the country — on the seashore MATERIAL away from resorts and develop- ments, on the plains, or in the mountains far from any floodlit ski slope — you can see thousands of stars. The Milky Way appears as a beautiful pearly swath across the heavens. What you’re seeing is the cumulative glow from millions of faint stars, individually indistinguishable with the naked eye. At a great observation place, such as Cerro Tololo in the Chilean Andes, you can see even more stars. -
Globular Cluster Club
Globular Cluster Observing Club Raleigh Astronomy Club Version 1.2 22 June 2007 Introduction Welcome to the Globular Cluster Observing Club! This list is intended to give you an appreciation for the deep-sky objects known as globular clusters. There are 153 known Milky Way Globular Clusters of which the entire list can be found on the seds.org site listed below. To receive your Gold level we will only have you do sixty of them along with one challenge object from a list of three. Challenge objects being the extra-galactic globular Mayall II (G1) located in the Andromeda Galaxy, Palomar 4 in Ursa Major, and Omega Centauri a magnificent southern globular. The first two challenge your scope and viewing ability while Omega Centauri challenges your ability to plan for a southern view. A Silver level is also available and will be within the range of a 4 inch to 8 inch scope depending upon seeing conditions. Many of the objects are found in the Messier, Caldwell, or Herschel catalogs and can springboard you into those clubs. The list is meant for your viewing enrichment and edification of these types of clusters. It is also meant to enhance your viewing skills. You are encouraged to view the clusters with a critical eye toward the cluster’s size, visual magnitude, resolvability, concentration and colors. The Astronomical League’s Globular Clusters Club book “Guide to the Globular Cluster Observing Club” is an excellent resource for this endeavor. You will be asked to either sketch the cluster or give a short description of your visual impression, citing seeing conditions, time, date, cluster’s size, magnitude, resolvability, concentration, and any star colors. -
The Case of the Peculiar Globular Cluster NGC 6712 F
References Hatzes, A.P. & Cochran, W.D. 1994b, ApJ Pasquini, L., Pallavicini, R. Pakull, M. 1988, 432, 763. A&A 191, 266. Baranne, A., et al., 1996, A&A Suppl Ser Hatzes, A.P. & Cochran, W.D. 1998, MNRAS Pasquini, L. 1992, A&A 266, 347. 119,1. 293, 469. von der Lühe, O., Solanki, S., Reinheimer, Butler, R.P., et al. 1996, PASP 108, 500. Kaufer, A., et al. 1999, The Messenger 95, 8. Th. 1996, in IAU Symp. 176, S t e l l a r Hatzes, A.P. & Cochran, W.D. 1993, ApJ Larson, A. et al. 1993, PASP 105, 825. Surface Structure 147–163. Wa l k e r, 413, 339. Lambert, D.L. 1987, ApJS 65, 255. G.A.H., Yang, S., Campbell, B., and Irwin, Hatzes, A.P. & Cochran, W.D. 1994a, ApJ Merline, W.J. 1996, ASP Conf. Ser. 135, p. A.W. 1989, ApJL 343, L21. 422, 366. 208. Crowded Field Photometry with the VLT: the Case of the Peculiar Globular Cluster NGC 6712 F. PARESCE1, G. DE MARCHI2, G. ANDREUZZI 3, R. BUONANNO 3, F. FERRARO4, B. PALTRINIERI3, L. PULONE 3 1European Southern Observatory, Garching, Germany 2European Space Agency, STScI, Baltimore, USA 3Osservatorio Astronomico di Roma, Rome, Italy 4Osservatorio Astronomico di Bologna, Bologna, Italy 1. Introduction study that best illuminate the perform- 2. VLT Observations of ance of this instrument combination for NGC 6712 The Hubble Space Te l e s c o p e crowded field photometry that might be opened up the exciting possibility of of interest to anyone contemplating do- NGC 6712 (a = 18h 53m 04.3², d = carrying out very deep, high-precision ing this sort of work with the VLT in the –08º 42¢ 21.5²) is a relatively metal stellar photometry in very crowded future. -
The Agb Newsletter
THE AGB NEWSLETTER An electronic publication dedicated to Asymptotic Giant Branch stars and related phenomena Official publication of the IAU Working Group on Red Giants and Supergiants No. 286 — 2 May 2021 https://www.astro.keele.ac.uk/AGBnews Editors: Jacco van Loon, Ambra Nanni and Albert Zijlstra Editorial Board (Working Group Organising Committee): Marcelo Miguel Miller Bertolami, Carolyn Doherty, JJ Eldridge, Anibal Garc´ıa-Hern´andez, Josef Hron, Biwei Jiang, Tomasz Kami´nski, John Lattanzio, Emily Levesque, Maria Lugaro, Keiichi Ohnaka, Gioia Rau, Jacco van Loon (Chair) Editorial Dear Colleagues, It is our pleasure to present you the 286th issue of the AGB Newsletter. A healthy 30 postings are sure to keep you inspired. Now that the Leuven workshop has happened, we are gearing up to the IAU-sponsored GAPS 2021 virtual discussion meeting aimed to lay out a roadmap for cool evolved star research: we have got an exciting line-up of new talent as well as seasoned experts introducing the final session – all are encouraged to contribute to the meeting through 5-minute presentations or live discussion and the White Paper that will follow (see announcement at the back). Those interested in the common envelope process will no doubt consider attending the CEPO 2021 virtual meeting on this topic organised at the end of August / star of September. Great news on the job front: there are Ph.D. positions in Bordeaux, postdoc positions in Warsaw and another one in Nice. Thanks to Josef Hron and P´eter Abrah´am´ for ensuring the continuation of the Fizeau programme for exchange in the field of interferometry. -
Dynamical Modelling of Stellar Systems in the Gaia Era
Dynamical modelling of stellar systems in the Gaia era Eugene Vasiliev Institute of Astronomy, Cambridge Synopsis Overview of dynamical modelling Overview of the Gaia mission Examples: Large Magellanic Cloud Globular clusters Measurement of the Milky Way gravitational potential Fred Hoyle vs. the Universe What does \dynamical modelling" mean? It does not refer to a simulation (e.g. N-body) of the evolution of a stellar system. Most often, it means \modelling a stellar system in a dynamical equilibrium" (used interchangeably with \steady state"). vs. the Universe What does \dynamical modelling" mean? It does not refer to a simulation (e.g. N-body) of the evolution of a stellar system. Most often, it means \modelling a stellar system in a dynamical equilibrium" (used interchangeably with \steady state"). Fred Hoyle What does \dynamical modelling" mean? It does not refer to a simulation (e.g. N-body) of the evolution of a stellar system. Most often, it means \modelling a stellar system in a dynamical equilibrium" (used interchangeably with \steady state"). Fred Hoyle vs. the Universe 3D Steady-state assumption =) Jeans theorem: f (x; v)= f I(x; v;Φ) observations: 3D { 6D integrals of motion (≤ 3D?), e.g., I = fE; L;::: g Why steady state? Distribution function of stars f (x; v; t) satisfies [sometimes] the collisionless Boltzmann equation: @f (x; v; t) @f (x; v; t) @Φ(x; t) @f (x; v; t) + v − = 0: @t @x @x @v Potential , mass distribution @f (x; v; t) ; t ; t ; t + @t 3D observations: 3D { 6D integrals of motion (≤ 3D?), e.g., I = fE; L;::: -
My Finest NGC Album
My Finest NGC Album A detailed record of my journey through The Royal Astronomical Society of Canada’s Finest NGC list Name: ______________________________ Centre or Home Location: ______________________________ The New General Catalogue or NGC contains 7,840 entries and forms the core of most people's " life list" of observing targets. The NGC was originally published in 1888 by J.L.E. Dreyer and therefore predated photographic astronomy. The Finest NGC list, compiled by Alan Dyer complements the Messier List, as there is no overlap. The list features many fine deep-sky treasures as well as a few somewhat more challenging objects. Once you have observed all of the objects on this list, application forms can be found on the RASC website at www.rasc.ca. The FNGC certificate has been awarded since 1995. Here is an overview of the Finest NGC Observing List Finest NGC Objects Number Notes Open Clusters 12 Including the famous Double Cluster in Perseus, NGC 7789 in Cassiopeia, and NGC 6633 in Ophiuchus. Globular Clusters 2 NGC 5466 in Bootes and NGC 6712 in Scutum. Diffuse Nebulae 14 Includes the great Veil Nebula as well as the North America and Rosette nebulae. Planetary Nebulae 24 Includes many fine PN's like the Ghost of Jupiter, the Cat's Eye, the Blinking Planetary, the Helix, the Blue Snowball, and the Clown Face nebulae. Galaxies 58 Includes the amazing NGC 4565 in Coma Berenices, NGC 253 in Sculptor, and NGC 5907 in Draco. Total 110 The Finest NGC list can be started during any season. Why Record Your Observations? Recording observations is important for two reasons. -
RASC Finest NGC Observing Program Checklist
RASC Finest NGC Observing Program Checklist Use this checklist to monitor your progress. Version 1.0a. Edited on 9 June 2021. Record your detailed observations on the provided observing forms or your own log sheets. Sketching is optional but highly encouraged. The "+" column denotes special combination objects. E.g. FNGC # 26 is for NGC 1973 with 1975 and 1977. Number NGC + Alternate ID Con Cls RA 2000 Decl 2000 Mag Size Rating Done The Autumn Sky 1 NGC 7009 Saturn Nebula Aqr PN 21h04m10.9s -11°21'48" 8.3 28" !! q 2 NGC 7293 Helix Aqr PN 22h29m38.5s -20°50'14" 6.3 16.0' !! q 3 NGC 7331 Deer Lick Group Peg Gal 22h37m04.3s +34°24'59" 10.2 9.1'x 3.4' !! q 4 NGC 7635 Bubble Nebula Cas EN 23h20m43.0s +61°12'31" 11 16.0'x 9.0' q 5 NGC 7789 OCL 269 Cas OC 23h57m24.0s +56°42'30" 7.5 25.0' !! q 6 NGC 185 MCG 8-2-10 Cas Gal 00h38m57.9s +48°20'15" 10.2 10.7'x 8.9' q 7 NGC 281 PacMan Nebula Cas EN 00h53m00.0s +56°37'00" 7.4 30.0' !! q 8 NGC 457 ET Cluster Cas OC 01h19m35.0s +58°17'12" 5.1 20.0' q 9 NGC 663 Collinder 20 Cas OC 01h46m09.0s +61°14'06" 6.4 14.0' q 10 IC 289 PN G138.8+02.8 Cas PN 03h10m19.3s +61°19'01" 12 45" q 11 NGC 7662 Blue Snowball And PN 23h25m54.0s +42°32'05" 8.6 17" !! q 12 NGC 891 Silver Needle And Gal 02h22m33.6s +42°20'46" 10.9 11.7'x 2.3' !! q 13 NGC 253 Sculptor Galaxy Scl Gal 00h47m33.1s -25°17'20" 7.9 28.2'x 5.5' !! q 14 NGC 772 Arp 78 Ari Gal 01h59m20.0s +19°00'28" 10.6 5.9'x 3.2' q 15 NGC 246 Skull Nebula Cet PN 00h47m03.3s -11°52'19" 10.4 4.0' q 16 NGC 936 MCG 0-7-17 Cet Gal 02h27m37.5s -01°09'20" 11.2 4.5'x 3.4' q 17 -
ASTRONOMİ Terimleri
A tayf türü yıldızlar (Alm. Sterne von Typ A, pl; Fr. étoiles de type A, pl; İng. A type stars) ast. Etkin sıcaklıkları 7.500 ile 10.000 K, anakolda olanların kütlesi 1,6 ile 2,5 Güneş kütlesi aralığında olan, tayflarında güçlü hidrojen ve iyonlaşmış ağır element çizgileri görülen açık mavi yıldızlar. aa indeksi (Alm. aa Index, m; Fr. indice aa; İng. aa index) ast. Yaklaşık zıt kutuplarda 50 derece enlemlerinde bulunan iki istasyondan elde edilen K jeomanyetik aktivite indisinden hesaplanan günlük ya da yarım günlük jeomanyetik aktivite indeksi. Abell kataloğu (Alm. Abell-Katalog, m; Fr. catalogue Abell, m; İng. Abell catalogue) ast. 1958 yılında George O. Abell tarafından yayınlanan, 2712 yakın gökada kümesini içeren, her bir kümenin en az 50 gökada içermesi, Abell yarıçapı içinde bulunacak kadar derlitoplu olmaları, 33 ile 330 megaparsek arasındaki uzaklıklarda bulunmaları gibi kriterleri sağlayan gökadalar kataloğu. Abell yarıçapı (Alm. Abell-Radius, m; Fr. rayon d'Abel, m; İng. Abell radius) ast. Abell kataloğundaki gökada kümelerinden hareketle, uzunluğu 2,14 megaparsek kabul edilen, tipik bir gökada kümesinin yarıçapı. açık evren (Alm. offenes Universum, n; Fr. univers ouvert, m; İng. open universe) ast. Ortalama madde yoğunluğunun kritik madde yoğunluğuna oranı birden küçük olduğunda, uzayın geometrik şeklinin bir eyer yüzeyi gibi açık olduğunu, bir üçgenin iç açılarının toplamının 180 dereceden küçük olduğunu, kesişmeyen doğruların her noktada eşit uzaklıkta olmadıklarını, evrenin hiperbolik şekilde olduğunu öngören evren modeli. açık yıldız kümesi (Alm. galaktischer Haufen, m; offener Sternhaufen, m; Fr. amas galactique ouvert, m; amas ouvert, m; İng. galactic cluster; open cluster) ast. Birbirlerine kütleçekim kuvveti ile zayıfça bağlı bir kaç on ila bir kaç yüz genç yıldızdan oluşan topluluk.