DOCSLIB.ORG

Observing Galaxies in Andromeda 01 October 2015 22:25

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Observing Galaxies in Andromeda 01 October 2015 22:25 Observing galaxies in Andromeda 01 October 2015 22:25 Context As you look towards Andromeda you are looking below the galactic plane under the Perseus spiral arm of our galaxy which itself is about 7,000 light years away. There is a group of relatively local galaxies which are less than 20 million light years away. The bulk of the others are in the Perseus-Pisces supercluster wall of galaxies which runs through this constellation. It stretches from RA 3h +40 in Perseus to 23h +10 in Pegasus and is around 200 million light years away. The constellation is well placed from late summer to late autumn. Andromeda is a relatively rich constellation for galaxy observing. I have observed 38 galaxies in this constellation although many are faint. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! M31 / M 32 / M 110 MAG 3/8/8 This is the stand out group of galaxies in the sky and the constellation. These galaxies are generally the first galaxies that amateur astronomers observe first. M31 is visible to the naked eye in dark skies. All three are 2.6 million light years away. M31 whilst bright and large is fairly bland in appearance until you start to look a bit closer. With good conditions, the dark line of a dust lane is visible. I have to say that observing two of the globular clusters of this galaxy rank up there in my most memorable observations ever. This galaxy has a brighter region which has a designation NGC 206. M32 is very bright and I have seen it in binoculars as a very small bright blob. It is small being only 8,000 light years across. M110 can be a challenge to see with its low surface brightness. Having said that, I have seen it easily in my 80mm binoculars when the sky was transparent. NGC 891 M9 This is actually a tough galaxy to see due to its low surface brightness. However on a good night with the 16 By constellation Page 1 This is actually a tough galaxy to see due to its low surface brightness. However on a good night with the 16 inch it is large and extended, a really unique sight. It is part of the NGC 1023 (Perseus) group of galaxies and is about 30 million light years away. NGC 404 MAG 11 This galaxy is memorable to observe as it is close to the star Mirach and hence is known as Mirach’s ghost. It is a lovely circular low surface brightness glow that is visible with direct vision in my 10 inch reflector and was visible at low power with averted vision even with Mirach in the field of view. It is about 10 million light years away and relatively isolated. It is believed to have collided with another small galaxy 900 million years ago. NGC 529 (right of image) / NGC 536 (middle of image) MAG 12 Both of these galaxies could be seen without needing to use averted vision in the same field of view in my 6 mm eyepiece. They both looked round visually. NGC 536 had a field star embedded in its halo. I could not see NGC 531 (above 536) despite trying in my 10 inch scope. By constellation Page 2 NGC 97 MAG 12 Although small this galaxies surface brightness allowed me to see it with direct vision in my 10 inch scope. Other special galaxies and galaxy groups of note I have set out below a selection of observed galaxies and galaxy groups of note in the constellation. NGC 80 / NGC 83 GROUP MAG 12 This is a small group I have observed in Andromeda. There are two small faint circular galaxies both of which could be seen at the same time in the view of my 6 mm eyepiece using my 10 inch scope. By constellation Page 3 NGC 68 / NGC 71 GROUP (ARP 113) MAG 12/13 I observed the two brightest galaxies of this group in my 16 inch scope both of which required averted vision. NGC 7640 MAG 11 This is one of the more “local” galaxies in Andromeda. Its redshift indicates a distance of 17 million light years. At the eyepiece it is a lovely long but faint object which was only visible with averted vision in my 10 inch scope. It sits in a nice star field of 16 stars in my 9mm eyepiece. By constellation Page 4 Full list of observed galaxies in Andromeda ref1 SIZE SHAPE visual_ mag Comments MLY surf_brt INSTRUMENT scale ness NGC 224 large thin 5 3.4 Very large and 2.6 13.5 Skywatcher 10 inch oval bright NGC 221 medium circular 3 8.1 Small but easy to 2.6 12.4 TAL 1 see NGC 891 large slither 1 9.9 Amazing extended 32 13.6 Meade 16 inch faint galaxy NGC 529 very circular 1 12.1 Reasonably bright 214 13.8 Skywatcher 10 inch small round galaxy. In same FOV as NGC 536. NGC 97 very circular 1 12.3 Faint circular 213 13.0 Skywatcher 10 inch small object NGC 536 very oval 1 12.4 Reasonably bright 230 13.4 Skywatcher 10 inch small round galaxy. In same FOV as NGC 529. NGC 205 large oval <0.5 8.1 Oval very faint 2.7 14.0 20 x 80B glow NGC 812 very oval <0.5 11.2 Very low sbr oval 236 12.8 Meade 16 inch small NGC 7640 medium slither <0.5 11.3 Lovely long but 17 14.5 Skywatcher 10 inch faint galaxy NGC 108 very circular <0.5 12.1 Tough small object 212 13.3 Darkstar 14 inch small NGC 80 very circular <0.5 12.1 Oval shaped 253 13.2 Skywatcher 10 inch small galaxy next to NGC 83 NGC 846 very circular <0.5 12.1 Low sbr spiral 218 13.3 Darkstar 14 inch small NGC 679 very circular <0.5 12.3 Very faint object 225 13.8 Skywatcher 10 inch small close to the limit of visibility NGC 753 very circular <0.5 12.3 Very low SBR 217 13.9 Skywatcher 10 inch small circular object NGC 687 very circular <0.5 12.3 Very small circular 228 12.9 Skywatcher 10 inch small galaxy. By constellation Page 5 small galaxy. NGC 214 very circular <0.5 12.3 Low sbr oval 200 13.1 Darkstar 14 inch small NGC 252 very circular <0.5 12.4 Very small oval 224 12.8 Skywatcher 10 inch small faint galaxy NGC 393 very circular <0.5 12.5 Small core - hard 238 13.4 Darkstar 14 inch small to pick out NGC 528 very oval <0.5 12.5 Small AV object. 213 13.1 Meade 16 inch small Brighter than 515/517 NGC 982 very oval <0.5 12.5 Extended but very 262 12.2 Skywatcher 10 inch small faint edge on galaxy NGC 83 very circular <0.5 12.5 Very faint circular 283 13.4 Skywatcher 10 inch small galaxy next to NGC 80 NGC 818 very oval <0.5 12.5 Small oval 199 13.8 Darkstar 14 inch small NGC 43 very circular <0.5 12.6 Lovely glow next 213 13.4 Meade 16 inch small to star NGC 797 very circular <0.5 12.6 Faint circular glow 250 13.3 Meade 16 inch small NGC 160 very oval <0.5 12.6 Faint oval 236 14.3 Meade 16 inch small NGC 425 very circular <0.5 12.6 Very faint glow 288 12.4 Meade 16 inch small next to a field star NGC 183 very circular <0.5 12.7 Very small faint 236 14.1 Meade 16 inch small blob NGC 523 very thin <0.5 12.7 Low sbr faint 216 13.2 Meade 16 inch small oval galaxy NGC 551 very oval <0.5 12.7 Faint extended 218 12.9 Meade 16 inch small glow NGC 68 very circular <0.5 12.9 Brightest of a pair 259 14.2 Meade 16 inch small visible in this view NGC 513 very oval <0.5 12.9 Faint small galaxy, 265 11.1 Meade 16 inch small nearly visible with direct vision NGC 76 very circular <0.5 13.0 Tough small object 329 12.7 Meade 16 inch small to spot NGC 801 small slither <0.5 13.1 Very faint 256 13.8 Meade 16 inch extended object NGC 573 very circular <0.5 13.1 Small but relatively 77 10.9 Meade 16 inch small easy spot NGC 169 very oval <0.5 13.2 Very faint oval 201 99.9 Meade 16 inch small NGC 71 very circular <0.5 13.2 Fainter of a pair of 299 13.4 Meade 16 inch small galaxies visible NGC 653 very slither <0.5 13.4 Tough extended 0 12.1 Meade 16 inch small object NGC 620 very circular <0.5 14.0 Faint small object 99.9 Meade 16 inch small NGC 7831 very slither 12.8 Faint but visible 224 12.3 TAL 150P small with averted vision TARGET LIST AT 9 October 2015 Source - Anonymous galaxies book Galaxy groups Abell group 437 10th brightest is m13.3.
Load more

Recommended publications
  • On the Origin and Propagation of Ultra-High Energy Cosmic Rays (Measurements & Prediction Techniques)
    Dissertation On the Origin and Propagation of Ultra-High Energy Cosmic Rays (Measurements & Prediction Techniques) Nils Nierstenhoefer Wuppertal, 2011 University of Wuppertal Supervisor/First reviewer: Prof. Dr. K.-H. Kampert Second reviewer: Prof. Dr. M. Risse Motivation & Preface It is a long known fact that cosmic rays reach Earth with tremendous energies of even above 1020 eV. Despite of decades of intensive research, it was not possible to finally reveal the origin of these par- ticles. The main obstacle in this field is their rare occurrence. This is due to a very steep energy spectrum. To make this point more clear, one roughly expects to observe less than one particle per km2 in one century exceeding energies larger than 1020 eV. To overcome the limitation of low statis- tics, larger and larger cosmic ray detectors have been deployed. Today’s largest cosmic ray detector is the Pierre Auger observatory (PAO) which was constructed in the Pampa Amarilla in Argentina. It covers an area of 3000 km2 and provides the largest set of observations of ultra-high energy cosmic rays (UHECR) in history. A second difficulty in understanding the origin of UHECR should be pointed out: Galactic and extra- galactic magnetic fields might alter the direction of even the highest energy events in a way that they do not point back to their source. In 2007 and 2008, already before the completion of the full detector, the Auger collaboration pub- lished a set of three important papers [1, 2, 3]. The first paper dealt with the correlation of the arrival directions of the highest energetic events with the distribution of active galactic nuclei (AGN) closer than 75Mpc from a catalog compiled by Veron-Cetty and Veron (VC-V) [4].
    [Show full text]
  • We Had a Great Time on the Trip. We Had Some Representatives from the Vandenberg and Santa Barbara Clubs Along with Us for the Trip
    We had a great time on the trip. We had some representatives from the Vandenberg and Santa Barbara clubs along with us for the trip. The most notable thing on the trip up was a stop in La Canada Flintridge to refuel the bus and get a bite to eat. I pulled out my PST Coronado and did a little impromptu public Sun Gazing. The Sun was pretty active with a number of platform prominences as well as the ever-present flame types. A distinct sunspot group in a very disturbed area of the Sun with a bright spot had me wondering if there was a flare in progress (There wasn’t.) The patrons at the tables outside didn’t seem to object to seeing the Sun either. I had a little bit of a scare when we first got up to the gate as a couple of people who were going to meet us there were nowhere to be seen. Fortunately one of them was already on the grounds and the other showed up while we were in the Museum. Relief! As it turned out we all went on the tour of the grounds. Our tour guide Greg gave us a tour starting outside the 60” Dome. He talked about the various Solar Telescopes -the old Snow telescope which was always a non-performer because of the design of the building- too many air currents. He talked about the rivalry over the 60 and 150 ft tower solar instruments (looks like UCLA won this one over USC.) And we got a good look at the 150 ft tower.
    [Show full text]
  • Homogeneous Velocity-Distance Data for Peculiar Velocity Analysis. III
    Homogeneous Velocity-Distance Data for Peculiar Velocity Analysis. III. The Mark III Catalog of Galaxy Peculiar Velocities Jeffrey A. Willicka, St´ephane Courteaub, S.M. Faberc, David Bursteind, Avishai Dekele, and Michael A. Straussf,g a Dept. of Physics, Stanford University, Stanford, CA 94305-4060 ([email protected]) b NOAO/KPNO, 950 N. Cherry Ave., Tucson, AZ 85726 ([email protected]) c UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 ([email protected]) d Arizona State University, Dept. of Physics and Astronomy, Box 871504, Tempe, AZ 85287 ([email protected]) e Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel ([email protected]) f Dept. Astrophysical Sciences, Princeton University, Princeton, NJ 08544 ([email protected]) g Alfred P. Sloan Foundation Fellow ABSTRACT This is the third in a series of papers in which we assemble and analyze a homoge- neous catalog of peculiar velocity data. In Papers I and II, we described the Tully-Fisher (TF) redshift-distance samples that constitute the bulk of the catalog, and our method- ology for obtaining mutually consistent TF calibrations for these samples. In this paper, we supply further technical details of the treatment of the data, and present a subset of the catalog in tabular form. The full catalog, known as the Mark III Catalog of Galaxy Peculiar Velocities, is available in accessible on-line databases, as described herein. The electronic catalog incorporates not only the TF samples discussed in Papers I and II, but also elliptical galaxy Dn-σ samples originally presented elsewhere.
    [Show full text]
  • Multicolor Surface Photometry of Lenticular Galaxies
    The Astronomical Journal, 129:630–646, 2005 February # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. MULTICOLOR SURFACE PHOTOMETRY OF LENTICULAR GALAXIES. I. THE DATA Sudhanshu Barway School of Studies in Physics, Pandit Ravishankar Shukla University, Raipur 492010, India; [email protected] Y. D. Mayya Instituto Nacional de Astrofisı´ca, O´ ptica y Electro´nica, Apdo. Postal 51 y 216, Luis Enrique Erro 1, 72000 Tonantzintla, Pue., Mexico; [email protected] Ajit K. Kembhavi Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411007, India; [email protected] and S. K. Pandey1 School of Studies in Physics, Pandit Ravishankar Shukla University, Raipur 492010, India; [email protected] Receivedv 2003 Auggust 13; accepted 2004 October 20 ABSTRACT We present multicolor surface and aperture photometry in the B, V, R,andK0 bands for a sample of 34 lenticular galaxies from the Uppsala General Catalogue. From surface photometric analysis, we obtain radial profiles of surface brightness, colors, ellipticity, position angle, and the Fourier coefficients that describe the departure of isophotal shapes from a purely elliptical form; we find the presence of dust lanes, patches, and ringlike structure in several galaxies in the sample. We obtain total integrated magnitudes and colors and find that these are in good agreement with the values from the Third Reference Catalogue. Isophotal colors are correlated with each other, following the sequence expected for early-type galaxies. The color gradients in lenticular galaxies are more negative than the corresponding gradients in elliptical galaxies. There is a good correlation between BÀVand BÀR color gradients, and the mean gradients in the BÀV, BÀR,andVÀK0 colors are À0:13 Æ 0:06, À0:18 Æ 0:06, and À0:25 Æ 0:11 mag dexÀ1 in radius, respectively.
    [Show full text]
  • Curriculum Vitae Thomas Matheson
    Curriculum Vitae Thomas Matheson Address: NSF's National Optical-Infrared Astronomy Research Laboratory Community Science and Data Center 950 North Cherry Avenue Tucson, AZ 85719, USA Telephone: (520) 318{8517 Fax: (520) 318{8360 e-mail: [email protected] WWW: http://www.noao.edu/noao/staff/matheson/ Education: University of California, Berkeley, Berkeley, CA Department of Astronomy Ph.D. received June 2000 M.A. received June 1992 PhD Thesis Topic: The Spectral Characteristics of Stripped-Envelope Supernovae Thesis Advisor: Professor Alexei V. Filippenko Harvard University, Cambridge, MA Department of Astronomy & Astrophysics and Physics A.B. magna cum laude, received June 1989 Senior Thesis Topic: Transients in the Solar Transition Region Thesis Advisor: Professor Robert W. Noyes Employment: NSF's National Optical-Infrared Astronomy Research Laboratory (The Former National Optical Astronomy Observatory) Community Science and Data Center Head of Time-Domain Services 2017 { present Astronomer 2018 { present Associate Astronomer 2009 { 2018 (Tenure, 2011) Assistant Astronomer 2004 { 2009 Harvard-Smithsonian Center for Astrophysics Optical and Infrared Division Post-doctoral fellow 2000 { 2004 University of California, Berkeley Department of Astronomy Research Assistant 1991 { 2000 Harvard-Smithsonian Center for Astrophysics Solar and Stellar Physics Division Research Assistant 1989 { 1990 Thomas Matheson|Curriculum Vitae Teaching: Harvard University, Department of Astronomy, Teaching Assistant 2001, 2003 University of California, Berkeley,
    [Show full text]
  • History Committee Report NC185: Robotic Telescope— Page | 1 Suggested Celestial Targets with Historical Canadian Resonance
    RASC History Committee Report NC185: Robotic Telescope— Page | 1 Suggested Celestial Targets with Historical Canadian Resonance 2018 September 16 Robotic Telescope—Suggested Celestial Targets with Historical Canadian Resonance ABSTRACT: At the request of the Society’s Robotic Telescope Team, the RASC History Committee has compiled a list of over thirty (30) suggested targets for imaging with the RC Optical System (Ritchey- Chrétien f/9 0.4-metre class, with auxiliary wide-field capabilities), chosen from mainly “deep sky objects Page | 2 which are significant in that they are linked to specific events or people who were noteworthy in the 150 years of Canadian history”. In each numbered section the information is arranged by type of object, with specific targets suggested, the name or names of the astronomers (in bold) the RASC Robotic Telescope image is intended to honour, and references to select relevant supporting literature. The emphasis throughout is on Canadian astronomers (in a generous sense), and RASC connections. NOTE: The nature of Canadian observational astronomy over most of that time changed slowly, but change it did, and the accepted celestial targets, instrumental capabilities, and recording methods are frequently different now than they were in 1868, 1918, or 1968, and those differences can startle those with modern expectations looking for analogues to present/contemporary practice. The following list attempts to balance those expectations, as well as the commemoration of professionals and amateurs from our past. 1. OBJECT: Detail of lunar terminator (any feature). ACKNOWLEDGES: 18th-19th century practical astronomy (astronomy of place & time), the practitioners of which used lunar observation (shooting lunars) to determine longitude.
    [Show full text]
  • Neutral Hydrogen in Arp
    Neutral Hydrogen in Arp 158 Mansie G. Iyer and Caroline E. Simpson Department of Physics, Florida International University, Miami, Fl 33199 [email protected], [email protected] Stephen T. Gottesman Department of Astronomy, University of Florida, Gainesville, FL 32611 [email protected] and Benjamin K. Malphrus Department of Physical Sciences, Morehead State University, Morehead, KY 40351 [email protected] ABSTRACT We present 21 cm observations of Arp 158. We have performed a study of the neutral hydrogen (H i) to help us understand the overall formation and evolution of this system. This is a disturbed system with distinct optical knots connected by a linear structure embedded in luminous material. There is also a diffuse spray to the southeast. The H i seems to be made up of three distinct, kinematically separate systems. Arp 158 bears a certain optical resemblance to NGC 520 (Arp 157), which has been identified as a mid- stage merger. From our 21 cm observations of Arp 158, we also see a comparable H i arXiv:astro-ph/0405405v1 20 May 2004 content with NGC 520. These similarities suggest that Arp 158 is also an intermediate stage merger. Subject headings: galaxies: interacting – individual galaxy (Arp 158) – ISM: H i 1. INTRODUCTION In the early seventies, Toomre (1970) and Toomre & Toomre (1972), presented numerical models which demonstrated that strong tidal forces between interacting galaxies could result in features like plumes, shells, rings, tidal tails, and bridges. They also proposed that such strong collisions between galaxies would lead to orbital decay and eventual merging. In 1977, Toomre identified a series of galaxies that he believed represented galaxies at different stages of merging – 2 – (“The Toomre Sequence”) and proposed that the end product of such merging could be an elliptical galaxy.
    [Show full text]
  • And Ecclesiastical Cosmology
    GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc.
    [Show full text]
  • Characterizing the Radial Oxygen Abundance Distribution in Disk Galaxies? I
    A&A 623, A7 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834364 & c ESO 2019 Astrophysics Characterizing the radial oxygen abundance distribution in disk galaxies? I. A. Zinchenko1,2, A. Just2, L. S. Pilyugin1,2, and M. A. Lara-Lopez3 1 Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St., 03680 Kyiv, Ukraine e-mail: [email protected] 2 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12–14, 69120 Heidelberg, Germany 3 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark Received 2 October 2018 / Accepted 13 January 2019 ABSTRACT Context. The relation between the radial oxygen abundance distribution (gradient) and other parameters of a galaxy such as mass, Hubble type, and a bar strength, remains unclear although a large amount of observational data have been obtained in the past years. Aims. We examine the possible dependence of the radial oxygen abundance distribution on non-axisymmetrical structures (bar/spirals) and other macroscopic parameters such as the mass, the optical radius R25, the color g − r, and the surface brightness of the galaxy. A sample of disk galaxies from the third data release of the Calar Alto Legacy Integral Field Area Survey (CALIFA DR3) is considered. Methods. We adopted the Fourier amplitude A2 of the surface brightness as a quantitative characteristic of the strength of non- axisymmetric structures in a galactic disk, in addition to the commonly used morphologic division for A, AB, and B types based on the Hubble classification. To distinguish changes in local oxygen abundance caused by the non-axisymmetrical structures, the multiparametric mass–metallicity relation was constructed as a function of parameters such as the bar/spiral pattern strength, the disk size, color index g−r in the Sloan Digital Sky Survey (SDSS) bands, and central surface brightness of the disk.
    [Show full text]
  • A Search for Transiting Extrasolar Planets in the Open Cluster NGC 4755
    ResearchOnline@JCU This file is part of the following reference: Jayawardene, Bandupriya S. (2015) A search for transiting extrasolar planets in the open cluster NGC 4755. DAstron thesis, James Cook University. Access to this file is available from: http://researchonline.jcu.edu.au/41511/ The author has certified to JCU that they have made a reasonable effort to gain permission and acknowledge the owner of any third party copyright material included in this document. If you believe that this is not the case, please contact [email protected] and quote http://researchonline.jcu.edu.au/41511/ A SEARCH FOR TRANSITING EXTRASOLAR PLANETS IN THE OPEN CLUSTER NGC 4755 by Bandupriya S. Jayawardene A thesis submitted in satisfaction of the requirements for the degree of Doctor of Astronomy in the Faculty of Science, Technology and Engineering June 2015 James Cook University Townsville - Australia i STATEMENT OF ACCESS I the undersigned, author of this work, understand that James Cook University will make this thesis available for use within the University Library and, via the Australian Digital Thesis network, for use elsewhere. I understand that, as an unpublished work, a thesis has significant protection under the Copyright Act and; I do not wish to place any further restriction on access to this work. 2 STATEMENT OF SOURCES DECLARATION I declare that this thesis is my own work and has not been submitted in any form for another degree or diploma at any University or other institution of tertiary education. Information derived from the published or unpublished work of others has been acknowledged in the text and list of references is given.
    [Show full text]
  • The 2011 Observers Challenge List
    TMSP OBSERVER'S CHALLENGE 2011 By Kreig McBride and Tom Masterson All observations must be made at TMSP and 25 out of 30 objects must be viewed to earn a unique TMSP Observer's Award lapel pin. You must create a record of your observations which include date, time, instruments used and a brief description and/or sketch of the object. Your records will be returned to you. Size or ID Number V Magnitude Object Type Constellation RA Dec Description Separation The Sun! View 2 days noting changes. H-alpha, white 1 Sol -28m ½ degree Star Cancer 08h 39' +27d 07' light or projection is OK North Galactic Astronomical Catch this one before it sets. Next to the double star 31 2 N/A N/A Coma Berenices 12h 51' +27d 07' Pole Reference point Comae Berenices Omicron-2 a wide 4.9m, 9m double lies close by as does 3 U Cygni 5.9 – 12.1m N/A Carbon Star Cygnus 19.6h +47d 54' 6” diameter, 12.6m Planetary nebula NGC6884 4 M22 5.1m 7.8' Globular Cluster Sagittarius 18h 36.4' -23d 54' Rich, large and bright 5 NGC 6629 11.3m 15” Planetary Nebula Sagittarius 18h 25.7' -23d 12' Stellar at low powers. Central Star is 12.8m 6 Barnard 86 N/A 5' Dark Nebula Sagittarius 18h 03' -27d 53' “Ink Spot” Imbedded in spectacular star field Faint 1' glow surrounding 9.5m star w/a faint companion 7 NGC 6589-90 N/A 5' x 3' Reflection Nebula Sagittarius 18h 16.9'' -19d 47' 25” to its SW A 3.2m, B Reddish/Orange primary, B white, C is 10m companion 8 ETA Sagittarii 3.6m, C 10m, AB pair 3.6” Quadruple Star Sagittarius 18h 17.6' -36d 46' 93” distant at PA303d and D is 13m star 33”
    [Show full text]
  • Distant Arm - NGC772
    29 September 2016, Zeiss Cas 150/2250 Distant Arm - NGC772 Telescope: Zeiss Cassegrain 150/2250 Eyepieces: ATC53P - ATC Plossl, f=53mm, (42×, 530) ATC20K - ATC Kellner, f=20mm, (113×, 220) A-16 - Zeiss Abbe Ortho, f=16mm, (141×, 200) O-12.5 - CZJ Ortho, f=12.5mm, (180×, 140) Time: 2016/09/29 19:30-21:40UT Location: R´ıˇcanyˇ Weather: Clear sky with slight haze and decaying small thin clouds. Mount: Zeiss 1b Accessories: Baader/Zeiss T2 prism This was my typical backyard session. I could go out only for a short time after I put all three kids in to their beds. The night was still warm. Normally, I would try to take an advantage of it and go to some darker place. As I was alone with the kids for the whole week I was bound to stay in our backyard. During last couple of years, I have learnt to live with this handicap. There is always something interesting to look at, even with small refractors. Recently, I was explor- ing the capability of my largest telescope, 150mm Cassegrain. For this night, the main targets were two galaxies, NGC 660 and NGC 772, which I had troubles to locate two days before in 80mm refractor. I was curios how much of help the larger telescope would be. I did not jump to these two galaxies im- mediately. They were still low in the slight haze enhanced by the street lamps. I started a little bit higher in Andromeda with beau- tiful edge-on galaxy NGC 891 (V=10.0, 13:50 ×2:50, PA22◦).
    [Show full text]