Meade Instruments Corporation - Meade LX200 Instruction Manuals
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Arxiv:1704.01678V2 [Astro-Ph.GA] 28 Jul 2017 Been Notoriously Difficult, Resulting Mostly in Upper Lim- Highest Escape Fractions Measured to Date Among Low- Its (E.G
Submitted: 3 March 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 MRK 71 / NGC 2366: THE NEAREST GREEN PEA ANALOG Genoveva Micheva1, M. S. Oey1, Anne E. Jaskot2, and Bethan L. James3 (Accepted 24 July 2017) 1University of Michigan, 311 West Hall, 1085 S. University Ave, Ann Arbor, MI 48109-1107, USA 2Department of Astronomy, Smith College, Northampton, MA 01063, USA 3STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA ABSTRACT We present the remarkable discovery that the dwarf irregular galaxy NGC 2366 is an excellent analog of the Green Pea (GP) galaxies, which are characterized by extremely high ionization parameters. The similarities are driven predominantly by the giant H II region Markarian 71 (Mrk 71). We compare the system with GPs in terms of morphology, excitation properties, specific star-formation rate, kinematics, absorption of low-ionization species, reddening, and chemical abundance, and find consistencies throughout. Since extreme GPs are associated with both candidate and confirmed Lyman continuum (LyC) emitters, Mrk 71/NGC 2366 is thus also a good candidate for LyC escape. The spatially resolved data for this object show a superbubble blowout generated by mechanical feedback from one of its two super star clusters (SSCs), Knot B, while the extreme ionization properties are driven by the . 1 Myr-old, enshrouded SSC Knot A, which has ∼ 10 times higher ionizing luminosity. Very massive stars (> 100 M ) may be present in this remarkable object. Ionization-parameter mapping indicates the blowout region is optically thin in the LyC, and the general properties also suggest LyC escape in the line of sight. -
Meade Instruments Corporation Instruction Manual
Instruction Manual 16” LX200 Schmidt-Cassegrain Telescope Meade Instruments Corporation NOTE: Instructions for the use of optional accessories are not included in this manual. For details see the Meade General Catalog. The Meade Schmidt-Cassegrain Optical System (Diagram not to scale) In the Schmidt-Cassegrain design of the Meade 16” model, light enters from the right, passes through a thin lens (correcting plate) with two-sided aspheric correction, proceeds to a spherical primary mirror, and then to a convex aspheric secondary mirror. The convex secondary mirror multiplies the effective focal length of the primary mirror and results in a focus at the focal plane, with light passing through a central perforation in the primary mirror. The 16” model includes an oversize 16.375” primary mirror, yielding a fully illuminated field-of-view significantly wider than is possible with standard-size primary mirrors. Note that light ray (2) in the figure would be lost entirely, except for the oversize p r i m a r y. This phenomenon results in Meade 16” Schmidt- Cassegrains having off-axis field illuminations 10% greater, aperture-for-aperture, than other Schmidt-Cassegrains utilizing standard-size primary mirrors. WARNING! Never use the LX200 telescope to look at the Sun! Looking at or near the Sun will cause instant and irreversible damage to your eye. Eye damage is often painless, so there is no warning to the observer that damage has occurred until it is too late. Do not point the telescope or its viewfinder at or near the Sun. Do not look through the telescope or its viewfinder as it is moving. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
Arxiv:1803.10763V1 [Astro-Ph.GA] 28 Mar 2018
Draft version October 10, 2018 Typeset using LATEX default style in AASTeX61 TRACERS OF STELLAR MASS-LOSS - II. MID-IR COLORS AND SURFACE BRIGHTNESS FLUCTUATIONS Rosa A. Gonzalez-L´ opezlira´ 1 1Instituto de Radioastronomia y Astrofisica, UNAM, Campus Morelia, Michoacan, Mexico, C.P. 58089 (Received 2017 October 20; Revised 2018 February 20; Accepted 2018 February 21) Submitted to ApJ ABSTRACT I present integrated colors and surface brightness fluctuation magnitudes in the mid-IR, derived from stellar popula- tion synthesis models that include the effects of the dusty envelopes around thermally pulsing asymptotic giant branch (TP-AGB) stars. The models are based on the Bruzual & Charlot CB∗ isochrones; they are single-burst, range in age from a few Myr to 14 Gyr, and comprise metallicities between Z = 0.0001 and Z = 0.04. I compare these models to mid-IR data of AGB stars and star clusters in the Magellanic Clouds, and study the effects of varying self-consistently the mass-loss rate, the stellar parameters, and the output spectra of the stars plus their dusty envelopes. I find that models with a higher than fiducial mass-loss rate are needed to fit the mid-IR colors of \extreme" single AGB stars in the Large Magellanic Cloud. Surface brightness fluctuation magnitudes are quite sensitive to metallicity for 4.5 µm and longer wavelengths at all stellar population ages, and powerful diagnostics of mass-loss rate in the TP-AGB for intermediater-age populations, between 100 Myr and 2-3 Gyr. Keywords: stars: AGB and post{AGB | stars: mass-loss | Magellanic Clouds | infrared: stars | stars: evolution | galaxies: stellar content arXiv:1803.10763v1 [astro-ph.GA] 28 Mar 2018 Corresponding author: Rosa A. -
Deepsky User's Manual
Version 2014.1.2 By Steven S. Tuma and Dean Williams Copyright © 1996-2014 – All Rights Reserved 1 Table of Contents RELEASE NOTES ...................................................................................................... 7 Deepsky Release version 2014.01.02 ......................................................................................... 7 Deepsky Release version 2011.02.00 ......................................................................................... 7 Deepsky Release version 2011.01.01 ......................................................................................... 7 Deepsky Release version 2007.01.03 ....................................................................................... 10 INTRODUCTION .................................................................................................... 19 Welcome to Deepsky ............................................................................................................ 19 What’s Included ................................................................................................................... 19 AstroCards Add-on CD (available separately) ............................................................................ 19 What Is Deepsky? ................................................................................................................. 20 Deepsky Feature Overview ..................................................................................................... 21 SYSTEM REQUIREMENTS ...................................................................................... -
May 2003 Volume 10 Issue 7 II Hz 4
Hamilton Amateur Astronomers MayEvent 2003 Horizon Volume 10 Issue 7 II Hz 4 - An Odyssey by Tom Steckner It all started simply enough with an e-mail from An- one reference that seemed to be useful and authori- thony Tekatch: tative: http://www.noao.edu/image_gallery/html/ im0117.html (I’ll refer to this as “URL 1”). How- Hello Experts, ever, the only Herzog designated object they showed Would one of you like to tackle this question was something called II Hz 4 (“Hz” = “Herzog”). This for the newsletter? implied that there were at least two Herzog catalogues (i.e., inferred from the “II”) and that “Hz” was the stan- Would you please send me information on dard abbreviation for objects in this catalogue. So, back Herzog 2 the galaxy. I know it looks like this to Google, AltaVista, and Vizier. Nothing. So I went (0 0) and that it’s a gamma ray source for back to URL 1 to study it some more and noticed an the colliding galaxy effect. Yet I don’t have e-mail address at the bottom of it. What the heck, I the facts how; 1) far away it is and 2) where thought, and sent off a note - let’s see if we can get the it is of what constellation? Who may I ask NOAO to answer me. :-) for a telescopic 35mm photo of the Herzog 2 to buy for under $20. Question by Scott Florance, Seattle WA On the surface at least the request for informa- tion about “Herzog 2” seemed like it should be simple enough to satisfy. -
INFRARED SURFACE BRIGHTNESS FLUCTUATIONS of MAGELLANIC STAR CLUSTERS1 Rosa A
The Astrophysical Journal, 611:270–293, 2004 August 10 A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. INFRARED SURFACE BRIGHTNESS FLUCTUATIONS OF MAGELLANIC STAR CLUSTERS1 Rosa A. Gonza´lez Centro de Radioastronomı´a y Astrofı´sica, Universidad Nacional Autonoma de Me´xico, Campus Morelia, Michoaca´n CP 58190, Mexico; [email protected] Michael C. Liu Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; [email protected] and Gustavo Bruzual A. Centro de Investigaciones de Astronomı´a, Apartado Postal 264, Me´rida 5101-A, Venezuela; [email protected] Received 2003 November 27; accepted 2004 April 16 ABSTRACT We present surface brightness fluctuations (SBFs) in the near-IR for 191 Magellanic star clusters available in the Second Incremental and All Sky Data releases of the Two Micron All Sky Survey (2MASS) and compare them with SBFs of Fornax Cluster galaxies and with predictions from stellar population models as well. We also construct color-magnitude diagrams (CMDs) for these clusters using the 2MASS Point Source Catalog (PSC). Our goals are twofold. The first is to provide an empirical calibration of near-IR SBFs, given that existing stellar population synthesis models are particularly discrepant in the near-IR. Second, whereas most previous SBF studies have focused on old, metal-rich populations, this is the first application to a system with such a wide range of ages (106 to more than 1010 yr, i.e., 4 orders of magnitude), at the same time that the clusters have a very narrow range of metallicities (Z 0:0006 0:01, i.e., 1 order of magnitude only). -
July 2021 the Warren Astronomical Society Publication
Celebrating Sixty Years of the Warren Astronomical Society The W.A.S.P. Vol. 53, no. 7 Winner of the Astronomical League’s 2021 Mabel Sterns Award July 2021 The Warren Astronomical Society Publication 50 years Apollo 15 Mission Launched July 26, 1971- Returned August 7 The WASP Snack Volunteer Schedule Published by Warren Astronomical Society, Inc. The Snack Volunteer program is suspend- P.O. Box 1505 ed for the duration. When it resumes, vol- Warren, Michigan 48090-1505 unteers already on the list will be notified Dale Thieme, Editor by email. 2021 Officers President Diane Hall [email protected] 1st VP Dale Partin [email protected] 2ndVP Riyad Matti [email protected] Secretary Mark Kedzior [email protected] Treasurer Adrian Bradley [email protected] Outreach Bob Trembley [email protected] Publications Dale Thieme [email protected] Entire Board [email protected] The Warren Astronomical Society, Inc., is a local, non-profit organization of Discussion Group Meeting amateur astronomers. The Society holds meetings on the first Monday and third Thursday of each month, starting at 7:30 p.m. Come on over, and talk astronomy, space news, and whatnot! First Monday meeting: Third Thursday meeting: Cranbrook: Institute of Science Macomb Community College 1221 North Woodward Ave South campus, Bldg. J, Room J221 Bloomfield Hills, Michigan 14600 Twelve Mile Rd. Warren, Michigan Membership and Annual Dues Student Individual Senior Citizen for families In This Issue: $17.00 $30.00 $22.00 add $7.00 President’s Field of View ............................... 3 Astronomical League (optional) $7.50 Send membership applications and dues to the treasurer: Letters ......................................................... -
Fall 2005/Winter 2006
DOWN HOME gumbo astronomy from Chaos Manor South! Uncle Rod Mollise’s Fall 2005 – Winter 2006 Volume 14, Issue 4+ “A Newsletter for the Truly Skywatch Outbound!” Number 79 (New Series) : <[email protected]> Luckily, we here in Mobile, Alabama Grand Post were spared the worst, not experiencing anything like the In this Issue: devastating winds and water visited Katrina upon our brothers and sisters just to the west of us. “Near miss” is more Issue! than bad enough when you’re talking a storm as huge and deadly 1 Letter from the Coast as Katrina, but Mobile was back to A Letter from the Gulf something resembling normalcy in a few weeks. There are there are still 2 Denkmeier Powerswitch Coast plenty of signs of Bitch Katrina’s passing even four months down the line, though, and plenty of people in 3 DAS User’s Guide Part II Dear Friends (“Howdy Y’all”): the coastal areas of the county are still hurting bad. Some of you may have been 4 In Praise of DSCs wondering what happened to The main thing standing in the way Skywatch. I’ll confess that my little of Skywatch? Uncle Rod earns the newsletter has developed a small largest part of his livelihood as an 5 Apogee 25x100s following over the years; with each engineer at Northrop Grumman Ship issue being read by several Systems in Pascagoula, Mississippi thousand amateurs during the time (no, unfortunately, astronomy Tsunami from Space it’s current. And I have gotten some writers don’t get paid like Stephen 6 Kings, so most of us must hustle “whatever happened to Skywatch” emails recently. -
January 2021
The Newsletter of Westchester Amateur Astronomers January 2021 The Heart Nebula by Leandro Bento The Heart Nebula, catalogued as IC 1805 and Sharpless 2-190, is an emission nebula in Cassiopeia, 7500 light-years from Earth. Leo’s image shows a 2½-degree field. The hydrogen gas in IC 1805 fluoresces from radiation emitted by large hot stars in open cluster Collinder 26/Melotte 15 in the middle of the nebula. Open cluster NGC 1027 sits at the right edge but it’s a foreground object. William Optics RedCat 51 mm f/4.9 Petzval refractor, ASI ZWO533MC Pro, Optolong L-eNhance filter, iOpton SkyGuider mount. 68 x 180 sec subs with darks, flats and bias frames. SERVING THE ASTRONOMY COMMUNITY SINCE 1986 1 Westchester Amateur Astronomers SkyWAAtch January 2021 WAA January 2021 Meeting WAA February 2021 Meeting Friday, January 15 at 7:30 pm Friday, February 12 at 7:30 pm On-line via Zoom On-line via Zoom Microquasars Update on Mars Research Diana Hannikainen, Ph.D. Br. Robert Novak, Ph.D. Observing Editor Sky & Telescope Iona College & Goddard Spaceflight Microquasars are stellar-mass black holes in our gal- Flight Center axy that pull mass from a companion star. They emit Our regular Mars update with Br. Novak. There’s a lot X-rays and generate jets of subatomic particles along happening at Mars! their axis of rotation, just like galactic quasars but on a much smaller scale. Call: 1-877-456-5778 (toll free) for announcements, Diana Hannikainen got her undergraduate degree at weather cancellations, or questions. -
A Radio Continuum Study of the Magellanic Clouds VI
ASTRONOMY & ASTROPHYSICS JANUARY II 1998, PAGE 119 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 127, 119-138 (1998) A radio continuum study of the Magellanic Clouds VI. Discrete sources common to radio and X-ray surveys of the Magellanic Clouds? M.D. Filipovi´c1,2,3,W.Pietsch3,R.F.Haynes2,1,G.L.White1,P.A.Jones1,R.Wielebinski4, U. Klein5, K. Dennerl3, P. Kahabka3,6, and J.S. Lazendi´c7,1 1 University of Western Sydney, Nepean, P.O. Box 10, Kingswood, NSW 2747, Australia fi[email protected]; [email protected]; [email protected] 2 Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 2121, Australia mfi[email protected]; [email protected] 3 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, D-85740 Garching, Germany [email protected]; [email protected] 4 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, D-53121 Bonn, Germany [email protected] 5 Radioastronomisches Institut der Universitat Bonn, Auf dem H¨ugel 71, D-53121 Bonn, Germany [email protected] 6 Center for High Energy Astrophysics, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands [email protected] 7 Department of Astronomy, University of Belgrade, Studentski trg 13, 11000 Beograd, Serbia, Yugoslavia [email protected] Received March 3; accepted April 24, 1997 Abstract. By comparing Parkes telescope radio surveys new SMC sources are proposed for SNR candidates. with the X-ray ROSAT All-Sky Survey (RASS) we have The SMC SNR birth rate was estimated to be one found 71 discrete sources of both radio and X-ray emission every 350 (±70) yr and the SFR was estimated to be −1 in the Large Magellanic Cloud (LMC). -
1. Alignment Stars CDS ALIGNMENT STAR LIBRARY
- 20 - APPENDIX B: ALIGNMENT STAR LIBRARY AND STAR CHARTS: 1. Alignment Stars The CDS utilizes 33 bright and well-known stars to calibrate the telescope’s Object Library during the computerized alignment process. These stars were selected to allow observers from anywhere in the world on any given night, to be able to easily and quickly make precision alignments. The CDS Alignment Star Library and Star Charts are listed below for your reference: CDS ALIGNMENT STAR LIBRARY STAR NAME STAR # MAGNITUDE CONSTELL R/A DEC. ACHERNAR 13 0.5 ERIDANUS 01 37.7 -57 14 ACRUX A 121 1.3 CRUX 12 26.6 -63 06 ALBIREO 223 3.1 CYGNUS 19 30.8 +27 58 ALKAID 140 1.9 URSA MAJOR 13 47.6 +49 19 ALDEBARAN 33 0.9 TAURUS 04 35.9 +16 31 ALNILAM 50 1.7 ORION 05 36.2 -01 12 ALPHARD 95 2.0 HYDRA 09 27.6 -08 39 ALPHEKKA 165 2.2 CORONA BOR. 15 35.5 +26 43 ALTAIR 226 0.8 AQUILA 19 50.8 +08 52 ANTARES 177 0.9 SCORPIUS 16 29.5 -26 26 ARCTURUS 147 0.0 BOOTES 14 15.7 +19 11 BETELGUESE 56 0.4 ORION 05 55.2 +07 25 BOGARDUS 58 2.6 AURIGA 05 59.8 +37 13 CANOPUS 63 -0.7 CARINA 06 24.0 -52 42 CAPELLA 42 0.1 AURIGA 05 16.6 +46 00 CASTOR A 78 1.9 GEMINI 07 34.6 +31 53 DENEB 232 1.3 CYGNUS 20 41.5 +45 17 DENEBOLA 114 2.1 LEO 11 49.1 +14 34 DIPHDA 8 2.0 CETUS 00 43.6 -17 59 ENIF 238 2.4 PEGASUS 21 44.2 +09 53 FOMALHAUT 247 1.2 PISCES AUST.