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Stsci Newsletter: 1997 Volume 014 Issue 01
January 1997 • Volume 14, Number 1 SPACE TELESCOPE SCIENCE INSTITUTE Highlights of this issue: • AURA science and functional awards to Leitherer and Hanisch — pages 1 and 23 • Cycle 7 to be extended — page 5 • Cycle 7 approved Newsletter program listing — pages 7-13 Astronomy with HST Climbing the Starburst Distance Ladder C. Leitherer Massive stars are an important and powerful star formation events in sometimes dominant energy source for galaxies. Even the most luminous star- a galaxy. Their high luminosity, both in forming regions in our Galaxy are tiny light and mechanical energy, makes on a cosmic scale. They are not them detectable up to cosmological dominated by the properties of an distances. Stars ~100 times more entire population but by individual massive than the Sun are one million stars. Therefore stochastic effects times more luminous. Except for stars prevail. Extinction represents a severe of transient brightness, like novae and problem when a reliable census of the supernovae, hot, massive stars are Galactic high-mass star-formation the most luminous stellar objects in history is atempted, especially since the universe. massive stars belong to the extreme Massive stars are, however, Population I, with correspondingly extremely rare: The number of stars small vertical scale heights. Moreover, formed per unit mass interval is the proximity of Galactic regions — roughly proportional to the -2.35 although advantageous for detailed power of mass. We expect to find very studies of individual stars — makes it few massive stars compared to, say, difficult to obtain integrated properties, solar-type stars. This is consistent with such as total emission-line fluxes of observations in our solar neighbor- the ionized gas. -
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). -
Ioptron CEM40 Center-Balanced Equatorial Mount
iOptron®CEM40 Center-Balanced Equatorial Mount Instruction Manual Product CEM40 (#7400A series) and CEM40EC (#7400ECA series, as shown) Please read the included CEM40 Quick Setup Guide (QSG) BEFORE taking the mount out of the case! This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. You must hold the mount firmly when disengaging the gear switches. Otherwise personal injury and/or equipment damage may occur. Any worm system damage due to improper operation will not be covered by iOptron’s limited warranty. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while using a telescope. 2 Table of Contents Table of Contents ........................................................................................................................................ 3 1. CEM40 Introduction ............................................................................................................................... 5 2. CEM40 Overview ................................................................................................................................... 6 2.1. Parts List ......................................................................................................................................... -
6.- Methods for Latitude and Longitude Measurement
Chapter 6 Copyright © 1997-2004 Henning Umland All Rights Reserved Methods for Latitude and Longitude Measurement Latitude by Polaris The observed altitude of a star being vertically above the geographic north pole would be numerically equal to the latitude of the observer ( Fig. 6-1 ). This is nearly the case with the pole star (Polaris). However, since there is a measurable angular distance between Polaris and the polar axis of the earth (presently ca. 1°), the altitude of Polaris is a function of the local hour angle. The altitude of Polaris is also affected by nutation. To obtain the accurate latitude, several corrections have to be applied: = − ° + + + Lat Ho 1 a0 a1 a2 The corrections a0, a1, and a2 depend on LHA Aries , the observer's estimated latitude, and the number of the month. They are given in the Polaris Tables of the Nautical Almanac [12]. To extract the data, the observer has to know his approximate position and the approximate time. When using a computer almanac instead of the N. A., we can calculate Lat with the following simple procedure. Lat E is our estimated latitude, Dec is the declination of Polaris, and t is the meridian angle of Polaris (calculated from GHA and our estimated longitude). Hc is the computed altitude, Ho is the observed altitude (see chapter 4). = ( ⋅ + ⋅ ⋅ ) Hc arcsin sin Lat E sin Dec cos Lat E cos Dec cos t ∆ H = Ho − Hc Adding the altitude difference, ∆H, to the estimated latitude, we obtain the improved latitude: ≈ + ∆ Lat Lat E H The error of Lat is smaller than 0.1' when Lat E is smaller than 70° and when the error of Lat E is smaller than 2°, provided the exact longitude is known. -
A.K.A., a Simple Explanation of All Exoplanet Images to Date
TheThe RoleRole ofof StellarStellar MassMass inin High-ContrastHigh-Contrast ImagingImaging JustinJustin R.R. Crepp,Crepp, JohnJohn A.A. JohnsonJohnson (a.k.a.,(a.k.a., aa simplesimple explanationexplanation ofof CaliforniaCalifornia InstituteInstitute ofof TechnologyTechnology arXiv:1103:4910 (accepted to ApJ) allall exoplanetexoplanet imagesimages toto date)date) (1)(1) WhyWhy havehave thethe firstfirst handfulhandful ofof exoplanetexoplanet imagesimages beenbeen (5)(5) TableTable 11 andand ourour simulationsimulation resultsresults areare consistentconsistent withwith thethe aroundaround M,KM,K andand AA stars,stars, butbut nono spectralspectral typestypes inin between?between? (3)(3) TwoTwo additionaladditional observationalobservational resultsresults supportsupport presencepresence ofof twotwo differentdifferent planetplanet formationformation mechanisms:mechanisms: oneone operatingoperating ThisThis mustmust bebe tellingtelling usus somethingsomething aboutabout planetplanet formation.formation. interpretationinterpretation ofof BetaBeta PicPic bb andand thethe HRHR 87998799 planetsplanets asas closeclose toto starsstars thatthat resultsresults inin strongstrong correlationscorrelations betweenbetween starstar massmass formingforming byby ªcore-accretionº:ªcore-accretionº: andand planetplanet properties,properties, andand anotheranother operatingoperating furtherfurther fromfrom starsstars (or(or (i) Beta Pic b and HR 8799 bcde fall in the possiblypossibly atat allall separations)separations) wherewhere therethere existsexists -
GEORGE HERBIG and Early Stellar Evolution
GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study. -
Supernova Star Maps
Supernova Star Maps Which Stars in the Night Sky Will Go Su pernova? About the Activity Allow visitors to experience finding stars in the night sky that will eventually go supernova. Topics Covered Observation of stars that will one day go supernova Materials Needed • Copies of this month's Star Map for your visitors- print the Supernova Information Sheet on the back. • (Optional) Telescopes A S A Participants N t i d Activities are appropriate for families Cre with children over the age of 9, the general public, and school groups ages 9 and up. Any number of visitors may participate. Location and Timing This activity is perfect for a star party outdoors and can take a few minutes, up to 20 minutes, depending on the Included in This Packet Page length of the discussion about the Detailed Activity Description 2 questions on the Supernova Helpful Hints 5 Information Sheet. Discussion can start Supernova Information Sheet 6 while it is still light. Star Maps handouts 7 Background Information There is an Excel spreadsheet on the Supernova Star Maps Resource Page that lists all these stars with all their particulars. Search for Supernova Star Maps here: http://nightsky.jpl.nasa.gov/download-search.cfm © 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 Star Maps: Stars likely to go Supernova! Leader’s Role Participants’ Role (Anticipated) Materials: Star Map with Supernova Information sheet on back Objective: Allow visitors to experience finding stars in the night sky that will eventually go supernova. -
Search for Associations Containing Young Stars (SACY). V. Is
Astronomy & Astrophysics manuscript no. sacy˙1˙accepted˙arxiv˙2 c ESO 2018 October 2, 2018 Search for associations containing young stars (SACY) V. Is multiplicity universal? Tight multiple systems?;??;??? P. Elliott1;2, A. Bayo1;3;4, C. H. F. Melo1, C. A. O. Torres5, M. Sterzik1, and G. R. Quast5 1 European Southern Observatory, Alonso de Cordova 3107, Vitacura Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL 3 Max Planck Institut fur¨ Astronomie, Konigstuhl¨ 17, 69117, Heidelberg, Germany 4 Departamento de F´ısica y Astronom´ıa, Facultad de Ciencias, Universidad de Valpara´ıso, Av. Gran Bretana˜ 1111, 5030 Casilla, Valpara´ıso, Chile 5 Laboratorio´ Nacional de Astrof´ısica/ MCT, Rua Estados Unidos 154, 37504-364 Itajuba´ (MG), Brazil Received 21 March 2014 / Accepted 5 June 2014 ABSTRACT Context. Dynamically undisrupted, young populations of stars are crucial in studying the role of multiplicity in relation to star formation. Loose nearby associations provide us with a great sample of close (<150 pc) pre-main sequence (PMS) stars across the very important age range (≈5-70 Myr) to conduct such research. Aims. We characterize the short period multiplicity fraction of the search for associations containing young stars (SACY) sample, accounting for any identifiable bias in our techniques and present the role of multiplicity fractions of the SACY sample in the context of star formation. Methods. Using the cross-correlation technique we identified double-lined and triple-lined spectroscopic systems (SB2/SB3s), in addition to this we computed radial velocity (RV) values for our subsample of SACY targets using several epochs of fiber-fed extended range optical spectrograph (FEROS) and ultraviolet and visual echelle spectrograph (UVES) data. -
Exercises in Archaeoastronomy -2 -The Passage Mound of Newgrange Amelia Carolina Sparavigna
Exercises in Archaeoastronomy -2 -The passage mound of Newgrange Amelia Carolina Sparavigna To cite this version: Amelia Carolina Sparavigna. Exercises in Archaeoastronomy -2 -The passage mound of Newgrange. Philica, Philica, 2018. hal-01712819 HAL Id: hal-01712819 https://hal.archives-ouvertes.fr/hal-01712819 Submitted on 19 Feb 2018 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Exercises in Archaeoastronomy - 2 - The passage mound of Newgrange Amelia Carolina Sparavigna (Department of Applied Science and Technology, Politecnico di Torino) Published in enviro.philica.com Abstract Here it is given the second article of a series proposing exercises in archaeoastronomy. The reader can find exercises about the apparent motion of the sun, and its azimuth and altitude given in the horizontal coordinate system. As case study, we investigate the orientation of the prehistoric passage mound of Newgrange. In the previous article [1], we have introduced a series of exercises in archaeoastronomy. Let us start the series by studying the sun and its horizontal coordinates. After exercises on azimuth and altitude of the sun, we consider some prehistoric monuments. In particular we propose exercises on the passage mound of Newgrange, as a case study. -
Calibrating the Metallicity of M Dwarfs in Wide Physical Binaries with F-, G
MNRAS 000, 1–49 (2018) Preprint 16 May 2018 Compiled using MNRAS LATEX style file v3.0 Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K- primaries – I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics⋆ D. Montes1†, R. González-Peinado1, H. M. Tabernero2,1, J. A. Caballero3, E. Marfil1, F. J. Alonso-Floriano4,1, M. Cortés-Contreras3, J. I. González Hernández5,6, A. Klutsch7,1, and C. Moreno-Jódar8,1 1Departamento de Física de la Tierra y Astrofísica & UPARCOS-UCM (Unidad de Física de Partículas y del Cosmos de la UCM), Facultad de Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain 2Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante, Apdo. 99 E-03080, Alicante, Spain 3Centro de Astrobiología (INTA–CSIC), ESAC campus, Camino Bajo del Castillo s/n, E-28691 Villanueva de la Cañada, Madrid, Spain 4Leiden Observatory, Leiden University, 2300 RA Leiden, Netherlands 5Instituto de Astrofísica de Canarias (IAC), Calle Vía Lácteas/n, E-38200 La Laguna, Tenerife, Spain 6Departamento Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain 7INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy 8Escuela Técnica Superior de Ingeniería Aeronáutica y del Espacio, Plaza de Cardenal Cisneros 3, E-28040, Madrid, Spain Accepted 2018 May 09. Received 2018 May 09; in original form 2018 March 02 ABSTRACT We investigated almost 500 stars distributed among 193 binary or multiple systems made of late-F, G-, or early-K primaries and late-K or M dwarf companion candidates. -
Search for Associations Containing Young Stars (SACY) VII
A&A 590, A13 (2016) Astronomy DOI: 10.1051/0004-6361/201628253 & c ESO 2016 Astrophysics Search for associations containing young stars (SACY) VII. New stellar and substellar candidate members in the young associations?,?? P. Elliott1; 2, A. Bayo3, C. H. F. Melo1, C. A. O. Torres4, M. F. Sterzik5, G. R. Quast4, D. Montes6, and R. Brahm7; 8 1 European Southern Observatory, Alonso de Cordova 3107, Vitacura Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL 3 Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, 5030 Casilla, Valparaíso, Chile 4 Laboratório Nacional de Astrofísica/ MCT, Rua Estados Unidos 154, 37504-364 Itajubá (MG), Brazil 5 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 6 Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain 7 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 8 Millennium Institute of Astrophysics, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile Received 4 February 2016 / Accepted 7 March 2016 ABSTRACT Context. The young associations offer us one of the best opportunities to study the properties of young stellar and substellar objects and to directly image planets thanks to their proximity (<200 pc) and age (≈5−150 Myr). However, many previous works have been limited to identifying the brighter, more active members (≈1 M ) owing to photometric survey sensitivities limiting the detections of lower mass objects. -
2003 Astronomy Magazine Index
2003 astronomy magazine index Catchall (Martian crater), 11:30 observing Mars from, 7:32 hydrogen, 10:28 Subject index CCD (charge-coupled device) cameras, planets like, 6:48–53 Hydrus (constellation), 10:72–75 3:84–87, 5:84–87 seasons of, 3:72–73 A CCD techniques, 9:100–105 tilt of axis, 2:68, 5:72–73 I accidents, space-related, 7:42–47 Celestron C6-R (refractor), 11:84 EarthExplorer web site, 4:30 Achernar (star), 10:30 iceball, found beyond Pluto, 1:24 Celestron C8-N (reflector), 11:86 eclipses India, plans to visit Moon, 10:29 Advanced Camera for Surveys, 4:28 Celestron CGE-1100 (amateur telescope), in Australia (2003), 4:80–83 ALMA (Atacama Large Millimeter Array), infrared survey, 8:31 11:88 lunar integrating wavelengths, 4:24 3:36 Celestron NexStar 8 GPS (amateur telescope), of 2003, 5:18 Amalthea (Jupiter’s moon), 4:28 interferometry 1:84–87 of May 15, 2003, 5:60, 80–83, 88–89 techniques for, 7:48–53 Amateur Achievement Award, 9:32 Celestron NexStar 8i (amateur telescope), solar Andromeda Galaxy VLT interferometer, 2:32 11:89 of May 31, 2003, 5:80–83, 88–89 International Space Station, 3:31 picture of, 2:12–13 Centaurus A (NGC 5128) galaxy Edgar Wilson Award, 11:30 young stars in, 9:86–89 Internet, virtual observatories on, 9:80–85 1,000 Mira stars discovered in, 10:28 Egg Nebula, 8:36 Intes MK67 (amateur telescope), 11:89 Annefrank (asteroid), 2:32 picture of, 10:12–13 elliptical galaxies, 8:31 antineutrinos, 4:26 Io (Jupiter’s moon), 3:30 ripped apart satellite galaxy, 2:32 Eta Carinae (nebula), 5:29 ISAAC multi-mode instrument, 4:32 antisolar point, 10:18 Centaurus (constellation), 4:74–77 ETX-90EC (amateur telescope), 11:89 Antlia (constellation), 4:74–77 cepheid variable stars, 9:90–91 Europa (Jupiter’s moon), 12:30, 77 aphelion, 6:68–69 Challenger (space shuttle), 7:42–47 exoplanet magnetosphere, 11:28 J Apollo 1 (spacecraft), 7:42–47 J002E3 satellite, 1:30 Chamaeleon (constellation), 12:80–83 extrasolar planets.