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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. -
On the Weak-Wind Problem in Massive Stars: X-Ray Spectra Reveal a Massive Hot Wind in Mu Columbae
East Tennessee State University From the SelectedWorks of Richard Ignace September 10, 2012 On the Weak-Wind Problem in Massive Stars: X- Ray Spectra Reveal a Massive Hot Wind in mu Columbae. David P. Huenemoerder, Massachusetts nI stitute of Technology Lidia M. Oskinova, University of Potsdam Richard Ignace, East Tennessee State University Wayne L. Waldron, Eureka Scientific nI c. Helge Todt, University of Potsdam, et al. Available at: https://works.bepress.com/richard_ignace/61/ The Astrophysical Journal Letters, 756:L34 (5pp), 2012 September 10 doi:10.1088/2041-8205/756/2/L34 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ON THE WEAK-WIND PROBLEM IN MASSIVE STARS: X-RAY SPECTRA REVEAL A MASSIVE HOT WIND IN μ COLUMBAE David P. Huenemoerder1, Lidia M. Oskinova2, Richard Ignace3, Wayne L. Waldron4, Helge Todt2, Kenji Hamaguchi5,6, and Shunji Kitamoto7 1 Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, Cambridge, MA 02139, USA 2 Institute for Physics and Astronomy, University of Potsdam, D-14476 Potsdam, Germany 3 Department of Physics and Astronomy, East Tennessee State University, Johnson City, TN 37614, USA 4 Eureka Scientific Inc., 2452 Dellmer Street, Suite 100, Oakland, CA 94602, USA 5 CRESST and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771, USA 6 Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA 7 Department of Physics, Rikkyo University, Tokyo 171-8501, Japan Received 2012 June 16; accepted 2012 August 3; published 2012 August 22 ABSTRACT μ Columbae is a prototypical weak-wind O star for which we have obtained a high-resolution X-ray spectrum with the Chandra LETG/ACIS instrument and a low-resolution spectrum with Suzaku. -
2013 Trophy Winners - Saturday Participants Choice
2013 Trophy Winners - Saturday Participants Choice Class 1- A Body 1st Place: Dennis Bentley 1969 Dodge Dart 2nd Place: Joe Valenza 1964 Dodge Dart 3rd Place: Jerry & Judy Purchell 1967 Plymouth Barracuda Convertible Class 2- Pre 71 B Body 1st Place: Tom Brown 1962 Dodge Dart 2nd Place: Kendall Cayson 1966 Dodge Charger 3rd Place: Charles Carpenter 1969 Plymouth Road Runner Class 3 -71 & Up B Body 1st Place: Robert Craven 1972 Plymouth Class 4- C Body 1st Place: Donald Bueter 1963 Chrysler New Yorker 2nd Place: Jimmy Walden 1968 Plymouth Sport Fury Class 5- E Body 1st Place: Rod & Denise Nelms 1970 Plymouth Hemi Cuda 2nd Place: Bill Flynn 1971 Plymouth Cuda 3rd Place: Ola Nilsson 1970 Plymouth Cuda 340 Class 6- Truck and Van 1st Place: Mike & Chris Bilello 1964 Dodge D100 Town Wagon 2nd Place: Neil Hersman 2004 Dodge Ram 1500 Hemi GTX 3rd Place: Nathan Reichart 2007 Dodge Ram Class 7- Other Mopars 1st Place: Brian Hermany 1949 Dodge Wayfarer Business Coupe 2nd Place: Marshall Goodknight 1955 Chrysler 300 3rd Place: John GoodKnight 1955 Chrysler New Yorker St Regis Class 8- 2001 & Newer Not Classified Elsewhere 1st Place: John Sigountos 2010 Dodge Charger RT 2nd Place: Alvin Snellgrove 2009 Dodge Challenger SRT 8 3rd Place: Carol & William Ray 2008 Dodge Charger SRT Super bee Class 9 – FWD 1st Place: Doug McCabe 83 ½ Dodge Shelby Charger Class 10- AMC 1st Place: Kay & Manuel Cheek 1969 ½ AMC Hurst S/C Rambler 2nd Place: Earl Sheppard 1975 AMC Gremlin 3rd Place: Andre Gordon 1965 Rambler American Garlits Choice: Mike Myhvorld 1958 Plymouth -
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). -
2014 Garlits Trophy Winners Saturday--Participants’ Choice
2014 GARLITS TROPHY WINNERS SATURDAY--PARTICIPANTS’ CHOICE CLASS 1--“A” BODY 3RD PLACE--CHARLES SCHOSSER VEHICLE--1974 DODGE DART HANG 10 2ND PLACE--JOHN BALOW VEHICLE--1968 PLYMOUTH BARRACUDA 1ST PLACE--JOE VALENZA VEHICLE--1964 DODGE DART GT CLASS 2--“B” BODY PRE 1971 3RD PLACE--CHARLES DANCY VEHICLE--1968 PLYMOUTH GTX 2ND PLACE--BARRY WARD VEHICLE--1962 PLYMOUTH SAVOY 1ST PLACE--JIM BOYLE VEHICLE--1969 DODGE CORONET R/T CLASS 3--“B” BODY 1971 & NEWER 3RD PLACE--TOM BROWN VEHICLE--1972 DODGE CHARGER 2ND PLACE--DENNIS COSTANTINO VEHICLE--1972 DODGE CHARGER SE 1ST PLACE--PAUL REYNOLDS VEHICLE--1971 DODGE SUPER BEE 2014 GARLITS TROPHY WINNERS SATURDAY--PARTICIPANTS’ CHOICE CLASS 4--“C” BODY 3RD PLACE--STEVE GRYBOSKI VEHICLE--1967 PLYMOUTH SPORT FURY 2ND PLACE--NEIL MAHAR VEHICLE--1965 PLYMOUTH FURY III 1ST PLACE--MIKE BONADONNA VEHICLE--1965 PLYMOUTH FURY III CLASS 5--“E” BODY 3RD PLACE--BILL FLYNN VEHICLE--1971 PLYMOUTH CUDA 2ND PLACE--BILL PAULSON VEHICLE--1971 PLYMOUTH CUDA 1ST PLACE--LARRY GIBB VEHICLE--1970 DODGE CHALLENGER T/A CLASS 6--TRUCK & VAN 3RD PLACE--NAT WOLFE VEHICLE--1979 JEEP 442 2ND PLACE--MIKE & DEB WALKER VEHICLE--1965 DODGE A-100 1ST PLACE--MIKE BILELLO VEHICLE--1964 DODGE D-100 TOWN WAGON 2014 GARLITS TROPHY WINNERS SATURDAY--PARTICIPANTS’ CHOICE CLASS 7--OTHER MOPARS 3RD PLACE--NEWBOM SHELLMAN VEHICLE--1948 CHRYSLER TOWN & COUNTRY 2ND PLACE--DONALD HERMANY VEHICLE--1950 DODGE WAYFARER 1ST PLACE--MIKE MCANDREWS VEHICLE--1940 DESOTO CUSTOM BUS. COUPE CLASS 8--2001 & NEWER (NOT CLASSIFIED ELSEWHERE) 3RD PLACE--JIM PERDOMO -
Wanted in Stock
Wanted In Stock Vehicles that were used as part of daily work Runs/Drives 46-Dodge Bank Armored Car (Front Done, Back Unrestored) Metro Route Vans 47-Chrysler Suicide 4Dr (Needs Int. Radio Rblt. Wiper Not, Paint OK) Police Cars Milk Trucks 49-Dodge Business Coupe (Stock Eng/Trans, Smooth Seams, V Windshield, No Wings) Fire Cars Concession Trucks 49-DeSoto Club Coupe (Motor Out But Rblt, New Headlnr In) 50-Plymouth Business Coupe (New W/W/Whites, Good Chrom, OK Paint) Fire Trucks Beer/Pop Trucks 50-Dodge Wayfarer 2Dr Sdn (Stk Eng/Trans, 70% Ready For Paint, Smooth Seams) Mail Trucks Ice Cream Trucks 51-Plymouth Concord 2Dr Sdn (W/Int Kit Encl Headlnr) Animal Control Fuel Delivery 52-Dodge Station Wagon 4Dr (Older Restoration) Forestry Trucks Tankers Restorable 41-Dodge Box Van (Ex Langendorf Bread) (Int Redone, Eng Knocks) 46-Dodge 1 Ton P/U Short Bed Org Paint 47-Dodge Screen Side P/U (All Apart, Less 1 Dr) Service Other 48-Dodge Suicide 4Dr (Set Up For Chev S/B, Ford 9", Older Re-Done Int) Taxi’s Business Coupe’s 48-Dodge Suicide 4Dr (Stock, Runs But Had Eng Fire) Armored Cars Panel Side 48-Chrysler Winsor Highlander 4Dr (Visor, Spotlight, Fair Int, 1 Stuck Valve) 49-Dodge Roadster Conv. (Rough But Most There) Tow Trucks Sedan Delivery 50-Plymouth Business Coupe (W/O Rear Window And Eng/Trans Needs Floor) Ambulance Buses 52-Dodge Short Bed P/U (Deluxe 3 Window Cab) (W/O Eng/Trans) Hearse/Flower Cars 53-Dodge Long Bed P/U (Partial Restored Eng/Trans) Airporters Parts Cars 46-Dodge P/U Rough (W/O Eng/Trans, Rear Axle & Tail Gate) Flat Head 6 Cylinder Parts 46-Plymouth 4Dr (W/O Steering Box, Stuck Eng, Good Grill) Street Rod conversion left overs 48-Chrysler 4Dr (W/O Grill And Driver Side Rear Fender, Good Glass) 49-Plymouth Club Coupe (W/O Eng/Trans And Grill, Needs Floor, Good Glass) Speed Equipment/Dual Carbs & Exhaust/Heads 50-Plymouth Club Coupe (W/O Eng/Trans, Good Grill, Needs Floor) Overdrives 50-Plymouth Club Coupe (Rolling Chassi Only) N.O.S. -
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 ......................................................................................................................................... -
TRANSIT the Newsletter Of
TRANSIT The Newsletter of 05 January 2009 Hubble caught Saturn with the edge-on rings in 1996. Image courtesy Eric Karkoschka (UoA) Front Page Image - Saturn, like the Earth, is tilted on its axis compared to the plane of its orbit, being off vertical by 26.7 degrees. Saturn’s rings are aligned with its equator so that means that roughly twice every orbit of Saturn we on Earth see the rings edge on. We pass through the ring plane in September 2009 but at that time Saturn is on the other side of the Sun, so now is the best time to view Saturn in Leo with the almost disappeared rings when they are inclined at 0.8 degrees to our line of sight. The next ring plane crossing is March 2025 Last meeting : 12 December 2008. “The Large Hadron Collider” by Dr Peter Edwards of Durham University. Dr Edwards proved he was a skilled public communicator when he initially launched into a short history of particle physics – we all understood what he was talking about! After then explaining what the LHC was actually looking for and how their massive detectors work he explained the problems caused by the unfortunate accident when firing up the LHC for the first time. The prognosis for future collisions seems to have a varying date but perhaps the 2010 date is the most likely. We wish Dr Edwards and his LHC colleagues the best of luck in achieving an early target date. Next meeting : 09 January 2009 – Members night. The meeting will start with the Society 2009 AGM and follow on with short talks presented by members of the Society. -
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.