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The Desert Sky Observer
Desert Sky Observer Volume 32 Antelope Valley Astronomy Club Newsletter February 2012 Up-Coming Events February 10: Club Meeting* February 11: Moon Walk @ Prime Desert Woodlands February 13: Executive Board Meeting @ Don’s house February 18: Telescope Night and Star Party @ Devil's Punchbowl * Monthly meetings are held at the S.A.G.E. Planetarium on the Cactus School campus in Palmdale, the second Friday of each month. The meeting location is at the northeast corner of Avenue R and 20th Street East. Meetings start at 7 p.m. and are open to the public. Please note that food and drink are not allowed in the planetarium President Don Bryden Well I gave a star party and no one showed up! Not that I can blame them – it was raining and windy and cold – it even hailed! Still I dragged out the scope and got it ready to go. Briefly, between the clouds I looked at Jupiter and it was quite a treat. The Galilean moons were all tight to the planet either coming from just in front or behind. It gave a bejeweled look like a large ruby surrounded by four small diamonds. Even with the winds and clouds the sky was surprisingly steady and I went as high as 260x with ease, exposing the shadow of Europa transiting the planet. But soon more clouds came and inside we had a nice fire so I put the Artist's rendering DVD “400 Years of the Telescope” on and settled in for the night. My daughter had a few friends over after a skating party that afternoon and later when I went out for one more look they came out to see what was up. -
August 10Th 2019 August 2019 7:00Pm at the Herrett Center for Arts & Science College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting MVAS President’s Message August 2019 Saturday, August 10th 2019 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. Colleagues, Public Star Party follows at the I hope you found the third week of July exhilarating. The 50th Anniversary of the first Centennial Observatory moon landing was the common theme. I capped my observance by watching the C- SPAN replay of the CBS broadcast. It was not only exciting to watch the landing, but Club Officers to listen to Walter Cronkite and Wally Schirra discuss what Neil Armstrong and Buzz Robert Mayer, President Aldrin was relaying back to us. It was fascinating to hear what we have either accepted or rejected for years come across as something brand new. Hearing [email protected] Michael Collins break in from his orbit above in the command module also reminded me of the major role he played and yet others in the past have often overlooked – Gary Leavitt, Vice President fortunately, he is now receiving the respect he deserves. If you didn’t catch that, [email protected] then hopefully you caught some other commemoration, such as Turner Classic Movies showing For All Mankind, a spellbinding documentary of what it was like for Dr. Jay Hartwell, Secretary all of the Apollo astronauts who made it to the moon. Jim Tubbs, Treasurer / ALCOR For me, these moments of commemoration made reading the moon landing’s [email protected] anniversary issue from the Association of Lunar and Planetary Observers (ALPO) 208-404-2999 come to life as they wrote about the features these astronauts were examining – including the little craters named after the three astronauts. -
Filter Performance Comparisons for Some Common Nebulae
Filter Performance Comparisons For Some Common Nebulae By Dave Knisely Light Pollution and various “nebula” filters have been around since the late 1970’s, and amateurs have been using them ever since to bring out detail (and even some objects) which were difficult to impossible to see before in modest apertures. When I started using them in the early 1980’s, specific information about which filter might work on a given object (or even whether certain filters were useful at all) was often hard to come by. Even those accounts that were available often had incomplete or inaccurate information. Getting some observational experience with the Lumicon line of filters helped, but there were still some unanswered questions. I wondered how the various filters would rank on- average against each other for a large number of objects, and whether there was a “best overall” filter. In particular, I also wondered if the much-maligned H-Beta filter was useful on more objects than the two or three targets most often mentioned in publications. In the summer of 1999, I decided to begin some more comprehensive observations to try and answer these questions and determine how to best use these filters overall. I formulated a basic survey covering a moderate number of emission and planetary nebulae to obtain some statistics on filter performance to try to address the following questions: 1. How do the various filter types compare as to what (on average) they show on a given nebula? 2. Is there one overall “best” nebula filter which will work on the largest number of objects? 3. -
The Young Stellar Population of IC 1613 III
A&A 551, A74 (2013) Astronomy DOI: 10.1051/0004-6361/201219977 & c ESO 2013 Astrophysics The young stellar population of IC 1613 III. New O-type stars unveiled by GTC-OSIRIS,, M. Garcia1,2 and A. Herrero1,2 1 Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, 38200 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, Avda. Astrofísico Francisco Sánchez, s/n, 38071 La Laguna, Tenerife, Spain Received 9 July 2012 / Accepted 16 November 2012 ABSTRACT Context. Very low-metallicity massive stars are key to understanding the reionization epoch. Radiation-driven winds, chief agents in the evolution of massive stars, are consequently an important ingredient in our models of the early-Universe. Recent findings hint that the winds of massive stars with poorer metallicity than the SMC may be stronger than predicted by theory. Besides calling the paradigm of radiation-driven winds into question, this result would affect the calculated ionizing radiation and mechanical feedback of massive stars, as well as the role these objects play at different stages of the Universe. Aims. The field needs a systematic study of the winds of a large sample of very metal-poor massive stars. The sampling of spectral types is particularly poor in the very early types. This paper’s goal is to increase the list of known O-type stars in the dwarf irregular galaxy IC 1613, whose metallicity is lower than the SMC’s roughly by a factor 2. Methods. Using the reddening-free Q pseudo-colour, evolutionary masses, and GALEX photometry, we built a list of very likely O-type stars. -
How to Make $1000 with Your Telescope! – 4 Stargazers' Diary
Fort Worth Astronomical Society (Est. 1949) February 2010 : Astronomical League Member Club Calendar – 2 Opportunities & The Sky this Month – 3 How to Make $1000 with your Telescope! – 4 Astronaut Sally Ride to speak at UTA – 4 Aurgia the Charioteer – 5 Stargazers’ Diary – 6 Bode’s Galaxy by Steve Tuttle 1 February 2010 Sunday Monday Tuesday Wednesday Thursday Friday Saturday 1 2 3 4 5 6 Algol at Minima Last Qtr Moon Æ 5:48 am 11:07 pm Top ten binocular deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2244, NGC 2264, NGC 2301, NGC 2360 Top ten deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2261, NGC 2362, NGC 2392, NGC 2403 7 8 9 10 11 12 13 Algol at Minima Morning sports a Moon at Apogee New Moon Æ super thin crescent (252,612 miles) 8:51 am 7:56 pm Moon 8:00 pm 3RF Star Party Make use of the New Moon Weekend for . better viewing at the Dark Sky Site See Notes Below New Moon New Moon Weekend Weekend 14 15 16 17 18 19 20 Presidents Day 3RF Star Party Valentine’s Day FWAS Traveler’s Guide Meeting to the Planets UTA’s Maverick Clyde Tombaugh Ranger 8 returns Normal Room premiers on Speakers Series discovered Pluto photographs and NatGeo 7pm Sally Ride “Fat Tuesday” Ash Wednesday 80 years ago. impacts Moon. 21 22 23 24 25 26 27 Algol at Minima First Qtr Moon Moon at Perigee Å (222,345 miles) 6:42 pm 12:52 am 4 pm {Low in the NW) Algol at Minima Æ 9:43 pm Challenge binary star for month: 15 Lyncis (Lynx) Challenge deep-sky object for month: IC 443 (Gemini) Notable carbon star for month: BL Orionis (Orion) 28 Notes: Full Moon Look for a very thin waning crescent moon perched just above and slightly right of tiny Mercury on the morning of 10:38 pm Feb. -
Feb BACK BAY 2019
Feb BACK BAY 2019 The official newsletter of the Back Bay Amateur Astronomers CONTENTS COMING UP Gamma Burst 2 Feb 7 BBAA Meeting Eclipse Collage 3 7:30-9PM TCC, Virginia Beach NSN Article 6 Heart Nebula 7 Feb 8 Silent Sky Club meeting 10 10-11PM Little Theatre of VB Winter DSOs 11 Contact info 16 Feb 8 Cornwatch Photo by Chuck Jagow Canon 60Da, various exposures, iOptron mount with an Orion 80ED Calendar 17 dusk-dawn The best 9 out of 3465 images taken from about 10:00 PM on the 20th Cornland Park through 2:20 AM on the 21st. Unprocessed images (only cropped). Feb 14 Garden Stars 7-8:30PM LOOKING UP! a message from the president Norfolk Botanical Gardens This month’s most talked about astronomy event has to be the total lunar Feb 16 Saturday Sun-day eclipse. The BBAA participated by supporting the Watch Party at the 10AM-1PM Chesapeake Planetarium. Anyone in attendance will tell you it was COLD, but Elizabeth River Park manageable if you wore layers, utilized the planetarium where Dr. Robert Hitt seemed to have the thermostat set to 100 degrees, and drank copious amounts Feb 23 Skywatch of the hot coffee that Kent Blackwell brewed in the back office. 6PM-10PM The event had a huge following on Facebook but with the cold Northwest River Park temperatures, we weren’t sure how many would come out. By Kent’s estimate there were between 100–200 people in attendance. Many club members set up telescopes, as well as a few members of the public too. -
Report of Contributions
Mapping the X-ray Sky with SRG: First Results from eROSITA and ART-XC Report of Contributions https://events.mpe.mpg.de/e/SRG2020 Mapping the X- … / Report of Contributions eROSITA discovery of a new AGN … Contribution ID : 4 Type : Oral Presentation eROSITA discovery of a new AGN state in 1H0707-495 Tuesday, 17 March 2020 17:45 (15) One of the most prominent AGNs, the ultrasoft Narrow-Line Seyfert 1 Galaxy 1H0707-495, has been observed with eROSITA as one of the first CAL/PV observations on October 13, 2019 for about 60.000 seconds. 1H 0707-495 is a highly variable AGN, with a complex, steep X-ray spectrum, which has been the subject of intense study with XMM-Newton in the past. 1H0707-495 entered an historical low hard flux state, first detected with eROSITA, never seen before in the 20 years of XMM-Newton observations. In addition ultra-soft emission with a variability factor of about 100 has been detected for the first time in the eROSITA light curves. We discuss fast spectral transitions between the cool and a hot phase of the accretion flow in the very strong GR regime as a physical model for 1H0707-495, and provide tests on previously discussed models. Presenter status Senior eROSITA consortium member Primary author(s) : Prof. BOLLER, Thomas (MPE); Prof. NANDRA, Kirpal (MPE Garching); Dr LIU, Teng (MPE Garching); MERLONI, Andrea; Dr DAUSER, Thomas (FAU Nürnberg); Dr RAU, Arne (MPE Garching); Dr BUCHNER, Johannes (MPE); Dr FREYBERG, Michael (MPE) Presenter(s) : Prof. BOLLER, Thomas (MPE) Session Classification : AGN physics, variability, clustering October 3, 2021 Page 1 Mapping the X- … / Report of Contributions X-ray emission from warm-hot int … Contribution ID : 9 Type : Poster X-ray emission from warm-hot intergalactic medium: the role of resonantly scattered cosmic X-ray background We revisit calculations of the X-ray emission from warm-hot intergalactic medium (WHIM) with particular focus on contribution from the resonantly scattered cosmic X-ray background (CXB). -
Astronomy Magazine Special Issue
γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006. -
February 14, 2015 7:00Pm at the Herrett Center for Arts & Science Colleagues, College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, February 14, 2015 7:00pm at the Herrett Center for Arts & Science Colleagues, College of Southern Idaho. Public Star Party Follows at the It’s that time of year when obstacles appear in the sky. In particular, this year is Centennial Obs. loaded with fog. It got in the way of letting us see the dance of the Jovian moons late last month, and it’s hindered our views of other unique shows. Still, members Club Officers reported finding enough of a clear sky to let us see Comet Lovejoy, and some great photos by members are popping up on the Facebook page. Robert Mayer, President This month, however, is a great opportunity to see the benefit of something [email protected] getting in the way. Our own Chris Anderson of the Herrett Center has been using 208-312-1203 the Centennial Observatory’s scope to do work on occultation’s, particularly with asteroids. This month’s MVAS meeting on Feb. 14th will give him the stage to Terry Wofford, Vice President show us just how this all works. [email protected] The following weekend may also be the time the weather allows us to resume 208-308-1821 MVAS-only star parties. Feb. 21 is a great window for a possible star party; we’ll announce the location if the weather permits. However, if we don’t get that Gary Leavitt, Secretary window, we’ll fall back on what has become a MVAS tradition: Planetarium night [email protected] at the Herrett Center. -
The Extragalactic Distance Scale
The Extragalactic Distance Scale Published in "Stellar astrophysics for the local group" : VIII Canary Islands Winter School of Astrophysics. Edited by A. Aparicio, A. Herrero, and F. Sanchez. Cambridge ; New York : Cambridge University Press, 1998 Calibration of the Extragalactic Distance Scale By BARRY F. MADORE1, WENDY L. FREEDMAN2 1NASA/IPAC Extragalactic Database, Infrared Processing & Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA 2Observatories, Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena CA 91101, USA The calibration and use of Cepheids as primary distance indicators is reviewed in the context of the extragalactic distance scale. Comparison is made with the independently calibrated Population II distance scale and found to be consistent at the 10% level. The combined use of ground-based facilities and the Hubble Space Telescope now allow for the application of the Cepheid Period-Luminosity relation out to distances in excess of 20 Mpc. Calibration of secondary distance indicators and the direct determination of distances to galaxies in the field as well as in the Virgo and Fornax clusters allows for multiple paths to the determination of the absolute rate of the expansion of the Universe parameterized by the Hubble constant. At this point in the reduction and analysis of Key Project galaxies H0 = 72km/ sec/Mpc ± 2 (random) ± 12 [systematic]. Table of Contents INTRODUCTION TO THE LECTURES CEPHEIDS BRIEF SUMMARY OF THE OBSERVED PROPERTIES OF CEPHEID -
ASTRONOMY and ASTROPHYSICS the Elliptical Galaxy Formerly Known As the Local Group: Merging the Globular Cluster Systems
Astron. Astrophys. 358, 471–480 (2000) ASTRONOMY AND ASTROPHYSICS The elliptical galaxy formerly known as the Local Group: merging the globular cluster systems Duncan A. Forbes1,2, Karen L. Masters1, Dante Minniti3, and Pauline Barmby4 1 University of Birmingham, School of Physics and Astronomy, Edgbaston, Birmingham B15 2TT, UK 2 Swinburne University of Technology, Astrophysics and Supercomputing, Hawthorn, Victoria 3122, Australia 3 P. Universidad Catolica,´ Departamento de Astronom´ıa y Astrof´ısica, Casilla 104, Santiago 22, Chile 4 Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA Received 5 November 1999 / Accepted 27 January 2000 Abstract. Prompted by a new catalogue of M31 globular clus- al. 1995; Minniti et al. 1996). Furthermore Hubble Space Tele- ters, we have collected together individual metallicity values for scope studies of merging disk galaxies reveal evidence for the globular clusters in the Local Group. Although we briefly de- GC systems of the progenitor galaxies (e.g. Forbes & Hau 1999; scribe the globular cluster systems of the individual Local Group Whitmore et al. 1999). Thus GCs should survive the merger of galaxies, the main thrust of our paper is to examine the collec- their parent galaxies, and will form a new GC system around tive properties. In this way we are simulating the dissipationless the newly formed elliptical galaxy. merger of the Local Group, into presumably an elliptical galaxy. The globular clusters of the Local Group are the best studied Such a merger is dominated by the Milky Way and M31, which and offer a unique opportunity to examine their collective prop- appear to be fairly typical examples of globular cluster systems erties (reviews of LG star clusters can be found in Brodie 1993 of spiral galaxies. -
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).