The Proud Indian by Magda Streicher [email protected]
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Hubble Sees an Actively Star-Forming Galaxy, NGC 7090 17 September 2012
Hubble sees an actively star-forming galaxy, NGC 7090 17 September 2012 galaxy. Second, we observe dust lanes, depicted as dark regions inside the disc of the galaxy. In NGC 7090, these regions are mostly located in lower half of the galaxy, showing an intricate filamentary structure. Looking from the outside in through the whole disc, the light emitted from the bright center of the galaxy is absorbed by the dust, silhouetting the dusty regions against the bright light in the background. Dust in our galaxy, the Milky Way, has been one of the worst enemies of observational astronomers for decades. But this does not mean that these regions are only blind spots in the sky. At near-infrared wavelengths—slightly longer wavelengths than visible light—this dust is largely transparent and astronomers are able to study what is really behind it. At still longer wavelengths, the realm of radio astronomy, the dust itself can actually be observed, Credit: ESA/Hubble & NASA letting astronomers study the structure and properties of dust clouds and their relationship with star formation. (Phys.org)—This image portrays a beautiful view of Lying in the southern constellation of Indus (The the galaxy NGC 7090, as seen by the NASA/ESA Indian), NGC 7090 is located about thirty million Hubble Space Telescope. The galaxy is viewed light-years from the Sun. Astronomer John edge-on from the Earth, meaning we cannot easily Herschel first observed this galaxy on October 4, see the spiral arms, which are full of young, hot 1834. stars. The image was taken using the Wide Field Channel However, a side-on view shows the galaxy's disc of the Advanced Camera for Surveys aboard the and the bulging central core, where typically a Hubble Space Telescope and combines orange large group of cool old stars are packed in a light (colored blue here), infrared (colored red) and compact, spheroidal region. -
100 Closest Stars Designation R.A
100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79, -
Ioptron AZ Mount Pro Altazimuth Mount Instruction
® iOptron® AZ Mount ProTM Altazimuth Mount Instruction Manual Product #8900, #8903 and #8920 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. 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 observing. 2 Table of Content Table of Content ......................................................................................................................................... 3 1. AZ Mount ProTM Altazimuth Mount Overview...................................................................................... 5 2. AZ Mount ProTM Mount Assembly ........................................................................................................ 6 2.1. Parts List .......................................................................................................................................... 6 2.2. Identification of Parts ....................................................................................................................... 7 2.3. Go2Nova® 8407 Hand Controller .................................................................................................... 8 2.3.1. Key Description ....................................................................................................................... -
A Joint ESA-CONSTELLATION Workshop on the Formation of Brown Dwarfs
-ESA- Space Science Faculty Courtesy NASA/JPL-Caltech CONSTELLATION is a European Commission Sixth Framework Marie Curie Research Training Network (contract number MRTN-CT-2006-035890) A joint ESA-CONSTELLATION workshop on the formation of brown dwarfs Contact info: [email protected]! www.rssd.esa.int/BD2009 Gemini Observatory/AURA WORKSHOP Recipes for making brownies: theory vs. observations Scientific Rationale: The origin of Brown Dwarfs (BDs) is an important component of the theory of star formation. Recent ground based and satellite observations are revealing an increasing number of BDs; however, their origin remains somewhat mysterious as their mass is 2 orders of magnitude below the average Jeans mass in star-forming clouds. Explaining why they are so common thus requires detailed understanding of the fragmentation processes during star formation, as well as exploring other formation scenarios. This workshop will focus on recent theoretical and observational progresses in the field of BD formation as well as explore current and future perspectives. Our purpose is to bring together the leading experts working in this field, foster new collabora- tions and, in particular, promote extended interactions among young PhD/post-doc researchers. SOC: L. Spezzi (chair, ESTEC) B. Mer´ın(ESAC) D. Stamatellos (University of Cardiff) V. Konyves (CEA/Saclay,SAp) C. Alves de Oliveira (LAOG, Grenoble) LOC: L. Spezzi (co-chair) J. Walcher (co-chair) G. Beccari Program: 9 September 2009 08:30 - 10:00 Registration + Coffee 10:00 - 10:15 Opening 10:15 - 11:00 I. Bonnell, BD formation, an introductory review Session 1: Observations of BDs Chairman: E. Mouraux 11:00 - 11:30 K. -
FIXED STARS a SOLAR WRITER REPORT for Churchill Winston WRITTEN by DIANA K ROSENBERG Page 2
FIXED STARS A SOLAR WRITER REPORT for Churchill Winston WRITTEN BY DIANA K ROSENBERG Page 2 Prepared by Cafe Astrology cafeastrology.com Page 23 Churchill Winston Natal Chart Nov 30 1874 1:30 am GMT +0:00 Blenhein Castle 51°N48' 001°W22' 29°‚ 53' Tropical ƒ Placidus 02' 23° „ Ý 06° 46' Á ¿ 21° 15° Ý 06' „ 25' 23° 13' Œ À ¶29° Œ 28° … „ Ü É Ü 06° 36' 26' 25° 43' Œ 51'Ü áá Œ 29° ’ 29° “ àà … ‘ à ‹ – 55' á á 55' á †32' 16° 34' ¼ † 23° 51'Œ 23° ½ † 06' 25° “ ’ † Ê ’ ‹ 43' 35' 35' 06° ‡ Š 17° 43' Œ 09° º ˆ 01' 01' 07° ˆ ‰ ¾ 23° 22° 08° 02' ‡ ¸ Š 46' » Ï 06° 29°ˆ 53' ‰ Page 234 Astrological Summary Chart Point Positions: Churchill Winston Planet Sign Position House Comment The Moon Leo 29°Le36' 11th The Sun Sagittarius 7°Sg43' 3rd Mercury Scorpio 17°Sc35' 2nd Venus Sagittarius 22°Sg01' 3rd Mars Libra 16°Li32' 1st Jupiter Libra 23°Li34' 1st Saturn Aquarius 9°Aq35' 5th Uranus Leo 15°Le13' 11th Neptune Aries 28°Ar26' 8th Pluto Taurus 21°Ta25' 8th The North Node Aries 25°Ar51' 8th The South Node Libra 25°Li51' 2nd The Ascendant Virgo 29°Vi55' 1st The Midheaven Gemini 29°Ge53' 10th The Part of Fortune Capricorn 8°Cp01' 4th Chart Point Aspects Planet Aspect Planet Orb App/Sep The Moon Semisquare Mars 1°56' Applying The Moon Trine Neptune 1°10' Separating The Moon Trine The North Node 3°45' Separating The Moon Sextile The Midheaven 0°17' Applying The Sun Semisquare Jupiter 0°50' Applying The Sun Sextile Saturn 1°52' Applying The Sun Trine Uranus 7°30' Applying Mercury Square Uranus 2°21' Separating Mercury Opposition Pluto 3°49' Applying Venus Sextile -
Science Highlights
Science highlights First millimetre light for A project science team is now using the upgraded Australia Telescope Compact Array in its 3-mm observing mode, looking at a variety of astronomical First light at millimetre wavelengths for the sources and investigating the performance upgraded Australia Telescope Compact of the system. Some of the first Array occurred in November 2000, with a observations were of the SiO maser 3-mm observation of silicon monoxide emission from the circumstellar envelopes maser emission from the Orion nebula. of the evolved stars VX Sgr, R Dor, and R On Thursday 30 November 2000, three Aqr. The strong SiO emission from these years of designing, building, and testing stars can be detected easily in a single for the Narrabri and Sydney engineering 10-second integration time. The team also groups came to a climax at the Compact observed HCO+ absorption against the Array when two of the six dishes were fitted nuclear continuum source in the radio with the new 3-mm receiving systems and galaxy Centaurus A (Figure 9). Initial trained on a star-forming region within the results are available on the Web at Orion nebula containing silicon monoxide http://www.atnf.csiro.au/mnrf/3mm_details.html. (SiO) masers. At 11.45 p.m. the telescope captured its first cosmic millimetre-wave photons, achieving “first light”. Figure 8 shows the cross-power spectrum resulting from these first observations, at a frequency of 86.243 GHz. The millimetre photons from this source are produced by excited SiO molecules embedded within the star-forming clouds. -
Wavelength (Angstroms) Wavelength (Angstroms) 7.0 MBG03537-1351 -1
-15 -1 -2 -1 Fλ x 10 erg s cm A 1.0 3.0 5.0 7.0 4900 5100 5300 wavelength (angstroms) MBG22342-2228 a) -15 -1 -2 -1 Fλ x 10 erg s cm A 1.0 3.0 5.0 7.0 6400 6600 6800 7000 wavelength (angstroms) MBG22342-2228 b) -15 -1 -2 -1 Fλ x 10 erg s cm A 1.0 3.0 5.0 7.0 MBG03537-1351 6400 6600 6800 7000 wavelength (angstroms) Table 2. Spectroscopic characteristics in the red. − Name Vr [OI] [NII] [SII] [SII] log IHα FWHM EW MBG 63006583 67166730 Hα Hα km s−1 (ergs cm−2 s−1) kms−1 (A)˚ 02384–2112 4712 · · · 0.42 ··· ··· 13.39 141 20 03196–1939 4076 · · · 0.27 0.20 0.16 13.09 32 49 03288–1448 9234 · · · 0.34 0.13 0.12 13.58 99 31 03325–1002 9596 0.28 0.40 0.10 0.11 12.70 148 65 03537–1351 8891 · · · 0.84 ··· ··· 13.42 264 37 23362–0448 5990 · · · 0.43 0.11 0.11 13.39 117 17 arXiv:astro-ph/9612174v1 18 Dec 1996 1 0.60 0.50 m V/V 0.40 0.30 13.5 14.5 15.5 BLim Table 3. Spectroscopic characteristics in the blue. − Name [OIII] [OIII] log IHβ FWHM FWHM EW MBG 4959 5007 Hβ [OIII]λ5007 Hβ (ergs cm−2 s−1) kms−1 km s−1 (A)˚ 01325–1806 · · · 0.46 13.9 112 151 6 01486–0956 · · · 0.41: 14.2: < 296 < 354 3 01556–2002 · · · 2.53: 14.4: < 314 < 348 5 02027–2339 1.36 3.78 14.7 187 < 438 16 02028–0641 · · · 0.3 13.6 370 218 9 02399–2420 0.69: 1.69: 14.0: < 339 < 294 8 02384–2112 · · · 1.57 14.4 < 401 < 425 3 03325–1002 0.11 0.32 13.6 154 72 10 03353–2439 · · · 0.42 13.6 171 < 480 9 03424–2019 0.16 0.40 14.9 < 419 < 384 8 04002–1811 0.94 2.81 14.0: 230 306 4 21481–1330 0.33: 0.69 13.8 300 187 10 21300–1601 0.15 0.46 13.9 < 413 < 455 14 22342–2228 2.17 5.75 14.1 990 218 4 23318–1156 0.80 2.18 14.1 112 < 413 5 23383–1921 1.09 3.49 13.4: 278 < 467 23 23382–2047 0.18 0.69 13.8 311 271 7 arXiv:astro-ph/9612174v1 18 Dec 1996 Uncertainties higher than 20% are marked by a colon. -
Further Definition of the Mass-Metallicity Relation In
Further Definition of the Mass-Metallicity Relation in Globular Cluster Systems Around Brightest Cluster Galaxies Robert Cockcroft Department of Physics and Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1, Canada [email protected] William E. Harris Department of Physics and Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1, Canada [email protected] Elizabeth M. H. Wehner Utrecht University, PO Box 80125, 3508 TC Utrecht, The Netherlands [email protected] Bradley C. Whitmore Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218 [email protected] and Barry Rothberg arXiv:0906.2008v1 [astro-ph.CO] 10 Jun 2009 Naval Research Laboratory, Code 7211, 4555 Overlook Ave SW, Washington D.C. 20375 [email protected] ABSTRACT We combine the globular cluster data for fifteen Brightest Cluster Galaxies and use this material to trace the mass-metallicity relations (MMR) in their glob- ular cluster systems (GCSs). This work extends previous studies which correlate the properties of the MMR with those of the host galaxy. Our combined data sets –2– show a mean trend for the metal-poor (MP) subpopulation which corresponds to a scaling of heavy-element abundance with cluster mass Z ∼ M0.30±0.05. No trend is seen for the metal-rich (MR) subpopulation which has a scaling relation that is consistent with zero. We also find that the scaling exponent is independent of the GCS specific frequency and host galaxy luminosity, except perhaps for dwarf galaxies. We present new photometry in (g’,i’) obtained with Gemini/GMOS for the globular cluster populations around the southern giant ellipticals NGC 5193 and IC 4329. -
A Transiting, Terrestrial Planet in a Triple M Dwarf System at 6.9 Parsecs
Draft version June 24, 2019 Typeset using LATEX twocolumn style in AASTeX61 THREE RED SUNS IN THE SKY: A TRANSITING, TERRESTRIAL PLANET IN A TRIPLE M DWARF SYSTEM AT 6.9 PARSECS Jennifer G. Winters,1 Amber A. Medina,1 Jonathan M. Irwin,1 David Charbonneau,1 Nicola Astudillo-Defru,2 Elliott P. Horch,3 Jason D. Eastman,1 Eliot Halley Vrijmoet,4 Todd J. Henry,5 Hannah Diamond-Lowe,1 Elaine Winston,1 Xavier Bonfils,6 George R. Ricker,7 Roland Vanderspek,7 David W. Latham,1 Sara Seager,8, 9, 10 Joshua N. Winn,11 Jon M. Jenkins,12 Stephane´ Udry,13 Joseph D. Twicken,14, 12 Johanna K. Teske,15, 16 Peter Tenenbaum,14, 12 Francesco Pepe,13 Felipe Murgas,17, 18 Philip S. Muirhead,19 Jessica Mink,1 Christophe Lovis,13 Alan M. Levine,7 Sebastien´ Lepine´ ,4 Wei-Chun Jao,4 Christopher E. Henze,12 Gabor´ Furesz,´ 7 Thierry Forveille,6 Pedro Figueira,20, 21 Gilbert A. Esquerdo,1 Courtney D. Dressing,22 Rodrigo F. D´ıaz,23, 24 Xavier Delfosse,6 Chris J. Burke,7 Franc¸ois Bouchy,13 Perry Berlind,1 and Jose-Manuel Almenara6 1Center for Astrophysics j Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA 2Departamento de Matem´atica y F´ısica Aplicadas, Universidad Cat´olica de la Sant´ısimaConcepci´on,Alonso de Rivera 2850, Concepci´on, Chile 3Department of Physics, Southern Connecticut State University, 501 Crescent Street, New Haven, CT 06515, USA 4Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30302-4106, USA 5RECONS Institute, Chambersburg, Pennsylvania, 17201, USA 6Universit´eGrenoble Alpes, CNRS, IPAG, F-38000 -
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C. -
X-Ray Luminosities for a Magnitude-Limited Sample of Early-Type Galaxies from the ROSAT All-Sky Survey
Mon. Not. R. Astron. Soc. 302, 209±221 (1999) X-ray luminosities for a magnitude-limited sample of early-type galaxies from the ROSAT All-Sky Survey J. Beuing,1* S. DoÈbereiner,2 H. BoÈhringer2 and R. Bender1 1UniversitaÈts-Sternwarte MuÈnchen, Scheinerstrasse 1, D-81679 MuÈnchen, Germany 2Max-Planck-Institut fuÈr Extraterrestrische Physik, D-85740 Garching bei MuÈnchen, Germany Accepted 1998 August 3. Received 1998 June 1; in original form 1997 December 30 Downloaded from https://academic.oup.com/mnras/article/302/2/209/968033 by guest on 30 September 2021 ABSTRACT For a magnitude-limited optical sample (BT # 13:5 mag) of early-type galaxies, we have derived X-ray luminosities from the ROSATAll-Sky Survey. The results are 101 detections and 192 useful upper limits in the range from 1036 to 1044 erg s1. For most of the galaxies no X-ray data have been available until now. On the basis of this sample with its full sky coverage, we ®nd no galaxy with an unusually low ¯ux from discrete emitters. Below log LB < 9:2L( the X-ray emission is compatible with being entirely due to discrete sources. Above log LB < 11:2L( no galaxy with only discrete emission is found. We further con®rm earlier ®ndings that Lx is strongly correlated with LB. Over the entire data range the slope is found to be 2:23 60:12. We also ®nd a luminosity dependence of this correlation. Below 1 log Lx 40:5 erg s it is consistent with a slope of 1, as expected from discrete emission. -
Seeing the Light: the Art and Science of Astronomy
Chapter 1 Seeing the Light: The Art and Science of Astronomy In This Chapter ▶ Understanding the observational nature of astronomy ▶ Focusing on astronomy’s language of light ▶ Weighing in on gravity ▶ Recognizing the movements of objects in space tep outside on a clear night and look at the sky. If you’re a city dweller Sor live in a cramped suburb, you see dozens, maybe hundreds, of twin- kling stars. Depending on the time of the month, you may also see a full Moon and up to five of the eight planets that revolve around the Sun. A shooting star or “meteor” may appear overhead. What you actually see is the flash of light from a tiny piece of comet dust streaking through the upper atmosphere. Another pinpoint of light moves slowly and steadily across the sky. Is it a space satellite, such as the Hubble Space Telescope, or just a high-altitude airliner? If you have a pair of binoculars, you may be able to see the difference. Most air- liners have running lights, and their shapes may be perceptible. If you liveCOPYRIGHTED in the country — on the seashore MATERIAL away from resorts and develop- ments, on the plains, or in the mountains far from any floodlit ski slope — you can see thousands of stars. The Milky Way appears as a beautiful pearly swath across the heavens. What you’re seeing is the cumulative glow from millions of faint stars, individually indistinguishable with the naked eye. At a great observation place, such as Cerro Tololo in the Chilean Andes, you can see even more stars.