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Meeting Program
A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ. -
SAA 100 Club
S.A.A. 100 Observing Club Raleigh Astronomy Club Version 1.2 07-AUG-2005 Introduction Welcome to the S.A.A. 100 Observing Club! This list started on the USENET newsgroup sci.astro.amateur when someone asked about everyone’s favorite, non-Messier objects for medium sized telescopes (8-12”). The members of the group nominated objects and voted for their favorites. The top 100 objects, by number of votes, were collected and ranked into a list that was published. This list is a good next step for someone who has observed all the objects on the Messier list. Since it includes objects in both the Northern and Southern Hemispheres (DEC +72 to -72), the award has two different levels to accommodate those observers who aren't able to travel. The first level, the Silver SAA 100 award requires 88 objects (all visible from North Carolina). The Gold SAA 100 Award requires all 100 objects to be observed. One further note, many of these objects are on other observing lists, especially Patrick Moore's Caldwell list. For convenience, there is a table mapping various SAA100 objects with their Caldwell counterparts. This will facilitate observers who are working or have worked on these lists of objects. We hope you enjoy looking at all the great objects recommended by other avid astronomers! Rules In order to earn the Silver certificate for the program, the applicant must meet the following qualifications: 1. Be a member in good standing of the Raleigh Astronomy Club. 2. Observe 80 Silver observations. 3. Record the time and date of each observation. -
Carina Nebula Pillar Lithograph As the Initial Source of Information to Engage These Are Terms Students May Encounter While Doing Further Research on Star Formation
Carina Nebula Pillar National Aeronautics and Space Administration Carina Nebula Pillar Hubble Captures View of ‘Mystic Mountain’ To mark the 20th anniversary of Hubble’s launch and deployment into Earth orbit, NASA and the Space Telescope Science Institute issued this stunning image. The new photograph is reminiscent of a craggy fantasy mountaintop surrounded by wispy clouds. The image captures the chaotic activity on a three-light-year-tall pillar of gas and dust that is being eaten away by the brilliant light from nearby colossal young stars. Those massive stars are located above the pillar, off the image. Streamers of hot, ionized gas can be seen flowing off the ridges of the structure, and thin veils of gas and dust, illuminated by starlight, float around its towering peaks. Scorching radiation and fast winds (streams of charged particles) from the gigantic young stars in the nebula are shaping and compressing the pillar, causing new stars to form within it. The new stars buried inside the pillar are firing off jets of Close-up view of Carina Nebula Pillar gas that can be seen streaming from towering peaks. This This image reveals long jets of gas shooting in opposite turbulent cosmic pillar lies within a tempestuous stellar directions off the tip of a giant pillar of material. The jets nursery called the Carina Nebula, located 7,500 light-years are a signature of new star birth. The young star cannot away in the southern constellation Carina. be seen because it is buried deep inside the dense pillar. The Carina Nebula is one of the largest and brightest The jets are launched by a swirling disk of gas and dust nebulas in the sky. -
The Milky Way the Milky Way's Neighbourhood
The Milky Way What Is The Milky Way Galaxy? The.Milky.Way.is.the.galaxy.we.live.in..It.contains.the.Sun.and.at.least.one.hundred.billion.other.stars..Some.modern. measurements.suggest.there.may.be.up.to.500.billion.stars.in.the.galaxy..The.Milky.Way.also.contains.more.than.a.billion. solar.masses’.worth.of.free-floating.clouds.of.interstellar.gas.sprinkled.with.dust,.and.several.hundred.star.clusters.that. contain.anywhere.from.a.few.hundred.to.a.few.million.stars.each. What Kind Of Galaxy Is The Milky Way? Figuring.out.the.shape.of.the.Milky.Way.is,.for.us,.somewhat.like.a.fish.trying.to.figure.out.the.shape.of.the.ocean.. Based.on.careful.observations.and.calculations,.though,.it.appears.that.the.Milky.Way.is.a.barred.spiral.galaxy,.probably. classified.as.a.SBb.or.SBc.on.the.Hubble.tuning.fork.diagram. Where Is The Milky Way In Our Universe’! The.Milky.Way.sits.on.the.outskirts.of.the.Virgo.supercluster..(The.centre.of.the.Virgo.cluster,.the.largest.concentrated. collection.of.matter.in.the.supercluster,.is.about.50.million.light-years.away.).In.a.larger.sense,.the.Milky.Way.is.at.the. centre.of.the.observable.universe..This.is.of.course.nothing.special,.since,.on.the.largest.size.scales,.every.point.in.space. is.expanding.away.from.every.other.point;.every.object.in.the.cosmos.is.at.the.centre.of.its.own.observable.universe.. Within The Milky Way Galaxy, Where Is Earth Located’? Earth.orbits.the.Sun,.which.is.situated.in.the.Orion.Arm,.one.of.the.Milky.Way’s.66.spiral.arms..(Even.though.the.spiral. -
An Aboriginal Australian Record of the Great Eruption of Eta Carinae
Accepted in the ‘Journal for Astronomical History & Heritage’, 13(3): in press (November 2010) An Aboriginal Australian Record of the Great Eruption of Eta Carinae Duane W. Hamacher Department of Indigenous Studies, Macquarie University, NSW, 2109, Australia [email protected] David J. Frew Department of Physics & Astronomy, Macquarie University, NSW, 2109, Australia [email protected] Abstract We present evidence that the Boorong Aboriginal people of northwestern Victoria observed the Great Eruption of Eta (η) Carinae in the nineteenth century and incorporated the event into their oral traditions. We identify this star, as well as others not specifically identified by name, using descriptive material presented in the 1858 paper by William Edward Stanbridge in conjunction with early southern star catalogues. This identification of a transient astronomical event supports the assertion that Aboriginal oral traditions are dynamic and evolving, and not static. This is the only definitive indigenous record of η Carinae’s outburst identified in the literature to date. Keywords: Historical Astronomy, Ethnoastronomy, Aboriginal Australians, stars: individual (η Carinae). 1 Introduction Aboriginal Australians had a significant understanding of the night sky (Norris & Hamacher, 2009) and frequently incorporated celestial objects and transient celestial phenomena into their oral traditions, including the sun, moon, stars, planets, the Milky Way and Magellanic Clouds, eclipses, comets, meteors, and impact events. While Australia is home to hundreds of Aboriginal groups, each with a distinct language and culture, few of these groups have been studied in depth for their traditional knowledge of the night sky. We refer the interested reader to the following reviews on Australian Aboriginal astronomy: Cairns & Harney (2003), Clarke (1997; 2007/2008), Fredrick (2008), Haynes (1992; 2000), Haynes et al. -
Esoshop Catalogue
ESOshop Catalogue www.eso.org/esoshop Annual Report 2 Annual Report Annual Report Content 4 Annual Report 33 Mounted Images 6 Apparel 84 Postcards 11 Books 91 Posters 18 Brochures 96 Stickers 20 Calendar 99 Hubbleshop Catalogue 22 Media 27 Merchandise 31 Messenger Annual Report 3 Annual Report Annual Report 4 Annual Report Annual Report ESO Annual Report 2018 This report documents the many activities of the European Southern Observatory during 2018. Product ID ar_2018 Price 4 260576 727305 € 5.00 Annual Report 5 Apparel Apparel 6 Apparel Apparel Running Tank Women Running Tank Men ESO Cap If you love running outdoors or indoors, this run- If you love running outdoors or indoors, this run- The official ESO cap is available in navy blue and ning tank is a comfortable and affordable option. ning tank is a comfortable and affordable option. features an embroidered ESO logo on the front. On top, it is branded with a large, easy-to-see On top, it is branded with a large, easy-to-see It has an adjustable strap, measuring 46-60 cm ESO logo and website on the back and a smaller ESO logo and website on the back and a smaller (approx) in circumference, with a diameter of ESO 50th anniversary logo on the front, likely to ESO 50th anniversary logo on the front, likely to 20 cm (approx). raise the appreciation or the curiosity of fellow raise the appreciation or the curiosity of fellow runners. runners. Product ID apparel_0045 Product ID apparel_0015 (M) Product ID apparel_0020 (M) Price Price Price € 8.00 4 260576 720306 € 14.00 4 260576 720047 € 14.00 4 260576 720092 Product ID apparel_0014 (L) Product ID apparel_0019 (L) Price Price € 14.00 4 260576 720030 € 14.00 4 260576 720085 Product ID apparel_0013 (XL) Price € 14.00 4 260576 720023 Apparel 7 Apparel ESO Slim Fit Fleece Jacket ESO Slim Fit Fleece Jacket Men ESO Astronomical T-shirt Women This warm long-sleeve ESO fleece jacket is perfect This warm long-sleeve ESO fleece jacket is perfect This eye-catching nebular T-shirt features stunning for the winter. -
The VISTA Carina Nebula Survey⋆ I: Introduction and Source Catalog⋆⋆
Astronomy & Astrophysics manuscript no. paper-final c ESO 2014 December 2, 2014 The VISTA Carina Nebula Survey⋆ I: Introduction and source catalog⋆⋆ T. Preibisch1, P. Zeidler1,2, T. Ratzka1,3, V. Roccatagliata1, and M.G. Petr-Gotzens4 1 Universitats-Sternwarte¨ Munchen,¨ Ludwig-Maximilians-Universitat,¨ Scheinerstr. 1, 81679 Munchen,¨ Germany e-mail: [email protected] 2 Astronomisches Rechen-Institut, Zentrum fur¨ Astronomie der Universitat¨ Heidelberg, Monchhofstr.¨ 12–14, 69120 Heidelberg, Germany 3 Institute for Physics / IGAM, NAWI Graz, Karl-Franzens-Universitat,¨ Universitatsplatz¨ 5/II, 8010 Graz, Austria 4 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany Received 22 April 2014; accepted 6 October 2014 ABSTRACT Context. The Carina Nebula is one of the most massive and active star-forming regions in our Galaxy and has been studied with numerous multiwavelength observations in the past five years. However, most of these studies were restricted to the inner parts (∼< 1 square-degree) of the nebula, and thus covered only a small fraction of the whole cloud complex. Aims. Our aim was to conduct a near-infrared survey that covers the full spatial extent (∼ 5 square-degrees) of the Carina Nebula complex and is sensitive enough to detect all associated young stars through extinctions of up to AV ≈ 6 mag. Methods. We used the 4m Visible and Infrared Survey Telescope for Astronomy (VISTA) of ESO to map an area of 6.7 square- degrees around the Carina Nebula in the near-infrared J-, H-, Ks-bands. Results. The analysis of our VISTA data revealed 4 840 807 individual near-infrared sources, 3 951 580 of which are detected in at least two bands. -
The VISTA Carina Nebula Survey I
A&A 572, A116 (2014) Astronomy DOI: 10.1051/0004-6361/201424045 & c ESO 2014 Astrophysics The VISTA Carina Nebula Survey I. Introduction and source catalog, T. Preibisch1,P.Zeidler1,2, T. Ratzka1,3, V. Roccatagliata1, and M. G. Petr-Gotzens4 1 Universitäts-Sternwarte München, Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 München, Germany e-mail: [email protected] 2 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12–14, 69120 Heidelberg, Germany 3 Institute for Physics/IGAM, NAWI Graz, Karl-Franzens-Universität, Universitätsplatz 5/II, 8010 Graz, Austria 4 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany Received 22 April 2014 / Accepted 6 October 2014 ABSTRACT Context. The Carina Nebula is one of the most massive and active star-forming regions in our Galaxy and has been studied with numerous multiwavelength observations in the past five years. However, most of these studies were restricted to the inner parts (∼<1 square-degree) of the nebula, and thus covered only a small fraction of the whole cloud complex. Aims. Our aim was to conduct a near-infrared survey that covers the full spatial extent (∼5 square-degrees) of the Carina Nebula complex and is sensitive enough to detect all associated young stars through extinctions of up to AV ≈ 6mag. Methods. We used the 4m Visible and Infrared Survey Telescope for Astronomy (VISTA) of ESO to map an area of 6.7 square- degrees around the Carina Nebula in the near-infrared J-, H-, Ks-bands. Results. The analysis of our VISTA data revealed 4 840 807 individual near-infrared sources, 3 951 580 of which are detected in at least two bands. -
THE SKY TONIGHT Second Brightest Star in the Night Sky, Canopus
DECEMBER HAKIHEA Sailing in an Ocean of Stars HIGHLIGHTS The constellation of Carina is home to the THE SKY TONIGHT second brightest star in the night sky, Canopus. This brilliant beacon of light makes finding the TE ĀHUA O TE RAKI I TĒNEI PŌ constellation a breeze. Canopus has appeared in the mythology of many ancient cultures. Bright Stars This bright giant gets its modern name from For anyone new to the joys of star gazing, the mythological navigator of King Menelaus December heralds a beginner’s dream. Some of Sparta’s ship – some versions of the tale of the night sky’s brightest stars will illuminate suggest that Canopus was the helmsman or your experience. Orion, very much a summer pilot of the ship. constellation in Dunedin, will rise high in our northern night sky accompanied by his hunting Carina was once part of a much larger dogs – the constellations of Canis Major and constellation known as Argo Navis (the ship Argo) Canis Minor. Sirius, the ‘dog star’ impresses – three modern constellations formed this great with its luminosity; the brightest star in our ship in the sky, Carina the keel, Puppis the stern, night skies, it can be found at the head of and Vela the sails. In Greek mythology Argo was Canis Major (greater dog). the ship sailed by Jason and the Argonauts in search of the Golden Fleece. The origins of Argo For Harry Potter fans out there, you can Navis stem from ancient Greek, in the 1760s probably surmise where some of J K Rowling’s Nicolas Louis de Lacaille split the constellation inspiration came from! Orion itself boasts into its modern components. -
The Gaia-ESO Survey: the Present-Day Radial Metallicity Distribution of the Galactic Disc Probed by Pre-Main-Sequence Clusters?,?? L
A&A 601, A70 (2017) Astronomy DOI: 10.1051/0004-6361/201630078 & c ESO 2017 Astrophysics The Gaia-ESO Survey: the present-day radial metallicity distribution of the Galactic disc probed by pre-main-sequence clusters?,?? L. Spina1, S. Randich2, L. Magrini2, R. D. Jeffries3, E. D. Friel4, G. G. Sacco2, E. Pancino2; 5, R. Bonito8; 9, L. Bravi2, E. Franciosini2, A. Klutsch6, D. Montes10, G. Gilmore11, A. Vallenari12, T. Bensby13, A. Bragaglia14, E. Flaccomio8, S. E. Koposov15; 16, A. J. Korn17, A. C. Lanzafame6; 7, R. Smiljanic18, A. Bayo19, G. Carraro20, A. R. Casey11, M. T. Costado21, F. Damiani8, P. Donati14, A. Frasca6, A. Hourihane11, P. Jofré11; 22, J. Lewis11, K. Lind23, L. Monaco24, L. Morbidelli2, L. Prisinzano8, S. G. Sousa25, C. C. Worley11, and S. Zaggia12 (Affiliations can be found after the references) Received 17 November 2016 / Accepted 7 February 2017 ABSTRACT Context. The radial metallicity distribution in the Galactic thin disc represents a crucial constraint for modelling disc formation and evolution. Open star clusters allow us to derive both the radial metallicity distribution and its evolution over time. Aims. In this paper we perform the first investigation of the present-day radial metallicity distribution based on [Fe/H] determinations in late type members of pre-main-sequence clusters. Because of their youth, these clusters are therefore essential for tracing the current interstellar medium metallicity. Methods. We used the products of the Gaia-ESO Survey analysis of 12 young regions (age < 100 Myr), covering Galactocentric distances from 6.67 to 8.70 kpc. For the first time, we derived the metal content of star forming regions farther than 500 pc from the Sun. -
CBI Limits on 31 Ghz Excess Emission in Southern HII Regions
Mon. Not. R. Astron. Soc. 379, 297–307 (2007) doi:10.1111/j.1365-2966.2007.11967.x CBI limits on 31 GHz excess emission in southern H II regions , C. Dickinson,1 2 R. D. Davies,3 L. Bronfman,4 S. Casassus,4 R. J. Davis,3 T. J. Pearson,2 A. C. S. Readhead2 and P. N. Wilkinson3 1Jet Propulsion Laboratory, 4800 Oak Grove Drive, M/S 169-327, Pasadena, CA 91109, USA 2Chajnantor Observatory, California Institute of Technology, 1200 E. California Blvd., M/S 105-24, Pasadena, CA 91125, USA 3Jodrell Bank Observatory, University of Manchester, Macclesfield, Cheshire SK11 9DL 4Departamento de Astronom´ıa, Universidad de Chile, Casilla 36-D, Santiago, Chile Accepted 2007 May 4. Received 2007 May 1; in original form 2007 February 22 ABSTRACT We have mapped four regions of the southern Galactic plane at 31 GHz with the Cosmic Background Imager. From the maps, we have extracted the flux densities for six of the brightest H II regions in the southern sky and compared them with multifrequency data from the literature. The fitted spectral index for each source was found to be close to the theoretical value expected for optically thin free–free emission, thus confirming that the majority of flux at 31 GHz is due to free–free emission from ionized gas with an electron temperature of ≈7000–8000 K. We also found that, for all six sources, the 31-GHz flux density was slightly higher than the predicted value from data in the literature. This excess emission could be due to spinning dust or another emission mechanism. -
Models of Radio Recombination Line Sources
Aust. J. Phys., 1979,32,261-77 Models of Radio Recombination Line Sources M.J. Batty School of Physics, University of Sydney, Sydney, N.S.W. 2006; present address: Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California 91103, U.S.A. Abstract Models for the southern HII regions RCW38, RCW49, the Carina Nebula, G305+0 and M17 are constructed using a range of line and continuum data. Electron temperatures in the range 5000-7300 K are derived from the analysis, and in most cases these are consistent with estimates obtained from radio continuum measurements. The presence of a low temperature (.;; 4000 K) outer region in RCW 38 is suggested by the low frequency line data. Density inhomogeneities are found to be significant in all sources, while the predicted line widths are consistent with an observed lack of collisional broadening at low frequencies. 1. Introduction Our current understanding of the physical conditions in gaseous nebulae has been aided by the use of radiofrequency recombination lines as probes of nebular electron temperature and density. In particular, it has been possible to interpret a wide range of recombination line and radio continuum data in terms of models with nonuniform electron density structure (e.g. Brocklehurst and Seaton 1972; Cato 1973; Lockman and Brown 1975). These models generally have the following characteristics: (i) a uniform, or near-uniform, electron temperature; (ii) spherical symmetry; (iii) a centrally peaked electron density distribution. The interpretation of nebular radio recombination lines has been concentrated on northern HII regions (mainly the Orion Nebula) due to the availability of obser vational data.