DOCSLIB.ORG

Our Changing View of Saturn

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Our Changing View of Saturn Newsletter WELLINGTON ASTRONOMICAL SOCIETY April 2011, Volume 41, Number 3, ISSN 01147706, www.was.org.nz Wednesday,6thofApril, 7:30PMatCarterObservatory THIS MONTH’S MEETING FEATURES Our Changing View of Saturn ... over the last 400 years (with special emphasis on its ring system) Description: The talk consists of two distinct sections. The first one outlines important milestones in the history of the observation of the planet Saturn. The second part focusses on the ring system and some of the more recent discoveries and their attempted explanations. In this issue: Presidents rePort 2 AUrorA AstronoMY sCHooL 5 CoUnCiL oF tHe WeLLinGton CAnCeLed 5 AstronoMiCAL soCietY inC. 2 AstronoMY WitHoUt Borders oBserVinG At PAUAtAHAnUi 3 Presents: GLoBAL AstronoMY MontH tAWA CoLLeGe AstronoMY CLUB 3 APriL 2011 6 oBserVinG At tHoMAs KinG 3 GreAt ideAs to Get tHe PUBLiC in YoUr MArCH AreA inVoLVed in GAM APriL 2011 7 CrossWord AnsWers 3 rAsnz ConFerenCe 2011, nAPier, MAY 27 GLoBULAr CLUsters oF tHe AUtUMn sKY 4 to 30. 7 stArGAzers Astro CAMP 5 tHe eVeninG sKY in APriL 2011 9 WAs APriL’s tALK resUMee 5 Cross Word WitH MUrrAY ForBes 10 04-2011 Presidents Report COUNCIL OF THE WELLINGTON Last months talk with Hari Mogosanu late this month but we will be involved ASTRONOMICAL showed us what she was doing in the with the program at Tawa College on SOCIETY INC. Dessert in the USA . She lived in a Mars Astronomy month. surface simulation for two weeks. This Observing at the Thomas King was an excellent presentation and this Observatory is every Friday evening but President: showed with the number of questions ring Ross Powell first. GordonHudson that were asked after the show. Thanks [email protected] Hari for a great presentation. The WAS Dobsonian telescopes are all Ph 04 236 5125 out on hire at present. Anyone wanting The societies CCD camera the ST7 is to hire one of the societies Dobsonians Vice-President: RogerButland getting quite a lot of use at present as should call Chris Monigatti. [email protected] Roger Butland and myself have been Ph 04 478 0419 sorting out the problems with focus and The WAS Research Group was arranging the filter wheel so that it can approached by the Gifford Observatory Secretary: RossPowell be controlled. This is now done and we Trust to see if any of our members would [email protected] are ready to start imaging variable stars. be interested in using the Observatory Ph 04 389 9765 all be it with a different telescope The observing at the Pauatahanui installed which would possibility be a Treasurer: JohnTalbot Observatory had to be canceled on C14 with a CCD camera attached. This [email protected] the 5th of March but 12th of March proposal is still under discussion. There Ph 04 293 4620 which was our backup night was nice is no further update on this. and clear. Chris tells me that only one student and his dad show up. However I have been working on the Thomas Chris managed to take a couple of King Observatory fixing the dome so Newsletter Editor: photos through the telescope. that it will not come off in high winds. HaritinaMogosanu I have also stripped the walls of the [email protected] We are not having a very good run for display panels and the room is about to any observing at Pauatahanui over the be painted. Work still needs to be done last 12 months when the observatory Committee on the steps going up to the telescope. was only used three times last year. FrankAndrews We are waiting for thePainters to come [email protected] We are considering moving the in and paint the walls. ChrisMonigatti observatory to a more accessible site Carter Observatory decided to start [email protected] which would mean it would get more running two observing evenings each Mob o21 890 222 use but not necessary better weather. week starting on Tuesday 5th of April JohnHomes Watch for further developments on this. and this evening will be run by the [email protected] The weekend camp at Tatum Park Phoenix Society while the WAS will run AlineHomes will be on April 8-9 see article in this the Saturday night observing this will [email protected] newsletter. start on the 9th of April. We therefore require two volunteers every Saturday Positions Outside Council The next observing at Pauatahanui will evening so put your name forward to Email newsletter be on April 30th starting at 8.00pm. Ross Powell as soon as possible. MurrayForbes This year we have added an extra [email protected] Next months talk will be another of our Saturday to the observing at Pautahanui popular Video’s the title is ‘Telescope each month so if one is clouded or Hunting the Edge of Space’. rained out we will have the following www.was.org.nz Saturday to fall back on. Remember the RASNZ conference coming up in May in Napier and now Because of the Full Moon on the 18th is a good time to register. this is why our observing evening is Page 2 ISSN 01147706, NUMBER 3, VOLUME 41, WAS NEWSLETTER March Crossword Tawa College answers Astronomy Club invites students, parents, and friends Across of Tawa College to a presentation 6. VENUs‚ - a very cloudy planet; followed by observing session at the 9. DEIMOS‚ - one of the Moons of Mars; school celebrating: 10. SOHo‚ - satellite observatory studying the sun; 11. MESSIER‚ - a catalogue; 12. eCLiPSINGBINArY‚ - clip singer in bay Saturn Watch – Global Star Party – (anagram); 15. ANDROMEDA‚ - Largest galaxy Saturday 2 April, talk Saturday 9 April, talk in the Local Group; 16. BINArY‚ - a double star; begins 7:00 pm begins 7:00 pm 18. dAY‚ - 24 hours; 20. LMC‚ - could be mistaken for a cloud; 23. BiGBAnGtHEORY‚ ‘Changing Views of Saturn’ followed by observing Saturn, the - A cosmological model; 24. HST‚ - an by roland idaczyk Moon, and the fabulous southern orbiting telescope; 26. NOVA‚ - a new star; night sky 29. BAr‚ - some spiral galaxies have one; Galileo’s drawing of Saturn, 30. HoUr‚ - unit of time; 31. NOON‚ - mid- ‘Can Kiwis help colonise Mars?’ day; 34. PAVo‚ - The Peacock constellation; 1610, 1616 35. KePLER‚ - early German astronomer by Haritina Mogosanu - formulated 3 laws of planetary motion; 36. CLUSTER‚ - An open or globular ...; 40. AZIMUtH‚ - horizontal angle around the sky; 44. LEO‚ - A lion circling the earth; 45. KiWi‚ - new zealander; 46. VIRGo‚ - Constellation with spica; 47. DENEB‚ - alpha Cygnus; 48. ATOM‚ - smallest indivisible piece of a element; 50. APoGEE‚ - When the Moon is furthest from the earth; 51. PRECESSION‚ - son’s recipe (anagram); 53. SIDEREAL‚ - star time; 54. FUSION‚ - process that powers stars; Down 1. iCe‚ - frozen liquid; 2. GAs‚ - solid, liquid Hubble Space Telescope, March 22, 2004 or ...; 3. PeLe‚ - volcano on io; 4. IO‚ - one of the Galilean satellites; 5. ZODIAC‚ - also a small inflated rubber boat; 6. eV GA‚ - alpha P.t.A. building – above the Canteen, at the end of the rugby Lyr; 7. sCHMIDT‚ - type of telescope; 8. SEYFERT‚ - type of galaxy with unusally field. in the event of cloudy skies, this event will continue, bright nucleus; 13. sHePHERD‚ - astronaut; although observing will be replaced by video. 14. rUtHCRISP‚ - Carter observatory’s public telescope; 17. nAdir‚ - opposite to zenith; 19. APHeLION‚ - one phial (anagram); 21. HALo‚ - angels and galaxies both have one; 22. PoLARIS‚ - the north star; OBSERVING AT 25. sCORPiUs‚ - constellation with a sting; 27. PANDORA‚ - a shepherd satellite of saturn’s THOMAS KING F ring, also the first women in Greek mythology; 28. oBAFGKM‚ - spectral classes; 32. tAUrUs‚ OBSERVING AT All public observing evenings - You don’t want this constellation in a China shop; will be held at the Thomas King 33. JODRELLBAnK‚ - site of the Lovell radio PAUATAHANUI telescope; 35. KiLoGrAM‚ - The SI unit of Observatory run by our Observatory mass; 37. LoKi‚ - volcano on io; 38. sMC‚ - The next observing evening at Director Ross Powell. from 8:30. satellite galaxy to the Milky Way; 39. GIOTTO‚ Pauatahanui is on April 30th Ring Ross on 389 9765 to check - name of ESA spacecraft that intercepted starting at 8.00pm. If doubtful Halley’s comet; 41. UFo‚ - flying saucer; if there are public observing evenings 42. HYADES‚ - an open cluster in taurus; please ring Chris Monigatti on on most FRIDAYS, starting as soon as 43. GiBBoUs‚ - a phase of the Moon; his mobile 021 890 222 to see if it gets dark depending on the weather 49. MASS‚ - i weight 6 times less on the Moon, the session is going ahead. but still have the same ???; 52. ION‚ - an and Ross’s availability. arrested atom; WAS NEWSLETTER VOLUME 41, NUMBER 3, ISSN 01147706 Page 3 Globular clusters of the Autumn sky As we move into the autumn we get to see The rivalry between this cluster and a number of globular clusters gracing our Omega Centauri for “best glob” is evening skies and this article will cover legendary. Visible to the unaided eye near some of the brightest and best. to the SMC it is an easy object to find in binoculars it is even better with the use What is a globular cluster? of a telescope. The cluster is roughly the There are two types of star clusters in and same size of the Full Moon and is the around our galaxy. second brightest globular cluster in the sky and has a very bright and dense core. Open clusters that are found along the It is a massive globular cluster containing plane of our Galaxy and come in a variety millions of stars and is about 16,700 light of sizes, ages and are “loose” or “open” in 47 Tucanae years away and 120 light years across.
Load more

Recommended publications
  • XMM-Newton Observations of the Galactic Globular Clusters NGC 2808 and NGC 4372
    A&A 480, 397–407 (2008) Astronomy DOI: 10.1051/0004-6361:20078327 & c ESO 2008 Astrophysics XMM-Newton observations of the Galactic globular clusters NGC 2808 and NGC 4372 M. Servillat, N. A. Webb, and D. Barret CESR, Université Paul Sabatier, CNRS, 9 avenue du Colonel Roche, 31400 Toulouse, France e-mail: [email protected] Received 20 July 2007 / Accepted 28 November 2007 ABSTRACT Aims. Galactic globular clusters harbour binary systems that are detected as faint X-ray sources. These close binaries are thought to play an important role in the stability of the clusters by liberating energy and delaying the inevitable core collapse of globular clusters. The inventory of close binaries and their identification is therefore essential. Methods. We present XMM-Newton observations of two Galactic globular clusters: NGC 2808 and NGC 4372. We use X-ray spectral and variability analysis combined with ultra-violet observations made with the XMM-Newton optical monitor and published data from the Hubble Space Telescope to identify sources associated with the clusters. We compare the results of our observations with estimates from population synthesis models. Results. Five sources out of 96 are likely to be related to NGC 2808. Nine sources are found in the field of view of NGC 4372, none being located inside its half-mass radius. We find one quiescent neutron star low mass X-ray binary candidate in the core of NGC 2808, and propose that the majority of the central sources in NGC 2808 are cataclysmic variables. An estimation leads to 20±10 cataclysmic variables with luminosity above 4.25 × 1031 erg s−1.
    [Show full text]
  • 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).
    [Show full text]
  • High-Precision Asteroseismology of Dense Stellar Fields
    Experimental Astronomy https://doi.org/10.1007/s10686-021-09711-1 ORIGINAL ARTICLE HAYDN High-precision AsteroseismologY of DeNse stellar fields Andrea Miglio1,2,3 · Leo´ Girardi4 · Frank Grundahl5 · Benoit Mosser6 · Nate Bastian7 · Angela Bragaglia3 · Karsten Brogaard5,8 · Gael¨ Buldgen9 · William Chantereau7 · William Chaplin1 · Cristina Chiappini10 · Marc-Antoine Dupret11 · Patrick Eggenberger9 · Mark Gieles12,13 · Robert Izzard14 · Daisuke Kawata15 · Christoffer Karoff5 · Nadege` Lagarde16 · Ted Mackereth1,17,18,19 · Demetrio Magrin4 · Georges Meynet9 · Eric Michel20 · Josefina Montalban´ 1 · Valerio Nascimbeni4 · Arlette Noels11 · Giampaolo Piotto21 · Roberto Ragazzoni4 · Igor Soszynski´ 22 · Eline Tolstoy23 · Silvia Toonen1,24 · Amaury Triaud1 · Fiorenzo Vincenzo1,25 Received: 29 July 2020 / Accepted: 9 February 2021 / © The Author(s) 2021 Abstract In the last decade, the Kepler and CoRoT space-photometry missions have demon- strated the potential of asteroseismology as a novel, versatile and powerful tool to perform exquisite tests of stellar physics, and to enable precise and accurate char- acterisations of stellar properties, with impact on both exoplanetary and Galactic astrophysics. Based on our improved understanding of the strengths and limitations of such a tool, we argue for a new small/medium space mission dedicated to gath- ering high-precision, high-cadence, long photometric series in dense stellar fields. Such a mission will lead to breakthroughs in stellar astrophysics, especially in the metal poor regime, will elucidate the evolution and formation of open and globular clusters, and aid our understanding of the assembly history and chemodynamics of the Milky Way’s bulge and a few nearby dwarf galaxies. Keywords Stars: low-mass · Globular clusters · Galaxy: bulge · Galaxies: dwarf · Asteroseismology A list of people who have expressed interest for HAYDN is available here: https://www.asterochronometry.eu/haydn/people.html Andrea Miglio [email protected] Extended author information available on the last page of the article.
    [Show full text]
  • ESO Annual Report 2004 ESO Annual Report 2004 Presented to the Council by the Director General Dr
    ESO Annual Report 2004 ESO Annual Report 2004 presented to the Council by the Director General Dr. Catherine Cesarsky View of La Silla from the 3.6-m telescope. ESO is the foremost intergovernmental European Science and Technology organi- sation in the field of ground-based as- trophysics. It is supported by eleven coun- tries: Belgium, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and the United Kingdom. Created in 1962, ESO provides state-of- the-art research facilities to European astronomers and astrophysicists. In pur- suit of this task, ESO’s activities cover a wide spectrum including the design and construction of world-class ground-based observational facilities for the member- state scientists, large telescope projects, design of innovative scientific instruments, developing new and advanced techno- logies, furthering European co-operation and carrying out European educational programmes. ESO operates at three sites in the Ataca- ma desert region of Chile. The first site The VLT is a most unusual telescope, is at La Silla, a mountain 600 km north of based on the latest technology. It is not Santiago de Chile, at 2 400 m altitude. just one, but an array of 4 telescopes, It is equipped with several optical tele- each with a main mirror of 8.2-m diame- scopes with mirror diameters of up to ter. With one such telescope, images 3.6-metres. The 3.5-m New Technology of celestial objects as faint as magnitude Telescope (NTT) was the first in the 30 have been obtained in a one-hour ex- world to have a computer-controlled main posure.
    [Show full text]
  • Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
    Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al.
    [Show full text]
  • FY13 High-Level Deliverables
    National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................
    [Show full text]
  • Arxiv:Astro-Ph/0507464V2 14 Jan 2009 Eso H Ai Fitgae A-Vpooer.The Photometry
    Astrophysics and Space Science DOI 10.1007/s•••••-•••-••••-• Horizontal Branch Stars: The Interplay between Observations and Theory, and Insights into the Formation of the Galaxy M. Catelan1,2 c Springer-Verlag •••• Abstract We review and discuss horizontal branch importance of bright type II Cepheids as tracers of (HB) stars in a broad astrophysical context, includ- faint blue HB stars in distant systems is also empha- ing both variable and non-variable stars. A reassess- sized. The relationship between the absolute V mag- ment of the Oosterhoff dichotomy is presented, which nitude of the HB at the RR Lyrae level and metallic- provides unprecedented detail regarding its origin and ity, as obtained on the basis of trigonometric parallax systematics. We show that the Oosterhoff dichotomy measurements for the star RR Lyr, is also revisited. and the distribution of globular clusters in the HB Taking into due account the evolutionary status of RR morphology-metallicity plane both exclude, with high Lyr, the derived relation implies a true distance mod- statistical significance, the possibility that the Galac- ulus to the LMC of (m−M)0 = 18.44 ± 0.11. Tech- tic halo may have formed from the accretion of dwarf niques providing discrepant slopes and zero points for galaxies resembling present-day Milky Way satellites the MV (RRL) − [Fe/H] relation are briefly discussed. such as Fornax, Sagittarius, and the LMC—an argu- We provide a convenient analytical fit to theoretical ment which, due to its strong reliance on the ancient model predictions for the period change rates of RR RR Lyrae stars, is essentially independent of the chem- Lyrae stars in globular clusters, and compare the model ical evolution of these systems after the very earli- results with the available data.
    [Show full text]
  • Central Kinematics of the Globular Cluster NGC 2808: Upper Limit on the Mass of an Intermediate-Mass Black Hole,
    A&A 542, A129 (2012) Astronomy DOI: 10.1051/0004-6361/201219375 & c ESO 2012 Astrophysics Central kinematics of the globular cluster NGC 2808: upper limit on the mass of an intermediate-mass black hole, N. Lützgendorf1, M. Kissler-Patig1,K.Gebhardt2,H.Baumgardt3, E. Noyola4,5, B. Jalali6, P. T. de Zeeuw1,7, and N. Neumayer1 1 European Southern Observatory (ESO), Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany e-mail: [email protected] 2 Astronomy Department, University of Texas at Austin, Austin, TX 78712, USA 3 School of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, Australia 4 Instituto de Astronomia, Universidad Nacional Autonoma de Mexico (UNAM), AP 70-264, 04510 Mexico 5 University Observatory, Ludwig Maximilians University, 81679 Munich, Germany 6 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany 7 Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands Received 10 April 2012 / Accepted 18 April 2012 ABSTRACT Context. Globular clusters are an excellent laboratory for stellar population and dynamical research. Recent studies have shown that these stellar systems are not as simple as previously assumed. With multiple stellar populations as well as outer rotation and mass segregation they turn out to exhibit high complexity. This includes intermediate-mass black holes (IMBHs) which are proposed to sit at the centers of some massive globular clusters. Today’s high angular resolution ground based spectrographs allow velocity-dispersion measurements at a spatial resolution comparable to the radius of influence for plausible IMBH masses, and to detect changes in the inner velocity-dispersion profile.
    [Show full text]
  • Curriculum Vitæ: Manuela Zoccali Associate Professor, Puc
    CURRICULUM VITÆ: MANUELA ZOCCALI ASSOCIATE PROFESSOR, PUC PERSONAL INFORMATION Name: Manuela Surname: Zoccali Birth place: Reggio Calabria, Italy Birth date: September 11th, 1971 Citizenship: Italian Current Position: Profesor Asociado Departamento de Astronomía y Astrofísica P. Universidad Católica de Chile Av. Vicuña Mackenna 4860, 782-0436, Macul, Santiago, Chile Telephone: +56-2-354-7253 Fax: +56-2-354-4948 e-mail: [email protected] SPOKEN LANGUAGES Italian: mother tongue English: fluent Spanish: fluent French: basic EDUCATIONAL BACKGROUND 1995 — Laurea (Bachelor) Degree in Astronomy , Università di Padova, Italy (Magna cum Laude) Thesis title: Funzione di luminosità e di massa dell'ammasso globulare galattico NGC1261. Advisors: Prof. M. Capaccioli, Prof. G. Piotto 2000 — PhD in Astronomy, Università di Padova, Italy (no marks for Phd, in Italy) Thesis title: Observational Constraints on the Evolutionary and Dynamical Properties of Low Mass Stars. Advisor: Prof. G. Piotto EMPLOYMENT HISTORY 2000 – 2003 Post-doctoral Fellowship at the European Southern Observatory (ESO), Garching bei München, Germany 2003 – 2004 Post-doctoral Princeton-PUC Prize Fellowship between the University of Princeton (NJ, USA) and the P. Univ. Católica de Chile. 2004 – 2008 Assistant Professor, P. Universidad Católica de Chile. 2008 – Present Associate Professor, P. Universidad Católica de Chile. PRIMARY RESEARCH INTERESTS Stellar Populations, Globular Star Clusters, The Galactic Bulge, Stellar Abundances, The Initial Mass Function, Galaxy Formation and Evolution. TEACHING 2004 – 2009 Teaching of Astronomy courses for Astronomy students at the undergraduate (Astronomy, Astronomy Lab I and II, Galactic Astronomy) and graduate levels (Topics in Astrophysics, Galaxy Formation). Physics courses for undergraduate Engineering students (Classical Mechanics). 2005 – 2009 Advisor of 2 PhD (F.
    [Show full text]
  • Testing Metal Poor Stellar Models and Isochrones with Hst Parallaxes of Metal Poor Stars
    Draft version November 11, 2018 Preprint typeset using LATEX style AASTeX6 v. 1.0 TESTING METAL POOR STELLAR MODELS AND ISOCHRONES WITH HST PARALLAXES OF METAL POOR STARS B. Chaboyer1,2, B.E. McArthur3, E. O'Malley1, G.F. Benedict3, G. A.Feiden4, T.E. Harrison5, A. McWilliam6, E.P. Nelan7, R.J. Patterson8, A. Sarajedini9 1Dept. of Physics and Astronomy, Dartmouth College, Hanover, NH 03755 USA 2Max-Planck-Institut f¨urAstrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching bei M¨unchen, Germany 3McDonald Observatory, University of Texas, Austin, TX 78712 USA 4Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20, Uppsala, Sweden 5Dept. of Astronomy, New Mexico State University, Las Cruces, NM 88003 USA 6The Observatories of the Carnegie Institute of Washington, Pasadena, CA 91101 USA 7Space Telescope Science Institute, Baltimore, MD 21218 USA 8Dept. of Astronomy, University of Virginia, Charlottesville, VA 22904 USA 9Dept. of Astronomy, University of Florida, Gainesville, FL 32611 USA ABSTRACT Hubble Space Telescope (HST) fine guidance sensor observations were used to obtain parallaxes of eight metal-poor ([Fe=H] < −1:4) stars. The parallaxes of these stars determined by the new Hipparcos reduction average 17% accuracy, in contrast to our new HST parallaxes which average 1% accuracy and have errors on the individual parallaxes ranging from 85 to 144 microarcseconds. This parallax data has been combined with HST ACS photometry in the F606W and F814W filters to obtain the absolute magnitudes of the stars with an accuracy of 0.02 to 0.03 magnitudes. Six of these stars are on the main sequence (with −2:7 < [Fe=H] < −1:8), and suitable for testing metal-poor stellar evolution models and determining the distances to metal-poor globular clusters.
    [Show full text]
  • SOAR Publications Sorted by Year Then Author (Last Updated November 24, 2016 by Nicole Auza)
    No longer maintained, see home page for current information! SOAR publications Sorted by year then author (Last updated November 24, 2016 by Nicole Auza) ⇒If your publication(s) are not listed in this document, please fill in this form to enable us to keep a complete list of SOAR publications. Contents 1 Refereed papers 1 2 Conference proceedings 35 3 SPIE Conference Series 39 4 PhD theses 46 5 Meeting (incl. AAS) abstracts 47 6 Circulars 55 7 ArXiv 60 8 Other 61 1 Refereed papers (2016,2015, 2014, 2013, 2012, 2011, 2010, 2009, 2008, 2007, 2006, 2005) 2016 [1] Alvarez-Candal, A., Pinilla-Alonso, N., Ortiz, J. L., Duffard, R., Morales, N., Santos- Sanz, P., Thirouin, A., & Silva, J. S. 2016 Feb, Absolute magnitudes and phase coefficients of trans-Neptunian objects, A&A, 586, A155 URL http://adsabs.harvard.edu/abs/2016A%26A...586A.155A [2] A´lvarez Crespo, N., Masetti, N., Ricci, F., Landoni, M., Pati˜no-Alvarez,´ V., Mas- saro, F., D’Abrusco, R., Paggi, A., Chavushyan, V., Jim´enez-Bail´on, E., Torrealba, J., Latronico, L., La Franca, F., Smith, H. A., & Tosti, G. 2016 Feb, Optical Spectro- scopic Observations of Gamma-ray Blazar Candidates. V. TNG, KPNO, and OAN Observations of Blazar Candidates of Uncertain Type in the Northern Hemisphere, AJ, 151, 32 URL http://adsabs.harvard.edu/abs/2016AJ....151...32A [3] A´lvarez Crespo, N., Massaro, F., Milisavljevic, D., Landoni, M., Chavushyan, V., Pati˜no-Alvarez,´ V., Masetti, N., Jim´enez-Bail´on, E., Strader, J., Chomiuk, L., Kata- giri, H., Kagaya, M., Cheung, C.
    [Show full text]
  • Summary of Eighth Meeting on Hot Subdwarfs and Related Objects
    Open Astron. 2017; 26: 120–133 Review Article Anthony Eugene Lynas-Gray* Summary of Eighth Meeting on Hot Subdwarfs and Related Objects https://doi.org/10.1515/astro-2017-0429 Received Sep 30, 2017; accepted Dec 15, 2017 Abstract: Subjects discussed during the Eighth Meeting on Hot Subdwarfs and Related Objects are summarised. In par- ticular, a succinct presentation is given of challenges to stellar evolution arising from recent observations. Mention is also made of topics not covered in the meeting such as the need for small revisions to stellar envelope opacities currently in use. I conclude with a brief discussion of current developments which will influence future hot subdwarf research and necessary initiatives that need to be taken. Keywords: stars: subdwarfs, stars: evolution, stars: chemically peculiar 1 Subjects Discussed bility are given by Ge et al. (2010, 2015) while Pavlovskii & Ivanova (2015) and Pavlovskii et al. (2017) model the asymptotic response of donor stars in interacting binary Heber (2009, 2016) and Lynas-Gray (2004) review the de- systems to very rapid mass-loss, characterised by adia- velopment of hot subdwarf research. For more detailed batic expansion throughout their interiors. Han’s conclu- summaries of early work, see Zwicky (1965a,b) and Green- sions were: a) the Roche model may be invalid for extreme stein (1987). Much of the work discussed during the Eighth mass ratios, b) Roche lobe overflow (RLOF) may be more Meeting on Hot Subdwarfs and Related Objects (hereafter stable than previously supposed and c) Common Envelope sdOB8) reflects advances made since Heber (2016) submit- (CE) ejection may be more efficient for red giant – Main ted his review for publication.
    [Show full text]