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Správa O Činnosti Organizácie SAV Za Rok 2017
Astronomický ústav SAV Správa o činnosti organizácie SAV za rok 2017 Tatranská Lomnica január 2018 Obsah osnovy Správy o činnosti organizácie SAV za rok 2017 1. Základné údaje o organizácii 2. Vedecká činnosť 3. Doktorandské štúdium, iná pedagogická činnosť a budovanie ľudských zdrojov pre vedu a techniku 4. Medzinárodná vedecká spolupráca 5. Vedná politika 6. Spolupráca s VŠ a inými subjektmi v oblasti vedy a techniky 7. Spolupráca s aplikačnou a hospodárskou sférou 8. Aktivity pre Národnú radu SR, vládu SR, ústredné orgány štátnej správy SR a iné organizácie 9. Vedecko-organizačné a popularizačné aktivity 10. Činnosť knižnično-informačného pracoviska 11. Aktivity v orgánoch SAV 12. Hospodárenie organizácie 13. Nadácie a fondy pri organizácii SAV 14. Iné významné činnosti organizácie SAV 15. Vyznamenania, ocenenia a ceny udelené organizácii a pracovníkom organizácie SAV 16. Poskytovanie informácií v súlade so zákonom o slobodnom prístupe k informáciám 17. Problémy a podnety pre činnosť SAV PRÍLOHY A Zoznam zamestnancov a doktorandov organizácie k 31.12.2017 B Projekty riešené v organizácii C Publikačná činnosť organizácie D Údaje o pedagogickej činnosti organizácie E Medzinárodná mobilita organizácie F Vedecko-popularizačná činnosť pracovníkov organizácie SAV Správa o činnosti organizácie SAV 1. Základné údaje o organizácii 1.1. Kontaktné údaje Názov: Astronomický ústav SAV Riaditeľ: Mgr. Martin Vaňko, PhD. Zástupca riaditeľa: Mgr. Peter Gömöry, PhD. Vedecký tajomník: Mgr. Marián Jakubík, PhD. Predseda vedeckej rady: RNDr. Luboš Neslušan, CSc. Člen snemu SAV: Mgr. Marián Jakubík, PhD. Adresa: Astronomický ústav SAV, 059 60 Tatranská Lomnica http://www.ta3.sk Tel.: 052/7879111 Fax: 052/4467656 E-mail: [email protected] Názvy a adresy detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty Dúbravská cesta 9, 845 04 Bratislava Vedúci detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty prof. -
The Discovery of Herbig-Haro Objects in Ldn 673
Draft version December 4, 2017 Typeset using LATEX default style in AASTeX61 THE DISCOVERY OF HERBIG-HARO OBJECTS IN LDN 673 T. A. Rector1 | R. Y. Shuping2 | L. Prato3 | H. Schweiker4, 5, 6 | 1Department of Physics and Astronomy, University of Alaska Anchorage, Anchorage, AK 99508, USA 2Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA 3Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA 4National Optical Astronomy Observatory, Tucson, AZ 85719, USA 5Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 6WIYN Observatory, Tucson, AZ 85719, USA ABSTRACT We report the discovery of twelve faint Herbig-Haro (HH) objects in LDN 673 found using a novel color-composite imaging method that reveals faint Hα emission in complex environments. Follow-up observations in [S II] confirmed their classification as HH objects. Potential driving sources are identified from the Spitzer c2d Legacy Program catalog and other infrared observations. The twelve new HH objects can be divided into three groups: Four are likely associated with a cluster of eight YSO class I/II IR sources that lie between them; five are colinear with the T Tauri multiple star system AS 353, and are likely driven by the same source as HH 32 and HH 332; three are bisected by a very red source that coincides with an infrared dark cloud. We also provide updated coordinates for the three components of HH 332. Inaccurate numbers were given for this object in the discovery paper. -
The Future of the GBT
The Future of the GBT Felix J. Lockman NRAO Green Bank Arecibo, July 2009 UNOFFICIAL The Future of the GBT Felix J. Lockman NRAO Green Bank Arecibo, July 2009 Characteristics of the GBT Large Collecting Area Sensitive to Low Surface Brightness Sky Coverage & Tracking (>85%) Angular Resolution Frequency Coverage Radio Quiet Zone Unblocked Aperture state-of-art receivers & detectors modern control software flexible scheduling Unique capabilities which complement EVLA, VLBA, and ALMA The Advantage of Unblocked Optics Dynamic Range Near sidelobes reduced by a factor >10 from conventional antennas Gain & Sensitivity The 100 meter diameter GBT performs better than a 120 meter conventional antenna Reduced Interference 2002 panels active surface retroreflectors for future metrology A telescope designed to be enhanced Unique active surface →Unlike any other radio telescope← Green Bank and the GBT A telescope that works well over a factor of 1000 in frequency/wavelength / energy -- equivalent to the range from the infrared (10μ) to the soft X-ray (0.01μ) GALEX HST Chandra Spitzer “...just hitting its stride” Future Prospects & Development at NRAO and in the US Radio Community ~ 2008 NRAO Staff Retreat 4 AOC Auditorium, NRAO, Socorro, NM ~ April 10-11, 2008 A telescope for fundamental physics The fastest pulsars test our understanding of matter at the most extreme densities “A Radio Pulsar Spinning at 716 Hz” Hessels et al 2006 Science A telescope for fundamental physics The fastest pulsars test our understanding of matter at the most extreme densities -
LIST of PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute
LIST OF PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute of Department of Science and Technology, Govt. of India) Manora Peak, Naini Tal - 263 129, India (1955−2020) ABBREVIATIONS AA: Astronomy and Astrophysics AASS: Astronomy and Astrophysics Supplement Series ACTA: Acta Astronomica AJ: Astronomical Journal ANG: Annals de Geophysique Ap. J.: Astrophysical Journal ASP: Astronomical Society of Pacific ASR: Advances in Space Research ASS: Astrophysics and Space Science AE: Atmospheric Environment ASL: Atmospheric Science Letters BA: Baltic Astronomy BAC: Bulletin Astronomical Institute of Czechoslovakia BASI: Bulletin of the Astronomical Society of India BIVS: Bulletin of the Indian Vacuum Society BNIS: Bulletin of National Institute of Sciences CJAA: Chinese Journal of Astronomy and Astrophysics CS: Current Science EPS: Earth Planets Space GRL : Geophysical Research Letters IAU: International Astronomical Union IBVS: Information Bulletin on Variable Stars IJHS: Indian Journal of History of Science IJPAP: Indian Journal of Pure and Applied Physics IJRSP: Indian Journal of Radio and Space Physics INSA: Indian National Science Academy JAA: Journal of Astrophysics and Astronomy JAMC: Journal of Applied Meterology and Climatology JATP: Journal of Atmospheric and Terrestrial Physics JBAA: Journal of British Astronomical Association JCAP: Journal of Cosmology and Astroparticle Physics JESS : Jr. of Earth System Science JGR : Journal of Geophysical Research JIGR: Journal of Indian -
A Multi-Transition Molecular Line Study of Infrared Dark Cloud G331.71+00.59
Research in Astron. Astrophys. 2013 Vol. 13 No. 1, 28 – 38 Research in http://www.raa-journal.org http://www.iop.org/journals/raa Astronomy and Astrophysics A multi-transition molecular line study of infrared dark cloud G331.71+00.59 Nai-Ping Yu and Jun-Jie Wang National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; [email protected] NAOC-TU Joint Center for Astrophysics, Lhasa 850000, China Received 2012 March 12; accepted 2012 August 3 Abstract Using archive data from the Millimeter Astronomy Legacy Team Survey at 90 GHz (MALT90), carried out using the Mopra 22-m telescope, we made the first multi-transition molecular line study of infrared dark cloud (IRDC) MSXDC G331.71+00.59. Two molecular cores were found embedded in this IRDC. Each of these cores is associated with a known extended green object (EGO), indicating places of massive star formation. The HCO+ (1–0) and HNC (1–0) transitions show promi- nent blue or red asymmetric structures, suggesting outflow and inflow activities of young stellar objects (YSOs). Other detected molecular lines include H13CO+ (1– 0), C2H (1–0), HC3N (10–9), HNCO(40;4–30;3) and SiO (2–1), which are typical of hot cores and outflows. We regard the two EGOs as evolving from the IRDC to hot cores. Using public GLIMPS data, we investigate the spectral energy distribution of EGO G331.71+0.60. Our results support this EGO being a massive YSO driving the outflow. G331.71+0.58 may be at an earlier evolutionary stage. -
Physical Processes in the Interstellar Medium
Physical Processes in the Interstellar Medium Ralf S. Klessen and Simon C. O. Glover Abstract Interstellar space is filled with a dilute mixture of charged particles, atoms, molecules and dust grains, called the interstellar medium (ISM). Understand- ing its physical properties and dynamical behavior is of pivotal importance to many areas of astronomy and astrophysics. Galaxy formation and evolu- tion, the formation of stars, cosmic nucleosynthesis, the origin of large com- plex, prebiotic molecules and the abundance, structure and growth of dust grains which constitute the fundamental building blocks of planets, all these processes are intimately coupled to the physics of the interstellar medium. However, despite its importance, its structure and evolution is still not fully understood. Observations reveal that the interstellar medium is highly tur- bulent, consists of different chemical phases, and is characterized by complex structure on all resolvable spatial and temporal scales. Our current numerical and theoretical models describe it as a strongly coupled system that is far from equilibrium and where the different components are intricately linked to- gether by complex feedback loops. Describing the interstellar medium is truly a multi-scale and multi-physics problem. In these lecture notes we introduce the microphysics necessary to better understand the interstellar medium. We review the relations between large-scale and small-scale dynamics, we con- sider turbulence as one of the key drivers of galactic evolution, and we review the physical processes that lead to the formation of dense molecular clouds and that govern stellar birth in their interior. Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, 69120 Heidelberg, Germany e-mail: [email protected], [email protected] 1 Contents Physical Processes in the Interstellar Medium ............... -
Early Stages of Massive Star Formation
Early Stages of Massive Star Formation Vlas Sokolov Munchen¨ 2018 Early Stages of Massive Star Formation Vlas Sokolov Dissertation an der Fakultat¨ fur Physik der Ludwig–Maximilians–Universitat¨ Munchen¨ vorgelegt von Vlas Sokolov aus Kyjiw, Ukraine Munchen,¨ den 13 Juli 2018 Erstgutachter: Prof. Dr. Paola Caselli Zweitgutachter: Prof. Dr. Markus Kissler-Patig Tag der mundlichen¨ Prufung:¨ 27 August 2018 Contents Zusammenfassung xv Summary xvii 1 Introduction1 1.1 Overview......................................1 1.2 The Interstellar Medium..............................2 1.2.1 Molecular Clouds..............................5 1.3 Low-mass Star Formation..............................9 1.4 High-Mass Star and Cluster Formation....................... 12 1.4.1 Observational perspective......................... 14 1.4.2 Theoretical models............................. 16 1.4.3 IRDCs as the initial conditions of massive star formation......... 18 1.5 Methods....................................... 20 1.5.1 Radio Instrumentation........................... 20 1.5.2 Radiative Processes in the Dark Clouds.................. 22 1.5.3 Blackbody Dust Emission......................... 23 1.5.4 Ammonia inversion transitions....................... 26 1.6 This Thesis..................................... 28 2 Temperature structure and kinematics of the IRDC G035.39–00.33 31 2.1 Abstract....................................... 31 2.2 Introduction..................................... 32 2.3 Observations.................................... 33 2.3.1 GBT observations............................ -
Eric Keto Publications REFEREED JOURNALS 2014
{ 1 { Eric Keto Publications REFEREED JOURNALS 2014 (1) Chitsazzadeh, S., Di Francesco, J., Schnee, S., Friesen, R. K., Shimajiri, Y., Langston, G. I., Sadavoy, S. I., Bourke, T. L., Keto, E., Pineda, J. E., Takakuwa, S., Tatematsu, K., 2014, ApJ, 790, 129-150 "Physical and Chemical Characteristics of L1689-SMM16, an Oscillating Prestellar Core in Ophiuchus" (2) Zhang, Q. Qiu, K., Girart, J., Hauyu, L., Tang, Y.-W., Koch, P., Li, Z.-Y., Keto, E., Ho, P.T.P., Rao, R., Lai, S.-P., Ching, T.-C., Frau, P., Chen, H.-H., Li, H.-B., Padovani, M., Bontemps, S., Csengeri, T., Juarez, C., 2014, ApJ in press, arXiv:1407.3984, "Magnetic Fields and Massive Star Formation" (3) Inoue, M., Algaba-Marcos, J. C., Asada, K., Chang, C.-C., Chen, M.-T., Han, J., Hi- rashita, H., Ho, P.T.P., Hsieh, S.-N., Huang, T., Jiang, H., Koch, P. M., Kubo, D. Y., Kuo, C.-Y., Liu, B., Martin-Cocher, P., Matsushita, S., Meyer-Zhao, Z., Naka- mura, M., Nishioka, H., Nystrom, G., Pradel, N., Pu, H.-Y., Raffin, P. A., Shen, H.-Y., Snow, W., Srinivasan, R., Wei, T.-S., Blundell, R., Burgos, R., Grimes, P., Keto, E., Paine, S., Patel, N., Sridharan, T. K., Doeleman, S. S., Fish, V., Brisken, W., Napier, P., 2014, Radio Science Journal, in press, arXiv:1407.2450 "Greenland Telescope Project | Direct Confirmation of Black Hole with Sub-millimeter VLBI" (4) van Loo, S., Keto, E., Zhang, Q., 2014, ApJ, 789, 37-50, "Core and Filament Formation in Magnetized, Self-gravitating Isothermal Layers" (5) Keto, E., Burkert, A., 2014, MNRAS, 441, 1468-1473, "From filaments to oscillating starless -
Publications 2012
Publications - print summary 27 Feb 2013 1 *Abramowski, A.; Acero, F.; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Balzer, A.; Barnacka, A.; Barres de Almeida, U.; Becherini, Y.; Becker, J.; and 201 coauthors "A multiwavelength view of the flaring state of PKS 2155-304 in 2006". (C) A&A, 539, 149 (2012). 2 *Ackermann, M.; Ajello, J.; Ballet, G.; Barbiellini, D.; Bastieri, A.; Belfiore; Bellazzini, B.; Berenji, R.D. and 57 coauthors "Periodic emission from the Gamma-Ray Binary 1FGL J1018.6–5856". (O) Science, 335, 189-193 (2012). 3 *Agliozzo, C.; Umana, G.; Trigilio, C.; Buemi, C.; Leto, P.; Ingallinera, A.; Franzen, T.; Noriega-Crespo, A. "Radio detection of nebulae around four luminous blue variable stars in the Large Magellanic Cloud". (C) MNRAS, 426, 181-186 (2012). 4 *Ainsworth, R.E.; Scaife, A.M.M.; Ray, T.P.; Buckle, J.V.; Davies, M.; Franzen, T.M.O.; Grainge, K.J.B.; Hobson, M.P.; Shimwell, T.; and 12 coauthors "AMI radio continuum observations of young stellar objects with known outflows". (O) MNRAS, 423, 1089-1108 (2012). 5 *Allison, J.R.; Curran, S.J.; Emonts, B H.C.; Geréb, K.; Mahony, E.K.; Reeves, S.; Sadler, E.M.; Tanna, A.; Whiting, M.T.; Zwaan, M.A. "A search for 21 cm H I absorption in AT20G compact radio galaxies". (C) MNRAS, 423, 2601-2616 (2012). 6 *Allison, J R.; Sadler, E.M.; Whiting, M.T. "Application of a bayesian method to absorption spectral-line finding in simulated ASKAP Data". (A) PASA, 29, 221-228 (2012). 7 *Alves, M.I.R.; Davies, R.D.; Dickinson, C.; Calabretta, M.; Davis, R.; Staveley-Smith, L. -
Annual Report 2019
Annual Report 2019 IRAM Annual Report 2019 Published by IRAM © 2020 Director of publication Karl-Friedrich Schuster Edited by Cathy Berjaud, Frédéric Gueth With contributions from: Sébastien Blanchet, Edwige Chapillon, Antonio Córdoba, Isabelle Delaunay, Paolo Della Bosca, Eduard Driessen, Bertrand Gautier, Olivier Gentaz, Bastien Lefranc, Santiago Navarro, Roberto Neri, Juan Peñalver, Jérôme Pety, Francesco Pierfederici, Christophe Risacher, Miguel Sánchez Portal, Murielle Serlet, Karl-Friedrich Schuster, Karin Zacher Contents Introduction 4 Highlights of research with the IRAM telescopes 6 30-meter telescope 18 NOEMA 25 Grenoble headquarters 33 Frontend Group 33 Backend Group 37 Superconducting Devices Group 39 Mechanical Group 41 Computer Group 44 Science Software 45 IRAM ARC Node 47 Outreach 47 Personnel & Finance 50 Annexes 54 Telescope schedules 54 Publications 74 Committees 94 4 Introduction This annual report has been edited during complicated times of the corona virus epidemy but this should not distract us from looking back on 2019 which was thoroughly positive for IRAM although at the same time not without new challenges. The year 2019 was rich of important events and scientific results. In fact, NOEMA and powerful new instruments at the 30-meter telescope produce so much high-quality data that we are clearly entering in a new phase of how science is done with the IRAM facilities. At the same time IRAM users have started now to fully embrace the possibilities which are available through large programs and their significant impact on all fields of millimetre wave astronomy. The required infrastructure to treat the very important data flows which are generated through large programs and the ever-increasing performance of the IRAM instruments is now reaching a mature status with the direct optical fibre connections from the observatories to the Granada office and the Grenoble headquarter, the upgraded infrastructure in data storage and computing and finally the very significant advances in data reduction software. -
Newsletter Submillimeter Array Newsletter Number 20 | July 2015
SMA Newsletter Submillimeter Array Newsletter Number 20 | July 2015 CONTENTS FROM THE DIRECTOR 1 From the Director SCIENCE HIGHLIGHTS: Dear SMA Newsletter readers, 2 Nuclear Ashes and Outflow in the Eruptive Star Nova I am pleased to congratulate Thomas Kaminski (ESO Chile and MPI Bonn), Hua-Bai Vul 1670 Li (The Chinese University of Hong Kong), Jean Turner (UCLA) and their colleagues 5 Magnetic Fields Shape for their recent publications in Nature, summarized in this Newsletter. Collectively Molecular Cloud Structures 7 A Cosmic Factory of Stars these publications highlight the relative ease and utility of the SMA to observe bright, and Soot – SMA Reveals a chemically rich, galactic sources, and nearby galaxies; and further demonstrate the SMA’s Super Star Cluster of Highly Efficient Star Formation in relatively unique polarization capability. NGC 5253 I would also like to thank members of the SMA correlator group for their continued efforts TECHNICAL HIGHLIGHTS: to provide additional wideband signal-processing capacity. We now regularly observe with bu A SWARM of ROACHs the first tranche of SWARM, albeit at 3/4 speed, in parallel with the aging ASIC correlator, Has Been Deployed for Submillimeter Array Science in service since 2002. While not yet perfect, the additional 2x1.5 GHz bands, coupled with bp Securing Service - Availability the original 2x2 GHz bands of the ASIC correlator and double sideband receiver operation in Hawaii Using Virtual Infrastructure result in an instantaneous bandwidth of 14 GHz. This provides additional flexibility OTHER NEWS during spectral line observations and improves the continuum sensitivity of the SMA by about 40%. -
Resultados Concurso Apex 2007
Resultados Concurso Apex 2012-B Propuesta: 2012B-20 Investigador Principal: Guido Garay, Universidad de Chile. Título: Mapping The Structure of an Extreme Massive Star Forming Core. Resumen: The infrared dark cloud (IRDC) SDC335 is among the most massive and extreme objects in the recently constructed Spitzer catalogue of IRDCs. Within it are two of the most luminous candidate high mass protostars known. However compared to other candidate massive star forming clouds, SDC335 is in a very quiscent region making it a prime candidate for studying the initial conditions of massive star formation. The remarkable kinetics of SDC335 indicating infall along its _laments have recently been imaged in an ALMA Cycle 0 project. Here we request time to map SDC335 with LABOCA and SABOCA to image the dust continuum emission. In combination with the shorter wavelength data from HiGAL, these APEX observations will allow us to construct temperature and density maps of the region as well as better constrain the nature of the two young massive protostars within it. Tiempo asignado: 10 Horas Propuesta: 2012B-12 Investigador Principal: David R. Rodriguez, Universidad de Chile. Título: Characterizing Phoenix Giant Disks. Resumen: We are studying a new class of _rst-ascent giant stars that are surrounded by substantial dusty disks that are sometimes being accreted by the host giant star| Phoenix Giants. We propose APEX-LABOCA observations of a subset of the most infrared-bright systems to constrain their disk dust mass. Such observations will enable probes into the origin of the Phoenix Giant phenomenon. Tiempo asignado: 8 horas Propuesta: 2012B-17 Investigador Principal: Leopoldo Infante, Universidad de Chile.