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Joint Institute for VLBI in Europe Biennial Report 2011-2012
Joint Institute For VLBI in Europe 11-12 Biennial report 2011-2012 The Joint Institute for VLBI in Europe (JIVE) was established as a scientific foundation in December 1993. JIVE’s mandate is to support the operations of the European VLBI Network (EVN) in the widest sense. JIVE’s operations are supported via multi‐national funds from the following organisations: Netherlands Institute for Radio Astronomy (ASTRON), the Netherlands, National Center for Scientific Research (CNRS), France National Geographical Institute (IGN), Spain, Italian National Institute of Astrophysics (INAF), Italy, Max Planck Institute for Radio Astronomy (MPIfR), Germany, National Astronomical Observatories of China (NAOC), China, National Research Foundation (NRF), South Africa Netherlands Organisation for Scientific Research (NWO), the Netherlands, Onsala Space Observatory (OSO), Sweden, Science & Technology Facilities Council (STFC), UK Joint Institute for VLBI in Europe | Biennial report 2011‐2012 Contents 1. INSTITUTE ....................................................................................................................................................... 1 1.1. preparing for the next funding cycle ..................................................................................................... 1 1.2. enhancing the VLBI capabilities ............................................................................................................. 2 1.3. JIVE events ............................................................................................................................................ -
The Size Distribution of the Neptune Trojans and the Missing Intermediate-Sized Planetesimals
The Astrophysical Journal Letters, 723:L233–L237, 2010 November 10 doi:10.1088/2041-8205/723/2/L233 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE SIZE DISTRIBUTION OF THE NEPTUNE TROJANS AND THE MISSING INTERMEDIATE-SIZED PLANETESIMALS Scott S. Sheppard1 and Chadwick A. Trujillo2 1 Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Rd. NW, Washington, DC 20015, USA; [email protected] 2 Gemini Observatory, 670 North A’ohoku Place, Hilo, HI 96720, USA Received 2010 July 29; accepted 2010 September 29; published 2010 October 20 ABSTRACT We present an ultra-deep survey for Neptune Trojans using the Subaru 8.2 m and Magellan 6.5 m telescopes. 2 The survey reached a 50% detection efficiency in the R band at mR = 25.7 mag and covered 49 deg of sky. mR = 25.7 mag corresponds to Neptune Trojans that are about 16 km in radius (assuming an albedo of 0.05). A paucity of smaller Neptune Trojans (radii < 45 km) compared with larger ones was found. The brightest Neptune Trojans appear to follow a steep power-law slope (q = 5 ± 1) similar to the brightest objects in the other known stable reservoirs such as the Kuiper Belt, Jupiter Trojans, and main belt asteroids. We find a roll-over for the Neptune Trojans that occurs around a radius of r = 45 ± 10 km (mR = 23.5 ± 0.3), which is also very similar to the other stable reservoirs. All the observed stable regions in the solar system show evidence for Missing Intermediate-Sized Planetesimals (MISPs). -
Trailing (L5) Neptune Trojans: 2004 KV18 and 2008 LC18
Trailing (L5) Neptune Trojans: 2004 KV18 and 2008 LC18 Pu Guan, Li-Yong Zhou,∗ Jian Li Astronomy Department, Nanjing University, Key Laboratory of Modern Astronomy and Astrophysics in MOE, Nanjing 210093, China November 11, 2018 Abstract The population of Neptune Trojans is believed to be bigger than that of Jupiter Trojans and that of asteroids in the main belt, although only eight members of this far distant asteroid swarm have been observed up to now. Six leading Neptune Trojans around the Lagrange point L4 dis- covered earlier have been studied in detail, but two trailing ones found recently around the L5 point, 2004 KV18 and 2008 LC18, have not been investigated yet. In this paper, we report our investigations on the dynamical behaviors of these two new Neptune Trojans. Our calculations show that the asteroid 2004 KV18 is a temporary Neptune Trojan. Most probably, it was captured into the trailing Trojan cloud no earlier than 2.03 105 yr ago, and it will not keep this identity no later than 1.65 105 yr in future. Based on the× statistics on our orbital simulations, we argue that this object is more× like a scattered Kuiper belt object. On the contrary, the orbit of asteroid 2008 LC18 is much more stable. Among the clone orbits spread within the orbital uncertainties, a considerable portion of clones may survive on the L5 tadpole orbits for 4Gyr. The strong depen- dence of the stability on the semimajor axis and resonant angle suggests that further observations are badly needed to confine the orbit in the stable region. -
Dr. Alex Harrison Parker Postdoctoral Fellow in Planetary Astronomy
Dr. Alex Harrison Parker Postdoctoral Fellow in Planetary Astronomy Department of Astronomy University of California at Berkeley Phone: 360-599-5346 B-20 Hearst Field Annex #3411 [email protected] Berkeley, CA 94720-3411 www.astro.uvic.ca/~alexhp/ Higher Education Institution Field Degree Years University of Victoria Astronomy PhD 2007|2011. University of Washington Physics & Astronomy BSc 2005|2007. Whatcom Community College Physics AAS 2002|2005. PhD Details \Ultra-Wide Trans-Neptunian Binaries: Tracers of the Outer Solar System's History" | Advised by Dr. JJ Kavelaars, National Research Council of Canada | Thesis archived online at http://hdl.handle.net/1828/3400 | Enrolled September 2007 | Defended July 2011 | Awarded November 2011 Professional Appointments University of California at Berkeley - Postdoctoral Fellow 2013 | Present. University of California at Berkeley Department of Astronomy Ongoing support for New Horizons post-Pluto/Kuiper Belt mission development. Kuiper Belt Binaries team lead for CFHT-OSSOS Large Program. See \Ongoing Research" document. New Horizons Outer Solar System Science Fellow 2011 | 2013. Harvard-Smithsonian Center for Astrophysics, Cambridge MA USA. Survey specialist; searching for candidate Kuiper Belt Objects for NASA's New Horizons spacecraft to visit after its 2015 Pluto encounter. Perform advanced survey image analysis, trajectory analysis, target orbit and physical characterization. Manage central astrometry database and target submission to the Minor Planet Center. Science case development for remote-sensing observations of Kuiper Belt Objects at medium range (0.1-0.5 AU). National Science Foundation | Graduate Research Fellow 2008 | 2011. University of Victoria, Victoria BC Canada. PhD research in binary Kuiper Belt Object orbits, dynamics, and origin. -
2011 Hm102: Discovery of a High-Inclination L5 Neptune Trojan in the Search for a Post-Pluto New Horizons Target
The Astronomical Journal, 145:96 (6pp), 2013 April doi:10.1088/0004-6256/145/4/96 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. 2011 HM102: DISCOVERY OF A HIGH-INCLINATION L5 NEPTUNE TROJAN IN THE SEARCH FOR A POST-PLUTO NEW HORIZONS TARGET Alex H. Parker1, Marc W. Buie2,DavidJ.Osip3, Stephen D. J. Gwyn4, Matthew J. Holman1, David M. Borncamp2, John R. Spencer2, Susan D. Benecchi5, Richard P. Binzel6, Francesca E. DeMeo6,Sebastian´ Fabbro4, Cesar I. Fuentes7, Pamela L. Gay8, J. J. Kavelaars4, Brian A. McLeod1, Jean-Marc Petit9, Scott S. Sheppard5, S. Alan Stern2, David J. Tholen10, David E. Trilling7, Darin A. Ragozzine1,11, Lawrence H. Wasserman12, and the Ice Hunters13 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected] 2 Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA 3 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 4 Canadian Astronomy Data Centre, National Research Council of Canada, 5071 W. Saanich Road, Victoria, BC V9E 2E7, Canada 5 Department of Terrestrial Magnetism, Carnegie Institute of Washington, 5251 Broad Branch Road NW, Washington, DC 20015, USA 6 Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 7 Department of Physics & Astronomy, Northern Arizona University, S San Francisco St, Flagstaff, AZ 86011, USA 8 The Center for Science, Technology, Engineering and Mathematics (STEM) Research, Education, and Outreach, Southern -
SSSC Commissioning Notes
SSSC Commissioning Notes In this document, the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Solar System Science Collaboration (SSSC) has compiled a series of commissioning notes, proposing on-sky observing strategies during commissioning that would enhance opportunities for science validation and testing of the Rubin Observatory’s data management pipelines. The SSSC has ranked the commissioning notes below into priorities (high, medium, and low) based on the expected contribution to verifying the scientific capability of Rubin Observatory and informing Year 1 LSST operations. PROPOSED HIGH PRIORITY WIDE-FAST-DEEP OBSERVING COMMISSIONING TASKS Validation of Incremental Template Generation Proposed by: Meg Schwamb & Mario Jurić Email Contact for Further Information: [email protected], [email protected] RA(s)/Decs(s): Agnostic to the specific pointing and cadence of observations Filter(s) Required: grizy Brief Description of Observing strategy: Wide-Fast-Deep (WFD) cadence might be preferable to fully characterize the incremental template generation pipelines, but observing strategy is flexible. The main constraint is obtaining the appropriate number of images per filter that meet the criteria for template generation. Rationale: These proposed observations will test and validate the incremental template generation capability of the data management pipelines and confirm incremental templates can be successfully generated at the start of operations for Solar System objects to be detected 1 in -
Long-Range Kuiper Belt Targets Observed by the Hubble Space Telescope ⇑ S.D
Icarus 246 (2015) 369–374 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus New Horizons: Long-range Kuiper Belt targets observed by the Hubble Space Telescope ⇑ S.D. Benecchi a,b, , K.S. Noll c, H.A. Weaver d, J.R. Spencer e, S.A. Stern e, M.W. Buie e, A.H. Parker f a Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719, United States b Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road, NW, Washington, DC 20015, United States c NASA Goddard Space Flight Center, 8800 Greenbelt Road, Code 693, Greenbelt, MD 20771, United States d Space Department, Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, United States e Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302, United States f Department of Astronomy, University of California at Berkeley, B-20 Hearst Field Annex #3411, Berkeley, CA 94720, United States article info abstract Article history: We report on Hubble Space Telescope (HST) observations of three Kuiper Belt Objects (KBOs), discovered Received 5 February 2014 in our dedicated ground-based search campaign, that are candidates for long-range observations from the Revised 14 April 2014 New Horizons spacecraft: 2011 JY31, 2011 HZ102, and 2013 LU35. Astrometry with HST enables both cur- Accepted 15 April 2014 rent and future critical accuracy improvements for orbit precision, required for possible New Horizons Available online 2 May 2014 observations, beyond what can be obtained from the ground. Photometric colors of all three objects are red, typical of the Cold Classical dynamical population within which they reside; they are also the Keywords: faintest KBOs to have had their colors measured. -
2004 KV18: a Visitor from the Scattered Disc to the Neptune Trojan Population J
Mon. Not. R. Astron. Soc. 426, 159–166 (2012) doi:10.1111/j.1365-2966.2012.21717.x 2004 KV18: a visitor from the scattered disc to the Neptune Trojan population J. Horner1 and P. S. Lykawka2 1Department of Astrophysics, School of Physics, University of New South Wales, Sydney, NSW 2052, Australia 2Astronomy Group, Faculty of Social and Natural Sciences, Kinki University, Shinkamikosaka 228-3, Higashiosaka-shi, Osaka 577-0813, Japan Accepted 2012 July 12. Received 2012 July 12; in original form 2012 June 14 ABSTRACT Downloaded from We have performed a detailed dynamical study of the recently identified Neptunian Trojan 2004 KV18, only the second object to be discovered librating around Neptune’s trailing Lagrange point, L5. We find that 2004 KV18 is moving on a highly unstable orbit, and was most likely captured from the Centaur population at some point in the last ∼1 Myr, having originated in http://mnras.oxfordjournals.org/ the scattered disc, beyond the orbit of Neptune. The instability of 2004 KV18 is so great that many of the test particles studied leave the Neptunian Trojan cloud within just ∼0.1–0.3 Myr, and it takes just 37 Myr for half of the 91 125 test particles created to study its dynamical behaviour to be removed from the Solar system entirely. Unlike the other Neptunian Trojans previously found to display dynamical instability on 100-Myr time-scales (2001 QR322 and 2008 LC18), 2004 KV18 displays such extreme instability that it must be a temporarily captured Trojan, rather than a primordial member of the Neptunian Trojan population. -
Institute for Astronomy University of Hawai'i at M¯Anoa Publications in Calendar Year 2013
Institute for Astronomy University of Hawai‘i at Manoa¯ Publications in Calendar Year 2013 Aberasturi, M., Burgasser, A. J., Mora, A., Reid, I. N., Barnes, J. E., & Privon, G. C. Experiments with IDEN- Looper, D., Solano, E., & Mart´ın, E. L. Hubble Space TIKIT. In ASP Conf. Ser. 477: Galaxy Mergers in an Telescope WFC3 Observations of L and T dwarfs. Evolving Universe, 89–96 (2013) Mem. Soc. Astron. Italiana, 84, 939 (2013) Batalha, N. M., et al., including Howard, A. W. Planetary Albrecht, S., Winn, J. N., Marcy, G. W., Howard, A. W., Candidates Observed by Kepler. III. Analysis of the First Isaacson, H., & Johnson, J. A. Low Stellar Obliquities in 16 Months of Data. ApJS, 204, 24 (2013) Compact Multiplanet Systems. ApJ, 771, 11 (2013) Bauer, J. M., et al., including Meech, K. J. Centaurs and Scat- Al-Haddad, N., et al., including Roussev, I. I. Magnetic Field tered Disk Objects in the Thermal Infrared: Analysis of Configuration Models and Reconstruction Methods for WISE/NEOWISE Observations. ApJ, 773, 22 (2013) Interplanetary Coronal Mass Ejections. Sol. Phys., 284, Baugh, P., King, J. R., Deliyannis, C. P., & Boesgaard, A. M. 129–149 (2013) A Spectroscopic Analysis of the Eclipsing Short-Period Aller, K. M., Kraus, A. L., & Liu, M. C. A Pan-STARRS + Binary V505 Persei and the Origin of the Lithium Dip. UKIDSS Search for Young, Wide Planetary-Mass Com- PASP, 125, 753–758 (2013) panions in Upper Sco. Mem. Soc. Astron. Italiana, 84, Beaumont, C. N., Offner, S. S. R., Shetty, R., Glover, 1038–1040 (2013) S. C. -
A Proposal for a Research Settlement on 2011 HM102 and a Framework
Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 7 April 2021 doi:10.20944/preprints202104.0215.v1 1 The Trojan Initiative: A Proposal For A Research Settlement On 2011 HM102 and A Framework for Future Settlement on Asteroids Briana Chen1*, Geetika Chitturi1*, Archit Kalra1*, Raghav Sriram1* 1: Carmel High School *: All authors contributed equally to the production of this manuscript and are hence written in alphabetical order. © 2021 by the author(s). Distributed under a Creative Commons CC BY license. Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 7 April 2021 doi:10.20944/preprints202104.0215.v1 2 Contents Abstract…………...………………………………………………………………………….....…4 Reason for Settling 2011 HM102…………………………………………………………....……...5 Population……..……………………………………………………………………………….….6 Travel to Settlement..……………………………………………………………………………...7 Antimatter Engine…………………………………………………………………………7 Settlement Materials .……………………………………………………………………………..9 Settlement Design .………………………………………………………………………………11 A Model For the Simulation of Artificial Gravity…………………………………….....11 Layout of Structure……………………………………………………………………....13 Power Sources…………………………………………………………………………...16 Shielding and Protection………………………………………………………….……..18 Maintenance of Life.………………………………………………………………………….....20 Importance of Growing Food………………………………………………….……...…20 Sustainable Crop Growth…………………………………………………….……...…..20 Water Recovery…………………………………………………………….……...…….22 Oxygen Recycling………………………………………………………….……………23 Eliminating Carbon Dioxide…………………………………………………………….24 Air Filtration………………………………………………….………………….………24 -
The Dynamics of Ringed Small Bodies
THE DYNAMICS OF RINGED SMALL BODIES A Thesis Submitted by Jeremy R. Wood For the Award of Doctor of Philosophy 2018 Abstract In 2013, the startling discovery of a pair of rings around the Centaur 10199 Chariklo opened up a new subfield of astronomy - the study of ringed small bodies. Since that discovery, a ring has been discovered around the dwarf planet 136108 Haumea, and a re-examination of star occultation data for the Centaur 2060 Chiron showed it could have a ring structure of its own. The reason why the discovery of rings around Chariklo or Chiron is rather shocking is because Centaurs frequently suffer close encounters with the giant planets in the Centaur region, and these close encounters can not only fatally destroy any rings around a Centaur but can also destroy the small body itself. In this research, we determine the likelihood that any rings around Chariklo or Chiron could have formed before the body entered the Centaur region and survived up to the present day by avoiding ring-destroying close encounters with the giant planets. And in accordance with that, develop and then improve a scale to measure the severity of a close encounter between a ringed small body and a planet. We determine the severity of a close encounter by finding the minimum dis- tance obtained between the small body and the planet during the encounter, dmin, and comparing it to the critical distances of the Roche limit, tidal dis- ruption distance, the Hill radius and \ring limit". The values of these critical distances comprise our close encounter severity scale. -
The Proposed Origin of Our Solar System with Planet Migration DOI
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Digital Commons The Proceedings of the International Conference on Creationism Volume 8 Article 35 2018 The proposed origin of our solar system with planet migration DOI: https://doi.org/10.15385/jpicc.2018.8.1.10 Wayne R. Spencer none Follow this and additional works at: http://digitalcommons.cedarville.edu/icc_proceedings Part of the The unS and the Solar System Commons Browse the contents of this volume of The Proceedings of the International Conference on Creationism. Recommended Citation Spencer, W.R. 2018. The proposed origin of our solar system with planet migration. In Proceedings of the Eighth International Conference on Creationism, ed. J.H. Whitmore, pp. 71–81. Pittsburgh, Pennsylvania: Creation Science Fellowship. Spencer, W.R. 2018. The proposed origin of our solar system with planet migration. In Proceedings of the Eighth International Conference on Creationism, ed. J.H. Whitmore, pp. 71–81. Pittsburgh, Pennsylvania: Creation Science Fellowship. THE PROPOSED ORIGIN OF OUR SOLAR SYSTEM WITH PLANET MIGRATION Wayne R. Spencer, Independent scholar, Irving, TX 75063 USA, [email protected] ABSTRACT Two new models to explain the origin and history of our solar system are reviewed from a creation perspective, the Grand Tack model and the Nice model. These new theories propose that the four outer planets formed closer to the Sun, as well as closer together, than today. Then their orbits underwent periods of migration. Theories developed in the research on extrasolar planet systems are today being applied to our own solar system.