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" Tnos Are Cool": a Survey of the Trans-Neptunian Region VI. Herschel
Astronomy & Astrophysics manuscript no. classicalTNOsManuscript c ESO 2012 April 4, 2012 “TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel⋆/PACS observations and thermal modeling of 19 classical Kuiper belt objects E. Vilenius1, C. Kiss2, M. Mommert3, T. M¨uller1, P. Santos-Sanz4, A. Pal2, J. Stansberry5, M. Mueller6,7, N. Peixinho8,9 S. Fornasier4,10, E. Lellouch4, A. Delsanti11, A. Thirouin12, J. L. Ortiz12, R. Duffard12, D. Perna13,14, N. Szalai2, S. Protopapa15, F. Henry4, D. Hestroffer16, M. Rengel17, E. Dotto13, and P. Hartogh17 1 Max-Planck-Institut f¨ur extraterrestrische Physik, Postfach 1312, Giessenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Konkoly Observatory of the Hungarian Academy of Sciences, 1525 Budapest, PO Box 67, Hungary 3 Deutsches Zentrum f¨ur Luft- und Raumfahrt e.V., Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany 4 LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, France 5 Stewart Observatory, The University of Arizona, Tucson AZ 85721, USA 6 SRON LEA / HIFI ICC, Postbus 800, 9700AV Groningen, Netherlands 7 UNS-CNRS-Observatoire de la Cˆote d’Azur, Laboratoire Cassiope´e, BP 4229, 06304 Nice Cedex 04, France 8 Center for Geophysics of the University of Coimbra, Av. Dr. Dias da Silva, 3000-134 Coimbra, Portugal 9 Astronomical Observatory of the University of Coimbra, Almas de Freire, 3040-04 Coimbra, Portugal 10 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris, France 11 Laboratoire d’Astrophysique de Marseille, CNRS & Universit´ede Provence, 38 rue Fr´ed´eric Joliot-Curie, 13388 Marseille Cedex 13, France 12 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Camino Bajo de Hu´etor 50, 18008 Granada, Spain 13 INAF – Osservatorio Astronomico di Roma, via di Frascati, 33, 00040 Monte Porzio Catone, Italy 14 INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy 15 University of Maryland, College Park, MD 20742, USA 16 IMCCE, Observatoire de Paris, 77 av. -
Colours of Minor Bodies in the Outer Solar System II - a Statistical Analysis, Revisited
Astronomy & Astrophysics manuscript no. MBOSS2 c ESO 2012 April 26, 2012 Colours of Minor Bodies in the Outer Solar System II - A Statistical Analysis, Revisited O. R. Hainaut1, H. Boehnhardt2, and S. Protopapa3 1 European Southern Observatory (ESO), Karl Schwarzschild Straße, 85 748 Garching bei M¨unchen, Germany e-mail: [email protected] 2 Max-Planck-Institut f¨ur Sonnensystemforschung, Max-Planck Straße 2, 37 191 Katlenburg- Lindau, Germany 3 Department of Astronomy, University of Maryland, College Park, MD 20 742-2421, USA Received —; accepted — ABSTRACT We present an update of the visible and near-infrared colour database of Minor Bodies in the outer Solar System (MBOSSes), now including over 2000 measurement epochs of 555 objects, extracted from 100 articles. The list is fairly complete as of December 2011. The database is now large enough that dataset with a high dispersion can be safely identified and rejected from the analysis. The method used is safe for individual outliers. Most of the rejected papers were from the early days of MBOSS photometry. The individual measurements were combined so not to include possible rotational artefacts. The spectral gradient over the visible range is derived from the colours, as well as the R absolute magnitude M(1, 1). The average colours, absolute magnitude, spectral gradient are listed for each object, as well as their physico-dynamical classes using a classification adapted from Gladman et al., 2008. Colour-colour diagrams, histograms and various other plots are presented to illustrate and in- vestigate class characteristics and trends with other parameters, whose significance are evaluated using standard statistical tests. -
(90377) SEDNA and (90482) ORCUS1 Chadwick A
The Astrophysical Journal, 627:1057–1065, 2005 July 10 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. NEAR-INFRARED SURFACE PROPERTIES OF THE TWO INTRINSICALLY BRIGHTEST MINOR PLANETS: (90377) SEDNA AND (90482) ORCUS1 Chadwick A. Trujillo Gemini Observatory, Northern Operations Center, 670 North A’ohoku Place, Hilo, HI 96720; [email protected] Michael E. Brown California Institute of Technology, Division of Geological and Planetary Sciences, MS 150-21, Pasadena, CA 91125; [email protected] David L. Rabinowitz Physics Department, Yale Center for Astronomy and Astrophysics, Yale University, P.O. Box 208121, New Haven, CT 06520-8121; [email protected] and Thomas R. Geballe Gemini Observatory, Northern Operations Center, 670 North A’ohoku Place, Hilo, HI 96720; [email protected] Received 2004 March 26; accepted 2005 March 16 ABSTRACT We present low-resolution K-band spectra taken at the Gemini 8 m telescope of (90377) Sedna and (90482) Orcus (provisional designations 2003 VB12 and 2004 DW, respectively), currently the two minor planets with the greatest absolute magnitudes (i.e., the two most reflective minor planets). We place crude limits on the surface composition of these two bodies using a Hapke model for a wide variety of assumed albedos. The unusual minor planet Sedna was discovered on UT 2003 November 14 at roughly 90 AU, with 1.6 times the heliocentric and perihelion dis- tances of any other bound minor planet. It is the first solar system object discovered between the Kuiper Belt and the Oort Cloud and may represent a transition population between the two. -
On the Irrelevance of Being a PLUTO! Size Scale of Stars and Planets
On the irrelevance of being a PLUTO! Mayank Vahia DAA, TIFR Irrelevance of being Pluto 1 Size Scale of Stars and Planets Irrelevance of being Pluto 2 1 1 AU 700 Dsun Irrelevance of being Pluto 3 16 Dsun Irrelevance of being Pluto 4 2 Solar System 109 DEarth Irrelevance of being Pluto 5 11 DEarth Venus Irrelevance of being Pluto 6 3 Irrelevance of being Pluto 7 Solar System visible to unaided eye Irrelevance of being Pluto 8 4 Solar System at the beginning of 20 th Century Irrelevance of being Pluto 9 Solar System of my text book (30 years ago) Irrelevance of being Pluto 10 5 Asteroid Belt (Discovered in 1977) Irrelevance of being Pluto 11 The ‘Planet’ Pluto • Pluto is a 14 th magnitude object. • It is NOT visible to naked eye (neither are Uranus and Neptune). • It was discovered by American astronomer Clyde Tombaugh in 1930. Irrelevance of being Pluto 12 6 Prediction of Pluto • Percival Lowell and William H. Pickering are credited with the theoretical work on Pluto’s orbit done in 1909 based on data of Neptune’s orbital changes. • Venkatesh Ketakar had predicted it in May 1911 issue of Bulletin of the Astronomical Society of France. • He modelled his computations after those of Pierre-Simon Laplace who had analysed the motions of the satellites of Jupiter. • His location was within 1 o of its correct location. • He had predicted ts orbital period was 242.28 (248) years and a distance of 38.95 (39.53) A.U. • He had also predicted another planet at 59.573 A.U. -
Tnos Mueller
TNOs are Cool: A Survey of the Transneptunian Region Thomas M¨uller& The TNOs-are-Cool Team MPE Garching (37 members, 19 institutes, 9 countries) 1 Thomas M¨uller TNOs are Cool! • OT KP with 370 hours Overview • PACS and SPIRE photometric point-source observations • characterisation of about 140 Trans-Neptunian Objects (with known orbits) • target with a few mJy up to 400 mJy • Key element: highly reliable photometric ac- curacy in 3 (6) bands • time-critical observations with follow-on constraint (confusion noise) 2 Science Goals in a Nut Shell • Radiometric size and albedo solutions - accurate sizes (! volumes) of TNOs ! primordial (D> 200 km) size distribution - accurate spectroscopic and polarimetric modeling - albedo vs Size vs Colour vs Composition vs Orbit vs Binarity vs ... ! probe formation and evolution processes • Thermophysical properties (from 3 to 6 Pacs/Spire bands) - temperatures & thermal inertia ! ice vs rock surface, surface type - emissivity ! grain size information - beaming parameter ! surface roughness • Binary densities: mass from Ke- • Thermal lightcurves pler's 3rd law, volume from Herschel ! disentangle albedo/shape ! basic geophysical parameter ! spin-axis orientation ! interior structure/composition ! thermal inertia ! binary formation mechanism ! large surface structures 3 Thomas M¨uller TNOs are Cool! Herschel Study of the Kuiperbelt & TNOs: ! a benchmark for understanding the solar system debris disk, and extra-solar ones as well! M¨uller et al. 2009, Earth, Moon & Planet 105, 209-219 4 Thomas M¨uller TNOs -
Transneptunian Object Taxonomy 181
Fulchignoni et al.: Transneptunian Object Taxonomy 181 Transneptunian Object Taxonomy Marcello Fulchignoni LESIA, Observatoire de Paris Irina Belskaya Kharkiv National University Maria Antonietta Barucci LESIA, Observatoire de Paris Maria Cristina De Sanctis IASF-INAF, Rome Alain Doressoundiram LESIA, Observatoire de Paris A taxonomic scheme based on multivariate statistics is proposed to distinguish groups of TNOs having the same behavior concerning their BVRIJ colors. As in the case of asteroids, the broadband spectrophotometry provides a first hint about the bulk compositional properties of the TNOs’ surfaces. Principal components (PC) analysis shows that most of the TNOs’ color variability can be accounted for by a single component (i.e., a linear combination of the col- ors): All the studied objects are distributed along a quasicontinuous trend spanning from “gray” (neutral color with respect to those of the Sun) to very “red” (showing a spectacular increase in the reflectance of the I and J bands). A finer structure is superimposed to this trend and four homogeneous “compositional” classes emerge clearly, and independently from the PC analy- sis, if the TNO sample is analyzed with a grouping technique (the G-mode statistics). The first class (designed as BB) contains the objects that are neutral in color with respect to the Sun, while the RR class contains the very red ones. Two intermediate classes are separated by the G mode: the BR and the IR, which are clearly distinguished by the reflectance relative increases in the R and I bands. Some characteristics of the classes are deduced that extend to all the objects of a given class the properties that are common to those members of the class for which more detailed data are available (observed activity, full spectra, albedo). -
Water Ice in the Kuiper Belt Comes Through Three Separate Distinct Processes
AJ, in press Water ice in the Kuiper belt M.E. Brown Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 [email protected] E.L. Schaller NASA Dryden Aircraft Operations Facility, Palmdale, CA 93550 and National Suborbital Education and Research Center, University of North Dakota, Grand Forks, ND, 85202 W.C. Fraser Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 ABSTRACT We examine a large collection of low resolution near-infrared spectra of Kuiper belt objects and centaurs in an attempt to understand the presence of water ice in the Kuiper belt. We find that water ice on the surface of these objects occurs in three separate manners: (1) Haumea family members uniquely show surfaces of nearly pure water ice, presumably a consequence of the fragmentation of the icy mantle of a larger differentiated proto-Haumea; (2) large objects with absolute magnitudes of H < 3 (and a limited number to H = 4.5) have surface coverings of water ice – perhaps mixed with ammonia – that appears to be related to possibly ancient cryovolcanism on these large objects; and (3) smaller KBOs and centaurs which are neither Haumea family arXiv:1204.3638v1 [astro-ph.EP] 16 Apr 2012 members nor cold-classical KBOs appear to divide into two families (which we refer to as “neutral” and “red”), each of which is a mixture of a common nearly-neutral component and either a slightly red or very red component that also includes water ice. A model suggesting that the difference between neutral and red objects s due to formation in an early compact solar system either inside or outside, respectively, of the ∼20 AU methanol evaporation line is supported by the observation that methanol is only detected on the reddest objects, which are those which would be expected to have the most of the methanol containing mixture. -
Integral-Field Spectroscopy of (90482) Orcus-Vanth
Astronomy & Astrophysics manuscript no. main c ESO 2018 August 1, 2018 Integral-field spectroscopy of (90482) Orcus-Vanth⋆ Benoˆıt Carry1,2,3, Daniel Hestroffer4, Francesca E. DeMeo2,5, Audrey Thirouin6, J´erˆome Berthier4, Pedro Lacerda7, Bruno Sicardy2,8,9, Alain Doressoundiram2, Christophe Dumas10, David Farrelly11, and Thomas G. M¨uller12 1 European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Ca˜nada, Madrid, Spain e-mail: [email protected] 2 LESIA, Observatoire de Paris, CNRS, 5 place Jules Janssen, 92190 Meudon, France 3 Universit´eParis 7 Denis-Diderot, 5 rue Thomas Mann, 75205 Paris CEDEX, France 4 IMCCE, Observatoire de Paris, UPMC, CNRS, 77 av. Denfert Rochereau 75014 Paris, France 5 Department of Earth, Atmospheric, and Planetary Sciences, MIT, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 6 Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Apt 3004, 18080 Granada, Spain 7 Queen’s University, Belfast, County Antrim BT7 1NN, Ireland 8 Universit´ePierre et Marie Curie, 4, Place Jussieu, 75252 Paris cedex 5, France 9 Institut Universitaire de France, 103, Bld Saint Michel, 75005 Paris, France 10 Alonso de C´ordova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile 11 Utah State University, 0300 Old Main Hill, Logan, UT 84322, USA 12 Max-Planck-Institut f¨ur extraterrestrische Physik (MPE), Giessenbachstrasse, 85748 Garching, Germany Received ; accepted ABSTRACT Aims. We seek to constrain the surface composition of the Trans-Neptunian Object (90482) Orcus and its small satellite Vanth, as well as their mass and density. Methods. We acquired near-infrared spectra (1.4–2.4 µm) of (90482) Orcus and its companion Vanth using the adaptive-optics-fed integral-field spectrograph SINFONI mounted on Yepun/UT4 at the European Southern Observatory Very Large Telescope. -
Prerequisites for Explosive Cryovolcanism on Dwarf Planet-Class Kuiper Belt Objects ⇑ M
Icarus 246 (2015) 48–64 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Prerequisites for explosive cryovolcanism on dwarf planet-class Kuiper belt objects ⇑ M. Neveu a, , S.J. Desch a, E.L. Shock a,b, C.R. Glein c a School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404, USA b Department of Chemistry and Biochemistry, Arizona State University, Tempe, AZ 85287-1404, USA c Geophysical Laboratory, Carnegie Institution of Washington, 5251 Broad Branch Rd. NW, Washington, DC 20015, USA article info abstract Article history: Explosive extrusion of cold material from the interior of icy bodies, or cryovolcanism, has been observed Received 30 December 2013 on Enceladus and, perhaps, Europa, Triton, and Ceres. It may explain the observed evidence for a young Revised 21 March 2014 surface on Charon (Pluto’s surface is masked by frosts). Here, we evaluate prerequisites for cryovolcanism Accepted 25 March 2014 on dwarf planet-class Kuiper belt objects (KBOs). We first review the likely spatial and temporal extent of Available online 5 April 2014 subsurface liquid, proposed mechanisms to overcome the negative buoyancy of liquid water in ice, and the volatile inventory of KBOs. We then present a new geochemical equilibrium model for volatile exso- Keywords: lution and its ability to drive upward crack propagation. This novel approach bridges geophysics and geo- Charon chemistry, and extends geochemical modeling to the seldom-explored realm of liquid water at subzero Interiors Pluto temperatures. We show that carbon monoxide (CO) is a key volatile for gas-driven fluid ascent; whereas Satellites, formation CO2 and sulfur gases only play a minor role. -
“Tnos Are Cool”: a Survey of the Trans-Neptunian Region VI
A&A 541, A94 (2012) Astronomy DOI: 10.1051/0004-6361/201118743 & c ESO 2012 Astrophysics “TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel/PACS observations and thermal modeling of 19 classical Kuiper belt objects E. Vilenius1,C.Kiss2, M. Mommert3,T.Müller1, P. Santos-Sanz4,A.Pal2, J. Stansberry5, M. Mueller6,7, N. Peixinho8,9, S. Fornasier4,10,E.Lellouch4, A. Delsanti11, A. Thirouin12, J. L. Ortiz12,R.Duffard12,D.Perna13,14, N. Szalai2, S. Protopapa15,F.Henry4,D.Hestroffer16,M.Rengel17, E. Dotto13, and P. Hartogh17 1 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Konkoly Observatory of the Hungarian Academy of Sciences, 1525 Budapest, PO Box 67, Hungary 3 Deutsches Zentrum für Luft- und Raumfahrt e.V., Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany 4 LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, France 5 Stewart Observatory, The University of Arizona, Tucson AZ 85721, USA 6 SRON LEA/HIFI ICC, Postbus 800, 9700AV Groningen, The Netherlands 7 UNS-CNRS-Observatoire de la Côte d’Azur, Laboratoire Cassiopée, BP 4229, 06304 Nice Cedex 04, France 8 Center for Geophysics of the University of Coimbra, Av. Dr. Dias da Silva, 3000-134 Coimbra, Portugal 9 Astronomical Observatory of the University of Coimbra, Almas de Freire, 3040-04 Coimbra, Portugal 10 Univ. Paris Diderot, Sorbonne Paris Cité, 4 rue Elsa Morante, 75205 Paris, France 11 Laboratoire d’Astrophysique de Marseille, CNRS & Université de Provence, 38 rue Frédéric Joliot-Curie, 13388 Marseille Cedex 13, France 12 Instituto de Astrofísica de Andalucía (CSIC), Camino Bajo de Huétor 50, 18008 Granada, Spain 13 INAF – Osservatorio Astronomico di Roma, via di Frascati, 33, 00040 Monte Porzio Catone, Italy 14 INAF – Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy 15 University of Maryland, College Park, MD 20742, USA 16 IMCCE, Observatoire de Paris, 77 Av. -
The Surface of the Transneptunian Object 90482 Orcus
A&A 437, 1115–1120 (2005) Astronomy DOI: 10.1051/0004-6361:20042533 & c ESO 2005 Astrophysics The surface of the transneptunian object 90482 Orcus C. de Bergh1, A. Delsanti1,2,G.P.Tozzi3,E.Dotto4, A. Doressoundiram1, and M. A. Barucci1, 1 LESIA, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France e-mail: [email protected] 2 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, Hawaii 96822, USA 3 INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy 4 INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone (Roma), Italy Received 14 December 2004 / Accepted 11 March 2005 Abstract. In April 2004, we obtained visible and near-infrared spectroscopy and photometry of the Transneptunian Object (TNO) 90482 Orcus (2004 DW) with the European Southern Observatory (ESO) 8-m telescopes of the Very Large Telescope (VLT) in Chile. This object, discovered on February 17, 2004, is one of the largest known TNOs, and it belongs to the dynamical class of Plutinos. The high signal-to-noise ratio visible spectrum recorded on April 11, 2004, is nearly flat, in good agreement with the BVRI photometry we obtained the same night and with photometric measurements from Rabinowitz et al. (2004, IAU Circ., 8295). The near-infrared spectra (J, H,andK bands) were obtained on April 11, 12, and 21, 2004. Relatively strong absorptions attributed to water ice were detected around 1.5 and 2 µm. We compare these data with spectra of Orcus obtained at the 3.56-m Telescopio Nazionale Galileo (TNG) by Fornasier et al. -
Future Surveys of the Kuiper Belt 573
Trujillo: Future Surveys of the Kuiper Belt 573 Future Surveys of the Kuiper Belt Chadwick A. Trujillo Gemini North Observatory The next decade of Kuiper belt object (KBO) science will be completely dominated by the output of two surveys. These two surveys, the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) and the Large Synoptic Survey Telescope (LSST), will increase the total number of known KBOs by factors of 25 to 150 over the next decade. This discovery rate will not be uniform — it will come as a large flood of information during the first year of operation. If software development allows, additional depth may be gained in successive years if data can be combined across years to find bodies that are too faint to be detected in an individual visit. Not only will the surveys increase the number of objects dramatically, but they will also be sensitive to heliocentric distances far beyond 100 AU due to their multiyear survey methodology. In this work, we outline a basic timeline of operation of these two powerful surveys and the science that will be enabled by their data output, as well as other significant advances in KBO surveys expected in the next decade. 1. INTRODUCTION de Bergh et al., 2005; Cruikshank et al., 2005; Stern, 2005; Trujillo et al., 2005; Gaudi et al., 2005; Brown et al., 2005; The coming decade should see a dramatic increase in our Matese et al., 2005; Doressoundiram et al., 2005; Licandro knowledge of the Kuiper belt object (KBO) population due et al., 2006; Rabinowitz et al., 2006; Barkume et al., 2006; entirely to new telescopic survey experiments.