DOCSLIB.ORG

(155140) 2005 UD and (3200) Phaethon*

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
(155140) 2005 UD and (3200) Phaethon* The Planetary Science Journal, 1:15 (15pp), 2020 June https://doi.org/10.3847/PSJ/ab8e45 © 2020. The Author(s). Published by the American Astronomical Society. New Evidence for a Physical Link between Asteroids (155140) 2005 UD and (3200) Phaethon* Maxime Devogèle1 , Eric MacLennan2, Annika Gustafsson3 , Nicholas Moskovitz1 , Joey Chatelain4, Galin Borisov5,6, Shinsuke Abe7, Tomoko Arai8, Grigori Fedorets2,9, Marin Ferrais10,11,12, Mikael Granvik2,13 , Emmanuel Jehin10, Lauri Siltala2,14, Mikko Pöntinen2, Michael Mommert1 , David Polishook15, Brian Skiff1, Paolo Tanga16, and Fumi Yoshida8 1 Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001, USA; [email protected] 2 Department of Physics, P.O. Box 64, FI-00014 University of Helsinki, Finland 3 Department of Astronomy & Planetary Science, Northern Arizona University, P.O. Box 6010, Flagstaff, AZ 86011, USA 4 Las Cumbres Observatory, CA, USA 5 Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, UK 6 Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72, Tsarigradsko Chaussèe Blvd., Sofia BG-1784, Bulgaria 7 Aerospace Engineering, Nihon University, 7-24-1 Narashinodai, Funabashi, Chiba 2748501, Japan 8 Planetary Exploration Research Center, Chiba Institute of Technology, Narashino, Japan 9 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK 10 Space sciences, Technologies & Astrophysics Research (STAR) Institute University of Liège Allée du 6 Août 19, B-4000 Liège, Belgium 11 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388, Marseille, France 12 Space sciences, Technologies, France 13 Division of Space Technology, LuleåUniversity of Technology, Box 848, SE-98128 Kiruna, Sweden 14 Nordic Optical Telescope, Apartado 474, E-38700 S/C de La Palma, Santa Cruz de Tenerife, Spain 15 Faculty of Physics, Weizmann Institute of Science, 234 Herzl St. Rehovot 7610001, Israel 16 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, CS34229, F-06304 Nice Cedex 4, France Received 2020 January 29; revised 2020 April 25; accepted 2020 April 27; published 2020 May 20 Abstract In 2018, the near-Earth object (155140) 2005 UD (hereafter UD) experienced a close fly by of the Earth. We present results from an observational campaign involving photometric, spectroscopic, and polarimetric observations carried out across a wide range of phase angles (0°.7–88°). We also analyze archival NEOWISE observations. We report an absolute magnitude of HV=17.51±0.02 mag and an albedo of pV=0.10±0.02. UD has been dynamically linked to Phaethon due their similar orbital configurations. Assuming similar surface properties, we derived new estimates for the diameters of Phaethon and UD of D=5.4±0.5 km and D=1.3±0.1 km, respectively. Thermophysical modeling of NEOWISE data suggests a surface thermal inertia +120 – – of G = 300-110 and regolith grain size in the range of 0.9 10 mm for UD and grain sizes of 3 30 mm for Phaethon. The light curve of UD displays a symmetric shape with a reduced amplitude of Am(0)=0.29 mag and increasing at a linear rate of 0.017 mag/° between phase angles of 0° and ∼25°. Little variation in light-curve morphology was observed throughout the apparition. Using light-curve inversion techniques, we obtained a sidereal rotation period P=5.235±0.005 hr. A search for rotational variation in spectroscopic and polarimetric properties yielded negative results within observational uncertainties of ∼10% μm−1 and ∼16%, respectively. In this work, we present new evidence that Phaethon and UD are similar in composition and surface properties, strengthening the arguments for a genetic relationship between these two objects. Unified Astronomy Thesaurus concepts: Near-Earth objects (1092); CCD observation (207); Astronomical techniques (1684); Photometry (1234); Polarimetry (1278); Spectroscopy (1558) 1. Introduction near-Earth space suggests that any dynamical correlation between the two bodies would not be maintained for more The Apollo-type near-Earth object (NEO; 155140) 2005UD than a few thousand years (Schunová et al. 2014). (hereafter UD) was discovered by the Catalina Sky Survey in (3200)Phaethon is an intriguing NEO both in terms of 2005 (Christensen et al. 2005, MPEC 2005-U22). Ohtsuka ( ) ( ) orbital elements and physical properties. It displays a highly et al. 2006 and Jewitt & Hsieh 2006 showed that it displays eccentric orbit (e=0.89) associated with a very low perihelion orbital properties and photometric colors similar to the well- ( = ) ( ) distance q 0.14 au . Its close approaches to the Sun suggest known NEO 3200 Phaethon, suggesting a genetic relation- that its surface experiences large diurnal and seasonal ship between the two. However, more recent dynamical temperature variations. Phaethon has also been linked to the analyses have raised questions regarding a formal link Geminid meteor stream (Whipple 1983; Ryabova 2012). ( ) Ryabova et al. 2019 , though the chaotic nature of orbits in However, very low levels of activity centered on just a few * days around perihelion are too low to explain the observed Partially based on data collected with 2 m RCC telescope at Rozhen National Geminid meteor flux (Li & Jewitt 2013). Phaethon is also Astronomical Observatory. considered to be the parent of three other meteor streams, all belonging to the Geminid meteor complex. These streams Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further correspond to the intersection of the orbit of the Earth with that distribution of this work must maintain attribution to the author(s) and the title of Phaethon’s at different epochs (Babadzhanov & Obrubov of the work, journal citation and DOI. 1987; Jakubík & Neslušan 2015). However, one of these 1 The Planetary Science Journal, 1:15 (15pp), 2020 June Devogèle et al. Table 1 D∼5 km. These discrepancies in albedo and size could result Osculating Orbital Elements of Phaethon and Its Two Companions 2005 UD from Phaethon having an uncommon or inhomogeneous and 1999 YC at Epoch 59,000.0 MJD Obtained with the JPL Horizons Service surface. Variation of the linear degree of polarization was Phaethon 2005 UD 1999 YC indeed observed as a function of the rotation phase suggesting ( a ( ) that the surface of Phaethon is not uniform Borisov et al. 2018; au 1.271 1.275 1.422 ) e 0.890 0.872 0.831 Devogèle et al. 2018 . i (°) 22.259 28.668 38.232 The spectrum of Phaethon displays a blue slope compatible ω (°) 265.2 19.7 64.8 with a B-type taxonomy in the Bus and Binzel (visible; Bus & Ω (°) 322.2 207.6 156.4 Binzel 2002) and Bus-DeMeo (NIR inclusive; DeMeo et al. 2009) systems. Spectral variation with rotation was found by Kareta et al. (2018), however, with marginal significance. Phaethon is the target of the Japanese Aerospace Exploration streams, the daytime Sextantids, seems to be more closely Agency’s Demonstration and Experiment of Space Technology ( ) related to UD than it is to Phaethon Ohtsuka et al. 2005, 2006 . for INterplanetary voYage Phaethon fLyby dUSt science Phaethon and UD are also dynamically associated with ( +) ( ) ( DESTINY mission. It is planned to launch in 2022 and another asteroid, 225416 1999 YC Kasuga & Jewitt 2008, will perform a high-speed fly by of Phaethon (Arai et al. 2018). ) + hereafter YC . However, while Phaethon and UD display A possible mission extension for DESTINY would be a flyby photometric colors and spectra indicative of a blue slope and a of UD. As a result, ground-based campaigns of telescopic B-type spectral classification, YC shows redder colors more observations focused on both objects have been organized for consistent with a C-type classification (Kasuga & Jewitt 2008). mission preparation purposes. In this work, we present Table 1 compares the orbital elements of the parent body photometric, spectroscopic, and polarimetric results for UD Phaethon with its two putative family members UD and YC. and discuss its relation with its suspected parent body, Though the current osculating orbital elements of Phaethon and UD are different, particularly the longitude of ascending node Phaethon. and the argument of perihelion angles, they display similar In the next section, we present a summary of our secular variations in orbital elements with a time lag observations of UD in photometry, spectroscopy, and polari- Δt∼4600 yr (Ohtsuka et al. 2006). This means that ∼4600 metry. We also detail the thermal data used from NEOWISE. yr ago, the orbital elements of Phaethon were similar to those For each technique, the data acquisition and reduction of UD today. In the case of YC, the semimajor axis is procedures are detailed. Section 3 is devoted to discussion of significantly different from that of Phaethon and UD. If YC is the results from each technique. From the photometry, we genetically related to Phaethon and UD, these differences can discuss the rotation period and pole determination of UD. As only be explained if the orbit of YC was perturbed during a our observations span a large range of phase angles, we also close planetary encounter (Ohtsuka et al. 2008). If these three determined the photometric phase curve, estimation of the asteroids are actually related, their formation mechanism is absolute H magnitude, size of UD, and the variation of the unclear and could involve YORP spin-up and fission (Pravec amplitude as a function of the phase angle. The visible et al. 2010), impacts with other asteroids, or thermally driven spectroscopy allowed us to determine the taxonomic type of separation during a perihelion passage (Granvik et al. 2016). UD and compare it with the spectrum of Phaethon. Polarimetric Phaethon has been the subject of many studies to understand observations allowed for characterization of the phase-polar- its physical properties.
Load more

Recommended publications
  • (101955) Bennu from OSIRIS-Rex Imaging and Thermal Analysis
    ARTICLES https://doi.org/10.1038/s41550-019-0731-1 Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis D. N. DellaGiustina 1,26*, J. P. Emery 2,26*, D. R. Golish1, B. Rozitis3, C. A. Bennett1, K. N. Burke 1, R.-L. Ballouz 1, K. J. Becker 1, P. R. Christensen4, C. Y. Drouet d’Aubigny1, V. E. Hamilton 5, D. C. Reuter6, B. Rizk 1, A. A. Simon6, E. Asphaug1, J. L. Bandfield 7, O. S. Barnouin 8, M. A. Barucci 9, E. B. Bierhaus10, R. P. Binzel11, W. F. Bottke5, N. E. Bowles12, H. Campins13, B. C. Clark7, B. E. Clark14, H. C. Connolly Jr. 15, M. G. Daly 16, J. de Leon 17, M. Delbo’18, J. D. P. Deshapriya9, C. M. Elder19, S. Fornasier9, C. W. Hergenrother1, E. S. Howell1, E. R. Jawin20, H. H. Kaplan5, T. R. Kareta 1, L. Le Corre 21, J.-Y. Li21, J. Licandro17, L. F. Lim6, P. Michel 18, J. Molaro21, M. C. Nolan 1, M. Pajola 22, M. Popescu 17, J. L. Rizos Garcia 17, A. Ryan18, S. R. Schwartz 1, N. Shultz1, M. A. Siegler21, P. H. Smith1, E. Tatsumi23, C. A. Thomas24, K. J. Walsh 5, C. W. V. Wolner1, X.-D. Zou21, D. S. Lauretta 1 and The OSIRIS-REx Team25 Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the for- mation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA’s Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid (101955) Bennu’s surface is globally rough, dense with boulders, and low in albedo.
    [Show full text]
  • The Opposition and Tilt Effects of Saturn's Rings from HST Observations
    The opposition and tilt effects of Saturn’s rings from HST observations Heikki Salo, Richard G. French To cite this version: Heikki Salo, Richard G. French. The opposition and tilt effects of Saturn’s rings from HST observa- tions. Icarus, Elsevier, 2010, 210 (2), pp.785. 10.1016/j.icarus.2010.07.002. hal-00693815 HAL Id: hal-00693815 https://hal.archives-ouvertes.fr/hal-00693815 Submitted on 3 May 2012 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Accepted Manuscript The opposition and tilt effects of Saturn’s rings from HST observations Heikki Salo, Richard G. French PII: S0019-1035(10)00274-5 DOI: 10.1016/j.icarus.2010.07.002 Reference: YICAR 9498 To appear in: Icarus Received Date: 30 March 2009 Revised Date: 2 July 2010 Accepted Date: 2 July 2010 Please cite this article as: Salo, H., French, R.G., The opposition and tilt effects of Saturn’s rings from HST observations, Icarus (2010), doi: 10.1016/j.icarus.2010.07.002 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript.
    [Show full text]
  • Extended Mission Orbit #2 (XMO2, ~1500 Km Altitude)
    Carol A. Raymond Deputy Principal Investigator SBAG 17 Jet Propulsion Laboratory, Caltech 13 Jun 2017 • Spacecraft and instruments are healthy and data return has been excellent to date • Primary mission ended on June 30 2016. All mission objectives and Level-1 requirements were met. • Extended mission at Ceres ends June 30 2017. All mission objectives and Level-1 requirements were met. • Primary mission data archive complete pending ongoing review; extended mission archive is up to date • NASA is considering options for continued operations beyond June 2017 2 • Loss of third reaction wheel on April 23rd limits Dawn’s lifetime – but otherwise does not affect the mission – dependent on hydrazine jets for attitude control – Lifetime decreases with orbit altitude • Dawn is currently in a ~20000x50000 km eccentric orbit • Recently performed opposition observation • Four special journal issues in work: – Icarus: Geological Mapping (in revision) – Icarus: Mineralogical Mapping (submitted) – MAPS: Composition/Crosscutting (in submission) – Icarus: Occator Crater (in progress) – Interest in a special issue on ground ice: contact Britney Schmidt if you would like to participate 3 Ceres Extended Mission Timeline Start of End of End of Extended Mission Extended Mission Project Operations Operations XM1 Science Plan Extended Mission Orbit #1 (XMO1, ~385 km altitude) • Obtain IR spectra of high-priority targets (VIR) ✓ • Expand high-resolution color imaging (FC) ✓ • Improve elemental mapping (GRaND) ✓ • Expand high-resolution surface coverage for topography
    [Show full text]
  • A Tale of Two Sides: Pluto's Opposition Surge in 2018 and 2019
    EPSC Abstracts Vol. 14, EPSC2020-546, 2020, updated on 27 Sep 2021 https://doi.org/10.5194/epsc2020-546 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. A Tale of Two Sides: Pluto's Opposition Surge in 2018 and 2019 Anne Verbiscer1, Paul Helfenstein2, Mark Showalter3, and Marc Buie4 1University of Virginia, Charlottesville, VA, USA ([email protected]) 2Cornell University, Ithaca, NY, USA ([email protected]) 3SETI Institute, Mountain View, CA, USA ([email protected]) 4Southwest Research Institute, Boulder, CO, USA ([email protected]) Near-opposition photometry employs remote sensing observations to reveal the microphysical properties of regolith-covered surfaces over a wide range of solar system bodies. When aligned directly opposite the Sun, objects exhibit an opposition effect, or surge, a dramatic, non-linear increase in reflectance seen with decreasing solar phase angle (the Sun-target-observer angle). This phenomenon is a consequence of both interparticle shadow hiding and a constructive interference phenomenon known as coherent backscatter [1-3]. While the size of the Earth’s orbit restricts observations of Pluto and its moons to solar phase angles no larger than α = 1.9°, the opposition surge, which occurs largely at α < 1°, can discriminate surface properties [4-6]. The smallest solar phase angles are attainable at node crossings when the Earth transits the solar disk as viewed from the object. In this configuration, a solar system body is at “true” opposition. When combined with observations acquired at larger phase angles, the resulting reflectance measurement can be related to the optical, structural, and thermal properties of the regolith and its inferred collisional history.
    [Show full text]
  • Near-Infrared Photometry of Mercury Richard W
    Georgia Journal of Science Volume 76 No.2 Scholarly Contributions from the Article 4 Membership and Others 2018 Near-Infrared Photometry of Mercury Richard W. Schmude Jr. Gordon State College, [email protected] Follow this and additional works at: https://digitalcommons.gaacademy.org/gjs Recommended Citation Schmude, Richard W. Jr. (2018) "Near-Infrared Photometry of Mercury," Georgia Journal of Science, Vol. 76, No. 2, Article 4. Available at: https://digitalcommons.gaacademy.org/gjs/vol76/iss2/4 This Research Articles is brought to you for free and open access by Digital Commons @ the Georgia Academy of Science. It has been accepted for inclusion in Georgia Journal of Science by an authorized editor of Digital Commons @ the Georgia Academy of Science. Near-Infrared Photometry of Mercury Acknowledgements I am grateful to Gordon State College for a Faculty Development Grand which was awarded in 2014 and enabled me to purchase the SSP-4 photometer. This research articles is available in Georgia Journal of Science: https://digitalcommons.gaacademy.org/gjs/vol76/iss2/4 Schmude: Near-Infrared Photometry of Mercury NEAR-INFRARED PHOTOMETRY OF MERCURY Richard W. Schmude, Jr. Gordon State College ABSTRACT This report summarizes 100 brightness measurements of Mercury made between May 2014 and September 2017 in the J and H near-infrared filters. Brightness models are reported for the J (solar phase angles between 52.3° and 124.5°) and H (solar phase angles between 38.6° and 133.0°) filters. Additional conclusions are as follows: Mercury’s brightness is within 0.1 magnitudes, at a given phase angle, for waxing and waning phases, and the geometric albedos at a solar phase angle of 0° are estimated to be 0.16 ± 0.03 and 0.24 ± 0.05 for the J and H filters, respectively.
    [Show full text]
  • Brightness of Saturn's Rings with Decreasing Solar Elevation
    Planetary and Space Science 58 (2010) 1758–1765 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Brightness of Saturn’s rings with decreasing solar elevation Alberto Flandes a,Ã, Linda Spilker a, Ryuji Morishima a, Stuart Pilorz b,Ce´dric Leyrat c, Nicolas Altobelli d, Shawn Brooks a, Scott G. Edgington a a Jet Propulsion Laboratory/California Institute of Technology, Pasadena, USA b SETI Institute, Mountain View, USA c Observatoire de Paris-LESIA, France d European Space and Astronomy Center, European Space Agency (ESAC/ESA), Madrid, Spain article info abstract Article history: Early ground-based and spacecraft observations suggested that the temperature of Saturn’s main rings Received 5 January 2010 (A, B and C) varied with the solar elevation angle, B0. Data from the composite infrared spectrometer Received in revised form (CIRS) on board Cassini, which has been in orbit around Saturn for more than five years, confirm this 31 March 2010 variation and have been used to derive the temperature of the main rings from a wide variety of Accepted 6 April 2010 geometries while B0 varied from near À243 to 03 (Saturn’s equinox). Available online 18 April 2010 Still, an unresolved issue in fully explaining this variation relates to how the ring particles are Keywords: organized and whether even a simple mono-layer or multi-layer approximation describes this best. We Planetary rings present a set of temperature data of the main rings of Saturn that cover the 233Frange of B0 angles Rings of Saturn 3 3 obtained with CIRS at low (a 30 ) and high (aZ120 ) phase angles.
    [Show full text]
  • Opposition Effect on Comet 67P/Churyumov-Gerasimenko Using Rosetta-OSIRIS Images
    Opposition effect on comet 67P/Churyumov-Gerasimenko using Rosetta-OSIRIS images Nafiseh Masoumzadeh, Nilda Oklay, Ludmilla Kolokolova, Holger Sierks, Sonia Fornasier, Maria A. Barucci, Jean-Baptiste Vincent, Cécilia Tubiana, Carsten Güttler, Frank Preusker, et al. To cite this version: Nafiseh Masoumzadeh, Nilda Oklay, Ludmilla Kolokolova, Holger Sierks, Sonia Fornasier, etal..Op- position effect on comet 67P/Churyumov-Gerasimenko using Rosetta-OSIRIS images. Astronomy and Astrophysics - A&A, EDP Sciences, 2017, 599, A11 (8 p.). 10.1051/0004-6361/201629734. insu-01473386 HAL Id: insu-01473386 https://hal-insu.archives-ouvertes.fr/insu-01473386 Submitted on 16 Sep 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 599, A11 (2017) Astronomy DOI: 10.1051/0004-6361/201629734 & © ESO 2017 Astrophysics Opposition effect on comet 67P/Churyumov-Gerasimenko using Rosetta-OSIRIS images N. Masoumzadeh1;? , N. Oklay1, L. Kolokolova11, H. Sierks1, S. Fornasier13, M. A. Barucci13, J.-B. Vincent1, C. Tubiana1, C. Güttler1, F. Preusker22, F. Scholten22, S. Mottola22, P. H. Hasselmann13, C. Feller13, C. Barbieri4, P. L. Lamy5, R. Rodrigo6; 7, D. Koschny8, H. Rickman9; 10, M. F. A’Hearn11; 12; 1, J.-L. Bertaux14, I.
    [Show full text]
  • Astronomy & Astrophysics Detailed Phase
    A&A 376, 672–685 (2001) Astronomy DOI: 10.1051/0004-6361:20011028 & c ESO 2001 Astrophysics Detailed phase function of comet 28P/Neujmin 1? C. E. Delahodde1,2,K.J.Meech3,O.R.Hainaut1, and E. Dotto4 1 European Southern Observatory, Casilla 19001, Santiago, Chile 2 Institut d’Astrophysique de Marseille, Traverse du Siphon, 13376 Marseille Cedex 12, France 3 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 4 Osservatorio Astronomico di Torino, Strada Osservatorio 20, 100025 Pino Torinese (TO), Italy Received 11 April 2001 / Accepted 10 July 2001 Abstract. In 2000, comet 28P/Neujmin 1 was an ideal candidate for a phase function study: during its April opposition it reached a phase angle of α =0.8◦, and previous observations at similar heliocentric distances (r ≥ 4 AU) indicated that the comet was likely to be inactive. We observed this comet using ESO’s NTT and 2.2m telescopes at La Silla, on 6 epochs from April to August 2000, covering α = 0.8–8◦. These data were combined with a large set of data from 1985 to 1997. In order to disentangle the rotation effects from the phase effects, we obtained complete rotation coverage at opposition, providing us with a lightcurve template. We have obtained an improved rotation period of 12.75 0.03 hrs, with a full amplitude of ∆m =0.45 0.05 mag, which yields an axis ratio lower limit of 1.51 0.07. For each subsequent epochs, we have obtained enough rotation coverage to re-synchronize the lightcurve fragments with the template, and determine the magnitude change caused by the phase function.
    [Show full text]
  • Spectrogoniometry and Modeling of Martian and Lunar Analog Samples and Apollo Soils ⇑ Jeffrey R
    Icarus 223 (2013) 383–406 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Spectrogoniometry and modeling of martian and lunar analog samples and Apollo soils ⇑ Jeffrey R. Johnson a, , Michael K. Shepard b, William M. Grundy c, David A. Paige d, Emily J. Foote d a Johns Hopkins University Applied Physics Laboratory, 11101 Johns Hopkins Road, 200-W230, Laurel, MD 20723-6005, United States b Bloomsburg University, 400 East Second St., Bloomsburg, PA 89557, United States c Lowell Observatory, 1400 West Mars Hill Rd., Flagstaff, AZ 86001, United States d University of California, Los Angeles, 595 Charles Young Drive East, Box 951567, Los Angeles, CA 90095-1567, United States article info abstract Article history: We present new visible/near-infrared multispectral reflectance measurements of seven lunar soil simu- Received 17 May 2012 lants, two Apollo soils, and eight martian analog samples as functions of illumination and emission angles Revised 19 November 2012 using the Bloomsburg University Goniometer. By modeling these data with Hapke theory, we provide Accepted 4 December 2012 constraints on photometric parameters (single scattering albedo, phase function parameters, macro- Available online 19 December 2012 scopic roughness, and opposition effect parameters) to provide additional ‘‘ground truth’’ photometric properties to assist analyses of spacecraft data. A wide range of modeled photometric properties were Keywords: variably related to albedo, color, grain size, and surface texture. Finer-grained samples here have high Spectrophotometry single-scattering albedo values compared to their coarser-grained counterparts, as well as lower macro- Regoliths Mars, Surface scopic roughness values. The Mars analog samples and Apollo soils exhibit slightly lower opposition Moon, Surface effect width parameter values than the lunar analogs, whereas the opposition effect magnitude is not Radiative transfer well constrained by the models.
    [Show full text]
  • Photometric Correction of Chang'e-1 Interference Imaging
    remote sensing Technical Note Photometric Correction of Chang’E-1 Interference Imaging Spectrometer’s (IIM) Limited Observing Geometries Data with Hapke Model Xuesen Xu 1,2,3 , Jianjun Liu 2,*, Dawei Liu 2, Bin Liu 2 and Rong Shu 1,3 1 School of Physics and Optoelectronic Engineering, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310024, China; [email protected] (X.X.); [email protected] (R.S.) 2 Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; [email protected] (D.L.); [email protected] (B.L.) 3 Key Laboratory of Space Active Opto-Electronics Technology, Chinese Academy of Sciences, Shanghai 200083, China * Correspondence: [email protected] Received: 2 September 2020; Accepted: 4 November 2020; Published: 10 November 2020 Abstract: The main objective of this study is to develop a Hapke photometric model that is suited for Chang’E-1 (CE-1) Interference Imaging Spectrometer (IIM) data. We first divided the moon into three areas including ‘maria’, ‘new highland’ and old ‘highland’ with similar photometry characteristic based on the Hapke parameters of the moon derived from Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera (WAC) multispectral data. Then, we selected the sample data in the ‘maria’ area and obtained a new set of Hapke model’s parameters that can best fit these data. Result shows that photometric correction using Hapke model with these new derived parameters can eliminate the effect of variations in viewing and luminating geometry, especially ‘opposition surge’, more efficiently than the empirical model.
    [Show full text]
  • An Example Based on Lunar Photometry
    Local topographic effects on photometry and reflectance spectra of planetary surfaces: An example based on lunar photometry Item Type Article; text Authors Domingue, D.; Vilas, F. Citation Domingue, D., & Vilas, F. (2007). Local topographic effects on photometry and reflectance spectra of planetary surfaces: An example based on lunar photometry. Meteoritics & Planetary Science, 42(10), 1801-1816. DOI 10.1111/j.1945-5100.2007.tb00539.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 26/09/2021 09:57:10 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656345 Meteoritics & Planetary Science 42, Nr 10, 1801–1816 (2007) Abstract available online at http://meteoritics.org Local topographic effects on photometry and reflectance spectra of planetary surfaces: An example based on lunar photometry Deborah DOMINGUE1* and Faith VILAS2† 1Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, Maryland 20723, USA 2Planetary Astronomy Group, Astromaterials Research and Exploration Science, NASA Johnson Space Center/KR, Houston, Texas 77058, USA †Present address: MMT Observatory, P.O. Box 210065, The University of Arizona, Tucson, Arizona 85721–0065, USA *Corresponding author. E-mail: [email protected] (Received 22 May 2006; revision accepted 19 April 2007) Abstract–The photometric properties of the average lunar surface are characterized using Hapke’s equations and whole disk observations ranging from 0.36 to 1.06 μm. Synthetic spectra across a crater topographic profile are created using the modeling results. The synthetic spectra are examined for spectral variations created by changes in lighting conditions induced by the topography.
    [Show full text]
  • Photometric Properties of Ceres from Telescopic Observations Using Dawn Framing Camera Color Filters
    Photometric Properties of Ceres from Telescopic Observations using Dawn Framing Camera Color Filters Vishnu Reddy Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Email: [email protected] Jian-Yang Li Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Bruce L. Gary Hereford Arizona Observatory, Hereford, Arizona, USA Juan A. Sanchez Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Robert D. Stephens Center for Solar System Studies, Landers, California, USA Ralph Megna Riverside Astronomical Society, Riverside, California, USA Daniel Coley Center for Solar System Studies, Landers, California, USA Andreas Nathues Max-Planck Institute for Solar System Research, Goettingen, Germany Lucille Le Corre Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Martin Hoffmann Max-Planck Institute for Solar System Research, Goettingen, Germany Pages: 40 Figures: 9 Tables: 5 1 Proposed Running Head: Ceres Photometry Dawn Editorial correspondence to: Vishnu Reddy Planetary Science Institute 1700 East Fort Lowell Road, Suite 106 Tucson 85719 (808) 342-8932 (voice) [email protected] 2 Abstract The dwarf planet Ceres is likely differentiated similar to the terrestrial planets but with a water/ice dominated mantle and an aqueously altered crust. Detailed modeling of Ceres’ phase function has never been performed to understand its surface properties. The Dawn spacecraft began orbital science operations at the dwarf planet in April 2015. We observed Ceres with flight spares of the seven Dawn Framing Camera color filters mounted on ground-based telescopes over the course of three years to model its phase function versus wavelength.
    [Show full text]