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The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
Sesquicentennial!
Sesquicentennial! Canada's Amazing Astronomy/Space Achievements 1867-2017 ----- John Percy Department of Astronomy & Astrophysics and OISE/UT University of Toronto My History with Schools and STAO ● Faculty of Ed (1963-4) ● Bloor CI (1964-5) ● Member of STAO (1971-) ● Consulting with the Ministry, textbook publishers, STAO projects, giving workshops etc. (1971-) ● STAO Honorary President (1988-91) ● STAO Service Award (1991) ● STAO Jack Bell Award (1999) Why Teach/Learn Astronomy/Science? Awareness of science Interest in science Understanding of science Appreciation of science Engagement in science Attitude to science Skills in science Science in culture Major Grade Nine Expectation “Students will … identify scientists, including Canadians, who have made contributions to (astronomy/space).” Specifically: “Assess, on the basis of research, and report on the contributions of Canadian governments, organizations, businesses, and/or individuals...” [also grade six 1.1, SES4U: A2.2, B1] ----- STSE: Connects with history, economics, politics ----- This becomes a typical assignment/assessment: research and report, using all relevant scientific skills, on these contributions, and why they are significant Practical Astronomy/Space Practical astronomy: “describe various reasons that humankind has had for studying (astronomy/space)...” 5 In the beginning ..... sky motions provided a clock, calendar, and compass for both pre-technological and technological societies. Students can make these observations! Spacebanter.com 6 Aboriginal Astronomy First Nations people used the sky as a clock, calendar, and compass, and incorporated the sky into their culture and spirituality, as they still do Cheryl Bartlett, co-developer of Integrative Science 7 Practical Astronomy: to 1850 “by the Mother Country, for the Mother Country” In locations across the country, simple instruments were used for.. -
Constraining Mineralogical Composition of Asteroid Ryugu with Ground-Based Observations
Constraining Mineralogical Composition of Asteroid Ryugu with Ground-Based Observations Lucille Le Corre1, Vishnu Reddy2, Juan A. Sanchez1, Driss Takir3, Ed A. Cloutis4, Audrey Thirouin5, Jian-Yang Li1, Seiji Sugita6, Eri Tatsumi6. 1Planetary Science Institute, Tucson, Arizona, USA 2Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA 3SETI Institute, Mountain View, CA, USA 4Department of Geography, University of Winnipeg, Winnipeg, Manitoba, Canada 5Lowell Observatory, Flagstaff, AZ, USA 6Dept. of Earth and Planetary Science, University of Tokyo, Tokyo, Japan In preparation for the arrival of the Japanese Space Agency’s (JAXA) Hayabusa2 sample return mission to near-Earth asteroid (NEA) (162173) Ryugu, we took the opportunity to characterize the target with a ground-based telescope. We observed Ryugu using the SpeX instrument in Prism mode on NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, on July, 12 2016 when the asteroid was 18.87 visual magnitude, at a phase angle of 13.3°. The NIR spectra were used to constrain Ryugu’s surface composition, determine meteorite analogs and study spectral affinity to other asteroids. We also modeled its photometric properties using archival data. Using the Lommel-Seeliger model we computed the predicted flux for Ryugu at a wide range of viewing geometries as well as albedo quantities such as geometric albedo, phase integral, and spherical Bond albedo. Our computed albedo quantities are consistent with results from Ishiguro et al. (2014). In previous work, Ryugu’s visible spectrum revealed that it can be classified as a C-type object. In addition, not all previous ground-based observations of Ryugu detected the 0.7 µm absorption feature due to the presence of phyllosilicates. -
Nature of Bright C-Complex Asteroids
Publ. Astron. Soc. Japan (2014) 00(0), 1–20 1 doi: 10.1093/pasj/xxx000 Nature of bright C-complex asteroids Sunao HASEGAWA,1,* Toshihiro KASUGA,2 Fumihiko USUI,3 and Daisuke KURODA4 1Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara 252-5210, Japan 2Public Relations Center, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan 3Center for Planetary Science, Graduate School of Science, Kobe University, 7-1-48, Minatojima-minamimachi, Chuo-Ku, Kobe 650-0047, Japan 4Okayama Astronomical Observatory, Graduate School of Science, Kyoto University, 3037-5 Honjo, Kamogata-cho, Asakuchi, Okayama 719-0232, Japan ∗E-mail: [email protected] Received ; Accepted Abstract Most C-complex asteroids have albedo values less than 0.1, but there are some high-albedo (bright) C-complex asteroids with albedo values exceeding 0.1. To reveal the nature and origin of bright C-complex asteroids, we conducted spectroscopic observations of the asteroids in visible and near-infrared wavelength regions. As a result, the bright B-, C-, and Ch-type (Bus) asteroids, which are subclasses of the Bus C-complex, are classified as DeMeo C-type aster- oids with concave curvature, B-, Xn-, and K-type asteroids. Analogue meteorites and material (CV/CK chondrites, enstatite chondrites/achondrites, and salts) associated with these spec- tral types of asteroids are thought to be composed of minerals and material exposed to high temperatures. A comparison of the results obtained in this study with the SDSS photometric data suggests that salts may have occurred in the parent bodies of 24 Themis and 10 Hygiea, as well as 2 Pallas. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
The Minor Planet Bulletin 37 (2010) 45 Classification for 244 Sita
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 2, A.D. 2010 APRIL-JUNE 41. LIGHTCURVE AND PHASE CURVE OF 1130 SKULD Robinson (2009) from his data taken in 2002. There is no evidence of any change of (V-R) color with asteroid rotation. Robert K. Buchheim Altimira Observatory As a result of the relatively short period of this lightcurve, every 18 Altimira, Coto de Caza, CA 92679 (USA) night provided at least one minimum and maximum of the [email protected] lightcurve. The phase curve was determined by polling both the maximum and minimum points of each night’s lightcurve. Since (Received: 29 December) The lightcurve period of asteroid 1130 Skuld is confirmed to be P = 4.807 ± 0.002 h. Its phase curve is well-matched by a slope parameter G = 0.25 ±0.01 The 2009 October-November apparition of asteroid 1130 Skuld presented an excellent opportunity to measure its phase curve to very small solar phase angles. I devoted 13 nights over a two- month period to gathering photometric data on the object, over which time the solar phase angle ranged from α = 0.3 deg to α = 17.6 deg. All observations used Altimira Observatory’s 0.28-m Schmidt-Cassegrain telescope (SCT) working at f/6.3, SBIG ST- 8XE NABG CCD camera, and photometric V- and R-band filters. Exposure durations were 3 or 4 minutes with the SNR > 100 in all images, which were reduced with flat and dark frames. -
Occultation Newsletter Volume 8, Number 4
Volume 9, Number 2 May 2002 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Articles Page (701) Oriola observations (4/21/2002) . .. 4 The Newly Confirmed Binary Star, 43 Tau or Zodiacal Catalog 614 . 5 Uncertainty Is Not the Same As Standard Error . .. 5 The Spectacular Grazing Occultation of Jupiter On August 18, 1990 . 7 Occultations and Small Bodies . .. .. 8 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . 13 IOTA European Section (IOTA/ES) . 13 IOTA on the World Wide Web. Back Cover IOTA’s Telephone Network . Back Cover ON THE COVER: A drawing of chords from the data obtained during the Occultation of HIP 19388 by 345 Tercidina. Image from http://sorry.vse.cz/~ludek/mp/results/ A WWW page maintained by Jan Manek, [email protected] Publication Date: December 2002 2 Occultation Newsletter, Volume 9, Number 2; May 2002 International Occultation Timing Association, Inc. (IOTA) What to Send to Whom Membership and Subscription Information All payments made to IOTA must be in United States Send new and renewal memberships and subscriptions, back funds and drawn on a US bank, or by credit card charge to issue requests, address changes, email address changes, graze VISA or MasterCard. If you use VISA or MasterCard, include prediction requests, reimbursement requests, special requests, your account number, expiration date, and signature. (Do not and other IOTA business, but not observation reports, to: send credit card information through e-mail. It is neither secure Art Lucas nor safe to do so.) Make all payments to IOTA and send them Secretary & Treasurer to the Secretary & Treasurer at the address on the left. -
The Minor Planet Bulletin Is Open to Papers on All Aspects of 6500 Kodaira (F) 9 25.5 14.8 + 5 0 Minor Planet Study
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 32, NUMBER 3, A.D. 2005 JULY-SEPTEMBER 45. 120 LACHESIS – A VERY SLOW ROTATOR were light-time corrected. Aspect data are listed in Table I, which also shows the (small) percentage of the lightcurve observed each Colin Bembrick night, due to the long period. Period analysis was carried out Mt Tarana Observatory using the “AVE” software (Barbera, 2004). Initial results indicated PO Box 1537, Bathurst, NSW, Australia a period close to 1.95 days and many trial phase stacks further [email protected] refined this to 1.910 days. The composite light curve is shown in Figure 1, where the assumption has been made that the two Bill Allen maxima are of approximately equal brightness. The arbitrary zero Vintage Lane Observatory phase maximum is at JD 2453077.240. 83 Vintage Lane, RD3, Blenheim, New Zealand Due to the long period, even nine nights of observations over two (Received: 17 January Revised: 12 May) weeks (less than 8 rotations) have not enabled us to cover the full phase curve. The period of 45.84 hours is the best fit to the current Minor planet 120 Lachesis appears to belong to the data. Further refinement of the period will require (probably) a group of slow rotators, with a synodic period of 45.84 ± combined effort by multiple observers – preferably at several 0.07 hours. The amplitude of the lightcurve at this longitudes. Asteroids of this size commonly have rotation rates of opposition was just over 0.2 magnitudes. -
I N S I D E T H I S I S S
February / février 2008 Volume/volume 102 Number/numéro 1 [728] This Issue's Winning Astrophoto! FEATURING A FULL COLOUR SECTION! The Journal of the Royal Astronomical Society of Canada Cassiopeia Rising Over the Plaskett by Charles Banville, Victoria Centre. This is a montage of two pictures I took using a Canon 20Da and a Canon EF 17-40mm f/4L lens. The foreground image was acquired at the Dominion Astrophysical Observatory in Victoria on 2007 July 26. That evening the Plaskett Dome was illuminated by a bright 12-day-old Moon. The star trails were created using 87 light frames of 1 minute each taken from Cattle Point on 2007 August 8. Le Journal de la Société royale d’astronomie du Canada [Editor’s Note: The two-member team of Dietmar Kupke and Paul Mortfield of the Toronto Centre selected this late-entry image from among the 30 or so entries to the “Own the Back Cover” con- test. Thanks to all the submitters. We welcome further entries, so don’t delay – send in yours now! INSIDE THIS ISSUE Watch the back cover of the April issue for the next winner.] One Hundred Editions of the Observer's Handbook · Seriously Seeking Ceres! Mont-Mégantic Dark-Sky Reserve Conference, 2007 September 19-21 Duplicity of ZC1042: My First Double-Star Discovery In Memory of Gertrude Jean Southam Building for the International Year of Astronomy (IYA2009) THE ROYAL ASTRONOMICAL SOCIETY OF CANADA February / février 2008 NATIONAL OFFICERS AND COUNCIL FOR 2007-2008/CONSEIL ET ADMINISTRATEURS NATIONAUX Honorary President Robert Garrison, Ph.D., Toronto President Scott Young, B.Sc., Winnipeg Vol. -
The Minor Planet Bulletin 36, 188-190
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 3, A.D. 2010 JULY-SEPTEMBER 81. ROTATION PERIOD AND H-G PARAMETERS telescope (SCT) working at f/4 and an SBIG ST-8E CCD. Baker DETERMINATION FOR 1700 ZVEZDARA: A independently initiated observations on 2009 September 18 at COLLABORATIVE PHOTOMETRY PROJECT Indian Hill Observatory using a 0.3-m SCT reduced to f/6.2 coupled with an SBIG ST-402ME CCD and Johnson V filter. Ronald E. Baker Benishek from the Belgrade Astronomical Observatory joined the Indian Hill Observatory (H75) collaboration on 2009 September 24 employing a 0.4-m SCT PO Box 11, Chagrin Falls, OH 44022 USA operating at f/10 with an unguided SBIG ST-10 XME CCD. [email protected] Pilcher at Organ Mesa Observatory carried out observations on 2009 September 30 over more than seven hours using a 0.35-m Vladimir Benishek f/10 SCT and an unguided SBIG STL-1001E CCD. As a result of Belgrade Astronomical Observatory the collaborative effort, a total of 17 time series sessions was Volgina 7, 11060 Belgrade 38 SERBIA obtained from 2009 August 20 until October 19. All observations were unfiltered with the exception of those recorded on September Frederick Pilcher 18. MPO Canopus software (BDW Publishing, 2009a) employing 4438 Organ Mesa Loop differential aperture photometry, was used by all authors for Las Cruces, NM 88011 USA photometric data reduction. The period analysis was performed using the same program. David Higgins Hunter Hill Observatory The data were merged by adjusting instrumental magnitudes and 7 Mawalan Street, Ngunnawal ACT 2913 overlapping characteristic features of the individual lightcurves. -
The Minor Planet Bulletin (Warner Et Al
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 35, NUMBER 4, A.D. 2008 OCTOBER-DECEMBER 143. THE LIGHTCURVE OF ASTEROID 5331 ERIMOMISAKI 05 and Jan 09, respectively. The Vincent data were taken under poor conditions, which is reflected by the large error bars. Caleb Boe, Russell I. Durkee However, the data support the proposed period and were crucial in Shed of Science Observatory completing the curve. Analysis was performed using MPO 5213 Washburn Ave S. Minneapolis, MN 55410, USA Canopus. Silvano Casulli Acknowledgments Vallemare Di Borbona Observatory, Vallemare di Borbona, ITALY Thanks to Raoul Behrend for posting Casulli’s results on his website and for coordinating the exchange of data. Dr. Fiona Vincent School of Physics & Astronomy Special thanks to the Tzec Maun Foundation and its founder, University of St. Andrews Michael K. Wilson, for providing free access to telescopes for North Haugh, St. Andrews KY16 9SS, Scotland, UK students and researchers. David Higgins References Hunters Hill Observatory Ngunnawal, Canberra 2913 Behrend, R. (2007). Observatoire de Geneve web site, AUSTRALIA http://obswww.unige.ch/~behrend/page1cou.html (Received: 2008 June 1) Warner, B.D., Harris A.W. , Pravec, P. Kaasalainen, M., and Benner, L.A.M. (2007). Lightcurve Photometry Opportunities October-December 2007 Asteroid 5331 Erimomisaki was observed between 2007 http://minorplanetobserver.com/astlc/default.htm Nov. 30 and 2008 Jan. 9. A synodic period of 24.26 ± 0.02 h with a mean amplitude of 0.27 ± 0.02 mag was derived. Observations of 5331 Erimomisaki were carried out over ten nights between 2007 November and 2008 January. -
The Minor Planet Bulletin (Warner Et 2010 JL33
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 3, A.D. 2011 JULY-SEPTEMBER 127. ROTATION PERIOD DETERMINATION FOR 280 PHILIA – the lightcurve more readable these have been reduced to 1828 A TRIUMPH OF GLOBAL COLLABORATION points with binning in sets of 5 with time interval no greater than 10 minutes. Frederick Pilcher 4438 Organ Mesa Loop MPO Canopus software was used for lightcurve analysis and Las Cruces, NM 88011 USA expedited the sharing of data among the collaborators, who [email protected] independently obtained several slightly different rotation periods. A synodic period of 70.26 hours, amplitude 0.15 ± 0.02 Vladimir Benishek magnitudes, represents all of these fairly well, but we suggest a Belgrade Astronomical Observatory realistic error is ± 0.03 hours rather than the formal error of ± 0.01 Volgina 7, 11060 Belgrade 38, SERBIA hours. Andrea Ferrero The double period 140.55 hours was also examined. With about Bigmuskie Observatory (B88) 95% phase coverage the two halves of the lightcurve looked the via Italo Aresca 12, 14047 Mombercelli, Asti, ITALY same as each other and as in the 70.26 hour lightcurve. Furthermore for order through 14 the coefficients of the odd Hiromi Hamanowa, Hiroko Hamanowa harmonics were systematically much smaller than for the even Hamanowa Astronomical Observatory harmonics. A 140.55 hour period can be safely rejected. 4-34 Hikarigaoka Nukazawa Motomiya Fukushima JAPAN Observers and equipment: Observer code: VB = Vladimir Robert D. Stephens Benishek; AF = Andrea Ferrero; HH = Hiromi and Hiroko Goat Mountain Astronomical Research Station (GMARS) Hamanowa; FP = Frederick Pilcher; RS = Robert Stephens.