The Discoveries
Blue Mountains Observatory Research Welcomes Collabaration With Other Observatories
LAWRENCE KRAUSS
WE ARE ALL STARDUST
BINARY ASTEROID DISCOVERIES 1
2478 TOKAI
Electronic Telegram No. 824 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html
(2478) TOKAI
D. Higgins, Canberra, Australia; P. Pravec and P. Kusnirak, Ondrejov Observatory; B. Warner, Palmer Divide Observatory, Colorado Springs, CO; A. Galad, Modra Observatory; J. Oey, Leura, N.S.W., Australia; R. Goncalves, Linhaceira, Tomar, Portugal; and W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ, report that photometric observations obtained during Jan. 20-28 reveal that minor planet (2478) is a synchronous binary system with a period of 25.885 +/- 0.007 hours. A combined rotation lightcurve has an amplitude of 0.41 mag, and superimposed mutual events indicate a lower limit on a secondary-to-primary mean-diameter ratio of 0.72. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2007 CBAT 2007 January 30 (CBET 824) Daniel W. E. Green
5481 KIUCHI
Electronic Telegram No. 1339 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://www.cfa.harvard.edu/iau/cbat.html
(5481) KIUCHI
P. Kusnirak and P. Pravec, Ondrejov Observatory; J. Oey, Leura, N.S.W., Australia; R. Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA, U.S.A.; M. Husarik, Skalnate Pleso Observatory; and J. Ries, McDonald Observatory, report that photometric observations obtained during Mar. 13 to Apr. 6 reveal that minor planet (5481) is a binary system with an orbital period of 20.90 +/- 0.01 hr. The primary shows a period of 3.6196 +/- 0.0002 hr, and it has a lightcurve amplitude of 0.10 mag, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events indicate a secondary-to-primary mean-diameter ratio of 0.33 +/- 0.02. The mean absolute R magnitude is H = 12.98 +/- 0.1, assuming G = 0.15 +/- 0.2. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2008 CBAT 2008 April 15 (CBET 1339) Daniel W. E. Green
10208 1997 QN1
Electronic Telegram No. 1087 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://www.cfa.harvard.edu/iau/cbat.html
(10208) 1997 QN1
J. Oey, Leura, N.S.W., Australia; P. Pravec and P. Kusnirak, Ondrejov Observatory; Yu. Krugly and V. Chiorny, Institute of Astronomy of Kharkiv National University, Main Astronomical Observatory, National Academy of Science of Ukraine; and J. Ries, McDonald Observatory, report that photometric observations obtained during Aug. 6-Sept. 18 reveal that minor planet (10208) is a binary system with an orbital period of 58.55 +/- 0.02 hr. The primary shows a period of 3.3484 +/- 0.0001 hr, and it has a light- curve amplitude of 0.13 mag. Mutual eclipse/occultation events, with a depth of 0.21 mag on Sept. 15, indicate a secondary-to-primary mean-diameter ratio of 0.46 +/- 0.02. Calibrated data give an estimated mean absolute magnitude H_R = 14.2 +/- 0.2, assuming G = 0.15 +/- 0.2. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2007 CBAT 2007 September 25 (CBET 1087) Daniel W. E. Green
2691 SERSIC
Electronic Telegram No. 2766 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(2691) SERSIC
J. Oey, Leura, N.S.W., Australia; P. Pravec and P. Kusnirak, Ondrejov Observatory; N. Morales and A. Thirouin, Instituto de Astrofisica de Andalucia; J. Pollock, Appalachian State University; and D. E. Reichart, K. M. Ivarsen, J. B. Haislip, and A. LaCluyze, Physics and Astronomy Department, University of North Carolina, Chapel Hill, report that photometric observations taken during 2011 June 3-July 7 reveal that minor planet (2691) is a binary system with an orbital period of 26.81 +/- 0.01 hr. The primary light-curve component shows a period of 3.8811 +/- 0.0003 hr and it has an amplitude of 0.21 mag. Observed mutual eclipse/occultation events were up to 0.45-mag deep. From a depth of the secondary event, they estimate a lower limit on the secondary-to-primary mean-diameter ratio of 0.43 +/- 0.02. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2011 CBAT 2011 July 16 (CBET 2766) Daniel W. E. Green To un-subscribe from the IAU Circulars Mailing List for ASNSW Members, please send a blank email to: iaucirculars-unsubscribe@asnsw.com
99913 1997 CZ5
Electronic Telegram No. 2648 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(99913) 1997 CZ5
D. Higgins, Canberra, Australia; P. Pravec, P. Kusnirak, and K. Hornoch, Ondrejov Observatory; J. Pollock, Appalachian State University; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ, U.S.A.; J. Oey, Leura, N.S.W., Australia; J. Brinsfield, Via Capote Observatory, Thousand Oaks, CA, U.S.A.; and D. E. Reichart, K. M. Ivarsen, J. B. Haislip, and A. LaCluyze, Physics and Astronomy Department, University of North Carolina, Chapel Hill; and R. Durkee, Shed of Science Observatory, Minneapolis, MN, U.S.A., report that photometric observations obtained during Jan. 8-30 reveal that minor planet (99913) is a binary system with an orbital period of 14.68 hr. The primary shows a period of 2.83507 +/- 0.00002 hr, and it has a lightcurve amplitude of 0.19 mag. Mutual eclipse/occultation events that are 0.033- and 0.042-magnitude deep indicate a secondary-to-primary mean-diameter ratio of 0.19 +/- 0.02. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2011 CBAT 2011 February 3 (CBET 2648) Daniel W. E. Green To un-subscribe from the IAU Circulars Mailing List for ASNSW Members, please send a blank email to: iaucirculars-unsubscribe@asnsw.com
15700 1987 QD
Electronic Telegram No. 2540 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(15700) 1987 QD
R. Durkee, Shed of Science Observatory, Minneapolis, MN; P. Pravec, K. Hornoch, and P. Kusnirak, Ondrejov Observatory; D. Pray, Carbuncle Hill Observatory, W. Brookfield, MA, U.S.A.; V. Chiorny and V. Shevchenko, Kharkiv Observatory; J. Oey, Leura, N.S.W., Australia; N. Gaftonyuk and Yu. Krugly, Simeiz Observatory; D. Higgins, Canberra, Australia; J. Vilagi and S. Gajdos, Modra Observatory; M. Husarik and M. Pikler, Skalnate Pleso Observatory; and J. G. Ries, McDonald Observatory, University of Texas, report that photometric observations obtained during Sept. 6-Oct. 13 reveal that minor planet (15700) is a binary-system candidate. A primary rotation period of 3.0586 +/- 0.0001 hr with a lightcurve amplitude of 0.07 mag was resolved. Superimposed to the primary lightcurve were attenuations with depths 0.1-0.3 mag and durations up to 3.5 hours that had shapes characteristic of mutual events in a binary system. A conclusive solution for the orbit period was not obtained, however, so this object remains a serious suspect for being binary, but confirmation must come from future observations. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2010 CBAT 2010 November 6 (CBET 2540) Daniel W. E. Green To un-subscribe from the IAU Circulars Mailing List for ASNSW Members, please send a blank email to: iaucirculars-unsubscribe@asnsw.com
2121 SEVASTOPOL
Electronic Telegram No. 2427 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Room 209; Dept. of Earth and Planetary Sciences; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbat@iau.org; cbatiau@eps.harvard.edu URL http://www.cfa.harvard.edu/iau/cbat.html
(2121) SEVASTOPOL
D. Higgins, Canberra, Australia; P. Pravec and P. Kusnirak, Ondrejov Observatory; J. Pollock, Appalachian State University; J. Oey, Leura, N.S.W., Australia; M. Husarik and G. Cervak, Skalnate Pleso Observatory; and D. E. Reichart, K. M. Ivarsen, J. B. Haislip, and A. LaCluyze, Physics and Astronomy Department, University of North Carolina, Chapel Hill, report that photometric observations obtained during July 23-Aug. 24 reveal that minor planet (2121) is a binary system with an orbital period of 37.1 hr. The primary shows a period of 2.90640 +/- 0.00002 hr, and it has a lightcurve amplitude of 0.20 mag. Mutual eclipse/occultation events that are 0.2-mag deep indicate a secondary-to-primary mean-diameter ratio of 0.41 +/- 0.02. The secondary rotates synchronously with the orbital motion and shows an amplitude of 0.06 mag in the combined lightcurve of the system. Due to the high solar phase, the observed eclipse/occultation events also describe the satellite-shadow transit and satellite’s passage through the parent body’s shadow. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2010 CBAT 2010 August 26 (CBET 2427) Daniel W. E. Green
3868 MENDOZA
Electronic Telegram No. 1835 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://www.cfa.harvard.edu/iau/cbat.html
(3868) MENDOZA
J. Oey, Leura Observatory, Leura, N.S.W., Australia; P. Pravec, P. Kusnirak, and K. Hornoch, Ondrejov Observatory; J. Brinsfield, Via Capote Observatory, Thousand Oaks, CA, U.S.A.; V. Chiorny, Kharkiv Observatory; D. Pray, Carbuncle Observatory, W. Brookfield, MA, U.S.A.; and M. Pikler and M. Husarik, Skalnate Pleso Observatory, report that photometric observations obtained during Apr. 25 to May 25 reveal that minor planet (3868) is a binary system with an orbital period of 24.38 hr. The primary shows a period of 2.77090 +/- 0.00005 hr and has a lightcurve amplitude of 0.10 mag, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events with a depth of 0.05 mag indicate a secondary-to-primary mean-diameter ratio of 0.22 +/- 0.02. The mean absolute R-band magnitude and the slope parameter of the system are H_R = 12.30 +/- 0.04 and G_R = 0.23 +/- 0.05. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2009 CBAT 2009 June 6 (CBET 1835) Daniel W. E. Green
15268 1990 WF3
Electronic Telegram No. 1542 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://www.cfa.harvard.edu/iau/cbat.html
(15268) 1990 WF3
J. Oey, Leura Observatory, N.S.W., Australia; P. Pravec, P. Kusnirak, and K. Hornoch, Ondrejov Observatory; R. Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA, U.S.A.; S. Gajdos and L. Kornos, Modra Observatory; and V. Chiorny, Institute of Astronomy, Kharkiv National University, report that photometric observations obtained during Sept. 24-Oct. 9 reveal that minor planet (15268) is a binary system with an orbital period of 25.07 +/- 0.02 hr. The primary shows a period of 2.4224 +/- 0.0001 hr, and it has a lightcurve amplitude of 0.07 mag, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.27. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2008 CBAT 2008 October 20 (CBET 1542) Daniel W. E. Green To un-subscribe from the IAU Circulars Mailing List for ASNSW Members, please send a blank email to: iaucirculars-unsubscribe@asnsw.com
WE ARE THE BEST AT WHAT WE DO
BINARY ASTEROID DISCOVERIES 2
6186 ZENON
(6186) ZENON
(6186) ZENON
V. Benishek, Belgrade Astronomical Observatory; P. Pravec, Ondrejov Observatory; N. Gaftonyuk, Simeiz Observatory; M. Husarik and G. Cervak, Skalnate Pleso Observatory; and J. Oey, Blue Mountains Observatory, Leura, NSW, Australia, report that photometric observations taken with a 0.35-m telescope at the Sopot Observatory in Serbia, a 1.0-m telescope at the Simeiz Observatory, a 0.61-m telescope at the Skalnate Pleso Observatory, and a 0.35-m telescope at the Blue Mountains Observatory during 2016 Oct. 31-2017 Jan. 1 reveal that minor planet (6186) is a binary system with an orbital period of 14.392 +/- 0.004 hr. Mutual eclipse/occultation events that are 0.08- to 0.16-magnitude deep indicate a secondary-to-primary mean-diameter ratio of 0.28 +/- 0.03. The eclipsing/occulting secondary has a synchronous rotation with an observed lightcurve amplitude of 0.04 mag. Superimposed to the eclipse/occultation lightcurve are two rotational lightcurves with periods 2.6832 +/- 0.0002 hr and 3.2981 +/- 0.0002 hr, each with an amplitude of 0.08 mag; their behavior in the mutual events — they are present with unchanged shapes during the events — indicates that none of them belongs to the eclipsing/occulting secondary. This suggests that, while one of the short periods belongs to the primary, the other belongs to a third body in the system (compare with other cases of this kind in Pravec et al. 2016, Icarus 267, 267). NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2017 CBAT 2017 January 14 (CBET 4346) Daniel W. E. Green Electronic Telegram No. 4374 Central Bureau for Astronomical Telegrams Mailing address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
12326 SHIRASAKI
(12326) SHIRASAKI
(12326) SHIRASAKI
D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.; P. Pravec, Ondrejov Observatory; V. Benishek, Belgrade Astronomical Observatory; J. Oey, Blue Mountains Observatory, Leura, NSW, Australia; and V. Chiorny, Kharkiv Observatory, report that photometric observations taken with a 0.50-m telescope at the Sugarloaf Mountain Observatory, a 0.35-m telescope at the Sopot Observatory in Serbia, a 0.35-m telescope at the Blue Mountains Observatory, and a 0.70-m telescope at the Chuguev station of the Kharkiv Observatory in Ukraine during 2016 Nov. 5-Dec. 6 reveal that minor planet (12326) is a binary system with an orbital period of 25.06 +/- 0.02 hr. The primary shows a period of 2.7286 +/- 0.0001 hr and has a lightcurve amplitude of 0.12 mag at solar phases 5-7 degrees, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that are 0.06- to 0.12-magnitude deep indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.24. Superimposed to the primary and the eclipse/occultation lightcurves is a second rotational lightcurve with a period of 12.7 +/- 0.1 hr, derived assuming two pairs of maxima/minima per period, and an observed lightcurve amplitude of 0.03-0.04 mag. It remains to be seen from future studies whether the second rotational lightcurve belongs to the eclipsing/occulting secondary or a possible third body in the system. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2017 CBAT 2017 January 12 (CBET 4345) Daniel W. E. Green Electronic Telegram No. 4346 Central Bureau for Astronomical Telegrams Mailing address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
5112 KUSAJI
Electronic Telegram No. 4336 Central Bureau for Astronomical Telegrams Mailing address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(5112) KUSAJI
V. Chiorny, Kharkiv Observatory; P. Pravec, Ondrejov Observatory; D. Romeuf, Lyon University; R. Montaigut, A. Leroy, and C. Gillier, OPERA Observatory, France; V. Benishek, Belgrade Astronomical Observatory; A. Marchini, R. Papini, and F. Salvaggio, Dipartimento di Scienze Fisiche, Della Terra e Dell’Ambiente, University of Siena; and J. Oey, Blue Mountains Observatory, Leura, NSW, Australia, report that photometric observations taken with a 0.70-m telescope at the Chuguev station of the Kharkiv Observatory in Ukraine, a 0.36-m telescope at Pommier Observatory in France, a 0.20-m telescope at the OPERA Observatory, a 0.35-m telescope at the Sopot Observatory in Serbia, a 0.30-m telescope at the Astronomical Observatory of the University of Siena, and a 0.61-m telescope at the Blue Mountains Observatory during 2016 Oct. 25 to Nov. 1 reveal that minor planet (5112) is a binary system with an orbital period of 20.74 +/- 0.01 hr. The primary shows a period of 2.7995 +/- 0.0001 hr and has a lightcurve amplitude of 0.12 mag at solar phases 4-8 degrees, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that are 0.10- to 0.17-magnitude deep indicate a secondary-to-primary mean-diameter ratio of 0.31 +/- 0.02. The secondary’s rotation appears synchronous with the orbital motion and it has a lightcurve amplitude of 0.02-0.03 mag in the combined primary-plus-secondary lightcurve, suggesting a moderately elongated secondary shape with the equatorial axis ratio being about 1.3. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2016 CBAT 2016 November 10 (CBET 4336) Daniel W. E. Green Electronic Telegram No. 4345 Central Bureau for Astronomical Telegrams Mailing address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
20325 JULIANOEY
(20325) 1998 HO_27
(20325) 1998 HO_27
D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.; P. Pravec, Ondrejov Observatory; V. Benishek, Belgrade Observatory; J. Pollock, Appalachian State University; W. Cooney and J. Gross, Sonoita Research Observatory; D. Terrell, Southwest Research Institute; D. E. Reichart, J. B. Haislip and A. P. LaCluyze, University of North Carolina, Chapel Hill; and A. Verveer and T. Spuck, Perth Observatory, report that photometric observations obtained during 2014 Nov. 22-Dec. 20 reveal that minor planet (20325) is a binary system with an orbital period of 23.54 +/- 0.01 hr. The primary shows a period of 3.24474 +/- 0.00008 hr, and it has a lightcurve amplitude of 0.13 mag, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that are 0.09- to 0.19-magnitude deep indicate a secondary-to-primary mean-diameter ratio of 0.30 +/- 0.02. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2014 CBAT 2014 December 24 (CBET 4039) Daniel W. E. Green
2343 SIDING SPRING
Electronic Telegram No. 4206 Central Bureau for Astronomical Telegrams Mailing address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(2343) SIDING SPRING
J. Pollock, D. Caton, and R. Hawkins, Appalachian State University (ASU); P. Pravec, Ondrejov Observatory; D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.; W. Cooney and J. Gross, Sonoita Research Observatory, Sonoita, AZ, U.S.A.; D. Terrell, Southwest Research Institute; J. Oey, Blue Mountains Observatory, Leura, NSW, Australia; V. Benishek, Belgrade Astronomical Observatory; A. Galad and S. Gajdos, Modra Observatory; R. Groom and K. Stranger, Perth Observatory; V. Chiorny, Kharkiv Observatory; D. Reichart and J. Haislip, University of North Carolina at Chapel Hill; and A. Smith, Gemini North, report that photometric observations taken with a 0.35-m telescope at the ASU’s Dark Sky Observatory (near Boone, NC, USA), a 0.50-m telescope at the Sugarloaf Mountain Observatory, a 0.50-m telescope at the Sonoita Research Observatory, a 0.35-m telescope at the Blue Mountains Observatory, a 0.35-m telescope at the Sopot Observatory in Serbia, a 0.60-m telescope at the Modra Observatory, a 0.36-m telescope at the Perth Observatory, and a 0.70-m telescope at the Grakovo station of the Kharkiv Observatory in Ukraine during Oct. 6-Nov. 21 reveal that minor planet (2343) is a binary system with an orbital period of 11.789 +/- 0.003 hr. The primary shows a period of 2.10637 +/- 0.00008 hr, and has a lightcurve amplitude of 0.15 mag at solar phases 2-15 degrees, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that are 0.04 to 0.06 magnitude deep indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.19. An additional brightness variation with a period of 20.01 +/- 0.03 hr and an amplitude of 0.04 mag is present in the observed lightcurve, that suggests a presence of a third body in the system. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2015 CBAT 2015 December 1 (CBET 4206) Daniel W. E. Green
1338 DUPONTA
Electronic Telegram No. 910 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html
(1338) DUPONTA
S. Gajdos, L. Kornos, J. Vilagi, and A. Galad, Modra Observatory; P. Pravec, Ondrejov Observatory; R. Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA; V. Reddy, Department of Earth System Science and Policy, University of North Dakota, Grand Forks; R. Dyvig, Quinn, SD; D. Higgins, Canberra, Australia; J. Oey, Leura, N.S.W., Australia; and D. Pray, Carbuncle Hill Observatory, Greene, RI, report that photometric observations obtained during Mar. 6-26 reveal that minor planet (1338) is a binary system with an orbital period of 17.57 +/- 0.01 hr. The primary shows a period of 3.85453 +/- 0.00009 hr, and it has a lightcurve amplitude of 0.23 mag. Mutual eclipse/occultation events that are 0.06- to 0.12-mag deep indicate a secondary-to-primary mean-diameter ratio of 0.23 +/- 0.02. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2007 CBAT 2007 March 27 (CBET 910) Daniel W. E. Green
8306 SHOKO
Circular No. 9268 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION New postal address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. CBATIAU@EPS.HARVARD.EDU ISSN 0081-0304 URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(8306) SHOKO
P. Pravec, P. Kusnirak, K. Hornoch, and A. Galad, Ondrejov Observatory and European Southern Observatory, La Silla; Yu. N. Krugly and V. Chiorny, Kharkiv Observatory; R. Inasaridze, O. Kvaratskhelia, and V. Ayvazian, Abastumani Observatory; O. Parmonov, Maidanak Observatory; J. Pollock, Appalachian State University; S. Mottola, Calar Alto Observatory; J. Oey, Blue Mountains Observatory, Leura, NSW; D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.; J. Zizka and J. Vrastil, Charles University, Prague; I. Molotov, Keldish Institute of Applied Mathematics, Moscow; and D. E. Reichart, K. M. Ivarsen, J. B. Haislip, and A. LaCluyze, Physics and Astronomy Department, University of North Carolina at Chapel Hill, report that photometric observations obtained during 2013 Sept. 7-Dec. 7 reveal that minor planet (8306) is a binary system with an orbital period of 36.20 +/- 0.04 hr. The primary shows a period of 3.3503 +/- 0.0002 hr, and it has a lightcurve amplitude of 0.11 mag at solar phases 3-13 deg, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that are up to 0.26 mag deep indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.40. The secondary shows a period equal to the orbital period, indicating synchronous rotation. Residuals of the fit show an additional brightness variation that may be due to rotation of a third body of the system. The mean absolute R magnitude of the system is H_R = 14.83 +/- 0.07, assuming G = 0.24 +/- 0.11. These observations were run as a part of their photometric project “NEOSource” within its task to study binary and multiple systems among minor-planet pairs [i.e., pairs of minor planets that are in highly similar heliocentric orbits (see Vokrouhlicky and Nesvorny 2008, A.J. 136, 280; Pravec et al. 2010, Nature 466, 1085)]. Minor planet (8306) was selected as a target when found that it appears paired with minor planet 2011 SR_158 using the method of Pravec and Vokrouhlicky (2009, Icarus 204, 580), modified with use of the mean elements from AstDyS-2 (see website URL http://hamilton.dm.unipi.it/astdys2/) and with backward integrations of their orbits using the method of Vokrouhlicky (2009, Ap.J. 706, L37). The integrations indicate that the pair separated from a single body between 300 and 650 kyr ago. V1369 CENTAURI = NOVA CENTAURI 2013 Visual magnitude estimates: Dec. 12.166 UT, 4.3 (R. Salvo, Montevideo, Uruguay); 14.23, 3.6 (Salvo); 15.28, 3.5 (W. Souza, Sao Paulo, Brazil); 16.281, 4.5 (Souza); 26.250, 4.1 (Souza); 28.302, 4.1 (Souza). (C) Copyright 2013 CBAT 2013 December 28 (9268) Daniel W. E. Green
32039 2000 JO23
Electronic Telegram No. 1147 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://www.cfa.harvard.edu/iau/cbat.html
(32039) 2000 JO23
D. Pray, Carbuncle Hill Observatory, Greene, RI; P. Pravec, P. Kusnirak and K. Hornoch, Ondrejov Observatory; D. Higgins, Canberra, Australia; W. Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; J. Oey, Leura, N.S.W., Australia; A. Galad, L. Kornos, S. Gajdos, and J. Vilagi, Modra Observatory; R. Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA; F. Marchis and M. Baek, SETI Institute; B. Macomber, University of California at Berkeley; V. Reddy, Department of Earth System Science and Policy, University of North Dakota, Grand Forks; and M. Husarik and M. Pikler, Skalnate Pleso Observatory, report that photometric observations obtained during Sept. 3-Nov. 8 reveal that minor planet (32039) is a binary system. Mutual events observed on Sept. 16.3, Oct. 1.3, and 8.8 suggest an orbital period of 360 hr, and their depth of 0.32 mag indicates a lower limit on the secondary-to-primary mean-diameter ratio of 0.58. Two additive lightcurve components have been observed, one with a period of 3.2990 +/- 0.0002 or 6.5979 +/- 0.0009 hr and amplitude 0.05 mag, and the other one with a period of 11.099 +/- 0.003 hr and amplitude 0.08 mag. The former appears to be a rotation lightcurve of the primary, but an interpretation of the latter lightcurve component as belonging to the secondary is less certain and model-dependent. Calibrated data give an estimated mean absolute magnitude H_R = 15.39 and slope parameter G = 0.25, both with formal uncertainties of 0.03. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2007 CBAT 2007 November 23 (CBET 1147) Daniel W. E. Green To un-subscribe from the IAU Circulars Mailing List for ASNSW Members, please send a blank email to: iaucirculars-unsubscribe@asnsw.com
357439 2004 BL86
Electronic Telegram No. 4063 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(357439) 2004 BL_86
J. Pollock, Appalachian State University; P. Pravec, Ondrejov Observatory; J. Oey, Blue Mountains Observatory, Leura, NSW; and D. E. Reichart, J. B. Haislip and A. P. LaCluyze, University of North Carolina, Chapel Hill, report that photometric observations obtained during 2015 Jan. 20-24 reveal that minor planet (357439) is a binary system with an orbital period of 13.80 +/- 0.05 hr. The primary shows a period of 2.6205 +/- 0.0003 hr, and it has a lightcurve amplitude of 0.17 mag at solar phases 99-109 deg, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that are 0.05- to 0.07-magnitude deep indicate a secondary-to-primary mean-diameter ratio of 0.21 +/- 0.02. Minor planet 2004 BL_86 was discovered eleven years ago by the LINEAR program (cf. MPEC 2004-B80) and was later numbered (357439). Lance A. M. Benner, on behalf of the radar team reports that Goldstone delay-Doppler radar (8560-MHz, 3.5-cm, 3.75-m resolution) images obtained on 2015 Jan. 26 confirm that (357439) is a binary system. Preliminary estimates for diameters of the components are 300 m for the primary and 50-100 m for the secondary. Forty-four minor planets passing close to the earth have now been found to have companions via radar (eight of those discovered first via optical photometry), and at least two such minor planets have more than one companion. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2015 CBAT 2015 January 30 (CBET 4063) Daniel W. E. Green
4541 MIZUNO
Electronic Telegram No. 4097 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(4541) MIZUNO
D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.; P. Pravec, K. Hornoch, P. Kusnirak, J. Vrastil and H. Kucakova, Ondrejov Observatory; Yu. N. Krugly and V. Shevchenko, Kharkiv Observatory; R. Inasaridze and V. Ayvazian, Abastumani Observatory; J. Oey, Blue Mountains Observatory, Leura, NSW; W. Cooney and J. Gross, Sonoita Research Observatory, Sonoita, AZ, USA; D. Terrell, Southwest Research Institute; and I. Molotov, Keldysh Institute of Applied Mathematics, Moscow; report that photometric observations obtained during Feb. 24-Apr. 25 reveal that minor planet (4541) is a binary system with an orbital period of 29.68 +/- 0.01 hr. The primary shows a period of 2.82784 +/- 0.00005 hr, and it has a lightcurve amplitude of 0.08 mag at solar phases 3-15 deg, suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that are 0.06- to 0.15-magnitude deep indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.24. The mean absolute R magnitude of the system is H_R = 12.50 +/- 0.04 and the slope parameter G = 0.11 +/- 0.04. V. Reddy and D. Takir, Planetary Science Institute, Tucson, report that near-infrared spectroscopic observations (0.7-2.5 microns) of minor planet (4541), obtained on Apr. 26 using the NASA Infrared Telescope Facility on Mauna Kea, show that it is an S-type minor planet with surface composition dominated by the minerals olivine and pyroxene. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2015 CBAT 2015 May 10 (CBET 4097) Daniel W. E. Green
8474 RETTIG
Electronic Telegram No. 4122 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
(8474) RETTIG
V. Chiorny, Kharkiv Observatory; V. Benishek, Belgrade Astronomical Observatory, Serbia; P. Pravec and P. Kusnirak, Ondrejov Observatory; Yu. N. Krugly, Kharkiv Observatory; J. Oey and R. Groom, Blue Mountains Observatory, Leura, NSW, Australia; V. Reddy, Planetary Science Institute; D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.; W. Cooney and J. Gross, Sonoita Research Observatory, Sonoita, AZ, U.S.A.; D. Terrell, Southwest Research Institute; R. Inasaridze, V. Ayvazian and V. Zhuzhanidze, Abastumani Observatory; R. Montaigut and A. Leroy, OPERA Observatory, France; and I. Molotov, Keldysh Institute of Applied Mathematics, Moscow, report that photometric observations obtained during May 19-July 23 reveal that minor planet (8474) is a binary system with an orbital period of 30.54 +/- 0.01 hr. Mutual eclipse/occultation events that are 0.60- to 0.93-magnitude deep indicate a lower limit on the secondary-to-primary mean-diameter ratio of 0.86. Rotations of the components appear to be synchronous with the orbital motion and an amplitude of the combined primary plus secondary rotational lightcurve is 0.34 mag at solar phases 7-15 deg. NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2015 CBAT 2015 July 26 (CBET 4122) Daniel W. E. Green