Discoveries - Minor Planet Photometry

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Discoveries

Announcements of discoveries:
2017

Discovery of binary Minor Planet 1798 Watts in CBET 4374

Discovery of binary Minor Planet 6186 Xenon in CBET 4346

Discovery of binary Minor Planet 12326 Shirasaki in CBET 4345


2016

Naming of binary Minor Planet 20325 Julianoey in CBAT 4039

Discovery of binary Minor Planet 5112 Kusaji in CBET 4336


2015

Discovery of binary Minor Planet 2343 Siding Spring in CBAT 4206
Discovery of binary Minor Planet 8474 Rettig in CBAT 4122
Discovery of binary Minor Planet 4541 Mizuno in CBAT 4097
Discovery of binary Minor Planet 357439 2004 BL86 in CBAT 4063

2013
Discovery of binary Minor Planet (8306) SHOKO in CBAT 9268

2011

Discovery of binary Minor Planet 2691 Sersic in CBET 2766 (Primary Investigator)
Discovery of binary Minor Planet 99913 1997 CZ5 in CBET 2648

2010

Serious suspect for binary  asteroid 15700 1987 QD in CBET 2540
Discovery of binary Minor Planet 2121 Sevastopol in CBET 2427

2009

Discovery of binary Minor Planet 3868 Mendoza in CBET 1835 (Primary Investigator)

2008

Discovery of binary Minor Planet 5481 Kiuchi in CBET 1339
Discovery of binary Minor Planet 15268 1990 WF3 in CBET 1542 (Primary Investigator)



2007

Discovery of binary Minor Planet 10208 1997 QN1 in CBET 1087 (Primary Investigator)
Discovery of binary minor planet 2478 Tokai in CBET 824
Discovery of binary minor planet 1338 Duponta in CBET 910
Discovery of binary minor planet (32039) 2000 JO23 CBET 1147

Variable star


AAVSO Unique Identifier (AUID) of 000-BJV-939 = VSX J155453.9-262107



                                                 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

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                                                 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

                                                 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
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                        (C) Copyright 2011 CBAT
2011 February 3                  (CBET 2648)              Daniel W. E. Green

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                                                 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

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                                                 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

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                                                 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

                                                 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


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

                                                 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


                                                 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

                                                 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

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                                                  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

                                                 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


                                                 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


                                                 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


                                                 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


Named (20325) Julianoey

(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

                                                 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


(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


(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


(1798) WATTS
    D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.;
P. Pravec, H. Kucakova, J. Vrastil, K. Hornoch, and P. Kusnirak, Ondrejov
Observatory; W. Cooney and J. Gross, Sonoita Research Observatory, Sonoita,
AZ, U.S.A.; D. Terrell, Southwest Research Institute; B. Flanagan and B.
Pellerin, Madrona Peak Observatory, Medina, TX, U.S.A.; and J. Oey, Blue
Mountains Observatory, Leura, NSW, Australia, report that photometric
observations taken with a 0.50-m telescope at the Sugarloaf Mountain
Observatory, a 0.65-m telescope at the Ondrejov Observatory, a 0.50-m
telescope at the Sonoita Research Observatory, a 0.6-m telescope at the
Madrona Peak Observatory, and a 0.35-m telescope at the Blue Mountains
Observatory during 2017 Jan. 31-Mar. 15 reveal that minor planet (1798) is
a binary system with an orbital period of 26.96 +/- 0.01 hr.  The primary
shows a period of 3.5060 +/- 0.0004 hr and has a lightcurve amplitude of
0.06 mag at solar phase 5 degrees, suggesting a nearly spheroidal shape.
Mutual eclipse/occultation events that are 0.06- to 0.11-magnitude deep
indicate a secondary-to-primary mean-diameter ratio of 0.25 +/- 0.02.
The mean absolute R magnitude in the Cousins system is H_R = 12.81 +/- 0.08,
assuming the phase relation slope parameter G = 0.24 +/- 0.11.


NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
     superseded by text appearing later in the printed IAU Circulars.

                        (C) Copyright 2017 CBAT
2017 March 19                    (CBET 4374)              Daniel W. E. Green


 
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