CBAT Asteoidi

(1830) POGSON
     D. Higgins, Canberra, Australia; P. Pravec and P. Kusnirak, Ondrejov
Observatory; J. Oey, Leura, N.S.W., Australia; and D. Pray, Carbuncle Hill
Observatory, Greene, RI, report that photometric observations obtained
during Apr. 18 to May 9 reveal that minor planet (1830) is a binary system
with an orbital period of 24.240 +/- 0.005 hr.  The primary shows a period
of 2.5702 +/- 0.0001 hr, and it has a lightcurve amplitude of 0.12 mag.
Mutual eclipse/occultation events that are 0.08- to 0.22-mag deep indicate
a lower limit on the secondary-to-primary mean-diameter ratio of 0.32.

(4951) IWAMOTO
     V. Reddy, Department of Earth System Science and Policy,
University of North Dakota, Grand Forks; R. Dyvig, Badlands
Observatory, Quinn, SD; P. Pravec and P. Kusnirak, Ondrejov
Observatory; A. Galad, L. Kornos, S. Gajdos, and J. Vilagi, Modra
Observatory; D. Pray, Carbuncle Hill Observatory, Greene, RI; W.
Cooney, J. Gross, and D. Terrell, Sonoita Research Observatory,
Sonoita, AZ; Yu. Krugly, Kharkiv Observatory; J. Ries, McDonald
Observatory; K. Archer, Ironwood Observatory, Oahu, HI; J. Oey,
Leura, N.S.W., Australia; M. Pikler and M. Husarik, Skalnate Pleso
Observatory; R. Durkee, Minneapolis, MN; F. Colas, Pic du Midi
Observatory; and A. Harris, Space Science Institute, report that
photometric observations obtained during 2006 Dec. 25.1 to 2007 Mar.
23.9 UT reveal that minor planet (4951) is a synchronous binary
system with a period of 118.0 +/- 0.2 hours.  A combined rotation
lightcurve has an amplitude of 0.34 mag, and superimposed mutual
events indicate a lower limit on a secondary-to-primary mean-
diameter ratio of 0.76.  An estimated mean absolute magnitude in
the Cousins R system of 13.26 +/- 0.05 and measured color index of
V-R = +0.48 +/- 0.03 give an absolute V magnitude of 13.74 +/- 0.06.
This yields estimated mean diameters for the two bodies of 4.0 and
3.5 km (uncertain by about 20 percent), assuming a geometric V
albedo of 0.20 +/- 0.07 for its 'S' classification from 'SMASS II'
visible spectroscopy.  The system's parameters are extraordinary in
comparison with other known small binaries, in terms of system
angular momentum and evolution to its present synchronous state;
thus, further observations are warranted.

(121) HERMIONE
     P. Descamps, Institut de Mecanique Celeste et de Calcul des Ephemerides
(IMCCE), Paris; F. Marchis, University of California at Berkeley; J. Pollock,
Appalachian State University; J. Berthier and F. Vachier, Institut de
Mecanique Celeste et de Calcul des Ephemerides, Paris; T. Michalowski, Adam
Mickiewicz University; and J.-P. Teng, A. Peyrot, and C. Benard, Les Makes
Observatory, Reunion Island, report that a photometric observation program
initiated in March 2007 of the minor planet (121) Hermione confirms the
bilobated shape of the primary suggested by direct Keck adaptive-optics
imaging taken in 2003 (IAUC 8264; Marchis et al. 2005, Icarus 178, 450).
According to the orbital model of the satellite companion (cf. IAUC 7980),
the system is currently viewed edge-on.  The lightcurves recorded mostly at
the Make Observatory (Reunion Island) over seven nights reveal the high
amplitude of the brightness variation (up to 0.75), with a morphology
typical of a contact binary composed of two unequal components with a size
ratio of about 0.6.  Follow-up photometric observations that will help to
refine and improve the shape and pole solution of Hermione (currently V
about 12.6) are encouraged.  The current amplitude is about 0.6 mag, but
this should quickly decrease, as the equatorial plane will open to the
line-of-sight.

(88611) TEHARONHIAWAKO I (SAWISKERA)
     The companion to minor planet (88611) Teharonhiawako = 2001
QT_297 (cf. IAUCs 7733 and 7765) has been named Sawiskera (cf. MPC
59388).

COMET 133P/ELST-PIZARRO
     D. Jewitt, P. Lacerda, and N. Peixinho, University of Hawaii,
report that comet 133P/Elst-Pizarro = minor planet (7968) Elst-
Pizarro has become active after a long period of quiescence.
Optical observations with the University of Hawaii 2.2-m telescope
on June 11 UT show a straight tail at least 20" long in p.a. 256
deg.  The apparent red magnitude within an aperture 8" in projected
diameter is approximately 19.5.  Activity in 133P was last observed
in 2002 December.  The re-emergence of activity near perihelion (T
= 2007 June 29.3 TT; e.g., Nakano 2007, ICQ 2007 Comet Handbook) is
consistent with the identification of this object as an ice-bearing
minor planet or "main-belt comet" (Hsieh et al. 2004, A.J. 127,
2997).  Further observations to characterize the evolution of the
mass loss in the coming months are encouraged.

(6265) 1985 TW3
     D. Higgins, Canberra, Australia; and P. Pravec and P. Kusnirak, Ondrejov
Observatory, report that photometric observations obtained during July 15-25
reveal that minor planet (6265) is a binary system with an orbital period of
15.86 +/- 0.01 hr.  The primary shows a period of 2.7091 +/- 0.0001 hr, and
it has a lightcurve amplitude of 0.28 mag.  Mutual eclipse/occultation events
that are 0.06- to 0.12-mag deep indicate a lower limit on the secondary-to-p
rimary mean-diameter ratio of 0.24 +/- 0.02.

S/2007 (702) 1
      P. Rojo, Universidad de Chile; and J. L. Margot, Cornell University,
report the discovery on July 26.3 UT of a satellite of (702) Alauda (V =
11.9) from adaptive-optics J-, H-, and K_s-band imaging with the ESO 8-m
Very Large Telescope UT4/YEPUN on Cerro Paranal, Chile.  The satellite was
observed at two epochs on each of two consecutive nights.  On July 26.265
UT, the companion was at a separation of 0".58 (projected separation about
900 km) in p.a. 20 deg.  The primary-to-secondary H-band flux ratio is about
1250, yielding a diameter ratio of about 35.  This is the first satellite
discovered to a large minor planet of type B in the SMASSII taxonomy (Bus
and Binzel 2002, Icarus 158, 146).  Alauda (a = 3.2 AU, e = 0.02, i = 21
deg) has been identified as the largest member of a dynamical family
(Foglia and Masi 2004, Minor Planet Bull. 41, 100; Gil-Hutton 2006, Icarus
183, 93).

S/2007 (702) 1
      P. Rojo, Universidad de Chile; and J. L. Margot, Cornell University,
report the discovery on July 26.3 UT of a satellite of (702) Alauda (V =
11.9) from adaptive-optics J-, H-, and K_s-band imaging with the ESO 8-m
Very Large Telescope UT4/YEPUN on Cerro Paranal, Chile.  The satellite was
observed at two epochs on each of two consecutive nights.  On July 26.265
UT, the companion was at a separation of 0".58 (projected separation about
900 km) in p.a. 20 deg.  The primary-to-secondary H-band flux ratio is about
1250, yielding a diameter ratio of about 35.  This is the first satellite
discovered to a large minor planet of type B in the SMASSII taxonomy (Bus
and Binzel 2002, Icarus 158, 146).  Alauda (a = 3.2 AU, e = 0.02, i = 21
deg) has been identified as the largest member of a dynamical family
(Foglia and Masi 2004, Minor Planet Bull. 41, 100; Gil-Hutton 2006, Icarus
183, 93).

2007 DT103
     L. A. M. Benner, S. J. Ostro, J. D. Giorgini, J. Van Brimmer, L. Juare,
J. S. Jao, R. F. Jurgens, and M. A. Slade, Jet Propulsion Laboratory,
California Institute of Technology (CIT); and M. W. Busch, CIT, report that
Goldstone (8560-mHz, 3.5-cm) radar observations during July 26, 28, and Aug.
1 reveal that minor planet 2007 DT103 (cf. MPEC 2007-F20; MPO 121877) is a
binary system.  Preliminary estimates for the component diameters are about
0.3 km and > 80 m.  The maximum orbital distance between the components is
at least 0.45 km.

(32008) 2000 HM53
     P. Pravec, P. Kusnirak, and K. Hornoch, Ondrejov Observatory; J.
Vilagi, L. Kornos, and A. Galad, Modra Observatory; D. Higgins, Canberra,
Australia; V. Chiorny, Institute of Astronomy, Kharkiv National University,
National Academy of Science of Ukraine; D. Pray, Carbuncle Hill Observatory,
Greene, RI; 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; and R. Dyvig, Quinn, SD, report
that photometric observations obtained during Aug. 5-Sept. 14 reveal that
minor planet (32008) is a binary system with an orbital period of 40.24 +/-
0.02 hr -- or, less likely, 20.12 +/- 0.01 hr.  The primary shows a period
of 3.0171 +/- 0.0001 hr, and it has a lightcurve amplitude of 0.19 mag.
Mutual eclipse/occultation events indicate a lower limit on the secondary-
to-primary mean-diameter ratio of 0.4.  Calibrated data give an estimated
mean absolute magnitude H_R = 14.17 +/- 0.1, assuming G = 0.15 +/- 0.2.

(1453) FENNIA
     B. D. Warner, Palmer Divide Observatory, Colorado Springs, CO; A. W.
Harris, Space Science Institute; P. Pravec, Ondrejov Observatory; R. D.
Stephens, Goat Mountain Astronomical Research Station, Yucca Valley, CA; D.
Pray, Carbuncle Hill Observatory, Greene, RI; W. Cooney, J. Gross, and D.
Terrell, Sonoita Research Observatory, Sonoita, AZ; S. Gajdos and A. Galad,
Modra Observatory; and Yu. Krugly, Institute of Astronomy of Kharkiv
National University, Main Astronomical Observatory of National Academy of
Science of Ukraine, report that photometric observations made during Nov.
4-23 reveal that minor planet (1453) is a binary system with an orbital
period of 22.99 +/- 0.01 hr.  The primary shows a period of 4.4121 +/-
0.0001 hr, and it has a lightcurve amplitude of 0.18 mag, suggesting a
nearly spheroidal shape.  Mutual eclipse/occultation events indicate a
lower limit on the secondary-to-primary mean-diameter ratio of 0.28 +/-
0.02.

(7225) HUNTRESS
     D. Pray, Carbuncle Hill Observatory, Greene, RI, U.S.A.; P. Pravec, P.
Kusnirak, and K. Hornoch, Ondrejov Observatory; M. Husarik, M. Pikler, and
G. Cervak, Skalnate Pleso Observatory; S. Gajdos, Modra Observatory; and F.
Colas and J. Lecacheux, IMCCE and Pic du Midi Observatory, report that
photometric observations obtained during 2007 Dec. 7 to 2008 Jan. 17 reveal
that minor planet (7225) is a binary system with an orbital period of 14.67
+/- 0.01 hr.  The primary shows a period of 2.4400 +/- 0.0001 hr, and it has
a lightcurve amplitude of 0.11 mag, suggesting a nearly spheroidal shape.
Mutual eclipse/occultation events indicate a secondary-to-primary
mean-diameter ratio of 0.21 +/- 0.02.

(153591) 2001 SN_263
     M. C. Nolan, E. S. Howell, Arecibo Observatory; L. A. M. Benner,
S. J. Ostro, and J. D. Giorgini, Jet Propulsion Laboratory; M. W. Busch,
California Institute of Technology; L. M. Carter and R. F. Anderson,
Smithsonian Institution; C. Magri, University of Maine; D. B. Campbell and
J. L. Margot, Cornell University; and R. Vervack, Johns Hopkins University,
report that Arecibo radar delay-Doppler images (2380 MHz, 12.6 cm) obtained
on 2008 Feb. 12 show that minor planet (153591) is a triple system.
Based on range extents at 75-m resolution, preliminary estimates of average
diameters are 2 km, 1 km, and 400 m for the three components.

(153591) 2001 SN_263
     M. C. Nolan and E. S. Howell, Arecibo Observatory; L. A. M.
Benner, S. J. Ostro, and J. D. Giorgini, Jet Propulsion Laboratory;
M. W. Busch, California Institute of Technology; L. M. Carter and
R. F. Anderson, Smithsonian Institution; C. Magri, University of
Maine at Farmington; D. B. Campbell and J. L. Margot, Cornell
University; R. J. Vervack, Jr., Applied Physics Laboratory, Johns
Hopkins University; and M. K. Shepard, Bloomsburg University,
report that Arecibo radar delay-Doppler images (2380 MHz, 12.6 cm),
obtained on 2008 Feb. 12 and 13, show that minor planet (153591) is
a triple system.  Based on range extents at 75-m resolution,
preliminary estimates of average diameters are 2 km, 1 km, and 400
m for the three components.  The orbital separation for the larger
two components is at least 10 km.

COMET P/2008 G2 (SHOEMAKER)
     While examining Apr. 10 single-night observations of minor planets
reported by the Catalina Sky Survey to the Minor Planet Center, T. B. Spahr
identified a candidate (first observation given below) for comet P/1994 J3
= 1994k = 1994 XXVIII (Shoemaker, a.k.a. Shoemaker 4; cf. IAUC 5991, 5998,
etc.).  The undersigned then identified a corresponding candidate in the
Catalina data from Apr. 1.  In each case the observer was R. A. Kowalski,
and nothing was reported about the object's appearance.  The indicated
correction to the prediction on MPC 56803 (ephemeris on MPC 60734) is
-1.7 days.

COMET P/2008 G2 (SHOEMAKER)
     Comet P/1994 J3 = 1994k = 1994 XXVIII (Shoemaker, a.k.a.
'Shoemaker 4'; cf. IAUC 5991, 5998, etc.) was identified by T. B.
Spahr in single-night observations of minor planets (first
observation tabulated below) that were reported by the Catalina Sky
Survey to the Minor Planet Center, with additional observations
found by B. G. Marsden (see CBET 1347 for additional details).  The
indicated correction to the prediction on MPC 56803 (ephemeris on
MPC 60734) is Delta(T) = -1.7 days.  The available astrometry,
orbital elements, and ephemeris appear on MPEC 2008-H20.

2008 HJ
     R. Miles, Stourton Caundle, Dorset, UK, reports that photometric
observations of minor planet 2008 HJ (cf. MPEC 2008-H26, MPO 139312),
obtained using the 2.0-m Faulkes Telescope South during Apr. 28-29, reveal
that this Apollo-type object has the shortest known rotation period of any
natural body in the solar system at 42.67 +/- 0.04 s.  It exhibits a light
curve comprised of two similar maxima and minima with an amplitude of 0.8 mag.
Assuming an absolute magnitude of H = 25.8 and a geometric albedo of 0.2,
2008 HJ has presumed approximate dimensions 12 x 24 m.  The fastest
previously known rotator was 2000 DO8, which has a rotation period of 78 s
(Whiteley et al. 2002, Icarus 157, 139).

2005 NB_7
     P. Kusnirak and P. Pravec, Ondrejov Observatory; A. Galad and L. Kornos,
Modra Observatory; and W. Cooney, J. Gross, and D. Terrell, Sonoita Research
Observatory, Sonoita, AZ, U.S.A., report that photometric observations
obtained during Apr. 30-May 11 reveal the following information for the
binary minor planet 2005 NB_7 (cf. IAUC 8936):  orbital period = 15.28 +/-
0.01 hr (same as the secondary's rotation period); primary's rotation period
= 3.4883 +/- 0.0002 hr; primary's lightcurve amplitude = 0.13 mag, suggesting
a nearly spheroidal shape; secondary's lightcurve amplitude = 0.09 mag; lower
limit on the secondary-to-primary mean-diameter ratio = 0.32.

2007 TY_430
     S. S. Sheppard, Carnegie Institution of Washington; and C. A.
Trujillo, Gemini Observatory, report the discovery of a satellite
to the transneptunian minor planet 2007 TY_430 (cf. MPEC 2008-M38)
on images taken on 2007 Oct. 14 at Mauna Kea; images were obtained
on several dates with the 8.3-m Subaru, 8.2-m Gemini, and 6.5-m
Magellan telescopes.  At discovery, the binary had a separation of
about 0".6 (or at least 13000 km between components) in p.a. about
230 deg.  The two components appear to have a brightness within
about 0.1 mag of each other.  The individual components' g'-i'
colors also appear to be very similar.  Ongoing monitoring of the
binary shows a period of well over 1 year.

S/2008 (35107) 1
     W. J. Merline, Southwest Research Institute (SwRI); A. R.
Conrad, W. M. Keck Observatory (WMKO); J. D. Drummond, Starfire
Optical Range, AFRL; P. M. Tamblyn, Binary Astronomy, Dillon, CO,
and SwRI; C. Dumas and B. Carry, European Southern Observatory; R.
D. Campbell and R. W. Goodrich, WMKO; C. R. Chapman, SwRI; and W.
M. Owen, Jet Propulsion Laboratory, report the first-ever near-
infrared imaging of a close-approaching binary minor planet:  on
Aug. 9 UT, over a span of about 1 hr, they obtained J-, H-, and
K_p-band images -- using the 10-m Keck II Telescope (+ NIRC2/AO
adaptive-optics system) on Mauna Kea -- of clearly-separated
components of (35107) 1991 VH, which was first suspected as a
binary by Pravec et al. (IAUC 6607).  On Aug. 9.236 the satellite,
designated S/2008 (35107) 1, was 0".08 (projected separation 3.1
km) in p.a. 105 deg from the primary (the smallest angular and
physical separations yet for a binary minor planet using adaptive
optics).  The brightness difference was Delta(K_p) approximately
2.0 mag.  The observed separation and size ratio are consistent
with the parameters derived by Pravec et al. (2006, Icarus 181, 63).

(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.

SUPERNOVA 2004iq
     E. Kankare and S. Mattila, Tuorla Observatory; S. Ryder, Anglo-Australian
Observatory; A. Alonso-Herrero, T. Diaz Santos, and L. Colina, Instituto de
Estructura de la Materia, Consejo Superior de Investigaciones Cientificas
(CSIC); J. Kotilainen and H. Lehto, Tuorla Observatory; M. A. Perez-Torres,
C. Romero-Canizales, and A. Alberdi, Instituto de Astrofisica de Andalucia,
CSIC; P. Vaisanen, South African Astronomical Observatory; and A. Efstathiou,
European University of Cyprus, report the discovery of an apparent supernova
in near-infrared images of the luminous infrared galaxy IRAS 17138-1017.  The
new object was detected in F110W, F160W, and F187N NICMOS images obtained
with the Hubble Space Telescope on 2004 Sept. 23.0 UT, located at R.A =
17h16m35s.900, Decl. = -10o20'37".85 (equinox 2000.0), which is 1".50 east
and 1".12 north of the galaxy's H-band nucleus; 2004iq has magnitudes
18.3, 17.0, and 16.6 in the F110W, F160W, and F187N bands, respectively --
consistent with the core-collapse supernova template light curves of Mattila
and Meikle (2001, MNRAS, 234, 235) with a total line-of-sight extinction of
up to six magnitudes in V.  Nothing is visible at the position of 2004iq in
J, H, and K-band Altair/NIRI adaptive-optics images obtained with the
Gemini-North Telescope on 2008 June 25.5 to limiting magnitudes of
approximately 22.0, 20.5, and 20.0, respectively.  No known minor planets
were near the source within 10' at the time of the NICMOS observations.
Thanks to the high spatial resolution (FWHM about 0".15) of the data, they
were able to determine that the source was stationary with a precision of
0".02 when compared to the field stars between the first and the last
NICMOS images that were separated by about 40 minutes.  This rules out any
solar-system object (Delta < 10000 AU) as the origin for the transient
source, as it would have a proper motion larger than 0.1 arcsec/hour.
Furthermore, due to the high ecliptic latitude (about 13 deg) of IRAS
17138-1017, a minor planet close to its stationary point can also be ruled
out as the origin of the source.  A variable foreground star also provides
a very improbable alternative explanation, given the small field-of-view
(19".8 x 19".8) of the NICMOS frames.  Based on these arguments and the
fact that large numbers of core-collapse supernovae are expected in the
nuclear regions of IRAS 17138-1017 as a result of the large star-formation
rate therein (Kankare et al. 2008, Ap.J. Let., accepted;
http://lanl.arxiv.org/abs/0810.2885) it is concluded that explanations
other than a supernova for this object are extremely unlikely.  Searches
of non-publicly-accessible observatory archives for observations in 2004
and 2005 that could include IRAS 17138-1017 are encouraged.

2009 DD_45
     R. P. Binzel, M. Birlan, and F. E. DeMeo, Paris Observatory,
report on their 0.8- to 2.5-micron spectroscopic measurements of
2009 DD_45 (cf. MPEC 2009-D80) on Mar. 2.6 UT using the NASA
Infrared Telescope Facility 3-m reflector on Mauna Kea.  Absorption
bands revealed at 1 and 2 microns show the characteristics of the
S-type class of minor planets.   Using the average albedo value of
0.36 for small near-earth objects in this class (Delbo et al. 2003,
Icarus 166, 116), and based on its H magnitude (25.4), the mean
diameter is estimated to be 19 +/- 4 m.  The Apollo-type object
passed only 0.000482 AU from the earth on Mar. 2.57 (cf. MPEC
2009-E10).

(4607) SEILANDFARM
     D. Pray, Carbuncle Observatory, W. Brookfield, MA, U.S.A.; P. Kusnirak
and P. Pravec, Ondrejov Observatory; J. Gross, W. Cooney, and D. Terrell,
Sonoita Research Observatory, Sonoita, AZ; and R. Durkee, Minneapolis, MN,
report that photometric observations obtained during Jan. 17-Feb. 25 reveal
that minor planet (4607) is a binary system with an orbital period of 31.63
+/- 0.02 hr.  The primary shows a period of 3.9683 +/- 0.0001 hr, and it has
a lightcurve amplitude of 0.15 mag, suggesting a nearly spheroidal shape.
Mutual eclipse/occultation events indicate a lower limit on secondary-to-
primary mean-diameter ratio of 0.29.

(2577) LITVA
     B. D. Warner, Palmer Divide Observatory and Space Science Institute,
Colorado Springs, CO, U.S.A.; P. Pravec, Ondrejov Observatory; A. W. Harris,
Space Science Institute, La Canada, CA, U.S.A.; D. Higgins, Hunters Hill
Observatory, Ngunnawal, ACT, Australia; C. Bembrick, Mt. Tarana Observatory,
Bathurst, NSW, Australia; and J. Brinsfield, Via Capote Observatory, Thousand
Oaks, CA, U.S.A. report that photometric observations obtained during Feb.
28-Mar. 8 reveal that minor planet (2577) is a binary system with an orbital
period of 35.78 +/- 0.05 hr.  The primary shows a period of 2.8141 +/- 0.0006
hr, and it has a lightcurve amplitude of 0.24 mag.  Mutual eclipse/occultation
events indicate a secondary-to-primary mean-diameter ratio of 0.35 +/- 0.02.
The periods and amplitudes were determined using a subset of data (Mar. 4-8).
Data on Feb. 28 and Mar. 1 show no events and fit the same primary period, but
the lightcurve has a slightly different shape; this may indicate that the
primary lightcurve is evolving with changing viewing aspect, and so additional
observations are warranted as the moon clears the area.

(6708) BOBBIEVAILE
     D. Pray, Carbuncle Observatory, W. Brookfield, MA, U.S.A.; K. Hornoch,
P. Kusnirak, and P. Pravec, Ondrejov Observatory; V. Chiorny and Yu. Krugly,
Kharkiv Observatory; M. Husarik and M. Pikler, Skalnate Pleso Observatory;
F. Marchis, B. Macomber, and M. Kislak, SETI Institute and University of
California at Berkeley; and J. Vilagi and S. Gajdos, Modra Observatory,
report that photometric observations obtained during Apr. 16 to May 3 reveal
that minor planet (6708) is a binary system with an orbital period of
24.7 hr.  The primary shows a period of 8.221 +/- 0.002 hr, assuming a bi-
modal lightcurve, and it has a lightcurve amplitude of 0.08 mag, suggesting
a nearly spheroidal shape.  Mutual eclipse/occultation events with a depth
of 0.31 mag indicate a lower limit on the secondary-to-primary mean-diameter
ratio of 0.57.  The mean absolute R-band magnitude of the system is H =
12.81 +/- 0.14, assuming G = 0.25 +/- 0.2.

2009 HC_82
     Another minor planet in a retrograde orbit but showing no
apparent cometary features has been discovered (cf. MPEC 2009-J04)
by the Catalina Sky Survey.  The following orbital elements are
from MPO 157545:

(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.

(136617) 1994 CC
     M. Brozovic and L. A. M. Benner, Jet Propulsion Laboratory
(JPL), California Institute of Technology (CIT); M. C. Nolan and E.
S. Howell, Arecibo Observatory; C. Magri, University of Maine at
Farmington; J. D. Giorgini, JPL; P. A. Taylor, Arecibo Observatory;
J. L. Margot, University of California, Los Angeles; M. W. Busch,
CIT; M. K. Shepard, Bloomsburg University; L. M. Carter,
Smithsonian Institution; J. S. Jao, J. Van Brimmer, C. R. Franck,
M. A. Silva, M. A. Kodis, D. T. Kelley, and M. A. Slade, JPL; A.
Bramson, University of Wisconsin; K. J. Lawrence, JPL; J. T.
Pollock, Appalachian State University; P. Pravec, Ondrejov
Observatory; and D. E. Reichart, K. M. Ivarsen, J. Haislip, M. C.
Nysewander, and A. P. LaCluyze, University of North Carolina,
Chapel Hill, report that Goldstone (8560-MHz, 3.5-cm) and Arecibo
(2380-MHz, 12.6-cm) delay-Doppler radar images obtained on June
12-15 reveal that minor planet (136617) is a triple system.
Visible range extents in 19-m-resolution Goldstone data from June
12 suggest preliminary diameter estimates of 650 m for the primary
and at least 50 m and 100 m for the satellites, whose orbital
separations from the primary were at least 0.5 km and 1.2 km.
Photometry obtained with the Panchromatic Robotic Optical
Monitoring and Polarimetry Telescopes (PROMPT) reveals a 0.05-mag-
deep attenuation centered on June 3.04 UT, suggesting a satellite
eclipse/occultation, and yields a lightcurve amplitude of 0.09 mag
and rotation period of 2.3886 +/- 0.0001 hr for the primary.

(26471) 2000 AS152
     B. D. Warner, Palmer Divide Observatory and Space Science Institute,
Colorado Springs, CO; A. W. Harris, Space Science Institute, La Canada, CA;
and D. Pray, Carbuncle Hill Observatory, West Brookfield, MA, report that
photometric observations obtained during July 13-19 reveal that minor planet
(26471) is a binary system with an orbital period of 1.634 +/- 0.001 days.
The primary shows a period of 2.6866 +/- 0.0002 hr and has a lightcurve
amplitude of 0.22 mag.  Mutual eclipse/occultation events indicate the lower
limit of the secondary-to-primary mean diameter to be 0.38 +/- 0.02.  The
observations for July 19 indicate the possibility that a shadow event, where
the shadow of the secondary transited the primary, was also observed.  If
this is the case, then continued observations at different phase angles may
show an evolution in the combined and separated lightcurves.

S/2009 (93) 1 AND S/2009 (93) 2
     F. Marchis and B. Macomber, Carl Sagan Center at the SETI
Institute and University of California at Berkeley; J. Berthier and
F. Vachier, Institut de Mecanique Celeste et de Calcul des
Ephemerides, Observatoire de Paris; and J. P. Emery, University of
Tennessee, Knoxville, report that adaptive-optics images were
recorded of (93) Minerva, a large C-type main-belt asteroid, with
the 10-m Keck II telescope [+ NIRC2 camera (angular resolution up
to 0".042, corresponding to a spatial resolution of 65 km) + Fe II
filter (central wavelength at 1.64 microns)] between Aug. 16.57 and
16.64 UT, with the target at r = 2.117 AU and phase angle 20.0 deg.
The direct images reveal that the large minor planet has an almost-
spherical shape with an average diameter of 145 km.  Additionally,
these observations show the presence of a companion about 4 km in
diameter at 0".41 (projected distance of 630 km) in p.a. 275 deg
detected in every image recorded over the 1.8-hr baseline.  Careful
analysis of three images indicates the presence of a second
satellite (about 3 km) and located closer to the primary at an
apparent distance of 380 km (0".25) in p.a. 209 deg.  With (87)
Sylvia (cf. IAUC 8582), (45) Eugenia (cf. IAUC 8817), and (216)
Kleopatra (cf. IAUC 8980), this is the fourth multiple system with
two small-kilometer-sized satellites to be discovered and imaged in
the main asteroid belt.

2000 CO_101
     P. A. Taylor, M. C. Nolan, and E. S. Howell, Arecibo Observatory, NAIC;
C. Magri, University of Maine at Farmington; L. A. M. Benner, M. Brozovic,
and J. D. Giorgini, Jet Propulsion Laboratory, California Institute of
Technology; M. W. Busch, California Institute of Technology; M. K. Shepard,
Bloomsburg University; and J. L. Margot, University of California, Los
Angeles, report that Arecibo (2380-MHz, 12.6-cm) radar observations made on
Sept. 26 reveal that minor planet 2000 CO_101 (cf. MPEC 2000-D04) is a binary
system.  Preliminary estimates of the component diameters, based on visible
range extents, are 525 m for the primary and 45 m for the secondary.  The
maximum range-Doppler separation between the components was 560 m and 1.1 Hz
at Sept. 26.95 UT.

(1509) ESCLANGONA
     B. D. Warner, Palmer Divide Observatory and Space Science Institute,
Colorado Springs, CO; P. Pravec and P. Kusnirak, Ondrejov Observatory; A.
W. Harris, Space Science Institute, La Canada, CA; R. Durkee, Shed of
Science Observatory, Minneapolis, MN; R. D. Stephens, Goat Mountain Research
Station, Landers, CA; M. Husarik and M. Pikler, Skalnate Pleso Observatory; F.
Marchis and A. E. Reiss, SETI Institute and University of California at
Berkeley; J. Vilagi, S. Gajdos, and L. Kornos, Modra Observatory; W. Cooney,
J. Gross, and D. Terrell, Sonoita Research Observatory, Sonoita, AZ; and F.
Vachier, Institut de Mecanique Celeste et de Calcul des Ephemerides,
Observatoire de Paris, report that photometric observations of minor planet
(1509) obtained during Sept. 9-Oct. 27 reveal two distinct periods:
3.25285 +/- 0.00002 and 6.6423 +/- 0.0003 hr.  The lightcurve components
associated with two periods are linearly additive and have amplitudes of
0.13 and 0.04 mag, respectively.  It appears likely that these two lightcurve
components are due to the rotations of the primary and secondary, respectively,
of the wide binary reported in 2003 by Merline et al. (IAUC 8075).  The
separation of the two objects observed by Merline et al. is so large that
catching mutual events (occultations and/or eclipses) is unlikely.  Previous
CCD observations (Warner 2005, Minor Planet Bull. 32, 54-58) did not show any
indications of a secondary period or mutual events.

S/2009 (317) 1
     W. J. Merline, Southwest Research Institute (SwRI); P. M. Tamblyn,
Binary Astronomy, Dillon, CO, and SwRI; J. D. Drummond, Starfire Optical
Range, AFRL; J. C. Christou, Gemini Observatory; A. R. Conrad, W. M. Keck
Observatory; B. Carry, Observatoire de Paris, France; C. R. Chapman, SwRI;
C. Dumas, European Southern Observatory, Chile; D. D. Durda, SwRI;
W. M. Owen, Jet Propulsion Laboratory; and B. L. Enke, SwRI, write:
"We report the discovery on Nov. 24.4 UT of a satellite of minor planet
(317) Roxane from Kp-band imaging using the 8-m Gemini-North telescope
(+ Altair/NIRI adaptive optics system).  On Nov. 24.39992 UT, the
satellite was at separation 0".27 (projected separation 245 km) and
position angle 76 deg.  The satellite was imaged in Kp-, H-, and J-bands and
was tracked for more than 26 hours.  The brightness difference in Kp-band is
about 2.7 mag, giving an estimated diameter (primary diameter assumed
of 19 km) of the satellite of 5 km.  This binary has characteristics very
similar to the other wide binaries previously reported by our group
(see IAUCs 7827, 8075, 8232, 8293, 8297), all being consistent with the EEB
formation mechanism of Durda et al. (2004 Icarus 170, 243).  Among
binaries that can be resolved by imaging, this appears to be the first
E-type.  Given the recent detection of dual lightcurve periods in (1509)
Esclangona (CBET 2020), it is possible that separate spin periods could be
extracted from lightcurve data on (317)."

S/2009 (317) 1
     W. J. Merline, Southwest Research Institute (SwRI); P. M.
Tamblyn, Binary Astronomy, Dillon, CO, U.S.A., and SwRI; J. D.
Drummond, Starfire Optical Range, Air Force Research Laboratory;
J. C. Christou, Gemini Observatory; A. R. Conrad, W. M. Keck
Observatory; B. Carry, Observatoire de Paris; C. R. Chapman, SwRI;
C. Dumas, European Southern Observatory (Chile); D. D. Durda, SwRI;
W. M. Owen, Jet Propulsion Laboratory; and B. L. Enke, SwRI, report
the discovery on Nov. 24.4 UT of a satellite of minor planet (317)
Roxane from K_p-band imaging using the 8-m Gemini-North telescope
(+ Altair/NIRI adaptive-optics system).  On Nov. 24.39992, the
satellite was at separation 0".27 (projected separation 245 km) and
position angle 76 deg.  The satellite was imaged in K_p-, H-, and
J-bands and was tracked for more than 26 hours.  The brightness
difference in the K_p band is about 2.7 mag, giving an estimated
diameter (primary diameter assumed of 19 km) of the satellite of 5
km.  This binary has characteristics that are very similar to the
other wide binaries previously reported by the authors (see IAUCs
7827, 8075, 8232, 8293, 8297), all being consistent with the EEB
formation mechanism of Durda et al. (2004, Icarus 170, 243).  Among
binaries that can be resolved by imaging, this appears to be the
first of type E.  Given the recent detection of dual lightcurve
periods in (1509) Esclangona (CBET 2020), it is possible that
separate spin periods could be extracted from lightcurve data of
(317).

(2131) MAYALL
     B. Warner, Palmer Divide Observatory; P. Pravec, P. Kusnirak, and
K. Hornoch, Ondrejov Observatory; J. Vilagi, L. Kornos, S. Gajdos, P. Veres,
and A. Galad, Modra Observatory; W. Cooney, J. Gross, and D. Terrell,
Sonoita Research Observatory, Sonoita, AZ; and Yu. Krugly and V. Chiorny,
Kharkiv Observatory, report that photometric observations obtained during
Nov. 30-Dec. 16 reveal that minor planet (2131) is a binary system with an
orbital period of 23.48 +/- 0.01 hr.  The primary shows a period of 2.5678
+/- 0.0001 hr and has a lightcurve amplitude of 0.09 mag, suggesting a
nearly spheroidal shape.  The secondary rotates synchronously with the
orbital motion, and its lightcurve component has an amplitude of 0.05 mag.
Observed mutual-eclipse/occultation events indicate a secondary-to-primary
mean-diameter ratio of 0.28 +/- 0.02.
     Observations in 2005 (Warner 2005, Minor Planet Bull. 32, 54-58) and
2007 (Warner et al. 2007, Minor Planet Bull. 34, 23) showed no indications
of (2131) being binary.

COMET P/2010 A2 (LINEAR)
     Further to IAUC 9105, the following improved orbital elements
(from MPEC 2010-A78) for this comet are like those of a minor
planet in the inner part of the main belt:  T = 2009 Nov. 17.248 TT,
q = 1.97580 AU, e = 0.13178, Peri. = 125.600 deg, Node = 321.073
deg, i = 5.099 deg (equinox 2000.0), P = 3.43 years.
     J. V. Scotti, Lunar and Planetary Laboratory, reports that
there is no distinct nuclear condensation on CCD images of this
comet taken by R. S. McMillan with the Spacewatch 1.8-m f/2.7
reflector on Jan. 8.2 and 12.4 UT; on Jan. 8, the coma size was
about 8" x 11", with a sharper edge on the northern boundary, and a
long, narrow tail at least 4'.6 long in p.a. 279 deg; a faint spike
extended 0'.34 in p.a. 137 deg.
     D. Jewitt, University of California at Los Angeles; and J.
Annis and M. Soares-Santos, Fermilab, report observations of P/2010
A2 from Jan. 11 and 12 UT with the WYNN 3.5-m telescope on Kitt
Peak.  The object appears as a point-like body of red mag 23.0 +/-
0.5 located 2".5 +/- 0".5 east of the apex of a broad, low-surface-
brightness dust tail; the latter lacks strong condensation and is
more than 5' in length (see website URL
http://www2.ess.ucla.edu/~jewitt/MBC5.html).  The detected nucleus
is approximately 150-200 m in diameter (assuming albedo 0.1),
connected to the tail by an unresolved light bridge.  With
semimajor axis less than Jupiter's, and Tisserand parameter 3.6,
P/2010 A2 is the fifth recognized example of a main-belt comet (MBC),
differing from other MBCs in being an inner-belt object (orbit
consistent with membership in the Flora family).  The location of
the nucleus outside the tail suggests a recent impulsive origin for
P/2010 A2, perhaps from a recent collision between two previously
unseen minor planets, with radiation pressure driving the
separation between the nucleus and the tail.  In this scenario, the
bridge consists of large impact-produced particles slowly
separating from the nucleus under radiation pressure and Kepler
shear.  Future observations are encouraged to test this hypothesis.
     J. Licandro, Instituto de Astrofisica de Canarias; G. P. Tozzi,
Istituto Nazionale di Astrofisica, Arcetri; and T. Liimets, Nordic
Optical Telescope (NOT) and Tatru Observatory, report that 5-min R-
and V-band exposures obtained on Jan. 14.945-14.985 UT with the
2.5-m NOT (+ ALFOSC) shows the presence of an asteroidal object 2"
east of (and moving at the same rate as) the uncondensed "dust
swarm" of P/2010 A2, which itself is 4' long (177000 km at the
comet's distance) and about 5" wide in p.a. 277 deg.  Similar
reports of the comet's appearance have been received from other
observers, including R. Haver and L. Buzzi.

COMET P/2010 A2 (LINEAR)
     [Editor's note:  this CBET contains additional information that
could not be published on IAUC 9109 because of printing/space constraints,
due to the great interest in this unusual object.]
     Further to IAUC 9105, the following improved orbital elements (from
MPEC 2010-A78) for this comet are like those of a minor planet in the inner
part of the main belt: