Jul-Sep, 34-3 - MinorPlanet.Info

Transcription

THE MINOR PLANET
BULLETIN
BULLETIN OF THE MINOR PLANETS SECTION OF THE
ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS
VOLUME 34, NUMBER 3, A.D. 2007 JULY-SEPTEMBER
CCD PHOTOMETRY OF ASTEROID 22 KALLIOPE
Can Gungor
Department of Astronomy, Ege University
35100 Bornova Izmir TURKEY
[email protected]
53.
Kwee, K.K. and von Woerden, H. (1956). Bull. Astron. Inst. Neth.
12, 327
Trigo-Rodriguez, J.M. and Caso, A.S. (2003). “CCD Photometry
of asteroid 22 Kalliope and 125 Liberatrix” Minor Planet Bulletin
30, 26-27.
(Received: 13 March)
CCD photometry of asteroid 22 Kalliope taken at
Tubitak National Observatory during November 2006 is
reported. A rotational period of 4.149 ± 0.0003 hours
and amplitude of 0.386 mag at Johnson B filter, 0.342
mag at Johnson V are determined.
The observation of 22 Kalliope was made at Tubitak National
Observatory located at an elevation of 2500m. For this study, the
410mm f/10 Schmidt-Cassegrain telescope was used with a SBIG
ST-8E CCD electronic imager. Data were collected on 2006
November 27. 305 images were obtained for each Johnson B and
V filters. Exposure times were chosen as 30s for filter B and 15s
for filter V. All images were calibrated using dark and bias frames
and sky flats.
Figure 1. Lightcurve of 22 Kalliope for Johnson B filter. X axis is
JD-2454067.00. Ordinate is relative magnitude.
During this observation, Kalliope was 99.26% illuminated and the
phase angle was 9º.87 (Guide 8.0). Times of observation were
light-time corrected. Reduction of frames was made with IRAF
software. For differential photometry, GSC 1876 748 was used as
a comparison star. The times of minima were computed by the
Kwee-van Woerden method (Kwee & van Woerden, 1956).
The rotational period for 22 Kalliope from the data presented is
4.149 ± 0.0003 hours. This is similar to the Trigo-Rodriguez
(2003) value of 4.144 hours. The amplitude of lightcurve for filter
B is 0.386 mag while the amplitude for filter V is 0.342 mag.
Lightcurves are presented in Figure 1 for filter B and Figure 2 for
filter V.
Acknowledgments
Many thanks to Tubitak National Observatory for use telescope
time allocation and other facilities.
Figure 2. Lightcurve of 22 Kalliope for Johnson V filter. X axis is
JD-2454067.00. Ordinate is relative magnitude.
References
Guide 8.0 Software, http://www.planetpluto.com
SUBSCRIPTION INCREASE NOTICE
See page 55.
Minor Planet Bulletin 34 (2007)
Available on line http://www.minorplanetobserver.com/mpb/default.htm
54
PHOTOMETRY OF ATEN ASTEROID (66146) 1998 TU3
Tom Richards
Woodridge Observatory
8 Diosma Rd
Eltham, Vic 3095, Australia
[email protected]
An eleven-point moving average was constructed for the phase
plot, which gave an amplitude of 0.10 ± 0.01 mag, rather less than
published figures, e.g. in Pravec et al (2005). The epoch used was
JD 2452919.2132
Fuller information may be found on the first author’s website,
http://www.woodridgeobsy.org.
Greg Bolt
Craigie, WA, Australia
References
David Higgins
Hunters Hill Observatory
Ngunnawal, Canberra ACT, Australia
Colin Bembrick
Mt Tarana Observatory
Bathurst, NSW, Australia
Bembrick, C. (2005). “Asteroid Research and Amateur Input”.
Southern Stars, 44:3, 16-19.
Binzel, R.P., Lupishko, D.F., Di Martino, M., Whiteley, R.J. and
Hahn, G.J. (2002). “Physical Properties of Near Earth Objects” in
Asteroids III (W. F. Bottke, A. Cellino, P. Paolicchi, R. P. Binzel,
eds.), pp. 255-271. Univ. Arizona Press, Tucson.
(Received: 21 March )
Harris, A.W., Warner, B.D. (2006). “Minor Planet Lightcurve
Parameters”.
http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html
Eleven sets of photometric data for (66146) 1998 TU3
were obtained over a 14 day period in 2003 October. A
synodic rotation period of 2.3779 ± 0.0004 h with
amplitude 0.10 mag was derived, close to other
published data.
Hartley, M., Russell, K. S., Savage, A. Asher, D. J., Broughton, J.,
Hergenrother, C. W., Williams G. V., and Nakano, S. (1999).
“1998 TU3” M P E C 1998 U03, available from
http://adsabs.harvard.edu/abs/.
Minor planet (66146) 1988 TU3 was discovered by the LINEAR
NEO survey on 1998 Oct 13. Orbital elements show it is an Aten
asteroid (Tesi et al 1998 and Hartley et al 1999). It has been
assigned to the taxonomic class Q (Whiteley 2001) and based on
its albedo its diameter is given at 3.6 km (Binzel et al 2002).
Higgins, D. (2007). “Minor Planet Lightcurves”.
http://www.david-higgins.com/Astronomy/asteroid/lightcurves
.htm
Harris & Warner (2006) give a period of 2.375 h, referencing
Világi (2002) and Pravec et al. (2005). Világi’s paper shows
lightcurves from two nights in 2001 October, but provides no
period. Pravec et al.’s table gives a period of 2.3767 ± 0.0009 h,
listing Vilagi’s paper as the source. It also lists a period of 2.37741
± 0.00004 h, from dates in Aug-Sep 2003 near those of the present
study. For another discussion of some of the data in the present
paper see (Bembrick, 2005).
The present study was triggered by a request for observations of
this earth-crossing asteroid at a close opposition. It consists of
eleven observation sets, as follows, all obtained with unfiltered
CCD cameras (except Higgins who used an R filter). Obs lists the
observer’s initials (see author list above), and Data the number of
data points in the observation set (with a total of 4689). Richards
used an 18 cm refractor, Bolt a 25 cm SCT, Higgins a 25 cm SCT,
and Bembrick a 40 cm SCT. Higgins’s data and results are
available separately on his personal website (Higgins 2007) for
which there is a quoted period of 2.37745 + 0.00005 h, as well as
a phase plot.
All observations were corrected for light-time. Period analysis was
carried out in Peranso 2.10 (Vanmunster, 2007). Numerous period
analysis algorithms were applied, but ANOVA (SchwarzenbergCzerny 1996) produced the minimum period error and visually the
tightest phase plot, as shown in the Figure. The resulting period
was 2.3779 ± 0.0004 h, slightly higher than the published periods
given above. A phase plot on the present data using the nearest
published period figure of 2.37741 h, is noticeably less coherent.
Lightcurve for (66146) 1998 TU3, corrected for light-time and
phased to 2.3779 h.
1
2
3
4
5
6
7
8
9
10
11
Date
2003.10.06
2003.10.06
2003.10.07
2003.10.08
2003.10.09
2003.10.13
2003.10.14
2003.10.15
2003.10.16
2003.10.17
2003.10.19
Obs
TR
GB
GB
GB
CB
TR
DH
GB
TR
TR
TR
Data
638
745
547
732
162
115
267
524
506
358
95
Phase
29.8
29.9
30.4
31.1
31.8
35.8
37.0
38.2
39.4
40.6
43.1
LPAB
7.4
7.4
6.7
6.1
5.5
2.9
2.3
1.8
1.4
1.0
0.2
BPAB
-19.8
-19.8
-19.7
-19.7
-19.5
-18.9
-18.6
-18.4
-18.2
-18.0
-17.4
55
Pravec, P., Wolf, M., and Sarounova, L. (2005). “Ondrejov
Asteroid Photometry Project”, posted on
http://www.asu.cas.cz/~ppravec/neo.htm.
Schwarzenberg-Czerny, A. (1996). Ap J.460, L107-110.
Tesi, L., Forti, G., Garradd, G. J., Broughton, J., Rogers, J. E.
,Blythe, M., Shelly, F., Bezpalko, M., Stuart, J., Viggh, H., Sayer,
R., Griffin, I. P., Mendez, O., Scheck, J., Salvo, R., and Williams,
G. V. (1998). “1998 TU3” MPEC 1999-C09, available from
http://adsabs.harvard.edu/abs/
Vanmunster, T. (2007) “PERANSO Period Analysis and Light
Curve Software”.
http://users.skynet.be/fa079980/peranso/index.htm.
Világi, J. (2002). “Asteroid photometry program at Modra
Observatory” in Proceedings of Asteroids, Comets, Meteors –
ACM 200, pp. 907-910.
Figure 1. Dramatic upturn in number of asteroid rotations reliably
known. (Figure credit: Alan W. Harris).
Whiteley, R.J. (2001). A Compositional and Dynamical Survey of
the Near-Earth Asteroids. PhD. Thesis, University of Hawaii.
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enabled by the CCD revolution. Asteroid observations remain an
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contributions by free electronic subscribers are rare. If you are
reading this electronically, and the MPB is valuable to you, please
think again about making a voluntary contribution (page 94).
Figure 2. Number of lightcurves published each year in the MPB,
showing amateur contributions as the major contributor to the
upturn in Figure 1. (Data compiled by Derald Nye.)
140
120
Pages Published per Year in
the Minor Planet Bulletin
100
Pages
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80
60
40
20
0
1985
1990
1995
2000
2005
Year
Figure 3. Total number of MPB pages published each year since
1985. Final column is a projection for total pages in 2007. (Figure
credit: Bob Werner).
Richard P. Binzel, Editor
Minor Planet Bulletin
56
LIGHTCURVE ANALYSIS OF 22 KALLIOPE
Acknowledgement
Kevin B. Alton
70 Summit Ave
Cedar Knolls, NJ 07927
[email protected]
The assistance and encouragement by Brian D. Warner to conduct
my first photometric survey of an asteroid is gratefully
appreciated.
References
(Received: 1 April
Revised: 29 April)
Lightcurves for 22 Kalliope were obtained over five
nights in January and February 2007 using a CCD
camera. Filtered (I-band) photometric exposures were
used to calculate the synodic period (4.148288 hr) and
estimate the axial ratio (a/b ≥ 1.51).
22 Kalliope (~181 km) was first detected by Hind in 1852. Margot
and Brown (2003) discovered that Kalliope is orbited by a
companion satellite, since named Linus. Although the original
objective of this photometric campaign was to capture eclipse
events (1E2 and 2E1) that were predicted for this binary system
from late February through early April, poor weather conditions
precluded this possibility.
Equipment utilized included a 0.2-m Vixen VC200L catadioptric
(f/6.4) with an SBIG ST 402ME CCD camera mounted at the
primary focus running at –10° C and B, V and I filters based upon
the Bessell specification. I-band imaging was carried out on a
total of seven nights, five of which produced acceptable light
curves and are reported herein. Multiple bandwidth (V, B, and I)
filtered images were taken only on a single evening (February 10,
2007). Exposures were unbinned and 15 sec for each filter. A
typical session lasted from 2.5 to 4 hours with exposures
automatically taken at least every 90 seconds. Image acquisition
(raw lights, darks and flats) was performed using CCDSOFT 5
(SBIG) while calibration and registration were accomplished with
AIP4WIN (Berry and Burnell 2005). Further image reduction
with MPO Canopus (Warner 2006) was achieved using at least
four non-varying comparison stars to generate light curves by
differential aperture photometry. Instrumental readings were
light-time corrected but not reduced to standard magnitudes.
Berry, R. and Burnell, J. (2005). AIP4WIN version 2.1.0,
Willmann-Bell, Inc, Richmond, VA.
Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L.,
Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne,
H, and Zeigler, K. (1989). “Photoelectric Observations of
Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.
Margot, J.L. and Brown, M.E. (2003). “A Low Density M-type
Asteroid in the Main Belt”. Science 300, 1939-1942.
Michalowki, T., Velichko, F.P. (1990). “Photoelectric Photometry,
Parameters of Rotation and Shapes of 22 Kalliope and 79
Eurynome”. Acta Astron 40, 321-332.
Trigo-Rodríguez, J.M. and Caso, A.S. (2003). “CCD Photometry
of Asteroids 22 Kalliope and 125 Liberatrix”. Minor Planet
Bulletin 30, 26-27.
Vannmunster, T. (2006). Peranso Period Analysis Software,
Peranso version 2.10, CBA Belgium Observatory.
Warner, B.D. (2006). MPO Software, Canopus version 9.2.1.0.
Bdw Publishing, Colorado Springs, CO.
A total of 1283 photometric readings in I-band produced
lightcurves that spanned three weeks. Relevant aspect parameters
for Kalliope taken at the mid-point from each session are shown in
the table. Lightcurves exhibited the expected bimodality consistent
with an asteroid having a triaxial ellipsoid shape. MPO Canopus
provided a period solution for the folded data sets using Fourier
analysis (Harris 1989). The synodic period, determined to be
4.148288 ± 0.000001 hr, was in excellent agreement with
rotational periods for 22 Kalliope published by Michalowski and
Velichko (1990) and Trigo-Rodríguez and Caso (2003).
Periodograms produced using “Peranso” (Vannmunster 2006) by
applying periodic orthogonals to fit observations and analysis of
variance (ANOVA) to evaluate fit quality, confirmed this period
determination.
The estimated peak-to-peak maximum change in magnitude
(0.445 mag) suggests an axial ratio (a/b) of at least 1.51 where a/b
≥ 100.4•∆mag. This value falls within the range (1.32 – 1.6) reported
by other investigators (Michalowski and Velichko 1990). V-, B-,
and I-band filtered images of Kalliope showed no notable color
effects.
UT Date
(2007)
No.
Obs
Phase
Angle
LPAB
BPAB
%Phase
Coverage
Jan 26
Feb 8
Feb 9
Feb 10
Feb 17
322
250
251
209
251
15.4
18.5
18.7
19
20
88.5
89.9
90.1
90.3
91.2
8.5
8.9
8.9
9.0
9.1
63.2
88.9
87.1
105.5
85.5
57
LIGHTCURVE RESULTS FOR 81 TERPSICHORE,
242 KRIEMHILD, 503 EVELYN, 522 HELGA, AND
578 HAPPELIA
Michael Fauerbach, Thomas Bennett, Scott A. Marks
Egan Observatory
Florida Gulf Coast University
10501 FGCU Blvd.
Fort Myers, FL 33965
[email protected]
(Received: 11 April)
We report lightcurve periods of five main belt asteroids
observed at the Egan Observatory during the late 2005
early 2006 observing campaign.
The Evelyn L. Egan Observatory is located on the campus of
Florida Gulf Coast University in Fort Myers, Florida. Details on
the equipment and experimental methods can be found in
Fauerbach and Bennett (2005). The data were analyzed with MPO
Canopus Version 9, which employs differential aperture
photometry to determine the values used for analysis. Canopus
was also used for period analysis, using the Fourier analysis
algorithm developed by Harris (1989). The targets were chosen by
comparing well placed asteroids to the list of known lightcurve
parameters maintained by Harris and Warner (2006). We focused
our observations on those asteroids for which only one prior
–sometimes incomplete or inconclusive – measurement had been
published.
81 Terpsichore. The period of this asteroid was first derived by
K.W. Zeigler (1990) in 1985. Zeigler derived a period of 11.02 h,
which fits well with our derived period of 11.027 ± 0.010 h. The
observed magnitude was less than 0.1 magnitude.
242 Kriemhild. Warner (2005) derived a rotational period for this
asteroid of 4.543 ± 0.005 h, which is in excellent agreement with
our period of 4.545 ± 0.010 h. Due to the different viewing
geometry of the observations in 2005 and 2006, our data show a
significantly larger amplitude of about 0.3 magnitude versus the
0.08 magnitude measured by Warner.
± 0.010 h. In the meantime Licchelli (2006) had published his
results on 522 Helga, taken just prior to ours, which are in
excellent agreement with our independently derived results.
Combining the two data sets – yielding phase angle coverage from
11.9o prior to opposition to 16.4o after opposition – would be an
interesting undertaking.
578 Happelia. Robinson (2002) derived a period of 10.00 ± 0.05 h
for this asteroid. This is in good agreement with our measurement
of 10.061 ± 0.010 h.
The results are summarized in the table below, and the individual
lightcurve graphs are presented afterwards. For display purposes,
we binned the data in each graph by a factor of two.
Acknowledgements
We would like to dedicate this paper to the memory of the late
Mrs. Evelyn L. Egan. Without her generous support, this work, as
well as all the educational activities around the observatory, would
not have been possible.
References
Fauerbach, M. and Bennett, T. (2005). “First Photometric
Lightcurve measurements from the Evelyn L. Egan Observatory,”
Minor Planet Bul. 32-2, 34-35
Harris, A.W., and Warner B.D. (2006).
Kamel, L., Lundgren, K. (1999). “The Lightcurve of 503 Evelyn,”
Minor Planet Bul. 26, 4-5.
Lagerkvist, C.-I., Erikson, A., Lahulla, F., Di Martino, M.,
Nathues, A., and Dahlgren, M. (2001). Icarus 149, 190-197.
Licchelli, D. (2005). “Lightcurve Analysis of Asteroids 78, 126,
522, 565, 714, 1459, 6974”. Minor Planet Bul. 33-1, 11-13.
503 Evelyn. The only previously existing lightcurve measurement
for 503 Evelyn was made by Kamel and Lundgren (1999) in 1996.
They derived a rotational period of 38.71 h, which is in good
agreement with our derived period of 38.70 ± 0.01 h. Our
observed amplitude of 0.35 magnitude is however significantly
smaller than the previously observed amplitude of almost 1
magnitude.
Robinson, L.E. (2002). “Photometry of Five Difficult Asteroids:
309 Fraternitas, 366 Vincentina 421 Zahringia, 578 Happelia, 959
Anne”. Minor Planet Bul. 29-1, 30-31.
522 Helga. At the time of our observations of asteroid 522 Helga
only one published period by Lagerkvist et al. (1991) of 3.4 h
existed. After the first night on target, it became obvious that this
result could not be correct. Utilizing measurements from late
October to early December of 2005, we derived a period of 8.126
Zeigler, K.W. (1990). “Photoelectric Photometry of Asteroids 81
Terpsichore, 381 Myrrha, and 1986 DA”. Minor Planet Bul. 17, 13.
#
Name
Date Range
(mm/dd/yyyy)
81 Terpsichore 01/05/2006 - 03/07/2006
242 Kriemhild
12/02/2005 - 12/04/2005
503 Evelyn
12/02/2005 - 03/03/2006
522 Helga
10/29/2005 - 12/03/2005
578 Happelia
10/27/2005 - 10/30/2005
Warner, B.D. (2005). “Lightcurve Analysis for Asteroids 242,
893, 921, 1373, 1853, 2120, 2448, 3022, 6490, 6517, 7187, 7757,
and 18108”. Minor Planet Bul. 32-1, 4-7.
Data
Phase
LPAB
BPAB
Pts
365 18.5,1.3,1.9 161.5,163.4
4.3,2.9
149
16.4,16.8
23.6
-1.0
497
5.1,25.6
60.0,77.0 -0.7,+1.8
245
11.1,16.4
0.4,3.5 -4.8,-4.6
229
5.9,6.8
21.3
-0.7
Per
(h)
11.027
4.545
38.70
8.126
10.061
PE
0.010
0.010
0.01
0.010
0.010
58
THE ROTATION PERIODS OF
36 ATALANTE AND 416 VATICANA
James W. Brinsfield
Via Capote Observatory
5180 Via Capote, Thousand Oaks CA 91320
[email protected]
(Received: 7 April)
Lightcurves for 36 Atalante and 416 Vaticana were
obtained at Via Capote Observatory during 2007
February-March. The synodic rotation periods were
found to be: 9.93±0.01 hr and 5.38±0.01hr, respectively.
A lower amplitude (0.06 mag.) than previously reported
may be due to a more pole-on aspect for 416 Vaticana.
Observations of 36 Atalante and 416 Vaticana were made using a
Takahashi Cassegrain at prime focus resulting in a focal length of
136 inches and a focal ratio of f11.5. The CCD imager was an Alta
U6 featuring a 1024x1024 array of 24 µ-meter pixels. The CCD
was operating at a temperature of –30°C. All observations were
made at 1x binning yielding an image scale of 1.43” per pixel. All
images were un-guided, 45 second exposures. Images were dark
59
and flat field corrected. Images were measured using MPO
Canopus (Bdw Publishing). All observations were made using
unfiltered differential photometry and all data were light-time
corrected. Period analysis was also done with Canopus,
incorporating the Fourier analysis algorithm by Harris (1989).
36 Atalante. Observations were conducted on four consecutive
nights from UT March 10-13. A total of 232 observations were
made. The synodic period was found to be 9.93 ± 0.01 hr, which
agrees well with previous reports, e.g., Harris (1980) and Schober
(1981). The amplitude of the curve was 0.12 ± 0.02 mag.
416 Vaticana. Observations were conducted on 3 consecutive
nights from UT February 15-17. A total of 130 observations were
made. Miles (1990) and Michalowski (2000) both report a period
of 5.372 hr, consistent with the 5.38 ± 0.01 hr result based on my
analysis. Both Miles and Michalowski reported an amplitude of
about 0.37 mag, which is considerably larger than the 0.06 ± 0.01
mag. value seen at this, perhaps more pole-on aspect, apparition.
References
Harris, A.W., and Young, J.W. (1980). Icarus 43, 20-32.
H., and Zeigler, K.W. (1989). “Photoelectric Observations of
Michalowski, T., Pych, W., Berthier, J., Kryszczynska, A.,
Kwiatkowski, T., Boussuge, J., Fauvaud, S., Denchev, P., and
Baranowski, R. (2000). Astron. Astrophys. Suppl. Ser. 146, 471479.
Miles, R. (1990). Minor Planet Bul. 17, 25-29.
Schober, H.J., Schroll, A. (1982). Astron. Astrophys. 1 0 7, 402405.
ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY
OBSERVATORY – NOVEMBER 2006
Richard Ditteon, Scot Hawkins
Rose-Hulman Institute of Technology CM 171
5500 Wabash Avenue
Terre Haute, IN 47803
[email protected]
(Received: 14 Feb
Revised: 4 April)
Lightcurves for 23 asteroids were obtained at the Oakley
Observatory over six nights in November of 2006: 24
Themis, 26 Proserpina, 57 Mnemosyne, 66 Maja, 67
Asia, 89 Julia, 143 Adria, 159 Aemilia, 179
Klytaemnestra, 227 Philosophia, 242 Kriemhild, 298
Baptistina, 340 Eduarda, 381 Myrrha, 536 Merapi, 563
Suleika, 665 Sabine, 799 Gudula, 1046 Edwin, 1087
Arabis, 1321 Majuba, 1621 Druzhba, 2152 Hannibal,
and 5142 Okutama.
on the campus of Rose-Hulman Institute of Technology in Terre
Haute, Indiana. The data gave us useful lightcurves and rotational
periods for 23 asteroids. Of these 23 periods, 14 agreed reasonably
well with previously published periods, 5 periods disagreed or
removed ambiguity from previously published periods, and 4 were
completely new results.
Three telescopes were used on all but one night. Each telescope is
a 14-inch Celestron optical tube assembly mounted on a
Paramount ME. One camera was an Apogee AP-8p which
operated unfiltered at a pixel scale of 2.00 arcseconds per pixel.
The other two cameras were SBIG STL-1001E which used a V
filter at a pixel scale of 1.75 arcseconds per pixel. Two minute
exposures were used for all data frames. Images were calibrated
with master twilight flats and master darks. About half of the
images were calibrated using MaxImDL and half using CCDSoft.
All images were then measured with MPO Canopus.
Asteroids were selected based on their position in the sky one hour
after sunset. Priority was given to asteroids without previously
published lightcurves, but asteroids with well known periods were
also targeted with the hope that the new data would help with
shape modeling and determination of the pole orientation. After
the first two nights, it was realized that there was considerable
We were able to collect data on a total of 32 main belt asteroids
over six nights in November of 2006 from the Oakley Observatory
60
24
Themis
8.376
0.001
0.14
Amplitude
Error
(mag)
0.03
26
Proserpina
9, 10
110
13.06
0.03
0.21
0.01
57
Mnemosyne
21 – 24
62
12.66
0.03
0.14
0.01
66
Maja
21 – 24
114
9.736
0.009
0.30
0.04
67
Asia
21, 22, 23
55
15.90
0.02
0.26
0.04
89
Julia
21 – 24
164
11.38
0.01
0.20
0.02
21, 22, 23
60
Not found
>0.08
0.01
9, 10
110
11.0
0.1
0.07
0.04
Number
Name
Dates of
Observation
Nov 2006
21 – 24
Number
of Data
Points
206
Period (h)
Period
Error (h)
Amplitude
(mag)
124
Alkeste
143
Adria
159
Aemilia
21 – 24
199
16.37
0.02
0.24
0.04
179
Klytaemnestra
21 – 24
63
11.13
0.02
0.55
0.02
227
Philosophia
9, 10
112
Not found
0.35
0.05
242
Kriemhild
21 – 24
51
4.558
0.15
0.02
276
Adelheid
21, 22, 23
127
Not found
>0.08
0.02
298
Baptistina
9, 10
107
9.301
0.001
0.10
0.07
340
Eduarda
9, 10
103
8.04
0.02
0.25
0.03
381
Myrrha
21 – 24
180
6.572
0.002
0.34
0.05
529
Preziosa
21 – 24
185
Not found
0.20
0.08
536
Merapi
21 – 24
122
8.809
0.23
0.05
538
Friederike
21 – 24
190
Not found
0.10
0.05
563
Suleika
21 – 24
123
5.628
0.002
0.28
0.01
665
Sabine
21 – 24
124
4.294
0.001
0.50
0.04
799
Gudula
9, 10, 21 – 23
182
14.814
0.003
0.30
0.03
904
Rockefellia
21, 22, 23
134
Not found
0.10
0.03
953
Painleva
9, 10
75
Not found
0.10
0.03
1046
Edwin
9, 10
109
5.30
1071
Brita
9, 10
46
Not found
1087
Arabis
21 – 24
239
5.797
1321
Majuba
9, 10
103
5.207
1621
Druzhba
21 – 24
210
2152
Hannibal
21 – 24
4155
Watanabe
5142
Okutama
0.003
0.008
0.3
0.1
0.01
0.03
0.001
0.40
0.02
0.009
0.25
0.05
47.9
0.5
>1.00
0.05
273
5.978
0.001
0.32
0.04
9, 10
110
Not found
9, 10, 21 – 23
189
3.803
time remaining before morning twilight. So on the last four nights
additional asteroids were targeted after the initial asteroids had set.
To our knowledge, this is the first reported observations of the
period for the following asteroids: 799 Gudula, 1621 Druzhba,
2152 Hannibal, and 5142 Okutama. Our measurements confirm
the periods given by Harris and Warner (2006) for the following
asteroids: 24 Themis, 57 Mnemosyne, 66 Maja, 67 Asia, 89 Julia,
143 Adria, 179 Klytaemnestra, 242 Kriemhild, 381 Myrrha, 536
Merapi, 563 Suleika, 665 Sabine, 1046 Edwin, and 1087 Arabis.
On the following 5 asteroids, we report new periods or remove
ambiguities from previously published values: 26 Proserpina, 159
Aemilia, 298 Baptistina, 340 Eduarda, and 1321 Majuba.
0.02
0.001
0.3
0.1
0.27
0.05
and CCDSoft to aim the telescope and operate the camera. It also
automatically takes twilight flats, darks, and bias frames. We
were able to get 23 reasonable lightcurves in six nights of
observing which shows that the experiment was a success.
However, improvements can be made. In particular we learned
that it is important to at least take a quick look at the data while
the observing run is in progress. If we had done this, we could
have increased the exposure times for asteroids that proved to be
fainter than predicted. And perhaps, we could have acquired more
data on asteroids with periods longer than 8 hours.
The results are summarized in the table below with individual
lightcurve plots after the table. The results and lightcurves are
presented without comment except when necessary.
Due to large uncertainties on the individual data points, no
repeatable pattern was found for the following asteroids: 124
Alkeste, 227 Philosophia, 276 Adelheid, 529 Preziosa, 538
Friederike, 904 Rockefellia, 953 Painleva, 1071 Brita, 4155
Watanabe. For these asteroids the amplitude reported in the table
is actually the full range observed.
26 Proserpina. Our results agree fairly well with the period of
13.13 h reported by Scaltriti and Zappalà (1979). Our data clearly
eliminate any ambiguity in the measured period, as it does not
support either the 10.6 h reported by Chang, et al. (1981) or the
6.67 h period reported by Riccioli, et al. (2001).
The observations were made primarily to test a custom program
used to control the telescopes and cameras. The program reads a
text file containing the target names and interfaces with TheSky6
67 Asia. The data from 21 November and 23 November show
minima that match nicely with a period as shown. Clearly more
data are needed.
61
159 Aemilia. According to the list of Harris and Warner (2006)
this asteroid’s period is about 25 h. We had four consecutive
nights of data with more than 7 hours of data each night and got a
good fit to the data with a shorter period.
298 Baptistina. Even though our data are noisy, our observations
do not support the 7 h period found by Wisniewski, et al. (1997).
340 Eduarda. Two nights of data result in a period slightly longer
than the 0.32 d (7.68 h) reported by Lagerkvist (1978). Our data,
with amplitude of 0.20 and points with individual uncertainties of
0.02, are inconsistent with the shorter period.
563 Suleika. Period given in the Harrison and Warner (2006) list
is 5.69 h.
665 Sabine. Data includes simultaneous observations on two
telescopes on three of the four nights.
1321 Majuba. The accepted 6.78 h period of Majuba is based on a
single night’s data collected by Binzel (1987). The paper mentions
that the data are consistent with either 6.78h or 5.4h, although the
former was favored. Our data from two nights confirms that the
latter value was close to correct.
1621 Druzhba. Based on a single night, Wisniewski, et al. (1997)
reported that the period had to be greater than 12 h. We were able
to determine the period based on four consecutive nights of data to
be 47.9 ± 0.5 h. Due to the difficulties with a 48 h period, we were
not able to obtain more than 40% phase coverage. However, this
was clearly enough to determine the period as seen in the raw data
plot shown. This asteroid will need more data to get higher
precision on the period as well as coverage of the full cycle.
References
Binzel, R.P. (1987). “A photoelectric survey of 130 asteroids.”
Icarus 72, 135-208.
Chang, Y.C., Zhou, X.-h., Yang, X.-y., Zhang, Y.-y., Li, X.-q.,
Wu, Z.-x. (1981). “Lightcurves of variable asteroids. IV.” Acta
Astron. Sin. 22, 169-173.
Harris, A.W. and Warner, B.D. (2006).
Lagerkvist, C.-I. (1978). “Photographic photometry of 110 main
belt asteroids.” Astron. Astrophys. Suppl. 31, 361-381.
Riccioli, D., Blanco, C., and Cigna, M. (2001). “Rotational
periods of asteroids II.” Planetary and Space Sci. 49, 657-671.
Scaltriti, F., and Zappala, V. (1979). “Photoelectric photometry
and rotation periods of the asteroids 26 Proserpina, 194 Prokne,
287 Nephthys, and 554 Peraga.” Icarus 39, 124-130.
Wisniewski, W.Z., Michalowski, T.M., Harris, A.W., and
McMillan, R.S. (1997). “Photometric Observations of 125
Asteroids.” Icarus 126, 395-449.
62
63
64
PHOTOMETRY FROM GMARS AND SANTANA
OBSERVATORIES – EARLY 2007
Robert D. Stephens
Goat Mountain Astronomical Research Station (GMARS)
11355 Mount Johnson Court, Rancho Cucamonga, CA 91737
[email protected]
(Received: 1 April)
Lightcurve period and amplitude results from Santana
and GMARS Observatories are reported for 2007
January to March: 386 Siegena (9.760 ± 0.002 hours and
0.11 mag.), 1790 Volkov (10.7419 ± 0.0022 hours and
0.09 mag.), 2086 Newell (78.2 ± 0. 1 hours and 1 mag.)
The author operates telescopes at two observatories. Santana
Observatory (MPC Code 646) is located in Rancho Cucamonga,
California and GMARS (Goat Mountain Astronomical Research
Station, MPC G79) located at the Riverside Astronomical
Society’s observing site. Stephens (2006) gives equipment details.
1790 Volkov and 2086 Newell were selected for lightcurve studies
from a list of targets provided by Pravec (2006) for the
Photometric Survey of Asynchronous Binary Asteroids. 386
Siegena was selected to follow up on the author’s observations
described in Stephens (2005). The author measured the images
using MPO Canopus, which employs differential aperture
photometry to produce the raw data. Period analysis was done
using Canopus, which incorporates the Fourier analysis algorithm
(FALC) developed by Harris (1989).
The results are summarized in the table below. Column 2 gives the
dates over which the observations were made, Column 3 gives the
number of actual runs made during that time span and column 4
gives the number of observations used. Column 5 is the range of
phase angles over the full data range. If there are three values in
the column, this means the phase angle reached a minimum with
the middle valued being the minimum. Columns 6 and 7 give the
range of values for the Phase Angle Bisector (PAB) longitude and
latitude respectively. Column 8 gives the period and column 9
gives the error in hours. Columns 10 and 11 give the amplitude
and error in magnitudes.
386 Siegena. Siegena was originally reported to have a 9.763 hour
period (Zappala 1982). It was observed again in 1979 and 1980
Harris and Young 1983 and 1989). The resulting period was
inconclusive but consistent with the Zappala period. The
amplitude in 1979 was about 0.1 magnitudes and somewhat higher
in 1980. Observations obtained in 2004 Stephens (2005) suggested
a period of 15.98 hours. Despite the favorable 2004 opposition, the
observations were extremely noisy, perhaps because it was in
dense star fields. 2007 again presented a favorable opposition and
observations were obtained using the 0.30m SCT/RCX operated at
Santana Observatory.
65
Asteroid
Dates
Sess
Phase
7
Data
Points
1,502
386 Siegena
2007 02/24 – 03/11
1790 Volkov
2086 Newell
2007 01/13 – 21
2007 01/13 – 02/17
LPAB
BPAB
4
10
643
1,454
6.3, 10.8
141.5, 141.4
13.4, 9.3
9.3, 0.4, 9.6
133.6, 134.3
129.3, 130.3
It was difficult to differentiate between a typical bimodal
lightcurve with a period of 19.51 hr and a monomodal lightcurve
with a period of 9.760 hr. The shorter solution was selected
because the Zappala lightcurve observed at (PAB) longitude 333.6
presents a bimodal shape using the reported 9.763 hr period. Also,
an unusual dip in the 2007 lightcurve following the extrema
repeats itself in the bimodal lightcurve.
1790 Volkov. Observations were obtained on January 13 with the
GMARS 0.35m SCT/RCX using a SBIG ST9e CCD camera. All
subsequent observations obtained with the GMARS 0.35m SCT
using a SBIG ST1001e CCD Camera.
2086 Newell. Observations were obtained on January 13 with the
GMARS 0.35m SCT using a SBIG ST1001e CCD camera. All
subsequent observations obtained with the Santana 0.30m
SCT/RCX using a SBIG ST1001e CCD Camera.
Acknowledgements
Thanks are given to Dr. Alan Harris of the Space Science Institute,
Boulder, CO, and Dr. Petr Pravec of the Astronomical Institute,
Czech Republic, for their ongoing support of all amateur asteroid
work. Also, thanks to Brian Warner for his continuing work and
enhancements to the software program “Canopus” which makes it
possible for amateur astronomers to analyze and collaborate on
asteroid rotational period projects and for maintaining the CALL
Web site which helps coordinate collaborative projects between
amateur astronomers.
References
Harris, A.W. and Young, J. (1989). “Asteroid lightcurve
observations from 1979-1981.” Icarus 81, p. 314-364.
Pravec, P. (2006). Photometric Survey of Asynchronous Binary
Asteroids. http://www.asu.cas.cz/~asteroid/binastphotsurvey.htm.
Stephens, R.D. (2005). “Rotational Periods of 96 Aegle, 386
Siegena, 390 Alma, 544 Jetta, 2771 Polzunov, and (5917) 1991
HG.” Minor Planet Bulletin 32 1-2
Stephens, R.D. (2006). “Asteroid Lightcurve Photometry From
Santana and GMARS Observatories – September to December
2006.” Minor Planet Bulletin 34, 31-32.
Zappala, V., Scaltriti, F., Lagervist, C., Rickman, H., and Harris,
A.W. (1982). “Photometric photometry of asteroids 33
Polyhymnia nad 386 Siegena.” Icarus 52, 196-201.
-10.0, -8.7
Per
(h)
9.760
5.9, 5.8
-1.6, 0.0
10.7419
78.2
PE
Amp
AE
0.002
0.11
0.02
0.0022
0.1
0.09
1
0.03
0.2
66
ASTEROID LIGHTCURVE ANALYSIS FROM
VOLUNTEER OBSERVATORY DECEMBER 2006 TO
APRIL 2007
least 0.4 mag and, assuming a bi-modal lightcurve, the acquired
data indicates the period could be in the range of 45+ hrs.
1602 Indiana. 45 sec exposures were used with a clear filter. The
derived period after one night of observations in March 2007 is
2.610 ± 0.001 hr and amplitude 0.175 ± 0.047 mag.
Michael L. Fleenor
10305 Mantooth Lane
Knoxville, TN 37932 USA
[email protected]
3497 Innanen. Clear filter, 45 sec exposures. Derived period from
one night’s observations in April 2007 is 7.310 ± 0.001 hr and
amplitude 0.563 ± 0.043 mag.
Lightcurve period and amplitude results for eight
asteroids observed at Volunteer Observatory during
December 2006 to April 2007 are reported: 78 Diana,
623 Chimaera, 888 Parysatis, 1502 Arenda, 1602
Indiana, 3497 Innanen, 4374 Tadamori, and (34777)
2001RH.
The author operates Volunteer Observatory at Knoxville,
Tennessee at an elevation of 330 meters. Instrumentation utilized
for asteroid photometry includes a 0.35m Meade SCT mounted on
an Astrophysics 1200 GTO mounting and an SBIG ST10XME
CCD camera. The image scale for all observations was
approximately 1.21 arc-seconds per pixel with 2x2 binning and
data were acquired with either an R band photometric filter or
custom blue blocking clear filter. The CCD operating temperature
was maintained between -10ºC and -30ºC depending on ambient
conditions. Image acquisition and observatory automation is
accomplished with Maxim DL and Astronomer’s Control Panel
software. Additional details of the equipment used are located at
the author’s personal website: http://www.mikefleenor.com.
All images were measured using MPO Canopus which employs
differential aperture photometry to determine the values used for
analysis. The period determination was accomplished with
Canopus incorporating the Fourier analysis algorithm developed
by Harris (1989). Amplitude determination was accomplished
using photometry data generated by Canopus and the author’s
custom MS Excel spreadsheets.
4374 Tadamori. Observed with clear filter during two nights in
March 2007 using 45 sec exposures. Derived period is 4.503 ±
0.001 hr and amplitude 0.827 ± 0.046 mag.
(34777) 2001 RH. R band, 90 sec exposures. Observations during
four nights in January 2007 revealed a period of 7.495 ± 0.001 hrs.
with an amplitude of 0.400 ± 0.018mag. These findings are
consistent with those of Stephens and Warner (2007). Their
reported period was 7.4947 ± 0.0004 hr. and amplitude 0.40 mag.
Acknowledgements
Special thanks are given to Brian Warner for his continuing work
and enhancements to MPO Canopus. The StarBGone! feature
saved many data points that would’ve been utterly lost as several
of the targets were tracked through dense stellar fields.
References
Harris, A.W. and Young, J.W. (1989), Icarus 81, 314-364.
Licchelli, D. (2006), Minor Planet Bul. 33, 11-13.
Stephens, R.D. and Warner, B.D. (2007). Minor Planet Bul. 34,
46.
Warner, B.D. (2003). A Practical Guide to Lightcurve Photometry
and Analysis. Bdw Publishing, Colorado Springs, CO.
Targets were selected from the list of asteroid photometry
opportunities published by Brian Warner and Alan Harris on the
Collaborative Asteroid Lightcurve Link (CALL) website (Harris
2006, 2007). Lightcurve period and amplitude results are
summarized and plots are presented below. Additional comments
are given as warranted.
78 Diana. 30 sec exposures, R band. Period derived after a single
session in January 2007 was 7.346 ± 0.001 hr and amplitude 0.258
± 0.010 mag. The period obtained is similar to the value of 7.225
hrs. reported by Harris & Young (1989) and 7.300 ± 0.001 hr.
reported by Licchelli (2006). During the 2005 apparition the
amplitude reported was 0.15 mag.
623 Chimaera. 90 sec exposures, R band. Period derived after
three nights of observations in December 2006 was 14.635 ±
0.001 hr. and amplitude 0.180 ± 0.013 mag.
888 Parysatis. 30 sec exposures were used with an R band filter
for four nights in December 2006 to derive a period of 5.933 ±
0.001 hr and amplitude 0.242 ± 0.010 mag.
1502 Arenda. R band, 90 sec exposures. Three nights in January
2007 revealed this object to be a very slow rotator. Amplitude is at
67
THE ROTATION PERIODS OF
242 KRIEMHILD AND 1094 SIBERIA
Colin Bembrick
PO Box 1537, Bathurst, NSW 2795, AUSTRALIA
[email protected]
Greg Crawford
Bagnall Beach Observatory
Salamander Bay, NSW, AUSTRALIA
Julian Oey
Leura Observatory
Leura, NSW, AUSTRALIA
Bill Allen
Vintage Lane Observatory
Blenheim, NEW ZEALAND
(Received: 1 April Accepted: 31 March)
Minor planet 242 Kriemhild was observed over nine
nights in Jan and Feb 2007 and 1094 Siberia over eight
nights in Dec 2006 and Jan 2007. The synodic period
derived for the former was 4.5478 ± 0.0014 hr. The
values for the latter were 21.15 ± 0.01 hr. The peak-topeak amplitude of Kriemhild was 0.13 magnitudes,
implying an axial ratio (a/b) of 1.13. For Siberia the
magnitude variation was at least 0.45 implying a ratio
(a/b) > 1.51.
Minor planet 242 Kriemhild was discovered by J.Palisa at Vienna
in 1884. This main-belt asteroid has a quoted diameter of 41.5 km
and an albedo of 0.14 (Guide, 2002). Observations by Warner in
2004 yielded a rotation period of 4.543 ± 0.005 hr. (Warner,
2005). That lightcurve was somewhat noisy and in the latest
rotational parameter list (Harris and Warner, 2006) it is assigned a
quality value of only 2. Hence it was recently re-listed for
observation (Warner et al, 2007).
Minor planet 1094 Siberia (1926 CB) was discovered in 1926 by
S. Beljavskij. This inner main belt asteroid has a quoted diameter
of 18.1 km and an albedo of 0.083 (Guide, 2002). The latest list of
parameters (Harris & Warner, 2006) has no data for this asteroid.
Observations were conducted from four sites – three in Australia
and one in New Zealand. All observations utilised unfiltered
differential photometry and were light-time corrected. The aspect
data (Tables I & 2) also shows the percentage of the lightcurves
observed each night. Analysis was carried out using the “Peranso”
software (Vanmunster, 2006), using various routines available
including the “FALC” routine (based on Harris, et al, 1989).
242 Kriemhild: The final analysis determined a synodic period of
4.5478 ± 0.0014 hr, which was used to compile the composite
lightcurve, with the arbitrary epoch of minimum at JD
2454120.078. The peak-to-peak variation in the lightcurve implies
an axial ratio (a/b) of 1.13 if viewed at an equatorial aspect. Full
phase coverage was achieved and this is considered a secure
result. It confirms the result of Warner (2005). Kriemhild is thus a
“fast rotator” for asteroids of this size (see Pravec et al, 2002).
68
1094 Siberia: Full phase coverage for this asteroid was not
achieved and a period of 21.15 ± 0.01 hr was adopted as best
fitting the available data. Other periods, including one close to 19
hr, cannot be entirely ruled out. The composite lightcurve has been
compiled with an arbitrary epoch of maximum at JD 2454079.295.
It appears that Siberia is a “slow rotator” for asteroids of this size
(Pravec et al, 2002).
References
GUIDE version 8 (2002). http://www.projectpluto.com
Harris, A.W. and Warner, B.D. (2006). “Minor Planet Lightcurve
Parameters”. Last Updated March 2006.
Asteroids 3, 24, 60, 261, and 863”. Icarus 77, 171-186.
Pravec, P., Harris, A.W., and Michalowski, T. (2002). “Asteroid
Rotations” in Asteroids III (W.F. Bottke, A. Cellino, P. Paolicchi,
R.P. Binzel, eds.), 113-122. Univ. Arizona Press, Tucson.
Vanmunster, T. (2006). Peranso ver 2.0. http://www.peranso.com
Warner, B.D. (2005). “Lightcurve Analysis for Asteroids 242,
893, 921, 1373, 1853, 2120, 2448, 3022, 6490, 6517, 7187, 7757,
and 18108”. Minor Planet Bulletin 32, 4-7.
Warner, B.D., Harris, A.W., Pravec, P., Kaasalainen, M. and
Benner, L.A.M. (2007). “Lightcurve Photometry Opportunities
January – March 2007”. Minor Planet Bulletin 34, 24-25.
Table I. Aspect data for Kriemhild in 2007.
UT Date
2007
2007
2007
2007
2007
2007
2007
2007
2007
Jan
Jan
Jan
Jan
Jan
Jan
Jan
Feb
Feb
19
20
25
26
27
28
30
01
14
LPAB
BPAB
136.2
136.3
136.4
136.4
136.5
136.5
136.5
136.6
136.8
-14.2
-14.2
-14.2
-14.2
-14.2
-14.2
-14.1
-14.1
-13.8
Phase
Angle
10.3
10.0
8.5
8.3
8.0
7.8
7.4
7.1
7.7
%Phase
Coverage
111
121
100
164
148
164
132
125
127
Table 2. Aspect data for Siberia in 2006/2007.
UT Date
2006
2006
2006
2006
2006
2007
2007
2007
Dec
Dec
Dec
Dec
Dec
Jan
Jan
Jan
10
18
25
26
28
04
05
19
LPAB
BPAB
90.2
90.6
90.8
90.9
90.9
91.2
91.3
92.3
-17.2
-16.9
-16.5
-16.5
-16.3
-15.8
-15.7
-14.3
Phase
Angle
11.5
9.7
9.4
9.4
9.7
11.1
11.4
15.9
%Phase
Coverage
22
27
29
29
10
28
25
16
LIGHTCURVES OF 25 PHOCEAE, 468 LINA,
482 PETRINA, 551 ORTRUD, 741 BOTOLPHIA,
834 BURNHAMIA, 2839 ANNETTE,
AND 3411 DEBETENCOURT
Robert K. Buchheim
Altimira Observatory
18 Altimira, Coto de Caza, CA 92679 USA
[email protected]
(Received: 7 April
Revised: 25 April)
Lightcurves and synodic rotation period results for the
following asteroids are presented: 25 Phoceae P = 9.945
±0.002 hrs, ∆m ≈ 0.03 mag.; 468 Lina 16.33 ± 0.02 hrs,
0.15 mag; 482 Petrina 15.73 ± 0.02 hrs, 0.5 mag; 551
Ortrud 17.416 ± 0.002 hrs, 0.15 mag; 741 Botolphia
23.93 ± 0.02 hrs, ∆m≈ 0.15 mag; 834 Burnhamia 13.875
± 0.001 hrs, 0.2 mag; for 2839 Annette 10.4595 ±
0.0001 hrs, 0.65 mag; 3411 Debetencourt 9.93 ± 0.01
hrs, 0.35 mag. Slope parameters are also suggested for
three of these asteroids.
Altimira Observatory is located in southern California, and is
equipped with a 0.28-m Schmidt-Cassegrain telescope (Celestron
NexStar-11 operating at F/6.3), and CCD imager (ST-8XE
NABG, with Johnson-Cousins filters). Details of the equipment
and instrument characterization are available at the author’s
website (http://www.geocities.com/oca_bob).
Asteroid lightcurves were determined by differential photometry,
generally using a two-color imaging sequence (e.g. VV-RR-etc.)
throughout each night, although for the lightcurves in this paper,
69
only the R-band data is reported. None of these asteroids showed
any color variation as they rotated.
25 Phoceae. The lightcurve of this asteroid has been previously
well-established at P = 9.945 hr, with amplitude of at least _m ≈
0.18 mag (peak-to-peak) by Groeneveld and Kuiper (1954). A
lightcurve for the October, 2006 apparition was collected to
support the evaluation of successful IOTA observations of the
October 3, 2006 occultation of HIP 115725 by this asteroid. The
very small amplitude (∆m = 0.03 mag peak-to-peak) suggests that
the asteroid was at a nearly “pole on” orientation. Dr. Behrend’s
website has a partial lightcurve from other observers that is
consistent with this result.
468 Lina. Tedesco (1979) provided a partial lightcurve for this
object and suggested a period of either 8.3 or 16.6 hrs. Antonini
and Behrend (2006) report a lightcurve with an apparent period of
20.92 hrs and a very complex “multi-peak” shape. My lightcurve
is based on five nights in December, 2005 (i.e. the same apparition
as that of Antonini and Behrend). It is best fit by a period of 16.33
± 0.02 hrs, amplitude of ∆m = 015 mag (peak-to-peak) and an
unusual “three peak” shape. This is consistent with Tedesco’s
result. I tried to match my data to other periods in the range 16 to
24 hours, but there was no acceptable fit; hence, the discrepancy
with the conclusion of Antonini and Behrend is unresolved.
my equipment, and provided typical SNR ≈ 20 in the R-band CCD
images. Its lightcurve has a best-fit period of P = 9.93
± 0.001 hr. The amplitude of its brightness variation is ∆m ≈ 0.35
mag. This is apparently the first reported lightcurve for this object.
Phase Curves
I attempted to determine phase curves for three of these asteroids.
Since many “lightcurve” nights were contaminated by haze or
unstable atmospheric conditions, I devoted separate clear and
stable nights to calibrating the color indices and V-mag brightness
of all of the comparison stars used on all lightcurve runs. Landolt
standard stars were used to confirm the system transforms, and to
determine the extinction and zero-points in V- and R-bands on
these “calibration” nights. The calibrated comp stars were then
used as secondary standards to determine the asteroids’ magnitude
and color index. All of these calculations were accomplished using
Brian Warner’s MPO Canopus/Photored program.
The “reduced magnitude” of an asteroid is the brightness that it
would have if it were at a solar distance of R = 1AU and an Earth
distance of D = 1AU. Measured V-mag brightness of the midpoint
of the lightcurve was translated into reduced magnitude by
VR = V – 5 log RD
482 Petrina. Charbonnel (2002) reports a provisional lightcurve
period of 18 hrs, based on a partial lightcurve gathered on a single
night in 2002. The best fit period is P = 15.73 ±0.02 hrs, and the
amplitude of brightness variation is ∆m ≈ 0.5 mag. Considering
the deep, sharp minimum that was caught on both nights, the
period seems fairly secure, and should be interpreted as a
refinement of Charbonnel’s result.
for each night of observation. The phase curve is the plot of V R vs.
solar phase angle.
551 Ortrud. Robinson (2002) has reported a period of 13.05 hrs
for this asteroid, based on four long nights of photometry. His
result gives an apparently reasonable lightcurve with complex
shape highlighted by one very “sharp” peak and one “long
plateau” peak. Barbotin and Charbonnel (2003) report a lightcurve
with a provisional period of 17.59 hrs. Poncy (2006) reports a
complete lightcurve based on four nights of observation, with a
period of 17.4 hrs. My lightcurve is a good match to that of
Poncy, with best-fit period P = 17.416 ± 0.002 hrs, amplitude of
∆m≈ 0.15 mag, and a shape that is virtually identical to Poncy’s.
834 Burnhamia. The phase curve for 834 Burnhamia is shown
with the best fit to the data having an absolute magnitude of H =
9.55, and slope parameter of G = 0.25. The relatively large slope
parameter represents an object that displays only a very modest
“opposition surge” in brightness at small phase angles.
741 Botolphia. Roy and Martinez (2002), and Bernasconi (2005)
have reported a period of 23.93 hrs. My lightcurve matches their
results, with a best-fit period of P = 23.93 ± 0.02 hrs and ∆m ≈
0.15 mag.
834 Burnhamia. Lightcurves for this object have been reported by
Bernasconi (2006), whose data shows P = 13.898 ± 0.03 hrs (for
the 2005 apparition), and P = 13.85 ± 0.03 hrs (for the 2006
apparition). My data are consistent with his, showing a best-fit
period of P = 13.875 ± 0.001 hrs, and amplitude of ∆m ≈ 0.2 mag.
2839 Annette. Warner (2006) reported a lightcurve period of
10.457 hrs, using two nights in late 2005. I devoted seven nights
during the same apparition (October and November 2005) to this
object. My lightcurve indicates a period P = 10.4595 ± 0.0001 hr
with amplitude ∆m = 0.65 mag (peak-to-peak). These lightcurve
parameters are in good agreement with Warner’s.
3411 Debetencourt. This asteroid happened to be in the same field
as 468 Lina for four nights. It was faint, near the practical limit of
551 Ortrud. The phase curve of 551 Ortrud is shown with the bestfit curve using the equations of Bowell, et al (1989). The best-fit
parameters are H = 9.72 and G = 0.28. The slope parameter
appears to be definitely larger than the “default” value of 0.15.
2839 Annette. The phase curve for this asteroid indicates an
absolute magnitude of H = 14.35 and slope parameter not
noticeably different from the “default” G = 0.15. This absolute
magnitude is significantly fainter than the H = 12.3 that is reported
at the Small Bodies Node.
References:
Antonini, P., and Behrend, R. (2006). “Courbes de rotation
d'astéroïdes et de comètes, CdR.” http://obswww.unige.ch/
~behrend/page3cou.html
Barbotin, E., and Charbonnel, S. (2003). http://obswww.unige.ch/
Bernasconi, L. (2005). http://obswww.unige.ch/~behrend/
page2cou.html
Bernasconi, L., (2006). http://obswww.unige.ch/~behrend/
page3cou.html
Bowell, E. et al. “Application of Photometric Models to
Asteroids” in Binzel, R. P., et al (ed) Asteroids II, Univ. of
Arizona Press.
70
Charbonnel, S. (2002). http://obswww.unige.ch/~behrend/
page2cou.html
Groeneveld, I. and Kuiper, G.P. (1954), “Photometric Studies of
Asteroids. I”. Astrophysical Journal 120, 200-220.
Poncy, R., (2006).
page2cou.html
http://obswww.unige.ch/~behrend/
Robinson. L.E. (2002). “Lightcurve photometry of 551 Ortrud,
1118 Hanskya, and 1916 Boreas from Sunflower Observatory”.
Minor Planet Bulletin 33, 37-38.
Roy, R., and Martinez, P. (2002). http://obswww.unige.ch/
Tedesco, E. F. (1979). PhD Dissertation, New Mexico State
University.
Warner, B. D. (2006). “Asteroid Lightcurve Analysis at the
Palmer Divide Observatory – Late 2005 and Early 2006,” Minor
Planet Bulletin 33, 59-62.
NASA Small Bodies Node (2007). http://pdssbn.astro.umd.edu/
SBNcgi/sbdbatt
71
72
ASTEROID LIGHTCURVE ANALYSIS AT
THE PALMER DIVIDE OBSERVATORY –
DECEMBER 2006 – MARCH 2007
Brian D. Warner
Palmer Divide Observatory/Space Science Institute
17995 Bakers Farm Rd., Colorado Springs, CO 80908
[email protected]
Lightcurves for 32 asteroids were obtained at the Palmer
Divide Observatory from late December 2006 through
March 2007: 22
Kalliope, 36 Atalante, 92
Undina, 108 Hecuba, 154 Bertha, 170 Maria, 275
Sapientia, 572 Rebekka, 708 Raphaela, 947 Monterosa,
1072 Malva, 1323 Tugela, 1348 Michel, 2449 Kenos,
3225 Hoag, 3410 Vereshchagin, 4764 Joneberhart, 4765
Wasserburg, 4898 Nishiizumi, 6646 Churanta, 6870
Pauldavies, (7783) 1994 JD, 9554 Dumont, (9873) 1992
GH , (16585) 1992 QR, (16681) 1994 EV7, (30856)
1991 XE, (40250) 1998 XG16, (69350) 1993 YP,
(101549) 1998 YY29, (138666) 2000 RX96, and 2001
BE10.
Observations of 32 asteroids were made at the Palmer Divide
Observatory from December 2006 through March 2007. One of
four telescopes/camera combinations was used: 0.5m RitcheyChretien/FLI IMG-1001E, 0.35m SCT/FLI IMG-1001E, 0.35m
SCT/ST-9E, or 0.35m SCT/STL-1001E. The scale for each was
about 2.5 arcseconds/pixel. Exposure times were 20–300s.
Observations were made with a Clear filter, except those for 22
Kalliope, where a V filter was used. Guiding was used when
exposures exceeded 60 seconds. All images were measured using
MPO Canopus, which employs differential aperture photometry to
determine the values used for analysis. Period analysis was also
done using Canopus, which incorporates the Fourier analysis
algorithm developed by Harris (1989).
The results are summarized in the table below, as are individual
plots. The data and curves are presented without comment except
when warranted. Column 3 gives the full range of dates of
observations; column 4 gives the number of data points used in the
analysis. Column 5 gives the range of phase angles. If there are
three values in the column, the phase angle reached a minimum
with the middle value being the minimum. Columns 6 and 7 give
the range of values, or average if the range was relatively small,
for the Phase Angle Bisector (PAB) longitude and latitude
respectively. Columns 8 and 10 give the period and amplitude of
the curve while columns 9 and 11 give the respective errors in
hour and magnitudes. An "(H)" follows the name of an asteroid in
the table if it is a member of the Hungaria group or family.
22 Kalliope. Observations were made in support of a program
under Jean-Luc Margot (Cornell University) during a season of
mutual eclipse and occultation events involving the asteroid's
satellite, Linus. A weak event was apparently captured on
February 27 (Warner 2007). Two others may have been observed
on March 8 and 13. The period of 4.14828 hr for the primary
rotation agrees well with numerous previous determinations
(Harris 2007).
36 Atalante. The period of 9.9280 agrees with the 9.93 hr period
reported by Harris (1980) and Schober (1982).
92 Undina. The period of 15.941 hr agrees with the 15.94 hr
period of Schober et al (1979).
108 Hecuba. The only previously reported period was that of
14.46 hr by Blanco et al (1994), which the data obtained at PDO
could not be made to fit. Instead, a period of 17.859 hr was
adopted.
154 Bertha. This asteroid was worked in hopes of determining
which, if any, of previously reported periods was correct. Harris
(1989a) >12 hr; Kamel (1998) 27.6 hr. A period of 22.30 ± 0.03 hr
provided the best fit of the PDO data.
170 Maria. Previously reported periods were 13.14 hr (Denchev,
2000) and 5.510 hr (Blanco, 2000). The PDO period of 13.120 hr
agrees with the former and could not be fit to the latter.
275 Sapientia. The only previously reported period was that of
>20 hr by Denchev (2000). PDO data indicates a period of 14.766
± 0.006 hr and a slightly unusual curve with only a single obvious
maximum. With a low amplitude, there is a possibility that the
viewing aspect was pole-on and that the true period might be
approximately double the stated period. A possible solution was
found at 29.53 ± 0.03 hr, however the fit of some of the data was
not as good and so the shorter period was adopted.
572 Rebekka. The period of 5.656 hr agrees with that of 5.65
reported by Lagerkvist et al (1998).
947 Monterosa. The PDO data do not support the previously
reported period of 2.376 hr by Behrend (2007).
2449 Kenos. Wisniewski et al (1997) reported a period of 4.118 hr
but also gave one of 3.86 hr as a possibility. Coverage of more
than one cycle on each of two consecutive nights at PDO resolved
the ambiguity, with a period of 3.8492 ± 0.0008 hr being adopted.
4765 Wasserburg. The adopted period is 3.67 ± 0.02 hr and is the
one used for the lightcurve plot. However, an alternate solution,
with a weak bimodal shape, is seen at 6.07 hr. Given the low
amplitude, it cannot be certain if the aspect was pole-on, which
would often present a monomodal curve and so might lead to
finding one-half the true period. Additional follow-up will be
required to resolve the ambiguity.
(69350) 1993 YP. The period of 31.79 hr is the best fit to an
assumed bimodal curve.
Acknowledgements
Funding for observations at the Palmer Divide Observatory is
provided by NASA grant NNG06GI32G, by National Science
Foundation grant AST-0607505, and by a Gene Shoemaker NEO
Grant from the Planetary Society.
References
Behrend, R. (2007). Observatoire de Geneve web site,
http://obswww.unige.ch/~behrend/page_cou.html
Blanco, C., Di Martino, M., Lazzarin, M., Cellino, A., Riccioli, D.
(1994). “Seventy-Five Years of Hirayama Asteroid Families”,
ASP Conf. Ser. 63, 280-285.
73
Blanco, C., Di Martino, M., and Riccioli, D. (2000). Planet. Space
Sci. 48, 271-284.
Schober, H.J., Scaltriti, F., and Zappala, V. (1979) Astron.
Astrophys. Suppl. Ser. 36, 1-8.
Denchev, P. (2000). Planet. Space Sci. 48, 987-992.
Schober, H.J. and Schroll, A. (1982) Astron. Astrophys. 107, 402405.
Warner B. and Margot, J.L. (2007). CBET 861.
H., and Zeigler, K.W. (1989b). “Photoelectric Observations of
Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186
Wisniewski, W.Z., Michalowski, T.M., Harris, A.W. and
McMillan, R.S. (1997) Icarus 126, 395-449.
Harris, A.W., Warner, B.D., and Pravec, P. (2007) Asteroid
Lightcurve Parameters
http://www.MinorPlanetObserver.com/astlc/default.htm.
Kamel, L. (1998) Minor Planet Bul. 25, 1-2.
Lagerkvist, C.-I., Belskaya, I., Erikson, A., Schevchenko, V.,
Mottola, S., Chiorny, V., Magnusson, P., Nathues, A., and
Piironen, J. (1998) Astron. Astrophys. Suppl. Ser. 131, 55-62.
#
22
36
92
108
154
170
275
572
708
947
1072
1323
1348
2449
3225
3410
4764
4765
4898
6646
6870
7783
9554
9873
16585
16681
30856
40250
69350
101549
138666
Name
Kalliope
Atalante
Undina
Hecuba
Bertha
Maria
Sapientia
Rebekka
Raphaela
Monterosa
Malva
Tugela
Michel
Kenos (H)
Hoag (H)
Vereshchagin
Joneberhart (H)
Wasserburg (H)
Nishiizumi (H)
Churanta (H)
Pauldavies (H)
1994 JD (H)
Dumont (H)
1992 GH (H)
1992 QR (H)
1994 EV7 (H)
1991 XE (H)
1998 XG16 (H)
1993 YP (H)
1998 YY29 (H)
2000 RX96 (H)
2001 BE10
Date Range
(mm/dd)
2006-2007
Data
Pts
Phase
02/25-03/14
02/27-03/02
03/02-09
03/04-09
01/01-16
01/01-17
01/01-10
02/04-05
02/11-22
01/01-07
02/04-06
01/16-19
01/23-25
03/09-14
03/13-21
03/18-21
01/17-19
12/26-27
01/23-24
01/10-02/06
02/23-25
01/16-19
12/26-01/10
02/18-22
02/21-23
02/06-21
01/23-24
12/22-01/09
02/18-25
01/23-02/16
01/24-02/21
01/17-19
1438
773
1280
868
786
740
594
184
560
247
326
508
219
125
180
86
199
90
129
138
142
533
164
155
136
294
201
181
223
335
299
132
20.8-21.7
11.7-12.6
13.7-14.8
11.0-12.4
12.4-15.2
21.2-23.3
14.2-16.6
12.1-12.5
5.9-10.7
21.0-22.4
8.4-9.1
9.7-10.5
16.5-17.2
5.0-3.5
12.9-15.4
8.7-10.4
8.6-8.8
15.2-15.8
18.9-18.6
20.6-9.1
8.2-7.5
9.5-10.3
17.4-24.7
9.7-7.4
7.8-6.8
10.5,8.1,8.9
17.1-17.2
15.0-18.4
3.0,1.6,2.8
11.4-17.6
11.5,10.9,18.1
44.6-39.0
LPAB
94.0
136.2
113.4
131.7
62.3
50.7
63.4
114.4
129.6
58.7
118.6
95.8
86.6
172.2
160.2
162.9
113.0
69.6
137.6
134.5
163.2
114.7
69.6
162.2
162.9
143.8
121.4
234.5
153.0
128.2
132.1
141.5
BPAB
Per
(h)
PE
9.4 4.14828 0.00003
14.3
9.9280 0.0001
3.6
15.941
0.002
2.7
17.859
0.005
12.9
22.30
0.03
14.5
13.120
0.002
-5.0
14.766
0.006
-13.4
5.656
0.002
2.9
20.918
0.005
3.1
5.164
0.001
10.2
10.080
0.005
18.5
19.50
0.02
1.0
8.095
0.004
-5.7
3.8492 0.0008
-15.4
2.3717 0.0002
-0.8
2.5780 0.0006
-13.0
5.483
0.002
0.5
3.67
0.02
22.6
3.289
0.002
14.1
5.8711 0.0002
9.1
4.487
0.001
13.0
31.83
0.03
-0.5
28.7
0.1
6.8
2.9257 0.0003
5.7
5.273
0.005
11.9
5.3148 0.0002
27.4
5.353
0.003
7.9
20.90
0.01
2.3
31.79
0.04
17.9
56.50
0.25
-15.6
8.6827 0.0004
-6.4
4.196
0.002
Amp
(m)
AE
0.48
0.13
0.20
0.11
0.10
0.21
0.06
0.40
0.45
0.23
0.17
0.25
0.47
0.20
0.13
0.10
0.97
0.04
0.23
0.73
0.50
0.85
0.40
0.27
0.23
0.92
0.70
0.32
0.45
0.70
0.80
0.32
0.02
0.02
0.02
0.02
0.02
0.02
0.01
0.02
0.02
0.02
0.02
0.02
0.02
0.03
0.02
0.02
0.03
0.01
0.02
0.02
0.02
0.03
0.05
0.02
0.03
0.02
0.02
0.05
0.05
0.05
0.03
0.03
74
75
76
77
78
LIGHTCURVE ANALYSIS OF
1489 ATTILA AND 1696 NURMELA
Robert D. Stephens
11355 Mount Johnson Court, Rancho Cucamonga, CA 91737
[email protected]
Glenn Malcolm
7430 Lippizan Drive, Riverside, CA 92509
(Received: 27 March )
Observations of 1489 Attila and 1696 Nurmela were
made in early 2007 with period and lightcurve amplitude
results of 11.28 ± 0.01 hours, 0.42 mag. and 3.1587 ±
0.0001 hours, 0.33 mag., respectively.
The authors selected the targets from the list of asteroid
photometry opportunities published by Brian Warner and Alan
Harris on the Collaborative Asteroid Lightcurve Link (CALL)
website (Harris 2006). The authors measured the images using
MPO Canopus, which employs differential aperture photometry to
produce the raw data. Period analysis by Stephens was done using
Canopus, which incorporates the Fourier analysis algorithm
(FALC) developed by Harris (1989).
The results are summarized in the table below. Column 2 gives
the dates over which the observations were made, Column 3 gives
the number of actual runs made during that time span and column
4 gives the number of observations used. Column 5 is the range of
phase angles over the full data range. If there are three values in
the column, this means the phase angle reached a minimum with
the middle valued being the minimum. Columns 6 and 7 give the
range of values for the Phase Angle Bisector (PAB) longitude and
latitude respectively. Column 8 gives the period and column 9
gives the error in hours. Columns 10 and 11 give the amplitude
and error in magnitudes.
1489 Attila. Observations were obtained on February 25 and
March 11 with the authors’ 0.35m SCT at GMARS. Additional
observations were obtained on March 13 to 17 with Stephens’
0.30m SCT/RCX operated at Santana Observatory. All
observations were obtained with an SBIG ST1001 CCD camera
with the image scale of approximately 2.2 arcseconds per pixel at
Santana Observatory and 2.4 arcseconds per pixel at GMARS.
1696 Nurmela. All observations were obtained with the authors’
second GMARS telescope, a 0.35m SCT/RCX using a SBIG ST9e
CCD camera with an image scale of approximately 1.9 arcseconds
per pixel.
Asteroid
Dates
Sess
1489 Attila
2007 02/25 – 03/17
1696 Nurmela
2007 03/17 – 25
Acknowledgements
Thanks are given to Brian Warner for his continuing work and
enhancements to the software program “Canopus” which makes it
possible for amateur astronomers to analyze and collaborate on
asteroid rotational period projects and for maintaining the CALL
Web site which helps coordinate collaborative projects between
amateur astronomers.
References
Harris, A.W. and Warner, B.D. (2006). http://www.minorplanet
observer.com/astlc/LC.zip
Phase
LPAB
6
Data
Points
690
0.7, 8.9
154.3, 154.6
3
420
2.8, 6.4
174.1, 174.5
BPAB
PE
0.0, 0.2
Per
(h)
11.28
Amp
AE
3.9, 3.5
3.1587
0.01
0.42
0.04
0.0001
0.33
0.03
79
ASTERIOD LIGHTCURVE ANALYSIS AT HUNTERS HILL
OBSERVATORY AND COLLABORATING STATIONS –
DECEMBER 2006 – APRIL 2007
David Higgins
Hunters Hill Observatory (E14)
7 Mawalan Street
Ngunnawal ACT 2913, Australia
[email protected]
Julian Oey
Leura Observatory (E17)
94 Rawson Pde. Leura Australia
(Received: 9 April)
Lightcurves for the following asteroids were obtained at
Hunters Hill Observatory and collaborating stations and
then analysed to determine the synodic period and
amplitude: 865 Zubaida, 1164 Kobolda, 2328 Robeson,
3851 Alhambra, (6555) 1989 UU1, 13006 Schwaar,
(29337) 1995 AE1.
out other periods.
3851 Alhambra. The data for this target fit a period of around 26
hours but for the last session. No reason can be found for any error
in the last session of data and as a result a fit at double the period
(53 hr) was found. However, there are large gaps in the plot and so
no definitive period can be given at this time. Note that two
additional sessions of data were obtained but they are not shown in
the plot since they are too short to assist in defining the curve's
shape. Since the prime focus at the two observatories is on targets
for the BinAstPhotSurvey, no further observations of this target
are planned.
13006 Schwaar. This was a difficult target and so no clean
lightcurve could be achieved. The strongest fit was found at 6.8
hrs but other periods are not ruled out. The data were sent to Dr.
Petr Pravec for analysis but nothing out of the ordinary was found
and he also indicated that the strongest fit was around 6.8hrs
(Pravec 2007). The plot shown in this paper has been Binned 2
(average 2 data points inside a 10 minute period)
Acknowledgements
Hunters Hill Observatory is equipped as described in Higgins
(2005). All observations reported here were made using a clear
filter with guided exposure times of 240 seconds. MaxIm
DL/CCD, driven by ACP4, was used for telescope and camera
control while calibration and image measurements were
undertaken by MPO Canopus (version 9). Leura Observatory is
equipped as described in Oey 2006.
The SBIG ST-8E used by Hunters Hill was funded by The
Planetary Society under the 2005 Gene Shoemaker NEO Grants
program. Thanks go to Brian D. Warner for his continued
development and support for the data analysis software, MPO
Canopus v 9 and in particular his development of StarBGone
which has enabled me to gather data even in the presence of
interfering background stars.
Targets were chosen either from the CALL list provided by
Warner (2006) or from Binary Asteroid Photometric Survey list
provided by Dr. Petr Pravec (2005). Results are summarised in the
table below with the individual plots presented at the end.
Additional comment, where appropriate, is provided. Binary
candidates and collaborative targets for which Hunters Hill was
not the Principal Observer are not included. Binary candidates will
be reported separately by Pravec. The strategy is to work objects
carefully for potential deviations that would indicate the presence
of a satellite. Considerable effort was made to identify and
eliminate sources of observational errors that might corrupt the
observations and lead to false attenuation events. It was
particularly important to identify and eliminate data points
affected by faint background stars, bad pixels, and cosmic ray hits.
References
2328 Robeson. This asteroid was initially observed by Oey in
December of 2006. However his sessions were too short to
indicate any viable period. Higgins took up the target and was able
to achieve longer observation sessions at the right phase angle to
allow the data to be tied together. The data were sent to Dr. Petr
Pravec for analysis, who concurred with the period. However, due
to the fragmentary and noisy nature of the data, he could not rule
Name
865
1164
2328
3851
5129
6555
13006
29337
Zubaida
Kobolda
Robeson
Alhambra
Groom
1989 UU1
Schwaar
1995 AE1
Date Range
04
28
07
10
28
20
18
10
Jan
Jan
Dec
Mar
Jan
Jan
Dec
Mar
– 11
– 30
06 –
- 08
– 16
– 27
06 –
– 27
Jan 07
Jan 07
11 Jan 07
Apr 07
Feb 07
Mar 07
11 Jan 07
Mar 07
Harris, A.W., Warner B.D. (2006). “Minor Planet Lightcurve
Parameters,” Minor Planet Center website,
http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html.
Higgins, D. (2005). “Asteroid Lightcurve Analysis at Hunters Hill
Observatory and Collaborating Stations - Autumn/Winter 2005,”
Minor Planet Bulletin 33, 8-11.
Oey, J. (2007). “Lightcurve Analysis of 1495 Helsinki,” Minor
Planet Bulletin 34, 2.
Pravec, P. (2005). “Photometric Survey of Asynchronous Binary
Asteroids,” http://www.asu.cas.cz/~asteroid/binastphotsurvey.htm.
Pravec, P, (2007). Private communication.
Warner, B.D. (2006). CALL Website,
http://www.minorplanetobserver.com/astlc/default.htm.
Session
5
3
11
7
5
9
5
3
Period
Hrs
11.363
4.141
18.632
>26
3.6395
12.6778
6.8
4.5066
P.E.
0.004
0.002
0.004
0.0003
0.0003
0.0
0.0002
Amp
Mag
0.38
0.30
0.2
>0.2
0.18
0.27
0.17
0.38
Amp
Error
0.03
0.01
0.04
0.03
0.02
0.02
0.03
0.01
80
81
Bisque.
LIGHT CURVE ANALYSIS OF 8 ASTEROIDS FROM
LEURA AND OTHER COLLABORATING
OBSERVATORIES
1301 Yvonne. This target was selected as a test subject for the new
setup for Kingsgrove Observatory. The derived period of 7.3200 ±
0.0001 h is in agreement with previous work by Pray (2004) with
the exception that the amplitude was 0.60 ± 0.03 mag compared
with that obtained in this current apparition of 0.90 ± 0.03 mag.
This can be explained by the phase angle difference of around 7°
for Pray versus 22° for this work.
Julian Oey
Leura Observatory
94 Rawson Pde. Leura Australia
[email protected]
J. Világi, Š. Gajdoš, L. Kornoš, A. Galád
Modra Observatory
842 48 Bratislava, Slovakia
1241 Dysona. This target was selected from a list of target
suggested in the CALL website (Warner 2006). Behrend (2002)
previously reported a period of 8.856 h. However, correspondence
with Behrend indicated that his data covered short segments of the
curve and so there were a number of other possible solutions. The
observations from Leura Observatory from April 21 to May 6,
2006, produced a unique period of 8.6080 ± 0.0005 h.
The synodic periods for several asteroids were obtained
during the second half of 2006: 1301 Yvonne, 7.3200h;
1241 Dysona, 8.6080h; 2910 Yoshkar-Ola, 3.4233h,
3105 Stumpff, 5.0369h; 3258 Somnium, 5.3379h; 3850
Peltier, 2.4289h; (6263) 1980 PX, 3.464h; 3665
Fitzgerald, 2.4142h; 12696 Camus, 3.78h.
Kingsgrove Observatory is a new addition to Oey’s observation
platform. The observatory is equipped with a 10” Meade Schmidt
Cassegrain Telescope operating with a focal reducer at f/5.2 The
telescope is mounted on a fixed pier using a CG-11 Losmandy
equatorial mount modified to accept the Gemini robotic controller.
Recently a new SBIG ST-402ME was purchased to make the
telescope fully functional for photometry work. The combined
telescope and camera has a working resolution of 1.41”/pixel at
1x1 binning. When longer than a 2-minute exposures were
required, a separate 120mm achromatic refractor guide scope and
SBIG ST-4 camera were used for guiding. Kingsgrove
Observatory will perform work mainly on targets in the Southern
Hemisphere because surrounding buildings and vegetation prevent
the telescope viewing more than 2-hours worth of Northern
Hemisphere targets.
Leura Observatory’s location and instrumentation has been
documented previously in Oey (2006). Leura Observatory has
joined the Photometry Survey of Asynchronous Binary Asteroid
(PSABA) project directed by Petr Pravec. All except 1301
Yvonne, 1241 Dysona and 12696 Camus were selected from the
list provided by the above project. Modra Observatory used a
0.6m,f/5.5 reflector with an AP8p CCD camera. Image dimensions
were 25 arcminutes square (1.5 arcseconds per pixel). All images
were taken through clear filter.
Image analysis was done using MPO Canopus, which employs
differential aperture photometry and the Fourier period analysis
algorithm developed by Harris (1989). All images were unfiltered.
Dark frames and flat fields were used for image calibration. Other
software used were TheSky 6 Pro and CCDSoft V5 from Software
# Name
1301
1241
2910
3105
3258
3850
6263
12696
Yvonne
Dysona
Yoshkar-Ola
Stumpff
Somnium
Peltier
1980 PX
Camus
Date (mm/dd) Points
2006
11/13 - 04/12
223
04/21 - 05/06
248
09/23 - 10/04
323
10/31 - 11/28
471
10/09 - 10/15
356
09/28 - 10/18
260
10/12 - 10/28
196
10/10
61
2910 Yoshkar-Ola and 3850 Peltier. Both minor planets were
recommended targets for observation as part of the PSABA
project. There were no previous lightcurve parameters reported for
either of these asteroids. The period for 2910 Yoshkar-Ola was
found to be 3.4233 ± 0.0001 h while that for 3850 Peltier was
determined to be 2.4289 ± 0.0001 h.
3105 Stumpff. The derived period is 5.0369 ± 0.0001 h with an
amplitude of 0.34 ± 0.05 mag. No previous published parameters
were found. Observations at Modra on Oct. 31 and Nov. 8 showed
an unexpected brightening, near phase 0.8, that could not be
explained by an intervening background star. Subsequent
observations over five more sessions were not able to reproduce
the above anomaly and so no reasonable explanation can be
offered.
3258 Somnium. This asteroid was a target within the PSABA
project and had no previously reported lightcurve parameters. Our
data (five sessions by Leura and one session at Modra) revealed a
synodic period of 5.3379 ± 0.0002 h with an amplitude of 0.80 ±
0.05 mag.
(6263) 1980 PX. This was another target in PSABA program. A
significant attenuation was noted Oct. 10, indicating that this
target might be binary. However, because the asteroid was fading
rapidly, it was not possible to obtain sufficient observations to
confirm this possibility. The data we did obtain indicates a period
of 3.464 ± 0.002 h and amplitude of 0.05 ± 0.05 mag. The next
favorable apparition is in 2009. At that time, the asteroid will be
bright enough for most observers to try to confirm if the asteroid is
indeed a binary.
12696 Camus. This asteroid was worked because it happened to be
in the same field with 3258 Somnium. The derived period derived
is 3.78 ± 0.04 h.
Period (h)
7.3200
8.6080
3.4233
5.0369
5.3379
2.4289
3.464
3.78
±
±
±
±
±
±
±
±
0.0001
0.0005
0.0001
0.0001
0.0002
0.0001
0.002
0.04
Amp. (m)
0.90
0.24
0.36
0.35
0.80
0.10
0.05
0.40
±
±
±
±
±
±
±
±
PA
LPAB
BPAB
0.05 21.5,23.2
50.5,52.7 -42.9,-44.0
0.05 10.2,13.1 195.3,195.5 -24.1,-24.4
0.05 12.8,11.3 223.3,226.7 -21.3,-21.1
0.02
6.8,14.3
41.5,43.4
-9.4,-9.1
0.05
4.5,4.7
17.1,17.7
-5.8,-5.3
0.05
8.0
13.6,15.0
-7.3,-7.6
0.05
6.9,16.3
9.9,12.6
-2.0,-2.2
0.05
3.0
17.3
-6.3
82
Acknowledgements
I would like to thank Dr. Petr Pravec of the Astronomical Institute,
Czech Republic, for his encouragement and support to the amateur
astronomical community through his PSABA project. The work
at Modra has been supported by the Slovak Grant Agency for
Science VEGA, Grant 1/3074/06.
References
Behrend, R. (2002). Observatoire de Geneve web site.
http://obswww.unige.ch/~behrend/page_cou.html
H., and Zeigler, K.W. (1989), “Photoelectric Observations of
Oey, J. (2006), “Lightcurve analysis of 10 Asteroids from Leura
Observatory.” Minor Planet Bul. 33, 96-99.
Pray, D. (2004), “Lightcurve analysis of Asteroids 1225, 1301,
2134, 2741, and 3974.” Minor Planet Bul. 31, pp. 6-8.
Warner, B.D. (2006). Collaborative Asteroid Lightcurve
Link(CALL).
http://www.minorplanetobserver.com/astlc/default.htm.
83
LIGHTCURVE ANALYSIS OF (12735) 1991 VV1
Brian D. Warner
17995 Bakers Farm Rd., Colorado Springs, CO 80908
[email protected]
Petr Pravec, Peter Kušnirák
Astronomical Institute, CZ-25165 Ond_ejov
CZECH REPUBLIC
David Higgins
Hunters Hill Observatory, Ngunnawal, Canberra 2913
AUSTRALIA
Zuzana Kaňuchová, Marek Husárik
Skalnaté Pleso Observatory, SK 059 60 Tatranská Lomnica
SLOVAKIA
Adrián Galád, Jozef Világi
Modra Observatory
Dept of Astronomy, Physics of the Earth, and Meteorology
FMFI UK Bratislava SK-84248
SLOVAKIA
Observations of the main-belt asteroid (12735) 1991
VV1 were made by the authors from July through
September 2006. Data from two observing sessions
appeared to show deviations indicative of an eclipse or
occultation by a satellite. However, extensive follow-up
observations failed to provide confirming evidence and
so the nature of the aberrations cannot be explained. The
data did permit finding the synodic rotation period of the
asteroid, that being 3.2606 ± 0.0001 hr with the
amplitude of the lightcurve being 0.21 ± 0.03 mag.
Warner began observing (12735) 1991 VV1 on July 31, 2006.
However, the next observations were not until nearly one month
later, on August 28. The data from that session showed an
unexpected deviation of nearly 0.1 mag, which might have
indicated an eclipse or occultation event by a satellite. Notice was
sent to the Binary Asteroid Group under the supervision on Petr
Pravec at the Ondřejov Observatory in the Czech Republic, of
which the co-authors are members. The only other observer that
recorded an apparent deviation was Higgins, on September 11.
However, the cause of those deviations was attributed to improper
subtraction of a field star during measurements.
During the span from late July to mid-September, the phase angle
varied from 16.7° to 19.9°, reaching a minimum of 13.6° in midAugust. The PAB longitude changed by only six degrees and the
PAB latitude stayed within a degree of 19°. Thus the viewing
circumstances were virtually unchanged and the lack of additional
events could not be attributed to changing geometry. After
observing the asteroid over a total span of nearly seven weeks and
with only one set of observations showing deviations, the
campaign was closed for lack of conclusive evidence and the need
to cover more urgent and promising targets.
In addition to finding the lightcurve parameters: synodic period
3.2606 ± 0.0001 hr, amplitude 0.21 ± 0.03 mag, calibrated data at
Ond_ejov was used to find HR = 13.50 ± 0.2, assuming G = 0.15 ±
0.2. If V-R is assumed to be 0.45, this gives H = 13.95.
Acknowledgements
Funding for observations at the Palmer Divide Observatory is
provided by NASA grant NNG06GI32G, National Science
Foundation grant AST-0607505, and by a 2007 Gene Shoemaker
NEO Grant from the Planetary Society. The work at Ondřejov
was supported by the Grant Agency of the Czech Republic, Grant
205/05/0604. The work at Skalnaté Pleso Observatory was
supported by VEGA: the Slovak Grant Agency for Science (grant
No. 4012). The work at Modra was supported by the Slovak Grant
Agency for Science VEGA, Grant 1/3074/06. The SBIG ST-8E
used by Hunters Hill was funded by The Planetary Society under
the 2005 Gene Shoemaker NEO Grants program.
Observer
Warner
Kušnirák
Galád/Világi
Kańuchová/Husárik
Higgins
Dates (mm/dd) 2006
07/31, 08/29-31, 09/13
09/01, 11, 13, 17
09/02, 09, 10
09/02
09/11, 12
84
2454105.0. This is a slightly different result to that by Higgins
(2007) posted on his website, where a value of 11.363 ± 0.004 h is
quoted. The peak-to-peak variation of 0.38 magnitudes in the
lightcurve implies an axial ratio (a/b) of 1.42 (if viewed at an
equatorial aspect). Full phase coverage was achieved with a high
density of points and this is considered a secure result.
References
Bembrick, C.S., Richards, T., Bolt, G., Pereghy, B., Higgins, D.
and Allen, W.H. (2004). “172 Baucis – A Slow Rotator”. Minor
Planet Bulletin 31, 51-52.
Fig 1. The combined data set lightcurve for (12375) 1991 VV1.
The “stray” data near phase 0.9 are from Warner on Aug. 28.
THE ROTATION PERIOD OF 865 ZUBAIDA
Colin Bembrick
PO Box 1537, Bathurst, NSW 2795, AUSTRALIA
[email protected]
Greg Crawford
Bagnall Beach Observatory
Salamander Bay, NSW, AUSTRALIA
GUIDE version 8 (2002). http://www.projectpluto.com
Harris, A.W. and Warner, B.D. (2006). “Minor Planet Lightcurve
Parameters”. Last Updated March 2006.
Higgins D. (2007). “Minor Planet Lightcurves”.
http://www.davidhiggins.com/Astronomy/asteroid/lightcurves.htm
Vanmunster, T. (2006). Peranso ver 2.0. http://www.peranso.com
Greg Bolt
Craigie, WA 6025, AUSTRALIA
Bill Allen
Vintage Lane Observatory
Blenheim, NEW ZEALAND
Table I. Aspect data for Zubaida in 2007.
(Received: 1 April Accepted: 31 March)
Minor planet 865 Zubaida was observed over 10 nights
in Jan 2007. The synodic period was determined as
11.3533 ± 0.0061 h. The peak-to-peak amplitude of
Zubaida was 0.38 magnitudes, implying an axial ratio
(a/b) of 1.42.
Minor planet 865 Zubaida (1917 BO) was discovered by Max
Wolf at Heidelberg in 1917. It is an inner main-belt asteroid with a
quoted diameter of 20.7 km and an albedo of 0.039 (Guide, 2002).
The latest list of rotational parameters (Harris & Warner, 2006)
has no quoted period.
UT Date
2007 Jan
2007 Jan
2007 Jan
2007 Jan
2007 Jan
2007 Jan
2007 Jan
2007 Jan
2007 Jan
2007 Jan
The observations of Zubaida were conducted from four sites – one
in New Zealand and three in Australia. The locations of these sites
are listed in Bembrick et al (2004) and enabled a longitude spread
of some 58 degrees. All observations were made using unfiltered
differential photometry and were light time corrected. The aspect
data (Table I) also shows the percentage of the lightcurve
observed each night. PAB is the Phase Angle Bisector.
Period analysis was carried out using the “Peranso” software
(Vanmunster, 2006). Various routines available in Peranso were
used (including the “FALC” routine based on Harris et al 1989)
and these gave near identical results, with a single strong peak in
the power spectrum. The final analysis determined a period of
11.3533 ± 0.0061 h with an arbitrary epoch of minimum at
05
06
07
08
10
11
14
16
17
18
LPAB
101.9
102.0
102.1
102.2
102.3
102.4
102.7
102.8
102.9
103.0
BPAB
-18.9
-18.9
-18.9
-18.8
-18.7
-18.6
-18.4
-18.3
-18.2
-18.1
Phase
Angle
12.4
12.5
12.6
12.7
13.0
13.2
13.8
14.3
14.6
14.9
%Phase
Coverage
31
50
61
23
44
78
31
42
50
31
85
GENERAL REPORT OF POSITION OBSERVATIONS
BY THE ALPO MINOR PLANETS SECTION
FOR THE YEAR 2006
Frederick Pilcher
4438 Organ Mesa Loop
Las Cruces, NM 88011 USA
During the year 2006 a total of 1855 positions of 566 different
minor planets were reported by members of the Minor Planets
Section. Of these 93 are CCD images (denoted C), and 24 are
photographic measures (denoted P). All the rest are approximate
visual positions.
The summary lists minor planets in numerical order, the observer
and telescope aperture (in cm), UT dates of the observations, and
the total number of observations in that period. The year is 2006
in each case.
Positional observations were contributed by the following
observers:
Observer, Instrument
Location
Planets
Arlia, Saverio
15 cm f/6 reflector
Buenos Aires,
Argentina
Bookamer, Richard E.
41 cm reflector
Micco, Florida
USA
Faure, Gerard
20 cm Celestron,
10 cm binoculars
Col de L'Arzelier,
France
96
Faure, Gerard, and
Dos Santos, Henri
20 cm Celestron
Col de L'Arzelier,
France
1
Garrett, Lawrence
32 cm f/6 reflector
20x80 mm binoculars
Fairfax, Vermont,
USA
Harvey, G. Roger
74 cm Newtonian
Concord, North
Carolina, USA
2
180
15
115
Positions
24P
520
290(93C)
2
Stephenville,
257
536
Texas, USA
Sep 19, 20 observations
from Kenton, Oklahoma, USA
Pryal, Jim
20 cm f/10 SCT
Federal Way, WA USA
4
8
Watson, William W.
20 cm Celestron
Tonawanda, NY USA
and vicinity. Oct.
observations from
Portal, AZ USA
7
28
NO.
OBS.
Garrett, 32
Aug 25
2
Faure, 20
Jun 11
6C
Mar 29-31
2
Faure and Dos Santos, 10
Garrett, 9, 32
Aug 6-25
2
14 Irene
Faure, 20
Sep 1
3C
15 Eunomia
Garrett, 9, 32
Aug 6-25
2
22 Kalliope
Bookamer, 41
Dec 30
3
25 Phocaea
Pryal, 20
Oct 28
2
44 Nysa
Bookamer, 41
Dec 30
3
54 Alexandra
Bookamer, 41
Nov 28
3
68 Leto
Pryal, 20
Sep 28
2
70 Panopaea
Bookamer, 41
Nov 30
3
75 Eurydike
Bookamer, 41
Faure, 20
Pryal, 20
Aug 12
Jul 2
Aug 26
2
8C
2
91 Aegina
Faure, 20
Jun 10
3C
102 Miriam
Bookamer, 41
May 17
2
105 Artemis
Bookamer, 41
Faure, 20
Mar 30
Jun 10
3
2C
109 Felicitas
Faure, 20
Sep 1
4C
117 Lomia
Watson, 20
Oct 21-25
4
119 Althaea
Watson, 20
Sep18-22
3
137 Meliboea
Bookamer, 41
Mar 30
3
139 Juewa
Bookamer, 41
Jan 7
3
147 Protogeneia
Bookamer, 41
Jan 12
2
151 Abundantia
Bookamer, 41
Jan 6
2
153 Hilda
Bookamer, 41
Apr 16
2
171 Ophelia
Bookamer, 41
Jun
2
174 Phaedra
Bookamer, 41
Feb 20
2
177 Irma
Watson, 20
Oct 19-23
5
186 Celuta
Bookamer, 41
Pryal, 20
Watson, 20
Sep 6
Sep 28
Sep 21-22
3
2
2
188 Menippe
Bookamer, 41
Apr 17
4
191 Kolga
Garrett, 32
Aug 25
2
195 Eurykleia
Bookamer, 41
Apr 14
2
197 Arete
Bookamer, 41
May 30
2
200 Dynamene
Bookamer, 41
Garrett, 32
Aug 5
Aug 25
2
2
201 Penelope
Bookamer, 41
Jul 15
2
202 Chryseïs
Garrett, 32
Apr 30
2
212 Medea
Bookamer, 41
Jan 6
2
217 Eudora
Bookamer, 41
Jul 26
2
224 Oceana
Bookamer, 41
Jan 10
2
228 Agathe
Bookamer, 41
Jul 4
3
231 Vindobona
Bookamer, 41
Jun 23
2
236 Honoria
Bookamer, 41
Apr 29
2
244 Sita
Bookamer, 41
Dec 19
2
249 Ilse
Bookamer, 41
Aug 14
3
257 Silesia
Bookamer, 41
Feb 5
3
268 Adorea
Bookamer, 41
Feb 26
3
33
414
OBSERVING
PERIOD (2006)
2 Pallas
6 Hebe
Observations of positions of minor planets by members
of the Minor Planets Section in calendar year 2006 are
summarized.
OBSERVER &
APERTURE (cm)
1 Ceres
4 Vesta
(Received: 5 April)
Hudgens, Ben
38 cm f/5 reflector
MINOR
PLANET
14
86
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
279 Thule
Bookamer, 41
Jan 2
3
601 Nerthus
Bookamer, 41
Jul 26
3
292 Ludovica
Bookamer, 41
Feb 22
2
603 Timandra
298 Baptistina
Bookamer, 41
Oct 18
3
Faure, 20
Hudgens, 38
Nov 28
Dec 12
2
2
300 Geraldina
Bookamer, 41
Dec 21
3
608 Adolfine
Hudgens, 38
Sep 30
2
612 Veronika
301 Bavaria
Bookamer, 41
Aug 15
3
Faure, 20
Hudgens, 38
Jun 24-Jul
Jun 28
305 Gordonia
Bookamer, 41
May 14
3
616 Elly
Bookamer, 41
Mar 26
4
311 Claudia
Bookamer, 41
Nov 23
4
623 Chimaera
Bookamer, 41
Dec 18
3
312 Pierretta
Bookamer, 41
May 5
2
637 Chrysothemis
318 Magdalena
Bookamer, 41
Sep 20
3
Faure, 20
Hudgens, 38
Nov 19
Nov 12
2
2
322 Phaeo
Bookamer, 41
Jun 1
2
638 Moira
Bookamer, 41
Feb 18
4
640 Brambilla
Bookamer, 41
Feb 26
3
329 Svea
Bookamer, 41
Aug 1
2
341 California
Bookamer, 41
Aug 1
3
642 Clara
Bookamer, 41
Jan 30
3
349 Dembowska
Arlia, 15
Sep 15-21
9P
645 Agrippina
Bookamer, 41
Jan 4
3
672 Astarte
Bookamer, 41
Sep 21
3
359 Georgia
Bookamer, 41
Apr 15
2
362 Havnia
Bookamer, 41
Aug 14
2
678 Fredegundis
Bookamer, 41
Jul 16
3
683 Lanzia
Bookamer, 41
Jan 18
3
685 Hermia
Bookamer, 41
Aug 18
3
695 Bella
Watson, 20
Oct 22-23
2
700 Auravictrix
Bookamer, 41
Feb 5
3
14(11C)
2
369 Aëria
Bookamer, 41
Sep 20
2
370 Modestia
Bookamer, 41
May 30
3
371 Bohemia
Bookamer, 41
Garrett, 32
Sep 10
Aug 31-Sep 1
2
3
380 Fiducia
Bookamer, 41
Oct 1
2
707 Steïna
Bookamer, 41
Aug 28
4
393 Lampetia
Harvey, 73
Dec 20
6
710 Gertrud
Hudgens, 38
May 17
2
396 Aeolia
Bookamer, 41
Jun 19
2
717 Wisibada
Bookamer, 41
Sep 12
4
401 Ottilia
Bookamer, 41
Jun 22
3
723 Hammonia
Bookamer, 41
Jan 3
3
409 Aspasia
Faure, 20
Jun 11-Sep 1
725 Amanda
Faure, 20
Oct 27
2
414 Liriope
Bookamer, 41
Dec 19
3
731 Sorga
Bookamer, 41
Jun 22
3
422 Berolina
Bookamer, 41
Nov 25
3
737 Arequipa
Bookamer, 41
Mar 4
4
424 Gratia
Bookamer, 41
Sep 22
3
743 Eugenisis
Bookamer, 41
Jan 18
3
443 Photographica
Bookamer, 41
Oct 4
2
747 Winchester
Bookamer, 41
Jan 28
3
451 Patientia
Hudgens, 38
Oct 28
2
748 Simeïsa
Bookamer, 41
Jan 2
3
459 Signe
Bookamer, 41
Sep 25
3
752 Sulamitis
Bookamer, 41
May 31
2
465 Alekto
Bookamer, 41
Aug 14
3
756 Lilliana
Bookamer, 41
Apr 15
3
466 Tisiphone
Bookamer, 41
Jan 3
2
759 Vinifera
Bookamer, 41
Jul 28
3
474 Prudentia
Bookamer, 41
Jul 28
3
760 Massinga
Bookamer, 41
Jan 14
2
477 Italia
Bookamer, 41
Jul 29
3
764 Gedania
Bookamer, 41
Jan 20
3
482 Petrina
Bookamer, 41
Apr 14
2
767 Bondia
Bookamer, 41
Jul 26
3
486 Cremona
Bookamer, 41
Jan 19
3
790 Pretoria
Bookamer, 41
Jan 23
2
489 Comacina
Bookamer, 41
Feb 8
2
798 Ruth
Bookamer, 41
Jun 1
3
490 Veritas
Harvey, 73
Jan 28
6
799 Gudula
Bookamer, 41
Oct 14
3
492 Gismonda
Bookamer, 41
Jul 26
3
802 Epyaxa
500 Selinur
Bookamer, 41
Jun 18
2
Faure, 20
Hudgens, 38
Apr 22
Mar 1
2
2
806 Gyldenia
507 Laodica
Bookamer, 41
Jul 24
3
Faure, 20
Hudgens, 38
Feb 1
Jan 3-6
2
2
521 Brixia
Bookamer, 41
Jun 22
2
807 Ceraskia
Hudgens, 38
Aug 26-30
4
522 Helga
Faure, 20
Dec 25-26
532 Herculina
Arlia, 15
Jul 19-Aug 29
565 Marbachia
Bookamer, 41
571 Dulcinea
585 Bilkis
13C
2
813 Baumeia
Bookamer, 41
Jan 18
3
15P
820 Adriana
Hudgens, 38
Jul 19
2
Nov 23
3
822 Lalage
Bookamer, 41
Dec 17
3
Bookamer, 41
Sep 10
3
824 Anastasia
Bookamer, 41
Sep 12
3
Bookamer, 41
Sep 18
2
825 Tanina
Bookamer, 41
Jun 19
3
587 Hypsipyle
Hudgens, 38
Mar 1
2
826 Henrika
Bookamer, 41
Hudgens, 38
Jul 14
Jun 28
3
2
600 Musa
Bookamer, 41
Jul 24
3
87
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
834 Burnhamia
Bookamer, 41
Sep 16
3
1085 Amaryllis
Bookamer, 41
Aug 18
3
845 Naëma
Bookamer, 41
Sep 23
3
1089 Tama
Bookamer, 41
Oct 25
3
866 Fatme
Bookamer, 41
Mar 31
2
1094 Siberia
Hudgens, 38
Dec 15
2
867 Kovacia
Faure, 20
Nov 18
2
1100 Arnica
Hudgens, 38
Jun 19
2
869 Mellena
Hudgens, 38
Aug 26-30
4
1107 Lictoria
Bookamer, 41
Dec 8
3
870 Manto
Faure, 20
Hudgens, 38
Oct 26
Oct 13
2
2
1113 Katja
Bookamer, 41
Nov 25
3
Hudgens, 38
Jul 15-16
4
1115 Sabauda
Bookamer, 41
Mar 1
3
1152 Pawona
Bookamer, 41
Hudgens, 38
Mar 24
Mar 25
4
2
876 Scott
879 Ricarda
Hudgens, 38
Oct 13
2
880 Herba
Hudgens, 38
Nov 11
2
1159 Granada
881 Athene
Bookamer, 41
Faure, 20
Sep 22
Jun 11-Jul 2
4
9C
Faure, 20
Hudgens, 38
Sep 1
Aug 31
3
2
1177 Gonnessia
Bookamer, 41
Mar 25
3
882 Swetlana
Bookamer, 41
Faure, 20
Sep 16
Aug 31-Sep 1
3
2
1187 Afra
Bookamer, 41
Hudgens, 38
Oct 12
Oct 13
3
2
886 Washingtonia
Bookamer, 41
Jun 24
4
1189 Terentia
Bookamer, 41
Dec 17
3
902 Probitas
Bookamer, 41
Faure, 20
Hudgens, 38
Sep 20
Oct 26
Sep 15
3
2
2
1190 Pelagia
Hudgens, 38
Oct 18
2
1191 Alfaterna
Hudgens, 38
Jun 30
2
906 Repsolda
Bookamer, 41
Sep 18
3
1203 Nanna
Hudgens, 38
Jan 6
2
911 Agamemnon
Hudgens, 38
Jul 29-30
2
1204 Renzia
Bookamer, 41
Oct 23
3
916 America
Bookamer, 41
Aug 19
3
1211 Bressole
Hudgens, 38
Oct 28
2
918 Itha
Bookamer, 41
Aug 20
3
1214 Richilde
Bookamer, 41
Hudgens, 38
Oct 25
Sep 30
3
2
919 Ilsebill
Faure, 20
Nov 28
2
935 Clivia
Hudgens, 38
Sep 15
2
1216 Askania
Hudgens, 38
Jun 30
2
1219 Britta
Bookamer, 41
Oct 23
3
1223 Neckar
Hudgens, 38
Jan 6
2
1227 Geranium
Hudgens, 38
Oct 13
2
1242 Zambesia
Bookamer, 41
Oct 1
3
1245 Calvinia
Bookamer, 41
Jul 4
3
1248 Jugurtha
Bookamer, 41
Jan 4
3
1257 Móra
Faure, 20
Jun 23-26
6
1258 Sicilia
Hudgens, 38
Aug 31
2
1261 Legia
Hudgens, 38
May 17
2
1264 Letaba
Bookamer, 41
Jun 15
3
1268 Libya
Bookamer, 41
Jan 2
3
1269 Rollandia
Hudgens, 38
Jun 19
2
940 Kordula
Bookamer, 41
Jul 29
3
953 Painleva
Bookamer, 41
Oct 22
3
957 Camelia
Hudgens, 38
Oct 13
2
964 Subamara
Hudgens, 38
Sep 15
2
969 Leocadia
Garrett, 32
Nov 25
2
972 Cohnia
Bookamer, 41
Aug 15
3
979 Ilsewa
Bookamer, 41
Jul 16
3
983 Gunila
Bookamer, 41
Jul 14
3
984 Gretia
Bookamer, 41
Jul 16
5
997 Priska
Hudgens, 38
Aug 21
2
998 Bodea
Faure, 20
Hudgens, 38
Oct 16
Sep 18-19
2
3
1013 Tombecka
Bookamer, 41
Oct 22
3
1273 Helma
Hudgens, 38
Aug 25
2
1017 Jacqueline
Hudgens, 38
Oct 21
2
1275 Cimbria
Bookamer, 41
Aug 16
3
1023 Thomana
Bookamer, 41
Jan 31
3
1279 Uganda
Hudgens, 38
Jun 15
2
1024 Hale
Hudgens, 38
Dec 14
2
1281 Jeanne
Bookamer, 41
Apr 27
3
1030 Vitja
Hudgens, 38
Mar 1
2
1283 Komsomolia
Hudgens, 38
Nov 23
2
1039 Sonneberga
Hudgens, 38
Jun 28
2
1284 Latvia
Bookamer, 41
Aug 26
3
1040 Klumpkea
Hudgens, 38
Oct 28
2
1285 Julietta
Hudgens, 38
Oct 18
2
1050 Meta
Hudgens, 38
Oct 18
2
1289 Kutaïssi
Hudgens, 38
Oct 13
2
1051 Merope
Hudgens, 38
Sep 30
2
1290 Albertine
1055 Tynka
Bookamer, 41
Jul 14
3
Faure, 20
Hudgens, 38
Oct 26-27
Oct 13
2
2
1293 Sonja
1059 Mussorgskia
Bookamer, 41
Apr 16
3
Bookamer, 41
Hudgens, 38
Jul 22
Jul 19
4
2
1062 Ljuba
Bookamer, 41
Apr 27
3
1296 Andrée
Bookamer, 41
Mar 4
3
1070 Tunica
Faure, 20
Jun 29
3
1297 Quadea
Hudgens, 38
Nov 23
2
1071 Brita
Bookamer, 41
Sep 27
3
1300 Marcelle
Hudgens, 38
Oct 18
2
1078 Mentha
Bookamer, 41
Feb 23
3
1305 Pongola
Hudgens, 38
May 18
2
88
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
1309 Hyperborea
Hudgens, 38
Nov 11
2
1604 Tombaugh
Faure, 20
Jul 26-27
2
1310 Villigera
Bookamer, 41
Feb 21
3
1613 Smiley
1320 Impala
Faure, 20
May 26-27
5
Bookamer, 41
Hudgens, 38
Jan 23
Jan 31
3
2
1329 Eliane
Bookamer, 41
Aug 14
3
1623 Vivian
Hudgens, 38
Jan 31
2
1629 Pecker
Hudgens, 38
May 16-17
2
1332 Marconia
Faure, 20
Jun 29-30
2
1336 Zeelandia
Hudgens, 38
Aug 30
2
1631 Kopff
Bookamer, 41
Aug 25
3
1633 Chimay
Hudgens, 38
Dec 12
2
1348 Michel
Hudgens, 38
Dec 12-14
4
1653 Yakhontovia
Bookamer, 41
Jan 25
3
1350 Rosselia
Faure, 20
Hudgens, 38
Aug 31-Sep 1
Aug 30
2
2
1676 Kariba
Hudgens, 38
Jun 28
2
1353 Maartje
Faure, 20
Sep 2
5C
1682 Karel
1362 Griqua
Hudgens, 38
Dec 14
2
Bookamer, 41
Faure, 20
Hudgens, 38
Sep 12
Aug 31-Sep 1
Aug 31
3
2
2
1364 Safara
Hudgens, 38
May 16-17
2
1690 Mayrhofer
Hudgens, 38
Oct 18
2
1365 Henyey
Faure, 20
Nov 18
2
1692 Subbotina
Hudgens, 38
Sep 15
2
1367 Nongoma
Harvey, 73
Jul 31
3
1695 Walbeck
Hudgens, 38
Oct 18
2
1369 Ostanina
Bookamer, 41
Jul 28
3
1702 Kalahari
Hudgens, 38
Jul 16
2
1384 Kniertje
Bookamer, 41
Feb 17-Mar 1
4
1711 Sandrine
Hudgens, 38
Sep 19
2
1385 Gelria
Bookamer, 41
Jan 20
4
1717 Arlon
Hudgens, 38
Jan 20
2
1388 Aphrodite
Faure, 20
Apr 22
2
1720 Niels
Hudgens, 38
Jan 3-6
2
1397 Umtata
Bookamer, 41
Faure, 20
May 18
Jun 23
3
2
1723 Klemola
Hudgens, 38
Aug 25
2
1424 Ruvuma
Bookamer, 41
Sep 18
3
1724 Vladimir
Hudgens, 38
Dec 15
2
1729 Beryl
Hudgens, 38
Jul 29-30
2
1756 Giacobini
Hudgens, 38
Nov 23
2
1773 Rumpelstilz
Faure, 20
Hudgens, 38
Apr 22
Apr 3
2
2
1434 Margot
Hudgens, 38
Sep 19
2
1435 Garlena
Hudgens, 38
Jan 6
2
1444 Pannonia
Hudgens, 38
Mar 1
2
1453 Fennia
Hudgens, 38
Apr 3
2
1777 Gehrels
Hudgens, 38
Jun 19
2
1456 Saldanha
Hudgens, 38
Aug 21
2
1784 Benguella
Hudgens, 38
Jul 29-30
2
1462 Zamenhof
Hudgens, 38
Apr 3
3
1797 Schaumasse
Hudgens, 38
Oct 13
2
1467 Mashona
Bookamer, 41
Aug 18
3
1798 Watts
Hudgens, 38
Dec 15
2
1493 Sigrid
Bookamer, 41
Aug 2
3
1804 Chebotarev
Hudgens, 38
Nov 11
2
1495 Helsinki
Hudgens, 38
Jun 19
2
1808 Bellerophon
Hudgens, 38
Dec 12-14
4
1503 Kuopio
Bookamer, 41
Dec 21
3
1847 Stobbe
1509 Eslangona
Hudgens, 38
Jun 28
2
Faure, 20
Hudgens, 38
Jul 26
Jul 19
2
2
1515 Perrotin
Hudgens, 38
Oct 28
2
1848 Delvaux
Hudgens, 38
Aug 30
2
1879 Broederstroom
1517 Beograd
Hudgens, 38
Jun 19
2
Bookamer, 41
Hudgens, 38
Dec 21
Dec 14
3
2
1523 Pieksämäki
Hudgens, 38
Jan 3-6
2
1888 Zu Chong-Zhi
Hudgens, 38
Jan 6
2
1535 Päijänne
Hudgens, 38
Oct 23
2
1909 Alekhin
Faure, 20
Aug 31-Sep 1
2
1542 Schalén
Hudgens, 38
Jul 29-30
2
1913 Sekanina
Hudgens, 38
Sep 19
2
1550 Tito
Bookamer, 41
Faure, 20
Nov 22
Dec 25-26
3
2
1939 Loretta
Hudgens, 38
May 17
2
1551 Argelander
Hudgens, 38
Aug 31
2
1950 Wempe
Hudgens, 38
Jan 20
2
1562 Gondolatsch
Bookamer, 41
Hudgens, 38
Feb 28
Mar 1
4
2
1953 Rupertwildt
Harvey, 73
Oct 24
3
1980 Tezcatlipoca
1581 Abanderada
Hudgens, 38
May 17
2
Bookamer, 41
Hudgens, 38
Nov 23
Nov 23
3
2
1582 Martir
Hudgens, 38
Jun 15
2
1988 Delores
Harvey, 73
Dec 15
3
1584 Fuji
Hudgens, 38
Sep 20
2
1996 Adams
Faure, 20
Hudgens, 38
Oct 16-27
Oct 13
4
2
1587 Kahrstedt
Bookamer, 41
Mar 4
3
1999 Hirayama
1590 Tsiolkovskaja
Bookamer, 41
Garrett, 32
Apr 27
Apr 30
3
2
Bookamer, 41
Hudgens, 38
Feb 20
Mar 1
3
2
2007 McCuskey
Hudgens, 38
May 16-17
2
1592 Mathieu
Faure, 20
Apr 23
2
2023 Asaph
Bookamer, 41
Oct 14
3
1599 Giomus
Hudgens, 38
Dec 12
2
2027 Shen Guo
Hudgens, 38
Nov 12
2
1601 Patry
Hudgens, 38
Sep 15
2
2047 Smetana
Harvey, 73
Apr 2
3
89
MINOR
PLANET
2050 Francis
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
Faure, 20
Hudgens, 38
May 28
May 26
4
2
2058 Róka
Hudgens, 38
Jun 28
2
2077 Kiangsu
Harvey, 73
Hudgens, 38
Nov 18
Nov 23
6
2
2091 Sampo
Faure, 20
Hudgens, 38
Nov 27
Oct 28
2
2
2094 Magnitka
Bookamer, 41
Hudgens, 38
Mar 19
Mar 1
3
2
2098 Zyskin
Hudgens, 38
Aug 31
2131 Mayall
Bookamer, 41
Hudgens, 38
2140 Keremovo
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
2634 James Bradley
Hudgens, 38
Dec 15
2
2651 Karen
Hudgens, 38
Oct 28
2
2670 Chuvashia
Hudgens, 38
Oct 21
2
2674 Pandarus
Harvey, 73
Feb 28
2
2675 Tolkien
Faure, 20
Aug 31
2
2699 Kalinin
Hudgens, 38
Nov 23
2
2754 Efimov
Hudgens, 38
Sep 15
2
2
2802 Weisell
Faure, 20
May 26-27
2
Aug 3
Aug 21
3
2
2819 Ensor
Hudgens, 38
Aug 25
2
Faure, 20
Jul 27
2
2834 Christy Carol
Hudgens, 38
Jan 6
2
2150 Nyctimene
Hudgens, 38
Oct 23
2
2862 Vavilov
Hudgens, 38
Mar 1
2
2873 Binzel
2151 Hadwiger
Hudgens, 38
Nov 11
2
Faure, 20
Hudgens, 38
Jun 23-24
Jun 15
3
2
2152 Hannibal
Bookamer, 41
Garrett, 32
Nov 18
Nov 23
4
2
2886 Tinkaping
Harvey, 73
Jan 4
3
2165 Young
Hudgens, 38
Aug 25
2
2909 Hoshi-no-ie
Hudgens, 38
Nov 23
2
2910 Yoshkar-Ola
Harvey, 73
Sep 24
3
2950 Rousseau
Faure, 20
Nov 18
7
2961 Katsurahama
Hudgens, 38
Nov 23
2
2983 Poltava
Hudgens, 38
Dec 15
2
2989 Imago
Harvey, 73
Hudgens, 38
Sep 17
Sep 19
3
2
3002 Delasalle
Faure, 20
Hudgens, 38
May 26-27
May 18
2
2
3036 Krat
Hudgens, 38
Sep 30
2
3039 Yangel
Faure, 20
Jun 23
2
2183 Neufang
Hudgens, 38
Oct 18
2
2215 Sichuan
Hudgens, 38
Nov 23
2
2222 Lermontov
Hudgens, 38
Jan 3-6
2
2228 Soyuz-Apollo
Hudgens, 38
Nov 23
2
2233 Kuznetsov
Hudgens, 38
Oct 21
2
2237 Melnikov
Hudgens, 38
Dec 12
2
2241 Alcathous
Harvey, 73
Jan 26
3
2258 Viipuri
Hudgens, 38
Dec 14
2
2259 Sofievka
Hudgens, 38
Sep 30
2
3043 San Diego
Hudgens, 38
Aug 31
2
2274 Ehrsson
Bookamer, 41
Hudgens, 38
Mar 18
Mar 25
3
2
3060 Delcano
Hudgens, 38
Aug 25
2
2276 Warck
Hudgens, 38
Jun 28
2
3065 Sarahill
Harvey, 73
Jan 4
3
2288 Karolinum
Hudgens, 38
Mar 1
2
3073 Kursk
Harvey, 73
Nov 18
3
2294 Andronikov
Faure, 20
Aug 22
2
3077 Henderson
Hudgens, 38
Dec 12
2
2302 Florya
Hudgens, 38
Aug 25
2
3115 Baily
Hudgens, 38
Aug 30
2
2323 Zverev
Hudgens, 38
Jan 31
2
3156 Ellington
Faure, 20
Hudgens, 38
Apr 22
Mar 25
2
2
2333 Porthan
Hudgens, 38
Dec 12-14
4
2348 Michkovitch
Hudgens, 38
Mar 1
2
3184 Raab
Faure, 20
Oct 27
2
3197 Weissman
Hudgens, 38
Dec 14
2
3216 Harrington
Faure, 20
Harvey, 73
Sep 1
Aug 29
2
3
2357 Phereclos
Harvey, 73
Feb 28
3
2364 Seillier
Hudgens, 38
Mar 25
2
2369 Chekhov
Harvey, 73
Nov 24
3
3248 Farinella
Hudgens, 38
Jun 30
2
2376 Martynov
Hudgens, 38
Sep 30
2
3258 Somnium
Harvey, 73
Hudgens, 38
Sep 24
Oct 21
3
2
2426 Simonov
Hudgens, 38
Jun 20
2
2430 Bruce Helin
Garrett, 32
Nov 23
2
3279 Solon
Harvey, 73
Nov 19
3
2444 Lederle
Hudgens, 38
Jan 3-6
2
3353 Jarvis
Faure, 20
Aug 22
2
3431 Nakano
Hudgens, 38
Sep 15
2
2466 Golson
Hudgens, 38
Aug 30
2
2501 Lohja
Faure, 20
Hudgens, 38
Apr 22
Mar 25
2
2
3438 Inarradas
Hudgens, 38
Sep 19
2
3439 Lebofsky
Harvey, 73
Sep 24
3
2510 Shandong
Faure, 20
Hudgens, 38
Sep 1
Sep 15
2
2
3444 Stephanian
Hudgens, 38
Jan 20
2
2535 Hämeenlinna
Hudgens, 38
Mar 1
2
3453 Dostoevsky
Faure, 20
Jun 29-30
5
3500 Kobayashi
2569 Madeline
Hudgens, 38
Oct 13
2
2572 Annschnell
Harvey, 73
May 24
3
Bookamer, 41
Faure, 20
Hudgens, 38
Aug 16
Jul 26
Aug 21
3
2
2
2574 Ladoga
Hudgens, 38
Sep 19
2
3533 Toyota
Hudgens, 38
Nov 23
2
3550 Link
Hudgens, 38
Dec 15
2
2621 Goto
Hudgens, 38
Dec 12-14
4
90
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
3560 Chenquian
Faure, 20
Aug 22
2
3631 Sigyn
Hudgens, 38
Sep 19
2
3648 Raffinetti
Harvey, 73
May 24
3652 Soros
Hudgens, 38
3662 Dezhnev
Harvey, 73
Hudgens, 38
3724 Annenskij
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
4950 House
Faure, 20
Harvey, 73
Hudgens, 38
Oct 27-Nov 28
Oct 30
Nov 12
4
3
2
3
4988 Chushuho
Harvey, 73
Sep 24
3
Jun 15
2
5073 Junttura
Harvey, 73
Feb 1
3
Sep 24
Oct 23
3
2
5104 Skripnichenko
Faure, 20
May 27
2
5135 Nibutani
Hudgens, 38
May 17
2
Faure, 20
Hudgens, 38
Oct 27
Oct 13
2
2
5142 Okutama
Bookamer, 41
Faure, 20
Oct 22
Sep 2
3
2C
3728 IRAS
Hudgens, 38
Jan 31
2
3731 Hancock
Hudgens, 38
Dec 14
2
5143 Heracles
Garrett, 32
Nov 11
3
3763 Qianxuesen
Hudgens, 38
May 16-17
2
5171 Augustesen
Harvey, 73
Sep 24
3
5183 Robyn
Hudgens, 38
Jun 15
2
3773 Smithsonian
Hudgens, 38
Sep 19
2
3786 Yamada
Hudgens, 38
Aug 21
2
5192 Yabuki
Hudgens, 38
Oct 28
2
3816 Chugainov
Hudgens, 38
Jan 31
2
5199 Dortmund
Hudgens, 38
Jun 28
2
5220 Vika
Hudgens, 38
Jul 16
2
3851 Zichichi
Hudgens, 38
Oct 18
2
3870 Mayré
Faure, 20
Jul 26
2
5222 Ioffe
Faure, 20
Jun 11
13C
5241 1990 YL
Faure, 20
Harvey, 73
Nov 19
Nov 19
2
3
3913 Chemin
Faure, 20
Sep 1
5C
3921 Klement'ev
Harvey, 73
Nov 24
3
5247 Krylov
Faure, 20
May 27-28
2
3973 Ogilvie
Faure, 20
Hudgens, 38
Jul 26
Jul 29-30
2
2
5288 Nankichi
Harvey, 73
Dec 16
3
4080 Galinskij
Harvey, 73
Oct 24
3
5292 1991 AJ1
Hudgens, 38
Dec 15
2
5325 Silver
Faure, 20
Apr 23
2
4082 Swann
Hudgens, 38
Aug 30
2
4102 Gergana
Harvey, 73
Feb 1
3
5329 Decaro
Harvey, 73
Dec 16
3
5332 1990 DA
Faure, 20
Feb 2
2
5350 Epetersen
Hudgens, 38
Jun 19
2
5361 Goncharov
Harvey, 73
Apr 2
3
5363 Kupka
Harvey, 73
Dec 15
3
4214 Veralynn
Hudgens, 38
Dec 15
2
4149 Harrison
Harvey, 73
Apr 2
3
4155 Watanabe
Faure, 20
Garrett, 32
Nov 18
Nov 25
2
2
4253 Märker
Harvey, 73
Sep 15
3
5374 Hokutosei
Harvey, 73
Jan 4
3
4278 Harvey
Harvey, 73
Oct 24
3
5505 Rundetaarn
Harvey, 73
Dec 16
3
4288 1989 TQ1
Faure, 20
Hudgens, 38
Oct 16
Oct 13
2
2
5602 1991 VM1
Harvey, 73
May 24
3
4299 Wiyn
Hudgens, 38
Oct 28
2
5671 Chanal
Faure, 20
Sep 1-2
4C
5719 Křižik
Hudgens, 38
Aug 25
2
5740 Toutoumi
Harvey, 73
Hudgens, 38
Nov 19
Nov 12
3
2
5745 1991 AN
Harvey, 73
Nov 27
2
5764 1985 CS1
Faure, 20
Hudgens, 38
May 26-27
May 17
2
2
5781 Barkhatova
Harvey, 73
Hudgens, 38
Dec 16
Dec 15
3
2
5840 Raybrown
Harvey, 73
Oct 30
3
4334 1983 RO3
Harvey, 73
Nov 19
3
4335 Verona
Faure, 20
Hudgens, 38
Oct 16-17
Oct 13
2
2
4349 Tibúrcio
Faure, 20
Hudgens, 38
Dec 25-26
Nov 23
2
2
4353 Onizaki
Hudgens, 38
Jul 19
2
4420 Alandreev
Bookamer, 41
Faure, 20
Hudgens, 38
Aug 20
Jul 27
Aug 21
4
2
2
4421 Kayor
Harvey, 73
Dec 16
3
5870 Baltimore
Faure, 20
Aug 31-Sep 1
2
4428 Khotinok
Hudgens, 38
Aug 25
2
6042 Cheshirecat
4541 Mizuno
Harvey, 73
Nov 24
3
Faure, 20
Harvey, 73
Hudgens, 38
Dec 1
Nov 24
Dec 12
2
6
2
4644 Oumo
Hudgens, 38
May 18
2
6111 Davemckay
4712 Iwaizumi
Hudgens, 38
Sep 19
2
Harvey, 73
Hudgens, 38
Oct 24
Oct 21
3
2
4718 Araki
Harvey, 73
Hudgens, 38
Feb 1
Mar 1
3
2
6155 Yokosugano
Faure, 20
Nov 18
2
6260 Kelsey
4732 Froeschlé
Harvey, 73
Nov 27
3
Harvey, 73
Hudgens, 38
Aug 29
Aug 30
3
2
4843 Megantic
Harvey, 73
Feb 1
3
6261 Chione
Harvey, 73
Jan 27
6
6266 Letzel
Harvey, 73
May 24
3
6354 Vangelis
Hudgens, 38
Nov 23
2
4860 Gubbio
Faure, 20
Hudgens, 38
Oct 17-26
Oct 23
3
2
4931 Tomsk
Hudgens, 38
Sep 30
2
6361 1978 VL11
Hudgens, 38
Apr 3
2
4935 Maslachkova
Harvey, 73
Jan 4
3
6371 Heinlein
Harvey, 73
Jan 27
3
91
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
MINOR
PLANET
OBSERVER &
APERTURE (cm)
OBSERVING
PERIOD (2006)
NO.
OBS.
6387 1989 WC
Harvey, 73
Nov 27
3
17260 2000 JQ58
Harvey, 73
Feb 1
3
6393 1990 HM1
Harvey, 73
Jan 26
3
17512 1992 RN
Hudgens, 38
Jun 20
2
6406 1992 MJ
Faure, 20
Hudgens, 38
Jul 27
Jul 29-30
2
2
17681 Tweedledum
Harvey, 73
Nov 18
3
6425 1994 WZ3
Faure, 20
Oct 27
2
17700 1997 GM40
Hudgens, 38
Dec 12
2
18105 2000 NT3
Harvey, 73
Nov 27
3
6495 1992 UB1
Harvey, 73
Aug 29
3
18301 Konyukhov
Harvey, 73
Sep 17
3
6794 Masuisakura
Garrett, 32
Hudgens, 38
Nov 25
Nov 11
2
2
18487 1996 AU3
Faure, 20
Jun 23
2
6934 1994 YN2
Hudgens, 38
Jul 19
2
18590 1997 YO10
Hudgens, 38
Jul 19
2
6979 Shigefumi
Harvey, 73
Hudgens, 38
Aug 29
Sep 19
3
2
19288 1996 FJ5
Harvey, 73
Hudgens, 38
Oct 24
Oct 23
3
2
7083 Kant
Harvey, 73
Oct 24
3
20691 1999 VY72
Hudgens, 38
Jul 19
2
7088 Ishtar
Harvey, 73
Jan 27
6
21056 1991 CA1
Harvey, 73
Jan 7
3
7262 Sofue
Faure, 20
Hudgens, 38
May 27-28
Jun 4
2
2
21558 Alisonliu
Hudgens, 38
Jun 20
2
22321 1991 RP
Hudgens, 38
Aug 30
2
7389 Michelcombes
Faure, 20
Harvey, 73
Nov 19
Oct 30
2
3
22412 1995 UQ4
Harvey, 73
Nov 27
3
7467 1989 WQ1
Faure, 20
Nov 19
4
23183 2000 OY21
7496 Miroslavholub
Harvey, 73
Hudgens, 38
Nov 18
Nov 23
3
2
Faure, 20
Harvey, 73
Feb 1
Jan 25
2
6
23187 2000 PN9
7604 Kridsadaporn
Harvey, 73
Dec 18
3
Hudgens, 38
Watson, 20
Mar 7
Mar 8
26361 1999 AJ5
7660 1993 VM1
Harvey, 73
Sep 17
3
Harvey, 73
Hudgens, 38
Oct 30
Oct 28
3
2
7736 Nizhnij Novgorod Hudgens, 38
Oct 21
2
26858 Misterrogers
Harvey, 73
Oct 30
3
7749 Jackschmitt
Faure, 20
Garrett, 32
Harvey, 73
Hudgens, 38
Nov
Nov
Nov
Nov
2
3
3
2
27496 2000 GC125
Hudgens, 38
Nov 23
2
29564 1998 ED6
Harvey, 73
Aug 29
3
30522 2001 MQ15
Harvey, 73
Nov 27
3
7825 1991 TL1
Harvey, 73
Oct 24
3
7843 1994 YE1
Harvey, 73
Nov 19
3
32814 1990 XZ
Harvey, 73
Hudgens, 38
Nov 18
Nov 12
3
2
7895 Kaseda
Hudgens, 38
Jan 31
2
34777 2001 RH
Harvey, 73
Dec 15
3
8145 Valujki
Harvey, 73
Hudgens, 38
Oct 24
Oct 21
3
2
37152 2000 VV56
Hudgens, 38
May 18
2
51149 2000 HF52
8479 1987 HD2
Harvey, 73
May 24
3
Harvey, 73
Hudgens, 38
Nov 18
Nov 12
3
2
8532 1992 YW3
Harvey, 73
Dec 16
3
68950 2002 QF15
Faure, 20
Harvey, 73
May 28
May 22
4
6
8648 Salix
Harvey, 73
Sep 17
3
9452 Rogerpeeters
Harvey, 73
Jan 4
3
85709 1998 SG36
Harvey, 73
Mar 30
6
85804 1998 WQ5
Harvey, 73
Jan 4
6
101496 1998 XM3
Hudgens, 38
Nov 11
2
134340 Pluto
Bookamer, 41
Sep 21-23
3
137032 1998 UO1
Harvey, 73
Oct 2
6
143678 2003 SA224
Harvey, 73
Feb 27
6
144901 2004 WG1
Harvey, 73
Apr 2
6
2001 SG276
Faure, 20
Apr 23
5
2004 FX31
Harvey, 73
Sep 15
6
2004 XL14
Harvey, 73
Dec 19
6
2004 XP14
Harvey, 73
Hudgens, 38
Jul 4
Jul 3
6
3
2005 TF49
Harvey, 73
Apr 12
6
2006 BX39
Harvey, 73
Feb 8
6
2006 BN55
Harvey, 73
Jan 29
6
2006 NM
Faure, 20
Aug 22
5
2006 RZ
Harvey, 73
Oct 3
6
2006 XD2
Harvey, 73
Dec 19
6
27-28
22-23
18
23
10064 1988 UO
Harvey, 73
Oct 30
3
10479 1982 HJ
Hudgens, 38
Jun 20
2
11271 1988 KB
Harvey, 73
May 29
3
11395 1998 XN77
Faure, 20
Jun 30-Jul 1
11405 1999 CV3
Bookamer, 41
Hudgens, 38
Watson, 20
Jul 29
Aug 30
Aug 5
3
2
2
11574 D'Alviella
Hudgens, 38
Aug 25
2
11873 1989 WS2
Harvey, 73
Dec 15
3
12081 1998 FH115
Harvey, 73
Hudgens, 38
Oct 30
Oct 13
3
2
12832 1997 CE1
Harvey, 73
Nov 18
3
13233 1998 FC66
Harvey, 73
Sep 15
3
13255 1998 OH14
Harvey, 73
Dec 15
3
14211 1999 NT1
Harvey, 73
Aug 29
3
14356 1987 SF6
Faure, 20
Aug 31-Sep 1
2
16525 Shumarinaiko
Harvey, 73
Apr 2
3
16720 1995 WT
Harvey, 73
Hudgens, 38
Nov 27
Dec 15
10(5C)
3
2
8
10
92
LIGHTCURVE PHOTOMETRY OPPORTUNITIES
JULY-SEPTEMBER 2007
belt asteroids where the maximum phase angle is about 30°.
However, the extra effort can and will pay off.
Brian D. Warner
17995 Bakers Farm Rd.
Colorado Springs, CO 80908 USA
[email protected]
The fourth list gives a brief ephemeris for planned radar targets.
Supporting optical observations made to determine the
lightcurve’s period, amplitude, and shape are needed to
supplement the radar data. Reducing to standard magnitudes is not
required but high precision work usually is, i.e., on the order of
0.01-0.03mag. A geocentric ephemeris is given for when the
asteroid is brighter than 16.0 (in most cases). The date range may
not always coincide with the dates of planned radar observations,
which – for Arecibo – are limited to a relatively narrow band of
declinations.
Alan W. Harris
Space Science Institute
La Canada, CA 91011-3364 USA
Petr Pravec
Astronomical Institute
CZ-25165 Ondrejov, Czech Republic
Mikko Kaasalainen
Rolf Nevanlinna Institute
FIN-00014 University of Helsinki, Finland
Lance A.M. Benner
Jet Propulsion Laboratory
Pasadena, CA 91109-8099 USA
We present here four lists of “targets of opportunity” for the
period 2007 July – September. The first list is those asteroids
reaching a favorable apparition during this period, are <15m at
brightest, and have either no or poorly constrained lightcurve
parameters. By “favorable” we mean the asteroid is unusually
brighter than at other times. In many cases, a favorable apparition
may not come again for many years. The goal for these asteroids is
to find a well-determined rotation rate, if at all possible. Don’t
hesitate to solicit help from other observers at widely spread
longitudes should the initial finding for the period indicated that it
will be difficult for a single station to find the period.
The Low Phase Angle list includes asteroids that reach very low
phase angles. Getting accurate, calibrated measurements (usually
V band) at or very near the day of opposition can provide
important information for those studying the “opposition effect”,
which is when objects near opposition brighten more than simple
geometry would predict.
The third list is of those asteroids needing only a small number of
lightcurves to allow Kaasalainen and others to complete a shape
model. Some of the asteroids have been on the list for some time,
so work on them is strongly encouraged in order to allow models
to be completed. For these objects, we encourage you to do
absolute photometry, meaning that the observations are not
differential but absolute values put onto a standard system, such as
Johnson V. If this is not possible or practical, accurate relative
photometry is also permissible. This is where all differential
values are against a calibrated zero point that is not necessarily on
a standard system.
When working any asteroid, keep in mind that the best results for
shape and spin axis modeling are obtained when lightcurves are
obtained over a range of phase angles, let alone viewing aspects at
different apparitions. Higher phase angles allow shadowing effects
to influence the lightcurve and help constrain the modeling
solution. If at all possible, try to get lightcurves not only close to
opposition when the asteroid is usually near its brightest, but
before and after, e.g., when the phase angle is 15° or more. This
can be difficult because of the geometry involved, especially main
Those obtaining lightcurves in support of radar observations
should contact Dr. Benner directly at the email given above. There
are two web sites of particular interest for coordinate radar and
optical observations. Future targets (up to 2010) can be found at
http://echo.jpl.nasa.gov/~lance/future.radar.nea.periods.html. Past
radar targets, for comparison to new data, can be found at
http://echo.jpl.nasa.gov/~lance/radar.nea.periods.html.
Once you have data and have analyzed them, it’s important that
you publish your results, if not part of a pro-am collaboration, then
in the Minor Planet Bulletin. It’s also important to make the data
available at least on a personal website or upon request.
Note that the lightcurve amplitude in the tables could be more, or
less, than what’s given. Use the listing as a guide and doublecheck your work.
Funding for Warner and Harris in support of this article is
provided by NASA grant NNG06GI32G and by National Science
Foundation grant AST-0607505.
Lightcurve Opportunities
Brightest
Lightcurve Data
#
Name
Date
V
Dec U
Per.
Amp.
--------------------------------------------------------1880 McCrosky
7 01.0 15.0 -21 0
5527 1991 UQ3
7 01.4 14.6 -22 0
5877 1990 FP
7 01.4 14.6 -26 2 8.91
0.09
1858 Lobachevskij
7 03.5 14.3 -23 2 7.00
0.48
3300 McGlasson
7 06.8 14.0 -52 0
1209 Pumma
7 06.8 14.1 -25 0
1166 Sakuntala
7 07.3 10.4 -21 2 6.30
0.40
7559 1985 VF
7 07.4 14.4 -30 0
6091 Mitsuru
7 08.8 14.4 -39 0
5235 Jean-Loup
7 10.9 14.4 -17 0
2713 Luxembourg
7 13.0 15.0 -24 2 3.579 0.58
2440 Educatio
7 14.7 14.4 -14 0
15407 1997 WM16
7 15.3 15.0 -20 0
3492 Petra-Pepi
7 15.4 14.7 -11 0
15549 2000 FN
7 16.2 14.4 -17 0
4909 Couteau
7 16.5 14.7 -21 0
1925 Franklin-Adams
7 17.0 14.3 -21 0
137 Meliboea
7 17.9 11.4 + 1 2 15.13
0.20
15779 Scottroberts
7 18.3 14.1 -10 0
86324 1999 WA2
7 18.3 14.7 -17 0
1241 Dysona
7 19.4 13.5 -38 2 8.856 0.25
6265 1985 TW3
7 20.3 14.6 -30 0
4066 Haapavesi
7 20.4 14.5 -11 0
6028 1994 ER1
7 21.8 14.6 -21 0
2287 Kalmykia
7 22.6 14.2 -25 0
3403 Tammy
7 23.8 14.7 -11 0
2141 Simferopol
7 24.3 14.3 -15 0
4498 Shinkoyama
7 25.7 14.7 -15 0
7930 1987 VD
7 25.9 14.6 -15 1 long? 0.1
1752 van Herk
7 25.9 14.4 -13 0
3991 Basilevsky
7 26.1 14.5 -17 0
17583 1994 WV2
7 26.7 14.1 -13 0
6831 1991 UM1
7 27.6 14.6 -25 0
226 Weringia
7 28.5 11.9 -14 1
0.1
93
Lightcurve Opportunities (continued)
Low Phase Angle Opportunities
Brightest
Lightcurve Data
#
Name
Date
V
Dec U
Per.
Amp.
--------------------------------------------------------669 Kypria
7 30.9 14.0 - 7 0
7318 Dyukov
8 02.2 14.2 -16 0
357 Ninina
8 03.0 12.9 -15 2 34.97
0.12
1251 Hedera
8 05.4 13.2 -16 2 15.015 0.41
1555 Dejan
8 06.1 13.6 -18 0
1240 Centenaria
8 06.8 12.5 -20 1 14.
0.08
15161 2000 FQ48
8 07.1 14.8 +11 0
294 Felicia
8 07.5 12.2 -16 0
30105 2000 FO3
8 08.4 13.9 -36 0
6420 Riheijyaya
8 08.4 14.7 -10 0
1978 Patrice
8 11.4 13.9 -25 0
4563 Kahnia
8 14.1 14.7 -16 0
5364 1980 RC1
8 17.6 14.7 -10 0
4225 1989 BN
8 19.4 14.7 -19 0
1135 Colchis
8 19.7 12.9 -16 2 23.47
0.45
6649 Yokotatakao
8 20.1 14.1 -12 0
3647 Dermott
8 20.4 14.5 -17 0
1084 Tamariwa
8 20.4 13.5 - 8 2 6.153 0.27
10701 1981 PF
8 20.5 14.6 -12 0
194 Prokne
8 20.7 9.5 - 5 2 15.67
0.27
5945 Roachapproach
8 20.7 14.9 -20 0
3915 Fukushima
8 22.7 15.0 - 2 2 8.40
0.64
46436 2002 LH5
8 23.4 14.7 +15 0
85275 1994 LY
8 25.2 14.0 -29 0
622 Esther
8 25.6 12.0 -14 2 47.5
0.57
911 Agamemnon
8 26.3 14.6 -13 1 7.
0.40
3330 Gantrisch
8 27.2 14.4 -20 0
3069 Heyrovsky
8 29.7 14.7 - 6 0
1118 Hanskya
8 30.8 13.7 - 3 2 15.61
0.18
3163 Randi
9 04.0 13.9 - 3 0
2637 Bobrovnikoff
9 04.2 13.8 -10 0
2623 Zech
9 04.5 13.8 - 8 0
4140 Branham
9 05.1 14.4 -14 0
1608 Munoz
9 05.1 14.1 - 9 0
2250 Stalingrad
9 06.7 14.6 - 7 0
501 Urhixidur
9 07.8 12.5 -14 1 15.0
0.1
575 Renate
9 08.7 13.2 - 8 2 3.678 0.20
2633 Bishop
9 08.7 14.6 -11 0
10597 1996 TR10
9 08.9 14.6 - 8 0
1325 Inanda
9 11.4 12.9 -11 1 8.
0.04
2896 Preiss
9 11.4 14.0 - 4 0
8722 Schirra
9 11.8 14.6 + 1 0
6176 Horrigan
9 14.2 14.7 -13 0
828 Lindemannia
9 14.4 14.4 - 4 ?
4583 Lugo
9 15.0 14.7 - 4 0
1607 Mavis
9 15.9 12.9 -16 0
3687 Dzus
9 16.4 14.3 +18 1 7.44
0.1
1418 Fayeta
9 17.4 13.0 - 3 0
570 Kythera
9 19.4 12.8 + 0 2 8.120 0.18
1565 Lemaitre
9 20.8 14.0 +38 0
5746 1991 CK
9 21.9 13.9 + 0 0
2687 Tortali
9 22.9 14.7 -12 2 21.75
0.19
10562 1993 UB1
9 23.0 14.4 - 9 0
1070 Tunica
9 23.0 14.7 - 6 0
1099 Figneria
9 23.1 13.2 - 8 0
1432 Ethiopia
9 23.4 13.3 -13 0
1002 Olbersia
9 23.5 13.9 + 5 0
464 Megaira
9 23.5 12.3 -16 2 12.91
0.08
13474 V'yus
9 23.6 15.0 +11 0
4070 Rozov
9 23.8 14.7 + 7 0
2123 Vltava
9 24.6 14.7 + 2 0
844 Leontina
9 24.9 13.4 + 3 0
20936 4835 T-1
9 25.8 14.7 -20 0
3509 Sanshui
9 26.2 14.7 +14 0
650 Amalasuntha
9 26.4 14.7 + 4 0
2010 Chebyshev
9 27.0 14.7 + 1 0
1501 Baade
9 28.5 13.7 - 1 2 15.132 0.40
4614 Masamura
9 29.7 14.4 + 1 0
#
Name
Date
α
V
Dec
--------------- ------------------------------------556 Phyllis
07 03.1
0.30 13.0
-24
1166 Sakuntala
07 07.3
0.79 10.5
-21
64 Angelina
07 07.9
0.28 11.6
-23
868 Lova
07 09.6
0.52 13.9
-21
52 Europa
07 14.0
0.97 11.0
-19
644 Cosima
07 30.0
0.21 13.9
-19
1251 Hedera
08 05.3
0.65 13.2
-16
1555 Dejan
08 05.9
0.50 13.7
-18
294 Felicia
08 07.5
0.22 12.2
-16
27 Euterpe
08 11.4
0.71 10.2
-17
73 Klytia
08 17.0
1.00 12.4
-16
1069 Planckia
08 17.0
0.13 13.9
-14
334 Chicago
08 25.7
0.62 12.9
-13
277 Elvira
08 29.0
0.69 13.2
-08
114 Kassandra
09 03.4
0.21 12.3
-07
30 Urania
09 03.8
1.00
9.7
-06
2623 Zech
09 04.4
0.74 13.9
-08
575 Renate
09 08.8
0.95 13.3
-08
35 Leukothea
09 15.5
0.15 13.2
-03
1418 Fayeta
09 17.5
0.29 13.1
-03
1074 Beljawskya
09 18.5
0.32 13.7
-03
570 Kythera
09 19.4
0.66 12.9
+00
209 Dido
09 19.8
0.26 12.5
-02
5746 1991 CK
09 21.9
0.21 14.0
+00
431 Nephele
09 23.8
0.99 12.1
-02
844 Leontina
09 25.0
0.98 13.4
+03
312 Pierretta
09 28.3
0.22 12.4
+01
Shape/Spin Modeling Opportunities
Brightest
Per
# Name
Date
V
Dec
(h)
Amp.
U
--------------------------------------------------------377 Campania
7 17.1 12.6 -11
8.507
0.16 3
59 Elpis
7 24.7 11.4 -10 13.69
0.1
3
40 Harmonia
8 03.0
9.3 -22
8.910 0.15-0.36 4
334 Chicago
8 25.7 12.9 -13
7.35
0.15-0.67 2
487 Venetia
8 26.4 11.4 -20 13.28
0.05-0.30 2
114 Kassandra
9 03.4 12.2 -07 10.758
0.25 3
Radar-Optical Opportunities
4954 Eric
An extended campaign for this asteroid is planned for Arecibo in
October and November. However, lightcurves prior to this time
can help establish the spin axis solution.
It will be brighter than 15th magnitude from about mid-July 2007
until mid-March 2008, when it will traverse about 120 degrees
across the sky. It will be between 100-160 degrees from the Sun
throughout, so it should be a tractable target for months.
The period is well-known, 12.057 hr, so it makes better sense to
observe it one to three nights every few weeks in order to get both
the entire curve – if possible – and any changes in the curve as it
moves through a very large range of PAB values.
Date
Geocentric
Mag
2007/08 RA(2000) DC(2000)
V
α
E
LPAB BPAB
--------------------------------------------------------07/01
23 22.45 -28 50.3 15.34 30.5 117 323.7 -18.7
07/31
23 46.61 -28 29.9 14.07 26.0 136 332.9 -18.0
08/30
23 28.22 -26 36.3 12.41 15.3 158 339.7 -13.8
09/29
22 15.63 -11 53.0 11.67 26.3 146 344.7 -0.6
10/29
21 29.73 +15 59.0 12.26 53.6 112 358.6 20.1
11/28
21 50.28 +39 53.8 12.82 61.9
99
27.7 35.6
12/28
23 33.38 +58 03.8 13.12 55.6 103
62.6 38.5
01/27
3 19.16 +61 46.4 13.57 45.2 112
90.6 30.8
02/26
6 01.90 +49 07.8 14.42 39.2 111 111.0 20.6
03/27
7 29.22 +36 20.9 15.41 36.6 101 127.1 12.7
04/16
8 13.08 +29 32.4 16.00 34.7
93 136.5
8.8
94
2007 DT103
This asteroid will make a quick fly-by in late July and early
August. An ephemeris is given below but it should be considered
only approximate. Note that the positions are geocentric and that
parallax shift will be several arcminutes. An updated ephemeris
can be obtained from the Minor Planet Center website:
http://www.cfa.harvard.edu/iau/MPEph/MPEph.html
Date
Geocentric
2007
RA(2000)
DC(2000) E.D.
V
α
E
---------------------------------------------------07/29
3 03.13
+71 06.3 0.024 15.50 109.2
70
07/30
1 34.80
+58 54.9 0.023 14.86
97.1
82
07/31
0 56.67
+45 42.6 0.025 14.50
85.2
93
08/01
0 36.53
+34 08.3 0.028 14.36
74.8 104
08/02
0 24.23
+24 52.4 0.031 14.38
66.5 112
08/03
0 15.94
+17 41.8 0.036 14.48
59.9 118
08/04
0 09.95
+12 08.9 0.041 14.62
54.7 123
08/05
0 05.39
+ 7 48.5 0.046 14.77
50.5 127
08/06
0 01.77
+ 4 21.5 0.051 14.93
47.1 131
08/07 23 58.80
+ 1 34.0 0.057 15.08
44.1 134
08/08 23 56.30
- 0 43.7 0.063 15.23
41.5 136
08/09 23 54.13
- 2 38.8 0.068 15.37
39.2 138
08/10 23 52.22
- 4 16.2 0.074 15.51
37.2 140
THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly
journal of the Minor Planets Section of the Association of Lunar and
Planetary Observers – ALPO. Beginning with volume 32, the current and
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Jul-Sep, 34-3 - MinorPlanet.Info

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