Index to observations received from ARPS
members
Observations received FROM ARPS MEMBERS
January 2010
December 2009
December provided a reasonable
amount of observing time but the number of NEOs discovered by the surveys was
much reduced, 34 new objects compared to the 116 they picked up in November, so
NEO follow-up work was quieter than of late. As well as following objects on
the NEO Confirmation page, the opportunity was taken to follow 2009 WZ104 on
several nights to try and determine its light curve. This is an Aten discovered
on Nov. 25 by the Catalina Sky Survey and was brighter than 17th mag. for the
first two weeks in December. However, not enough coverage was obtained to be
able to find an unambiguous period, but it is likely to be longer than 6-8
hours.
The unusual artificial
satellite 9U01FF6 mentioned last month in TA Vol 46 No 548 p211 (2009) which is
in a 30+ day, very elongated orbit, taking it as close to us as 5 Earth
diameters and about twice as far as the Moon at apogee, was picked up again on Dec.
27, three days before perigee. It was only 5" from the prediction
calculated with FindOrb using positions from the previous two returns and
taking into account Solar Radiation Pressure. Unfortunately the weather stopped
any further observations but it should be visible next on the night of
2009 overall was an
exceptionally good year for observing at Great Shefford, producing the best
observing figures since my observatory was commissioned in May 2002. Several
statistics follow, with the previous best figures and year in parentheses: The
most nights used (202 vs. 183 in 2003), the most hours spent at the telescope
(938h vs. 838h in 2005), the largest amount of time the CCD shutter was open
(24d 00h vs. 22d 03h in 2007) and far and away the largest number of images
taken in a year (148,361 vs. 92,025 in 2007). That last statistic is in part to
do with more Minor Planet photometry being done in 2009 than before, with many
objects being followed for long periods of time, collecting many images during
a night. The total number of images taken since 2002 passed the 1/2 million
mark during the year and now stands at 570,575.
2009 generally seems to have
beaten my previous records by 8-12% all round. Lets hope 2010 doesn't let us
down!
13089
KC2009 12 25.90247 05 00 05.09 +24 58 41.5 J95 = MBA
13089
KC2009 12 25.91824 05 00 04.30 +24 58 37.8 J95
13089
KC2009 12 25.92431 05 00 04.01 +24 58 36.3 17.4 R J95
35015 C2009 12 10.84439 04 55 59.06 +20 47
28.7 J95 = MBA
35015
C2009 12 10.85017 04 55 58.72 +20 47 26.7 J95
35015
C2009 12 10.85593 04 55 58.35 +20 47 24.4 17.8 R J95
85834 C2009 12 10.84439 04 55 57.32 +20 55
07.2 J95 = MBA
85834
C2009 12 10.85017 04 55 56.93 +20 55 07.2 J95
85834
C2009 12 10.85593 04 55 56.54 +20 55 07.1 17.7 R J95
97527
KC2009 12 20.95114 05 21 14.83 +25 37 26.7 J95 = MBA
97527
KC2009 12 20.97756 05 21 13.36 +25 37 23.8 19.4 R J95
A4178
KC2009 12 20.83796 02 25 29.83 +13 33 08.9 J95 = MBA
A4178
KC2009 12 20.91889 02 25 29.39 +13 33 30.5 19.3 R J95
F5012
KC2009 12 20.83796 02 25 40.88 +13 28 07.6 J95 = MBA
F5012
KC2009 12 20.91889 02 25 41.92 +13 28 13.2 19.6 R J95
I9595 KC2009 12 25.90247 04 59 53.31 +25 01
10.9 18.5 R J95 = MBA
I9595 IC2009 12 25.91824 04 59 52.43 +25 01
08.8 J95
I9595 IC2009 12 25.92431 04 59 52.13 +25 01
07.2 J95
M2573 KC2009 12 20.83796 02 24 53.27 +13 27
15.5 J95 = MBA
M2573
KC2009 12 20.91889 02 24 52.32 +13 27 25.1 19.5 R J95
M5403
C2009 12 10.84728 04 56 27.29 +20 55 51.1 J95 = MBA
M5403
C2009 12 10.85880 04 56 26.62 +20 55 51.6 J95
M5403
C2009 12 10.87064 04 56 25.96 +20 55 49.8 19.4 R J95
K01TC7L C2009 12 10.84728 04 56
31.22 +20 51 55.0
J95 = MBA
K01TC7L C2009 12 10.85880 04 56 30.48 +20 51
51.7 J95
K01TC7L C2009 12 10.87572 04 56
29.41 +20 51 46.4 19.8 R J95
K03T03Q KC2009 12 27.96857 06 56 59.72 +36 14 38.8 J95 = MBA
K03T03Q KC2009 12 27.97433 06 56 59.35 +36
14 38.6 J95
K03T03Q KC2009 12 27.98011 06 56 58.95 +36
14 38.0 J95
K03T03Q KC2009 12 27.98587 06 56 58.55 +36
14 37.6 J95
K03T03Q KC2009 12 28.00227 06 56 57.52 +36
14 37.0 19.0 R J95
K03UD5C KC2009 12 20.95114 05 20 49.41 +25
24 23.9 J95 = MBA
K03UD5C KC2009 12 20.96606 05 20 48.61 +25
24 22.7 20.1 R J95
K03UD5C KC2009 12 21.02986 05 20 45.03 +25
24 18.8 19.9 R J95
K09V70Z KC2009 12 20.95114 05 21 22.61 +25
28 04.9 J95 = MBA
K09V70Z KC2009 12 20.97756 05 21 20.88 +25
28 06.5 20.1 R J95
K09V70Z KC2009 12 21.02986 05 21 17.46 +25
28 10.0 20.6 R J95
K09V70Z KC2009 12 22.90947 05 19 17.91 +25
30 13.2 20.6 R J95
K09V70Z HC2009 12 22.94440 05 19 15.68 +25
30 16.3 J95
K09V70Z KC2009 12 23.98771 05 18 10.03 +25
31 20.5 20.5 R J95
K09V70Z KC2009 12 24.00982 05 18 08.68 +25
31 22.3 J95
K09V70Z KC2009 12 24.01285 05 18 08.48 +25
31 22.2 J95
K09W01L KC2009 12 27.95454 05 18 45.41 +65
31 00.4 J95 = Amor
K09W01L KC2009 12 27.95839 05 18 44.59 +65
31 04.2 J95
K09W01L KC2009 12 27.96223 05 18 43.73 +65
31 08.1 19.0 R J95
K09W11D C2009
12 04.01664 04 44 31.87 +33 38 20.6 J95 = Apollo
K09W11D C2009 12 04.02050 04 44
30.10 +33 38 40.4
J95
K09W11D C2009 12 04.02437 04 44
28.34 +33 39 00.6 18.2 R J95
K09W25V C2009 12 01.01337522 47 37.19 +60 31
31.1 J95 = Apollo
K09W25V C2009 12 01.01691022 46
29.18 +60 31 52.5
J95
K09W25V C2009 12 01.01931622 45
42.88 +60 32 05.9 14.6 R J95
K09W52A
EC2009 12 01.05017 05 33 27.09 +27 44 24.7 J95 = Apollo
K09W52A C2009 12 01.05308 05 33
32.34 +27 44 20.3 19.2 R J95
K09WA4Z C2009 12 03.79271 22 28
41.83 +48 58 54.1
J95 = Aten
K09WA4Z C2009 12 03.80601 22 28 58.33 +48 56
43.9 J95
K09WA4Z C2009 12 03.81797 22 29
13.18 +48 54 46.0 15.5 R J95
K09WA4Z C2009 12 06.75992 23 24
37.38 +40 07 43.5 16.0 R J95
K09WA4Z C2009 12 06.80573 23 25
18.53 +39 58 56.4 16.0 R J95
K09WA4Z C2009 12 06.84885 23 25
57.25 +39 50 34.7 15.9 R J95
K09WA4Z C2009 12 10.79603 00 16
36.50 +27 25 45.9
J95
K09WA4Z C2009 12 10.89301 00 17
31.66 +27 08 21.7
J95
K09WA4Z C2009 12 10.93725 00 17
57.09 +27 00 22.2 16.9 R J95
K09X00D C2009 12 07.87129 04 40
48.82 +25 05 22.1
J95 = Apollo
K09X00D C2009 12 07.87554 04 40
48.04 +25 05 02.8
J95
K09X00D C2009 12 07.87981 04 40
47.26 +25 04 43.5 17.0 R J95
K09X00D C2009 12 10.97269 04 31
09.43 +20 47 38.3
J95
K09X00D C2009 12 10.98038 04 31 07.88 +20 46 56.7 J95
K09X00D C2009 12 10.98806 04 31
06.33 +20 46 15.0 17.0 R J95
K09X00O
C2009 12 10.95275 07 38 34.91 +22 53 40.6 J95 = Apollo
K09X00O
C2009 12 10.95853 07 38 35.98 +22 53 39.0 J95
K09X00O
C2009 12 10.96429 07 38 37.04 +22 53 38.8 18.6 R J95
K09X00O KC2009 12 25.93684 08 56 13.94 +20
01 39.8 J95
K09X00O KC2009 12 25.94184 08 56 16.48 +20
01 32.8 J95
K09X00O KC2009 12 25.94691 08 56 19.05 +20
01 24.9 18.0 R J95
K09X00V
C2009 12 10.90816 07 43 50.13 +35 18 33.2 18.5 R J95 = BR59279 = Apollo
K09X00V
C2009 12 10.94246 07 43 37.70 +35 18 36.9 J95
K09X00V C2009
12 10.94607 07 43 36.41 +35 18 36.6
18.6 R J95
K09X00V
KC2009 12 26.87743 06 44 43.77 +33 59 36.2 J95
K09X00V
KC2009 12 26.88204 06 44 43.10 +33 59 34.9 J95
K09X00V
KC2009 12 26.88661 06 44 42.46 +33 59 32.7 19.1 R J95
K09X00X
KC2009 12 17.79930 03 52 41.09 +30 07 22.4 J95 = MBA
K09X00X
KC2009 12 17.81092 03 52 40.52 +30 07 17.8 20.1 R J95
K09X01Q C2009 12 10.84728 04 56
37.10 +20 54 24.8 19.6 R J95 = 9XBC944 = Apollo
K09X01Q C2009 12 10.85880 04 56
34.34 +20 53 44.0 20.1 R J95
K09X01Q
C2009 12 10.87572 04 56 30.34 +20 52 45.3 20.5 R J95
K09X02F C2009
12 12.90492 05 01 52.41 +15 01 03.5 J95 = BR67918 = Apollo
K09X02F C2009 12 12.90779 05 01
51.90 +15 01 07.6
J95
K09X02F C2009 12 12.91065 05 01
51.39 +15 01 10.5
J95
K09X02F C2009 12 12.91476 05 01
50.69 +15 01 16.2 18.7 R J95
K09X02F
KC2009 12 25.95954 04 25 16.80 +20 02 46.9 J95
K09X02F KC2009
12 25.98019 04 25 13.34 +20 03 16.5 J95
K09X02F
KC2009 12 25.98816 04 25 11.98 +20 03 27.7 19.2 R J95
K09X02P
KC2009 12 13.76632 02 46 24.48 +22 45 56.2 J95 = Apollo
K09X02P
KC2009 12 13.76819 02 46 25.43 +22 46 49.1 J95
K09X02P
KC2009 12 13.76997 02 46 26.35 +22 47 39.3 17.8 R J95
K09X06T KC2009 12 26.00089 07 33 45.53 +15 45 02.7 J95 = Apollo
K09X06T KC2009 12 26.00569 07 33 43.63 +15
45 05.3 J95
K09X06T KC2009 12 26.01063 07 33 41.69 +15
45 07.5 18.1 R J95
K09X06Z KC2009 12 17.82179 05 47 22.75 +27
34 35.3 J95 = Apollo
K09X06Z KC2009 12 17.82679 05 47 25.75 +27
36 20.1 J95
K09X06Z KC2009 12 17.83211 05 47 28.93 +27 38
11.0 18.5 R J95
K09X06Z
KC2009 12 26.81824 06 52 30.90 +50 39 21.1 J95
K09X06Z
KC2009 12 26.82858 06 52 33.39 +50 40 04.1 J95
K09X06Z
KC2009 12 26.83884 06 52 35.82 +50 40 46.4 19.9 R J95
K09X08F C2009 12 12.95237 04 39
53.92 +20 53 01.6
J95 = 9XBF423 = MBA
K09X08F C2009 12 12.95600 04 39
53.25 +20 53 08.3
J95
K09X08F C2009 12 12.96027 04 39
52.36 +20 53 18.0 20.4 R J95
K09Y00F
KC2009 12 17.90180 05 51 34.56 +22 41 34.9 J95 = BR88827 = Aten
K09Y00F KC2009 12 17.90476 05 51 33.22 +22
41 39.6 J95
K09Y00F KC2009 12 17.90982 05 51 30.93 +22
41 47.6 18.8 R J95
K09Y00F KC2009 12 25.90247 05 00 06.74 +24 57
40.0 J95
K09Y00F
KC2009 12 25.91824 05 00 00.83 +24 57 50.6 19.5 R J95
K09Y00G KC2009 12 19.12565 11 17 38.51 +00
23 41.6 J95 = Apollo
K09Y00G KC2009 12 19.12946 11 17 40.06 +00
23 32.0 J95
K09Y00G KC2009 12 19.13312 11
17 41.55 +00 23 22.5 18.9 R J95
K09Y00S
KC2009 12 19.91111 09 14 13.24 +63 09 57.3 18.3 R J95 = Apollo
K09Y00S
IC2009 12 19.91492 09 14 15.15 +63 10 16.6 J95
K09Y00S
KC2009 12 19.91951 09 14 17.43 +63 10 38.9 18.5 R J95
K09Y00R KC2009 12 19.90207 04 34 58.54 +22 01 06.9 J95 = 9Y8B0A0 = Aten
K09Y00R KC2009 12 19.90449 04 34 54.75 +22
01 09.3 J95
K09Y00R
KC2009 12 19.90718 04 34 50.67 +22 01 10.2 19.5 R J95
K09Y00R KC2009 12 22.86352 03 12 36.42 +21
08 12.5 J95
K09Y00R KC2009 12 22.87565 03 12 10.26 +21
07 37.9 J95
K09Y00R KC2009 12 22.88105 03 11 58.53 +21
07 20.7 19.7 R J95
K09Y00R KC2009 12 25.76576 01 32 47.91 +16
41 12.7 19.9 R J95
K09Y00R KC2009 12 25.78176 01 32 11.43 +16
39 11.5 20.2 R J95
K09Y00R FC2009 12 25.81832 01 30 48.04 +16
34 30.9 20.1 R J95
K09Y06U KC2009 12 21.00230 09 14 41.47 +22
57 19.5 J95 =
9Y8CBFF = Apollo
K09Y06U KC2009 12 21.01123 09 14 40.39 +22
57 41.9 20.5 R J95
K09Y06V IC2009 12 20.95114 05 21 01.95 +25
31 44.3 J95 =
9Y8CF0B = Amor
K09Y06V KC2009 12 20.97449 05 20 58.72 +25
31 18.0 21.1 R J95
K09Y18P IC2009 12 26.84765 05 58 56.96 +11
58 04.8 J95 =
K09Y18P KC2009 12 26.85236 05 58 56.62 +11
58 01.5 19.3 R J95
K09Y18P KC2009 12 26.85935 05 58 56.12 +11
57 54.0 J95
GS9
GS9
GS9
GS9
Hi
Merry Christmas to all.
It is cold outside.
Regards John.
Eros No.433 (unusual listing)
Near Earth Asteroids.
No. 159402 / No. 2002 WP / No.
2006 UR
OBS
TEL 0.25-m f/5.5 Schmidt-Cassegrain + CCD
AC2 jfmto@blueyonder.co.uk
K02W00P C2009 12 20.85001 02 33 02.22 +25 48
07.5 16.4 V J93
K02W00P C2009 12 20.85102 02 33 02.17 +25 48
13.0 16.3 V J93
K02W00P C2009 12 20.85306 02 33 02.02 +25 48
23.9 16.4 V J93
K06U00R C2009 12 20.88003 07 45 09.22 +14 55
52.5 16.0 V J93
K06U00R C2009 12 20.88498 07 45 10.24 +14 55
36.8 16.1 V J93
K06U00R C2009 12 20.88993 07 45 11.27 +14 55
21.6 16.1 V J93
00433 C2009 12
20.81537 22 56 30.47 +07 11 12.3
13.0 V J93
00433 C2009 12
20.81769 22 56 30.79 +07 11 14.0
12.9 V J93
00433 C2009 12 20.82000
22 56 31.07 +07 11 15.1 12.9
V J93
F9402 C2009 12
20.83869 09 30 06.49 +53 26 56.1
15.1 V J93
F9402 C2009 12
20.84031 09 30 06.29 +53 26 54.0
15.2 V J93
F9402 C2009 12
20.84192 09 30 06.07 +53 26 52.6
15.1 V J93
----- end -----
Minus 5°C at 22.00hrs.
Telescope tube iced up but customized dew heater doing its job. The Dome was
frozen up when opening up as daytime temperatures never went above minus 2°C all day long.
Severe frost like needles sticking up on everything.
Best wishes john.
Eros. No 433 (unusual
listing)
NEO’s
159402
2007 MK13
2005 MC
OBS
TEL 0.25-m f/5.5 Schmidt-Cassegrain + CCD
AC2 jfmto@blueyonder.co.uk
K05M00C C2010 01 04.89021 08 54 40.34 +08 28
51.7 16.0 V J93
K05M00C C2010 01 04.89364 08 54 39.64 +08 28
39.2 16.1 V J93
K05M00C C2010 01 04.89719 08 54 38.88 +08 28
26.6 16.1 V J93
00433 C2010 01 04.79836 23 31 23.07 +09 38 28.5 12.9 V J93
00433 C2010 01
04.80068 23 31 23.40 +09 38 29.6
13.0 V J93
00433 C2010 01
04.80302 23 31 23.74 +09 38 30.9
13.0 V J93
F9402 C2010 01 04.81856
08 48 57.16 +48 12 54.4 15.5
V J93
F9402 C2010 01
04.82369 08 48 56.45 +48 12 48.1
15.5 V J93
F9402 C2010 01
04.82541 08 48 56.17 +48 12 46.2
15.5 V J93
K07M13K C2010 01 04.83543 07 58 14.15 +63 02
27.6 15.7 V J93
K07M13K C2010 01 04.84036 07 58 12.01 +63 03
07.5 15.7 V J93
K07M13K C2010 01 04.84281 07 58 10.89 +63 03
27.4 15.4 V J93
----- end -----
OBS R. Miles
TEL 2.0-m f/10.0 Ritchey-Chretien + CCD
AC2
K10A30L C2010 01 12.48271 07 32
55.47 +09 54 40.2 16.2 R
F65
K10A30L C2010 01 12.48321 07 32
54.21 +09 54 42.8 16.1 R
F65
K10A30L C2010 01 12.48379 07 32
52.75 +09 54 45.8 16.3 R
F65
K10A30L C2010 01 12.48433 07 32
51.36 +09 54 48.7 16.3 R
F65
K10A30L C2010 01 12.48486 07 32
50.03 +09 54 51.4 16.3 R
F65
K10A30L C2010 01 12.48538 07 32
48.71 +09 54 54.2 16.3 R
F65
K10A30L C2010 01 12.48597 07 32
47.22 +09 54 57.2 16.1 R
F65
K10A30L C2010 01 12.48657 07 32
45.72 +09 55 00.3 16.2 R
F65
K10A30L C2010 01 12.48712 07 32
44.32 +09 55 03.1 16.2 R
F65
K10A30L C2010 01 12.48766 07 32
42.95 +09 55 05.9 16.2 R
F65
K10A30L C2010 01 12.48820 07 32
41.58 +09 55 08.8 16.3 R
F65
K10A30L C2010 01 12.48927 07 32
38.86 +09 55 14.3 16.1 R
F65
K10A30L C2010 01 12.48982 07 32
37.42 +09 55 17.2 16.3 R
F65
K10A30L C2010 01 12.49036 07 32
36.08 +09 55 19.9 16.3 R
F65
K10A30L C2010 01 12.49091 07 32
34.67 +09 55 22.8 16.3 R
F65
K10A30L C2010 01 12.49147 07 32
33.27 +09 55 25.6 16.3 R
F65
K10A30L C2010 01 12.49202 07 32
31.84 +09 55 28.5 16.1 R
F65
K10A30L C2010 01 12.49258 07 32
30.42 +09 55 31.4 16.2 R
F65
K10A30L C2010 01 12.49311 07 32
29.08 +09 55 34.1 16.2 R
F65
K10A30L C2010 01 12.49365 07 32
27.67 +09 55 37.0 16.2 R
F65
K10A30L C2010 01 12.49475 07 32
24.87 +09 55 42.6 16.2 R
F65
K10A30L C2010 01 12.49529 07 32
23.47 +09 55 45.5 16.1 R
F65
K10A30L C2010 01 12.49582 07 32
22.10 +09 55 48.4 16.2 R
F65
K10A30L C2010 01 12.49640 07 32
20.62 +09 55 51.3 16.3 R
F65
K10A30L C2010 01 12.49747 07 32
17.88 +09 55 56.7 16.3 R
F65
K10A30L C2010 01 12.49801 07 32
16.47 +09 55 59.6 16.1 R
F65
K10A30L C2010 01 12.49855 07 32 15.07
+09 56 02.4 16.0 R
F65
----- end -----
OBS D. Sergison
TEL 2.0-m f/10.0 Ritchey-Chretien + CCD
AC2
K10A30L C2010 01 12.52573 07 31
03.84 +09 58 23.2 16.1 R
F65
K10A30L C2010 01 12.52641 07 31
02.03 +09 58 26.8 16.2 R
F65
K10A30L C2010 01 12.52703 07 31
00.37 +09 58 30.0 16.2 R
F65
K10A30L C2010 01 12.52763 07 30
58.77 +09 58 33.0 16.2 R
F65
K10A30L C2010 01 12.52835 07 30
56.84 +09 58 36.8 16.1 R
F65
K10A30L C2010 01 12.52894 07 30
55.26 +09 58 39.9 16.1 R
F65
K10A30L C2010 01 12.52953 07 30
53.70 +09 58 42.9 16.2 R
F65
K10A30L C2010 01 12.53019 07 30
51.92 +09 58 46.3 16.2 R
F65
K10A30L C2010 01 12.53076 07 30
50.39 +09 58 49.3 16.2 R
F65
K10A30L C2010 01 12.53252 07 30
45.68 +09 58 58.4 16.0 R
F65
K10A30L C2010 01 12.53331 07 30 43.55
+09 59 02.5 16.1 R
F65
K10A30L C2010 01 12.53389 07 30
42.02 +09 59 05.5 16.0 R
F65
K10A30L C2010 01 12.53451 07 30
40.33 +09 59 08.7 15.9 R
F65
K10A30L C2010 01 12.53506 07 30
38.84 +09 59 11.6 15.9 R
F65
K10A30L C2010 01 12.53563 07 30
37.32 +09 59 14.5 16.0 R
F65
K10A30L C2010 01 12.53622 07 30
35.73 +09 59 17.5 16.0 R
F65
K10A30L C2010 01 12.53679 07 30
34.21 +09 59 20.4 16.0 R
F65
K10A30L C2010 01 12.53820 07 30 30.40 +09 59
27.8 16.1 R
F65
K10A30L C2010 01 12.53877 07 30
28.85 +09 59 30.7 16.1 R
F65
K10A30L C2010 01 12.53937 07 30
27.25 +09 59 33.7 16.1 R
F65
K10A30L C2010 01 12.53990 07 30
25.80 +09 59 36.6 16.0 R
F65
----- end -----
OBS R. Miles
TEL 2.0-m f/10.0 Ritchey-Chretien + CCD
AC2
K10A30L
C2010 01 12.57066 07 30 28.13 +10 26 26.0 16.0 R
E10
K10A30L
C2010 01 12.57219 07 30 23.75 +10 26 38.3 16.3 R
E10
K10A30L
C2010 01 12.57294 07 30 21.58 +10 26 44.4 16.2 R
E10
K10A30L
C2010 01 12.57368 07 30 19.45 +10 26 50.5 16.0 R
E10
K10A30L
C2010 01 12.57440 07 30 17.39 +10 26 56.3 16.1 R
E10
K10A30L
C2010 01 12.57753 07 30 08.32 +10 27 22.2 16.2 R
E10
K10A30L
C2010 01 12.57969 07 30 02.01 +10 27 39.8 16.1 R
E10
----- end -----
OBS R. Miles
TEL 2.0-m f/10.0 Ritchey-Chretien + CCD
AC2
K10A61N C2010 01 18.40561 08 57
42.55 +21 08 09.1 19.8 V
F65
K10A61N C2010 01 18.40623 08 57
42.95 +21 08 15.3 19.7 V
F65
K10A61N C2010 01 18.40687 08 57
43.38 +21 08 21.2 19.8 V
F65
K10A60O
C2010 01 15.64201 10 44 18.35 +34 37 50.0 18.3 V
F65
K10A60O
C2010 01 15.64267 10 44 17.89 +34 37 48.3 18.5 V
F65
K10A60O
C2010 01 15.64331 10 44 17.41 +34 37 46.8 18.4 V
F65
K10A60O
C2010 01 15.64413 10 44 16.79 +34 37 44.8 18.3 V
F65
----- end -----
OBS R. Miles
TEL 2.0-m f/10.0 Ritchey-Chretien + CCD
AC2
K10A15A C2010 01 19.39898 06 55
25.68 +27 52 29.0 20.9 R
F65
K10A15A C2010 01 19.40229 06 55
25.47 +27 52 28.5 20.8 R
F65
K10A15A C2010 01 19.40508 06 55
25.29 +27 52 28.0 20.7 R
F65
K10A15A C2010 01 19.40804 06 55
25.10 +27 52 27.6 21.2 R
F65
K10A15A C2010 01 19.46134 06 55
21.69 +27 52 18.8 21.1 R
F65
K10A15A C2010 01 19.46413 06 55 21.52 +27 52
18.4 21.6 R
F65
K10A15A C2010 01 19.46683 06 55
21.35 +27 52 17.9 21.2 R
F65
K10A15A C2010 01 19.46991 06 55
21.15 +27 52 17.4 21.1 R
F65
K10A15A C2010 01 19.47300 06 55
20.96 +27 52 16.9 21.1 R
F65
K10A15A C2010 01 19.51614 06 55
18.23 +27 52 09.7 21.0 R
F65
K10A15A C2010 01 19.51822 06 55
18.10 +27 52 09.0 21.1 R
F65
----- end -----
OBS R. Miles
TEL 2.0-m f/10.0 Ritchey-Chretien + CCD
AC2
K10B02K C2010 01 22.43957 03 54
12.67 -17 05 45.2 17.7 R
E10
K10B02K
C2010 01 22.44228 03 54 15.79 -17 05 14.4 17.5 R
E10
K10B02K
C2010 01 22.44398 03 54 17.72 -17 04 55.3 17.9 R
E10
K10B02K
C2010 01 22.44559 03 54 19.59 -17 04 36.9 17.8 R
E10
K10B02K
C2010 01 22.44720 03 54 21.40 -17 04 19.0 18.1 R
E10
K10B02K C2010 01 22.44879 03 54
23.18 -17 04 01.1 18.2 R
E10
K10B02K
C2010 01 22.45384 03 54 28.93 -17 03 03.9 17.8 R
E10
K10B02K
C2010 01 22.45545 03 54 30.79 -17 02 46.1 18.1 R
E10
-----
end -----
COM Stack of 4 images, total integration time = 320
s
OBS A. Debackère
TEL 2.0-m f/10.0 Ritchey-Chretien + CCD
AC2
K10A15A C2010 01 22.46034 06 52 28.77
+27 44 00.5 21.2 V
F65
K10A15A C2010 01 22.46234 06 52
28.64 +27 44 00.2 22.0 V
F65
K10A15A C2010 01 22.46438 06 52
28.52 +27 43 59.7 21.5 V
F65
K10A15A C2010 01 22.46649 06 52
28.41 +27 43 59.3 21.4 V
F65
F65
----- end -----
Images
Colleagues,
Here attached are two stacked images of these
enigmatic objects made 1.5
hours apart in sub-arcsecond seeing using
Faulkes. There appears to be some
evolution in the head of the comet during this time
interval. Note that the
head of the coma appears rather rectilinear or
flattened in shape. The coma
also appears to have moved slightly further away
from the asteroid in the
later image.
A shorter-exposure, stacked image taken more than 1 hour later
still, seemed to show further changes in the form of
the coma.
The asteroid, 2010 AA15 is about V=21.5 and appears
to have a slow rotation
rate, probably in excess of 12 hours. There is no evidence of remanant
cometary activity.
Note that it has a very similar orbit to the comet
according to the MPC and so the two are clearly
physically associated.
There is no evidence of fragments at the head of the
coma although the
rectilinear feature may be caused by metre-size
fragments aligned in some
way and slowly breaking up.
Occultations
ASTEROIDAL OCCULTATION - REPORT
====================================
EAON
- EUROPEAN ASTEROIDAL OCCULTATION NETWORK
1.
DATE: 2010 Jan 05
2.
OBSERVER Name:
Address:
White Lodge, Bank Lane, Warton,
Tel:
+44 (0)1772 632450 Email: ae@f2s.com
3.
OBSERVING STATION - Warton Bank Observatory North - fixed single station
Nearest City:
Latitude :
53d 44' 25.6"N
Longitude: 002d 54' 25.4"W
Height above ellipsoid: 65m (EGM96 Geoid
Height = 52.4m)
Datum WGS 84 - all coordinates
4.
TIMING OF EVENTS OCCULTATION
RECORDED? NEGATIVE
Type of event:
(S)tart observation (I)nterrupt start (D)isappearance (B)link (F)lash
(E)nd observation (J)Interrupt end (R)eappearance (O)ther (specify)
Event
Time (UTC) Accuracy
Code
(HH MM SS.ss) (+/-S.ss)
S
22 00 00 (Central predicted
time here: ~22:02:04 UT)
E
22 03 57
5.
TELESCOPE Type: Schmidt-Cassegrain Aperture:
406mm + f/3.3 reducer
Mount: Altazimuth 'goto' Motor drive: Yes
Magnification: Video f.o.v. ~ 15' x 11'
6.
TIMING
Timekeeping:
Mode: On-screen display - BlackBoxCamera 'STVASTRO'
inserter.
Device: VIDEO - Watec 902H2 Ultimate CCIR
video camera at Cass. focus.
Gain Control MANUAL, gain
Recording: Sony DCR-
Backup: MSF 60KHz time signal beeps on audio
track - synch. confirmed.
7.
OBSERVING CONDITIONS
Atmospheric transparency: Fair
Wind: Nil Temperature: -4C
Star image stability :
Good Star elevation: +38 degrees
No scintillation
Minor Planet visible on video? No (LM = 13)
8.
OBSERVATION QUALITY - Very Good
9.
ADDITIONAL COMMENTS
Report submitted to Gilles Regheere and
PLANOCCULT only.
Video clip examined frame-by-frame in
VirtualDub (6000 frames!) - star
present on every frame - NO occultation.
(Site INSIDE predicted track near N limit.)
Best
Regards:
Date:
2010 Jan 09
(Rev.
Jan 2010)
ASTEROIDAL OCCULTATION - REPORT
+------------------------------+ +------------------------------+
|
EAON | |
IOTA/ES |
| | |
INTERNATIONAL OCULTATION |
|
EUROPEAN ASTEROIDAL | | TIMING
ASSOCIATION |
|
OCCULTATION NETWORK | |
EUROPEAN SECTION |
+------------------------------+ +------------------------------+
1
DATE: 2009/12/12
2
OBSERVER: Name : Tim HAYMES Abbr: TVH
E-mail: tvh.observatory@btinternet.com
Address:
Hill Rise, Knowl Hill Common, RG10 9YD UK
3
OBSERVING STATION: Nearest city: MAIDENHEAD
Latitude:
N 51 30 22".0 (OSGB)
Longitude: W 00 48 52".7 (OSGB)
Altitude:
75 m
-
Single station
+----------------------------------+
4
TIMING OF EVENTS: | |
| OCCULTATION RECORDED: NEGATIVE |
| |
+----------------------------------+
Type of event
Start observation Interrupt-start Disappearance Blink
Flash
End observation Jnterrupt-end Reappearance Other (specify)
Comments
Event
Time (UT) P.E. Acc.
Code
HH MM SS.ss S.ss S.ss
S -
18:29:39 - -
:
D
- - -
:
R
- - -
:
E -
18:35:40 - -
:
Duration :
Mid-event :
5
TELESCOPE: Type: NEWTONIAN Aperture:
300mm F/4
Magnification: prime focus
Mount:EQUATORIAL Motor drive: YES
6
TIMING & RECORDING:
Time source: BT telephone
Sensor: Watec 120N+ 2/25th integration
Recording: Sony
Time insertion: Video Time Inserter
7
OBSERVING CONDITIONS:
Atmospheric transparency: GOOD Wind: NO
Temperature: 6 C
Star image stability: FAIR Minor planet visible: NO
8
ADDITIONAL COMMENTS:
23 miles north of the predicted centerline (
Photometric frame analysis performed (Limovie
/ AviSynth)
Clear sky.
ASTEROIDAL OCCULTATION - REPORT
+------------------------------+ +------------------------------+
|
EAON | |
IOTA/ES |
| | |
INTERNATIONAL OCULTATION |
|
EUROPEAN ASTEROIDAL | | TIMING
ASSOCIATION |
|
OCCULTATION NETWORK | |
EUROPEAN SECTION |
+------------------------------+ +------------------------------+
1
DATE: 2009/12/20
2
OBSERVER: Name : Tim V.HAYMES Abbr: TVH
E-mail: tvh.observatory@btinternet.com
Address:
Hill Rise, Knowl Hill Common, RG10
3
OBSERVING STATION: Nearest city: MAIDENHEAD
Latitude:
N 51 30 22".0 (OSGB)
Longitude: W 00 48 52".7 (OSGB)
Altitude:
75 m
-
Single station
+----------------------------------+
4
TIMING OF EVENTS: | |
| OCCULTATION RECORDED: NEGATIVE |
| |
+----------------------------------+
Type of event
Start observation Interrupt-start Disappearance Blink
Flash
End observation Jnterrupt-end Reappearance Other (specify)
Comments
Event
Time (UT) P.E. Acc.
Code
HH MM SS.ss S.ss S.ss
S -
22:26:00 - -
:
D
- - -
:
R
- - -
:
E -
22:41:00 - -
:
Duration :
Mid-event :
5
TELESCOPE: Type: NEWTONIAN Aperture:
300mm F/4
Magnification: prime focus
Mount:EQUATORIAL Motor drive: YES
6
TIMING & RECORDING:
Time source: MSF Anthorn
Sensor: Watec 120N+ 2/25th integration
Recording: Sony
Time insertion: Video Time Inserter
7
OBSERVING CONDITIONS:
Atmospheric transparency: GOOD Wind: NO
Temperature: -3 C
Star image stability: FAIR Minor planet visible: NO
8
ADDITIONAL COMMENTS:
North of the predicted centerline in the 1
sigma zone
Photometric frame analysis performed (Limovie
/ AviSynth)
Icy conditions. Difficulty opening the
observatory door.
ASTEROIDAL OCCULTATION -
REPORT
+------------------------------+ +------------------------------+
|
EAON | |
IOTA/ES |
| | |
INTERNATIONAL OCULTATION |
|
EUROPEAN ASTEROIDAL | | TIMING
ASSOCIATION |
|
OCCULTATION NETWORK | |
EUROPEAN SECTION |
+------------------------------+ +------------------------------+
1
DATE: 2009/12/25
2
OBSERVER: Name : Tim V.HAYMES Abbr: TVH
E-mail: tvh.observatory@btinternet.com
Address:
Hill Rise, Knowl Hill Common, RG10
3
OBSERVING STATION: Nearest city: MAIDENHEAD
Latitude:
N 51 30 22".0 (OSGB)
Longitude: W 00 48 52".7 (OSGB)
Altitude:
75 m
-
Single station
+--------------------------------------+
4
TIMING OF EVENTS: | |
| OCCULTATION RECORDED: INCONCLUSIVE |
| |
+--------------------------------------+
Type of event
Start observation Interrupt-start Disappearance Blink
Flash
End observation Jnterrupt-end Reappearance Other (specify)
Comments
Event
Time (UT) P.E. Acc.
Code
HH MM SS.ss S.ss S.ss
S -
23:
D
- - -
:
R
- - -
:
E -
Duration :
Mid-event :
5
TELESCOPE: Type: NEWTONIAN Aperture:
300 mm
Magnification: prime focus F/4
Mount: EQUATORIAL Motor drive: YES
6
TIMING & RECORDING:
Time source: MSF
Anthorn 60 KHz
Sensor: Watec 120N integrating video camera.
Recording: Sony
Time insertion: Video time inserter (Manual
synchronisation to UT)
7
OBSERVING CONDITIONS:
Atmospheric transparency: GOOD Wind: NO
Temperature: -1 rising to +2 C
Star image stability: FAIR Minor planet visible: YES
8
ADDITIONAL COMMENTS:
In the track. Photometric frame analysis
performed. Very poor recording.
Unknown at the time, but heavy dew on the
optical surfaces required a
integration setting 6 (32/25th sec
integration !!).
An observation made more difficult by the
small 0.3mag drop
Result: INCONCLUSIVE
Project NeilBone (coordinated by
2009 Dec 14
Please find attached a spreadsheet showing our
target list and a summary of
progress.
Note that some of the original targets have been now discounted
mainly because they do not attain a low-enough phase
angle but also if in
close proximity to the bright Moon when at
opposition.
We missed coverage of (770)
7 other target bodies to date - so 7 out of 8 is a
pretty good success rate.
The latest was (1645) Waterfield for which we have
images virtually at
opposition, some using the Tzec Maun robotic
telescope facility (thanks to
Darryl Sergison), and some taken during a live
observing session on the
Faulkes Telescope South during last Saturday's BAA
Christmas Meeting. I am
also pleased to say that for our project's namesake,
(7102) Neilbone we
already have 5 observing runs in the bag with more
planned - opposition is
on Jan 18.
Our next target passing through opposition is (581)
Tauntonia on Jan 4.
Current targets are shown in green on the
spreadsheet. Please make those
objects close to opposition your priority so this is
in order: (1645),
(121) and (581).
Thanks,
|
Project NeilBone: |
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List B - updated 2009 Dec 14 |
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Opposition |
|
Rotational |
Observed |
Notes |
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||
|
Asteroid |
Asteroid |
Asteroid |
Opposition |
Minimum |
Min. Observed |
V |
|
|
Lightcurve |
Observed |
Lightcurve |
|
|
|
Number |
Name |
Type |
Date |
Phase Angle |
Phase Angle |
Mag |
Dec. |
Period |
Amplitude |
Period |
Amplitude |
|
|
|
|
|
|
m d |
deg |
deg |
|
|
h |
mag |
|
mag |
|
|
|
|
|
|
2009 |
|
|
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|
|
150 |
Nuwa |
Cb |
10 23.8 |
0.08 |
0.10 |
11.5 |
+11 |
8.14 |
0.09 |
8.134 |
0.15 |
|
|
|
1130 |
Skuld |
S |
10 24.9 |
0.18 |
0.19 |
13.5 |
+12 |
4.81 |
0.5 |
4.806 |
0.26 |
|
|
|
384 |
Burdigala |
S |
11 08.7 |
0.13 |
0.17 |
12.1 |
+16 |
17 |
0.03 |
400 |
0.32 |
on-going |
|
|
770 |
|
S |
11 10.2 |
0.27 |
0.82 |
12.2 |
+18 |
5.951 |
0.40-0.55 |
|
|
missed coverage close to opposition |
|
|
138 |
Tolosa |
S |
11 15.1 |
0.08 |
0.08 |
11.5 |
+18 |
10.101 |
0.4 |
|
|
on-going |
|
|
1423 |
Jose |
S |
11 20.1 |
0.02 |
0.02 |
13.8 |
+20 |
12.307 |
0.68-0.82 |
|
|
on-going |
|
|
121 |
Hermione |
Ch |
12 08.1 |
0.17 |
0.17 |
11.6 |
+23 |
5.551 |
0.04-0.45 |
|
|
on-going |
|
|
1645 |
Waterfield |
XDC |
12 12.5 |
0.06 |
0.06 |
14.5 |
+23 |
4.861 |
0.2 |
|
|
on-going |
|
|
171 |
Ophelia |
C |
12 16.6 |
0.35 |
not a target |
12.2 |
+22 |
6.665 |
0.14-0.45 |
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2010 |
|
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|
581 |
Tauntonia |
Xk |
01 04.2 |
0.18 |
|
13.8 |
+23 |
16.54 |
0.06 |
|
|
on-going |
|
|
702 |
Alauda |
B |
01 08.8 |
0.28 |
not a target |
11.7 |
+23 |
8.36 |
0.1 |
|
|
|
|
|
7102 |
Neilbone |
? |
01 18.3 |
0.03 |
|
17.5 |
+21 |
? |
? |
|
|
on-going |
|
|
484 |
Pittsburghia |
S |
01 27.3 |
0.02 |
|
13.5 |
+18 |
10.63 |
0.37 |
|
|
on-going |
|
|
625 |
|
Sa |
01 28.8 |
0.09 |
not a target |
14.3 |
+18 |
21.101 |
0.5 |
|
|
too faint and near Moon when at opposition |
|
|
64 |
Angelina |
Xe |
01 29.6 |
0.003 |
|
10.2 |
+18 |
8.752 |
0.42 |
|
|
on going - near full Moon at opposition |
|
|
59 |
Elpis |
B |
03 13.3 |
0.18 |
|
11.9 |
+3 |
13.69 |
0.2 |
|
|
|
|
|
996 |
Hilaritas |
B |
03 15.8 |
0.05 |
|
14.3 |
+2 |
7.2 |
0.69 |
|
|
|
|
|
1451 |
Grano |
S |
03 17.2 |
0.08 |
|
14.2 |
+2 |
5.109 |
0.06 |
|
|
|
|
|
658 |
Asteria |
S |
03 23.9 |
0.16 |
|
14.4 |
-2 |
21.034 |
0.32 |
|
|
|
|
|
495 |
Eulalia |
S |
03 25.0 |
0.06 |
|
14.2 |
-2 |
29.2 |
0.3 |
|
|
|
|
|
73 |
Klytia |
S |
03 29.9 |
0.04 |
|
12.4 |
-4 |
8.297 |
0.35 |
|
|
|
|
|
1225 |
Ariane |
S |
03 31.2 |
0.10 |
|
14.2 |
-4 |
5.507 |
0.36 |
|
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2009 Dec 16
Dear All,
I have now analysed all images, etc. of (384)
Burdigala. Attached are the
latest results.
With Alessandro's latest datapoint from last night obtained
using the Bradford Robotic Telescope, it turns out
that the object turns
somewhat more slowly than I first thought and has a
rotation period close to
17.1 days (410+/-4 hr). The lightcurve amplitude is 0.34 +/- 0.03
mag.
These findings make this object the 13th slowest
known rotator in the Solar
System excluding our Sun and Moon - that's out of
more than 3800 such
objects.
There are some 830 asteroids which are intrinsically brighter than
H=10 for which we have an estimate of their rotation
period - amazingly
(384) Burdigala is the slowest known rotator in this
category! So quite
some discovery.
Doing phase angle studies in this way is a powerful
method for detecting
anomalous or unusual characteristics of
asteroids. It is possible to
discover a binary asteroid doing this type of
investigation. At present we
are in the very early stages of the project so no
doubt there will be more
surprises to come.
Note that although (384) is supposedly of a very
similar class of object to
that of (1130) Skuld, its phase curve fits a
relatively shallow linear
section having a coefficient of about 0.032 mag/deg
in contrast to (1130)
for which the main linear portion has a coefficient
close to 0.050 mag/deg.
(384) Burdigala also exhibits a more intense
opposition effect amounting to
about 0.33 magnitudes.
2009 December 29
Dear Fellow Observer,
Here are the provisional plots of the results for
asteroid (770)
were unable to follow this one through opposition
but have obtained an
accurate phase curve down to about 0.5 deg PhA - so
not bad at all. The
official rotation period for this object on the
MPC/JPL database is 5.951
hours but it became clear after trying to fit the
first 6-8 observing runs
that this period was incorrect. A period of 5.8202+/-0.0010 hr fits the
data uniquely, the object exhibiting a lightcurve
amplitude of 0.29 +/-0.02
mag at this apparition.
Searching the Web, I found observations from 2007
and from 2009 which also
found a period of about 5.819 hr. See: http://www2.ocn.ne.jp/~hamaten/00770bali-lc.htm
http://obswww.unige.ch/~behrend/page3cou.html#000770
The phase curve shown here has been normalised
relative to a linear phase
coefficient of 0.030 mag/deg. From the slope of the linear plot between
PhAs of 7-23 deg, it is clear that the linear
section has a slope lower than
this, probably around 0.026 mag/deg.
Now that we have results on 4 objects, it will be
worth starting to compare
the measured phase curves with theoretical ones
based on the H,G magnitude
system, seeing how different values for the Slope
Parameter, G, match our
results.
One other news item - some of us are using the Tzec
Maun remote observing
facilities for the project. I have submitted a report on our activities
to
the Tzec Maun foundation. The report can be accessed at: http://blog.tzecmaun.org/?p=562
Happy 2010,
P.S. Please
use my alternative email address as I am having trouble with my
btinternet one.
It is:
2010 Jan 2
Just a quick reminder that (581) Tauntonia reaches
opposition on the night
of January 3/4 and so this is the main priority
target for observation over
the next week.
I managed to image it last night when 15 degrees from the
98% illuminated Moon and obtained a good result
thanks to the crystal clear
sky. So we
are now poised to obtain good coverage as the Moon is waning and
moving further and further away from this asteroid,
which by the way is an
Xk type so rather unusual in nature.
2010 Jan 19
Dear Section Member,
Last October, I set up a special BAA project in
honour of our late Meteor
Section director, Neil Bone, who sadly died from
cancer last April at the
early age of 49.
Some weeks before he died, Neil learned that asteroid 1936
NB had been named after him as an acknowledgement of
all that he had done in
furthering amateur astronomy and popularising the
subject amongst the
public. It
turned out (and I was able to explain this to Neil in person)
that 'his' object has an unusual orbit which might
be indicative of it once
having been a comet.
I also pointed out to Neil that 'his' asteroid would
also pass through an extremely low phase angle (i.e.
Sun-Asteroid-Earth
angle) of 0.03 degrees when at opposition this
month. Such events are very
rare, and open up the possibility of measuring the
light-scattering
properties of the surface regolith on the body by
measuring the extent to
which objects brighten and fade as they approach and
recede from opposition
. A cometary
body is very unlikely to exhibit a significant extra
brightening at opposition (see Postscript).
I told Neil that we would be starting this project
to observe not only 'his'
asteroid but also any other bright asteroid that
attained a very low phase
angle at opposition - it was the excuse that I had
been looking for for
several years now, I said. In all, we have 14 members participating in
the
observing programme and we have been following 12
asteroids of which (7102)
Neilbone is the latest of nine objects to reach
opposition. This special
event occurred yesterday (Jan 18) and it was in
effect a once-in-a-lifetime
opportunity provided the skies were clear since
(7102) is unlikely to reach
very low phase angle again for many decades. Fortunately, I can now report
that using the Faulkes telescopes, we have been
successful in observing the
project's namesake asteroid at opposition under very
good skies even though
it was only 17th magnitude: thanks to the advantage
of using the 2.0 metres
of telescope aperture which Faulkes provides. So far, Darryl Sergison and I
have used Faulkes telescopes to observe (7102) on 18
nights. We shall now
follow (7102) from time to time over the next couple
of months to watch how
it fades.
If you would like to participate by operating one of
the Faulkes telescopes
to follow Neil's asteroid then do let me know. There will also be a lot of
deskwork to reduce the many images that we have
acquired, so volunteers here
would be also appreciated. N.B. On September 25, we are having an
Observers' Workshop at Burlington House and my
objective will be to show the
various tricks of the trade in using the latest
re-incarnation of the
software, Astrometrica for accurate astrometry/photometry
of asteroids and
comets. The
results of Project NeilBone will be used as some of the worked
examples. Jon
Shanklin and John Mason will also be participating as section
directors for the Comet and Meteor Section
respectively. I think it would
be a good idea to then follow up the BAA workshop a
few months later with a
dedicated ARPS Workshop to further encourage
interest in these subjects.
Watch this space.
Clear and tranquil skies,
Director,
Postscript:
Comets are very dark and their surfaces are normally composed
of extremely fine particles or dust. Such surfaces suppress the
re-reflection of sunlight limiting the amount of
multiple light scattering
taking place.
This means that little or no extra enhancement occurs as the
objects pass close to zero phase angle. Asteroids which have a rocky
surface usually show a 20-30% boost in brightness
under these
circumstances - it's often referred to as the
"Opposition Effect'.
2010 Jan 24
Colleagues,
Please find attached the results for (770) Bali, an
average S-type asteroid.
Unfortunately we missed catching it very close to
opposition but our results
are nonetheless very satisfying. You will see that I am attaching the
zipped Excel spreadsheet that has been developed to
analyse our
observational data.
There are two Excel versions included, the Excel
97-2003 'steam-driven' one and the latest
version. The spreadsheet now
includes two additional sheets compared to earlier
versions. One is for the
final phase curve, the other is for notes and a
summary of the findings re.
the main parameters.
As mentioned in Update No.11, our period does not
agree with that given in
the Harris/Warner rotation period database used by the
MPC and JPL. There
they give 5.9513 hr and amplitude 0.4 mag with a
confidence parameter of 3.
However, I mentioned previously some recent
literature references which
agree with our value:
5.8190 hr http://www2.ocn.ne.jp/~hamaten/00770bali-lc.htm
5.8194 hr http://obswww.unige.ch/~behrend/page3cou.html#000770
In summary:
Derived Parameters (this work):
Name: (770)
Epoch: 2009
Oct - 2010 Jan
PhA Range (deg):
0.49 - 26.26
Period (hr):
5.8205 +/-0.0010
Amplitude
(mag): 0.29 +/-0.015
V(1,1,0)
magnitude: 11.39 +/-0.02
Phase
Coeff. (mag/deg): 0.0443 +/-0.0013
Opp. Surge at PhA=0.4 deg (mag): 0.29 +/-0.02
Opp. Surge at PhA=1.0 deg (mag): 0.21 +/-0.02
Few observations were made of this object using
robotic telescopes - usually
we manage to double the number of observing runs by
use of robotic
telescopes, so overall a good result nonetheless. I have attached a copy of
the composite lightcurve fyi.
Cheers,
2010 Jan 24
Dear Observer,
A short note to mobilise the troops for coverage of
these two asteroids over
the next 7 days!
We have (484) Pittsburghia reaching a tiny
January 27 at 0700 UT, and (64) Angelina attaining a
miniscule 0.003 degrees
on Friday, January 29 at 1420UT. Unfortunately the bright, almost full Moon
will interfere with both of these more especially
with the (64) Angelina one
when the 99% illuminated Moon will be less than 10
degrees away from the
target asteroid, so it will be quite a battle. At least (64) will be very
bright itself at V=10.2 or even a little brighter
than this. Also, all of
the robotic telescopes are not operating because of
the full Moon (Faulkes
does not go any closer than 15 degrees to the
Moon. I am going to try and
plead with Tzec Maun to operate their Australian
observatory that night.
The TOA-150 refractor would be ideal to try
this. UK-based observers should
try and observe (64) say about 2-3 hours after
sunset on that Friday.
One other thing.
I have reduced all the data for (138) Tolosa but there is
something slightly odd with the result. We therefore need to resume
observations of this for the next 7-10 days.
Clear Skies,