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Photometry of seventeen asteroids
ICARUS 11)0, 295--306 (1992)
Photometry of Seventeen Asteroids V. G. SHEVCHENKO, V. G. CHIORNIJ, Y u . N. KRUGLY, D. F. LUP1SHKO, R. A. MOHAMED, AND F. P. VELICHKO Astronomical Observatory of Kharkou University, Sumskaya Street 35, Kharkov 310022, Ukraine
T. M1CHAgOWSKI ~ Astronomical Observatory. of Adam Mickiewicz University, ul. St~meczna 36, 60-286 Poznati, Poland AND V . V . AVRAMCHUK AND A . N . DOVGOPOL The Main Astronomical Observatory of the Ukrainian Academy of Sciences, Goloseevo, Kieu 252127, Ukraine Received June 3, 1992; revised September 14, 1992
w o r k s in the p h o t o n c o u n t i n g s y s t e m . It has a negligible t r a n s f o r m a t i o n to the U B V s y s t e m , so that the c o l o r diff e r e n c e b e t w e e n the a s t e r o i d and c o m p a r i s o n star d o e s
Results of photoelectric observations from Kharkov Astronomical Observatory (Ukraine) are reported. These observations were made between 1985 and 1991. We also include observations of 4 Vesta made in 1981 at Torufi Astronomical Observatory (Poland). Most of the lightcurves are in the V band. The first published observations for Asteroids 151,206, 550, and 705 are reported. We determine or revise synodic periods for four asteroids: 104, 206, 241, and 550. The phase curves are obtained for three asteroids: 44, 104, and 550. © 1992AcademicPress, Inc.
TABLE I Asteroid Parameters D(km)
Type
G
Period (hr)
Asteroid
(T) a
(Th) a
(T) a
(LM)a (PW)a
(L) a
(pw) a
(2)
(3)
(4)
(5)
(7)
(8)
4 Vesta 43 A r i a d n e , , Nyea ,5 Eugenia o, Angelina 10, Klymene ~51 Abondantia
501
V
0.338
0.33
5.342
65
S
-0.048
0.1b
5.751
73
E
0.440
0.43
FC
0.15
0.07
60
E
0.369
127
C
0.196
47
S
0.25
lO5 Loreley
160
C0
0.15
--
C
0.103
156
C
0.507
169
CP
0.043
INTRODUCTION
(1)
Earth-based observations, especially UBV photometry, are the m a i n s o u r c e o f our k n o w l e d g e o f the p h y s i c a l p r o p e r t i e s o f the asteroidal population. T h e U B V l i g h t c u r v e s m a y be u s e d to d e t e r m i n e spin periods, pole o r i e n t a t i o n s , and s h a p e s o f the asteroids. P h o t o m e t r i c o b s e r v a t i o n s are also useful for other p u r p o s e s , such as d e t e r m i n a t i o n o f the b r i g h t n e s s - s o l a r phase angle relation,
This paper is our report of the photoelectric photometry
2oo H e r s i l i a
o f a s t e r o i d s carried out at the C h u g u e v s k a y a Station o f the K h a r k o v A s t r o n o m i c a l O b s e r v a t o r y . T h e 7 0 - c m teles c o p e w a s u s e d with an u n c o o l e d S-8 p h o t o m u l t i p l i e r ( F E U - 7 9 ) . M o s t o f the data w e r e taken in the V-band o f the standard J o h n s o n U B V s y s t e m . T h e e x c e p t i o n s are 4 V e s t a in 1985 ( B - b a n d ) , 511 D a v i d a ( U B V p h o t o m e t r y ) , and 532 H e r c u l i n a (BV in 1986). The one-channel Kharkov Observatory photometer
]
238 Hypatla
2,1 ,87 511 532 55o 70, 705
214
(o)
0.59
6.421 5.699 8.752
0.07
9.
7.226 7.33 8.9
G. . . . . ia Venetia Dav~da H. . . . ~ina Senta
64
S
0.078
337
C
0.020
0.07
5.130
231
S
0.247
0.15
9.~05
40
S
0.25
ia
333
F
0.019 - 0 . 0 3
139
EMP
0.15
In1: . . . . .
Erminia
8.98~
8.88 8.998
0.20
20.555 8.727
" References: T, Tedesco 1989; Th, Tholen 1989; LM, Lagerkvist and Magnusson 1990; L, Lagerkvist et al. 1989; PW, present work.
Author may be reached via e-mail at: m i c h a s t r ~ p l p u a m l 1.bitnet.
295
0019-1035/92 $5.00 Copyright © 1992 by Academic Press, Inc. All rights of reproduction in any form resserved.
S H E V C H E N K O ET AL.
296 I
I
i
I
I
3.4
Period
xCi,~
"¢i"
0.,
~+
I
5.34~1E
hours
0
3.5 C ~o
× x,
~
,:'s ;> o
x
x -,.~-,.
x ""~Z~SoX,+ o ° ~
"*
'-J -; h'-'xc)
*
.
-i~
~
+
++oo°o+
0
x
x+X
xo
+
,
+
°
x:,O
Xo+~ x
×
3.6
•'r.2x +
~ ×× ~
n~ Date
3.7
=
I
I
o
=
0.2
I
Feb 2 5 . 0
-~xx -'.x+ x ~' x X×x x ~ x :,~-b'b Xx~
M a g n l t u d c ~tft
+
19el
4.2
V
0.027
0
1 9 8 1 Feb 25.9
44
Y
0.016
~"
19~i Feb 2 7 . 9
5.1
V
×
121
5 4
V
=
0,4
a
x +x
Feb 2 8 9
I
I
0.002 -0.023
I
0.6
=
I
0.8
1
Rotational phase FIG. 1.
4 Vesta. Zero phase at 1981 Feb 26.0000 corrected for light time.
!
Period
=
5.34212
00
0
hours
4.7
.lo
¢1
oc~
+ O0
4.8
% +
dR
cQ
0
"o ¢3
©
0
c~ +4+
4.9
Date
I
I
o
I
0.2
=
I
0.4
I
I
0.6
a
1985 May
9.8 i2.4
B
0
1 9 8 5 M a y 11.8 t 3 . 2
B
=
I
0.8
Rotational phase FIG. 2.
Ma~nltuclc shlR
~-
4 Vesta. Zero phase at 1985 May 10.0000 corrected for light time.
0.315 -0.024
|
I I
P H O T O M E T R Y OF S E V E N T E E N A S T E R O I D S I
I
I
I
I
Period
7.4
7.5 "0
297
=
I
6.42142
q<3 +
hours
~+
~+0 o
7.6
+
¢1
++
O
::> "0
0
7.7
o
0
0 0
o~
'0
c~.~ ~.
® o
°s /e
o
CO + ++
+ O
%
7.8
+ Date
7.9
M a g n i t u d e shIR
a
"Jr 1987 Oct. 20.0 21.0 (D 1987 Oct. 20.9 20.7 ~" 1987 Oct 28.9 i{].2
I 0
I
I
I
0.2
I
0.4
-0.003
V
-0.003 0.073
V
i
I 0.8
0.6
Rotational FIG. 3.
i
I
V
i I
phase
44 Nysa. Zero phase at 1987 Oct 23.0000 corrected for light time.
i
i
i
i
i
7.1 Period
6.42142
=
hours
+
7.2
+
"0
7.3
**+ +
+
++
¢,+ 2r
C~- + ,~, + +
y-
+
+
b
~+
7.4
0
+ 0
4~
+
+
0
-I,:3000
q)
cr~
O
O O
+
+
++ Q
+ ++ +
O+
+~o
dr
+O
~0+++
7.5 Date
a
Magnitude
+ 1987 Dec 9.7 4.2 (D 1987 Dec 18.7 8.7 "~ 1987 Dec 23.6 10.2
7.6 I
0.2
I
I
I
0.4 Rotational
FIG. 4.
I
0.6
I
I
0.8
phase
44 Nysa. Zero phase at 1987 Dec. 17.0000 corrected for light time.
V
shift 0.090
1/'
-0.010
V
-0.087
298
SHEVCHENKO
ET AL.
TABLE II Aspect Data, Photometric Results, and Comparison
Stars
Comparison
UT
x
Date
6
r
A
(x
Am
V(1.u)
R.A.
(1950)
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
152.0
9.4
2.379
1.398
4.2
0.13
3.46
81/02/25.9
151.7
9.4
2.378
1.398
4.4
0.13
3.47
81/02/28.0
151.2
9.5
2.376
1.399
5.1
0.13
3.48
81/03/~
1.0
150.9
9.5
2.375
1.399
5.4
0.13
3.50
85/05/
9.9
203.5
11.8
2.191
1.247
12.4
0.13
4.59’
203.1
11.6
2.190
1.255
13.2
0.13
4.62’
43 4.8
66.9
77.3
Obsf
(10)
(11)
(12)
6.15
Mi
0.4
-5.5
(9)
2.543
1.692
2.188
HO 90472 II
Mi
,,
,,
II 13
Mi
45.4 HD
Mi
1
47
119749
9.65’
V
9.36’
S,V
K,V
Ariadne
44 87/10/20.0
V
Vesta
81/02/25.0
90/01/
Dec. (1950)
4
85/05/11.9
stars
11.9
>0.08
6.94
4
19.5
21
24
0.05
7.45
5
06.9
17
25
11.84
Nysa 1.430
21.0
0.39
,I
II
7.46
S S
77.4
-5.5
2.187
1.419
20.7
0.39
77.3
-5.7
2.176
1.342
18.2
>0.29
7.38
5
07.4
17
07
10.65
S.V
69.8
-5.8
2.125
1.147
4.2
0.28
7.12
4
35.6
lb
15
10.82
K.S
87/12/18.8
67.6
-5.5
2.116
1.161
8.7
0.27
7.21
4 27.1
lb
02
7.75
K.S
87/12/23.7
67.7
7.29
U
22.5
lb
08
10.48
87/10/21.0 87/10/28.9 87/12/
9.8
-5.4
2.111
1.168 45
86/01/31.9
113.3
-4.7
2.797
128.6
0.5
6.4
0.11
7.62
7 36.9
lb
46
9.83
14.1
0.07
8.17
8 44.7
18 35
10.05
1.846
2.354
>O.l
1.484
91/09/11.0
10.3
-2.7
2.904
1.952
7.9
>0.2
8.74
10.1
-2.7
2.903
1.947
7.6
>0.2
8.68
91/09/14.0
9.8
-2.6
2.900
1.937
6.9
6.8
91/11/
1.8
5.4
-2.3
2.871
1.881
2.3
4.7
-1.6
2.865
1.885
4.5
1.2
-1.9
2.840
1.986 151
90/04/20.9
204.4
2.2
2.517
87/08/26.9
341.8
9.9
2.976
87/08/27.9
341.6
10.0
12.1
2.977
206
0.30
>0.18
8.66
0
41.7
1 37
12.28
Mi,K
0
40.3
1
28
10.78
M.V
0
M.K
8.34
0
23.5
04
11.07
s.v
0.30
8.52
0
20.0
-0
29
11.15
C,K
>O.l
8.95
0
07.7
-1
18
11.99
S.U
>O.ll
9.50
13
32.1
-7
15
12.09
K.M
Abundantia
1.515 lb5
K,S
Klymene
91/09/12.0
91/10/
S,V
Angellna
104
91/10/11.9
S
Eugenla
64 87/12/26.0
10.2
2.4
Loreley 1.984
4.5
0.08
8.04
22
37.9
2
02
10.65
S.V
1.983
4.3
0.08
8.06
22
37.3
2
02
10.19
s
43.1
-13
46
11.08
M.S
-13
41
10.91
M.S
Hersilia
91/05/13.9
236.8
5.9
2.836
1.832
2.7
jO.18
7.43
15
91/05/14.9
236.6
5.9
2.837
1.830
2.4
>0.18
7.43
15 42.7
299
PHOTOMETRY OF SEVENTEEN ASTEROIDS TABLE I I - - C o n t i n u e d (1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
238 Hypatia 88/08/15.9 326.9 12.1 2.795 1.798 4.6
> 0 . 0 9 8.24
21 40.2
-1 06 11.89 S,V
88/08/16.9 326.6 12.1 2,794 1.797 4.5
> 0 . 0 9 8.24
21 39.7
-1 17
88/08/19.9 326.0 11.9 2.791 1.794 4.3
> 0 . 0 9 8.28
21 37.0
-1 34 10.91
S,U
88/08/20,9 325.8 11.8 2.790 1.793 4.3
> 0 . 0 3 8.30
21 36.4
-1 47 12.34
S
88/08/21.9 325.6 11.8 2.790 1.793 4.4
> 0 . 1 0 8.22
21 35.3
-1 53 12.14 K,S
9.88
L,S
241 8ermanla 91/10/12.0
56.4
5.7 2.869 2.025 1 2 . 7
> 0 . 1 3 8.33
3 31.2
24 58 I i . 0 0
C,K
91/10/12.8
56.4
5.7 2.869 2.019 1 2 . 5
>0.06 - - -
91/10/16.0
56.0
5.7 2.872 1.997 1 1 . 4
>0.08 - - -
3 29.6
24 52
---
M,S
3 28.8
24 48
---
M,K
91/11/ 2.9
52.9
5.6 2.888 1.917 5.0
>0.1
7.87
3 16.0
23 54
9.15
C,S
86112/ 9.9
81.5 -9.7 2.497 1.521
0.05
8.53
5 25.5
13 31 10.37 S,V
487 Venetia 3.9
511Davlda 87/04/24.9 187.9 22.1 3.272 2.386
9.8
0.25
6.88
....
6.72
13 04.5
17 14 11.74 S,V
3 53.6
10 53 10.26 S,V
532 Hercullna 86/02/ 8.8
87105127.9
58.3 -9.1 2.815 2.487 20.3
182.1 2 2 . 3 2 . 3 1 2
1.700 23.5
>0.20
---
0.35
10.00
> 0 . 2 5 9.94
12 4 4 . 0
19 31
S,V
0 12.1
20 53 1 1 . 3 7
K,M
0 03.1
20 30 10.44 C,Kl
550 5 e n t a 91/09/
4.9
11.1
17.7 2.121
1.217
15.6
91/09/15.9
9.1 18.4 2.140 1.189 11.6
91/10/ 1.8
5.4 18.5 2.169 1.197 8.5
91/10/ 8.8
4.0 18.0 2.183 1.221
91/10/ 9.9
....
9.84
23 49.4
19 O0 12.10 C,S
9.6
> 0 . 2 7 9.84
23 44.4
18 02 12.67 K1,S
3.5 18.0 2.185 1.225 9.7
> 0 . 2 5 9.85
23 43.7
17 54 12.11
> 0 . 1 2 7.04
22 49.5
14 52 11.18 B,D
> 0 . 0 9 8.79
1 23.2
27 11 13.02 M,S
K,M
704 Interamnia 90/08/ 1.9 349.6 24.1 2.680 1.874 15.7 705 Erminla 90/10/18.9
29.8 17.0 2.875 1.910 6.0
N o t e . * denotes brightness in the standard B-band. " Key to observers: S, Shevchenko; C, Chiornij; K, Krugly; L, Lupishko; M, Mohamed; V, Velichko; Mi, Mich~owski; D, Dovgopol; P, Pluzshnik; KI, Kalashnikov; B, Belskaya.
not matter so much. The standard deviation for one measurement in the range V = 10-11 mag is equal to 0.015 mag for an integration time o f 30 sec (Lupishko et al. 1986, V e l i c h k o 1991). We normally obtained 20 to 70 data points per observing night. A nearby c o m p a r i s o n star o f roughly solar color w a s measured for each asteroid at similar frequencies (each m e a s u r e m e n t o f an asteroid had a corresponding comparison-star m e a s u r e m e n t within a few minutes o f time). Most o f the c o m p a r i s o n stars were calibrated to the standard s y s t e m using standard stars with asteroid-like
colors chosen from Blanco et al. (1968), Kazanasmas et al. (1981, 1982), or Landolt (1973, 1983). Most of the observations were made between 1985 and 1991. The only exceptions are data for 4 Vesta from 1981, carried out at Torufi Astronomical Observatory (Poland) with a 20-cm refractor and an uncooled RCA 1P21 photomultiplier. In addition to this article, a data file containing the original observations is available. This can be obtained through e-mail by sending a request to one of the authors (T. Michalowski).
300
S H E V C H E N K O ET AL. .
.
.
.
I
.
.
.
.
}
.
.
.
.
i
.
.
.
.
)
.
.
.
.
}
6.5
.
.
.
H
=
692
C
:
0 59
I
.
IV
I
I
8
III
~>. "o
8.2
0
8.4 7.5
U}
8.6 . . . .
t
. . . . . . .
5
.
10
.
,
.
.
.
.
i
15
,
.
.
•
20
30
FIG. 7.
44 Nysa.
We have determined the synodical periods and parameters of the HG magnitude system (see Bowell et al. 1989) if the lightcurves have allowed this. OBSERVATIONS
We observed 17 asteroids on 46 nights. These asteroids are listed in Table I. Column 2 gives their diameters according to Tedesco (1989). Their taxonomic types (Tholen 1989) are given in column 3. The G values of the HG magnitude system are in columns 4, 5, and 6 and were taken from Tedesco (1989), Lagerkvist and Magnusson (1990), and the present work, respectively. The periods
•
I
. . . .
i
. . . .
I
. . . .
I
.
.
.
I
.
7.4
~++++ ; ~ 4 ~ - ~
7.6 +
+++4-
+ +++4- +
O "O
7.8
e,,
i
19
. . . .
i
20
. . . .
I
,
,
21
,
,
I
22
,
,
•
•
i
23
1986 Jan 31 FIG. 6.
I
t
I
24
,
I
26
1987 Dec 25
Solar phase angle oz FIG. 5.
,
22
. . . .
,
25
45 Eugenia. H o u r s of U T corrected for light time.
64 Angelina. H o u r s of U T corrected for light time.
of rotation from Lagerkvist et al. (1989) are in column 7, while in column 8 we give the periods determined by us. Table II contains the aspect data for each asteroid on each night of observation. The asteroid names are listed as subheadings. The first column is the date of the observation, given to the center of the observed lightcurve. Columns 2 and 3 are the 1950 ecliptic longitude (X) and latitude (/3) of the asteroid, referring to the time in column I. Columns 3 and 4 are the distances in astronomical units from the asteroid to the Sun and the Earth, respectively, and column 6 is the solar phase angle (a). Columns 7 and 8 give the amplitude (Am) and reduced V(l,a) magnitude of the maximum light observed during the night, respectively. Columns 9, 10, and 11 refer to the comparison star, giving its 1950 right ascension and declination (for two stars these are replaced by the catalog numbers) and its V magnitude, respectively. The last column gives the codes for the observers, which are explained at the end of the table. Our observations are mainly presented as composite lightcurves which are constructed according to the procedure described by Magnusson and Lagerkvist (1990). Data are composited with the period shown in the figure. The points from different nights are shown by different symbols. Vertical shifts of the individual nights are made in order to obtain a good fit. The values of these shifts are displayed in the figure. The abscissas are the rotational phase with the zero point corrected for light-time as shown in the figures. The magnitudes have been reduced to unit heliocentric and geocentric distances and refer to Johnson V (except Vesta in 1985). If we have only one lightcurve for a given asteroid then the abscissas are the hours of UT corrected for light-time. We have obtained very short lightcurves for Asteroids
301
PHOTOMETRY OF SEVENTEEN ASTEROIDS I
I
I
I
I
I
8.5 =
Period
8.98400
hours
×
8.6
x
× ,~.
x
A
¢)
o5.OO ~ o *~x
8.7
8.8
x × ~ "~
~ o+
L~
"1o
~,~ + ~ ,~++~
a) o
"o ¢) a~
A
8.9
Date ¢~
9.1
I
,
I
,
0
1991
Sep
10.9
"/.9 7.6
0
1991
Sep
12.0
V'
-0,096
Y
-0.045
X
1991 Sep 13.9 1 9 9 1 Oct 8 . 7
6.9
Y
-0.019
2.3
V
0.247
A
1991 Oct 11.8
4.5
Y
,C~
1 9 9 1 Nov
12.1
V
1.8
,
I
0.I16 -0.291
,
I
0.4
0.2
Magnltude shlR
a
Jr
I
0.6
0.8
Rotational phase 104 Klymene. Zero phase at 1991 Sep 29.0800 corrected for light time.
FIG. 8.
43, 51 l, and 532, so we decided not to publish these figures in this paper. Those who want to use them can get them in machine-readable form either from us or from the next issue of the Asteroid Photometric Catalogue. We have been able to determine the phase curves for three asteroids: 44,104, and 550 (Figs. 5, 9, and 17, respectively). The method of Lagerkvist and Magnusson (1990) was used. Our results are presented as plots of reduced . . . .
,
. . . .
,
. . . .
,
. . . .
,
. . . .
,
V magnitude of the second Fourier component maxima against the solar phase angle. 4 Vesta
This asteroid is the best-observed asteroid reported in the literature. The Asteroid Photometric Catalogue-hereafter referred to as APC (Lagerkvist et al. 1987, 1988, and 1992a)--gives information on 110 lightcurves taken
. . . .
H =
8.11
G =
0 07
9.2
@
i=
9.4
+
> 9.6
'0
+
+
++
,
I
I
++
+
+
+ + %
+
++
++++
g) 0
@
9.8 9.5
. . . . 0
, 5
. . . .
, 10
•
i '
'
. . . .
' 15
i 20
. . . .
i 2.5
I
. . . .
21.5
30
Solar phase angle o{ FIG. 9.
104 K l y m e n e .
I
I
I
I
I
22
I
.
.
.
22.5 1990
FIG. 10.
I
.
I
23
.
.
.
.
23.5
Apr 20
151 Abundantia. Hours of U T corrected for light time.
302
SHEVCHENKO i
44 Nysa
I
Period =
7 . 2 2 8 hours
7.8 "0 =
E
©
;>
8.2
Date +
0
Magnltude V V
1907 Aug 26,8 1987 Aug 27.6
0.004 -0.009
8.4 I
,
0
I
,
I
0.2
,
0.4
I
i
I
0.6
,
I
0.8
1
Rotational phase FIG. 11. light time.
i
I
i
This asteroid has previously been observed during 14 apparitions (1949-1986). We observed Nysa during six nights in October-December 1987, while the phase angle changed in the range from 4° to 21 °. Our observations are presented in Fig. 3 (for large phase angles) and in Fig. 4 (for smaller ones). Note the increase in the lightcurve amplitude from 0.27 to 0.39 mag for these phase angles. We determined the G-value to be equal to 0.59 (see the phase curve in Fig. 5). Harris et al. (1989) reported that when they fitted their 1986 lightcurves to the HG magnitude relation, they yielded the slope parameter G = 0.51. They also observed a remarkable opposition spike for this asteroid. 45 Eugenia
165 Loreley. Zero phase at 1987 Aug 27.0900 corrected for
I
7.2
ET AL.
I
Period
i
?.330 houra
=
APC reports observations from eight oppositions. Our lightcurve (Fig. 6) supplements observations carried out in October 1985 (four nights) and on 17 January 1986 (see APC). 64 Angelina
=
7.4 ~.O
0
0
o
7.6
0
oOooO o o ® 0
cP Date
@
i
0
,
I
0.2
0
104 Klymene
IVlagnttude shift
+ 1991 May 13.8 © 1991 May 14.9
7.8
This asteroid has previously been observed during three oppositions. Our lightcurve (Fig. 7) is a supplement of those observed during 11 nights in January-March 1988 (APC).
0
i
V V I
0.4
0,006 -0.014 i
I
0.6
t
I
0.8
i
I
1
Rotational phase FIG. 12. light time.
206 Hersilia. Zero phase at 1991May 14.0900corrected for
during 17 oppositions. We present our lightcurves from two apparitions--1981 and 1985 (B-lightcurves). Because of the very small range of solar phase angles in our lightcurves we cannot make the phase curves. Our lightcurves are presented in Figs. I and 2. There are no previous 1981 lightcurves in APC, but our observations were taken at similar aspects to those in the 1951/52 opposition (see APC). In 1985, Vesta was also observed by others during three nights in April (APC). 43 Ariadne This asteroid has been observed during seven oppositions. Our lightcurve, consisting of 10 points, spans only 2 hr and supplements the observations made in November 1989 (see APC).
This asteroid was previously observed only during one night in 1977 and its period was not known with good accuracy (see Table I). Our six nights of observations (Fig. 8) in September-November 1991 allowed us to determine the period of rotation (8.984 + 0.001 hr) and the phase curve (G = 0.07--see Fig. 9). Lagerkvist and Magnusson (1990) found the average slope parameter for lowalbedo objects to be 0.09, so our G value is more consistent with typical values for C-type asteroids than that given by Tedesco (1989)--see Table 1. 151 Abundantia No previous lightcurve observations of this asteroid have been published. We present only a short lightcurve observed in 1990 (Fig. 10). 165 Loreley There are lightcurves from three oppositions in APC. Loreley, contrary to most asteroids, shows three maxima and three minima during its rotational period. We observed Loreley during two nights in 1987 (fourth apparition), but our observations do not cover the whole period (Fig. i I).
303
P H O T O M E T R Y OF S E V E N T E E N A S T E R O I D S I
I
I
1
Period =
8.88000 hours
8.2 4~
0
o +~q~
+ +
~+
+
+
+%,+
o
~
A+.
o
+
o
. x~.,~o
8.3
o°e
o
o
~+~
o x
.
+
xX'x
~,. "
+
o
~
A ~" ~
0
Jr o X
I
,
0
I
I
0.2
0.4
,
I
JO x~^'~r '
CO
,,~
xz~ 0 0 0
,~,~. ~
'~"
at
Date
8.4
~ ~
4.8 4.5
V Y
1988 Aug 19.8 1 9 8 8 /tug 2 0 . 9 1 9 8 6 /tu¢ :~t.8
4.3 4.3 4.4
Y Y Y
x
I
0.001 0008 -0.028 0013 0.012 ,
I
0.8
0.6
0
,.o+
Mag~tltude
1 9 8 8 Aug 15.8 1988 ~ 18.9
,
0 x"
x
1
Rotational phase 238 Hypatia. Zero phase at 1988 Aug 18.0000 corrected for light time.
FIG. 13.
i
7.8
i
Period -
8.998 h o u r s
o
-o
E o
8.2
8.2
o
Ii 8.4 8.4 e~
E I 0
,
I 0.2
i
I 0.4
,
I 0.6
i
I 0.8
I
Rotational phase Date
Magnitude shift
+ 1991 Oct 12.0 0 1991 Oct 12.8 1991 Oct 16.0
V -0.232 Vrel. 6.520 Vrel. 8.943
x
V
1991 N o v
2.8
~
8.6
'ID o
8.8
20
0.230
FIG. 14. 241 Germania. Zero phase at 1991 Oct 18.0000 corrected for light time.
22 1986 Dec
FIG. 15.
9
487 Venetia. Hours of UT corrected for light time.
304
SHEVCHENKO
I
ET AL.
I
9.1
Period
=
hours
20.55500
+
+++
9.2
XXX "H-T+ + +
9.3
'
.*A
xx× x~.×
+ +
A " ~ x
x xxx
+
9.4
o~
x xX xX× x
e
> 'lO
~××
9.5
O "O
©
9.6
I~tte q0
9.7
a
1991 Sep 1991 Sep
"~ 1991 Oct X 1991 ~ A
9.8
I
~nltudc
4.9 1 5 . 6 15.9
11.6
'¢
-0674
8.5
Y
9.6
Y
-0.584 -0604
1991 Oct
9.8
9.7
¥
-'0.~8
*
I
z
I
0.8
phase
550 Senta. Zero phase at 1991 Sep 26.0000 corrected for light time.
hr) which was consistent with the previously published one (see Table I). Lagerkvist et al. (1992b) observed this asteroid in February 1991 and found its rotation period to be 8.86 hr, which is in agreement with ours. 241 Germania
238 Hypatia
APC reported observations in 1981. Our lightcurves (Fig. 13) allowed us to determine the period (8.88 -+ 0.02
.
*
0.6
Our lightcurves from 1991 are the first observations reported for Hersilia (Fig. 12). We determined the period of rotation to be 7.33 _+ 0.03 hr.
.
I
0.4
206 Hersilia
.
~r
1.7
Rotational
.
-0803
88
0.2
FIG. 16.
ahlfl
V
I
.
.
.
.
~
.
.
.
.
I
.
.
.
.
J
.
.
.
.
r
H = C =
9
.
.
.
No previous lightcurve observations have been published in APC. We observed Germania on four nights in October-November 1991 (Fig. 14). The synodic period is found to be 8.998 _+ 0.003 hr. Because of very short runs
.
927 0 20
6.8 q~
\ ~r-~m 9.5
\ 7
\ \.
m
>
++++
+ +
7.2 t,,.* 7.4 t0.5 . . . .
i 5
. . . .
, . . . . 10
i . . . . 15
J 20
. . . .
i . . . . 25
I
21
30
Solar phase angle o¢ FIG. 17.
550 Senta.
.
.
.
.
I
.
1990
FIG. 18.
.
.
.
I
22
23 Aug
.
.
.
.
I
24
!
7041nteramnia. Hours of UT corrected ~ r l i g h t t i m e .
305
PHOTOMETRY OF SEVENTEEN ASTEROIDS
550 Senta 8.6 ¢ cl
+
8.8
~+
,4-
+~+
++ +
+
+
,
+
+4+
o
Our 1991 lightcurves (Fig. 16) are the first published ones for this asteroid. We have determined the rotational period to be 20.555 --- 0.005 hr. In spite of a small range of solar phase angles, we decided to determine the slope parameter and found G = 0.20 (see the phase curve in Fig. 17). 704 Interamnia
a..
9.2
I
I
18
i
I
1990
FIG. 19.
i
20
I
22 Oct
i
I
The APC gives information about lightcurves from three oppositions. Our incomplete lightcurve (Fig. 18) is the fourth apparition in which Interamnia was observed photoelectrically.
24
18
705 Erminia. Hours of UT corrected ~ r l i g h t t i m e .
during each night, we realize that other periods are still possible (for example, 12.73 hr). Lagerkvist et al. (1992b) observed Germania in August 1990 and suggested the most likely rotation period was about 15.2 hr, but they were unable to derive a unique solution. 487 Venetia
Our 1986 lightcurve (Fig. 15) spans only 5 hr, so we cannot use it to determine the synodic period. Venetia was observed in 1984 (see APC) but these lightcurves are very incomplete, too. 511 Davida
This is a very well observed asteroid. APC reports 48 lightcurves from 12 oppositions. Our observation spans a period of 2 hr and seems to be the only lightcurve from the 1987 apparition. We have also determined B - V = 0.70 mag and U - B = 0.37 mag, which are in agreement with those given by T e d e s c o (1989). 532 Herculina This asteroid has previously been observed during s e v e n a p p a r i t i o n s . H e r c u l i n a h a s v e r y u n u s u a l lightc u r v e s . T h e y e x h i b i t t w o m a x i m a a n d t w o m i n i m a in s o m e oppositions and only one maximum and one minimum in o t h e r s d u r i n g t h e s a m e r o t a t i o n p e r i o d . O u r r e l a t i v e p h o t o m e t r y l i g h t c u r v e t a k e n o n 27 M a y 1987 c o n t a i n s o n l y eight points, but many other observations were carried out in J a n u a r y - M a y 1987 ( s e e A P C ) . W e a l s o r e p o r t t h a t o n 8 F e b 1986 t h e V b r i g h t n e s s o f H e r c u l i n a w a s 6.72 m a g ( s e e T a b l e II) a n d B - V = 0 . 7 9 m a g .
705 Erminia
Our 1990 observation (Fig. 19) is the first published lightcurve for this asteroid. It seems to be only a part of the rotation cycle so we cannot determine the period of rotation. ACKNOWLEDGMENTS We thank C.-1. Lagerkvist for his valuable comments, P. Magnusson for his useful suggestions and his help in drawing all the figures, and I. N. Belskaya, E. Pluzschnik, N. I. Koshkin, and A. V. Kalashnikov for their assistance during the observations of the asteroids 704, 4, 104, and 550, respectively. T.M. is indebted to the Swedish Institute for having supported his stay at the Uppsala Astronomical Observatory, where this paper was prepared for publication. REFERENCES BLANCO, V. M., S. DEMERS, G. G. DOUGLAS, AND M. P. FITZGERALD 1968. Photoelectric Catalog o f Magnitudes and Colors o f Stars in the UBV System. Publ., U.S. Naval Obs., Washington. BOWELL, E., B. HAPKE, D. DOMINGUE, K. LUMME, J. PELTONIEMI, AND m. W. HARRIS 1989. Application of photometric models to asteroids. In Asteroids H (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 524-556. Univ. of Arizona Press, Tucson. HARRIS, A. W., J. W. YOUNG, L. CONTREIRAS, T. DOCKWEILER, L. BELKORA, H. SALO, W. D. HARRIS, E. BOWELL, M. POUTANEN, R. P. BINZEL, D. J. THOLEN, AND S. WANG 1989. Phase relations of high albedo asteroids: The unusual opposition brightening of 44 Nysa and 64 Angelina. Icarus 81, 365-374. KAZANASMAS, M. S., L. A. ZAVERSHNEVA, AND t . F. TOMAK 1981. Atlas and Catalogue o f Magnitudes o f PhotometHcal Standards. Naukova Dumka, Kiev. KAZANASMAS, M. S., L. A. ZAVERSHNEVA,AND L. F. TOMAK 1982. Atlas o f Photometrical Standards in the Star Areas. Naukova Dumka, Kiev. LAGERKVlST, C.-I., AND P. MAGNUSSON 1990. Analysis of asteroids lightcurves. II. Phase curves in a generalized HG-system. Astron. Astrophys. Suppl. Ser. 86, 119-165. LAGERKVIST,C.-I., M. A. BARUCCI,M. T. CAPRIA,M. FULCHIGNIONI, L. GUERRIERO, E. PEROZZl, AND V. ZAPPALA 1987. Asteroid Photometric Catalogue. Consiglio Nazionale delle Ricerche, Rome. LAGERKVIST,C.-I., M. A. BARUCCI,M. T. CAPRIA, M. FULCHIGNIONI,
306
SHEVCHENKO
P. MAGNUSSON,AND V. ZAPPALA 1988. Asteroid Photometric Catalogue, 1st update. Consiglio Nazionale delle Ricerche, Rome. LaGERKVlST, C.-I., A. W. HARRIS, AND V. ZAPPALA 1989. Asteroid lightcurve parameters. In Asteroids H (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 1162-1179. Univ. of Arizona Press, Tucson.
LAGERKVIST, C.-I., M. A. BARUCCI, M. T. CAPRIA, M. DAHLGREN, A. ERIKSON, M. FULCHIGNIONI, AND P. MAGNUSSON 1992a. Asteroid Photometric Catalogue, 2nd update. Uppsala Universitet, Uppsala. LAGERKVIST, C.-I., P. MAGNUSSON,H. DEBEHOGNE, M. HOFFMAN, A. ERIKSON, A. DE CAMPOS, AND G. CUTISPOTO 1992b. Physical studies of asteroids XXV: Photoelectric photometry of asteroids obtained at ESO and Hoher List Observatory. Astron. Astrophys. Suppl. Set'.. in press. LANDOLT, A. 1973. UBV photoelectric sequences in the celestial equatorial selected areas 92-115. Astron. J. 78, 959-1020.
ET AL.
LANDOLT, A. 1983. UBVRI photometric standard stars around the celestial equatorial. Astron. J. 88, 439-460. LUPISHKO, D. F., F. P. VELICHKO, AND V. G. SHEVCHENKO 1986. Asteroid 1627 Ivar. UBV photometry, period and sense of rotation. Kinem. Phys. Celest. Bodies 2, 39-43. MAGNUSSON, P., AND C.-I. LAGERKVIST 1990. Analysis of asteroid lightcurves. I. Data base and basic reduction. Astron. Astrophys. Suppl. Set'. 86, 45-51. TEDESCO, E. F. 1989. Asteroid magnitudes, UBV colors, and IRAS albedos and diameters. In Asteroids 11 (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 1090-1138. Univ. of Arizona Press, Tucson. THOLEN, D. J. 1989. Asteroid taxonomic classifications. In Asteroids I1 (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 1139-1150. Univ. of Arizona Press, Tucson. VELICHKO, F. P. 1991. Determination and Analysis o f the Rotational Parameters ¢~fAsteroids. Ph.D. thesis, University of Kiev.
Photometry of Seventeen Asteroids V. G. SHEVCHENKO, V. G. CHIORNIJ, Y u . N. KRUGLY, D. F. LUP1SHKO, R. A. MOHAMED, AND F. P. VELICHKO Astronomical Observatory of Kharkou University, Sumskaya Street 35, Kharkov 310022, Ukraine
T. M1CHAgOWSKI ~ Astronomical Observatory. of Adam Mickiewicz University, ul. St~meczna 36, 60-286 Poznati, Poland AND V . V . AVRAMCHUK AND A . N . DOVGOPOL The Main Astronomical Observatory of the Ukrainian Academy of Sciences, Goloseevo, Kieu 252127, Ukraine Received June 3, 1992; revised September 14, 1992
w o r k s in the p h o t o n c o u n t i n g s y s t e m . It has a negligible t r a n s f o r m a t i o n to the U B V s y s t e m , so that the c o l o r diff e r e n c e b e t w e e n the a s t e r o i d and c o m p a r i s o n star d o e s
Results of photoelectric observations from Kharkov Astronomical Observatory (Ukraine) are reported. These observations were made between 1985 and 1991. We also include observations of 4 Vesta made in 1981 at Torufi Astronomical Observatory (Poland). Most of the lightcurves are in the V band. The first published observations for Asteroids 151,206, 550, and 705 are reported. We determine or revise synodic periods for four asteroids: 104, 206, 241, and 550. The phase curves are obtained for three asteroids: 44, 104, and 550. © 1992AcademicPress, Inc.
TABLE I Asteroid Parameters D(km)
Type
G
Period (hr)
Asteroid
(T) a
(Th) a
(T) a
(LM)a (PW)a
(L) a
(pw) a
(2)
(3)
(4)
(5)
(7)
(8)
4 Vesta 43 A r i a d n e , , Nyea ,5 Eugenia o, Angelina 10, Klymene ~51 Abondantia
501
V
0.338
0.33
5.342
65
S
-0.048
0.1b
5.751
73
E
0.440
0.43
FC
0.15
0.07
60
E
0.369
127
C
0.196
47
S
0.25
lO5 Loreley
160
C0
0.15
--
C
0.103
156
C
0.507
169
CP
0.043
INTRODUCTION
(1)
Earth-based observations, especially UBV photometry, are the m a i n s o u r c e o f our k n o w l e d g e o f the p h y s i c a l p r o p e r t i e s o f the asteroidal population. T h e U B V l i g h t c u r v e s m a y be u s e d to d e t e r m i n e spin periods, pole o r i e n t a t i o n s , and s h a p e s o f the asteroids. P h o t o m e t r i c o b s e r v a t i o n s are also useful for other p u r p o s e s , such as d e t e r m i n a t i o n o f the b r i g h t n e s s - s o l a r phase angle relation,
This paper is our report of the photoelectric photometry
2oo H e r s i l i a
o f a s t e r o i d s carried out at the C h u g u e v s k a y a Station o f the K h a r k o v A s t r o n o m i c a l O b s e r v a t o r y . T h e 7 0 - c m teles c o p e w a s u s e d with an u n c o o l e d S-8 p h o t o m u l t i p l i e r ( F E U - 7 9 ) . M o s t o f the data w e r e taken in the V-band o f the standard J o h n s o n U B V s y s t e m . T h e e x c e p t i o n s are 4 V e s t a in 1985 ( B - b a n d ) , 511 D a v i d a ( U B V p h o t o m e t r y ) , and 532 H e r c u l i n a (BV in 1986). The one-channel Kharkov Observatory photometer
]
238 Hypatla
2,1 ,87 511 532 55o 70, 705
214
(o)
0.59
6.421 5.699 8.752
0.07
9.
7.226 7.33 8.9
G. . . . . ia Venetia Dav~da H. . . . ~ina Senta
64
S
0.078
337
C
0.020
0.07
5.130
231
S
0.247
0.15
9.~05
40
S
0.25
ia
333
F
0.019 - 0 . 0 3
139
EMP
0.15
In1: . . . . .
Erminia
8.98~
8.88 8.998
0.20
20.555 8.727
" References: T, Tedesco 1989; Th, Tholen 1989; LM, Lagerkvist and Magnusson 1990; L, Lagerkvist et al. 1989; PW, present work.
Author may be reached via e-mail at: m i c h a s t r ~ p l p u a m l 1.bitnet.
295
0019-1035/92 $5.00 Copyright © 1992 by Academic Press, Inc. All rights of reproduction in any form resserved.
S H E V C H E N K O ET AL.
296 I
I
i
I
I
3.4
Period
xCi,~
"¢i"
0.,
~+
I
5.34~1E
hours
0
3.5 C ~o
× x,
~
,:'s ;> o
x
x -,.~-,.
x ""~Z~SoX,+ o ° ~
"*
'-J -; h'-'xc)
*
.
-i~
~
+
++oo°o+
0
x
x+X
xo
+
,
+
°
x:,O
Xo+~ x
×
3.6
•'r.2x +
~ ×× ~
n~ Date
3.7
=
I
I
o
=
0.2
I
Feb 2 5 . 0
-~xx -'.x+ x ~' x X×x x ~ x :,~-b'b Xx~
M a g n l t u d c ~tft
+
19el
4.2
V
0.027
0
1 9 8 1 Feb 25.9
44
Y
0.016
~"
19~i Feb 2 7 . 9
5.1
V
×
121
5 4
V
=
0,4
a
x +x
Feb 2 8 9
I
I
0.002 -0.023
I
0.6
=
I
0.8
1
Rotational phase FIG. 1.
4 Vesta. Zero phase at 1981 Feb 26.0000 corrected for light time.
!
Period
=
5.34212
00
0
hours
4.7
.lo
¢1
oc~
+ O0
4.8
% +
dR
cQ
0
"o ¢3
©
0
c~ +4+
4.9
Date
I
I
o
I
0.2
=
I
0.4
I
I
0.6
a
1985 May
9.8 i2.4
B
0
1 9 8 5 M a y 11.8 t 3 . 2
B
=
I
0.8
Rotational phase FIG. 2.
Ma~nltuclc shlR
~-
4 Vesta. Zero phase at 1985 May 10.0000 corrected for light time.
0.315 -0.024
|
I I
P H O T O M E T R Y OF S E V E N T E E N A S T E R O I D S I
I
I
I
I
Period
7.4
7.5 "0
297
=
I
6.42142
q<3 +
hours
~+
~+0 o
7.6
+
¢1
++
O
::> "0
0
7.7
o
0
0 0
o~
'0
c~.~ ~.
® o
°s /e
o
CO + ++
+ O
%
7.8
+ Date
7.9
M a g n i t u d e shIR
a
"Jr 1987 Oct. 20.0 21.0 (D 1987 Oct. 20.9 20.7 ~" 1987 Oct 28.9 i{].2
I 0
I
I
I
0.2
I
0.4
-0.003
V
-0.003 0.073
V
i
I 0.8
0.6
Rotational FIG. 3.
i
I
V
i I
phase
44 Nysa. Zero phase at 1987 Oct 23.0000 corrected for light time.
i
i
i
i
i
7.1 Period
6.42142
=
hours
+
7.2
+
"0
7.3
**+ +
+
++
¢,+ 2r
C~- + ,~, + +
y-
+
+
b
~+
7.4
0
+ 0
4~
+
+
0
-I,:3000
q)
cr~
O
O O
+
+
++ Q
+ ++ +
O+
+~o
dr
+O
~0+++
7.5 Date
a
Magnitude
+ 1987 Dec 9.7 4.2 (D 1987 Dec 18.7 8.7 "~ 1987 Dec 23.6 10.2
7.6 I
0.2
I
I
I
0.4 Rotational
FIG. 4.
I
0.6
I
I
0.8
phase
44 Nysa. Zero phase at 1987 Dec. 17.0000 corrected for light time.
V
shift 0.090
1/'
-0.010
V
-0.087
298
SHEVCHENKO
ET AL.
TABLE II Aspect Data, Photometric Results, and Comparison
Stars
Comparison
UT
x
Date
6
r
A
(x
Am
V(1.u)
R.A.
(1950)
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
152.0
9.4
2.379
1.398
4.2
0.13
3.46
81/02/25.9
151.7
9.4
2.378
1.398
4.4
0.13
3.47
81/02/28.0
151.2
9.5
2.376
1.399
5.1
0.13
3.48
81/03/~
1.0
150.9
9.5
2.375
1.399
5.4
0.13
3.50
85/05/
9.9
203.5
11.8
2.191
1.247
12.4
0.13
4.59’
203.1
11.6
2.190
1.255
13.2
0.13
4.62’
43 4.8
66.9
77.3
Obsf
(10)
(11)
(12)
6.15
Mi
0.4
-5.5
(9)
2.543
1.692
2.188
HO 90472 II
Mi
,,
,,
II 13
Mi
45.4 HD
Mi
1
47
119749
9.65’
V
9.36’
S,V
K,V
Ariadne
44 87/10/20.0
V
Vesta
81/02/25.0
90/01/
Dec. (1950)
4
85/05/11.9
stars
11.9
>0.08
6.94
4
19.5
21
24
0.05
7.45
5
06.9
17
25
11.84
Nysa 1.430
21.0
0.39
,I
II
7.46
S S
77.4
-5.5
2.187
1.419
20.7
0.39
77.3
-5.7
2.176
1.342
18.2
>0.29
7.38
5
07.4
17
07
10.65
S.V
69.8
-5.8
2.125
1.147
4.2
0.28
7.12
4
35.6
lb
15
10.82
K.S
87/12/18.8
67.6
-5.5
2.116
1.161
8.7
0.27
7.21
4 27.1
lb
02
7.75
K.S
87/12/23.7
67.7
7.29
U
22.5
lb
08
10.48
87/10/21.0 87/10/28.9 87/12/
9.8
-5.4
2.111
1.168 45
86/01/31.9
113.3
-4.7
2.797
128.6
0.5
6.4
0.11
7.62
7 36.9
lb
46
9.83
14.1
0.07
8.17
8 44.7
18 35
10.05
1.846
2.354
>O.l
1.484
91/09/11.0
10.3
-2.7
2.904
1.952
7.9
>0.2
8.74
10.1
-2.7
2.903
1.947
7.6
>0.2
8.68
91/09/14.0
9.8
-2.6
2.900
1.937
6.9
6.8
91/11/
1.8
5.4
-2.3
2.871
1.881
2.3
4.7
-1.6
2.865
1.885
4.5
1.2
-1.9
2.840
1.986 151
90/04/20.9
204.4
2.2
2.517
87/08/26.9
341.8
9.9
2.976
87/08/27.9
341.6
10.0
12.1
2.977
206
0.30
>0.18
8.66
0
41.7
1 37
12.28
Mi,K
0
40.3
1
28
10.78
M.V
0
M.K
8.34
0
23.5
04
11.07
s.v
0.30
8.52
0
20.0
-0
29
11.15
C,K
>O.l
8.95
0
07.7
-1
18
11.99
S.U
>O.ll
9.50
13
32.1
-7
15
12.09
K.M
Abundantia
1.515 lb5
K,S
Klymene
91/09/12.0
91/10/
S,V
Angellna
104
91/10/11.9
S
Eugenla
64 87/12/26.0
10.2
2.4
Loreley 1.984
4.5
0.08
8.04
22
37.9
2
02
10.65
S.V
1.983
4.3
0.08
8.06
22
37.3
2
02
10.19
s
43.1
-13
46
11.08
M.S
-13
41
10.91
M.S
Hersilia
91/05/13.9
236.8
5.9
2.836
1.832
2.7
jO.18
7.43
15
91/05/14.9
236.6
5.9
2.837
1.830
2.4
>0.18
7.43
15 42.7
299
PHOTOMETRY OF SEVENTEEN ASTEROIDS TABLE I I - - C o n t i n u e d (1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
238 Hypatia 88/08/15.9 326.9 12.1 2.795 1.798 4.6
> 0 . 0 9 8.24
21 40.2
-1 06 11.89 S,V
88/08/16.9 326.6 12.1 2,794 1.797 4.5
> 0 . 0 9 8.24
21 39.7
-1 17
88/08/19.9 326.0 11.9 2.791 1.794 4.3
> 0 . 0 9 8.28
21 37.0
-1 34 10.91
S,U
88/08/20,9 325.8 11.8 2.790 1.793 4.3
> 0 . 0 3 8.30
21 36.4
-1 47 12.34
S
88/08/21.9 325.6 11.8 2.790 1.793 4.4
> 0 . 1 0 8.22
21 35.3
-1 53 12.14 K,S
9.88
L,S
241 8ermanla 91/10/12.0
56.4
5.7 2.869 2.025 1 2 . 7
> 0 . 1 3 8.33
3 31.2
24 58 I i . 0 0
C,K
91/10/12.8
56.4
5.7 2.869 2.019 1 2 . 5
>0.06 - - -
91/10/16.0
56.0
5.7 2.872 1.997 1 1 . 4
>0.08 - - -
3 29.6
24 52
---
M,S
3 28.8
24 48
---
M,K
91/11/ 2.9
52.9
5.6 2.888 1.917 5.0
>0.1
7.87
3 16.0
23 54
9.15
C,S
86112/ 9.9
81.5 -9.7 2.497 1.521
0.05
8.53
5 25.5
13 31 10.37 S,V
487 Venetia 3.9
511Davlda 87/04/24.9 187.9 22.1 3.272 2.386
9.8
0.25
6.88
....
6.72
13 04.5
17 14 11.74 S,V
3 53.6
10 53 10.26 S,V
532 Hercullna 86/02/ 8.8
87105127.9
58.3 -9.1 2.815 2.487 20.3
182.1 2 2 . 3 2 . 3 1 2
1.700 23.5
>0.20
---
0.35
10.00
> 0 . 2 5 9.94
12 4 4 . 0
19 31
S,V
0 12.1
20 53 1 1 . 3 7
K,M
0 03.1
20 30 10.44 C,Kl
550 5 e n t a 91/09/
4.9
11.1
17.7 2.121
1.217
15.6
91/09/15.9
9.1 18.4 2.140 1.189 11.6
91/10/ 1.8
5.4 18.5 2.169 1.197 8.5
91/10/ 8.8
4.0 18.0 2.183 1.221
91/10/ 9.9
....
9.84
23 49.4
19 O0 12.10 C,S
9.6
> 0 . 2 7 9.84
23 44.4
18 02 12.67 K1,S
3.5 18.0 2.185 1.225 9.7
> 0 . 2 5 9.85
23 43.7
17 54 12.11
> 0 . 1 2 7.04
22 49.5
14 52 11.18 B,D
> 0 . 0 9 8.79
1 23.2
27 11 13.02 M,S
K,M
704 Interamnia 90/08/ 1.9 349.6 24.1 2.680 1.874 15.7 705 Erminla 90/10/18.9
29.8 17.0 2.875 1.910 6.0
N o t e . * denotes brightness in the standard B-band. " Key to observers: S, Shevchenko; C, Chiornij; K, Krugly; L, Lupishko; M, Mohamed; V, Velichko; Mi, Mich~owski; D, Dovgopol; P, Pluzshnik; KI, Kalashnikov; B, Belskaya.
not matter so much. The standard deviation for one measurement in the range V = 10-11 mag is equal to 0.015 mag for an integration time o f 30 sec (Lupishko et al. 1986, V e l i c h k o 1991). We normally obtained 20 to 70 data points per observing night. A nearby c o m p a r i s o n star o f roughly solar color w a s measured for each asteroid at similar frequencies (each m e a s u r e m e n t o f an asteroid had a corresponding comparison-star m e a s u r e m e n t within a few minutes o f time). Most o f the c o m p a r i s o n stars were calibrated to the standard s y s t e m using standard stars with asteroid-like
colors chosen from Blanco et al. (1968), Kazanasmas et al. (1981, 1982), or Landolt (1973, 1983). Most of the observations were made between 1985 and 1991. The only exceptions are data for 4 Vesta from 1981, carried out at Torufi Astronomical Observatory (Poland) with a 20-cm refractor and an uncooled RCA 1P21 photomultiplier. In addition to this article, a data file containing the original observations is available. This can be obtained through e-mail by sending a request to one of the authors (T. Michalowski).
300
S H E V C H E N K O ET AL. .
.
.
.
I
.
.
.
.
}
.
.
.
.
i
.
.
.
.
)
.
.
.
.
}
6.5
.
.
.
H
=
692
C
:
0 59
I
.
IV
I
I
8
III
~>. "o
8.2
0
8.4 7.5
U}
8.6 . . . .
t
. . . . . . .
5
.
10
.
,
.
.
.
.
i
15
,
.
.
•
20
30
FIG. 7.
44 Nysa.
We have determined the synodical periods and parameters of the HG magnitude system (see Bowell et al. 1989) if the lightcurves have allowed this. OBSERVATIONS
We observed 17 asteroids on 46 nights. These asteroids are listed in Table I. Column 2 gives their diameters according to Tedesco (1989). Their taxonomic types (Tholen 1989) are given in column 3. The G values of the HG magnitude system are in columns 4, 5, and 6 and were taken from Tedesco (1989), Lagerkvist and Magnusson (1990), and the present work, respectively. The periods
•
I
. . . .
i
. . . .
I
. . . .
I
.
.
.
I
.
7.4
~++++ ; ~ 4 ~ - ~
7.6 +
+++4-
+ +++4- +
O "O
7.8
e,,
i
19
. . . .
i
20
. . . .
I
,
,
21
,
,
I
22
,
,
•
•
i
23
1986 Jan 31 FIG. 6.
I
t
I
24
,
I
26
1987 Dec 25
Solar phase angle oz FIG. 5.
,
22
. . . .
,
25
45 Eugenia. H o u r s of U T corrected for light time.
64 Angelina. H o u r s of U T corrected for light time.
of rotation from Lagerkvist et al. (1989) are in column 7, while in column 8 we give the periods determined by us. Table II contains the aspect data for each asteroid on each night of observation. The asteroid names are listed as subheadings. The first column is the date of the observation, given to the center of the observed lightcurve. Columns 2 and 3 are the 1950 ecliptic longitude (X) and latitude (/3) of the asteroid, referring to the time in column I. Columns 3 and 4 are the distances in astronomical units from the asteroid to the Sun and the Earth, respectively, and column 6 is the solar phase angle (a). Columns 7 and 8 give the amplitude (Am) and reduced V(l,a) magnitude of the maximum light observed during the night, respectively. Columns 9, 10, and 11 refer to the comparison star, giving its 1950 right ascension and declination (for two stars these are replaced by the catalog numbers) and its V magnitude, respectively. The last column gives the codes for the observers, which are explained at the end of the table. Our observations are mainly presented as composite lightcurves which are constructed according to the procedure described by Magnusson and Lagerkvist (1990). Data are composited with the period shown in the figure. The points from different nights are shown by different symbols. Vertical shifts of the individual nights are made in order to obtain a good fit. The values of these shifts are displayed in the figure. The abscissas are the rotational phase with the zero point corrected for light-time as shown in the figures. The magnitudes have been reduced to unit heliocentric and geocentric distances and refer to Johnson V (except Vesta in 1985). If we have only one lightcurve for a given asteroid then the abscissas are the hours of UT corrected for light-time. We have obtained very short lightcurves for Asteroids
301
PHOTOMETRY OF SEVENTEEN ASTEROIDS I
I
I
I
I
I
8.5 =
Period
8.98400
hours
×
8.6
x
× ,~.
x
A
¢)
o5.OO ~ o *~x
8.7
8.8
x × ~ "~
~ o+
L~
"1o
~,~ + ~ ,~++~
a) o
"o ¢) a~
A
8.9
Date ¢~
9.1
I
,
I
,
0
1991
Sep
10.9
"/.9 7.6
0
1991
Sep
12.0
V'
-0,096
Y
-0.045
X
1991 Sep 13.9 1 9 9 1 Oct 8 . 7
6.9
Y
-0.019
2.3
V
0.247
A
1991 Oct 11.8
4.5
Y
,C~
1 9 9 1 Nov
12.1
V
1.8
,
I
0.I16 -0.291
,
I
0.4
0.2
Magnltude shlR
a
Jr
I
0.6
0.8
Rotational phase 104 Klymene. Zero phase at 1991 Sep 29.0800 corrected for light time.
FIG. 8.
43, 51 l, and 532, so we decided not to publish these figures in this paper. Those who want to use them can get them in machine-readable form either from us or from the next issue of the Asteroid Photometric Catalogue. We have been able to determine the phase curves for three asteroids: 44,104, and 550 (Figs. 5, 9, and 17, respectively). The method of Lagerkvist and Magnusson (1990) was used. Our results are presented as plots of reduced . . . .
,
. . . .
,
. . . .
,
. . . .
,
. . . .
,
V magnitude of the second Fourier component maxima against the solar phase angle. 4 Vesta
This asteroid is the best-observed asteroid reported in the literature. The Asteroid Photometric Catalogue-hereafter referred to as APC (Lagerkvist et al. 1987, 1988, and 1992a)--gives information on 110 lightcurves taken
. . . .
H =
8.11
G =
0 07
9.2
@
i=
9.4
+
> 9.6
'0
+
+
++
,
I
I
++
+
+
+ + %
+
++
++++
g) 0
@
9.8 9.5
. . . . 0
, 5
. . . .
, 10
•
i '
'
. . . .
' 15
i 20
. . . .
i 2.5
I
. . . .
21.5
30
Solar phase angle o{ FIG. 9.
104 K l y m e n e .
I
I
I
I
I
22
I
.
.
.
22.5 1990
FIG. 10.
I
.
I
23
.
.
.
.
23.5
Apr 20
151 Abundantia. Hours of U T corrected for light time.
302
SHEVCHENKO i
44 Nysa
I
Period =
7 . 2 2 8 hours
7.8 "0 =
E
©
;>
8.2
Date +
0
Magnltude V V
1907 Aug 26,8 1987 Aug 27.6
0.004 -0.009
8.4 I
,
0
I
,
I
0.2
,
0.4
I
i
I
0.6
,
I
0.8
1
Rotational phase FIG. 11. light time.
i
I
i
This asteroid has previously been observed during 14 apparitions (1949-1986). We observed Nysa during six nights in October-December 1987, while the phase angle changed in the range from 4° to 21 °. Our observations are presented in Fig. 3 (for large phase angles) and in Fig. 4 (for smaller ones). Note the increase in the lightcurve amplitude from 0.27 to 0.39 mag for these phase angles. We determined the G-value to be equal to 0.59 (see the phase curve in Fig. 5). Harris et al. (1989) reported that when they fitted their 1986 lightcurves to the HG magnitude relation, they yielded the slope parameter G = 0.51. They also observed a remarkable opposition spike for this asteroid. 45 Eugenia
165 Loreley. Zero phase at 1987 Aug 27.0900 corrected for
I
7.2
ET AL.
I
Period
i
?.330 houra
=
APC reports observations from eight oppositions. Our lightcurve (Fig. 6) supplements observations carried out in October 1985 (four nights) and on 17 January 1986 (see APC). 64 Angelina
=
7.4 ~.O
0
0
o
7.6
0
oOooO o o ® 0
cP Date
@
i
0
,
I
0.2
0
104 Klymene
IVlagnttude shift
+ 1991 May 13.8 © 1991 May 14.9
7.8
This asteroid has previously been observed during three oppositions. Our lightcurve (Fig. 7) is a supplement of those observed during 11 nights in January-March 1988 (APC).
0
i
V V I
0.4
0,006 -0.014 i
I
0.6
t
I
0.8
i
I
1
Rotational phase FIG. 12. light time.
206 Hersilia. Zero phase at 1991May 14.0900corrected for
during 17 oppositions. We present our lightcurves from two apparitions--1981 and 1985 (B-lightcurves). Because of the very small range of solar phase angles in our lightcurves we cannot make the phase curves. Our lightcurves are presented in Figs. I and 2. There are no previous 1981 lightcurves in APC, but our observations were taken at similar aspects to those in the 1951/52 opposition (see APC). In 1985, Vesta was also observed by others during three nights in April (APC). 43 Ariadne This asteroid has been observed during seven oppositions. Our lightcurve, consisting of 10 points, spans only 2 hr and supplements the observations made in November 1989 (see APC).
This asteroid was previously observed only during one night in 1977 and its period was not known with good accuracy (see Table I). Our six nights of observations (Fig. 8) in September-November 1991 allowed us to determine the period of rotation (8.984 + 0.001 hr) and the phase curve (G = 0.07--see Fig. 9). Lagerkvist and Magnusson (1990) found the average slope parameter for lowalbedo objects to be 0.09, so our G value is more consistent with typical values for C-type asteroids than that given by Tedesco (1989)--see Table 1. 151 Abundantia No previous lightcurve observations of this asteroid have been published. We present only a short lightcurve observed in 1990 (Fig. 10). 165 Loreley There are lightcurves from three oppositions in APC. Loreley, contrary to most asteroids, shows three maxima and three minima during its rotational period. We observed Loreley during two nights in 1987 (fourth apparition), but our observations do not cover the whole period (Fig. i I).
303
P H O T O M E T R Y OF S E V E N T E E N A S T E R O I D S I
I
I
1
Period =
8.88000 hours
8.2 4~
0
o +~q~
+ +
~+
+
+
+%,+
o
~
A+.
o
+
o
. x~.,~o
8.3
o°e
o
o
~+~
o x
.
+
xX'x
~,. "
+
o
~
A ~" ~
0
Jr o X
I
,
0
I
I
0.2
0.4
,
I
JO x~^'~r '
CO
,,~
xz~ 0 0 0
,~,~. ~
'~"
at
Date
8.4
~ ~
4.8 4.5
V Y
1988 Aug 19.8 1 9 8 8 /tug 2 0 . 9 1 9 8 6 /tu¢ :~t.8
4.3 4.3 4.4
Y Y Y
x
I
0.001 0008 -0.028 0013 0.012 ,
I
0.8
0.6
0
,.o+
Mag~tltude
1 9 8 8 Aug 15.8 1988 ~ 18.9
,
0 x"
x
1
Rotational phase 238 Hypatia. Zero phase at 1988 Aug 18.0000 corrected for light time.
FIG. 13.
i
7.8
i
Period -
8.998 h o u r s
o
-o
E o
8.2
8.2
o
Ii 8.4 8.4 e~
E I 0
,
I 0.2
i
I 0.4
,
I 0.6
i
I 0.8
I
Rotational phase Date
Magnitude shift
+ 1991 Oct 12.0 0 1991 Oct 12.8 1991 Oct 16.0
V -0.232 Vrel. 6.520 Vrel. 8.943
x
V
1991 N o v
2.8
~
8.6
'ID o
8.8
20
0.230
FIG. 14. 241 Germania. Zero phase at 1991 Oct 18.0000 corrected for light time.
22 1986 Dec
FIG. 15.
9
487 Venetia. Hours of UT corrected for light time.
304
SHEVCHENKO
I
ET AL.
I
9.1
Period
=
hours
20.55500
+
+++
9.2
XXX "H-T+ + +
9.3
'
.*A
xx× x~.×
+ +
A " ~ x
x xxx
+
9.4
o~
x xX xX× x
e
> 'lO
~××
9.5
O "O
©
9.6
I~tte q0
9.7
a
1991 Sep 1991 Sep
"~ 1991 Oct X 1991 ~ A
9.8
I
~nltudc
4.9 1 5 . 6 15.9
11.6
'¢
-0674
8.5
Y
9.6
Y
-0.584 -0604
1991 Oct
9.8
9.7
¥
-'0.~8
*
I
z
I
0.8
phase
550 Senta. Zero phase at 1991 Sep 26.0000 corrected for light time.
hr) which was consistent with the previously published one (see Table I). Lagerkvist et al. (1992b) observed this asteroid in February 1991 and found its rotation period to be 8.86 hr, which is in agreement with ours. 241 Germania
238 Hypatia
APC reported observations in 1981. Our lightcurves (Fig. 13) allowed us to determine the period (8.88 -+ 0.02
.
*
0.6
Our lightcurves from 1991 are the first observations reported for Hersilia (Fig. 12). We determined the period of rotation to be 7.33 _+ 0.03 hr.
.
I
0.4
206 Hersilia
.
~r
1.7
Rotational
.
-0803
88
0.2
FIG. 16.
ahlfl
V
I
.
.
.
.
~
.
.
.
.
I
.
.
.
.
J
.
.
.
.
r
H = C =
9
.
.
.
No previous lightcurve observations have been published in APC. We observed Germania on four nights in October-November 1991 (Fig. 14). The synodic period is found to be 8.998 _+ 0.003 hr. Because of very short runs
.
927 0 20
6.8 q~
\ ~r-~m 9.5
\ 7
\ \.
m
>
++++
+ +
7.2 t,,.* 7.4 t0.5 . . . .
i 5
. . . .
, . . . . 10
i . . . . 15
J 20
. . . .
i . . . . 25
I
21
30
Solar phase angle o¢ FIG. 17.
550 Senta.
.
.
.
.
I
.
1990
FIG. 18.
.
.
.
I
22
23 Aug
.
.
.
.
I
24
!
7041nteramnia. Hours of UT corrected ~ r l i g h t t i m e .
305
PHOTOMETRY OF SEVENTEEN ASTEROIDS
550 Senta 8.6 ¢ cl
+
8.8
~+
,4-
+~+
++ +
+
+
,
+
+4+
o
Our 1991 lightcurves (Fig. 16) are the first published ones for this asteroid. We have determined the rotational period to be 20.555 --- 0.005 hr. In spite of a small range of solar phase angles, we decided to determine the slope parameter and found G = 0.20 (see the phase curve in Fig. 17). 704 Interamnia
a..
9.2
I
I
18
i
I
1990
FIG. 19.
i
20
I
22 Oct
i
I
The APC gives information about lightcurves from three oppositions. Our incomplete lightcurve (Fig. 18) is the fourth apparition in which Interamnia was observed photoelectrically.
24
18
705 Erminia. Hours of UT corrected ~ r l i g h t t i m e .
during each night, we realize that other periods are still possible (for example, 12.73 hr). Lagerkvist et al. (1992b) observed Germania in August 1990 and suggested the most likely rotation period was about 15.2 hr, but they were unable to derive a unique solution. 487 Venetia
Our 1986 lightcurve (Fig. 15) spans only 5 hr, so we cannot use it to determine the synodic period. Venetia was observed in 1984 (see APC) but these lightcurves are very incomplete, too. 511 Davida
This is a very well observed asteroid. APC reports 48 lightcurves from 12 oppositions. Our observation spans a period of 2 hr and seems to be the only lightcurve from the 1987 apparition. We have also determined B - V = 0.70 mag and U - B = 0.37 mag, which are in agreement with those given by T e d e s c o (1989). 532 Herculina This asteroid has previously been observed during s e v e n a p p a r i t i o n s . H e r c u l i n a h a s v e r y u n u s u a l lightc u r v e s . T h e y e x h i b i t t w o m a x i m a a n d t w o m i n i m a in s o m e oppositions and only one maximum and one minimum in o t h e r s d u r i n g t h e s a m e r o t a t i o n p e r i o d . O u r r e l a t i v e p h o t o m e t r y l i g h t c u r v e t a k e n o n 27 M a y 1987 c o n t a i n s o n l y eight points, but many other observations were carried out in J a n u a r y - M a y 1987 ( s e e A P C ) . W e a l s o r e p o r t t h a t o n 8 F e b 1986 t h e V b r i g h t n e s s o f H e r c u l i n a w a s 6.72 m a g ( s e e T a b l e II) a n d B - V = 0 . 7 9 m a g .
705 Erminia
Our 1990 observation (Fig. 19) is the first published lightcurve for this asteroid. It seems to be only a part of the rotation cycle so we cannot determine the period of rotation. ACKNOWLEDGMENTS We thank C.-1. Lagerkvist for his valuable comments, P. Magnusson for his useful suggestions and his help in drawing all the figures, and I. N. Belskaya, E. Pluzschnik, N. I. Koshkin, and A. V. Kalashnikov for their assistance during the observations of the asteroids 704, 4, 104, and 550, respectively. T.M. is indebted to the Swedish Institute for having supported his stay at the Uppsala Astronomical Observatory, where this paper was prepared for publication. REFERENCES BLANCO, V. M., S. DEMERS, G. G. DOUGLAS, AND M. P. FITZGERALD 1968. Photoelectric Catalog o f Magnitudes and Colors o f Stars in the UBV System. Publ., U.S. Naval Obs., Washington. BOWELL, E., B. HAPKE, D. DOMINGUE, K. LUMME, J. PELTONIEMI, AND m. W. HARRIS 1989. Application of photometric models to asteroids. In Asteroids H (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 524-556. Univ. of Arizona Press, Tucson. HARRIS, A. W., J. W. YOUNG, L. CONTREIRAS, T. DOCKWEILER, L. BELKORA, H. SALO, W. D. HARRIS, E. BOWELL, M. POUTANEN, R. P. BINZEL, D. J. THOLEN, AND S. WANG 1989. Phase relations of high albedo asteroids: The unusual opposition brightening of 44 Nysa and 64 Angelina. Icarus 81, 365-374. KAZANASMAS, M. S., L. A. ZAVERSHNEVA, AND t . F. TOMAK 1981. Atlas and Catalogue o f Magnitudes o f PhotometHcal Standards. Naukova Dumka, Kiev. KAZANASMAS, M. S., L. A. ZAVERSHNEVA,AND L. F. TOMAK 1982. Atlas o f Photometrical Standards in the Star Areas. Naukova Dumka, Kiev. LAGERKVlST, C.-I., AND P. MAGNUSSON 1990. Analysis of asteroids lightcurves. II. Phase curves in a generalized HG-system. Astron. Astrophys. Suppl. Ser. 86, 119-165. LAGERKVIST,C.-I., M. A. BARUCCI,M. T. CAPRIA,M. FULCHIGNIONI, L. GUERRIERO, E. PEROZZl, AND V. ZAPPALA 1987. Asteroid Photometric Catalogue. Consiglio Nazionale delle Ricerche, Rome. LAGERKVIST,C.-I., M. A. BARUCCI,M. T. CAPRIA, M. FULCHIGNIONI,
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P. MAGNUSSON,AND V. ZAPPALA 1988. Asteroid Photometric Catalogue, 1st update. Consiglio Nazionale delle Ricerche, Rome. LaGERKVlST, C.-I., A. W. HARRIS, AND V. ZAPPALA 1989. Asteroid lightcurve parameters. In Asteroids H (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 1162-1179. Univ. of Arizona Press, Tucson.
LAGERKVIST, C.-I., M. A. BARUCCI, M. T. CAPRIA, M. DAHLGREN, A. ERIKSON, M. FULCHIGNIONI, AND P. MAGNUSSON 1992a. Asteroid Photometric Catalogue, 2nd update. Uppsala Universitet, Uppsala. LAGERKVIST, C.-I., P. MAGNUSSON,H. DEBEHOGNE, M. HOFFMAN, A. ERIKSON, A. DE CAMPOS, AND G. CUTISPOTO 1992b. Physical studies of asteroids XXV: Photoelectric photometry of asteroids obtained at ESO and Hoher List Observatory. Astron. Astrophys. Suppl. Set'.. in press. LANDOLT, A. 1973. UBV photoelectric sequences in the celestial equatorial selected areas 92-115. Astron. J. 78, 959-1020.
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LANDOLT, A. 1983. UBVRI photometric standard stars around the celestial equatorial. Astron. J. 88, 439-460. LUPISHKO, D. F., F. P. VELICHKO, AND V. G. SHEVCHENKO 1986. Asteroid 1627 Ivar. UBV photometry, period and sense of rotation. Kinem. Phys. Celest. Bodies 2, 39-43. MAGNUSSON, P., AND C.-I. LAGERKVIST 1990. Analysis of asteroid lightcurves. I. Data base and basic reduction. Astron. Astrophys. Suppl. Set'. 86, 45-51. TEDESCO, E. F. 1989. Asteroid magnitudes, UBV colors, and IRAS albedos and diameters. In Asteroids 11 (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 1090-1138. Univ. of Arizona Press, Tucson. THOLEN, D. J. 1989. Asteroid taxonomic classifications. In Asteroids I1 (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.), pp. 1139-1150. Univ. of Arizona Press, Tucson. VELICHKO, F. P. 1991. Determination and Analysis o f the Rotational Parameters ¢~fAsteroids. Ph.D. thesis, University of Kiev.