SPACE DISTRIBUTION OF STARS AND DIFFUSE MATTER IN THE REGION OF IC 1396 ABSTRACT Space distribution of stars and the interstellar absorbing medium have been investigated in a field of 19.5 square degrees containing the galactic cluster IC 1396 by means of objective prism spectral classification and photographic UBV photometry. This open cluster is a central region of the large OB association Cep OB2 and the field itself is the densest part of the association. Distribution of the absorbing material is very irregular in the region. The average absorption at the distance of the association is 1.5m. In addition to the earliest type stars, late B and early A stars also show some concentration at the distance of the association. INTRODUCTION OB associations are known to be groups of the earliest type stars associated with a large amount of interstellar gas and dust. They are considered to be places of star formation. OB stars within an association probably do not form a gravitationally bound group; they seem to expand (Ambartsumian, 1949). It is natural to suppose that OB associations contain stars of lower mass too, for they may arise during the same processes as OB stars. However, large volumes and low spatial densities of the associations make it difficult to find the possible fainter association members. It would be interesting to investigate what kinds of stars other than OB stars originate from OB associations and what sort of relationship exists between space densities and kinematics of different type of stars within an association. The answers to these questions might well help us to understand the processes by which associations come into being. This is of special interest in the case of the local spiral arm which is probably not a density-wave arm (Lin et al. 1969) so there must be a triggering mechanism of star formation different from the galactic shock accompanying the density wave. The present work is based on the observational material gathered from the field around IC 1396 in the period 1969-1972 at Konkoly Observatory. The aim of this study is to search for stars having lower absolute magnitude than OB stars in the association Cep OB2 by investigating the stellar space density along the line of sight in the direction of the association. Association Cep OB2 lies near the outer edge of the local spiral arm. Its galactic coordinates are: l=97deg - 107deg; b=+2deg - +8deg. It contains two galactic clusters: IC 1396 and NGC 7160. IC 1396 is an O-type cluster (Markarian, 1951) embedded in a large HII region (Markarian, 1957); NGC 7160 is a very small B1 type cluster (Markarian, 1953). These clusters seem to be the centres of the expansion (Ambartsumian, 1959). The average distance of the association from the Sun is 830 pc (Simonson, 1968). Because of the large dimensions and low spatial density of the stars its structural investigations in the optical wavelengths were restricted to the most luminous stars. I have tried to extend the study to the fainter stars in the densest part of the association. The dark material is concentrated in the same volume as the association stars so it reduces the limiting distance of the study. The observational material available here allows a rough mapping of the space distribution of the absorbing clouds as well as the plotting of the distribution of different type stars in the direction of this part of the association. OBSERVATIONAL DATA a) Spectral classification Spectral classes of stars up to 13m in B colour have been derived from objective prism spectra obtained from four objective prism plates. These plates were taken with aid of the 60/90/180cm Schmidt telescope at Konkoly Observatory using an objective prism giving a dispersion of 580 A/mm at H_gamma. One exposure was taken on Kodak OaO plate with an exposure time of 24m, and three were taken on Kodak IIIa-J plates with the exposure times 120m, 96m and 60m. The widening was 18" on each plate (i. e. 0.16mm). Classification criteria are virtually the same as those described by Nassau and Seyfert (1946). The number of classified stars is 843. Sharpness of the classification criteria necessitates a dividing of classified stars into the following groups: earlier than B3; B3-B7; B8-A1; A2-A6; A7-F1; F2-F8; G0-G8; K-M. The numbers of stars in each of the different spectral groups are given below: earlier than B3 38 B3-B7 63 B8-A1 203 A2-A6 112 A7-F1 75 F2-F8 151 G0-G8 81 K0-M0 120 In principle, it is possible to distinguish the different luminosity classes of G-K stars at such a dispersion (Seitter, 1975) but as most K stars are between 7-9m they are somewhat overexposed on our plates. Because of this, their two-colour diagrams and distance modulus - colour excess diagrams were used estimating their luminosity classes (see below). b) Photographic photometry UBV photographic magnitudes of stars having objective prism spectra have been determined. Five plates were taken in each colour. The plate - filter combinations and exposure times were the following: plate filter exposure time U Kodak 103a-O Schott UG1 2mm 10m B Kodak 103a-O Schott GG13 " 4m V Kodak 103a-D Schott GG14 " 4m The photometric scale based on photoelectric magnitudes of 14 stars of the cluster IC 1396, was determined by B. A. Balazs at Kitt Peak National Observatory in 1967-68 using 36 and 16 inch telescopes. The transformation equations between the instrumental and international colour systems are the following: V_instr = V + 0.07(B-V) - 0.07 B-V_instr = 1.04(B-V) - 0.03 U-B_instr = 0.91(U-B) - 0.11(B-V) + 0.01
Figure 1.
The plates were measured using the Becker type iris photometer of the
Konkoly Observatory. Mean errors of the photometry: +-0.06m for both V
and B; +-0.08m for U. These errors are independent of the magnitude. In
addition to these random errors the ultraviolet filter had a field error
in a restricted area. Figure 1 shows the distribution of the stars of different
spectral groups as a function of the apparent B magnitude. A comparison of
the present spectral classification with the HD spectral types can be seen
in Fig. 2.
Figure 2.
INTERSTELLAR REDDENING AND ABSORPTION
Apparent stellar density strongly changes within the field presumably
due to dark foreground clouds. According to the surface stellar density
the field can be divided into six parts (Fig. 3). The surfaces of these
parts (A), the number of stars (N) and the surface stellar densities
(sigma) are given in the following table:
Part A(sq.deg) N sigma(star/square degree)
1 2.3 94 40.84
2 5.3 148 27.92
3 1.6 85 53.12
4 2.0 62 31.09
5 5.8 359 61.81
6 2.6 90 34.61
Figure 3.
Distance modulus - E_B-V colour excess diagrams have been drawn for each
part separately. This has been done using the B0-F8 stars and assuming that
all of these belong to the main sequence (Fig. 4). Absolute magnitudes and
intrinsic colours of the spectral types were taken from Allen (1973). There
is a strong reddening everywhere except in region 5 which contains the cluster
IC 1396. In the region of the cluster the dispersions of the colour excesses
are large; these dispersions are caused by a large number of small dark clouds
having different absorptions (Shajn and Gaze, 1951).
An interesting part of the field is region 3, situated east of the
cluster. In this region the reddening is about 0.8m, as in the almost
starless region 2, but the surface stellar density is nearly as high as
in the region of the cluster.
Figure 4.
In the literature there are different values of the total to selective
absorption for this region. Johnson (1965) found R=5.4 by infrared photometry
of the mu Cephei; in addition, he obtained R=4.8 by applying the variable
extinction method for the neighbouring association Cep OB3. Simonson (1968)
showed that neither of these methods is suitable for determining R in this
region; he also suggested that there is no reason to assume an abnormally high
value of R. The value R=3.0 has been adopted in this work.
Figure 5.
Figure 5 shows the total absorption, a_v as a function of the distance
assuming R=3.0 for each region separately. Except for region 5, there is
a strong foreground absorption everywhere, caused by clouds situated
200-400 pc from the Sun. In the region of the cluster this method gives
only a very smoothed picture of the dark material. The dust clouds seem
to be concentrated between 600-1100 pc and the reddening changes almost
from star to star.
The strong absorption makes possible a rough division of the late type
stars into different luminosity classes (Trumpler and Weaver, 1953), if
they are put onto the y-E_B-V diagrams obtained from the main sequence
stars. According to this estimation 64 G type stars are dwarfs, 14 are
giants; in addition, 27 K type stars are dwarfs and 93 are giants. It is
not possible to give a more accurate estimation of the absolute
magnitudes of these giants as the absorption does not increase beyond
1200 pc; thus, this method gives only a lower limit of their
luminosities and distances.
SPACE DISTRIBUTION OF STARS
Having evaluated the interstellar absorption it becomes possible for one
to solve the convolution equation
A(m)= Integral from -infinity to +infinity D(y) Phi(m-y) dy,
separately for each spectral class. Here A(m) is the number of stars in the
apparent magnitude interval (m - delta m, m + delta m); D(y) is the number of
stars between distance moduli y - delta y and y + delta y; and Phi(M=m-y) is
the luminosity
function of a given spectral and luminosity class. The apparent magnitudes m
and the distance moduli y are corrected for the absorption. To solve the
equation the matrix method described by Dolan (1974) was used. At the absolute
magnitudes of B8-A1 stars the absorption difference between the different parts
of the field may cause noticeable differences between the distance limits in
them. So it is not possible to deal with them together. Since it is only in
region 5 that there are sufficient stars for the reliable evaluation of the
equation, the densities of stars later than B7 have been calculated only for
this part of the field. In the case of stars later than A1 the plate limit is
within 500 pc even at the smallest absorption.
The space distribution of the three spectral groups earlier than A2 are
shown in Fig. 6, 7, 8. Straight lines show the field star densities assuming
that these are functions solely of the distance from the galactic
plane (Allen, 1973). Absolute values of the field star densities have been
estimated in the case of stars earlier than B3 and B3-B7 from the shape of
the density curve, and from van Rhijn's (1955) data in the case of B8-A1 stars.
Density of stars earlier than B3 shows a maximum between 2500 and 3500 pc;
it may well be that these stars form the upper edge of the Perseus spiral arm.
The line of sight goes 300 pc above the galactic plane at this distance. Stars
of the association are concentrated between 600 and 1100 pc. B3-B7 stars also
show a concentration between the same distance limits. It is more difficult
to decide whether or not there is a concentration of B8-A1 stars because the
plate limit is about 1150 PC. With the assumption that the space density of the
field A0 stars is nearly constant at a given galactic longitude and distance
from the galactic equator an extrapolation has been made for its value from
van Rhijn's (1955) data obtained at l=100deg, b=+7deg. The gradient of the
curve indicates that there is a concentration within 1100 PC.
Figure 6.
Figure 7. Space distribution of B3-B7 stars
Figure 8. Space distribution of B8-Al stars. The dashed line indicates
the plate limit.
Space density units are given as stars/10^3 pc^3, Error bars have been
calculated on the assumption that the star number in every field segment
has the statistical error N^1/2 (Dolan, 1974)
Figures 9a, b, and c show respectively the densities of A2-A6, A7-F1 as
well as F2-F8 stars. The density of A2-A6 stars is nearly constant
within the plate limit in this direction, whereas the densities of the
A7-F1 as well as the F2-F8 stars decrease in accordance with other observations
(McCuskey, 1956).
Figures 9a, b, c. Space distribution of A2-A6, A7-F1 and
F2-F8 stars. Dashed lines indicate the plate limit.
There are two possibilities for estimating the distance of K giants assuming
that all they belong to the same luminosity class. on the basis of the
available data, including the literature, it is not possible to decide whether
this assumption is true or not.
The first possibility is a statistical parallax calculation utilizing
the available proper motion data. The results obtained in this way are
independent of the photometry. The SAO Catalogue contains the proper motions
of 36 K type giants of our field. Their apparent magnitudes are between 8.0m
and 9.5m. From these data r=724 pc has been found to be the average distance.
It implies an absolute magnitude M_v=-2.3m, so these stars are bright giants
and they lie almost at the distance of the association.
The other method of distance estimation is based on the assumption that
these stars are of the third luminosity class, like the largest percentage
of the late type giants of the galactic field. Then their absolute magnitudes
are about +1.0m. In this case all these stars are nearer than 500 pc. Their
two-colour diagram (Fig. 10) confirms this assumption as being the average
colour excess in B-V about 0.2m, whereas at a distance 724 pc it ought
to be at least 0.5m.
Figure 10. Two-colour diagram of K giants. The dashed line indicates the
unreddened diagram of the third luminosity class taken from Golay (1974).
These two contradictory results indicate that either the kinematic or
photometric data contain some systematic error, or one of our preliminary
assumptions is not true (in particular, that they do not belong to the same
luminosity class). So neither of the above estimations can be accepted without
exact spectroscopic determination of the luminosity classes.
CONCLUSIONS
The distribution of stars in space shows that not only are OB stars
concentrated at the distance of the association, but later B stars as
well. There are, however, some signs of concentration of B8-A1 stars
too, even though this is not really significant. In particular, the slope
of the density curve shows that concentration does exist within 1100 pc.
In the distribution of stars later than A1 the association cannot be traced
because of the high foreground absorption and the limiting magnitude of the
spectral classification. Due to the high interstellar absorption the study
of B8-A1 stars has been restricted to an area of 5.8 square degrees including
the cluster whose angular diameter is about one degree (Trumpler, 1930;
Collinder, 1931; Markarian, 1951). Investigations of space distribution of
stars in galactic clusters indicate the existence of extended coronae, whose
diameters are 2.5-10 times larger than those of the clusters (Kholopov, 1968).
The central part of a cluster contains the brightest cluster members, whereas
the corona mainly consists of fainter stars. So it is possible that A0 or the
later association members - if they exist - form a gravitationally bound system
as the corona of the IC 1396. Reddish (1967) has found this feature to be true
for the association Cyg OB2; Kholopov (1974) also claims that the expansion is
the property of only the earliest type stars. The surface density of B8-A1
stars in region 5 is nearly constant; their distribution makes it difficult to
recognize the core of the cluster (Fig. 11). This figure shows as well that the
surface density of B8-A1 stars in region 3 is nearly the same as in the region
of the cluster. A0 stars in part 3 have a reddening of about 0.9m, they all
are behind a dust cloud. The constant surface density indicates that the high
concentration of the stars continues in this direction with a dark foreground
cloud in front of it. Nearly in the direction of the axis of this elongated
concentration are the NGC 7160, mu Cephei and numerous bright stars. The whole
association seems to have an elongated shape whose axis inclines to the
galactic plane at 20deg.
Figure 11.
ACKNOWLEDGEMENTS
I wish to thank to Dr L. G. Balazs for discussions and for his valuable
advice. I am grateful to Dr B. A. Balazs that he put the photoelectric
sequences at my disposal.
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Ambartsumian, V. A. 1949. AZh. 26. 3.
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Golay, M. 1974. Introduction to Astronomical Photometry p. 79-80.
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Johnson, H. L. 1965. ApJ. 141. 923.
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Kholopov, P. N. 1974. Astr. Tsirk. 847.
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TABLE
Spectra and UBV data of the survey stars
No. Sp. V B-V U-B remarks
1 A7 10.49 1.05 0.13
2 B8 9.96 0.62 0.12 BD +54deg 2560
3 F0 10.33 0.73 0.02
4 B0 8.89 0.52 -0.68 BD +54deg 2575
5 G0 11.50 0.71 -0.03
6 K2 9.14 1.28 1.19 BD +54deg 2579
7 A5 8.12 0.55 -0.33 BD +54deg 2581
8 K2 8.37 1.62 1.60 BD +54deg 2585
9 B5 9.27 0.42 -0.22 BD +54deg 2587
10 A0 10.14 0.67 0.27 BD +54deg 2589
11 A0 9.60 0.08 0.26 BD +54deg 2598
12 B2 9.04 0.52 -0.44 BD +54deg 2611
13 A0 11.51 0.80 0.63
14 A0 11.29 0.63 0.54
15 B0 8.27 0.74 -0.44 BD +54deg 2607
16 A7 11.42 0.60 0.07 blend
17 A0 11.82 0.74 0.53
18 F6 9.87 0.66 -0.10 BD +54deg 2601
19 A5 8.93 0.57 -0.26 BD +54deg 2593
20 B8 11.08 0.66 0.28
21 A0 11.28 0.99 0.22
22 A0 10.22 1.93 1.66
23 F0 10.04 1.39 0.58
24 A3 8.95 0.43 -0.05 BD +54deg 2573
25 F0 10.73 0.63 0.12 BD +54deg 2569
26 F8 9.62 1.55 0.97
27 B3 11.93 0.65 -0.12:
28 B8 10.96 0.61 0.20
29 A0 10.56 0.69 -0.05 BD +54deg 2556
30 F2 9.48 1.80 1.40 BD +54deg 2554
31 F5 10.30 0.95 -0.02: BD +54deg 2564
32 K5 9.05 2.16 2.28 BD +54deg 2557
33 G8 10.11 0.93 0.16
34 A2 8.93 0.45 -0.25: BD +54deg 2567
35 F8 10.70 0.72 0.03
36 B8 10.46 0.58 -0.17 BD +54deg 2573
37 A4 10.78 0.46 0.25:
38 B8 10.86 0.78 0.12
39 A2 10.53 0.68 0.18
40 A7 10.67 0.72 0.38
41 K0 7.54 1.16 0.43 BD +54deg 2590
42 K0 7.85 1.20 0.45: BD +54deg 2597
43 A0 10.69 0.60 0.18 BD +54deg 2600
44 A5 10.38 0.62 0.46
45 F2 10.64 0.31 0.16 BD +54deg 2605
46 A0 11.04 0.31 -0.07
47 A0 11.81 0.18 0.15
48 A0 10.68 0.44 0.16
49 A0 10.50 0.47 0.18
50 A0 11.54 0.57 0.16
51 B5 9.33 0.49 -0.52 BD +54deg 2610
52 A0 10.89 0.58 0.43
53 A2 10.15 0.70 -0.01 BD +54deg 2608
54 B9 8.14 0.44 0.12 BD +54deg 2606
55 G6 10.64 0.65 0.02
56 G4 9.73 0.75 0.02 BD +54deg 2594
57 B0 10.74 0.64 -0.46 BD +54deg 2592
58 A0 11.24 0.53 0.09
59 F0 11.36 0.66 0.16
60 B2 10.26 0.62 -0.30 BD +54deg 2588
61 B8 11.72 0.88 -0.25
62 B8 11.70 0.60 -0.43
63 B7 10.21 0.49 -0.04 BD +54deg 2578
64 A2 10.73 0.52 0.12
65 B5 10.44 0.37 -0.21
66 F0 11.05 0.91 0.42
67 A0 11.62 0.86 0.24
68 A0 11.38 0.98 -0.11
69 F0 10.60 0.65 0.11
70 K0 7.58 1.21 0.66 BD +54deg 2555
71 A0 11.41 0.83 0.30
72 A7 11.16 0.73 0.23
73 A2 10.54 0.46 0.27 BD +54deg 2552
74 A7 10.68 0.74 -0.06 BD +54deg 2548
75 A0 10.30 0.82 -0.02 BD +54deg 2546
76 F8 10.57 0.88 -0.07 BD +54deg 2549
77 F2 10.55 0.70 -0.01 BD +54deg 2550
78 B9 6.31 0.14 -- BD +54deg 2544
79 A0 10.42 0.80 -0.13 BD +54deg 2539
80 F4 10.86 0.84 -0.20
81 K5 8.88 1.70 0.04 BD +55deg 2585
82 K0 7.99 1.53 1.05 BD +54deg 2538
83 F4 10.46 0.89 -0.06 BD +55deg 2590
84 K2 10.03 1.47 0.31 BD +54deg 2571
85 F0 12.11 0.55 0.05 blend
86 B5 11.36 0.45 -0.23
87 K 8.84 1.36 1.41 BD +54deg 2582
88 F0 10.39 0.54 0.03 BD +54deg 2584
89 K 10.03 1.48 1.51
90 A0 11.12 0.44 0.40
91 F7 11.14 0.90 -0.20
92 G0 9.53 0.76 0.16 BD +54deg 2609
93 A0 11.36 0.22 0.31 blend
94 A0 9.81 0.47 0.35 BD +55deg 2622
95 A2 11.00 0.50 0.33
96 F0 9.47 0.36 -0.08
97 G 10.86 0.79 0.32
98 G8 10.74 0.79 0.14 blend
99 G2 9.80 0.66 0.05 BD +54deg 2612
100 A0 11.90 0.38 0.01
101 B5 7.89 0.38 -0.52 BD +54deg 2589
102 F2 10.70 0.52 0.22 blend
103 A0 9.25 0.27 -0.01 BD +55deg 2610
104 A5 8.95 0.57 -0.09 blend
105 A4 9.90 0.26 0.02 BD +55deg 2602
106 F0 11.02 0.84 -0.18
107 F2 11.20 0.87 -0.30
108 K 9.74 2.07 2.09
109 K5 9.08 2.17 1.92: BD +55deg 2581
110 K0 9.43 1.31 0.69 BD +55deg 2589
111 G8 10.74 0.83 0.54
112 K0 7.72 1.42 1.22 BD +55deg 2597
113 K2 8.86 1.57 1.54 BD +55deg 2598
114 A2 10.71 0.90 0.43
115 K2 9.28 1.64 1.62 BD +55deg 2601
116 B8 11.13 0.60 -0.44
117 B5 10.24 0.35 -0.11 blend
118 B7 10.76 0.48 -0.19 BD +55deg 2606, blend
119 G2 9.47 0.70 -0.03 BD +55deg 2608
120 A0 11.75 0.62 0.53
121 F2 10.80 0.79 0.13
122 G2 10.89 0.63 0.15
123 F0 9.92 0.54 0.15 BD +55deg 2621
124 K0 8.45 1.20 0.74 BD +55deg 2624
125 B6 10.20 0.36 -0.02 BD +55deg 2625
126 A0 11.18 0.48 0.40
127 A2 9.54 0.41 0.33 BD +55deg 2628
128 F5 9.70 0.64 0.00 BD +55deg 2632
129 A0 11.00 0.91 0.42
130 K7 9.25 1.70 1.55 BD +55deg 2635
131 F0 11.35 0.61 0.45
132 A5 10.81 0.47 0.34 BD +55deg 2618
133 F0 10.37 0.66 0.12
134 A0 11.84 0.90 0.50
135 A0 10.27 1.60 1.31 blend
136 F8 10.74 0.68 0.11
137 F5 11.36 0.73 0.12
138 K0 10.43 0.91 -- blend
139 B8 11.41 0.72 0.25 blend
140 G0 11.35 0.91 -- blend
141 G 11.46 2.19 --
142 F8 9.31 0.63 -0.13 BD +55deg 2596
143 F0 11.31 0.74 0.39
144 F0 10.75 0.79 -0.09
145 K2 9.27 1.43 0.04 BD +55deg 2583
146 F0 10.03 0.72 0.08 BD +55deg 2579
147 F0 10.06 0.60 -0.08 BD +55deg 2578
148 A0 7.86 0.59 -- BD +55deg 2576
149 G 11.66 1.01 0.03
150 G 10.46 1.04 0.08
151 F8 9.97 0.62 -0.27 BD +55deg 2574
152 G0 9.01 0.85 0.20 BD +55deg 2577
153 F8 10.10 0.75 -0.06 BD +55deg 2582
154 A3 9.52 0.42 0.15 BD +55deg 2586
155 B8 9.50 0.39 0.14 BD +55deg 2591
156 A0 10.57 0.68 0.08
157 B2 8.97 0.71 -0.38 BD +55deg 2592
158 K0 10.78 1.08 0.36
159 G0 11.35 0.98 -0.12
160 G0 10.56 0.72 0.14
161 K0 9.82 1.04 0.79 BD +55deg 2605
162 F8 10.85 0.98 0.16
163 A0 10.74 0.73 0.54 BD +55deg 2607
164 A0 12.36 0.49 -0.03
165 F2 10.45 0.53 0.15 BD +55deg 2616
166 F8 10.43 0.57 -0.01
167 A2 10.34 0.44 0.50
168 F2 10.70 0.58 0.19 BD +55deg 2619, blend
169 A0 11.02 0.43 0.44
170 F8 11.56 0.76 0.30
171 B8 11.31 0.87 0.20
172 F0 10.28 0.69 0.54
173 F5 10.19 0.65 -0.20
174 F8 10.33 0.95 0.25 blend
175 K0 9.12 1.60 1.19 BD +55deg 2634
176 F2 11.26 0.82 0.41
177 B5 10.31 0.36 0.32 BD +55deg 2559, edge
178 B5 10.92 0.78 0.06 edge
179 A0 11.67 0.86 0.18
180 G 11.92 0.83 --
181 F2 12.60 0.87 0.43 blend
182 K 10.57 1.57 1.28
183 B3 9.23 0.59 -- BD +55deg 2637
184 F2 9.74 0.35 0.19 BD +55deg 2629
185 F5 10.70 0.58 0.25
186 A2 11.15 0.49 0.38 blend
187 A2 11.33 0.54 0.42
188 F8 11.51 1.30 0.29
189 K7 8.39 1.82 1.65 BD +55deg 2620
190 A0 11.80 0.55 0.45
191 F8 11.20 0.74 0.05
192 F2 10.92 0.59 0.05
193 A0 12.63 0.90 0.11
194 F2 10.84 0.60 0.05
195 F8 11.56 0.77 0.00
196 A2 11.03 0.59 0.16
197 F5 10.74 1.60 1.34
198 B2 10.46 0.53 -0.30
199 F8 11.16 0.90 0.30
200 K0 7.62 1.44 1.06 BD +55deg 2595
201 F6 10.27 0.67 -0.07 BD +55deg 2580
202 B8 11.46 0.92 0.17
203 B3 8.62 0.78 -0.48 BD +55deg 2575, blend
204 B3 9.12 0.69 -0.31 BD +55deg 2569
205 F0 9.42 0.49 -0.04 BD +55deg 2568
206 A2 9.07 0.42 0.07 BD +55deg 2560
207 A0 11.16 0.97 0.27
208 F2 10.01 0.56 -0.01 BD +55deg 2584
209 K0 7.77 1.42 1.76 BD +55deg 2587
210 A0 11.36 0.90 0.43
211 A0 9.82 0.94 0.85 BD +55deg 2588
212 F0 11.63 0.86 0.22
213 F5 10.04 0.48 0.03
214 A0 11.79 0.70 0.22
215 F0 11.52 0.63 0.29
216 F2 11.43 0.71 -0.01
217 A5 11.55 0.95 0.35
218 K5 8.94 2.13 2.64 BD +55deg 2600
219 G5 9.47 1.12 0.42 BD +55deg 2604
220 A0 11.47 0.21 -- blend
221 A2 10.46 0.59 0.20 BD +55deg 2609
222 A7 11.63 0.57 0.56
223 A0 8.93 0.35 -0.04 BD +55deg 2613
224 F2 10.16 0.52 0.09 BD +55deg 2615
225 B8 11.04 0.59 0.03 BD +55deg 2626
226 F0 10.67 0.48 0.31
227 A2 11.37 0.57 0.49
228 F2 11.06 0.60 0.14
229 G2 10.48 0.64 0.21
230 A0 11.96 0.34 0.19
231 A2 11.72 0.37 0.04 blend
232 K5 10.71 1.80 1.77 blend
233 A0 12.42 0.11 -- blend
234 A7 10.66 0.40 0.17
235 G2 11.00 0.69 -0.04
236 G5 10.97 0.63 0.16
237 K5 9.22 1.33 0.92 BD +55deg 2633
238 A0 11.53 0.79 0.18
239 A0 11.51 0.57 0.78
240 A0 10.87 1.17 0.84
241 A0 11.04 0.74 0.41
242 A0 11.22 0.65 0.37
243 A7 11.06 0.59 0.40
244 K 10.87 1.30 1.11
245 A2 10.95 0.58 0.48
246 A0 11.08 0.34 0.15
247 A0 11.21 0.26 0.01
248 B2 10.40 0.72 -0.31
249 A0 11.01 0.44 0.35
250 G5 10.70 0.82 0.39
251 F6 10.73 0.78 0.30
252 K2 9.87 1.47 -- BD +56deg 2603
253 F4 10.94 1.04 0.13
254 A0 11.51 0.61 -0.22
255 A2 10.45 0.68 0.44 BD +56deg 2587
256 F8 11.43 0.73 -0.12
257 A2 10.20 0.71 0.25 BD +56deg 2583
258 K0 8.19 1.30 0.89 BD +56deg 2580
259 A0 11.67 0.87 0.58 blend
260 G2 10.95 0.93 0.37
261 F5 10.25 0.67 0.10
262 K0 8.05 1.26 -- BD +56deg 2565
263 A7 10.63 0.81 0.36
264 A0 11.49 0.88 0.55
265 A0 11.34 0.91 -0.05
266 A2 10.67 0.74 0.43
267 A4 11.52 0.82 0.35
268 F6 11.48 0.78 -0.09
269 F2 10.43 0.57 0.00
270 A0 11.81 0.72 0.04
271 A0 11.15 0.66 -0.01
272 A0 9.42 0.09 -0.02 BD +56deg 2608
273 F5 10.08 0.41 -0.15 BD +56deg 2611
274 A0 10.86 0.31 -0.11
275 K0 11.06 0.85 0.62
276 B2 11.48 0.56 -0.27
277 B6 10.11 0.34 -0.05
278 A0 11.23 0.53 0.38
279 G 11.48 0.92 0.44
280 F0 9.72 0.29 0.08 BD +56deg 2633
281 B2 9.25 0.70 -0.35 BD +56deg 2640
282 A0 11.53 0.96 0.29
283 A2 11.35 0.96 0.52
284 F8 11.35 0.80 0.45:
285 A0 11.58 0.85 0.49
286 F2 11.64 0.96 0.68:
287 A0 12.25 0.57 0.38
288 B5 10.73 0.44 -0.26
289 K2 10.15 1.54 1.42
290 F8 10.40 0.85 0.74 BD +56deg 2639
291 K5 9.50 1.68 2.27 BD +56deg 2637
292 A0 11.15 0.48 0.27
293 B3 8.92 0.29 -0.62 BD +56deg 2632
294 B3 9.49 0.21 -0.70 BD +56deg 2631
295 F8 11.27 0.43 0.25
296 A0 11.79 0.40 0.17
297 B7 11.05 0.25 -0.26
298 G0 11.29 0.65 0.29
299 B7 11.69 0.50 -0.07
300 K 11.08 1.05 0.00
301 K 8.61 0.94 0.79 BD +56deg 2624
302 A0 12.25 0.80 0.44
303 A0 11.10 1.23 0.84 blend
304 A7 12.10 0.50 0.56
305 F2 10.11 2.05 0.29
306 B2 9.21 0.23 -0.64 BD +56deg 2618
307 B0 7.40 0.14 -0.79 BD +56deg 2614
308 G0 9.80 0.51 -- BD +56deg 2609
309 G8 10.00 0.82 0.52 BD +56deg 2597
310 A4 10.98 0.73 0.43
311 A0 11.27 0.84 0.25
312 A2 9.51 0.59 0.11 BD +56deg 2591
313 B8 11.00 0.65 0.24
314 A0 11.35 0.81 0.65 blend
315 A0 9.22 0.30 -0.02 BD +56deg 2585
316 A0 11.27 0.76 0.29
317 A0 11.81 0.80 0.12:
318 A7 10.98 0.79 0.50
319 K 10.46 1.76 1.73
320 A4 10.07 0.74 0.80
321 G2 10.69 0.83 0.04
322 B8 10.68 0.67 0.00
323 K 9.62 1.77 1.37 BD +56deg 2572
324 A5 11.30 0.91 0.55
325 A7 11.46 0.88 0.29
326 G5 9.79 0.82 0.19 BD +56deg 2568
327 A7 11.37 1.71 1.27
328 A0 11.08 0.78 0.23
329 A5 10.22 0.60 0.09 BD +56deg 2566
330 B5 10.27 0.89 -0.06
331 B8 10.89 0.94 0.03
332 A6 10.77 1.06 0.62 blend
333 B0 11.54 0.98 0.15 edge
334 A2 11.68 0.95 0.14 blend
335 F0 11.56 0.77 0.46
336 A2 10.83 0.67 0.40:
337 F0 10.62 0.64 0.18
338 F0 10.39 0.78 -0.05
339 G0 10.02 0.56 0.18 BD +56deg 2579
340 F4 8.27 0.35 -0.23 BD +56deg 2581
341 B1 8.68 0.33 -0.83 BD +56deg 2584
342 F4 11.22 0.69 -0.08
343 F2 11.15 0.47 0.10
344 G2 10.37 0.68 0.05
345 K 10.12 1.20 1.22
346 F2 10.31 0.47 0.02
347 B8 10.63 0.12 -0.09 BD +56deg 2612
348 G2 10.82 0.48 0.38
349 K2 9.28 1.69 2.29 BD +56deg 2624
350 B8 9.98 1.07 0.97
351 K 11.06 1.31 1.12
352 F0 10.51 0.64 0.53 BD +56deg 2635
353 F0 10.58 0.57 0.51 BD +56deg 2638
354 F8 9.97 0.47 0.08 BD +56deg 2646
355 A5 10.59 0.64 0.03 BD +56deg 2647
356 F8 10.78 0.52 0.23 BD +56deg 2650
357 B5 10.60 0.57 -0.06
358 F8 11.50 0.62 0.05
359 K 10.34 1.77 1.58
360 G8 10.05 0.64 0.53
361 K5 9.42 1.44 2.36 BD +56deg 2666
362 K0 10.79 1.79 1.18
363 F2 11.30 0.47 0.35
364 B7 10.43 0.35 0.09 edge
365 F2 11.97 0.53 0.46
366 G8 11.59 0.47 0.44
367 F5 10.31 0.68 0.07 BD +56deg 2648
368 K0 9.85 1.14 1.13 BD +56deg 2644
369 A0 9.84 0.26 0.10: BD +56deg 2642
370 F5 12.03 0.63 0.22
371 A5 11.19 0.63 0.58
372 A2 11.36 0.45 0.16
373 B8 11.06 0.21 -0.31
374 F0 11.65 0.55 --
375 A0 11.48 0.36 0.43
376' B5 9.24 0.87 0.35 BD +56deg 2621
377' A7 9.42 0.35 0.14 BD +56deg 2606
378' K0 9.09 1.07 0.97 BD +56deg 2619
379' B8 10.57 0.34 -0.04
380' A2 10.71 0.58 0.37
381' F0 10.57 0.40 0.06
382' K 10.89 1.54 1.59
383' F0 11.70 0.69 0.41
384' B0 6.90 0.19 -0.72 BD +57deg 2374
385' F2 9.20 0.43 0.03 BD +56deg 2600
386' F2 9.65 0.41 -0.02 BD +56deg 2600
387' A2 10.10 0.45 2.04
388' O6 5.86 0.19 -0.60 BD +56deg 2717
389' B0 8.04 0.27 -0.77 BD +56deg 2717
390' B0 8.03 0.14 -0.68 BD +56deg 2717
391' F4 7.44 0.46 0.04 BD +56deg 2623
392' F4 8.76 0.62 0.08 BD +56deg 2623
393' B0.5 10.47 0.65 -0.35
394' B2 8.65 0.25 -0.57 BD +56deg 2610
395 A0 11.80 0.16 0.03
396 A0 11.42 0.26 0.38
397 F6 10.25 0.46 0.04
398 M0 9.15 1.76 2.45 BD +56deg 2616
399 K5 9.10 1.02 0.19 BD +56deg 2613
400 B1 9.16 0.36 -0.50 BD +56deg 2615
401 A0 11.45 0.28 0.08
402 B5 12.10 0.56 -0.18
403 K0 10.18 1.35 1.17
404 B3 10.32 0.37 -0.33 BD +56deg 2602
405 F6 10.15 0.57 -0.01 BD +56deg 2599
406 B5 10.81 0.52 -0.18
407 K0 10.30 1.29 0.25
408 A2 11.53 0.58 -0.29
409 B9 9.45 0.24 -0.19 BD +56deg 2594
410 B5 12.51 0.70 0.19
411 A0 12.57 1.06 0.17
412 F0 10.35 0.37 -0.04 BD +56deg 2568, blend
413 A0 11.04 0.36 0.15
414 K2 10.33 1.10 0.78
415 M 9.91 1.90 1.78
416 G8 8.13 0.87 -0.01 BD +56deg 2578
417 G8 10.69 0.95 0.22
418 B5 9.94 0.82 0.00 BD +56deg 2577
419 M 10.94 2.24 1.21
420 K5 10.18 1.44 1.43 BD +56deg 2576
421 A0 11.81 0.81 0.64
422 K0 8.08 1.26 0.83 BD +56deg 2574
423 A0 11.86 0.88 0.16
424 F8 10.29 0.88 0.05
425 G0 10.22 1.00 0.28
426 A0 11.96 1.07 0.45
427 F8 10.49 0.97 0.15 BD +56deg 2563
428 K0 7.68 1.77 1.67 BD +56deg 2561
429 B8 10.74 1.01 0.05
430 F8 10.81 0.96 0.14 edge
431 K0 9.48 1.35 -0.01:
432 A2 11.56 1.27 0.68
433 A5 11.43 0.83 0.57
434 K0 8.00 1.64 1.54 BD +56deg 2569
435 G8 11.72 0.96 0.12
436 K2 9.45 1.42 1.30 BD +56deg 2575
437 A0 11.73 0.92 0.39
438 K 8.70 1.59 1.59 BD +56deg 2582
439 F8 11.65 0.71 0.21
440 F5 10.59 0.51 0.13
441 G2 11.29 0.73 0.10
442 A3 10.01 0.24 0.06 BD +56deg 2593
443 A2 10.38 0.16 0.48
444 B5 11.30 0.45 -0.12
445 A0 9.39 0.05 -0.05 BD +56deg 2595
446 B3 10.11 0.25 -0.42
447 B3 8.38 0.41 -0.72 BD +56deg 2598
448 B3 9.46 0.14 -0.39 BD +56deg 2604
449 A0 12.14 0.46 0.16
450 B0 8.39 0.39 -0.79 BD +56deg 2620
451 B5 10.20 0.23 -0.52 BD +56deg 2622, blend
452 G2 11.14 0.40 0.53 blend
453 F8 12.62 0.92 0.36
454 K 11.96 1.41 0.08
455 F2 10.72 0.42 0.38
456 B8 10.74 0.48 0.22
457 K5 8.46 1.08 1.23 BD +56deg 2634
458 A5 11.68 0.70 0.72
459 K0 11.59 0.85 0.53 blend
460 A0 12.37 0.38 0.66
461 F5 11.71 0.65 0.54
462 F0 10.39 0.59 0.46 BD +56deg 2645
463 B8 11.54 0.53 0.22
464 A0 11.96 0.31 0.15 edge
465 K0 10.90 0.69 0.66
466 A0 12.01 0.63 0.64
467 A0 11.21 0.32 0.42
468 A0 11.18 0.32 0.35
469 A0 8.72 0.04 -0.06 BD +56deg 2652
470 A0 12.39 0.71 0.23
471 A2 11.64 0.37 0.52
472 F8 10.49 0.45 0.10
473 A2 11.21 0.44 0.69
474 F0 10.93 0.68 0.42
475 G5 9.70 0.53 0.29
476 F2 10.71 0.79 0.29
477 K2 8.52 1.48 1.75 BD +56deg 2636
478 F6 11.79 0.81 0.43
479 A0 12.36 0.45 0.48
480 K4 10.67 1.17 0.90
481 B8 11.25 0.12 -0.11
482 G0 10.67 0.67 0.50
483 A7 11.93 0.48 0.49
484 F2 11.50 0.71 0.46
485 B2 9.81 0.04 -0.65
486 A2 9.48 0.22 -0.12
487 B8 11.04 0.02 -0.16
488 A0 11.94 0.35 0.61
489 B8 10.70 0.25 -0.10
490 A0 11.94 0.49 0.10
491 B0 8.63 0.33 -0.79 BD +56deg 2605
492 B3 11.02 0.54 -0.20 edge
493 B5 10.86 0.82 0.11 blend
494 A0 11.19 0.85 0.38
495 K0 10.69 0.71 0.40
496 A0 11.96 0.90 -0.26 blend
497 F8 11.05 0.75 0.13
498 G8 10.02 0.74 0.17 BD +57deg 2347
499 B5 10.95 0.71 -0.13
500 K0 8.08 1.09 0.87 BD +56deg 2590
501 G8 11.72 0.72 0.35
502' B0 7.45 0.57 -0.45 BD +56deg 2589
503 A0 11.39 1.02 0.70
504 A0 11.31 0.90 1.01: blend
505 A2 11.28 0.85 0.56
506 A5 9.34 0.49 0.31 BD +56deg 2571
507 F8 9.44 0.86 0.41 BD +56deg 2570
508 F5 9.63 0.70 0.13 BD +56deg 2564
509 F8 7.82 0.82 -0.05 BD +56deg 2562
510 F8 10.44 0.75 0.03 edge
511 A0 11.25 1.19 0.24 blend
512 F6 9.41 0.75 0.22 BD +57deg 2316
513 F2 8.44 0.77 -0.22 BD +57deg 2317
514 A0 11.69 1.06 0.79
515 F8 11.73 1.02 0.70
516 F8 11.18 0.76 0.20
517 F6 11.57 0.99 0.40
518 A0 12.27 1.07 0.70
519 B8 10.72 0.50 0.14 BD +57deg 2336
520 A7 11.29 0.67 0.76:
521 F8 10.42 0.50 0.05 BD +57deg 2345
522 B3 9.92 0.29 -0.44 BD +57deg 2350
523 A2 10.71 0.71 0.45
524 K2 9.81 1.06 1.05 BD +57deg 2353
525 B8 10.34 0.58 0.10
526 M 10.65 1.83 1.37
527 F8 11.39 0.70 -0.13
528 K2 10.52 1.40 0.95
529 G5 11.04 0.82 0.16
530 A0 12.00 0.53 0.09
531 F0 11.04 0.79 -0.05
532 A5 11.58 0.65 0.46
533 A2 9.48 0.56 0.36 BD +57deg 2356
534 A0 11.31 0.42 0.03
535 A7 11.67 0.53 0.33
536 A4 10.84 0.47 0.41
537 A0 11.43 0.35 0.10
538 A0 12.45 0.38 0.20
539 A4 11.63 0.59 0.43 blend
540 B6 11.24 0.27 -0.25
541 A7 12.05 0.62 0.50
542 A5 11.26 0.32 0.41
543 A0 12.19 0.41 0.42
544 B2 9.95 0.06 -0.55 BD +57deg 2369
545 B7 10.58 0.13 -0.23
546 F 10.36 1.32 1.47
547 A2 12.01 0.29 0.35
548 K4 9.83 1.33 1.51 BD +56deg 2630
549 K 9.98 1.91 2.35 BD +56deg 2627
550 B8 9.04 0.37 0.09 BD +57deg 2386
551 F0 11.59 0.75 0.56
552 F 11.51 0.73 0.44
553 F 11.51 0.75 0.30
554 B8 11.39 0.43 0.11
555 F8 10.87 0.59 0.38
556 G5 11.01 0.58 0.43
557 K0 8.95 1.05 0.79 edge
558 A2 8.35 0.14 -0.07 BD +57deg 2402
559 F0 12.15 0.73 0.67
560 M 9.35 1.94 1.69 BD +57deg 2398
561 A0 9.95 0.12 0.38 BD +57deg 2395, blend
562 B3 9.48 0.49 -0.23 BD +57deg 2395, blend
563 A0 11.61 0.71 0.73
564 F0 11.58 0.72 0.59
565 B5 9.73 0.41 -- BD +57deg 2383
566 F0 12.02 0.43 0.37
567 A0 11.59 0.92 0.93
568 B5 10.01 0.12 -0.12 BD +57deg 2375
569 A6 10.68 0.46 -0.27
570 K0 8.38 1.20 1.28 BD +57deg 2371
571 A7 12.49 0.63 0.30 blend
572 G8 11.40 0.76 0.27
573 K0 7.90 1.05 0.79 BD +57deg 2359
574 F8 10.46 0.60 0.19
575 A0 11.77 0.42 0.17
576 K0 11.25 0.84 0.48
577 G8 10.79 0.80 0.31
578 F4 10.77 0.76 0.35
579 F6 12.69 0.76 0.51
580 B8 11.95 0.91 0.57
581 B2 9.53 0.23 -0.51 BD +57deg 2343
582 B7 10.15 0.32 -0.16 BD +57deg 2335
583 A0 11.18 0.42 -0.03
584 B3 9.39 0.29 -0.44 BD +57deg 2334
585 A0 11.57 0.90 0.82 blend
586 A0 11.37 0.91 0.36
587 B3 10.45 0.58 -0.21 BD +57deg 2327
588 K2 9.08 1.34 1.35 BD +57deg 2319
589 G0 11.47 0.84 0.13
590 A2 11.46 1.21 0.54 edge
591 K0 7.49 1.31 1.09 BD +57deg 2318
592 G2 10.39 0.79 0.05
593 G5 7.09 0.77 -0.23: BD +57deg 2322
594 F8 10.37 0.69 -- BD +57deg 2324
595 A7 9.61 0.34 0.15 BD +57deg 2332
596 B8 10.12 0.55 0.35 BD +57deg 2333
597 G 11.84 1.00 0.21
598 B5 9.92 0.38 -0.08 BD +57deg 2339
599 G2 11.67 0.85 0.51
600 K2 9.21 1.20 1.36 BD +57deg 2351
601 A2 11.77 0.74 0.85
602 B8 12.82 0.86 0.48
603 B8 10.39 0.34 0.10
604 G8 10.86 0.86 0.37
605 A2 11.33 0.65 0.78
606 A5 11.18 0.77 0.68
607 A5 10.89 0.81 0.70
608 B7 9.67 0.35 -0.31 BD +57deg 2363
609 F2 11.15 0.57 0.13 blend
610 F8 10.24 0.61 0.11 BD +57deg 2373
611 K4 9.36 1.60 2.24 BD +57deg 2381
612 B8 10.60 0.30 0.12 BD +57deg 2382
613 F2 11.79 0.71 0.24
614 A0 12.21 0.57 0.61
615 G0 10.80 0.91 0.51
616 A7 10.94 0.78 0.64 BD +57deg 2397
617 K0 10.33 1.45 1.25 BD +57deg 2400
618 A5 10.39 0.47 0.55
619 A0 10.42 0.46 0.43
620 A2 8.28 0.20 -0.05 BD +57deg 2403
621 A7 10.39 0.51 0.46 BD +57deg 2400
622 A4 11.35 0.48 0.52
623 G4 12.38 0.53 0.69
624 K0 11.75 0.71 0.15: edge
625 A0 12.05 0.26 0.21: edge
626 B0 11.17 0.34 -0.67
627 G5 10.71 0.72 0.48
628 G8 11.27 0.77 0.64
629 G5 8.40 0.73 0.08 BD +57deg 2399
630 K 11.98 1.31 1.14
631 A2 12.57 0.48 0.51
632 A2 11.46 0.44 0.49
633 M 7.23 2.03 2.36 BD +57deg 2396
634 A2 11.74 0.40 0.42
635 A0 9.30 0.40 0.29 BD +57deg 2391
636 K0 6.79 1.12 0.66 BD +57deg 2392
637 F8 11.71 0.71 0.22
638 K0 9.11 1.12 0.35 BD +57deg 2388
639 A4 11.35 0.49 0.49
640 G0 10.73 0.73 0.47
641 A0 10.74 0.49 0.52
642' B2 8.92 0.29 -0.62 BD +57deg 2380
643 A0 10.77 0.41 0.42
644 F8 11.36 0.59 0.15
645 B2 9.72 0.37 0.47 BD +57deg 2376
646 A2 10.15 0.36 0.56
647 A0 11.68 0.70 0.26
648 K2 9.32 1.25 1.41 BD +57deg 2367
649 A6 11.75 0.68 0.62
650 B6 9.97 0.42 -0.09 BD +57deg 2366
651 A0 11.63 0.60 0.55
652 B2 8.83 0.35 -0.29: BD +57deg 2360
653 A0 12.08 0.50 0.54
654 B2 8.51 0.58 0.60 BD +57deg 2354
655 B7 10.66 0.65 0.13 BD +57deg 2352
656 A2 7.97 0.30 -0.10 BD +57deg 2349
657 F2 8.80 0.49 0.06 BD +57deg 2342
658 A2 8.88 0.31 0.11 BD +57deg 2338
659 A2 9.05 0.37 0.19 BD +57deg 2337
660 G 11.68 0.84 0.41
661 F8 11.45 0.69 0.22
662 A4 10.10 0.82 0.48:
663 K5 7.98 1.45 1.44: BD +57deg 2323
664 A2 9.10 0.36 0.18 BD +57deg 2320
665 B8 10.78 1.04 0.46 edge
666 G8 11.69 1.61 1.30 blend
667 G0 9.29 0.73 0.15 BD +57deg 2321, edge
668 F8 11.86 1.00 0.48
669 K2 8.76 1.14 1.32 BD +57deg 2330
670 A3 10.12 0.46 0.37 BD +57deg 2330
671 A7 12.15 0.41 -0.03 blend
672 K4 10.08 1.62 1.77
673 G8 10.84 0.70 0.41
674 B8 11.10 0.65 0.27
675 A0 12.07 0.67 0.43
676 A0 12.32 0.54 0.46
677 K0 10.15 1.01 0.85 BD +57deg 2365
678 K4 9.29 2.03 2.92: BD +57deg 2368
679 K2 11.40 0.94 0.57
680 B8 11.69 0.44 -0.01
681 B5 11.41 0.32 -0.18
682 A0 11.62 0.52 -0.07
683 F0 11.65 0.73 0.15
684 F8 11.41 0.65 0.11
685 K4 10.46 1.40 1.69
686 F2 11.93 0.52 0.46
687 B7 9.97 0.15 -0.15 BD +57deg 2366
688 A0 11.45 0.44 -0.07
689 B2 10.56 0.37 -0.53:
690 F0 11.60 0.60 0.59
691 F8 10.22 0.67 0.44
692 F5 10.65 0.51 0.26
693 F5 9.81 0.50 0.21
694 F2 11.33 0.54 0.30
695 K0 11.82 0.62 0.95: edge
696 F2 11.67 0.52 0.50
697 A0 11.41 0.31 0.29
698 A2 10.47 1.14 1.37
699 K2 10.47 1.23 0.47
700 F8 11.52 0.58 0.19
701 F0 10.47 0.36 0.17 BD +57deg 2394
702 A0 11.30 0.34 0.22
703 F6 9.66 0.72 0.20 BD +57deg 2398
704 B7 9.62 0.53 0.18 BD +57deg 2387
705 F0 11.21 0.72 0.36 blend
706 G2 10.81 0.55 0.64 BD +57deg 2387
707 F8 11.07 0.75 0.30
708 A0 11.61 0.84 0.23
709 M 9.77 1.86 2.32 BD +57deg 2379
710 G5 10.74 0.63 0.32
711 A4 11.71 0.61 0.16
712 B3 8.49 0.41 -0.56 BD +57deg 2372
713 G8 11.19 0.65 0.26
714 A0 11.73 0.62 0.52
715 A4 11.20 0.49 0.71
716 A2 11.07 0.48 0.52
717 B8 11.26 0.51 -0.08
718 A0 11.51 0.68 -0.01
719 K2 10.64 1.64 1.62
720 A0 11.37 0.52 0.35
721 A4 11.37 0.70 0.61
722 B1 9.28 0.42 -0.35 BD +57deg 2343
723 A0 12.04 0.84 0.77
724 A0 12.20 0.74 0.38
725 F0 8.13 0.45 0.02 BD +57deg 2344
726 F4 10.92 0.68 0.19
727 B8 10.89 0.53 0.24
728 A0 11.84 0.60 1.02
729 A2 10.56 0.39 0.19 BD +57deg 2329
730 G5 9.94 0.97 0.15 BD +57deg 2328
731 K2 8.01 1.28 1.11: BD +58deg 2263
732 A0 10.54 1.07 0.19
733 F8 10.31 0.71 0.01 BD +58deg 2269
734 B0 7.90 0.92 -0.26 BD +58deg 2272
735 G2 11.04 0.76 0.05:
736 A4 10.48 0.40 0.36: BD +58deg 2278
737 F8 10.26 0.58 0.11 BD +58deg 2286
738 K2 10.48 1.47 1.69 BD +58deg 2280
739 B1 8.61 0.20 -0.58 BD +58deg 2283
740 F8 10.98 0.73 0.14
741 A2 10.37 0.27 0.34 BD +57deg 2348
742 A2 11.23 0.61 0.52
743 B3 9.88 0.48 -0.26 BD +58deg 2292
744 B3 10.01 0.16 -0.31:
745 K0 7.93 1.16 0.99: BD +58deg 2295
746 B8 11.14 0.55 -0.05
747 B2 10.67 0.70 0.24 BD +58deg 2297
748 G2 11.54 0.74 0.31
749 B8 7.76 0.27 -0.17 BD +58deg 2300
750 G8 11.01 0.75 0.55
751 A0 11.21 0.65 0.18
752 G2 11.42 0.67 0.41
753 B5 11.32 0.43 -0.03
754 B5 11.98 0.53 -0.03 blend
755 F5 10.86 0.56 0.24
756 A7 10.04 0.44 0.40 BD +57deg 2377
757 F6 10.23 0.38 -- BD +57deg 2389
758 B8 10.28 0.28 0.23 BD +57deg 2389
759 A4 11.37 0.49 0.76 blend
760 A4 11.17 0.44 0.60
761 A0 11.70 0.37 0.20
762 K5 8.57 1.17 2.87: edge
763 A0 12.01 0.33 0.35:
764 F8 11.17 0.55 0.34:
765 A0 12.76 0.59 0.23 blend
766 G8 11.66 0.43 0.49
767 A0 9.77 0.46 -0.29 BD +58deg 2315
768 F0 9.04 0.46 0.03 BD +58deg 2313
769 G0 9.90 0.53 0.00 BD +58deg 2312
770 F8 10.75 0.56 0.30
771 F0 11.67 0.67 0.49
772 G 12.04 0.85 0.29
773 A0 11.79 0.81 0.10
774 A0 11.06 0.68 0.33
775 A2 11.85 0.68 0.13
776 A2 11.42 0.68 0.01
777 F8 11.35 0.68 0.16:
778 A0 11.64 0.72 0.64:
779 A2 11.20 0.91 0.53:
780 A4 10.02 0.37 0.55 BD +58deg 2287, blend
781 F5 10.20 0.68 0.45 BD +58deg 2286
782 F6 10.21 0.50 0.15: BD +58deg 2284
783 F2 9.79 0.99 0.34 BD +58deg 2288
784 B5 9.87 0.90 0.10
785 F0 10.80 0.48 0.16:
786 K0 10.23 1.14 1.18: blend
787 A2 10.20 0.35 0.42: BD +58deg 2271
788 F2 11.56 0.84 0.42:
789 A4 11.77 1.13 0.70
790 F0 11.03 0.51 0.18
791 A2 10.68 0.97 0.73:
792 F3 10.98 0.62 0.30
793 A2 11.24 0.59 0.41:
794 F2 10.11 0.41 0.20: BD +58deg 2291
795 B5 8.38 0.15 -0.23 BD +58deg 2290
796 F0 10.43 0.39 0.29 blend
797 B5 10.40 0.68 0.11
798 F8 10.62 0.60 0.22 BD +58deg 2298
799 F8 9.73 0.43 0.50 BD +58deg 2285, blend
800 A7 10.76 0.48 0.50
801 G0 10.89 0.58 0.30
802 A7 10.39 0.42 0.25
803 F8 11.15 1.21 0.54 blend
804 F6 11.22 0.79 0.52
805 A0 11.37 0.57 0.21
806 F8 10.76 0.66 0.03
807 A2 9.21 0.40 0.03 BD +58deg 2318
808 B5 10.14 0.46 0.32
809 B2 9.21 0.30 -0.54 BD +58deg 2320
810 A0 10.72 0.42 0.25:
811 F2 9.50 0.45 0.28 BD +58deg 2322
812 A2 11.40 0.39 0.55
813 A0 11.78 0.69 0.19
814 A2 11.04 0.32 0.45
815 A2 11.89 0.25 0.60: edge
816 A7 11.19 0.41 0.37
817 F2 11.57 0.51 0.24
818 K 6.21 1.07 1.58 BD +58deg 2314
819 F2 10.56 0.52 0.29: BD +58deg 2310
820 G5 10.40 0.72 0.35 BD +58deg 2308
821 F8 10.81 0.92 0.62
822 B3 9.46 0.74 0.13 BD +58deg 2303
823 F8 11.19 0.73 0.41 blend
824 A4 11.73 0.90 0.18
825 F2 10.63 1.22 0.64:
826 K0 8.33 1.45 1.78: BD +58deg 2277
827 A2 11.30 0.90 0.73:
828 B8 10.64 0.66 0.07: BD +58deg 2293
829 B8 10.33 0.69 0.44:
830 A0 9.09 0.28 0.28: BD +58deg 2301
831 G0 9.59 0.58 0.25: BD +58deg 2304
832 F4 10.34 0.51 0.39
833 F6 12.32 0.54 0.48
834 A0 11.45 0.51 0.35
835 G2 11.51 0.41 0.41
836 A2 10.76 0.39 0.60
837 A0 12.45 0.44 0.32
838 A2 11.65 0.21 0.34
839 A0 7.73 0.25 -0.22 BD +57deg 2326
840 F5 12.14 0.81 0.84
841 F0 8.08 0.77 -0.01 blend
842 F0 8.81 0.57 0.25 blend
NOTES TO THE TABLE
A point (') at the right upper side of the running number denotes
photoelectrically measured magnitudes.
Blend is remarked if the photographic image of the measured star is
distorted by a neighbouring star.
A colon beside the U-B colour denotes that the ultraviolet magnitude of
the star is uncertain because of the field error of the ultraviolet filter.
Edge is remarked if the star is near the edge of the plate.
Photoelectric magnitudes and colours of stars were taken from the
following sources:
Balazs, B. A., private communication (376, 377, 378, 379, 380, 381,
382, 383, 387).
Eggen, 0. J. 1966. Roy. Obs. Bull. No. 120. (385, 386, 391, 392).
Deutschman, W. A., Davis, R. J., Schild, R. E. 1976. ApJ. Suppl.
30. 97. (293, 642).
Hiltner, W. A. 1956. ApJ. Suppl. 2. 389. (281, 307, 384, 502).
Simonson, S. C. 1968. ApJ. 154. 923. (388, 389, 390, 394).
Finding chart of the survey stars I.
Finding chart of the survey stars II.