star | * |
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mV | Spectral type | ![]() |
Campaigns | |
HD 203 | CMP | 00h 06m 50.0s | -23![]() |
6.18 | F2IV | 155 | 3 | |
HR 10 | HD 256 | VR,SV,CG | 00h 07m 18.3s | -17![]() |
6.23 | A2IV/V | 220 | 1,2,3 |
HD 693 | CMP | 00h 11m 15.8s | -15![]() |
4.89 | F5V | 8 | 2,3 | |
HD 16417 | CMP | 02h 36m 58.6s | -34![]() |
5.78 | G5IV | 2,3 | ||
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HD 20010A | IR | 03h 12m 04.4s | -28![]() |
3.85 | F8IV | 0 | 2,3 |
HD 17729 | CMP | 02h 49m 54.1s | -27![]() |
5.36 | A0V | 135 | 2,3 | |
HD 21790 | CMP | 03h 30m 37.0s | -05![]() |
4.74 | B9Vs | 72 | 3 | |
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HD 22049 | IR | 03h 32m 55.9s | -09![]() |
3.73 | K2V | 8 | 1,2,3 |
HD 22243 | CMP | 03h 34m 37.4s | -09![]() |
6.25 | A2V | 160 | 1,2,3 | |
HD 22713 | CMP | 03h 39m 01.1s | -05![]() |
5.96 | K1V | 3 | ||
o 2 Eridani | HD 26965A | VR | 04h 15m 16.3s | -07![]() |
4.41 | K1V | 2,3 | |
HD 25069 | CMP | 03h 58m 52.4s | -05![]() |
5.83 | G9V | 3 | ||
HD 26703 | CMP | 04h 13m 49.8s | +12![]() |
6.25 | K0 | 3 | ||
HR 1307 | HD 26676 | IR | 04h 13m 34.5s | +10![]() |
6.23 | B8Vn | 300 | 1,2,3 |
HD 26793 | CMP | 04h 14m 36.1s | +10![]() |
5.22 | B9Vn | 350 | 1,2,3 | |
HD 32743 | CMP | 05h 02m 48.7s | -49![]() |
5.38 | F2V | 0 | 3 | |
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HD 33262 | IR | 05h 05m 30.6s | -57![]() |
4.72 | F7V | 0 | 2,3 |
HD 35072 | CMP | 05h 19m 22.1s | -50![]() |
5.45 | F7III-IV | 3 | ||
HD 38382 | CMP | 05h 44m 28.3s | -20![]() |
6.34 | F8/G0V | 3 | ||
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HD 38392B | VR | 05h 44m 26.5s | -22![]() |
6.15 | K2V | 2,3 | |
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HD 38393A | IR | 05h 44m 27.7s | -22![]() |
3.60 | F7V | 15 | 2,3 |
HD 35386 | CMP | 05h 23m 12.0s | -26![]() |
6.49 | F6V | 3 | ||
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HD 38678 | IR | 05h 46m 57.3s | -14![]() |
3.60 | A2Vann | 245 | 1,2 |
HD 37935 | CMP | 05h 36m 55.1s | -66![]() |
6.30 | B9.5Ve | 3 | ||
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HD 39014 | IR | 05h 44m 46.4s | -65![]() |
4.35 | A7V | 206 | 1,2,3 |
HD 39963 | CMP | 05h 51m 23.1s | -64![]() |
6.36 | G8III | 3 | ||
HD 35580 | CMP | 05h 22m 22.1s | -56![]() |
6.08 | B8.5V | 1,2,3 | ||
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HD 39060 | VR,SV,IR,CG | 05h 47m 17.1s | -51![]() |
3.80 | A5V | 104 | 1,2,3 |
HD 40200 | CMP | 05h 54m 41.1s | -49![]() |
6.10 | B3V | 1,2,3 | ||
HD 41692 | CMP | 06h 06m 38.7s | -04![]() |
5.39 | B5IV | 20 | 3 | |
HR 2174 | HD 42111A | CG | 06h 08m 57.8s | +02![]() |
5.73 | A3V | 120 | 3 |
HD 42824 | CMP | 06h 12m 44.4s | -02![]() |
6.63 | A2V | 3 | ||
HD 155450 | CMP | 17h 12m 58.6s | -32![]() |
6.01 | B1II | 114 | ||
51 Ophiuchi | HD 158643 | IR,CG | 17h 31m 24.8s | -23![]() |
4.81 | A0V | 210 | 3 |
HD 160915 | CMP | 17h 43m 25.7s | -21![]() |
4.87 | F6/F7V | 0 | 3 |
To compensate for the relatively small number of measurements obtained
with our previous survey
using the Geneva system between 1989 and 1997,
a denser and long lasting photometric survey of Pictoris and
of some other
suspected
Pictoris-like star candidates was needed.
In October 1995 we began a circumstellar disk survey with
the accurate Strömgren uvby photometric system
being used almost permanently by the SAT group of the
Copenhagen University Observatory.
On behalf of a collaboration between Copenhagen Observatory and Institut
d'Astrophysique de Paris through INSU (CNRS),
we have performed three successive observational campaigns from
1995 to 1998, each season from October to April, using the SAT
automatic 50 cm Danish telescope
atop La Silla Observatory
(Florentin Nielsen et al. 1987; Florentin Nielsen 1993).
We report here the result of 3 years of observations of the stars listed
in Table 1. This circumstellar
program was conducted from 1995 to 1998.
As it could be noted only a small amount of stars were selected within our
program, the reason being that only about a dozen of stars could be surveyed
in a dense enough manner to be compatible with both the overall SAT
observing program and the fact that at least two comparison
stars should be observed simultaneously for each program star. The star list
being extremely short, the program stars have to be selected in an extremely
biased manner. They are in fact partly from our previous Geneva survey and
partly as being "probably" good candidates, either because some variability
is already suspected, or because they present some IR excess with known high
value to favour the probability of extinction by dust within the
disc.
Finally, during these three years as studies of dusty disks around A stars
were made by several teams, some
new stars were added to the program or suppressed from it during the
chain of campaigns. Note that particularly
Pictoris, HD 35580 (comparison, hereafter CMP),
HD 40200 (CMP), HR 10, HD 22049, HD 22243 (CMP),
HD 26676, HD 26793 (CMP) and HD 39014 were observed during all three
years, whereas some other stars were observed during only
one or two of our campaigns.
Copyright The European Southern Observatory (ESO)