Contents of: VI/111/./abstract/JBERGEAT_PROP_666.abs

The following document lists the file abstract/JBERGEAT_PROP_666.abs from catalogue VI/111.
A plain copy of the file (without headers/trailers) may be downloaded.


 As known since the Infrared Astronomical Satellite (IRAS), a
 number of evolved giant stars show extended emission which
 proved most prominent at the 60 mic. wavelength and images of
 structures up to several arcminutes were obtained.
 We propose to observe with ISO a sample of Long Period Variable
 (LPV) stars for which HIPPARCOS data should become available to us
 early in 1996 (PI and Co-I have two proposals on this astrometric
 program). From known distances, we shall calibrate structures
 found with ISO directly in u.a. or km, which is essential for their
 interpretation.
 We expect to deduce from these observations the morphology and
 magnitude of continuous or episodic mass loss of these stars.
 In the latter case, the history of events is important since it
 raises constraints on stellar evolution models. Also, calibration
 of the mass loss rates from other methods is planned.
 The ISOCAM infrared camera brings the unique opportunity of
 sensitive imaging at shorter wavelengths (we selected a raster
 mode in CAM01 at 15-16 mic. to get the better possible contrast)
 and a 13"-limit in resolution due to diffraction. In addition, a
 raster at 60 mic. will provide the large scale (8'x8') structure
 and background. Additional photometry of these variable stars is
 planned from 3.6 to 100 mic.
 A few symbiotic and peculiar stars were added to this program.

 IF A MODERATE REDUCTION IS TO BE APPLIED, STARS PRIORITIES SHOULD
 BE USED. IF DRASTIC, THE PHT22 PROGRAM OF PARTS 2 AND 4 SHOULD
 BE DELETED ( 900 S PER STAR, 42% OF THE TOTAL).

NOTE added on April 13th 1995 : we add a new object C65 with a
grade 3 with AOT's in the four segments (proposals 555 666 777 888).
There is no duplication with GT and these observations were not
already proposed in a previous (rejected) proposal. If this new
source cannot be accepted (for ex. on the grounds of duplication
with Open Time) it should be replaced by C3313 which has been
attributed grade 1 in the four proposals.

NOTE added on June 6th 1995 :

1.- GRADE 1 STARS :

THEY ARE TO BE IGNORED IF ALL THE GRADE 3 AND 6 STARS ARE KEPT
IN THE FINAL VERSION. WE DESCRIBE BELOW OUR POLICY FOR ANY
CHANGE WHICH COULD BE ASKED TO US IN THE FUTURE.

In addition to C3313 (ION 24 & 69 in PROP_555, ION 24 in PROP_666
ION 33 & 78 in PROP_777, ION 33 in PROP_888), we have maintained
four grade 1 stars which could replace grade 3 stars removed for
any reason in the future :

C4302 (ION 30 & 75 in PROP_555, ION 30 in PROP_666) should replace
any C__, C___ or C____ target further deleted from the Autumn list

HIC108928 (ION 11 & 56 in PROP_555, ION 11 in PROP_666) should
replace any HIC_____ or HIC______ target further deleted from the
Autumn list

C5228 (ION 36 & 81 in PROP_777, ION 36 in PROP_888) should replace
any C__, C___ or C____ target further deleted from the Spring list

HIC117078 (ION 14 & 59 in PROP_777, ION 14 in PROP_888) should
replace any HIC_____ or HIC______ target further deleted from the
Spring list

If the removed target is grade 6, please upgrade a grade 3 star
C65 (ION 93 & 94 in PROP_555, ION 42 in PROP_666): Autumn list
or C65 (ION 97 e& 98 in PRO_777, ION 43 in PROP_888): Spring list
if this is a C-target, or
HIC110478 (ION 12 & 57 in PROP_555, ION 12 in PROP_666) : Autumn l.
or HIC45058 (ION 8 & 53 in PROP_777, ION 8 in PROP_888) : Spring l.
if this is a HIC-target; then upgrade a grade 1 star to replace
the star upgraded from 3 to 6.

IF SUCH A CHANGE PROVES NECESSARY, PLEASE PROCEED GLOBALLY UPON
THE THREE ION's OF A GIVEN STAR: NO PARTIAL REPLACEMENT SHOULD
BE OPERATED.

2.- Due to increase in time costs, the photometry PHT3 is
restricted to three filters (usually 3.6, 16 and 25 mic.)
for all stars except for the symbiotics R Aqr, HM Sge & V1016 Cyg.

© Université de Strasbourg/CNRS

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