Contents of: VI/111/./abstract/KHURLEY_SGRQUIE2.abs

The following document lists the file abstract/KHURLEY_SGRQUIE2.abs from catalogue VI/111.
A plain copy of the file (without headers/trailers) may be downloaded.


==> In this proposal, more time is being requested for KHURLEY.SGRQUIES
==> This proposal requests an upgrade from Priority 3 for KHURLEY.SGRQUIES
The 3 known soft gamma repeaters appear to be a completely new manifestation of
neutron stars.  SGR 1806-20 and SGR 1900+14 have highly unusual stellar
counterparts, whose spectra peak in the far infrared, while they have not been
detected at submillimeter or millimeter wavelengths.  Their infrared spectra
appear to contain several components:  the photospheric emission from star(s)
dominates at shorter wavelengths, a bright point source dominates at 25
microns, while an extended source dominates at 60 microns.  Their far IR
spectra are consistent with simple dust models.  Since our original ISO
proposal was written, we have carried out a multi-wavelength observing program
and have found that SGR 1806-20 is orders of magnitude more luminous in the IR
than originally suspected; indeed, it appears to be a luminous blue variable
star, and perhaps the most luminous star in the galaxy.  We have also found
that SGR 1900+14 may have a peculiar double star system as its counterpart.
Our LWS observation of this source has already been done, although we do not
yet have the data.  Finally, we have not so far identified a mid-IR counterpart
to SGR0525-66.  Therefore, we are requesting
1. That our LWS01 priority 3 time on SGR 1806 be upgraded,
2. That our PHT32 priority 3 time on SGR 1806 at 200 microns be upgraded
3. That our SWS01 priority 3 time on SGR1900 and 1806 be upgraded, preferably
with a higher speed to improve the S/N
4. That new PHT32 observations be done on SGR1806-20 and 1900+14 at 60
microns to determine the extent of the sources
5. To upgrade the 25 micron raster PHT03 on SGR0525 (from the Spring
launch proposal)
6. To upgrade our Grade 1 25 micron PHT03 observations for calibration of SWS
spectra.
7. To perform CAM05 polarization measurements on SGR1900 and 1806.


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