<=== observer ===>
"MBARLOW",\
"Barlow, M.J.",\
"Department of Physics & Astronomy",\
"University College London",\
"Gower Street",\
"",\
"WC1E 6BT",\
"London",\
"United Kingdom",\
" 44  713807160",\
" 44  713807145",\
"mjb@star.ucl.ac.uk"

<=== proposal ===>
"DUST2",1,3,\
{"dust properties","AGB stars","planetary nebulae"},\
{"LWS consortium","Baluteau, J.","Caux, E.","Cox, P.","Emery, R.","Nisini, B.",\
"Omont, A.","Pequignot, D","Rieu, N-Q.","Cohen, M.","Greenhouse, M.",\
"Skinner, C.","Walker, H."}

<=== title ===>
The far-IR spectra of cool evolved stars, post-AGB objects and planetary
nebulae

<=== abstract ===>
SCIENTIFIC ABSTRACT
This proposal is to study the (currently unknown) far-infrared emission
properties of dust grains in the regions where they are formed. The study is
designed to reveal the spectral dependence of the dust continuum emission and
to find new dust emission features that will aid the full identification of the
grains. The targets will be M-giants, Miras, OH/IR  stars, S-stars, carbon
stars, post-AGB transition objects (pre-planetary nebulae), and ionised
planetary nebulae (PN) and their neutral shells (where present). These objects
are believed to be the main sources of the refractory dust grains that are
present in the general insterstellar medium. We will study the characteristics
of the dust emission spectra as a function of stellar mass, evolutionary stage
and chemical composition. None of the numerous mid-infared dust features now
known were predicted prior to their observational discovery and one can
expect a systematic study of the region longwards of 30um to reveal
new dust features that will provide important insights into the nature of
circumstellar and interstellar dust.

A LaTex file containing fuller details of this proposal is available from
mjb@star.ucl.ac.uk.

OBSERVATION SUMMARY
This proposal is split into four parts - this is part 2.
Full (43-196.7um) LWS grating spectra will be obtained for all
targets (LWS01 AOT in fast mode). The SWS Consortium is obtaining
2.43-45um low-resolution SWS grating spectra of the majority of
these targets (SWS01 AOT, speed code 1), and we will obtain similar
SWS spectra of the remainder of the targets. If objects in the
Orion-hole should be observable (i.e. a Spring launch), the total
amount of LWS Guaranteed (spacecraft) time allocated will be 28.39 hours, of
which 11.04 hours will be for Priority 1 targets. For an Autumn launch
(Sagittarius-hole observable), 27.86 hours of LWS Guaranteed (spacecraft)
time will be allocated, of which 10.82 hours will be for Priority 1
targets.


<=== scientific_justification ===>
The mid-infrared has already proven to be an extremely important region for
studying the properties of dust grains, via the measurement of their
characteristic solid state emission and absorption features. These studies have
yet to be extended systematically to wavelengths longer than 40um, although KAO
observations have already revealed features at 35um (perhaps MgS; Goebel and
Moseley, 1985, Ap.J., 290, L35) and at 44um  and 62um (ice translation bands,
e.g. Omont et al., 1990, Ap.J., 355, L27).  The exact spectroscopic
identification of the dust grains found in many circumstellar and nebular
environments has still to be achieved. ISO's ability to obtain systematically
the mid- and far-infrared spectra of many different classes of objects will
greatly increase our understanding of the detailed grain emission properties
and so aid their identification.

It is clear from a variety of observations that hydrocarbon emission bands can
be seen in 5-8um spectra in stars as cool as G-type, so that even such cool
stars can excite the mid-IR bands, both in reflection nebulae and in
circumstellar dust shells. Consequently, the study of stars in transition
between the AGB and the  planetary nebula regime provides a direct probe of the
photoexcitation of the hydrocarbon bands.  ISO permits observations of the long
wavelength very  broad bending modes of, for example, PAH molecules, which may
be  recognizable when the more commonly observed, sharper features in the
mid-IR are lacking.  The mass of gas in the neutral regions surrounding many
post-AGB objects and planetary nebulae is very poorly known. Observations of
the important coolant lines of [C II], [O I] and CO will allow a systematic
determination of the densities, temperatures and masses of these regions for
the first time.

The LWS grating resolving power of 150-300 is ideally suited to resolving and
measuring the detailed profiles of solid-state dust features, as well as for
finding low-contrast structure. We propose to observe a number of important
classes of objects, described in more detail below. The changes found in the
far-IR dust spectra of AGB stars as a function of spectral type are expected to
be due to the changing chemical composition of the gas out of which the grains
condense, while changes in the dust spectra found in post-AGB objects, relative
to the behaviour exhibited in the spectra of AGB stars of the same chemical
composition, are expected to be due to the changing physical conditions, e.g.
cooler gas and dust temperatures; the increasing fraction of atomic and
(eventually) ionised hydrogen; and the hardening of the stellar radiation
field.

The  full grating spectra will reveal strong atomic or molecular emission
lines, where present. A companion proposal describes LWS FP observations that
are to be made of lines which are expected to be be present in the spectra of a
number of these objects, but the full grating spectra will enable the detection
of strong lines, including those which were not expected in advance.


Full LWS grating scans (43-188um) will be obtained for all the targets. In
addition, 2.43-45um low resolution SWS01 grating  scans will be obtained for
the targets not being observed by the SWS Consortium. Such complete scans are
essential for this programme, aimed at studying the overall properties of the
dust emission, and for measuring a range of strong emission lines.

LWS AOT's:
          For all targets, LWS full grating spectra (43-196.7um) will
          be obtained with the LWS01 AOT, with four sample points
          per resolution element, using the fast scan option.
          For the bright targets, an integration time
          of one second per sample point will yield a high S/N ratio, and
          we will not obtain a complementary offset sky spectrum, since
          the targets will be much brighter than the sky. The required
          spacecraft time will therefore be 532 seconds per target.
          For the fainter targets, for which integration times of two
          seconds per sample point will be used, offset sky spectra will
          be obtained and the required spacecraft time for the whole LWS
          observation will be 1208 seconds per target.

SWS AOT's:
            Complete SWS spectra of many of our targets are scheduled to be
            obtained by the SWS Consortium (proposals by de Jong
            et al., Waters et al. and Beintema et al.). We will obtain
            SWS spectra of the remaining targets.
            The low-resolution SWS grating scan AOT, SWS01, will be used
            to obtain complete 2.43-45um SWS spectra at one eighth of
            the standard grating resolution. The additional spacecraft time
            required to obtain a complete SWS spectrum of this type is
            956 seconds (one second detector reset time; speed code 1).
            We will observe all but three of the sources
            in this mode, whose resolving power matches that
            of the LWS grating mode. The exceptions are
            two sources suspected of having strong 44um ice emission
            bands (IRAS14541-4204 and IRAS18059-3211) and one known to do
            so (IRAS09371+1212). They each have low 25um IRAS fluxes
            and were not detected at 12um, so they will
            be observed for 32 minutes each, from 29.5-45.2um only, using
            the SWS full-resolution grating mode with the AOT SWS06.


SPACECRAFT TIME SUMMARY:

Orion-hole observable (Spring launch)      Sgr-hole observable (Autumn launch)

Priority 1 time = 11.04 hrs  (38.9%)       Priority 1 time = 10.82 hrs  (38.9%)
Priority 2 time =  8.40 hrs  (29.6%)       Priority 2 time =  8.07 hrs  (29.0%)
Priority 3 time =  8.96 hrs  (31.5%)       Priority 3 time =  8.96 mins (32.1%)

Total S/C  time = 28.39 hrs                Total S/C time  = 27.86 hrs




Time distribution for spring launch targets:

        Team    top 40%    second 30%    last 30%
        LWS :    39740       30224        32244
      total :    39740       30224        32244

Time distribution for autumn launch targets:

        Team    top 40%    second 30%    last 30%
        LWS :    38968       29068        32244
      total :    38968       29068        32244



<=== autumn_launch_targets ===>
 1, "LWS01", 1.0, "N", "W Aql",     19.21156,  -7.13556, 1950, 0.,0.,532,0
 2, "LWS01", 1.0, "N", "Chi Cyg",   19.81069, +32.78667, 1950, 0.,0.,684,3
 3, "LWS01", 1.0, "N", "Chi Cyg off", 19.81069, +32.88667, 1950, 0.,0.,524,0
 4, "LWS01", 1.0, "N", "Pi1 Gru",   22.32811, -46.20056, 1950, 0.,0.,532,0
 5, "LWS01", 1.0, "N", "R Scl",      1.41108, -32.80139, 1950, 0.,0.,532,0
 6, "LWS01", 3.0, "N", "U Cam",      3.62467, +62.48833, 1950, 0.,0.,684,7
 7, "LWS01", 3.0, "N", "U Cam off",  3.62467, +62.58833, 1950, 0.,0.,524,0
 8, "LWS01", 1.0, "N", "U Ant",     10.54983, -39.30361, 1950, 0.,0.,532,0
 9, "LWS01", 2.0, "N", "AX Sgr",    18.09222, -18.56333, 1950, 0.,0.,532,10
10, "SWS01", 2.0, "N", "AX Sgr",    18.09222, -18.56333, 1950, 0.,0.,956,0
11, "LWS01", 3.0, "N", "S Sct",     18.79364,  -7.96639, 1950, 0.,0.,684,12
12, "LWS01", 3.0, "N", "S Sct off", 18.79364,  -7.86639, 1950, 0.,0.,524,0
13, "LWS01", 1.0, "N", "R Aqr",     23.68731, -15.56167, 1950, 0.,0.,684,14
14, "LWS01", 1.0, "N", "R Aqr off", 23.68731, -15.66167, 1950, 0.,0.,524,0
15, "LWS01", 3.0, "N", "UW Cen",    12.67386, -54.15417, 1950, 0.,0.,684,16
16, "LWS01", 3.0, "N", "UW Cen off",  12.67386, -54.25417, 1950, 0.,0.,524,17
17, "SWS01", 3.0, "N", "UW Cen",    12.67386, -54.15417, 1950, 0.,0.,956,0
18, "LWS01", 1.0, "N", "AC Her",    18.46911, +21.83056, 1950, 0.,0.,684,19
19, "LWS01", 1.0, "N", "AC Her off",  18.46911, +21.93056, 1950, 0.,0.,524,0
20, "LWS01", 1.0, "N", "HD 101584", 11.64275, -55.29694, 1950, 0.,0.,532,0
21, "LWS01", 3.0, "N", "Boomerang", 12.69856, -54.24722, 1950, 0.,0.,684,22
22, "LWS01", 3.0, "N", "Boomerang off", 12.69856, -54.34722, 1950, 0.,0.,524,23
23, "SWS01", 3.0, "N", "Boomerang", 12.69856, -54.24722, 1950, 0.,0.,956,0
24, "LWS01", 3.0, "N", "IRAS14541", 14.90425, -42.07472, 1950, 0.,0.,684,25
25, "LWS01", 3.0, "N", "IRAS14541 off", 14.90425, -42.17472, 1950, 0.,0.,524,26
26, "SWS06", 3.0, "N", "IRAS14541", 14.90425, -42.07472, 1950, 0.,0.,1730,0
27, "LWS01", 3.0, "N", "IRAS16342", 16.57139, -38.23750, 1950, 0.,0.,532,28
28, "SWS01", 3.0, "N", "IRAS16342", 16.57139, -38.23750, 1950, 0.,0.,956,0
29, "LWS01", 2.0, "N", "OH349.36",  17.25111, -37.91500, 1950, 0.,0.,532,30
30, "SWS01", 2.0, "N", "OH349.36",  17.25111, -37.91500, 1950, 0.,0.,956,0
31, "LWS01", 3.0, "N", "IRAS17347", 17.57942, -31.65306, 1950, 0.,0.,532,0
32, "LWS01", 1.0, "N", "HD 161796", 17.72814, +50.06306, 1950, 0.,0.,532,0
33, "LWS01", 1.0, "N", "89 Her",    17.89003, +26.05639, 1950, 0.,0.,532,0
34, "LWS01", 2.0, "N", "IRAS18059", 18.09944, -32.18944, 1950, 0.,0.,684,35
35, "LWS01", 2.0, "N", "IRAS18059 off", 18.09944, -32.28944, 1950, 0.,0.,524,36
36, "SWS06", 2.0, "N", "IRAS18059", 18.09944, -32.18944, 1950, 0.,0.,1730,0
37, "LWS01", 3.0, "N", "MWC 922",   18.30742, -13.04833, 1950, 0.,0.,532,38
38, "SWS01", 3.0, "N", "MWC 922",   18.30742, -13.04833, 1950, 0.,0.,956,0
39, "LWS01", 1.0, "N", "OH17.7",    18.46106, -14.51778, 1950, 0.,0.,532,0



<=== spring_launch_targets ===>
 1, "LWS01", 3.0, "N", "RS Cnc",     9.12717, +31.16806, 1950, 0.,0.,684,2
 2, "LWS01", 3.0, "N", "RS Cnc off",  9.12717, +31.16806, 1950, 0.,0.,524,3
 3, "SWS01", 3.0, "N", "RS Cnc",     9.12717, +31.16806, 1950, 0.,0.,956,0
 4, "LWS01", 1.0, "N", "W Aql",     19.21156,  -7.13556, 1950, 0.,0.,532,0
 5, "LWS01", 1.0, "N", "Chi Cyg",   19.81069, +32.78667, 1950, 0.,0.,684,6
 6, "LWS01", 1.0, "N", "Chi Cyg off", 19.81069, +32.88667, 1950, 0.,0.,524,0
 7, "LWS01", 1.0, "N", "Pi1 Gru",   22.32811, -46.20056, 1950, 0.,0.,532,0
 8, "LWS01", 1.0, "N", "R Scl",      1.41108, -32.80139, 1950, 0.,0.,532,0
 9, "LWS01", 3.0, "N", "U Cam",      3.62467, +62.48833, 1950, 0.,0.,684,10
10, "LWS01", 3.0, "N", "U Cam off",  3.62467, +62.58833, 1950, 0.,0.,524,0
11, "LWS01", 1.0, "N", "U Ant",     10.54983, -39.30361, 1950, 0.,0.,532,0
12, "LWS01", 1.0, "N", "UV Aur",    5.30925, +32.45917, 1950, 0.,0.,1115,13
13, "LWS01", 1.0, "N", "UV Aur off", 5.30925, +32.55917, 1950, 0.,0.,955,0
14, "LWS01", 3.0, "N", "RX Pup",    8.20783, -41.55500, 1950, 0.,0.,684,15
15, "LWS01", 3.0, "N", "RX Pup off", 8.20783, -41.65500, 1950, 0.,0.,524,0
16, "LWS01", 1.0, "N", "R Aqr",     23.68731, -15.56167, 1950, 0.,0.,684,17
17, "LWS01", 1.0, "N", "R Aqr off", 23.68731, -15.66167, 1950, 0.,0.,524,0
18, "LWS01", 2.0, "N", "UW Cen",    12.67386, -54.15417, 1950, 0.,0.,684,19
19, "LWS01", 2.0, "N", "UW Cen off",  12.67386, -54.25417, 1950, 0.,0.,524,20
20, "SWS01", 2.0, "N", "UW Cen",    12.67386, -54.15417, 1950, 0.,0.,956,0
21, "LWS01", 2.0, "N", "U Mon",     7.47339,  -9.67056, 1950, 0.,0.,684,22
22, "LWS01", 2.0, "N", "U Mon off",  7.47339,  -9.77056, 1950, 0.,0.,524,0
23, "LWS01", 1.0, "N", "IRAS04296", 4.49453, +34.49806, 1950, 0.,0.,684,24
24, "LWS01", 1.0, "N", "IRAS04296 off", 4.49453, +34.59806, 1950, 0.,0.,524,0
25, "LWS01", 1.0, "N", "AFGL 618",  4.65939, +36.02083, 1950, 0.,0.,532,0
26, "LWS01", 3.0, "N", "IRAS05506", 5.84442, +24.23639, 1950, 0.,0.,532,27
27, "SWS01", 3.0, "N", "IRAS05506", 5.84442, +24.23639, 1950, 0.,0.,956,0
28, "LWS01", 1.0, "N", "HD 44179",  6.29358, -10.61417, 1950, 0.,0.,532,0
29, "LWS01", 1.0, "N", "SAO 96709", 7.22372, +10.08556, 1950, 0.,0.,684,30
30, "LWS01", 1.0, "N", "SAO 96709 off", 7.22372, +10.18556, 1950, 0.,0.,524,0
31, "LWS01", 2.0, "N", "IRAS07173", 7.28950, -17.56139, 1950, 0.,0.,532,32
32, "SWS01", 2.0, "N", "IRAS07173", 7.28950, -17.56139, 1950, 0.,0.,956,0
33, "LWS01", 1.0, "N", "231.8+4.2", 7.66636, -14.59556, 1950, 0.,0.,532,0
34, "LWS01", 3.0, "N", "HD 65750",  7.93181, -58.99028, 1950, 0.,0.,532,0
35, "LWS01", 3.0, "N", "IRAS08351", 8.58531, -46.57083, 1950, 0.,0.,684,36
36, "LWS01", 3.0, "N", "IRAS08351 off", 8.58531, -46.67083, 1950, 0.,0.,524,37
37, "SWS01", 3.0, "N", "IRAS08351", 8.58531, -46.57083, 1950, 0.,0.,956,0
38, "LWS01", 1.0, "N", "IRAS09371", 9.62000, +12.20861, 1950, 0.,0.,684,39
39, "LWS01", 1.0, "N", "IRAS09371 off", 9.62000, +12.30861, 1950, 0.,0.,524,40
40, "SWS06", 1.0, "N", "IRAS09371", 9.62000, +12.20861, 1950, 0.,0.,1730,0
41, "LWS01", 1.0, "N", "HD 101584", 11.64275, -55.29694, 1950, 0.,0.,532,0
42, "LWS01", 3.0, "N", "Boomerang", 12.69856, -54.24722, 1950, 0.,0.,684,43
43, "LWS01", 3.0, "N", "Boomerang off", 12.69856, -54.34722, 1950, 0.,0.,524,44
44, "SWS01", 3.0, "N", "Boomerang", 12.69856, -54.24722, 1950, 0.,0.,956,0