<=== observer ===>
"SDRAPATZ",\
"Drapatz, S.",\
"",\
"Max-Planck-Institut fuer extraterrestrische Physik",\
"Giessenbachstrasse",\
"1603",\
"85740",\
"Garching b. Muenchen",\
"Germany",\
"49 89 32993880",\
"49 89 32993569",\
"timmer%mpei2@mpe.mpe-garching.mpg.de"
<=== proposal ===>
"MPEWARM2", 1, 2,\
{"circumstellar envelopes",\
"young stellar objects",\
"HII regions",\
"supernova remnants",\
"molecular clouds"},\
{"T. de Graauw",\
"B. Draine",\
"R. Genzel",\
"D. Hollenbach",\
"A. Moorwood",\
"E. Oliva",\
"J. Puget",\
"A. Sternberg",\
"R. Timmermann",\
"P. van der Werf",\
"E. van Dishoeck"}
<=== title ===>
Physical and Chemical Conditions in Dense, Warm Instellar Gas, Part 2 of 2
<=== abstract ===>
SCIENTIFIC ABSTRACT
The warm (100 - 5000 K), dense (n(H_2) > 10^3 cm^-3) interstellar
medium is a decisive component of the whole interstellar medium and is
closely coupled to key processes like star formation and evolution. It
is heated through a wide variety of astrophysically important processes
such as shocks of various types, X-ray irradiation, UV irradiation of
interface regions near HII regions, and stellar radiation in the environment
of young objects. A rich variety of lines in the IR and submm wavelength
region will provide a unique opportunity to investigate the physics,
chemistry and interrelation of corresponding phenomena by multi-line
spectroscopy of various molecules, atoms and ions. However, since allmost
all lines cannot be observed from ground based telescopes or even from an
airborne observatory (KAO) ISO would offer the first and only possibility
for this investigation.
We have selected four classes of objects each representing different
processes that heat the gas: (1.) photon-dominated regions at the
interfaces of HII regions (including reflection nebulae), (2.) shocks of
various types: strong shocks (J-type) in supernova remnants and moderate
or weak shocks (also C-type) in outflow sources, (3.) embedded sources
(star formation) where dust is radiatively heated by the central source
and gas is heated by dust, and (4.) regions of X-ray excitation.
For each class a small number of prototypical, bright sources and a
set of spectral lines in the ISO wavelength range has been selected.
The set of radiative transitions is selected thus that a maximum of
information can be gained for each individual class of objects.
Much emphasis is placed on the observation of (faint) important lines
rather than on mapping because of time constraints by the faintness of some of
the crucial lines. Using these sources as a kind of templates we also establish
a set of crucial lines with which different processes can be distinguished.
The primary target lines for all four classes are the rotational
transitions of H_2 in order to study directly the bulk of the warm gas.
Through observation of rotational transitions in oxygen-bearing
species such as OH, H_2O, and H_2^{18}O, and O_2, the oxygen
chemistry in interstellar clouds will be studied for the first time via direct
determination of all important reactants rather than by default.
Most of these molecules serve also as a major coolant and therefore their
abundances have a great impact on the energy balance of the warm molecular gas.
This balance is also determined by the cooling of fine-structure lines
where their contribution will be studied through a set of diagnostically
useful transitions.
We also propose the observation of a few selected rovibrational transitions
in molecular ions that become quite abundant in objects where the gas is excited
through X-ray irradiation. This unique possibility will enable us to get a
handle on that process. In a few objects where the gas is cold (T < 30 K)
absorption measurements will be performed. The study of the lowest
rotational transitions of H_2 and HD will provide a first and accurate
determination of their total column density in this general environment.
These observations are closely related to the emission measurements mentioned
above. Furthermore, a series of transitions in the first fundamental band
of H_2O, H_2^{18}O, CH_4, and CO_2 will be observed. Since a detailed
scientific proposal would by far exceed the granted space we include a list of
lines for each class of objects in the scientific justification.
OBSERVATION SUMMARY
We plan to take advantage of the spectroscopic capabilities of ISO over its
full wavelength range, using the following AOTs:
SWS: Medium and high resolution spectroscopy with the AOTs SWS01,SWS02,
SWS06,SWS07
LWS: Medium resolution full grating scans and high resolution line scans
with AOTs LWS01,LWS04
A detailed description of our observing strategy and outline of integration
times exceeds the limits of this abstract.
<=== scientific_justification ===>
Time distribution for spring launch targets
--------------------------------------------------
Team Total top 40% second 30% last 30%
SWS 275579 110054 84874 80651
AFM 10800 10800 0 0
JLP 18764 7488 7488 3744
TDG 7200 7200 0 0
--------------------------------------------------
total 312299 135542 92362 84395
Time distribution for autumn launch targets
--------------------------------------------------
Team Total top 40% second 30% last 30%
SWS 269087 105379 84224 79484
AFM 10800 10800 0 0
JLP 18764 7488 7488 3744
TDG 0 0 0 0
--------------------------------------------------
total 298607 123667 91712 83228
The following two tables contain the targets in their specific templates
that will be observed for the Orion hole and the Galactic center visibility
holes, respectively. The numbers specify the total observation time in
hours.
autumn launch targets:
----------------------
Object Priority
--------------------------------------------------------------------------------
1 2 3
--------------------------------------------------------------------------------
PDR: M17 7.53 2.00 1.00
S140 4.04
S106 4.04
--------------------------------------------------------------------------------
Refl. Nebulae: NGC 7023 2.35 2.11
R Cr A 3.17
IC 1396 3.17
--------------------------------------------------------------------------------
Shocks: DR 21 9.20
RCW 103 3.94
Cep A 8.89
W 28 A2 6.60
M 8E IRS1 2.29
--------------------------------------------------------------------------------
Emb. Sources: W3 (OH) 2.90
W51 IRS 2 1.90
NGC 7538 IRS1 2.90
--------------------------------------------------------------------------------
X-Ray heat. Sources: RCW 103 2.08
SN 1987A 2.20
SS 433 2.20
--------------------------------------------------------------------------------
Absorp. Spectr.: Sgr A West 2.86 2.86
W51 IRS2 2.30
Sgr B2 1.40 1.00
--------------------------------------------------------------------------------
spring launch targets:
----------------------
Object Priority
--------------------------------------------------------------------------------
1 2 3
--------------------------------------------------------------------------------
PDR: Orion 8.04
DR 21 2.65
S106 4.04
--------------------------------------------------------------------------------
Refl. Nebulae: NGC 1977 4.28
NGC 2023 3.60
Parsamyan 18 2.11
--------------------------------------------------------------------------------
Shocks: Orion BN/KL 8.72 2.03
IC 443 5.54
DR 21 7.57
Cep A 7.29
--------------------------------------------------------------------------------
Emb. Sources: W3 (OH) 1.90
NGC 2170 IRS2 2.90
T Tau 2.90
NGC 7538 IRS1 1.90
--------------------------------------------------------------------------------
X-Ray heat. Sources: IC 443 2.20
SN 1987A 2.20
Crab Nebula 2.08
SS 433 2.20
--------------------------------------------------------------------------------
Absorp. Spectr.: Orion IRc2 2.30
NGC 2170 IRS2 2.30
W51 IRS2 2.86
--------------------------------------------------------------------------------
The following tables specify the lines that will be observed for different
templates. The integration times have been calculated such that at least a S/N
ratio of 20 is achieved for each individual line. For fainter lines such as the
H2 v=0->0 S(0) transition where the integration times would become much too
long the integration time has been limited to 1200 sec (in special cases
3600 sec).
Table 1: Lines to be observed for PDRs near bright HII regions.
____________________________________________________
Line lambda AOT
[mu]
----------------------------------------------------
H_2 28.2188 SWS07
H_2 9.6649 SWS02
H_2 8.0251 SWS02
H_2 17.0348 SWS07
H_2 4.6933 SWS02
H_2 12.2786 SWS02
[SiII] 34.8160 SWS07
H_2 6.9095 SWS02
H_2 3.8451 SWS02
[FeIII] 22.93 SWS02
H_2 5.5097 SWS02
H_2 4.1801 SWS02
[NeIII] 15.55 SWS02
H_2 2.6262 SWS02
H_2 2.8017 SWS02
H_2 2.5503 SWS02
H_2 2.72 SWS02
HI n=13->9 14.1831 SWS02
OH 34.6035 SWS07
H_2O 40.6909 SWS07
H_2O 28.9137 SWS07
[FeII] 25.9882 SWS07
HI n=6->5 7.4599 SWS02
HD 112.1076 LWS04
[NII] 121.8981 LWS04
[CII] 157.740 LWS04
H_2O 113.54 LWS04
H_2O 125.35 LWS04
H_2O 179.53 LWS04
H_2^18O 181.05 LWS04
LWS scan (selected sources) 45-180 LWS01
---------------------------------------------------
Table 2: Lines to be observed for reflection nebulae.
____________________________________________________
Line lambda AOT
[mu]
----------------------------------------------------
H_2 28.2188 SWS02
H_2 9.6649 SWS02
H_2 8.0251 SWS02
H_2 17.0348 SWS02
H_2 6.9095 SWS02
H_2 12.2786 SWS02
[SiII] 34.8160 SWS02
OH 34.6035 SWS07
H_2O 40.6909 SWS07
H_2O 28.9137 SWS07
HI n=6->5 7.4599 SWS02
H_2 2.6262 SWS02
H_2 2.8017 SWS02
H_2 2.5503 SWS02
H_2 2.72 SWS02
HI n=13->9 14.1831 SWS02
HD 112.1076 LWS04
[NII] 121.8981 LWS04
[CII] 157.740 LWS04
H_2O 113.54 LWS04
H_2O 125.35 LWS04
H_2O 179.53 LWS04
H_2^18O 181.05 LWS04
LWS scan (selected sources) 45-180 LWS01
---------------------------------------------------
Table 3: Individual lines to be observed for shocked molecular gas.
____________________________________________________
Line lambda AOT
[mu]
----------------------------------------------------
H_2 28.2188 SWS07
HD 10.8719 SWS02
H_2 17.0348 SWS07
H_2 4.1809 SWS02
H_2 3.8451 SWS02
H_2 12.2786 SWS02
[SiII] 34.8160 SWS02
H_2 9.6649 SWS02
H_2O 35.4259 SWS07
H_2 8.0251 SWS02
H_2O 29.8366 SWS07
H_2 6.9095 SWS02
[SI] 25.2490 SWS02
H_2 5.5111 SWS02
HD 19.4326 SWS02
H_2 4.6924 SWS02
[FeII] 25.9882 SWS02
HD 28.5063 SWS07
HD 12.4812 SWS02
HD 37.7074 SWS07
HD 11.5915 SWS02
HD 23.0309 SWS02
H_2 3.23 SWS02
HD 16.8947 SWS02
[NiII] 6.634 SWS02
HD 15.0218 SWS02
H_2 2.6262 SWS02
H_2 2.8017 SWS02
H_2 3.00 SWS02
HD 13.5980 SWS02
H_2 2.553 SWS02
OH 34.6035 SWS07
OH 28.940 SWS07
HI n=6->5 7.4599 SWS02
H_2O 40.3367 SWS07
H_2O 31.7720 SWS07
OH 43.949 SWS02
HI n=7->6 12.3719 SWS02
H_2O 45.1114 SWS02
H_2O 43.3393 SWS02
H_2O 40.6909 SWS07
OH 44.666 SWS02
OH 39.514 SWS07
HI n=8->6 7.5025 SWS02
[NeII] 12.8149 SWS02
[NiI] 7.505 SWS02
OH 24.642 SWS07
H_3^+ 3.9530 SWS02
[SiVIII] 18.45 SWS02
HeH^+ 3.61 SWS02
[FeI] 24.04 SWS07
^12CO 4.6 SWS06
O_2 165.4113 LWS04
LWS scan (selected sources) 45-180 LWS01
H_2O 43.3407 SWS02
H_2O 71.5396 LWS04
H_2O 71.9467 LWS04
H_2O 74.9445 LWS04
H_2O 99.4926 SWS07
H_2O 96.1710 SWS07
H_2O 49.2817 LWS04
H_2O 28.9137 SWS07
H_2O 121.721 LWS04
H_2^18O 41.1599 SWS07
H_2O (not Orion) 125.524 LWS04
H_2O (not Orion) 113.538 LWS04
H_2O 179.527 LWS04
H_2^18O 181.049 LWS04
H_2O (not Orion) 82.031 LWS04
[SiI] 129.68 LWS04
[SiI] 68.474 LWS04
CH 149.091 LWS04
CH 149.390 LWS04
NH_3 124.91 LWS04
NH_3 124.88 LWS04
NH_3 124.80 LWS04
NH_3 124.65 LWS04
OH 163.121 LWS04
OH 163.396 LWS04
OH 119.441 LWS04
OH 119.234 LWS04
^18OH 120.172 LWS04
^18OH 119.966 LWS04
----------------------------------------------------
Table 4: Lines to be observed for shocked gas in the ionized parts of SNRs.
____________________________________________________
Line lambda AOT
[mu]
----------------------------------------------------
[FeII] 5.339 SWS02
[FeII] 17.9533 SWS02
[ArIII] 8.9910 SWS02
[FeII] 35.3491 SWS02
[PII] 32.87 SWS02
[NeIII] 36.02 SWS02
[FeIII] 33.04 SWS02
[NeVI] 7.642 SWS02
[FeI] 24.04 SWS02
[MgV] 5.609 SWS02
[SIII] 33.482 SWS02
[SIV] 10.5105 SWS02
[NeIII] 15.55 SWS02
[ArII] 6.9853 SWS02
[FII] 29.33 SWS02
[NiI] 7.505 SWS02
[NiIII] 7.347 SWS02
[NeII] 12.8149 SWS02
[SiII] 34.8160 SWS02
[OIV] 25.87 SWS02
[MgIV] 4.487 SWS02
[NiII] 6.634 SWS02
[SI] 25.2490 SWS02
[ClII] 33.281 SWS02
[ClI] 11.3333 SWS02
[SiIX] 2.584 SWS02
[ClII] 14.3678 SWS02
[NeV] 14.32 SWS02
HI Br alpha 4.0423 SWS02
[SIII] 18.7129 SWS02
[FI] 24.745 SWS02
[FeII] 25.9882 SWS02
[FeIII] 22.93 SWS02
[ArIII] 21.84 SWS02
[NeV] 24.28 SWS02
[SiIX] 3.92 SWS02
[NII] 121.8981 LWS04
[CII] 157.740 LWS04
[OIII] 88.356 LWS04
[OIII] 51.815 LWS04
[SiI] 129.68 LWS04
[SiI] 68.474 LWS04
[NIII] 57.317 LWS04
-----------------------------------------------------
Table 5: Lines to be observed for gas heated by embedded objects.
____________________________________________________
Line lambda AOT
[mu]
----------------------------------------------------
H_2 28.2188 SWS07
H_2 1) 17.0302 SWS02
H_2 6.9095 SWS02
H_2 3.23 SWS02
H_2 1) 12.2786 SWS02
H_2O 40.6909 SWS07
H_2 9.6649 SWS02
OH 2) 34.6035 SWS07
HI Pf alpha 2) 7.46 SWS02
H_2O 29.8366 SWS07
H_2O 2) 31.7720 SWS07
H_2O 45.1114 SWS02
HD 112.1076 LWS04
HD 56.2114 LWS04
H_2^18O 41.1599 SWS07
H_2O 49.2817 LWS04
H_2O 2) 28.9137 SWS07
H_2O 99.4926 SWS07
H_2O 96.1710 SWS07
H_2O 121.721 LWS04
H_2^18O 41.1599 SWS07
H_2O (not Orion) 125.524 LWS04
H_2O (not Orion) 113.538 LWS04
H_2O 179.527 LWS04
H_2^18O 181.049 LWS04
H_2O (not Orion) 82.031 LWS04
CH 149.091 LWS04
CH 149.390 LWS04
NH_3 124.91 LWS04
NH_3 124.88 LWS04
NH_3 124.80 LWS04
NH_3 124.65 LWS04
OH 2) 163.121 LWS04
OH 2) 163.396 LWS04
OH 119.441 LWS04
OH 119.234 LWS04
^18OH 120.172 LWS04
^18OH 119.966 LWS04
O_2 165.4113 LWS04
LWS scan (selected sources) 45-180 LWS01
-----------------------------------------------------
1) SWS07 for T Tau
2) not for T Tau
Table 6: Lines to be observed for X-ray excited gas.
____________________________________________________
Line lambda AOT
[mu]
----------------------------------------------------
H_2 9.6649 SWS02
[SiII] 34.8160 SWS02
H_2O 40.3367 SWS02
H_2O 39.3991 SWS02
[OIV] 25.87 SWS02
HI Br alpha 4.051 SWS02
H_2 4.6946 SWS02
[SiVIII] 18.45 SWS02
HeH^+ 3.61 SWS02
H_3^+ 16.331 SWS02
H_3^+ 3.953 SWS02
[NII] 121.898 LWS04
[CII] 157.740 LWS04
----------------------------------------------------
Table 7: Lines observed for absorption spectroscopy.
____________________________________________________
Line lambda AOT
[mu]
----------------------------------------------------
H_2 28.2188 SWS07
H_2 17.0348 SWS07
HD 112.1076 LWS04
O_2 165.4113 LWS04
H_2O 100.983 LWS04
H_2O 179.527 LWS04
H_2^18O 181.049 LWS04
____________________________________________________
CH_4 nu_4 band (not Orion) 7.40-7.65 SWS06
CH_4 nu_3 band (not Orion) 3.2-3.4 SWS06
----------------------------------------------------
<=== autumn_launch_targets ===>
1, "SWS02", 1.,"N", "W3(OH) ", 02.38806, +61.65000, 1950, 0.,0., 1236,3
2, "SWS07", 1.,"N", "W3(OH) ", 02.38806, +61.65000, 1950, 0.,0., 5606,0
3, "LWS04", 1.,"N", "W3(OH) ", 02.38806, +61.64500, 1950, 0.,0., 3190,0
4, "SWS07", 1.,"N", "W51 IRS2 ", 19.35622, +14.42028, 1950, 0.,0., 6842,0
5, "SWS02", 3.,"N", "NGC 7538 IRS1 ", 23.19358, +61.19806, 1950, 0.,0., 1236,0
6, "SWS07", 3.,"N", "NGC 7538 IRS1 ", 23.19358, +61.19806, 1950, 0.,0., 5606,0
8, "LWS04", 3.,"N", "NGC 7538 IRS1 ", 23.19358, +61.19806, 1950, 0.,0., 3686,0
9, "SWS02", 1.,"N", "RCW103 H2 ", 16.23056, -50.98694, 1950, 0.,0., 7476,0
10, "LWS01", 1.,"N", "RCW103 H2 ", 16.23056, -50.98694, 1950, 0.,0., 496,11
11, "LWS04", 1.,"N", "RCW103 H2 ", 16.23056, -50.98694, 1950, 0.,0., 476,0
12, "SWS02", 2.,"N", "SN1987A ", 05.59725, -69.29944, 1950, 0.,0., 7476,13
13, "LWS01", 2.,"N", "SN1987A ", 05.59725, -69.29944, 1950, 0.,0., 496,0
14, "SWS02", 2.,"N", "SS 433 knot5 ", 19.09167, +04.82778, 1950, 0.,0., 3738,15
15, "LWS01", 2.,"N", "SS 433 knot5 ", 19.09167, +04.82778, 1950, 0.,0., 496,0
16, "SWS02", 2.,"N", "SS 433 knot3 ", 19.10972, +05.04167, 1950, 0.,0., 3738,17
17, "LWS01", 2.,"N", "SS 433 knot3 ", 19.10972, +05.04167, 1950, 0.,0., 496,0
18, "LWS04", 1.,"N", "Sgr B2 ", 17.73617, -28.36722, 1950, 0.,0., 2000,0
19, "SWS07", 1.,"N", "Sgr B2 ", 17.73617, -28.36722, 1950, 0.,0., 3040,0
20, "SWS07", 2.,"N", "Sgr A West 1 ", 17.70767, -28.98861, 1950, 0.,0.,10280,0
22, "SWS07", 1.,"N", "W51 IRS2 ", 19.35622, +14.42028, 1950, 0.,0., 8280,0
23, "LWS04", 2.,"N", "Sgr B2 ", 17.73617, -28.36722, 1950, 0.,0., 3600,0
<=== spring_launch_targets ===>
1, "SWS02", 1.,"N", "W3(OH) ", 02.38806, +61.65000, 1950, 0.,0., 1236,2
2, "SWS07", 1.,"N", "W3(OH) ", 02.38806, +61.65000, 1950, 0.,0., 5606,0
3, "SWS02", 2.,"N", "NGC 2170 IRS2 ", 06.08872, -06.37333, 1950, 0.,0., 1236,4
4, "SWS07", 2.,"N", "NGC 2170 IRS2 ", 06.08872, -06.37333, 1950, 0.,0., 2185,0
6, "LWS04", 2.,"N", "NGC 2170 IRS2 ", 06.08872, -06.37333, 1950, 0.,0., 3686,0
7, "SWS02", 2.,"N", "NGC 2170 IRS3 ", 06.08933, -06.37500, 1950, 0.,0., 1236,8
8, "SWS07", 2.,"N", "NGC 2170 IRS3 ", 06.08933, -06.37500, 1950, 0.,0., 2185,0
9, "SWS02", 2.,"N", "T Tau ", 04.31783, +19.41806, 1950, 0.,0., 1236,10
10, "SWS07", 2.,"N", "T Tau ", 04.31783, +19.41806, 1950, 0.,0., 5606,0
11, "LWS01", 2.,"N", "T Tau ", 04.31783, +19.41806, 1950, 0.,0., 496,12
12, "LWS04", 2.,"N", "T Tau ", 04.31783, +19.41806, 1950, 0.,0., 3190,0
13, "SWS02", 3.,"N", "NGC 7538 IRS1 ", 23.19358, +61.19806, 1950, 0.,0., 1236,14
14, "SWS07", 3.,"N", "NGC 7538 IRS1 ", 23.19358, +61.19806, 1950, 0.,0., 5606,0
15, "SWS02", 3.,"N", "SN1987A ", 05.59722, -69.29944, 1950, 0.,0., 7476,16
16, "LWS01", 3.,"N", "SN1987A ", 05.59722, -69.29944, 1950, 0.,0., 496,0
17, "SWS02", 3.,"N", "Crab pos1 ", 05.52483, +21.99944, 1950, 0.,0., 3738,0
18, "SWS02", 3.,"N", "Crab pos2 ", 05.52383, +21.97250, 1950, 0.,0., 3738,0
19, "SWS02", 1.,"N", "IC443 H2 pos2 ", 06.24489, +22.38444, 1950, 0.,0., 7476,0
20, "SWS02", 2.,"N", "SS 433 knot5 ", 19.09167, +04.82778, 1950, 0.,0., 3738,21
21, "LWS01", 2.,"N", "SS 433 knot5 ", 19.09167, +04.82778, 1950, 0.,0., 496,0
22, "SWS02", 2.,"N", "SS 433 knot3 ", 19.10972, +05.04167, 1950, 0.,0., 3738,23
23, "LWS01", 2.,"N", "SS 433 knot3 ", 19.10972, +05.04167, 1950, 0.,0., 496,0
24, "SWS07", 1.,"N", "Orion IRc2 ", 05.54633, -05.40694, 1950, 0.,0., 8280,0
25, "SWS07", 3.,"N", "NGC 2170 IRS3 ", 06.08933, -06.37500, 1950, 0.,0., 8280,0
26, "SWS07", 1.,"N", "W51 IRS2 ", 19.35622, +14.42028, 1950, 0.,0., 8280,0
27, "LWS04", 1.,"N", "W51 IRS2 ", 19.35622, +14.42028, 1950, 0.,0., 2000,0
28, "SWS07", 2.,"N", "Sgr A West 1 ", 17.70767, -28.98861, 1950, 0.,0., 420,0
29, "SWS02", 3.,"N", "Orion IRc2 map", 05.53855, -05.40750, 1950, 0.,0., 420,30
30, "SWS02", 3.,"N", "Orion IRc2 map", 05.54244, -05.40750, 1950, 0.,0., 260,31
31, "SWS02", 3.,"N", "Orion IRc2 map", 05.54633, -05.40750, 1950, 0.,0., 260,32
32, "SWS02", 3.,"N", "Orion IRc2 map", 05.55022, -05.40750, 1950, 0.,0., 260,33
33, "SWS02", 3.,"N", "Orion IRc2 map", 05.55411, -05.40750, 1950, 0.,0., 260,34
34, "SWS02", 3.,"N", "Orion IRc2 map", 05.53855, -05.40722, 1950, 0.,0., 260,35
35, "SWS02", 3.,"N", "Orion IRc2 map", 05.54244, -05.40722, 1950, 0.,0., 260,36
36, "SWS02", 3.,"N", "Orion IRc2 map", 05.54633, -05.40722, 1950, 0.,0., 260,37
37, "SWS02", 3.,"N", "Orion IRc2 map", 05.55022, -05.40722, 1950, 0.,0., 260,38
38, "SWS02", 3.,"N", "Orion IRc2 map", 05.55411, -05.40722, 1950, 0.,0., 260,39
39, "SWS02", 3.,"N", "Orion IRc2 map", 05.53855, -05.40694, 1950, 0.,0., 260,40
40, "SWS02", 3.,"N", "Orion IRc2 map", 05.54244, -05.40694, 1950, 0.,0., 260,41
41, "SWS02", 3.,"N", "Orion IRc2 map", 05.54633, -05.40694, 1950, 0.,0., 260,42
42, "SWS02", 3.,"N", "Orion IRc2 map", 05.55022, -05.40694, 1950, 0.,0., 260,43
43, "SWS02", 3.,"N", "Orion IRc2 map", 05.55411, -05.40694, 1950, 0.,0., 260,44
44, "SWS02", 3.,"N", "Orion IRc2 map", 05.53855, -05.40666, 1950, 0.,0., 260,45
45, "SWS02", 3.,"N", "Orion IRc2 map", 05.54244, -05.40666, 1950, 0.,0., 260,46
46, "SWS02", 3.,"N", "Orion IRc2 map", 05.54633, -05.40666, 1950, 0.,0., 260,47
47, "SWS02", 3.,"N", "Orion IRc2 map", 05.55022, -05.40666, 1950, 0.,0., 260,48
48, "SWS02", 3.,"N", "Orion IRc2 map", 05.55411, -05.40666, 1950, 0.,0., 260,49
49, "SWS02", 3.,"N", "Orion IRc2 map", 05.53855, -05.40638, 1950, 0.,0., 260,50
50, "SWS02", 3.,"N", "Orion IRc2 map", 05.54244, -05.40638, 1950, 0.,0., 260,51
51, "SWS02", 3.,"N", "Orion IRc2 map", 05.54633, -05.40638, 1950, 0.,0., 260,52
52, "SWS02", 3.,"N", "Orion IRc2 map", 05.55022, -05.40638, 1950, 0.,0., 260,53
53, "SWS02", 3.,"N", "Orion IRc2 map", 05.55411, -05.40638, 1950, 0.,0., 260,0