<=== observer ===>
"PCOX",\
"Cox, P.",\
"",\
"Observatoire de Marseille",\
"2, Place Le Verrier",\
"",\
"13004",\
"Marseille",\
"France",\
"33 91959088",\
"33 91621190",\
"cox@obmara.cnrs-mrs.fr"
<=== proposal ===>
"ISM_IV01",1,2,\
{"HII regions","diffuse interstellar medium",\
"molecular clouds","star formation"},\
{"Churchwell, E.","Cassinelli, J.P.","Jourdain de Muizon",\
"LWS consortium","SWS Consortium",\
"Kessler, M."}\
<=== title ===>
CHEMICAL AND PHYSICAL CHARACTERISATION OF COMPACT HII REGIONS
ACROSS THE GALAXY
- PART 1 OF 2-
<=== abstract ===>
SCIENTIFIC ABSTRACT
It is proposed to use the ISO Long Wavelength Spectrometer (LWS), the Short
Wavelength Spectrometer (SWS) and the Camera (CAM) to investigate the infrared
spectra of compact HII regions. The selected sample of 60 sources covers in a
nearly homogeneous way the galactic plane from the center out to 25 kpc.
Together with the study of the physical conditions pertaining in these regions
of recent massive star formation, this will enable us to investigate in great
detail the problem of the present-day abundance distribution in the Galaxy. The
study of chemical abundances and their variation as a function of the distance
to the galactic center is of fundamental importance for our understanding of
galactic evolution. The abundances of heavy elements in the interstellar medium
provides a direct estimate of the enrichment due to nucleosynthesis in
successive generations of stars. The variation of one element relative to
another yields information on the formation paths of these elements. A detailed
knowledge of the abundance variation within a galaxy is a prerequisite to a
wide variety of studies such as the large scale distribution of the infrared
radiation, gamma rays and cosmic rays.
The infrared fine-structure lines are better suited than the optical lines (as
usually used) for abundance analysis in the Galaxy for two reasons. First, the
infrared lines are comparatively insensitive to the electron temperature so
that the correction for electron temperature, crucial in the optical studies,
is not required. Second, infrared lines are less attenuated by interstellar
extinction than their optical counterparts and provide a probe of the elemental
abundances through the galactic disk (although substantial extinction
corrections are still necessary), in particular in the inner regions, at
galactocentric distances less than 6 kpc where no optical measurements are
possible.
OBSERVATION SUMMARY
The compact HII regions have been selected according to the following criteria:
(1) The sources should be compact so as to be included in the field of view of
the Short Wavelength Spectrometer (20 arsec x 20 arcsec) and isolated so as to
avoid confusion problems with the larger field of view of the Long Wavelength
Spectrometer (1.65 arcmin).
(2) The sample should be uniformly distributed in galactocentric distance.
Compact HII regions near the galactic center (only observable in the infrared
and radio wavelengths) and sources associated with the molecular ring (at 5 kpc,
where HII regions are expected to be numerous and share similar abundance
properties) should be well represented in the sample.
(3) The selection is mainly based on both the sample of about 200 compact HII
regions extracted from the IRAS-LRS database (see Jourdain de Muizon et al.,
1989, A&A Suppl. 83, 337) and the study of star-forming regions in the outer
galaxy by Wouterloot and Brand (1990, A&A Suppl. 80, 149) for the sources at
distances greater than 10 kpc from the galactic centre.
(4) The fluxes in the four IRAS bands (12, 25, 60 and 100 um) should be strong
so as to minimize the integration times: the infrared luminosity of compact HII
regions being nearly equal to the luminosity output of the exciting star,
strong infrared fluxes should indicate strong fluxes in the fine-structure
lines. However we relaxed this criteria for regions far away from the galactic
centre (i.e. at distances greater than 15 kpc).
The final sample contains 60 sources which are presented in Table 1.
Due to time constraints a sub-sample of 30 sources was extracted for
observations with SWS and CAM.
<=== scientific_justification ===>
The galactocentric distances of the selected compact HII regions cover the
range from 0 to 24 kpc in a nearly homogeneous way (3 sources in average per
kiloparsec bin). In order to study the dispersion in the abundances at a given
distance from the galactic centre, we selected a larger number of sources at 2
positions, namely in the 5 kpc arm and at around 14 kpc.
TABLE 1:
--------------------------------------------------------------------------------
priority
Orion GC IRAS fluxes R_g size
name bands LWSWto LWSWto 12 25 60 100 (kpc) (")
----------------------------------------------------------------------
00468+6527 3 3 3 3 5 44 303 320 13.2
01420+6401 3 3 2 2 3 11 128 232 16.8
02044+6031 1234 L 2 1 1 2 1 1 12 105 387 465 13.1 20
02044+6031 * (W3) 2 2 2 2 2 2 696 1780 10590 12981 10.3 35
02575+6017 * 234 2 2 2 3 2 2 20 212 768 1083 10.2 30
02383+6241 3 3 3 3 3 11 150 248 16.1
02395+6244 1 1 1 1 1 1 10 91 255 226 16.2 30
04025+5313 1 1 1 1 2 5 45 64 19.2
05167+3858 1 1 2 2 1 2 35 85 22.6
05221+4139 1 1 1 1 3 15 117 138 18.4
05236+3828 3 3 3 3 4 5 120 237 14.4
05302+3739 3 3 2 2 1 1 7 22 21.9
05335+3609 3 2 2 2 7 21 45 24.2
05375+3540 LRS ***1 2 2 28 226 1708 1635 14.0 60
05393-0156 1234 L 3 3 284 4746 7894 35331 9.0 65
05588+2625 3 1 1 4 16 121 171 23.1
06084+1727 2 2 3 25 124 261 15.9
06145+1455 2 2 1 3 37 73 20.3
06158+1517 2 2 2 9 23 234 337 17.7 45
06208+0957 3 3 4 35 206 243 15.3
06412-0105 1234 L 1 1 14 159 612 532 14.9 45
06495+0217 3 3 2 2 34 82 17.1
08189-3602 1234 L 3 3 3 3 53 360 1781 2059 13.6 45
08282-4545 3 3 3 3 152 6 33 37 17.1
10589-6034 1234 L 3 3 3 3 40 313 1722 2109 11.0 45
11143-6113 1234 L 1 1 1 1 1 1 25 197 682 1389 11.2 30
12063-6259 1234 L 1 1 1 1 1 1 50 407 1819 2233 10.8 30
12073-6233 1234 L 2 2 2 2 577 4084 10672 11344 11.6 45
12331-6134 1234 L 2 2 3 3 49 230 1643 2589 8.6 45
15290-5546 1234 L 3 3 3 1 1 47 501 4824 6893 5.9 30
15384-5348 1234 L 3 2 2 94 607 5820 8348 7.8 45
15502-5302 1234 L 1 1 1 1 1 142 1210 11570 12440 5.3 30
15567-5236 1234 L 3 3 3 1 1 195 1076 7390 8360 5.1 30
16128-5109 1234 L 3 3 129 1069 6243 8409 6.7 60
17160-3707 1234 L 1 1 1 45 335 4246 10230 3.0 30
17221-3619 1234 L 2 2 3 2 42 245 2643 4669 6.1 45
17279-3350 1234 L 2 2 2 1 1 1 25 166 1239 3947 3.6 45
17455-2800 1234 L 1 1 1 1 1 1 83 469 2541 5487 0.2 30
18116-1646 1234 L 1 1 1 3 3 3 75 477 3619 6074 4.9 30
18162-2048 * 1234 1 1 1 1 1 1 26 347 2771 3709 6.8 30
18311-0809 LRS 3 3 3 3 27 184 1550 2947 4.2 60
18316-0602 * 1234 3 3 3 3 3 3 23 138 958 2136 5.9 30
18317-0757 1234 L 3 3 3 3 3 3 66 393 2252 3361 5.1 30
18434-0242 1234 L 2 2 2 1 1 1 217 1697 7504 11530 5.1 30
18469-0132 * 1234 2 1 1 1 1 1 25 224 1726 3390 4.5 30
18479-0005 1234 L 2 2 2 3 2 2 32 298 3705 5473 9.0 30
18502+0051 1234 L 3 2 2 3 2 2 29 250 1452 2240 5.6 30
19110+1045 * 1234 L 2 2 2 3 2 2 58 494 5913 7486 7.1 30
19207+1410 1234 L 1 1 1 1 1 1 93 524 4930 7431 7.6 30
19442+2427 * 1234 1 1 1 1 1 1 47 425 3447 5174 8.0 30
19598+3324 * (K3-50) 1 1 1 1 1 1 302 1780 10590 12981 9.9 10
DR21 * (no IRAS3 2 2 3 2 2 8.4 30
20406+4555 3 3 3 3 7 17 267 436 14.0
21190+5140 1234 L 1 1 1 1 1 1 39 337 590 406 15.0 20
21561+5806 3 3 3 3 2 6 51 80 14.1
21569+5923 3 3 3 2 2 31 61 14.9
22308+5812 1234 L 1 1 1 1 1 1 25 175 873 1038 12.4 20
22475+5939 1234 L 3 2 2 3 2 2 25 151 832 1066 12.3 30
23030+5958 1234 L 1 1 1 1 1 1 40 259 1549 1833 13.6 20
23133+6050 1234 L 2 1 1 2 1 1 45 579 2098 2694 12.8 30
--------------------------------------------------------------------------------
The priorities affected to the sources are given under the columns "priority".
Orion means "visibility hole on Orion", GC means "visibility hole in
Sagittarius" and LW, SW and to means LWS, SWS and total respectively.
The distribution in galactocentric radius split up into priorities with the two
different launch dates is as follows:
Distributions: Orion GC Totals
1 2 3 1 2 3 All Ori GC
R_g
2 1 0 0 1 0 0 1 1 1
4 1 1 0 1 0 0 2 2 1
6 3 2 5 2 1 4 10 10 7
8 3 3 1 3 2 0 7 7 5
10 1 3 0 1 2 2 5 4 5
12 2 3 1 2 3 1 6 6 6
14 4 1 3 4 2 3 9 8 9
16 1 0 3 1 3 2 7 4 6
18 1 0 3 1 2 3 6 4 6
20 2 0 0 2 0 0 2 2 2
22 0 0 1 0 2 0 2 1 2
24 1 0 0 1 1 0 2 1 2
26 0 0 0 0 1 0 1 0 1
total: 60 50 53
AOTs:
LWS01:
Systematic LWS grating spectra of all visible targets is proposed. Because the
sources are relatively bright the signal to noise ratio in the grating spectrum
is believed to be close to 100 for the majority of them. These spectra will
provide the intensities of the main lines coming from the compact HII region
itself but also from the associated photodissociation region, together with the
information on the emissivity of the dust which is responsible of the
underlying continuum. Since the sources are essentially bright, "off-source"
positions are not considered in this proposal except for specific targets where
source confusion is foreseen from IRAS maps.
Table 2 gives the brightest lines likely to be readily detected with the LWS
grating spectra. These spectra will gather at the same time the three most
important elements, Carbon, Nitrogen and Oxygen, which are obvious tracers of
the chemical evolution of our Galaxy (CNO cycle).
TABLE 2:
--------------------------------------------------------------------------------
Atom Log number Transition Wavelength Ionisation potential
abundance (um) range (eV)
--------------------------------------------------------------------------------
Oxygen 8.82 [OIII] 51.8 35.11-54.93
Oxygen 8.82 [OIII] 88.4 35.11-54.93
Oxygen 8.82 [OI] 63.2 0-13.62
Oxygen 8.82 [OI] 145.5 0-13.62
Carbon 8.52 [CII] 157.7 11.26-24.38
Nitrogen 7.96 [NII] 121.7 14.53-29.60
Nitrogen 7.96 [NIII] 57.33 29.60-16.34
--------------------------------------------------------------------------------
Some CO lines, at high J levels, could be detected in some sources directly
from their LWS grating spectrum since these lines are currently predicted to be
emitted from some parts of the photodissociation region and/or from shocked
regions at a sufficiently high level of intensity.
LWS04:
The other lines need the high spectral resolution capability of the LWS to
be used. For the brightest sources, with flux density greater than 5000 Jy at
100 um, we intend to measure 8 lines using the LWS FPs. The interest of these
lines are summarized hereafter:
1) The [13CII] line exhibits three distinct spectral components at 11.2, 63.2
and -65.2 km/sec relative to the [12CII] line, with relative intensities of
0.44, 0.20 and 0.36 respectively (Cooksy et al., 1986, Ap J Letters 305, L89).
The detection of these components clearly need the high spectral resolution of
the LWS for separation from the bright [12CII] line.
2) Three rotational lines of CO are considered for measurements with the
LWS FPs namely the transitions at 93.35 um (J=28-27), 137.20 um (J=19-18) and
186.00 um (J=14-13). These three lines will provide the information on the
physical state of the emitting region, at least its density and temperature.
3) One line of 13CO at 143.49 um (J=19-18) is proposed for detection. This
measurement will yield the true isotopic ratio 12C/13C since the high
rotational lines of CO are expected to be optically thin. This will allow the
interpretation of the [CII] line by suppressing the ambiguity due to potential
optical thickness.
4) Two forbidden lines of [SiI] at 68.47 and 129.68 um and one of [AlI] at
89.25 um are proposed to be searched for. Little is presently known about the
detectability of these lines from cool molecular regions but first results of
the COBE mission (Wright et al., 1991, preprint) indicate a marginal detection
of the 129.68 um [SiI] line. This later line needs low energy for collisional
excitation of the upper level of the transition, i.e. about 10 meV. Detection
of these lines will provide for the first time direct information about the
kinetic temperature of the emitting regions and may justify this search in the
bright sources of our sample.
SWS02:
Table 3 gives the lines which are proposed to be observed with the SWS for all
the sources within the SWS sub-sample. These lines originate from elements,
such as Neon and Sulfur, for which total abundances can be derived because
different ionization stages are accessible in the spectral domain of SWS.
Other lines, namely from Iron and Silicon, are considered in order to try to
give some clues on the formation/destruction mechanism of dust particles.
Apart from their importance in deriving the elemental abundances of Ne and S,
the fine-structure lines of [NeIII] and [SIII] provide a good diagnostic of the
internal density structure of the ionized region which is an essential
parameter for the interpretation of the line strength in the infrared. Moreover
the measurement of the [NeII] and [NeIII] lines, and the [SIII] and [SIV] lines
will provide the necessary information to derive the ionization structure of
the source. One [FeII] line, issued from a low energy level, is considered for
detection. Due to the low ionization energy required to produce [FeII], from 8
to 16 eV, a substantial contribution to the line intensity is expected to arise
from the photodissociation region.
TABLE 3:
--------------------------------------------------------------------------------
Atom Log number Transition Wavelength Ionisation potential
abundance (um) range (eV)
--------------------------------------------------------------------------------
Hydrogen 12.0 H4 alpha 4.051 0-13.60
Hydrogen 12.0 H9 alpha 38.87 0-13.60
Neon 7.92 [NeII] 12.80 21.56-40.96
Neon 7.92 [NeIII] 15.56 40.96-63.45
Magnesium 7.42 [MgIV] 4.50 80.14-109.31
Silicon 7.52 [SiII] 34.82 8.15-16.34
Sulphur 7.20 [SIII] 18.71 23.33-34.83
Sulphur 7.20 [SIV] 10.50 34.83-47.30
Iron 7.60 [FeII] 35.35 7.87-16.16
Iron 7.60 [FeIII] 22.90 16.16-30.65
Iron 7.60 [FeVI] 7.81 75.5-100
Iron 7.60 [FeVII] 9.51 100-128.3
--------------------------------------------------------------------------------
CAM01:
We propose to observe each source with CAM to get an impression of the source
structure. Since all of them are relatively strong, they can be observed in the
minimum CAM integration time. All sources will be observed in the CAM LW9 band
(at 15 micron) and at a shorter wavelength LW4 (6 micron).
Time distribution for autumn launch targets:
Team top 40% second 30% last 30%
LWS: 6140 4356 9228
SOT-LWS: 8640 6480 6480
SWS: 14686 4934 0
SOT-SWS: 8640 7528 5432
Time distribution for spring launch targets:
Team top 40% second 30% last 30%
LWS: 6640 3980 9552
SOT-LWS: 8640 6480 6480
SWS: 14686 4864 230
SOT-SWS: 8640 6480 6480
<=== autumn_launch_targets ===>
1, "LWS01",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0., 656,2
2, "SWS02",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0.,1118,3
3, "CAM01",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0., 80,4
4, "CAM01",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0., 80,0
5, "LWS01",1.0,"N","IRAS 04025+5313 ",04.04258,+53.22944,1950,0.,0., 656,0
6, "LWS01",1.0,"N","IRAS 05167+3858 ",05.27892,+38.97194,1950,0.,0., 656,0
7, "LWS01",1.0,"N","IRAS 05221+4139 ",05.36869,+41.65361,1950,0.,0., 656,0
8, "LWS01",1.0,"N","IRAS 05375+3540 ",05.62558,+35.11083,1950,0.,0., 656,0
9, "SWS02",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0.,1278,10
10,"LWS01",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0., 496,11
11,"CAM01",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0., 80,12
12,"CAM01",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0., 80,0
13,"LWS01",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0., 656,14
14,"SWS02",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0.,1118,15
15,"CAM01",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0., 80,16
16,"CAM01",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0., 80,0
17,"SWS02",1.0,"N","IRAS 15502-5302 ",15.83797,-53.04611,1950,0.,0.,1278,18
18,"LWS01",1.0,"N","IRAS 15502-5302 ",15.83797,-53.04611,1950,0.,0., 496,19
19,"LWS04",1.0,"N","IRAS 15502-5302 ",15.83797,-53.04611,1950,0.,0., 696,20
20,"CAM01",1.0,"N","IRAS 15502-5302 ",15.83797,-53.04611,1950,0.,0., 80,21
21,"CAM01",1.0,"N","IRAS 15502-5302 ",15.83797,-53.04611,1950,0.,0., 80,0
22,"LWS01",1.0,"N","IRAS 17160-3707 ",17.26739,-37.13056,1950,0.,0., 656,23
23,"LWS04",1.0,"N","IRAS 17160-3707 ",17.26739,-37.13056,1950,0.,0., 696,24
24,"SWS02",1.0,"N","IRAS 17160-3707 ",17.26739,-37.13056,1950,0.,0.,1118,25
25,"CAM01",1.0,"N","IRAS 17160-3707 ",17.26739,-37.13056,1950,0.,0., 80,26
26,"CAM01",1.0,"N","IRAS 17160-3707 ",17.26739,-37.13056,1950,0.,0., 80,0
27,"SWS02",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0.,1278,28
28,"LWS01",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0., 496,29
29,"LWS04",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0.,1356,30
30,"CAM01",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0., 80,31
31,"CAM01",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0., 80,0
32,"LWS01",1.0,"N","IRAS 18116-1646 ",18.19483,-16.77167,1950,0.,0., 656,33
33,"SWS02",1.0,"N","IRAS 18116-1646 ",18.19483,-16.77167,1950,0.,0.,1118,34
34,"CAM01",1.0,"N","IRAS 18116-1646 ",18.19483,-16.77167,1950,0.,0., 80,35
35,"CAM01",1.0,"N","IRAS 18116-1646 ",18.19483,-16.77167,1950,0.,0., 80,0
36,"SWS02",1.0,"N","IRAS 18162-2048 ",18.27028,-20.81344,1950,0.,0.,1278,37
37,"CAM01",1.0,"N","IRAS 18162-2048 ",18.27028,-20.81344,1950,0.,0., 80,38
38,"CAM01",1.0,"N","IRAS 18162-2048 ",18.27028,-20.81344,1950,0.,0., 80,0
39,"LWS01",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 656,40
40,"LWS04",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 940,41
41,"SWS02",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0.,1118,42
42,"CAM01",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 80,43
43,"CAM01",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 80,0
44,"SWS02",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0.,1278,45
45,"LWS04",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0.,1356,46
46,"CAM01",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0., 80,47
47,"CAM01",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0., 80,0
48,"LWS01",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 656,49
49,"LWS04",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 696,50
50,"SWS02",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0.,1118,51
51,"CAM01",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 80,52
52,"CAM01",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 80,0
53,"SWS02",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0.,1278,54
54,"LWS01",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0., 496,55
55,"CAM01",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0., 80,56
56,"CAM01",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0., 80,0
57,"LWS01",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0., 656,58
58,"SWS02",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0.,1118,59
59,"CAM01",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0., 80,60
60,"CAM01",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0., 80,0
61,"SWS02",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0.,1278,62
62,"LWS01",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0., 496,63
63,"CAM01",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0., 80,64
64,"CAM01",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0., 80,0
65,"LWS01",2.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0., 656,0
66,"SWS02",1.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0.,1278,67
67,"CAM01",1.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0., 80,68
68,"CAM01",1.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0., 80,0
69,"LWS01",2.0,"N","IRAS 02575+6017 ",02.95961,+60.28983,1950,0.,0., 656,70
70,"SWS02",2.0,"N","IRAS 02575+6017 ",02.95961,+60.28983,1950,0.,0.,1118,71
71,"CAM01",2.0,"N","IRAS 02575+6017 ",02.95961,+60.28983,1950,0.,0., 80,72
72,"CAM01",2.0,"N","IRAS 02575+6017 ",02.95961,+60.28983,1950,0.,0., 80,0
73,"LWS01",2.0,"N","IRAS 12073-6233 ",12.12269,-62.55417,1950,0.,0., 656,74
74,"LWS04",2.0,"N","IRAS 12073-6233 ",12.12269,-62.55417,1950,0.,0., 696,0
75,"LWS01",2.0,"N","IRAS 12331-6134 ",12.55264,-61.57583,1950,0.,0., 656,0
76,"LWS01",2.0,"N","IRAS 17221-3619 ",17.36928,-36.32111,1950,0.,0., 656,0
77,"SWS02",2.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0.,1278,78
78,"LWS01",2.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0., 496,79
79,"CAM01",2.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0., 80,80
80,"CAM01",2.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0., 80,0
81,"LWS01",2.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 656,82
82,"LWS04",2.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 696,83
83,"SWS02",2.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0.,1118,84
84,"CAM01",2.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 80,86
86,"CAM01",2.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 80,0
87,"LWS01",2.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0., 656,0
88,"SWS02",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0.,1278,89
89,"CAM01",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0., 80,90
90,"CAM01",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0., 80,0
91,"SWS02",2.0,"N","IRAS 18479-0005 ",18.79917,-00.09250,1950,0.,0.,1278,92
92,"LWS01",2.0,"N","IRAS 18479-0005 ",18.79917,-00.09250,1950,0.,0., 496,93
93,"LWS04",2.0,"N","IRAS 18479-0005 ",18.79917,-00.09250,1950,0.,0.,1356,94
94,"CAM01",2.0,"N","IRAS 18479-0005 ",18.79917,-00.09250,1950,0.,0., 80,95
95,"CAM01",2.0,"N","IRAS 18479-0005 ",18.79917,-00.09250,1950,0.,0., 80,0
<=== spring_launch_targets ===>
1, "LWS01",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0., 656,2
2, "SWS02",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0.,1118,3
3, "CAM01",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0., 80,4
4, "CAM01",1.0,"N","IRAS 02395+6244 ",02.65850,+62.73944,1950,0.,0., 80,0
5, "LWS01",1.0,"N","IRAS 04025+5313 ",04.04258,+53.22944,1950,0.,0., 656,0
6, "LWS01",1.0,"N","IRAS 05221+4139 ",05.36869,+41.65361,1950,0.,0., 656,0
7, "LWS01",1.0,"N","IRAS 05588+2625 ",05.98011,+26.41694,1950,0.,0., 656,0
8, "SWS02",1.0,"N","IRAS 06412-0105 ",06.68681,-01.08389,1950,0.,0.,1278,94
9, "SWS02",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0.,1278,10
10,"LWS01",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0., 496,11
11,"CAM01",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0., 80,12
12,"CAM01",1.0,"N","IRAS 11143-6113 ",11.23992,-61.22667,1950,0.,0., 80,0
13,"LWS01",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0., 656,14
14,"SWS02",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0.,1118,15
15,"CAM01",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0., 80,16
16,"CAM01",1.0,"N","IRAS 12063-6259 ",12.10639,-62.98694,1950,0.,0., 80,0
17,"SWS02",1.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0.,1278,18
18,"LWS01",1.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0., 496,19
19,"CAM01",1.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0., 80,20
20,"CAM01",1.0,"N","IRAS 17279-3350 ",17.46661,-33.84361,1950,0.,0., 80,0
21,"LWS01",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0., 656,22
22,"LWS04",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0.,1356,23
23,"SWS02",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0.,1118,24
24,"CAM01",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0., 80,25
25,"CAM01",1.0,"N","IRAS 17455-2800 ",17.75897,-28.01167,1950,0.,0., 80,0
26,"SWS02",1.0,"N","IRAS 18162-2048 ",18.27028,-20.81344,1950,0.,0.,1278,27
27,"CAM01",1.0,"N","IRAS 18162-2048 ",18.27028,-20.81344,1950,0.,0., 80,28
28,"CAM01",1.0,"N","IRAS 18162-2048 ",18.27028,-20.81344,1950,0.,0., 80,0
29,"LWS01",1.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 656,30
30,"LWS04",1.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 696,31
31,"SWS02",1.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0.,1118,32
32,"CAM01",1.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 80,33
33,"CAM01",1.0,"N","IRAS 18434-0242 ",18.72422,-02.70972,1950,0.,0., 80,0
34,"SWS02",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0.,1278,35
35,"LWS01",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0., 496,36
36,"LWS04",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0.,1356,37
37,"CAM01",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0., 80,38
38,"CAM01",1.0,"N","IRAS 18469-0132 ",18.78264,-01.54253,1950,0.,0., 80,0
39,"LWS01",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 656,40
40,"LWS04",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 940,41
41,"SWS02",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0.,1118,42
42,"CAM01",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 80,43
43,"CAM01",1.0,"N","IRAS 19207+1410 ",19.34572,+14.18056,1950,0.,0., 80,0
44,"SWS02",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0.,1278,45
45,"LWS04",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0.,1356,46
46,"CAM01",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0., 80,47
47,"CAM01",1.0,"N","IRAS 19442+2427 ",19.73714,+24.46806,1950,0.,0., 80,0
48,"LWS01",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 656,49
49,"LWS04",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 696,50
50,"SWS02",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0.,1118,51
51,"CAM01",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 80,52
52,"CAM01",1.0,"N","IRAS 19598+3324 ",19.99723,+33.40542,1950,0.,0., 80,0
53,"SWS02",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0.,1278,54
54,"LWS01",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0., 496,55
55,"CAM01",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0., 80,56
56,"CAM01",1.0,"N","IRAS 21190+5140 ",21.31825,+51.67750,1950,0.,0., 80,0
57,"LWS01",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0., 656,58
58,"SWS02",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0.,1118,59
59,"CAM01",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0., 80,60
60,"CAM01",1.0,"N","IRAS 22308+5812 ",22.51469,+58.21444,1950,0.,0., 80,0
61,"SWS02",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0.,1278,62
62,"LWS01",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0., 496,63
63,"CAM01",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0., 80,64
64,"CAM01",1.0,"N","IRAS 23030+5958 ",23.05136,+59.97444,1950,0.,0., 80,0
65,"LWS01",2.0,"N","IRAS 01420+6401 ",01.70153,+64.01694,1950,0.,0., 656,0
67,"LWS01",2.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0., 656,0
68,"SWS02",1.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0.,1278,69
69,"CAM01",1.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0., 80,70
70,"CAM01",1.0,"N","IRAS 02044+6031 ",02.07475,+60.52861,1950,0.,0., 80,0
71,"LWS01",2.0,"N","IRAS 05167+3858 ",05.27892,+38.97194,1950,0.,0., 656,0
72,"LWS01",2.0,"N","IRAS 05302+3739 ",05.50422,+37.65139,1950,0.,0., 656,0
73,"LWS01",2.0,"N","IRAS 05335+3609 ",05.55842,+36.15333,1950,0.,0., 656,0
74,"LWS01",2.0,"N","IRAS 05375+3540 ",05.62558,+35.11083,1950,0.,0., 656,0
75,"LWS01",2.0,"N","IRAS 06084+1727 ",06.14161,+17.45278,1950,0.,0., 656,0
76,"LWS01",2.0,"N","IRAS 06145+1455 ",06.24242,+14.93111,1950,0.,0., 656,0
77,"LWS01",2.0,"N","IRAS 06158+1517 ",06.26469,+15.29972,1950,0.,0., 656,78
78,"SWS02",2.0,"N","IRAS 06158+1517 ",06.26469,+15.29972,1950,0.,0.,1118,79
79,"CAM01",2.0,"N","IRAS 06158+1517 ",06.26469,+15.29972,1950,0.,0., 80,80
80,"CAM01",2.0,"N","IRAS 06158+1517 ",06.26469,+15.29972,1950,0.,0., 80,0
81,"LWS01",2.0,"N","IRAS 12073-6233 ",12.12269,-62.55417,1950,0.,0., 656,82
82,"LWS04",2.0,"N","IRAS 12073-6233 ",12.12269,-62.55417,1950,0.,0., 696,0
83,"LWS01",2.0,"N","IRAS 23133+6050 ",23.22264,+60.84611,1950,0.,0., 656,84
84,"LWS04",2.0,"N","IRAS 23133+6050 ",23.22264,+60.84611,1950,0.,0.,1356,0
85,"SWS02",1.0,"N","IRAS 23133+6050 ",23.22264,+60.84611,1950,0.,0.,1278,86
86,"CAM01",1.0,"N","IRAS 23133+6050 ",23.22264,+60.84611,1950,0.,0., 80,87
87,"CAM01",1.0,"N","IRAS 23133+6050 ",23.22264,+60.84611,1950,0.,0., 80,0
88,"SWS02",2.0,"N","W3 02219+6125 ",02.36586,+61.87778,1950,0.,0.,1278,89
89,"LWS01",2.0,"N","W3 02219+6125 ",02.36586,+61.87778,1950,0.,0., 496,90
90,"LWS04",2.0,"N","W3 02219+6125 ",02.36586,+61.87778,1950,0.,0., 696,91
91,"CAM01",2.0,"N","W3 02219+6125 ",02.36586,+61.87778,1950,0.,0., 80,92
92,"CAM01",2.0,"N","W3 02219+6125 ",02.36586,+61.87778,1950,0.,0., 80,0
93,"LWS01",1.0,"N","IRAS 06412-0105 ",06.68681,-01.08389,1950,0.,0., 496,94
94,"CAM01",1.0,"N","IRAS 06412-0105 ",06.68681,-01.08389,1950,0.,0., 80,95
95,"CAM01",1.0,"N","IRAS 06412-0105 ",06.68681,-01.08389,1950,0.,0., 80,0