<=== observer ===>
"MMORRIS",\
"Morris, M.",\
"UCLA",\
"Dept. of Astronomy-156205",\
"",\
"8979 Math-Scien",\
"",\
"Los Angeles, CA",\
"USA",\
"1 310 8253320",\
"1 310 2062096",\
"morris@osprey.astro.ucla.edu"
<=== proposal ===>
"GCSHOCK", 1, 2,\
{"abundances",\
"molecular clouds",\
"supernova remnants"},\
{"E.F. van Dishoeck",\
"Leiden Observatory",\
"P.O. Box 9513",\
"2300 RA Leiden",\
"The Netherlands",\
"H.J. Habing",\
"Leiden Observatory",\
"P.O. Box 9513",\
"2300 RA Leiden",\
"The Netherlands"}
<=== title ===>
LARGE-SCALE SHOCKS IN THE GALACTIC CENTER AND OTHER REGIONS
<=== abstract ===>
SCIENTIFIC ABSTRACT
Molecular gas within a few hundred parsecs of the Galactic center
displays considerable non-circular motion, perhaps as a response of the
gas to a central bar potential, or as a result of one or more violent
releases of energy in the past. The tumult characterizing molecular
cloud kinematics there is accompanied by strong shock interactions between
clouds, or between clouds and the ambient medium. We propose to
investigate, with 3.1 hours of ISO time, two examples of large-scale
shocks in the Galactic center region: AFGL 5376 and G-0.02-0.07.
In case the Galactic center is not visible, we propose instead
to study the shock in B35 near the lambda Orionis ring and
to map the H2O distribution in the SNR IC 443 for a total of 6 hr.
AFGL5376 is an unusually strong 25-micron infrared source which coincides with
a remarkable vertical shock rising almost 100 pc above the galactic plane at a
projected distance of 75 pc from the Galactic center. The shock is inferred
from a sharp discontinuity in the anomalous-velocity CO emission at this
location. G-0.02-0.07 is a series of compact HII regions aligned along the
interface between the dense, massive 50 km/s molecular cloud and the Sgr A
East nonthermal radio source with which it is interacting. The stars in these
HII regions may have formed as a result of cloud compression by a shock
associated with the expansion of Sgr A East, or as a result of the collision
of two clouds.
Both systems provide an unprecedented opportunity to study shocks under
very different conditions than encountered normally (large size, extreme
velocities, large magnetic fields). Since shocks radiate primarily in
the infrared, ISO will be uniquely qualified to study these regions and
to assess existing shock models in terms of their predictions for line
strengths. Comparison with more ``standard'' shocks such as Orion/KL and
IC 443 should help establish the importance of the high velocities and
strong fields. It will also be useful to compare the two proposed
sources with each other, inasmuch as their shocks may result from two
different causes.
In the case of the Sagittarius hole, both of our prime objects will be
unobservable. We propose in that case to observe the same lines in the shock
in the molecular cloud B35, which lies near the lambda Orionis ring. In
addition, we propose to map the H2O distribution in the IC 443 SNR shock in a
few lines. Although H2O will be observed in IC 443 in other proposals, these
are limited to only a few positions chosen on the basis of CO observations.
Observations of e.g. C I show that the various shock tracers do not
necessarily peak at the same position. Maps of the various clumps B, C, and G
in a few H2O lines would provide an unbiased view of the H2O distribution
through a shock (and its precursor) and would provide independent tests of the
models.
OBSERVATION SUMMARY
We propose to observe the fine structure lines of Fe I, Fe II, Fe II, S I, Si
II, Cl II and Ni II, and the pure rotational lines of H2, HD, OH and H2O using
SWS AOT02 and AOT7 at two positions within AFGL 5376 and one within
G-0.02-0.07. In addition, we will observe the longer wavelength lines of O I,
N II and C II and selected lines of H2O, OH and CO using the LWS AOT04 with 1
min/line. At position AFGL 5376-1, we will search for the atomic lines only.
The detailed lines are summarized in Table 1 in the Scientific Justification
section. The requested S/N on the continuum is 50-100 for the grating.
Fabry-Perot observations will be attempted for a few lines at S/N=10 on the
expected line strength. Concatenation of the SWS AOT2 and AOT7 observations is
required in order to have the same orientation of the slit on the source. It
is recommended for the LWS observations in order to save overhead for slewing.
In the case of the Galactic Center hole (spring launch), we propose to observe
the same lines in the shock in B35. In addition, we propose to map the various
clumps in IC 443 in the 179.527 mu o-H2O line with the LWS (100" beam, AOT02
or AOT04) and in the o-H2O 4_41-3_12 line at 31.7715 mu with the SWS (20"x40"
beam, most likely AOT07). We estimate an integration time of 2
min/raster point including overheads, which would allow detection of lines
with fluxes of 1E-15 W m-2 at a S/N>5 (SWS-FP) and 1E-17 W m-2 at a S/N>5
(LWS-Grating). The predicted line strengths are uncertain due to the
uncertain H2O abundance, excitation and beam filling factor. We therefore
suggest to carry out these observations at prior. 3, so that we can use the
results of the prior. 1 and 2 data of other IC 443 programs (in
which the co-I is involved) to optimize the observing strategy. For example,
if the lines are strong enough to be observed with the grating, we will use
LWS AOT02 so that several lines (p-H2O at 100.9828, o-H2O at 108.0730 and
75.3804 mu) can be observed simultaneously. The IC 443 clump G will be sampled
over a region of 1.5' x 3.0' (20 LWS points at 50" spacing, 35 SWS points at
30" step), and clumps B and C over 4' x 2' (32 LWS points at 50" step,
15 SWS points at 30" over smaller region). Detailed high-resolution CO 3-2
and/or C I maps of these regions at 20-30" have already been obtained.
<=== scientific_justification ===>
Autumn launch
TEAM: top 40% second 30% last 30%
SWS : 0. 0. 0.
LWS : 0. 0. 0.
CAM : 0. 0. 0.
PHT : 0. 0. 0.
SOT : 0. 0. 0.
THE : 0. 0. 0.
JLP : 0. 0. 0.
HJH : 4524. 4488. 2098.
AFM : 0. 0. 0.
MOH : 0. 0. 0.
Spring launch
TEAM: top 40% second 30% last 30%
SWS : 0. 0. 0.
LWS : 0. 0. 0.
CAM : 0. 0. 0.
PHT : 0. 0. 0.
SOT : 0. 0. 0.
THE : 0. 0. 0.
JLP : 0. 0. 0.
HJH : 0. 4489. 17111.
AFM : 0. 0. 0.
MOH : 0. 0. 0.
TABLE 1. SOURCE LIST: Orion Hole
==========================================================================
Source RA (1950) DEC IRAS FLUX (W/cm**2/sr)
-------------------------------------
12 25 60 100 mu
--------------------------------------------------------------------------
AFGL 5376-1 17 39 33.2 -29 06 45 7.4(-10) 1.9(-9)
AFGL 5376-2 17 39 51.9 -29 10 31 6.(-10) 2.1(-9)
G-0.02-0.07 17 42 40 -28 58 30 1.5(-8) 4.7(-8) 8.5(-8)** 6.6(-8)**
---------------------------------------------------------------------------
** saturated IRAS flux: lower limit
SOURCE LIST: Sagittarius hole
==============================================
Source RA (1950) DEC
----------------------------------------------
B 35 05 41 48 +09 08 07
IC443G map 06 13 41 +22 33 10
IC443B map 06 14 12 +22 26 50
IC443C map 06 14 42 +22 22 40
----------------------------------------------
TABLE 2. LINES TO BE OBSERVED IN AFGL 5376, G-0.02 AND B35
===========================================================================
Continuum Fluxes (Jy)
--------------------------------------------
Lambda Line GL 5376 G-0.02
mu ---------------------------
Pos. 1 Pos. 2
---------------------------------------------------------------------------
Grating:
3.84675 H2 S(13) 1.6e-3 4.1e-3 2.6e-2
4.18128 H2 S(11) 2.8e-3 7.0e-3 4.4e-2
4.69461 H2 S(9) 5.3e-3 1.4e-2 9.1e-2
5.51116 H2 S(7) 1.4e-2 4.3e-2 0.26
6.90952 H2 S(5) 4.6e-2 0.14 0.86
9.66491 H2 S(3) 0.18 0.40 3.09
10.6822 NiII 0.25 0.49 4.69
12.27861 H2 S(2) 0.38 0.61 4.05
12.813 Ne II 0.43 0.65 4.45
14.368 Cl II 0.57 0.76 8.5
17.03483 H2 S(1) 0.82 0.96 13.9
17.95 Fe II 0.92 1.02 16.5
22.93 Fe III 1.50 1.46 35.6
24.0424 Fe I 1.65 1.58 40.9
25.9882 Fe II 1.91 1.78 50.2
25.9402 o-H2O 5_41 - 4_14 1.00 0.95 50.0
28.21883 H2 S(0) 1.40 1.20 62.8
28.50197 HD R(3) 1.40 1.20 64.4
28.9138 p-H2O 4_40 - 3_13 1.45 1.25 66.7
28.94 OH 7/2 -- 5/2 1.45 1.25 66.7
31.7715 o-H2O 4_41 - 3_12 2.77 2.48 83.6
34.6294 OH 5/2 -- 3/2 3.30 2.96 99.0
34.814 Si II 3.33 3.00 101.
35.3491 Fe II 3.44 3.11 102.
37.70155 HD R(2) 2.50 2.05 114.
40.6904 o-H2O 4_32 - 3_03 2.65 2.30 128.
Fabry-Perot:
17.03483 H2 S(1) 0.82 0.96 13.9
25.9882 Fe II 1.91 1.78 50.2
31.7715 o-H2O 4_41 - 3_12 2.77 2.48 83.6
34.814 Si II 3.33 3.00 101.
LWS LINES AOT 4
119.4417 OH 5/2 + -- 3/2 - 648. 648. 3108.*
84.4204 OH 7/2 + -- 5/2 - 423. 527. 3537.*
180.4880 o-H2O 2_21 - 2_12 1386. 409. 1690.*
179.5265 o-H2O 2_12 - 1_01 1370. 413. 1710.*
174.6264 o-H2O 3_03 - 2_12 1300. 433. 1808.*
136.4944 o-H2O 3_30 - 3_21 806. 587. 2661.*
113.5366 o-H2O 4_14 - 3_03 602. 654. 3236.*
108.0730 o-H2O 2_21 - 1_10 572. 640. 3400.*
78.7414 o-H2O 4_23 - 3_12 376. 463. 3400.*
75.3804 o-H2O 3_21 - 2_12 348. 425. 3400.*
100.9828 p-H2O 2_20 - 1_11 532. 620. 3400.*
173.631 CO 15-14 1300. 435. 1800.*
100.461 CO 26-25 532. 620. 3400.*
181.0512 o-H218O 2_12 - 1_01 1390. 410. 1700.*
63.18 O I 242. 281. 3400.*
145.53 O I 890. 555. 2400.*
121.9 N II 670. 640. 3100.*
157.7 C II 1054. 505. 2200.*
------------------------------------------------------------------------
* IRAS 60 and 100 micron fluxes saturated
<=== autumn_launch_targets ===>
1, "SWS02", 3., "N", "AFGL 5376-1 ", 17.65922, -29.11250, 1950, 0., 0., 1502, 2
2, "SWS07", 3., "N", "AFGL 5376-1 ", 17.65922, -29.11250, 1950, 0., 0., 336, 3
3, "LWS04", 3., "N", "AFGL 5376-1 ", 17.65922, -29.11250, 1950, 0., 0., 260, 0
4, "SWS02", 1., "N", "AFGL 5376-2 ", 17.66442, -29.17528, 1950, 0., 0., 2704, 5
5, "SWS07", 1., "N", "AFGL 5376-2 ", 17.66442, -29.17528, 1950, 0., 0., 741, 6
6, "LWS04", 1., "N", "AFGL 5376-2 ", 17.66442, -29.17528, 1950, 0., 0., 1079, 0
7, "SWS02", 2., "N", "G-0.02-0.07 ", 17.71111, -28.97500, 1950, 0., 0., 2440, 8
8, "SWS07", 2., "N", "G-0.02-0.07 ", 17.71111, -28.97500, 1950, 0., 0., 969, 9
9, "LWS04", 2., "N", "G-0.02-0.07 ", 17.71111, -28.97500, 1950, 0., 0., 1079, 0
<=== spring_launch_targets ===>
1, "SWS07", 3., "N", "IC443G ", 6.21001, 22.52778, 1950, 0., 0., 247, 2
2, "SWS07", 3., "N", "IC443G ", 6.21903, 22.52778, 1950, 0., 0., 115, 3
3, "SWS07", 3., "N", "IC443G ", 6.22806, 22.52778, 1950, 0., 0., 115, 4
4, "SWS07", 3., "N", "IC443G ", 6.23708, 22.52778, 1950, 0., 0., 115, 5
5, "SWS07", 3., "N", "IC443G ", 6.24610, 22.52778, 1950, 0., 0., 115, 6
6, "SWS07", 3., "N", "IC443G ", 6.24610, 22.53611, 1950, 0., 0., 115, 7
7, "SWS07", 3., "N", "IC443G ", 6.23708, 22.53611, 1950, 0., 0., 115, 8
8, "SWS07", 3., "N", "IC443G ", 6.22806, 22.53611, 1950, 0., 0., 115, 9
9, "SWS07", 3., "N", "IC443G ", 6.21903, 22.53611, 1950, 0., 0., 115, 10
10, "SWS07", 3., "N", "IC443G ", 6.21001, 22.53611, 1950, 0., 0., 115, 11
11, "SWS07", 3., "N", "IC443G ", 6.21001, 22.54444, 1950, 0., 0., 115, 12
12, "SWS07", 3., "N", "IC443G ", 6.21903, 22.54444, 1950, 0., 0., 115, 13
13, "SWS07", 3., "N", "IC443G ", 6.22806, 22.54444, 1950, 0., 0., 115, 14
14, "SWS07", 3., "N", "IC443G ", 6.23708, 22.54444, 1950, 0., 0., 115, 15
15, "SWS07", 3., "N", "IC443G ", 6.24610, 22.54444, 1950, 0., 0., 115, 16
16, "SWS07", 3., "N", "IC443G ", 6.24610, 22.55278, 1950, 0., 0., 115, 17
17, "SWS07", 3., "N", "IC443G ", 6.23708, 22.55278, 1950, 0., 0., 115, 18
18, "SWS07", 3., "N", "IC443G ", 6.22806, 22.55278, 1950, 0., 0., 115, 19
19, "SWS07", 3., "N", "IC443G ", 6.21903, 22.55278, 1950, 0., 0., 115, 20
20, "SWS07", 3., "N", "IC443G ", 6.21001, 22.55278, 1950, 0., 0., 115, 21
21, "SWS07", 3., "N", "IC443G ", 6.21001, 22.56111, 1950, 0., 0., 115, 22
22, "SWS07", 3., "N", "IC443G ", 6.21903, 22.56111, 1950, 0., 0., 115, 23
23, "SWS07", 3., "N", "IC443G ", 6.22806, 22.56111, 1950, 0., 0., 115, 24
24, "SWS07", 3., "N", "IC443G ", 6.23708, 22.56111, 1950, 0., 0., 115, 25
25, "SWS07", 3., "N", "IC443G ", 6.24610, 22.56111, 1950, 0., 0., 115, 26
26, "SWS07", 3., "N", "IC443G ", 6.24610, 22.56944, 1950, 0., 0., 115, 27
27, "SWS07", 3., "N", "IC443G ", 6.23708, 22.56944, 1950, 0., 0., 115, 28
28, "SWS07", 3., "N", "IC443G ", 6.22806, 22.56944, 1950, 0., 0., 115, 29
29, "SWS07", 3., "N", "IC443G ", 6.21903, 22.56944, 1950, 0., 0., 115, 30
30, "SWS07", 3., "N", "IC443G ", 6.21001, 22.56944, 1950, 0., 0., 115, 31
31, "SWS07", 3., "N", "IC443G ", 6.21001, 22.57778, 1950, 0., 0., 115, 32
32, "SWS07", 3., "N", "IC443G ", 6.21903, 22.57778, 1950, 0., 0., 115, 33
33, "SWS07", 3., "N", "IC443G ", 6.22806, 22.57778, 1950, 0., 0., 115, 34
34, "SWS07", 3., "N", "IC443G ", 6.23708, 22.57778, 1950, 0., 0., 115, 35
35, "SWS07", 3., "N", "IC443G ", 6.24610, 22.57778, 1950, 0., 0., 115, 36
36, "LWS02", 3., "N", "IC443G ", 6.22806, 22.55278, 1950, 0., 0., 2210, 0
37, "SWS07", 3., "N", "IC443B ", 6.21863, 22.43889, 1950, 0., 0., 297, 38
38, "SWS07", 3., "N", "IC443B ", 6.22765, 22.43889, 1950, 0., 0., 110, 39
39, "SWS07", 3., "N", "IC443B ", 6.23667, 22.43889, 1950, 0., 0., 110, 40
40, "SWS07", 3., "N", "IC443B ", 6.24568, 22.43889, 1950, 0., 0., 110, 41
41, "SWS07", 3., "N", "IC443B ", 6.25470, 22.43889, 1950, 0., 0., 110, 42
42, "SWS07", 3., "N", "IC443B ", 6.25470, 22.44722, 1950, 0., 0., 110, 43
43, "SWS07", 3., "N", "IC443B ", 6.24568, 22.44722, 1950, 0., 0., 110, 44
44, "SWS07", 3., "N", "IC443B ", 6.23667, 22.44722, 1950, 0., 0., 110, 45
45, "SWS07", 3., "N", "IC443B ", 6.22765, 22.44722, 1950, 0., 0., 110, 46
46, "SWS07", 3., "N", "IC443B ", 6.21863, 22.44722, 1950, 0., 0., 110, 47
47, "SWS07", 3., "N", "IC443B ", 6.21863, 22.45555, 1950, 0., 0., 110, 48
48, "SWS07", 3., "N", "IC443B ", 6.22765, 22.45555, 1950, 0., 0., 110, 49
49, "SWS07", 3., "N", "IC443B ", 6.23667, 22.45555, 1950, 0., 0., 110, 50
50, "SWS07", 3., "N", "IC443B ", 6.24568, 22.45555, 1950, 0., 0., 110, 51
51, "SWS07", 3., "N", "IC443B ", 6.25470, 22.45555, 1950, 0., 0., 110, 52
52, "LWS02", 3., "N", "IC443B ", 6.23667, 22.44722, 1950, 0., 0., 3535, 0
53, "SWS07", 3., "N", "IC443C ", 6.22636, 22.38463, 1950, 0., 0., 297, 54
54, "SWS07", 3., "N", "IC443C ", 6.23273, 22.37826, 1950, 0., 0., 110, 55
55, "SWS07", 3., "N", "IC443C ", 6.23911, 22.37189, 1950, 0., 0., 110, 56
56, "SWS07", 3., "N", "IC443C ", 6.24548, 22.36551, 1950, 0., 0., 110, 57
57, "SWS07", 3., "N", "IC443C ", 6.25185, 22.35914, 1950, 0., 0., 110, 58
58, "SWS07", 3., "N", "IC443C ", 6.25774, 22.36503, 1950, 0., 0., 110, 59
59, "SWS07", 3., "N", "IC443C ", 6.25137, 22.37140, 1950, 0., 0., 110, 60
60, "SWS07", 3., "N", "IC443C ", 6.24500, 22.37778, 1950, 0., 0., 110, 61
61, "SWS07", 3., "N", "IC443C ", 6.23863, 22.38415, 1950, 0., 0., 110, 62
62, "SWS07", 3., "N", "IC443C ", 6.23225, 22.39052, 1950, 0., 0., 110, 63
63, "SWS07", 3., "N", "IC443C ", 6.23815, 22.39641, 1950, 0., 0., 110, 64
64, "SWS07", 3., "N", "IC443C ", 6.24452, 22.39004, 1950, 0., 0., 110, 65
65, "SWS07", 3., "N", "IC443C ", 6.25089, 22.38367, 1950, 0., 0., 110, 66
66, "SWS07", 3., "N", "IC443C ", 6.25727, 22.37730, 1950, 0., 0., 110, 67
67, "SWS07", 3., "N", "IC443C ", 6.26364, 22.37092, 1950, 0., 0., 110, 68
68, "LWS02", 3., "N", "IC443C ", 6.24500, 22.37778, 1950, 0., 0., 3535, 0
69, "SWS02", 2., "N", "B35 ", 5.69667, 9.12139, 1950, 0., 0., 2704, 70
70, "SWS07", 2., "N", "B35 ", 5.69667, 9.12139, 1950, 0., 0., 741, 71
71, "LWS04", 2., "N", "B35 ", 5.69667, 9.12139, 1950, 0., 0., 1044, 72