<=== observer ===>
"SCABRIT",\
"Cabrit, S.",\
"",\
"Observatoire de Grenoble",\
"BP 53X - Domaine Universitaire",\
"",\
"38041",\
"Grenoble CEDEX",\
"France",\
" 3376514568",\
" 3376448821",\
"cabrit@gag.observ-gr.fr"
<=== proposal ===>
"CAMFLOWS",\
1,\
3,\
{"bipolar outflows","circumstellar envelopes","star formation",\
"young stellar objects"},\
{"Boulanger, F.","Cesarsky, C.","Nordh, L.","Olofsson, G.",\
"Sibille, F.","Andre, P.","Siebenmorgen, R.","Boulade, O.","Lagage, P.O."}
<=== title ===>
Mid-infrared dust emission from young stellar objects: outflows and warm halos
<=== abstract ===>
SCIENTIFIC ABSTRACT:
We propose to investigate with ISOCAM the presence and properties of
extended mid-infrared emission associated with energetic bipolar
outflows and circumstellar dust halos around young stellar objects.
The first part of this proposal deals with bipolar molecular outflows. Recent
array maps in the H2 S(1)(1-0) line at 2.12 microns often reveal shock
emission regions along the flow axis, probably associated with a fast
protostellar jet entraining the molecular gas. We expect that shocks of
velocity greater than 60 km/s will have observable signatures in the ISOCAM
range in the form of [NeII] emission at 12.8microns, while the UV radiation
released in the shock front may excite a broad and faint halo of mid-infrared
emission from small, heated dust grains. Together with longer wavelength
information from SWS, LWS, and PHOT, the spatially resolved information
provided by ISOCAM observations of these signatures will yield important
constraints on true wind speeds, integrated mass-loss rates, and entrainment
processes in protostellar winds, all of which are necessary for assessing the
role of outflows in star formation and cloud evolution.
In the second part of this proposal, we focus on a selected sample of young
stellar objects in order to investigate their detailed geometry and emission
properties of the ISOCAM range. In particular we will
search for extended 3-11micron emission from faint halos of small transiently
heated dust particles. Such a component has been invoked recently to explain
the mid-infared excess of YSOs, although scattering by large particles and
non-spherical geometries offer other alternatives. Our ISOCAM
observations will provide stronger constraints that should help
develop coherent models of the circumstellar environment of these objects.
OBSERVATION SUMMARY:
Our sample of molecular flows concentrates on those with a well-defined
bipolar appearance, high radial velocities in CO lines, and/or evidence for
shock activity (e.g. H2 or SiO emission, temperature increase in CO).
In each flow, the high-velocity CO extent will be raster-mapped in two CVF
steps, one at the [NeII]12.8micron line and the other in the neighbouring
continuum. An independent estimate of line+continuum level will be obtained
with a deeper map in LW10 (8-15micron) for comparison with CVF maps. A
large scale map will be obtained with 6'' pfov to detect extended emission,
and a smaller area covered with pfov 3'' to reveal bright small-scale structure
(e.g. bow-shocks).
A ``strip'' map across one outflow lobe will also be made in LW2 (pfov
6''), to search for a faint halo of small dust grains extending beyond the
CO contours down to a level of 2.5e-2 mJy/arcsec2 (5 sigma). In B335
(autumn) or L1448 (spring) a larger map will be made in both LW2
and LW3 for comparison with PHOT 60 and 100micron maps (TPRAY_INFRABI
proposal).
Our sample of young stellar objects includes embedded objects in the rho
Oph cloud with indications from earlier photometric measurements of excess
10 microns infrared emission at scales >10" (autumn), or similar objects in
the Cha I cloud as well as intermediate luminosity YSOs with spectral
evidence for very small grain emission or with outflow (spring).
All objects are imaged with ISOCAM in LW5, LW6, LW7, LW8 (to discriminate
between scattered light and extended emission in the 7.7 and 11.3 bands),
with pfov and sensitivity level indicated in Tables 3 and 4. In addition,
a subset of sources (GSS30-IRS1, S1, WL22, DoAr25, IRS44, rho Oph A /
HD259431, LkHa25, T32, T33A/B, T29, T41) will be mapped in SW2, SW6, and
SW7 to search for the presence of extended 3.3micron feature emission and
to sample the ice band. Finally, a fully sampled CVF spectrum image from
5.5 to 8.5 micron will be taken of Source 1 and GSS30 (autumn) or T32 and
HD259431 (spring).
LINKED OBSERVATIONS
none
FIXED TIME OBSERVATIONS
none
CONCATENATION
<=== scientific_justification ===>
Details on observing procedure:
Outflow maps in CVF (NeII+continuum) and LW10 are done in raster with dN=16
(except in IRAS16393 where dN=8). The 6'' pfov map covers the whole
high-velocity CO area (cf. Tables 1 and 2). When the outflow is too large,
we will only perform a 1D raster along the flow axis (B335) or map only the
blue lobe (L1551). In flows smaller than 5' by 1' (see tables 1 and 2
below), the high-resolution map (3'' pfov) will cover most of the CO area
(raster with dN=16) while in the larger ones it will be more loosely
sampled, and only aimed at peaks of shock tracers (NH3, SiO, H2, HH
objects). We will attempt to reach a sensitivity of 1mJy/arcsec2 (10sigma)
in the two CVF filters, and 0.1mJy/arcsec2 (8sigma) in the LW10 filter.
Outflow ``strips'' in LW2: they consist of a 3 by 1 raster with
dN=16 perpendicular to the outflow axis. Three outflows in the
Autumn launch list (HH 7-11, VLA 1623, IRAS 16293) will already be mapped
in LW2 and LW3 as part of the CAM molecular cloud survey proposals, and
will not be observed here in LW2.
Broad ``Halo'' searches: To investigate a possible warm counterpart to the
cold dust ``halo'' searched by PHOT at 60 and 100microns, the red lobe of
B335 (autumn) or the blue lobe of L1448 (spring) will be mapped in both LW2
and LW3 over an area extending well beyond the CO contours (raster with
dN=dM=16).
YSOs: Tables 3 and 4 give the adopted pfov (fixed mainly by the saturation
limit on point sources or by any previously known extension at 12micron),
the filters used, and the expected detection limit.
Table 1: Outflow Area covered in Autumn list
Flow Name Flow size Area covered
(enclosed at 6''pfov) at 3'' pfov
--------------------------------------------
L1448 4'.3 by 1' Complete
HH 7-11 3' by 1' Complete
IRAS3282 8'.3 by 2' H2 in Blue lobe
VLA 1623 6' by 1' Complete
IRAS16293 5' by 3' Center
L483 3' by 1' Complete
G35.2N 3' by 1.5' Complete
L1157 6' by 2' SiO/NH3 peaks
B335 *[18' by 3'] HH119A/C *strip along flow axis
halo map: 6' by 9' (red lobe)
Table 2: Outflow Area covered in Spring list
Flow Name Flow size Area covered
(enclosed at 6''pfov) at 3'' pfov
--------------------------------------------
L1448 4'.3 by 1' Complete halo map: 4.5' by 6' (blue lobe)
HH 7-11 3' by 1' Complete
IRAS 3282 8'.3 by 2' Blue lobe
L1551 *[20' by 4.5'] center/HH29 *Blue lobe only
Orion B 4.5' by 1' Complete
NGC2071 6' by 2' EHV blue lobe
Mon-OB1 G 7' by 3' None
L1157 6' by 2' SiO/NH3 peaks
Table 3: Pfov, filters and detection level for YSOs (Autumn list)
pfov SW2,6,7 LW5,6,7,8 Detection level (10sigma)
GSS30-IRS1 1.5'' SW LW 10 mJy/arcsec2
DoAr25 6'' SW LW 0.3
rho Oph A 3'' SW LW 0.4
Source 1 6'' SW LW 1
IRS 37 6'' LW 0.2
WL 22 6'' SW LW 1
WL 1 6'' LW 0.2
WL 20 3'' LW 0.4
WL 9 6'' LW 0.2
IRS 44 3'' SW LW 3
Table 4: Pfov, filters and detection level for YSOs (Spring list)
pfov SW2,6,7 LW5,6,7,8 Detection level (10sigma)
L1551-IRS5 1.5'' LW 10 mJy/arcsec2
HD259431 1.5'' SW LW 10
LkHa25 1.5'' SW LW 2
T29 1.5'' SW LW 10
T32/HD97048 1.5'' SW LW 10
T30/31 3'' LW 0.4
T33A/B 3'' SW LW 3
C9-2 IRN 6'' LW 1
T41/HD97300 6'' SW LW 1
T42 6'' LW 1
T44 6'' LW 1
Time distribution for autumn launch targets:
Team top 40% second 30% last 30%
CAM : 18000 18000 18000
SOT : 7200 0 0
total : 25850 18275 17670
Time distribution for spring launch targets:
Team top 40% second 30% last 30%
CAM : 18000 18000 24800
SOT : 7200 0 0
total : 25030 19200 24620
<=== autumn_launch_targets ===>
1,"CAM01",1.0,"N","L1448 NeII 3 ", 3.37619, 30.55972,1950,0.,0.,2850,0
2,"CAM01",1.0,"N","L1448 LW10 3 ", 3.37619, 30.55972,1950,0.,0., 555,0
3,"CAM01",1.0,"N","L1448 NeII 6 ", 3.37619, 30.55972,1950,0.,0., 910,0
4,"CAM01",1.0,"N","L1448 strip ", 3.37619, 30.55972,1950,0.,0., 675,0
5,"CAM01",2.0,"N","HH 7-11 NeII 3 ", 3.43286, 31.09639,1950,0.,0.,2895,0
6,"CAM01",3.0,"N","IRAS 3282 6 ", 3.47089, 30.58722,1950,0.,0.,1605,0
7,"CAM01",3.0,"N","IRAS 3282 3 ", 3.47089, 30.58722,1950,0.,0.,1310,0
8,"CAM01",3.0,"N","IRAS 3282 strip ", 3.47089, 30.58722,1950,0.,0., 555,0
9,"CAM01",1.0,"N","VLA 1623 North ",16.39028,-24.29611,1950,0.,0.,2600,0
10,"CAM01",1.0,"N","VLA 1623 South ",16.39028,-24.29611,1950,0.,0.,2440,0
11,"CAM01",1.0,"N","VLA 1623 Off ",16.39028,-24.29611,1950,0.,0., 740,0
12,"CAM01",3.0,"N","IRAS 16293 6 ",16.48917,-24.37000,1950,0.,0.,1605,0
13,"CAM01",3.0,"N","IRAS 16293 3 ",16.48917,-24.37000,1950,0.,0., 740,0
14,"CAM01",3.0,"N","L483 3 ",18.24750, -4.68028,1950,0.,0.,1875,0
15,"CAM01",3.0,"N","L483 6 ",18.24750, -4.68028,1950,0.,0., 750,0
16,"CAM01",3.0,"N","L483 strip ",18.24750, -4.68028,1950,0.,0., 555,0
17,"CAM01",2.0,"N","G35.2N 3 ",18.92811, 1.60917,1950,0.,0.,1515,0
18,"CAM01",2.0,"N","G35.2N 6 ",18.92811, 1.60917,1950,0.,0., 670,0
19,"CAM01",3.0,"N","G35.2N strip ",18.92811, 1.60917,1950,0.,0., 555,0
20,"CAM01",2.0,"N","L1157 6 ",20.64433, 67.85917,1950,0.,0.,1320,0
21,"CAM01",2.0,"N","L1157 3 ",20.64433, 67.85917,1950,0.,0.,2440,0
22,"CAM01",2.0,"N","L1157 strip ",20.64433, 67.85917,1950,0.,0., 555,0
23,"CAM01",1.0,"N","B335 6 ",19.57646, 07.45667,1950,0.,0.,3315,0
24,"CAM01",1.0,"N","B335 3 ",19.57646, 07.45667,1950,0.,0.,1310,0
25,"CAM01",1.0,"N","B335 halo ",19.57646, 07.45667,1950,0.,0.,2955,0
26,"CAM01",1.0,"N","GSS30-IRS1 LW ",16.38889,-24.27167,1950,0.,0., 980,0
27,"CAM01",2.0,"N","GSS30-IRS1 SW ",16.38889,-24.27167,1950,0.,0.,1080,0
28,"CAM04",3.0,"N","GSS30-IRS1 CVF ",16.38889,-24.27167,1950,0.,0.,2380,0
29,"CAM01",1.0,"N","DoAr 25 ",16.38936,-24.60806,1950,0.,0.,2480,0
30,"CAM01",3.0,"N","rho Oph A ",16.39028,-24.29611,1950,0.,0.,2480,0
31,"CAM01",1.0,"N","Source 1 LW ",16.39242,-24.27897,1950,0.,0., 880,0
32,"CAM04",2.0,"N","Source 1 CVF ",16.39242,-24.27897,1950,0.,0.,2380,0
33,"CAM01",2.0,"N","Source 1 SW ",16.39242,-24.27897,1950,0.,0.,1080,0
34,"CAM01",2.0,"N","IRS37 ",16.40442,-24.37056,1950,0.,0.,1380,0
35,"CAM01",1.0,"N","WL 22 ",16.39931,-24.47131,1950,0.,0.,3160,0
36,"CAM01",2.0,"N","WL 1 ",16.40067,-24.36278,1950,0.,0.,1380,0
37,"CAM01",2.0,"N","WL 20 ",16.40386,-24.53467,1950,0.,0.,1580,0
38,"CAM01",3.0,"N","WL 9 ",16.40236,-24.44417,1950,0.,0.,1380,0
39,"CAM01",3.0,"N","IRS 44 ",16.40728,-24.54806,1950,0.,0.,1880,0
<=== spring_launch_targets ===>
1,"CAM01",1.0,"N","L1448 LW10 3 ", 3.37619, 30.55972,1950,0.,0., 555,0
2,"CAM01",1.0,"N","L1448 NeII 3 ", 3.37619, 30.55972,1950,0.,0.,2850,0
3,"CAM01",1.0,"N","L1448 LW10 6 ", 3.37619, 30.55972,1950,0.,0., 260,0
4,"CAM01",1.0,"N","L1448 NeII 6 ", 3.37619, 30.55972,1950,0.,0., 910,0
5,"CAM01",1.0,"N","L1448 halo ", 3.37619, 30.55972,1950,0.,0.,1290,0
6,"CAM01",2.0,"N","HH 7-11 NeII 3 ", 3.43286, 31.09639,1950,0.,0.,2895,0
7,"CAM01",1.0,"N","IRAS 3282 6 ", 3.47089, 30.58722,1950,0.,0.,1890,0
8,"CAM01",1.0,"N","IRAS 3282 3 ", 3.47089, 30.58722,1950,0.,0.,3005,0
9,"CAM01",1.0,"N","IRAS 3282 strip ", 3.47089, 30.58722,1950,0.,0., 555,0
10,"CAM01",2.0,"N","L1551-IRS5 3 ", 4.47778, 18.03111,1950,0.,0.,1980,0
11,"CAM01",2.0,"N","L1551-IRS5 6 ", 4.47778, 18.03111,1950,0.,0.,3885,0
12,"CAM01",2.0,"N","L1551-IRS5 strip", 4.47778, 18.03111,1950,0.,0.,1260,0
13,"CAM01",3.0,"N","L1551-IRS5 6 ", 4.47778, 18.03111,1950,0.,0.,3600,0
14,"CAM01",3.0,"N","L1551-IRS5 strip", 4.47778, 18.03111,1950,0.,0.,1260,0
15,"CAM01",3.0,"N","Orion B 3 ", 5.65361, -1.95000,1950,0.,0.,3005,0
16,"CAM01",3.0,"N","Orion B 6 ", 5.65361, -1.95000,1950,0.,0., 750,0
17,"CAM01",3.0,"N","Orion B strip ", 5.65361, -1.95000,1950,0.,0., 555,0
18,"CAM01",3.0,"N","NGC 2071 outer ", 5.74183, 0.34472,1950,0.,0., 750,0
19,"CAM01",3.0,"N","NGC 2071 inner ", 5.74183, 0.34472,1950,0.,0., 670,0
20,"CAM01",3.0,"N","NGC 2071 3 ", 5.74183, 0.34472,1950,0.,0.,1515,0
21,"CAM01",3.0,"N","NGC 2071 strip ", 5.74183, 0.34472,1950,0.,0., 555,0
22,"CAM01",3.0,"N","MonOB1-G ", 6.64083, 9.97444,1950,0.,0.,1605,0
23,"CAM01",3.0,"N","MonOB1-G strip ", 6.64083, 9.97444,1950,0.,0., 555,0
24,"CAM01",1.0,"N","L1157 3 ",20.64433, 67.85917,1950,0.,0.,4135,0
25,"CAM01",1.0,"N","L1157 6 ",20.64433, 67.85917,1950,0.,0.,1605,0
26,"CAM01",1.0,"N","L1157 strip ",20.64433, 67.85917,1950,0.,0., 555,0
27,"CAM01",3.0,"N","L1551-IRS5(star)", 4.47778, 18.03111,1950,0.,0., 880,0
28,"CAM01",1.0,"N","HD 259431 ", 6.50539, 10.36055,1950,0.,0.,1880,0
29,"CAM01",3.0,"N","HD 259431 CVF ", 6.50539, 10.36055,1950,0.,0.,2380,0
30,"CAM01",3.0,"N","LkHa25 ", 6.63319, 9.84817,1950,0.,0.,3280,0
31,"CAM01",1.0,"N","T29 ",11.10953,-77.37444,1950,0.,0.,1880,0
32,"CAM01",1.0,"N","T32/HD97048 ",11.11100,-77.38361,1950,0.,0.,1880,0
33,"CAM01",2.0,"N","T32 CVF ",11.11100,-77.38361,1950,0.,0.,2380,0
34,"CAM01",3.0,"N","T30/T31 ",11.10967,-77.44000,1950,0.,0.,1980,0
35,"CAM01",1.0,"N","T33A/B LW ",11.11394,-77.29195,1950,0.,0.,1780,0
36,"CAM01",2.0,"N","T33A/B SW ",11.11394,-77.29195,1950,0.,0.,1280,0
37,"CAM01",2.0,"N","C9-2 IRN ",11.12086,-77.45972,1950,0.,0.,1380,0
38,"CAM01",3.0,"N","T41/HD 97300 SW ",11.13831,-76.34167,1950,0.,0.,1280,0
39,"CAM01",2.0,"N","T41/HD 97300 LW ",11.13831,-76.34167,1950,0.,0.,1380,0
40,"CAM01",2.0,"N","T42 ",11.13942,-76.30167,1950,0.,0.,1380,0
41,"CAM01",2.0,"N","T44 ",11.14125,-76.31055,1950,0.,0.,1380,0