<=== observer ===>
"GOLOFSSO",\
"Olofsson, G.",\
"",\
"Stockholm Observatory",\
"",\
"",\
"S-133 36",\
"Saltsjobaden",\
"Sweden",\
"46 8 164455",\
"46 8 7174719",\
"olofsson@astro.su.se"
<=== proposal ===>
"D_SURMC",1,2,\
{"molecular clouds","star formation"},\
{"Ph. Andre","F. Boulanger","C. Cesarsky","M. Casali","J. Davies",\
"T. Montmerle","L. Nordh","P. Persi","F. Sibille","M. Perault"}
<=== title ===>
A deep search for low-mass protostellar objects and pre main-sequence
stars in nearby molecular clouds.
<=== abstract ===>
SCIENTIFIC ABSTRACT
In order to investigate the low-mass star-formation in molecular clouds one
needs both surveys of large areas to about 10 times the sensitivity of IRAS
- which is the topic of another proposal - and deep surveys of a limited
number of selected regions. Large area surveys will yield complete samples
of stellar populations in dark clouds, while deep surveys can be used in
attempts to extend the infrared luminosity function (LF) to much lower
luminosities.
The present proposal thus aims at a deep search for low- luminosity young
stars in a sample of nearby dense molecular cores with and without known
star-formation. It is obviously important to use the same filters (LW2 and
LW3) as for the large survey, but in order to avoid source confusion we
judge that the 3 arcsec. pixel field of view should be used. This however
means that only a very small fraction of the large survey can be covered by
this deep survey and we find it natural to favour the densest and/or
clustered parts of the regions.
With an integration time of 0.5 hour, objects with luminosities in the
range a few x 0.0001 - a few x 0.02 L-sun should be detectable, the actual
luminosity limit being dependent on the steepness of the energy
distributions.
OBSERVATION SUMMARY
As we expect the fields to contain many point sources in addition to
extended emission the beam shift method (AOT = CAM03) should be the most
efficient. The exact position of the reference field is a trade-off between
the wish to get a clean region and the risk of increasing differential
background for larger shifts (and the increased slew time). In most cases
we judge that a shift equal to one or two frames should suffice.The unit
integration time of 10 sec. and a total time on the target of 0.5 hours
gives, according to the "time calculator", S/N = 3 for 0.06 mJy in the LW2
filter and for 0.130 mJy in the LW3. For each region we propose to
concatenate the observations in the two filters in order to save some
slewing time.
<=== scientific_justification ===>
Time distribution for autumn launch targets:
Team top 40% second 30% last 30%
CAM : 5h
SOT : 3h
total : 8h
Time distribution for spring launch targets:
Team top 40% second 30% last 30%
CAM : 5h
SOT : 3h
total : 8h
<=== autumn_launch_targets ===>
1, "CAM01", 2.0, "N","Rho Oph A LW2",16.39028, -24.2917,1950, 0., 0., 1800,2
2, "CAM01", 2.0, "N","Rho Oph A LW3",16.39028, -24.2917,1950, 0., 0., 1800,0
3, "CAM01", 2.0, "N","Rho Oph B2 LW2",16.40722, -24.3361,1950, 0., 0., 1800,4
4, "CAM01", 2.0, "N","Rho Oph B2 LW3",16.40722, -24.3361,1950, 0., 0., 1800,0
5, "CAM01", 2.0, "N","Cham I N LW2",11.13889, -76.4667,1950, 0., 0., 1800,6
6, "CAM01", 2.0, "N","Cham I N LW3",11.13889, -76.4667,1950, 0., 0., 1800,0
7, "CAM01", 2.0, "N","B 335 LW2",19.57647, 7.4567,1950, 0., 0., 1800,8
8, "CAM01", 2.0, "N","B 335 LW3",19.57647, 7.4567,1950, 0., 0., 1800,0
9, "CAM01", 2.0, "N","Serpens HII LW2",18.45483, 1.2211,1950, 0., 0., 1800,10
10, "CAM01", 2.0, "N","Serpens HII LW3",18.45483, 1.2211,1950, 0., 0., 1800,0
11, "CAM01", 2.0, "N","Serpens SVS4 LW2",18.45708, 1.1806,1950, 0., 0., 1800,12
12, "CAM01", 2.0, "N","Serpens SVS4 LW3",18.45708, 1.1806,1950, 0., 0., 1800,0
13, "CAM01", 2.0, "N","Serpens SMM-peak LW2",18.45555, 1.1986,1950, 0., 0., 1800,14
14, "CAM01", 2.0, "N","Serpens SMM-peak LW3",18.45555, 1.1986,1950, 0., 0., 1800,0
15, "CAM01", 2.0, "N","RCrA IRAS 32 LW2",18.99328, -37.1981,1950, 0., 0., 1800,16
16, "CAM01", 2.0, "N","RCrA IRAS 32 LW3",18.99328, -37.1981,1950, 0., 0., 1800,0
<=== spring_launch_targets ===>
1, "CAM01", 2.0, "N","L1641 IR cluster LW2", 5.56458, -6.3981,1950, 0., 0., 1800,2
2, "CAM01", 2.0, "N","L1641 IR cluster LW3", 5.56458, -6.3981,1950, 0., 0., 1800,0
3, "CAM01", 2.0, "N","LBS 37 LW2", 5.64861, -1.7333,1950, 0., 0., 1800,4
4, "CAM01", 2.0, "N","LBS 37 LW3", 5.64861, -1.7333,1950, 0., 0., 1800,0
5, "CAM01", 2.0, "N","Cham I N LW2",11.13889, -76.4667,1950, 0., 0., 1800,0
6, "CAM01", 2.0, "N","Cham I N LW3",11.13889, -76.4667,1950, 0., 0., 1800,0
7, "CAM01", 2.0, "N","Cham I S LW2",11.08889, -77.1028,1950, 0., 0., 1800,8
8, "CAM01", 2.0, "N","Cham I S LW3",11.08889, -77.1028,1950, 0., 0., 1800,0
9, "CAM01", 2.0, "N","Serpens HII LW2",18.45483, 1.2211,1950, 0., 0., 1800,10
10, "CAM01", 2.0, "N","Serpens HII LW3",18.45483, 1.2211,1950, 0., 0., 1800,0
11, "CAM01", 2.0, "N","Serpens SVS4 LW2",18.45708, 1.1806,1950, 0., 0., 1800,12
12, "CAM01", 2.0, "N","Serpens SVS4 LW3",18.45708, 1.1806,1950, 0., 0., 1800,0
13, "CAM01", 2.0, "N","TMC 1 core LW2", 4.60888, 25.6100,1950, 0., 0., 1800,14
14, "CAM01", 2.0, "N","TMC 1 core LW3", 4.60888, 25.6100,1950, 0., 0., 1800,0
15, "CAM01", 2.0, "N","RCrA IRAS 32 LW2",18.99328, -37.1981,1950, 0., 0., 1800,16
16, "CAM01", 2.0, "N","RCrA IRAS 32 LW3",18.99328, -37.1981,1950, 0., 0., 1800,0