This is a resubmission of Phase II for Proposal 10566. There are changes
made according to the suggestions of the reviewer.
These changes are the following:
1) We use the default ACS-WFC-DITHER-LINE pattern (No of points: 2,
Point spacing: 3.011, Orient: 85.28) to bridge the gap between
the two detectors, with a ACS-WFC-DITHER-LINE subpattern (No of
points: 2, Point spacing: 0.146, Orient: 47.17) as suggested
in HST Phase II Proposal Instructions section 8.4.2 (page 156)
to have simultaneous elimination of hot pixels and cosmic ray hits.
With this subpattern we also minimize the effects of scale variation
across the detector.
2) We eliminated the number of short exposures and thus, we increased
the exposure times of the long ones. This was done after experimenting
with the ACS ETC, to maximize the S/N and with the use of the Orbit
Planner in APT. We include all the long exposures in the DITHER-LINE
pattern/subpattern and the short exposures (for the "System")
in a single DITHER-LINE pattern (to bridge the gap).
3) We use the "SAME ORIENT AS" requirement for visits No 2,3 and 4.
We request for Visit 2 the same orientation with Visit 1
("System" field) and the orientation of Visit 4 to be the same with
the one of Visit 3.
----- Submission 1 (Wed Apr 13 12:50:20 GMT 2005) -----
Phase II Proposal 10566 (proposal_10566) successfully submitted.
Unable to contact STScI submission server
Unable to contact STScI submission server
----- Submission 2 (Mon Jun 06 11:08:40 GMT 2005) -----
Assigned ID: 189
----- Submission 1 (Fri Jan 21 14:16:44 GMT 2005) -----
Phase I Proposal 189 (proposal) successfully submitted.
Star Formation in the LMC - The complete IMF of a Stellar AssociationWe propose to use the large improvement in sensitivity and wide-field resolution provided by ACS to obtain, for the first time, the complete Initial Mass Function (IMF) down to sub-solar masses of a very young stellar association in the Large Magellanic Cloud (LMC). Such an IMF will serve as a reference IMF typical of low-metallicity regions. We want to obtain VI deep (V ~ 26.5 mag) WFC photometry of the association LH 95 and a nearby background field pointing. Special care will be taken to treat all the complications which arise in the reduction of data for the purpose of calculating the IMF of a young association of stars. Our object of study has been chosen because it is one of the associations, which provide the best combination of spatial resolution, crowding, low extinction, nebular contamination, and background confusion in comparison to others in the Local Group. The region also has the advantage of being very young with indications that it is still forming stars, thus allowing us to search for sub-solar pre-main-sequence stars, as well as for an embedded proto-cluster.We require ACS/WFC imaging of two fields, the first centered on the association LH 95 (System) and the second on an area located 5.3 arcmin west from the first (Field). The selection of WFC is based on the fact that associations are elongated stellar systems covering few arcminutes of sky, requiring a wide field of view with high spatial resolution. Two broad-band filters will be used: F555W and F814W which are equivalent to Johnson-Cousins V and I respectively. Our analysis of both the fields to be observed has been done with a nominal S/N ~ 20 at V ~ 26.5 mag and I ~ 25.5 mag, assuming a flat continuum, as well as spectral distributions of late-type main-sequence stars down to M0. To reach S/N=20 at this magnitude, total exposure times of about 3,000 sec in F555W and about 2,000 sec in F814W are needed for each field with the WFC. Dithered observations using a sub-pixel box pointing pattern will be performed. We will also take parallel observations with NICMOS (NIC2) in F110W, F160W and F205W bands.
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