Assigned ID: 675 ----- Attempting Submission 1 (Fri Feb 24 20:39:09 GMT 2012) ----- HST Phase I Proposal 675 (isolated_YSOs_Cycle20.pdf.apt) successfully submitted. ----- Attempting Submission 2 (Fri Feb 24 21:52:45 GMT 2012) ----- ----- Attempting Submission 1 (Tue Jul 10 20:30:47 GMT 2012) ----- ----- Attempting Submission 2 (Tue Aug 14 03:13:32 GMT 2012) ----- The warning was: "Light from the flash may escape from WFC3 and possibly contaminate exposures in other SIs." The contact scientist should review if this will be a problem for the parallel ACS observations. Probing Isolated Massive Star Formation in the LMC Whether massive stars can form in isolation is one of the most debated questions in star formation. Observations of main sequence O-stars indicate that 5-10% of them form in isolation, but models of massive star formation suggest that massive stars should form in cluster environments. Isolated massive young stellar objects (YSOs) are better suited to address whether or not massive stars truly form in isolation since YSOs have had less time to disrupt their natal environment or move away from their stellar siblings. We have developed a unique sample of 7 candidates for isolated massive YSOs in the LMC. Within 80 pc, these objects are not associated with 1) other massive and intermediate-mass YSOs, 2) OB associations, and 3) giant molecular clouds (GMCs). In all cases ground-based H-alpha observations show that they are affiliated with non-elongated, small HII regions and therefore are unlikely to be part of a runaway population. We request WFC3/UVIS and IR observations in the F656N, F555W, F814W, F110W, and F160W bands to examine the interstellar environment and determine the main sequence and pre-main sequence (PMS) populations down to ~0.7 solar masses. In addition, coordinated parallel ACS/WFC F555W, F814W, and F658N observations will be used to assess the nearby control-field populations. From these observations we can search for lower-mass PMS stars, infer the local star formation history, and determine whether evidence exists for remnants of a disrupted GMC. With this statistically significant sample, we will have the ability to assess the possibility of massive stars forming in isolation. We have 2 different set-ups; one is in the RA limited regime for Cycle 20 (045403.6-671618.5) while the other 6 are not. Setup for 6 of the objects: For UVIS observations we picked UVIS-FIX as our aperture; this aperture was chosen in order to completely overlap the IR aperture IR-UVIS. It also allowed for our primary sources to never fall in the WFC3/UVIS chip gap. For time excess of 1200s in UVIS, we favored going deep into the I-band to locate more PMS stars. We also added some time to H-alpha as well. A 10 second exposure for 656N was added in order to aid in finding accurate surface brightnesses for compact HII regions if present. For UVIS we dither 3 points, using large spacing in our dithers (equivalent to the WFC3-UVIS-GAP-LINE) in order to cover the chip spacing. We dither 4 times in IR. For IR we chose STEP100 in order to get large dynamic range. We preferred to use most the IR time to go deep in the H-band (160W). For coordinated parallel ACS observations, we strongly preffered I-band observations to match exposure times with WFC3. Visit 2 is slightly different than Visit 3-7 due to shorter occulation time. Post-Flash was added for F656N observations to mitigate CTE effects. ETC calculator estimate about 0 electrons/pixel for the 10 second exposures, and about 1 electron/pixel for any other exposure (~400-700 seconds). We therefore chose 12e- as our flash value. Setup for RA-limited object: We went for a similar strategy. However, no 10 second exposure seemed possible. Only 3 dithers were possible in IR. We have one object requiring Schedulability = 100. If however, this is unneeded, we would desire it be be observed in the same way as the other 6 objects. If this project benefits from use of post-flash to mitigate CTE problems, we would consider applying it to our observations if it is developed enough for use. STAR FORMATION 12 false 0.0 0.0 false false false false SUPPORTED EXT-STAR YSO J2000 J2000 B=16.871 +/- 0.078, I=15.349 +/- 0.075 J=14.546 +/- 0.044, H=13.588 +/- 0.036, K=12.399 +/- 0.030 EXT-STAR YSO J2000 J2000 U=14.821 +/- 0.129, B=15.623 +/- 0.046, J=15.289 +/- 0.093, H=14.768 +/- 0.146, K=14.149 +/- 0.085 EXT-STAR YSO J2000 J2000 EXT-STAR YSO J2000 J2000 U=20.350 +/- 0.180, B=20.763 +/- 0.175, J=16.664 +/- 0.182, H=15.556 +/- 0.168, K=14.626 +/- 0.116 EXT-STAR YSO J2000 J2000 U=15.820 +/- 0.046, B=16.183 +/- 0.074, J=15.648 +/- 0.094, H=15.143 +/- 0.103, K=14.819 +/- 0.142 EXT-STAR YSO J2000 J2000 EXT-STAR YSO J2000 J2000 U=16.042 +/- 0.073, B=16.606 +/- 0.088, I=16.334 +/- 0.077, J=15.317 +/- 0.082, H=14.318 +/- 0.073, K=13.141 +/- 0.044 WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F656N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F656N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F656N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F656N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F656N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F656N WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F656N ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F658N POS-TARG DITHER 0.636 LINE false false 3 41.788 WFC3-IR-DITHER-LINE 1 false POS-TARG DITHER 0.636 LINE false false 2 41.788 WFC3-IR-DITHER-LINE 4 false /home/seale/Desktop/OP-cache/isolated_YSOs_Cycle20_PhaseII_3-v01.xml The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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