0Assigned ID: 247
----- Attempting Submission 1 (Thu Feb 23 23:50:15 GMT 2012) -----Dear Alison
I have resubmitted proposal 13009, with visit 81 and 91 changed to add/modify FLASH
for the WFC3 observations. In all three primary exposures of each visit there is now
FLASH=12.
All visits that were on hold can now be resumed and are ready for scheduling.
Thank you very much and cheers,
guido196293472----- Attempting Submission 1 (Tue Jul 03 18:31:44 GMT 2012) -----
----- Attempting Submission 2 (Tue Jul 03 19:53:14 GMT 2012) -----
----- Attempting Submission 3 (Mon May 13 21:05:21 GMT 2013) -----
----- Attempting Submission 4 (Mon Jun 03 20:15:13 GMT 2013) -----
----- Attempting Submission 5 (Wed Jun 19 14:17:24 GMT 2013) -----Finding chart confirmedStudying pre-main sequence stars across the metallicity ladderThe fundamental goal of any star formation theory is to determine where, when, why and how stars form. Understanding where pre-main sequence (PMS) stars are located, how old and massive they are and how much they grow in mass as they approach the main sequence will provide strong constraints to any such theories. We propose to use the HST to identify several thousands PMS stars in the Galaxy and Large and Small Magellanic Clouds (LMC/SMC), so as to probe widely different star-forming conditions. We will accurately measure for each object the position in the natal cloud, the age, the mass and the mass accretion rate. This can be done very efficiently by obtaining Halpha imaging of fields where deep HST photometry already exists in the V and I bands. We have developed a novel method to reliably measure the mass accretion rate using a combination of broad-band (V,I) and narrow-band (Halpha) photometry. Since no spectroscopy is needed, our method can provide the accretion rates for several hundred objects per observed field, including relatively mature PMS stars (20-30 Myr old) still approaching the MS. These observations will tremendously augment the value of archival data by increasing by an order of magnitude to more than 10,000 the number of stars with measured accretion rates, while reaching lower-metallicity environments (~1/3 solar for LMC and ~1/9 for SMC) similar to those in place when star formation in the Universe was at its peak, at redshift z~2. Such a large sample will allow us to study in detail and with high statistical significance how PMS stars accrete mass as a function of their age, chemical composition, mass and location in the star forming region.We plan to take images in the Halpha band of nine star forming regions in different environments for which deep HST photometry with the WFC3, ACS, or WFPC2 is already available in at least the V and I bands (for most young clusters also U or B are available for a proper reddening correction). Each of the nine selected star forming region will be observed as part of a visit lasting one orbit. A dithering pattern is used in each visit, with three or four pointings, meant to cover the gap between the WFC3 chips and to improve the sampling of the PSF.
For most targets, the primary orbit (WFC3) contains only exposures with the Halpha filter F656N, whereas the parallel orbit (ACS) contains short exposures in the V (F606W) and I (F814W) bands and longer exposures in the Halpha band (F658N). Exceptions are the fields containing target HIGH-HH901, for which observations in Halpha are already available but the V band is missing, and target HIGH-30DOR-OFF, for which observations are available in the B and I band but not in V, so besides the long Halpha exposures, also short exposures in V (F606W) will be taken.RESOLVED STELLAR POPULATIONS12falsefalse0.00.0falsefalsefalseSUPPORTEDSTELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONYOUNG ASSOCIATIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000STELLAR CLUSTERACCRETION DISKSTAR FORMING REGIONJ2000J2000WFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF656NACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WThe scheduling data was generated by CASM 21.0.CASM was run in Phase II mode.Primary only V, parallel V and I136449347000050.0(Tic-Visit
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