0
Assigned ID: 211
----- Attempting Submission 1 (Thu Apr 07 11:48:55 GMT 2016) -----
HST Phase I Proposal 211 (n44_medium-proposal_2016.apt) successfully submitted.
Receipt: # 211-1
0
----- Attempting Submission 1 (Mon Jul 18 12:51:04 GMT 2016) -----
HST Phase II Proposal 14689 (14689_MYSST_submitted.apt) successfully submitted.
Receipt: # 14689-1
----- Attempting Submission 2 (Wed Sep 14 11:37:10 GMT 2016) -----
HST Phase II Proposal 14689 (14689_MYSST_resubmitted.apt) successfully submitted.
Receipt: # 14689-2
----- Attempting Submission 3 (Thu Oct 06 15:54:34 GMT 2016) -----
HST Phase II Proposal 14689 (14689_MYSST_new_strategy.apt) successfully submitted.
Receipt: # 14689-3
----- Attempting Submission 4 (Mon Oct 10 13:20:20 GMT 2016) -----
MYSST: Mapping Young Stars in Space and Time - The HII Complex N44 in the LMC
The stellar initial mass function (IMF), and the timescale and lengthscale of star formation (SF) are critical issues for our understanding of how stars form. Low-mass pre-main-sequence (PMS) stars, having typical contraction times on the order of a few 10 Myr, are the live chronometers of the SF process and primary informants on the low-mass IMF of their host clusters. Our studies show that young star clusters, embedded in star-forming regions of the Large Magellanic Cloud (LMC), encompass rich samples of PMS stars, sufficient to study clustered SF in low-metallicities with optical HST photometry. Yet, the lack of a complete comprehensive stellar sample retains important questions about the universality of the IMF, and the time- and length-scale of SF across a typical molecular cloud unanswered. We propose to address these issues by employing both ACS and WFC3 with their high sensitivity and spatial resolving power to obtain deep photometry (m_555~29 mag) of the LMC star-forming complex N44. We will accomplish a detailed mapping of PMS stars that will trace the whole hierarchy of star formation springing from one giant molecular cloud. Our analysis will provide an unbiased determination of the timescale for SF and the sub-solar IMF down to the hydrogen burning limit in a variety of clustering scales for the first time. Our findings will have a significant impact on our comprehensive understanding of SF in the low-metallicity environment of the LMC. We maximize the HST observing efficiency using both ACS/WFC and WFC3/UVIS in parallel for the simultaneous observations of N44, its ensemble of HII regions and their young stellar clusters in the same F555W and F814W filters.
We request ACS/WFC and WFC3/UVIS imaging of the star-forming complex N44 in the Large Magellanic Cloud. The purposes of this program is the complete census of low- and intermediate-mass pre--main-sequence (PMS) stars in the complex. Observations in two well-used optical broad filters, F555W and F814W, equivalent to standard V- and I-band filters will be obtained. The cameras will operate in parallel, performing observations in different filters. In this manner we will cover the whole extent of the complex with the half number of orbits than that required for the use of only one camera. Both cameras achieve equivalently exceptional sensitivity in the required wavelength range, and large field coverage. Two main mosaics, each of 3x4 pointings will be needed for the coverage of the whole extent of the complex N44, each to be constructed by different camera. Depending on the orientation angle (and the epoch of observation) one of the camera will scan the northern part of N44 and the other the south, producing the corresponding mosaics. Our spatial coverage will thus include the northen super-bubble with the associations LH47/48 ("north" mosaic), and the southern molecular clump, where association LH49 is located ("south" mosaic). Three additional pointings are strategically selected and will be observed with the same strategy, attached to the east of the main mosaics in order to cover interesting features of the star-forming complex (pointings designated additionally as "field") and the galactic field. The complete mosaic will thus cover the most active star-forming regions in the HII complex together with a substantial area free from any radiative emission, comprising the field stellar population within the vicinity of the complex.
The science exposure times for this program have been estimated with both the ACS and WFC3 ETCs, based on our previous experience. We have assumed an optimum S/N ~ 20 to 5 at 26 < V < 29 for spectral energy distributions of late-type PMS stars down to M5 derived from the NextGen and AMES synthetic spectra libraries. We will perform dithered observations using a sub-pixel box pointing pattern. Observations of each pointing of the mosaics will be separated in different visits. Each visit will include two orbits. For the scientific success of the program an absolute minimum of exposure times of ~5,000 sec in F555W and ~3,500 sec in F814W are necessary. With our mosaicing strategy we will achieve in total longer exposures due to the significant overlap between the mosaics tiles. This secures our depth request of V ~ 29 mag. The mosaics (primary and parallel, or south and north) will be observed twice, which improves the schedulabitily and keeps the number of orbits per visit equal to 2. Each of the southern and northern halfs of N44 will be covered by only one of the cameras (observing in both filters), so that issues of consistency in PSFs, filter responses, CTEs, geometric distortions etc, betweent the cameras to be avoided. This ensures a uniform sample of detections for every part of the star-forming complex. Short exposures (in both F555W and F814W) in order to measure the bright stellar content of the region will be also performed. For reasons of complete coverage of the mosaics, WFC3 is being selected as the primary camera, but with our strategy all acquired data (both primary and parallel in both filters) will have equally significant value for the success of the program.
Short exposures warnings: For the performance of the necessary short exposures the parallel exposures overun the primary (a related warning is issued by APT). However, this is not an issue because the parallel exposures are as important as the primary.
Orientation angles: The orientation angles are determined based on the succesful coverage of the complete star-forming complex, while considering the need for flexibility in the scheduling of the visits due to roll angle constraints.
Stellar Populations
0
false
false
false
true
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SUPPORTED
STELLAR CLUSTER
STAR FORMING REGION
YOUNG ASSOCIATION
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Imaging
No
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Imaging
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ACS/WFC
Imaging
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Imaging
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Imaging
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Imaging
No
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The scheduling data was generated by CASM 24.2.
CASM was run in Phase II mode.
/Users/dgoulier/My Research/Proposals/HST/Cycle24/N44/apt/OP-cache/14689_MYSST_new_strategy_final-v25.xml
(Tic-Visit
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:data-volume 4583776
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(Tic-Obset
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(Tic-Orbit
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:orbit-number 1
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:si-vis-utilization 3217
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(Tic-Orbit
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:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3556
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true
2
0
Hst Same orient constraint links visits (25 26 27)
The scheduling data was generated by CASM 24.2.
CASM was run in Phase II mode.
/Users/dgoulier/My Research/Proposals/HST/Cycle24/N44/apt/OP-cache/14689_MYSST_new_strategy_final-v26.xml
(Tic-Visit
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:coron NIL
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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true
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Hst Same orient constraint links visits (25 26 27)
The scheduling data was generated by CASM 24.2.
CASM was run in Phase II mode.
/Users/dgoulier/My Research/Proposals/HST/Cycle24/N44/apt/OP-cache/14689_MYSST_new_strategy_final-v27.xml
(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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true
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