0
Assigned ID: 358
----- Attempting Submission 1 (Fri Apr 10 04:35:20 GMT 2015) -----
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIME
0
----- Attempting Submission 1 (Tue Jul 21 13:29:53 GMT 2015) -----
----- Attempting Submission 2 (Fri Aug 05 15:22:26 GMT 2016) -----
There are some warnings about parallels extending the alignment time, but I'm not sure how to eliminate these warnings.
parallels are important - I spent a significant amount of time making sure to fit them in.
Exploring the nature and synchronicity of early cluster formation in the Local Group
Globular clusters (GCs) are fossil relics from which we can obtain critical insights into star formation processes at very early epochs and the growth of galaxies over cosmological time. It has recently become clear that Galactic GCs are complex systems harboring multiple stellar populations with a variety of unexpected characteristics, posing severe difficulties for conventional formation models. Moreover, precision photometry from HST has enabled accurate relative age measurements for a large sample of Galactic GCs, revealing the presence of tight correlations in age-metallicity space that are difficult to explain in the canonical two-phase picture for the assembly of the GC system. We propose a new angle of attack on both these problems by conducting deep UV-optical imaging of old GCs in the Large Magellanic Cloud - one of our nearest neighbors and a representative of the class of dwarf galaxies usually assumed to be the "building blocks" of larger galaxies in LCDM cosmology. We will conduct the first thorough photometric characterisation of multiple populations in any extragalactic GCs, allowing us to begin assessing the universality of the multi-population phenomenon and its environmental dependence. Furthermore, the cluster main sequence turn-offs will be delineated with unprecedented clarity, facilitating the most precise comparison ever made between the ages of Galactic and external GCs. This constitutes arguably the most sensitive available test of the synchronicity of early star formation across the Local Group. As a bonus, we will be able to determine the distance to the LMC to a few percent accuracy using the method of subdwarf fitting.
To achieve our primary science goals we will observe using the ACS/WFC F606W and F814W filters, and the WFC3/UVIS F336W filter. In mid-optical passbands ACS/WFC is the preferred instrument due to its higher throughput; utilizing this camera and the (F606W,F814W) combination will also ensure data homogeneous with those obtained for Galactic GCs as part of the GC Treasury project (Sarajedini et al. 2007), facilitating a direct age comparison. The WFC3/UVIS F336W filter is critical for obtaining CMDs maximally sensitive to the presence of multiple populations, including light element abundance variations, and will ensure complementarity with the Cycle 21 UV Legacy survey of Galactic GCs (GO-13297) which also uses this filter. Although filters further into the UV in principle lead to even greater splitting of CMD fiducial sequences, F336W is the bluest filter for which we can obtain adequate S/N photometry for our (distant) targets.
Our targets span declinations of -58d to -84d, resulting in visibility periods of 58 to 61 min per orbit. Here we assume the shortest window of 58 min. Based on our experience from the GC Treasury program, we require (F606W,F814W) photometry with S/N= 20 at Mv = 8.0 in order to delineate the unevolved MS adequately for precise age measurements. At the distance and mean reddening of the LMC, this means S/N= 20 for MS stars (spectral type K0V) at V = 26.7. This can be achieved as follows:
Orbit 1: 6 min for guide star acquisition, 38.4 min total F606W exposure (3 x 12.8 min), 0.5 min short F606W exposure, 11.5 min imaging overhead, 1.5 min dithering overhead.
Orbit 2: 4 min for guide star re-acquisition, 43.8 min total F606W exposure (3 x 14.6 min), 9 min imaging overhead, 1 min dithering overhead.
Orbit 3: 4 min for guide star re-acquisition, 40.5 min total F814W exposure (3 x 13.5 min), 0.5 min short F814W frame, 11.5 min imaging overhead, 1.5 min dithering overhead.
Orbits 4-5: 4 min for guide star re-acquisition, 43.8 min total F814W exposure (3 x 14.6 min), 9 min imaging overhead, 1 min dithering overhead.
Total exposure times are 4960s in F606W and 7720s in F814W. According to the ETC these will result in S/N= 20.6 and 21.4, respectively, for MS stars at V = 26.7. The two short frames help with photometry of bright RGB stars, which will saturate in long exposures. Saturated star photometry is possible for both ACS/WFC and WFC3/UVIS and we will utilise this to better populate the bright CMD sequences.
The F336W imaging is more challenging; however from Figure 2 we need only reach ~2 mag below the MS turnoff, i.e., to V = 24.7. This may be achieved in four orbits:
Orbit 1: 6 min for guide star acquisition, 44.1 min total F336W exposure (3 x 14.7 min), 6.8 min imaging overhead, 1 min dithering overhead.
Orbits 2-4: 4 min for guide star re-acquisition, 46.2 min total F336W exposure (3 x 15.4 min), 6.8 min imaging overhead, 1 min dithering overhead.
The total exposure time is 10960s, leading to S/N= 11.3 for MS stars at V = 24.7. At the level of the MS turn-off and SGB, V = 22.7, we achieve S/N= 58.0. Overall we thus require a total of 9 orbits per GC for all three filters, bringing our total request to 54 orbits.
Our team possesses considerable experience in reducing HST observations. We will photometer the images with specifically tailored PSF-fitting software such as dolphot and/or daophot/allframe (Stetson 1994), and standardize the data onto the native HST system using the formalism of Sirianni et al. (2005) with the updated zeropoints from the STScI web site. This standardization approach is the same one we adopted in the Treasury program GO-10775, and the local subdwarf program GO-11704.
RESOLVED STELLAR POPULATIONS
12
false
false
false
false
false
false
SUPPORTED
STELLAR CLUSTER
GLOBULAR CLUSTER
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
ACS/WFC
Imaging
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No
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