0Assigned ID: 86
----- Attempting Submission 1 (Mon Mar 02 19:47:11 GMT 2020) -----
HST Phase I Proposal 86 successfully submitted.
Receipt: # 86-1
----- Attempting Submission 2 (Sat Mar 07 00:56:19 GMT 2020) -----
HST Phase I Proposal 86 successfully submitted.
Receipt: # 86-2FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser0----- Attempting Submission 1 (Mon Jun 22 16:50:43 GMT 2020) -----
HST Phase II Proposal 16289 successfully submitted.
Receipt: # 16289-1
----- Attempting Submission 2 (Tue Jun 30 12:59:47 GMT 2020) -----
----- Attempting Submission 3 (Wed Feb 10 14:19:24 GMT 2021) -----
----- Attempting Submission 5 (Wed Feb 24 17:06:34 GMT 2021) -----
HST Phase II Proposal 16289 successfully submitted.
Receipt: # 16289-5Based on the ETC and on archive images, we believe that the adopted flash levels are appropriate.
Comments and corrections are welcome.Multiple stellar populations in Globular Clusters: exploring the low mass regimeTwo broad scenarios have been suggested for the long-held problem of the formation of multiple populations (MPs) in Globular Clusters (GCs). According to the first option, GCs have experienced multiple star-formation episodes and provided a major contribution to the mass of the Galactic halo. As the alternative, there was a single star-formation episode, but a fraction of stars has successively accreted material processed and ejected by massive stars of the same generation. The mass functions (MFs) and the chemical composition of very-low mass M-dwarfs are the missing observational constraints to disentangle between the two scenarios.
Historically, MPs in the GCs have been mostly investigated from UV and visual filters that are very sensitive to the bizarre chemical composition of the GC stars more massive than ~0.6 solar masses. Due to the observational limits of the UV detectors, the faintest region of the color-magnitude diagram (CMD) is nearly unexplored. In the era of JWST, blind to the UV, the recent discovery, based on NIR HST photometry, of multiple sequences of very-low mass stars has provided a new window to study MPs.
We propose to combine F110W and F160W photometry, which allows us to investigate the MPs phenomenon in the poorly-explored M-dwarf regime, with F275W, F336W, and F438W data, mandatory to explore the brightest region of the CMD. From the synergy of NIR, optical and UV photometry we will constrain the chemical composition of the MPs and derive for the first time their mass-functions in the interval between ~0.1 and 0.8 solar masses. Our results will provide a major step forward to constrain the formation scenarios of MPsThe observing program is designed to image three globular clusters: NGC288, NGC5904 and NGC6121:
-- NGC288 and NGC5904 will be observed throght the F275W, F336W and F438W filters of UVIS/WFC3 and through the F110W and F160W filters of NIR/WFC3/
The field of view of each target is located about ~5 arcmin from the cluster center to overlap archive F814W WFC/ACS observations (from GO12193 and GO1329, for NGC288 and NGC5904, respectively).
Archive F814W images will be combined with the new observations in F275W, F336W and F438W to derive the pseudo two color diagram called chromosome map (F275W-2*F336W+f438W vs. F275W-F814W), which is sensitive to multiple stellar populations with different chemical composition. These optical and UV observations will be exploited to study stellar populations among stars more massive than ~0.6 solar masses.
F110W and F160W images of the same field of view will be used to investigate multiple populations among very low mass stars.
-- For NGC6121 UVIS/WFC3 images in F275W, F336W and F438W alone will be collected. Observations of NGC6121 will overlap archive F110W and F160W images from GO12602 and GO14725.
There are 18 1-orbit visits. The images are properly dithered to optimize the resulting photometric and astrometric quality.
The parallel will be taken through F606W and F814W filters of WFC/ACS to allow the investigation of photometric binaries from the F814W vs. F606W-F814W CMD.In the last twelve years our team has published over 220 papers involving two or more members of the team on topics directly related to this proposal. Including the paper on the discovery of multiple populations among M-dwarfs with HST (Milone et al. 2012, ApJ, 754, 34L).
Our team comprises internationally distinguished young and senior scientists who have made substantial contribution to the field of multiple populations in GCs. The strength of the present proposal is to put together the potentials of different observational techniques, such as photometry, astrometry and spectroscopy with modeling to investigate a key topic of outstanding interest in stellar and Galactic astronomy.
We have all the necessary personnel, experience and tools to perform a timely and careful data reduction and analysis of the results. Indeed, our team includes scientists who are spearheads in the analysis of HST data, in the stellar evolutionary and dynamical models, spectroscopy, and in the scenarios on the formation of multiple populations:
(1) A. Bellini, M. Libralato, E.P. Lagioia, A. P. Milone have a long experience in photometric and astrometric data analysis. They have developed sophisticated methods for the data analysis that are the state-ofthe- art for multiple-population studies. This dataset will be of foundamental importance for the PhD thesis of G. Cordoni and E. Dondoglio.
(2) F. D'Antona, S. Jang, A. Renzini, M, Tailo, E. Vesperini are experts in stellar evolution, mass functions, dynamical models crucial to understand how multiple populations formed and evolved.
(3) M. Carlos and A. F. Marino have reputation for possessing excellent skills in the spectral analysis, including spectra of Mdwarfs. They have given a fundamental contribution to the chemical characterisation of different stellar populations in GCs by combining synthetic spectra and multi-bandStellar Populations and the Interstellar Medium0falsefalsefalsefalsetruefalsefalseSUPPORTEDSTELLAR CLUSTERGLOBULAR CLUSTERYESJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERJ2000J2000WFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF160WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF160WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814W/private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit245755848041447009.xmlThe scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.1613340425000274.0(Tic-Visit
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