0 Assigned ID: 59 ----- Attempting Submission 1 (Sat Feb 29 20:29:32 GMT 2020) ----- HST Phase I Proposal 59 successfully submitted. Receipt: # 59-1 ----- Attempting Submission 2 (Wed Mar 04 23:35:09 GMT 2020) ----- HST Phase I Proposal 59 successfully submitted. Receipt: # 59-2 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 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 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 0 ----- Attempting Submission 1 (Mon Jun 22 17:12:59 GMT 2020) ----- Based on the ETC and on archive data, we believe that the adopted flah level are appropriate for our purposes. Suggestions and corrections are welcome. Understanding the Extreme Population in the Globular Cluster NGC 6402 (M14): Breaking the Degeneracy of Cluster Formation Scenarios Multiple populations are recognized to be a common trait of nearly all ancient Globular Clusters (GCs), but no model or scenario so far proposed for their formation satisfies all the observational constraints, and observations are still necessary to discriminate among competing models. HST observations have largely contributed to define the properties of multiple populations; in particular, HST observations have clearly revealed the photometric manifestation of the presence chemically distinct groups of stars. A recent spectroscopic investigation of NGC6402 has shown that this massive GC hosts three populations, including a primordial, a quasi-primordial and an extreme group, this latter displaying light elements abundances that in other GCs, (e.g.NGC2808), are associated with a very high helium. This peculiar distribution of abundances has stimulated innovative formation scenarios where the cluster requires two distinct sources and timescales of enrichment. We propose to derive the `chromosome map' two-color diagram that harnesses the unique UV capabilities of the UVIS channel of WFC3 and investigate the possible abundance gap in these spectro--photometric data, by separating the different groups. We will then determine the relative helium abundances of the groups, and discern between two competing scenarios for the formation of the extreme population in this cluster: either a scenario in which these stars formed from pristine gas mixed with ejecta of a supermassive star formed and living in the first ~5-15 Myr in the cluster core; or the Asympotic Giant Branch (AGB) scenario, in which the extreme stars are formed from the pure ejecta of super-- AGB stars. The observing program is designed to image the central regions globular cluster NGC6402 in fours WFC3/UVIS filters: F275W, F336W. F438W and F814W. The resulting photometry will be used 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. There are 13 1-orbit visits. The images are properly dithered to optimize the resulting photometric and astrometric quality. The parallel will be taken through F475W and F814W filters of WFC/ACS to allow the investigation of multiple populations with different helium abundance in the external regions from the F814W vs. F475W-F814W CMD. Our team involves internationally-recognized astronomers who have provided substantial contribution to he research on globular clusters and on their stellar populations. The strength of the present proposal is to put together the potentials of different observational techniques, such as photometry, astrometry and spectroscopy with modelling 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. P. Milone is expert in photometry and astrometry of HST data and developed sophisticated methods for the data reduction and for the determination of the relative helium abundance of the stellar populations in globular clusters. (2) E. Vesperini is one the major experts on dynamics of globular clusters and of their stellar populations. (3) V. Caloi, F. D'Antona and M. Tailo are experts in stellar evolution and in the scenarios on the formation and evolution of multiple population. (4) C. Johnson and A. Marino possess excellent skills in the spectral analysis and are responsible for some of the most important discoveries in the field of multiple populations of the last decade. C. Johnson has led the work on the discovery of the extreme chemical pattern of NGC6402. Stellar Populations and the Interstellar Medium 6 false false true false false false false SUPPORTED STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F438W ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F814W /tmp/OPVisit12629825401071971251.xml The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 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