0
Assigned ID: 255
----- Attempting Submission 1 (Fri Aug 17 11:28:56 GMT 2018) -----
First submission had indicated a problem with Visit 11. It looks as the poblem were related to APT Version 2.0.
In this submission there are no any indication of any problem because of that we are submitting again.
Resubmission due to "the safe-ing of HST earlier this fall, the Guide Star Acquisition time. ....we have released an updated version of APT that adds
an extra minute of GS Acq time and because of this your program is now overrun.", several visits were updated with the exposures time.
-1338593649
----- Attempting Submission 1 (Tue Dec 04 19:45:58 GMT 2018) -----
HST Phase II Proposal 15630 (go15630.v4.apt) successfully submitted.
Receipt: # 15630-1
----- Attempting Submission 2 (Tue Dec 04 20:03:18 GMT 2018) -----
----- Attempting Submission 3 (Thu Dec 06 16:53:19 GMT 2018) -----
A Full Characterisation of the Multiple Population Properties of Young Globular Clusters
Recent HST surveys of massive stellar clusters in the Galaxy and Magellanic Clouds have opened an entirely new window on the phenomenon of multiple populations (MPs, i.e. star-to-star abundance variations within clusters). First, the HST Galactic GC UV Legacy survey has found a strong trend between the present day mass of ancient globular clusters (GCs) and the properties of the multiple populations within them, namely an increase in the fraction of chemically anomalous (a.k.a. enriched or second generation) stars as a function of cluster mass. Secondly, the Magellanic Cloud survey has found a strong correlation between the cluster age and the properties of the MPs (at a fixed mass), with clusters younger than 2 Gyr not showing abundance variations and clusters above this age, showing them. Additionally, from 2 to ~10 Gyr the survey found an increase in the abundance spread ([N/Fe]) with increasing age.
These two surveys applied different strategies so that unfortunately the results are not directly comparable. Here we propose to put the two surveys on the same footing by observing a sub-sample of the Magellanic Cloud clusters with the F275W filter. By using the newly developed "chromosome maps" (exploiting the F275W, F336W, F438W, and F814W images) we will be able to directly compare the young, intermediate and ancient clusters in a homogeneous manner. It will also allow us to trace the evolution of MPs (in terms of their detailed abundances in N, O, and He), as a function of age. These observations will hopefully lead to new theories for the origin of MPs in an entirely unexpected direction from all previous work.
We propose to obtain imaging of 5 massive star clusters within the LMC/SMC, spanning a wide range of ages (2-8 Gyr), in order to search for elemental abundance spreads and multiple populations. All 5 clusters will be observed in the F275W, and 2 clusters in the F814W WFC3/UVIS filters. These filters will be additinal to alredy exciting early observations of the same clusters in F336W, F343N and F438W WFC3/UVIS filters,
which will provide accurate color-magnitude diagrams (CMD) for studies of these phenomena and build a "chromosome maps" in
prseudo-color-color diagrams (F275W, F336W, F438W and F814W).
A CMD for such a large range of stellar ages covers everything from red and very bright red giants down to the main sequence stars of various brightness and colors. To reach our science goals, it is crucial not to saturate the bright giants by using a short exposure in F814W filters and to reach a sufficient depth beyond the main-sequence turn-off using long exposures. It is also important for us to reach S/N~6 per single exposure for cluster RGB base mag limit and ~14-15 for the brighter in F275W WFC3/UVIS filter exposures. To cover the gap between the two WFC3/UVIS CCD, chips, we are using multi- dithered pointings with the sub-pixles steps in X and Y directions. In order to maximize the overlap with early observations we also require a specific orientation to match the orientation of those target clusters which have archival observations with the WFC3/UVIS. This orientation is specified in the Visit Orientation Requirement for these clusters/visits as follows:
NGC416: Visits 01-03, Min=250, Max=260 decimal degree
Lindsay1: Visits 04-06, Min=255, Max=265 decimal degree
NGC1783: Visits 07-08, Min=290, Max=300 decimal degree
NGC2121: Visits 09-11, Min=195, Max=205 decimal degree
NGC1978: Visits 11-14, Min=260, Max=270 decimal degree
Stellar Populations
3
false
false
false
false
false
false
false
SUPPORTED
STELLAR CLUSTER
GLOBULAR CLUSTER
OPEN CLUSTER
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
OPEN CLUSTER
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
OPEN CLUSTER
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
OPEN CLUSTER
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
WFC3/UVIS
Imaging
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No
F275W
WFC3/UVIS
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No
F275W
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F814W
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F275W
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:low-sky "N"
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:pcs-gap 0
)
(Tic-Orbit
:proposal-id 15630
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:dark-offset NIL
:dark-utilization 0
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)
(Tic-Orbit
:proposal-id 15630
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3486
:pcs-gap 0
)
true
3
0
The scheduling data was generated by CASM 26.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 15630
:visit-id "13"
:proposal-version -1
:trans-version "20181130"
:date "06-Dec-2018 11:45:42.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 1732464
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15630
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:obset-id "13"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15630
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:orbit-number 1
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:si-vis-utilization 3130
:al-overhead-at-end 122
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3486
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 15630
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:orbit-number 2
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:si-vis-utilization 3140
:al-overhead-at-end 122
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3486
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 15630
:visit-id "13"
:orbit-number 3
:pcs-time 302
:si-vis-utilization 3133
:al-overhead-at-end 122
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3486
:pcs-gap 0
)
true
3
0
The scheduling data was generated by CASM 26.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 15630
:visit-id "14"
:proposal-version -1
:trans-version "20181130"
:date "06-Dec-2018 11:45:44.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 2021232
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15630
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)
(Tic-Orbit
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:orbit-number 1
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:si-vis-utilization 3137
:al-overhead-at-end 122
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3486
:pcs-gap 0
)
true
1
0