0
Assigned ID: 3058
----- Attempting Submission 1 (Thu Mar 24 20:52:27 GMT 2022) -----
The number of orbits used exceeds the number allocated
Updated Phase 2 by shortening exposure times for remaining visits in Reduced Gyro Mode.
2B added - emailed by PI
313332347
----- Attempting Submission 1 (Tue Jul 12 22:38:54 GMT 2022) -----
HST Phase II Proposal 17212 successfully submitted.
Receipt: # 17212-1
----- Attempting Submission 3 (Thu Jul 14 18:05:55 GMT 2022) -----
HST Phase II Proposal 17212 successfully submitted.
Receipt: # 17212-3
----- Attempting Submission 4 (Thu Jul 14 19:40:27 GMT 2022) -----
HST Phase II Proposal 17212 successfully submitted.
Receipt: # 17212-4
----- Attempting Submission 5 (Thu Jul 28 15:11:48 GMT 2022) -----
HST Phase II Proposal 17212 successfully submitted.
Receipt: # 17212-5
----- Attempting Submission 6 (Thu Jul 28 19:00:23 GMT 2022) -----
----- Attempting Submission 7 (Thu Oct 13 00:16:20 GMT 2022) -----
----- Attempting Submission 8 (Thu Feb 02 00:03:35 GMT 2023) -----
----- Attempting Submission 9 (Fri Apr 21 01:30:55 GMT 2023) -----
----- Attempting Submission 10 (Wed Dec 06 17:31:06 GMT 2023) -----
----- Attempting Submission 11 (Wed Jul 03 22:09:03 GMT 2024) -----
----- Attempting Submission 12 (Mon Jan 27 13:26:08 GMT 2025) -----
The errors are generated by Visits that have already been completed. No errors for the Visits that still await scheduling.
Caught in the Act: The Hierarchical Formation of Abell 1185
Abell 1185 is a nearby example of a rich galaxy cluster still undergoing violent hierarchical assembly. Its brightest member galaxy, NGC 3550, is offset by 150 kpc from the cluster's dynamical center and is in the throes of cannibalizing several neighbors. Abell 1185 is also home to a population of intergalactic globular clusters, as well as the interacting system Arp 105, a spectacular collision between two galaxies that has spawned a compact region of intense star formation known as Ambartsumian's Knot as well as a 100-kpc-long tidal tail with embedded star clusters and newborn dwarf galaxies. Abell 1185 offers a unique opportunity to witness the ongoing birth of a dynamically young cluster and its constituents, a present-day analog to cluster formation at earlier epochs. We propose to carry out a comprehensive WFC3+ACS imaging survey of A1185 to learn more about the ongoing creation of galactic and intergalactic stellar populations in this dynamic environment. The resulting dataset will be of comparable legacy value to the ACS Treasury Survey of the Coma Cluster (GO 10861) for a fraction of the investment of time, providing a snapshot of a rich cluster environment that represents an important earlier stage in galaxy cluster evolution.
Field Selection: The WFC3/UVIS and ACS/WFC cameras will be used in Coordinated Parallel mode to mosaic the main body of A1185, covering a large contiguous area with 12 pointings. These fields include all of A1185's brightest galaxies as well as Arp 105 and the diffuse intracluster populations in the central regions. While WFC3 is our primary instrument, the ACS parallel fields are also an essential component of this program because they sample the southern regions of the cluster, effectively doubling our sky coverage at no additional cost. Together, they survey the inner 0.5 Mpc, sampling a wide range of local environments and mapping the distribution of intergalactic globular clusters including any substructure. Combining the primary WFC3 fields with parallel ACS fields allows the cluster to be mapped efficiently.
Exposure Times and Filters: These observations aim to reach the peak of the globular cluster luminosity function, allowing the brightest half of the globular cluster population in A1185 to be detected. This requires detecting point sources to V = 28.3 mag. The F475X and F600LP filters will be used for the primary WFC3 observations, as they provide an excellent wavelength baseline for reliable color/metallicity determination will reach the desired faint magnitudes as efficiently as possible to detect faint globular clusters at the distance of A1185. For WFC3/UVIS, F475X provides extra throughput and depth compared to F475W and has been used successfully for other extragalactic globular cluster programs, while the longpass F600LP filter is near the peak of the WFC3/UVIS efficiency curve and hence goes deep quickly. These filters are readily transformed to standard bands, allowing a straightforward comparison of the WFC3 results to the ACS fields, and to other programs, such as the Coma Treasury Survey. For the ACS parallel fields, the choice of F475W and F814W filters maximizes depth and wavelength coverage and are among the most common filters used for studies of extragalactic globular cluster systems, which facilitates comparison with previous results. These filters are also well matched to available archived images, such as the Hubble Frontier Fields parallel "blank" fields, which can be used to empirically determine the expected contamination from background sources, which is especially useful for quantifying A1185's intergalactic globular cluster population. These filter choices ensure that the WFC3/UVIS and ACS/WFC observations will reach comparable depths. The small overlap between the WFC3 and ACS fields allows robust empirical color transformations to be derived between these filter combinations. Using the WFC3/UVIS Exposure Time Calculator and assuming a typical globular cluster spectral energy distribution, a total integration time of 4155 sec will detect point sources down to V = 28.3 with S/N ~ 6.2 for the F475X filter, and 3190 sec with F600LP will yield S/N ~ 6.4, adequate for reliable separation of resolved and unresolved objects and with photometric errors that are small compared to the expected width of the globular cluster luminosity. This requires three orbits per field and hence a total of 39 orbits to observe the 13 primary and 13 coordinated parallel fields. A six-step dither pattern will be used to optimize drizzling reductions. For the parallel ACS/WFC observations, two orbits with F475W will detect globular clusters at V = 28.3 with S/N ~ 4.0, while one orbit with the F814W filter will have S/N ~ 4.7.
Dr. Michael Gregg has been PI or CoI on 35 HST programs to date. He is an internationally recognized expert on stellar populations in galaxies, galaxy clusters, gravitationally lensed quasars and more exotic types of active galaxies and quasars nearly buried by dust. Dr. Gregg has authored or co-authored more than 120 peer-reviewed papers in leading journals. He will contribute to all components of this research program, from data reductions to analysis to eventual publication of results.
Dr. Roberto De Propris has been PI or CoI of two HST programs to date. He is an internationally recognized expert on the birth and evolution of galaxies, galaxy interactions and stellar populations in galaxies. Dr. De Propris has published more than 140 papers in peer-reviewed journals. He will contribute to all components of this research program, with particular attention to interpretation of the results and comparison with theoretical and numerical models.
Dr. Michael West has been PI or CoI of 18 HST programs to date. He is an internationally recognized expert on galaxy formation and evolution, clusters of galaxies, and the environmental impact of the large-scale structure of the universe on galaxies and galaxy clusters. Dr. West has published nearly 100 peer-reviewed papers in leading journals. He will contribute to all components of this research, and will serve as PI of this program.
Galaxies
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CLUSTER OF GALAXIES
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