Submission #1 - May 22 - 3:40 PM
Submission #2 - May 23 - 9:27 PM
Submission #3 - May 24 - 1:50 PM
Submission #4 - May 24 - 5:43 PM503951718Your proposal could not be saved.
Submission aborted.
Assigned ID: 4044
----- Attempting Submission 1 (Mon May 22 19:40:48 GMT 2023) -----
HST Phase I Proposal 4044 successfully submitted.
Receipt: # 4044-1
----- Attempting Submission 2 (Wed May 24 01:26:53 GMT 2023) -----
HST Phase I Proposal 4044 successfully submitted.
Receipt: # 4044-2
----- Attempting Submission 3 (Wed May 24 17:50:15 GMT 2023) -----
HST Phase I Proposal 4044 successfully submitted.
Receipt: # 4044-3
----- Attempting Submission 4 (Wed May 24 21:43:20 GMT 2023) -----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
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
ORBITAL VISIBILITY OVERRUN
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
ORBITAL VISIBILITY OVERRUN
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
The specified GS Acq Scenario is not in the current list of valid scenarios.
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
The specified GS Acq Scenario is not in the current list of valid scenarios.
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 browserNov 08, 2024 - Re-submission by S. T. Sohn. Changed orientations for Visits 17, 18, 19, 20 following PC's suggestions.
Oct 24, 2024 - Re-submission by S. T. Sohn. Reverted visits 13 and 14 back following PC's suggestion.
Oct 23, 2024 – Re-submission by S. T. Sohn. Changed pointings for visits 15, 16, 17, 18, 19, 20. Changed exposure patterns for visits 13-20.
Oct 09, 2024 - Re-submission by S. T. Sohn. Changed pointings for visits 13 and 14 (repeates of 3 and 4). Changed exposure patterns to fit in each orbit.
Dec 21, 2023 - Re-submisison by S. T. Sohn. Reduced exposure times, and removed BEFORE requirement for visit 01
Oct 19, 2023 - Re-submission by S. T. Sohn. Original visits 03 / 04 / 05 / 06 with 2 orbits each have been now separated into single-orbits visits 03,04 / 05,06 / 07,08 / 09,10
Oct 13, 2023 - Re-submission by S. T. Sohn. Slightly shifted UMI-E3 southward to allow guide star in FGS2 for visit 05.
Oct 13, 2023 - Re-submission by S. T. Sohn. Previous version had a mistake of Visit 05 Schedulability set to 100. Fixed it by changing back to "None Selected".
Oct 09, 2023 - Re-submission by S. T. Sohn. Changed the POS-TARG values to the ones in WFC3 ISR 2023-05 following suggestion by the CS (Jay Anderson).
Sep 13, 2023 - Initial submission by S. T. Sohn-820095506----- Attempting Submission 1 (Wed Sep 13 14:33:45 GMT 2023) -----
----- Attempting Submission 2 (Tue Oct 10 00:08:14 GMT 2023) -----
----- Attempting Submission 3 (Fri Oct 13 11:45:18 GMT 2023) -----
----- Attempting Submission 4 (Fri Oct 13 16:50:56 GMT 2023) -----
----- Attempting Submission 5 (Thu Oct 19 16:39:18 GMT 2023) -----
----- Attempting Submission 7 (Thu Dec 21 16:29:55 GMT 2023) -----
----- Attempting Submission 8 (Wed Oct 09 19:33:50 GMT 2024) -----
----- Attempting Submission 9 (Wed Oct 23 23:24:02 GMT 2024) -----
HST Phase II Proposal 17434 successfully submitted.
Receipt: # 17434-9
----- Attempting Submission 10 (Thu Oct 24 19:30:24 GMT 2024) -----
----- Attempting Submission 11 (Fri Nov 08 19:53:01 GMT 2024) -----Warnings are for completed observations.Shedding Light on Dark Matter: Internal Proper Motions in Ursa MinorDetermination of the mass density profiles of dwarf galaxies (and specifically whether there is a central core or cusp) provides a critical test of both the properties of dark matter (DM) and the physics of cosmological structure formation. The Milky Way nearby classical dwarf spheroidal galaxies (dSphs) provide some of the best dynamical constraints. While large line-of-sight velocity datasets exist (some thousand stars per galaxy), interpretation is hindered by the well-known mass vs. velocity-anisotropy degeneracy of stellar dynamics. This can be resolved with proper motion (PM) measurements that yield 3-D velocity information. This is well beyond the reach of Gaia, given the small velocity dispersions of dSphs and the absence of bright stars. HST is the only observatory that can advance this problem, given its combination of photometric depth, high spatial resolution, and long time baselines. We propose to obtain HST imaging of eight previously imaged fields (four prime plus four parallels) in the nearby Ursa Minor dSph, to obtain high-accuracy PMs for thousands of stars in this galaxy. This unique data set will provide a direct determination of the velocity anisotropy profile. Through detailed dynamical modeling, this will constrain the DM density cusp slope with an uncertainty of only 0.1, allowing us to discriminate at 10-sigma confidence between a core or NFW cusp. The results will give unique constraints on both the nature of DM, and the physical mechanisms that shape DM density profiles in galaxies. The proposed program therefore shows how HST can still be used, after 33 years in orbit, to tackle unanswered fundamental questions in astrophysics.The primary goal of this program is to measure the internal proper motion kinematics of the dwarf spheroidal galaxy Ursa Minor using multi-epoch HST imaging data. We will target 8 primary WFC3/UVIS + 8 parallel ACS/WFC = 16 fields in total. Each target field will be observed for two orbits. The telescope orientation conditions are added as special requirements for each visit to match the filed coverages between the pre-existing first-epoch data and the second-epoch data that will be obtained through this program. This is essential for controlling systematics when measuring proper motions.All investigators are members of the HSTPROMO group, led by co-I van der Marel, which has published numerous papers reporting proper motion measurements of dwarf galaxies, globular clusters, individual stars along stellar streams, and distant Milky Way (MW) halo stars.
- PI Vitral is an expert in velocity anisotropy analysis and dynamical mass estimation, and has particularly published papers studying the internal kinematics and dynamics of MW globular clusters.
- Co-PI Sohn has led many HST programs over the past decade for measuring proper motions of M31, bulk proper motions of dwarf spheroidal galaxies in the Milky Way halo (Leo I, Draco, and Sculptor), individual proper motions of stars along stellar streams such as Sagittarius, Orphan, and Lethe, distant Milky Way globular clusters, and M31 satellites NGC 147 and 185. He has been the PI for several of these programs.
- Co-I del Pino-Molina is an expert in analysis of internal dynamics of dwarf galaxies in the Local Group.
- Co-I Bennet is an expert in satellites inside and outside of the LG, and has previous experience leading successful HST programs.
- Co-I Watkins is an expert in velocity anisotropy analysis and dynamical mass estimation, and has particularly published papers studying the internal kinematics and dynamics of MW globular clusters.
- Co-Is Libralato and Bellini are experts of data reduction, proper-motion measurements and internal kinematics of globular clusters.
- Co-I Chaname has done extensive work using Gaia and proper motion data to build dynamical models of dSphs.
- Co-Is Patel and van der Marel are experts in dynamical modeling of Local Group galaxies including both equilibrium and N-body modeling.
See list of refereed publications by the HSTPROMO group at http://www.stsci.edu/~marel/hstpromo.html#Papers.Stellar Populations and the Interstellar MediumGalaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VGALAXYDWARF ELLIPTICALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000L=3.9 x 10^5 Lsun, VWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF606WThe scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.This is a 2-orbit visit targeting the UMI-C1 field. We will image both the primary WFC3/UVIS and parallel ACS/WFC fields using the F606W filter. We have added Orient Ranges requirements and implemented a dither pattern via POS-TARG to align our images with the previous epoch images taken as part of GO-13470. We also added Timing Requirements of BEFORE 01-MAR-2024 to ensure that this visit is observed early in the cycle because for our astrometric analysis, it is important to evaluate the impact of our FLASH settings early in the cycle to determine whether we would need to adjust them for the other visits.(Tic-Visit
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)true11The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.This is a 1-orbit visit targeting the UMI-E2 field. We will image both the primary WFC3/UVIS and parallel ACS/WFC fields using the F606W filter. We have added Orient Ranges requirements and implemented a dither pattern via POS-TARG to align our images with the previous epoch images taken as part of GO-13470. We also added Timing Requirements of BEFORE 01-JAN-2025 to ensure that this visit is observed by the end of Cycle 31.(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
:proposal-id 17434
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:trans-version "20240604"
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(Tic-Obset
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(Tic-Orbit
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:data-volume 1718912
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(Tic-Obset
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(Tic-Orbit
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3151
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:trans-version "20240604"
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:data-volume 2007648
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(Tic-Obset
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(Tic-Orbit
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(Tic-Obset
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(Tic-Orbit
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:pcs-time 380
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:dark-offset NIL
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)true10The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.This is a 1-orbit visit targeting the UMI-E3 field. We will image both the primary WFC3/UVIS and parallel ACS/WFC fields using the F606W filter. We have added Orient Ranges requirements and implemented a dither pattern via POS-TARG to align our images with the previous epoch images taken as part of GO-13470. We also added Timing Requirements of BEFORE 01-JAN-2025 to ensure that this visit is observed by the end of Cycle 31.16996601480005.150000000000006(Tic-Visit
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:proposal-version -1
:trans-version "20240604"
:date "23-Oct-2024 14:01:40.0"
:trans-errors '(:WARNINGS 2 :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 2007648
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17434
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:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
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:internal-dur-at-end 1015
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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(Tic-Obset
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(Tic-Orbit
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:low-sky "N"
:pcs-visibility 3151
:pcs-gap 0
)true10The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.This is a 1-orbit visit targeting the UMI-E4 field. We will image both the primary WFC3/UVIS and parallel ACS/WFC fields using the F606W filter. We have added Orient Ranges requirements and implemented a dither pattern via POS-TARG to align our images with the previous epoch images taken as part of GO-13470. We also added Timing Requirements of BEFORE 01-JAN-2025 to ensure that this visit is observed by the end of Cycle 31.16997283740005.210000000000008(Tic-Visit
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:proposal-version -1
:trans-version "20240604"
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:trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 2007648
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17434
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:obset-id "09"
:pcs-mode "FGS"
)
(Tic-Orbit
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:al-overhead-at-end 108
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:trans-version "20240604"
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:si-bright-earth-limb-angle 20.0
:data-volume 1718912
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(Tic-Obset
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(Tic-Orbit
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)true10The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.This is a 1-orbit visit targeting the UMI-E4 field. We will image both the primary WFC3/UVIS and parallel ACS/WFC fields using the F606W filter. We have added Orient Ranges requirements and implemented a dither pattern via POS-TARG to align our images with the previous epoch images taken as part of GO-13470. We also added Timing Requirements of BEFORE 01-JAN-2025 to ensure that this visit is observed by the end of Cycle 31.16997454240005.210000000000008(Tic-Visit
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:trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:data-volume 2007648
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(Tic-Obset
:proposal-id 17434
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)
(Tic-Orbit
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:trans-version "20240604"
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:saa-model "29"
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:data-volume 1718912
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)
(Tic-Obset
:proposal-id 17434
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(Tic-Orbit
:proposal-id 17434
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)true10The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.This is a 2-orbit visit targeting the UMI-W3 field. We will image both the primary WFC3/UVIS and parallel ACS/WFC fields using the F606W filter. We have added Orient Ranges requirements and implemented a dither pattern via POS-TARG to align our images with the previous epoch images taken as part of GO-13470.1715068132000185.15000000000003(Tic-Visit
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:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 4015296
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:pcs-mode "FGS"
)
(Tic-Obset
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(Tic-Orbit
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:internal-dur-at-end 668
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:max-dark-utilization 1920
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:pcs-visibility 3151
:pcs-gap 0
)
(Tic-Orbit
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3151
:pcs-gap 0
)true22The scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode.This is a 2-orbit visit targeting the UMI-W4 field. We will image both the primary WFC3/UVIS and parallel ACS/WFC fields using the F606W filter. We have added Orient Ranges requirements and implemented a dither pattern via POS-TARG to align our images with the previous epoch images taken as part of GO-13470.1715079513000185.20999999999998(Tic-Visit
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(Tic-Obset
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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