0Assigned ID: 3967
----- Attempting Submission 1 (Fri May 19 13:01:30 GMT 2023) -----The specified GS Acq Scenario is not in the current list of valid scenarios.6/17/24
Updating orient range for visit 10 to 229-232 for guide star visibility as per Blair's email.
Thanks,
Kristen McQuinn
6/15/24
Orient ranges on visits 1,2,7,and 11 were changed to ensure visibility in RGM as requested via email by Blair Porterfield. visit 10 was unchanged as
the orient ranges still provide schedulable visits.
Kristen McQuinn
10/16/23
Visit 2 and 10 are changed. For both visits, I have now placed the target galaxies on one chipe and the bright stars on the other chip.
Pointings were adjusted slightly and,for visit 2, the orient ranges were changed.
I hope these configurations give us the best quality data!
10/12/2023
Adjusting the pointing + orients for visits 2 and 10 to avoid a bright star impacting the faint galaxy.
I will follow-up with david via email with details.
10/10/23
Adjusting based on comments from David Stark and Blair Poterfield:
Visit 5: changed to a orient range of 294-298 for guide star aquisition. But note that this also required a slight pointing change.
Hopefully the guide star is still viable.
Visits 2 & 10: adjusted the pointing to get more of the target galaxy on the detector. BUT, this also meant putting a bright
star on the same chip as the target. I will follow-up via email with David to ensure that this works.
Thanks!
Kristy McQuinn
9/24/2023
David Stark informed me that there are possibilities of glint artifacts for visits 2, 4,5 and 10. I have adjusted the pointings
and orient ranges slightly to (hopefully) reduce the possibilitiy.
Thanks,
Kristen McQuinn
I was notified by Blair Poterfield that Visit 9 was unscheduable becuase of the lack of quide stars.
As per her recommendation, I have flipped the orient range by ~180 degrees and
made a small adjustment to the pointing. Hopefully this does the trick to fix the guide star problem.
Thanks! Kristy McQuinn
January 10, 2025
I have confirmed the Phase II for visit 13 that is re-executed the failed visit 7.
Kristen McQuinn-2042404971----- Attempting Submission 1 (Thu Aug 31 18:54:39 GMT 2023) -----
----- Attempting Submission 2 (Fri Sep 15 10:31:11 GMT 2023) -----
----- Attempting Submission 3 (Sun Sep 24 15:47:15 GMT 2023) -----
----- Attempting Submission 4 (Tue Oct 10 12:24:07 GMT 2023) -----
----- Attempting Submission 5 (Thu Oct 12 16:09:45 GMT 2023) -----
----- Attempting Submission 6 (Mon Oct 16 17:14:24 GMT 2023) -----
----- Attempting Submission 7 (Sun Jun 16 02:41:57 GMT 2024) -----
HST Phase II Proposal 17480 successfully submitted.
Receipt: # 17480-7
----- Attempting Submission 8 (Mon Jun 17 15:50:45 GMT 2024) -----
----- Attempting Submission 9 (Fri Jan 10 15:32:15 GMT 2025) -----Already checked in previous submissions.The Turn-Down in the Baryonic Tully-Fisher Relation (BTFR)The baryonic Tully-Fisher relationship (BTFR) is a correlation between the total baryonic mass in a galaxy and the maximum velocity of a galaxy's rotation curve (Vmax), which is a tracer of the halo mass. Simulations predict that this power-law relationship will show an inflection at low baryonic masses in the sense that low mass galaxies will have higher values of Vmax than predicted from an extrapolation from higher masses. This inflection is due to the lowest mass galaxies' inability to accrete and retain baryons.
A recent analysis of low mass galaxies has shown evidence in support of this inflection, but with only four galaxies in the critical regime below the inflection point where the prediction can truly be tested. We have identified twelve additional Local Volume galaxies with suitably low baryonic masses and high quality HI velocity fields. Including these galaxies in the analysis will quadruple the number of systems in the key daignostic part of the BTFR, and will fully characterize this putative inflection. However, because these galaxies are nearby and star-forming, their distances cannot be accurately determined from their radial velocities nor from surface brightness fluctuations, and accurate distances are critical to the analysis. Fortunately, the galaxies are close enough that the HST can provide distances from their red giant branch tips through observations of their resolved stars. This type of work can only be done with nearby galaxies and their distances can only be accurately measured with space-based observations.The observations included ACS/WFC imaging in the F606W and F814W filters. The data will be used to measure the distances to the systems from resolved stars (TRGB method) and characterize the stellar properites (star formation histories and metallicities) of the galaxies.
Each of the 12 targets will be observed for 1 orbit. We use a 5x5 pixel dither implemented using pos-targ (equivalent to the ACS WFC DITHER LINE pattern #14) to reject cosmic rays and handle hot pixels. The first pointing is executed with both filters in ACS. After the dither, the observations are then repeated. The exposure time per orbit is split roughly equally between the F606W and F814W filters.
Each visit is 1-orbit. We have place ORIENT constraints to ensure we maximum coverage of the stellar disk and prevent the galaxy centers from falling in the ACS chip gap, while avoiding nearby bright stars.
If HST has to operate on a reduced gyros with reduce field of regard, our current orient requirements may not schedulable. In this case, we could explore if any other orients are possible. We have chosen the submitted orients to maximize the number of scheduling days, but it is possible there are a few additional orients that are viable.The team is comprised of scientists who have signficant expertise working with low mass galaxies and, specifically, with ALFALFA/SHIELD galaxies. Cannon has overseen all aspects of the ALFALFA offshoot program, SHIELD, and has led many of the oberving programs to accumulate the rich supporting data suite for our sample of galaxies. Specific expertise about the HST data is provided by Kristen McQuinn, Andrew Dolphin, and Evan Skillman, who have led multiple high-impact HST programs together measuring distances to nearby galaxies, including the majority of the existing distances to the SHIELD galaxies. Dolphin is also the author of the maximum likelihood TRGB fitting code (used to identify a maximum likelihood and also to calculate likelihood vs. distance modulus, which can be treated as a Bayesian posterior) and the CMD-fitting software. Cannon has deep experience with interferometric observations of low mass galaxies. Jackson Fuson and John Inoue have deep skills processing VLA data and fitting for rotation curve using sophisticated 3D modeling tools. Additional support on the neutral gas properties of galaxies is provided by Elizabeth Adams, and Evan Skillman. Martha Haynes is one of the co-PIs of the ALFALFA HI survey. John Salzer has led the effort to acquire ground-based imaging and spectroscopy of the SHIELD galaxies; he and Evan Skillman are experts in the analysis and interpretation of emission line spectra from low-mass galaxies. Katherine Rhode is an expert in ground-based observing and has been involved with the acquisiton of the ground-based data for the SHIELD galaxies. Our team has deep expertise in all aspects of the science to be carried out in this program and will deliver results efficiently in a timely manner.Stellar Populations and the Interstellar Medium6falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000GALAXYAMORPHOUS IRREGULARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYAMORPHOUS IRREGULARJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WThe scheduling data was generated by CASM 32.1.CASM was run in Phase II mode.1721583282000259.2762612334232(Tic-Visit
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