0Assigned ID: 75
----- Attempting Submission 1 (Tue Apr 02 03:54:50 GMT 2019) -----
HST Phase I Proposal 75 (vandokkum_df2.apt) successfully submitted.
Receipt: # 75-1
----- Attempting Submission 2 (Tue Apr 02 03:59:42 GMT 2019) -----The goal is to have 3 epochs, but still have a lot of scheduling flexibility.
Currently a visit is only 2 orbits, but 6 (7 for epoch 2) visits have to be scheduled within 5 (or 6, for epoch 2) days of each other (constituting a single epoch).
Then there are two 30-60 day windows: between the first visit of epoch 1 and the first visit of epoch 2, and between the first visit of
epoch 2 and the first visit of epoch 3.
If this leads to scheduling difficulties let me know and I can adjust! The 5 day window can be extended a bit, for instance.526129556----- Attempting Submission 1 (Sun Jul 28 11:22:21 GMT 2019) -----Deep imaging and a TRGB distance for the dark matter deficient galaxy NGC1052-DF2The galaxy NGC1052-DF2 has been the topic of intense debate since it was announced in March 2018, with 33 papers having been written on it in the past twelve months. It appears to have an unprecedented population of luminous globular clusters and an unprecedented low dark matter fraction. The interpretation is critically dependent on its distance. Initial studies found a distance of 19 Mpc from surface brightness fluctuations, but it has been suggested that the galaxy could be significantly closer. Almost all its properties are distance-dependent, and for D~13 Mpc it is not particularly unusual. This proposal requests deep HST imaging to unambiguously measure the distance to NGC1052-DF2 from the tip of the red giant branch (TRGB). With 20+20 orbits (19+19 requested and 1+1 existing) of F814W+F606W imaging the TRGB can be reliably detected out to D~20 Mpc, providing a distance with an uncertainty of ~5%. Additional science goals include a measurement of the morphology of the galaxy at large radii from star counts, an investigation of tidal streams that may be associated with the bright globular clusters, and a search for distant globular clusters in parallel UVIS fields.NGC1052-DF2 will be observed with ACS in F606W and F814W, with 19 orbits in each band.
The program is split in 19 2-orbit visits. Each visit has 1 orbit F814W and 1 orbit F606W.
The observations have no ORIENT constraints but are split in three epochs, to identify variable stars on the AGB.
Epoch 1 has visits 1-6; epoch 2 has visit 7-13; and epoch 3 has visits 14-19.
The first visit (visit 1) has no scheduling constraints. All visits in each epoch are scheduled to be executed within 5 days of each other. The first visit of the second epoch (visit 7) is scheduled to be executed within 30-60 days of the first visit of the first epoch. The first visit of the third epoch (visit 14) is scheduled to be executed within 30-60 days of the first visit of the second epoch.
Within each orbit, 4 exposures are taken in a 4-point dither pattern to remove cosmic rays, identify hot pixels, and dither over the chip gap. Furthermore, each visit has a POS_TARG so that the chip edge is not always in the same location, and also avoids the center of the galaxy. The POS_TARGs for visits 1-6 are 0,10; 0,13; 0,16; 0,-10; 0,-13; and 0,-16 (all in arcsec with respect to the WFCENTER aperture). These POS_TARGs repeat for the other epochs, as the chip gap will be in a different location due to the different ORIENTs of those epochs.
Due to the combination of POS_TARGs and timing constraints the chip gap will be dithered around the frame, yielding uniform coverage with the galaxy in the middle of the final, combined frame.Pieter van Dokkum wrote the initial papers on this galaxy, on the globular cluster population and the dark matter content, as well as a paper on the CMD of NGC1052-DF2 in the currently available HST data. He has extensive experience reducing and analyzing HST data. Charlie Conroy is an expert on stellar populations and developed the models that are used in the paper to predict what the CMDs will look like for different distances. Shany Danieli has experience measuring the TRGB in nearby galaxies (Danieli et al. 2017). The tool that is used to generate images from these models was developed by Shany Danieli. Jean Brodie, Aaron Romanowsky, and Diederik Kruijssen are experts on globular clusters. Roberto Abraham is an expert in the general area of galaxy formation Dhruba Dutta Chowdhury analyzed the dynamical evolution of the DF2 globular cluster system.Galaxies and the IGMCosmology6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF SPHEROIDALJ2000J2000ACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WPOS-TARGDITHERDITHER23.034Large dither over gap and then small dither to reject hot pixels and cosmic rays
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