0Assigned ID: 762
----- Attempting Submission 1 (Fri Mar 06 20:54:00 GMT 2020) -----
HST Phase I Proposal 762 successfully submitted.
Receipt: # 762-1
----- Attempting Submission 2 (Fri Mar 06 22:24:15 GMT 2020) -----
HST Phase I Proposal 762 successfully submitted.
Receipt: # 762-2
----- Attempting Submission 3 (Fri Mar 06 22:40:46 GMT 2020) -----
HST Phase I Proposal 762 successfully submitted.
Receipt: # 762-3
----- Attempting Submission 4 (Sat Mar 07 00:30:27 GMT 2020) -----
HST Phase I Proposal 762 successfully submitted.
Receipt: # 762-4
----- Attempting Submission 5 (Sat Mar 07 00:34:31 GMT 2020) -----
HST Phase I Proposal 762 successfully submitted.
Receipt: # 762-5FLASH 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
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.We ignore the WFC3 warnings about the post-flash as directed by the recent white paper.-627530344----- Attempting Submission 1 (Tue Jun 30 20:57:35 GMT 2020) -----We ignore the WFC3 warnings about the post-flash as directed by the recent white paper to minimize CTE problems.
We are aware of the caveats of calibration and processing of extended sources using COS.Pox 186: A Case of Complete Neutral Gas Blow-Away?Energetically, it is possible for a starburst in a dwarf galaxy to blow away and completely ionize its ISM, resulting in a very high escape fraction of its ionizing radiation. Finding examples of such galaxies would ease the tension between the energy needed to reionize the universe and the ionizing energy budget available to do so. Pox 186 is an exceptional dwarf galaxy with an active starburst, yet a non-detection in deep 21cm HI observations. Its optical spectrum also shows very highly ionized gas, with an extraordinary [OIII]/[OII] ratio (> 20), and evidence of an 800 km/s outflow. Thus, Pox 186 has many physical properties consistent with those of the Green Pea galaxies - low redshift analogs of the sources responsible for the reionization of the universe. However, Green Peas are dominated by bright star clusters embedded in larger systems many times more massive than the galaxies responsible for reionization. The lower mass of Pox 186 makes it a better match to the high redshift systems. When combined with its close proximity (D~18 Mpc), Pox 186 offers a unique laboratory to study in detail the extreme properties of a galaxy like those responsible for reionization.
We will image Pox 186 with both narrow and broadband filters and obtain a UV COS spectrum with the G160M grating. The imaging will allow us to study the ionization structure to confirm the density bounded nature of the galaxy. The UV spectrum will be used to study the structure of the outflow, the stars driving the outflow, and to directly compare what one could learn from a similar unresolved, high redshift system.This project will use 7 orbits for WFC3+UVIS multiband imaging of Pox 186 distributed over 2 visits. Our exposure times are set to detect the surface brightness emission at a distance of 1".0 from the center with a S/N > 3 per resolution element, using the ETC to verify the S/N for each filters listed exposure times. We will image the target in the F225W, F280N, F336W, F373N, F467M, F487N, F502N, F621M, and F658N filters. For all filters we will use a 3 point dithering pattern to sample the PSF and reduce the effect of cosmic rays. To reduce overhead and minimze CTE effects we use the UVIS2-C1K1C-SUB aperture for imaging in all but F280N, F373N, and F487N, and add a POST-FLASH flux to ensure a minimum charge packet of 20 electrons as recommended by the recent White paper. F280N, F373N, and F487N will use the full field of view (aperture UVIS2-C1K1C-CTE) to maximize the number of field stars that will be used to verify the alignment of the filters across the two visits.
Four orbits are dedicated to obtaining a deep FUV spectra using COS-G160M with CENWAVE=1533. We used COS ETC to estimate the exposure times for spectroscopic observations based on archival STIS observations (PID:8333) and then estimated the required exosure time to reach a S/N of 10 when binning by two resolution elements. The STIS data were also used to estimate the exposure time for obtaining the ACQ/Image using PSA/MirrorA for the recommended S/N = 20. To best remove the fixed pattern noise we cycle through the 4 FP-POS settings over the four orbits. The Bright Object Tool reports a warning about exceeding the local count rate in the ACQ/Image exposure, but there are no objects are present in the 21.5" field around the target in the archival F336W image. Therefore we ignore this warning.Dr. Jaskot, Scarlata, and Skillman are experts with extreme emission line galaxies. They have led multiple HST
programs (e.g., PID 15470, 14134, 13293) and have led and contributed to numerous scientific publications
studying the galaxy properties of extreme emission line galaxies. Dr. Skillman is also an expert in dwarf galaxies, their star-formation histories, metallicites, and gas properties. Dr. Mehta recently completed his PhD on investigating the extreme emission line galaxies, under the supervision of Dr. Scarlata, and has experience with handling HST imaging data as well as its reduction. Nathan Eggen has expertiese with IFU optical data, COS FUV spectra, and he is an expert on Pox 186.Galaxies6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF280NWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF373NWFC3/UVISImagingNoNoF467MWFC3/UVISImagingNoNoF487NWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF621MWFC3/UVISImagingNoNoF658NCOS/FUVSpectroscopicNoNoG160M1533POS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falseC:\Users\Nathan\Desktop\POX\OP-cache\eggen_hst_phase2_v5-v01.xmlThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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