0Assigned ID: 392
----- Attempting Submission 1 (Fri Mar 06 04:14:20 GMT 2020) -----
HST Phase I Proposal 392 successfully submitted.
Receipt: # 392-1
----- Attempting Submission 2 (Fri Mar 06 23:08:47 GMT 2020) -----
HST Phase I Proposal 392 successfully submitted.
Receipt: # 392-2
----- Attempting Submission 3 (Fri Mar 06 23:31:36 GMT 2020) -----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 browser0----- Attempting Submission 1 (Fri Jun 19 18:01:58 GMT 2020) -----The warning seem to arise from the fact that APT expects post-flashes based on the old 12 e-/pix level, whereas these are set to conform with the new 20 e-/pix level.Extinction Mapping in Leo P: Resolving the Dust Properties of the Lowest-Metallicity ISM in the Local UniverseLeo P is the closest extremely metal poor galaxy that is still forming stars - only 1.62 Mpc away, with a metallicity of only 0.03 Zsol. This makes it a unique object, able to provide insights onto the ISM at these extreme metallicities, and acting as a local laboratory for understanding primitive systems at high redshift. We propose using 6 orbits of HST imaging to obtain observations of Leo P in 4 UV-NIR filters. This data will enable us to perform panchromatic extinction mapping in Leo P - fitting the multiwavelength SEDs of its stars, and modelling the dust along the line-of-sight to each. We will thereby produce a resolved map of the dust extinction in Leo P - the first ever map of the cold star-forming ISM in an extremely metal poor galaxy. This dust map will tell us the amount, location, and properties, of the dust in Leo P - providing invaluable constraints on how the ISM evolves at the lowest metallicities, and supporting the calibration of metallicity corrections for primitive systems at high redshift.Our proposal is to observe the extremely metal poor nearby (1.62 Mpc) dwarf galaxy Leo P in four filters: F275W, F336W, F110W, and F160W. We will be observed the resolved stellar populations in Leo P, aiming to maximise the numbers of stars detected in all four bands. The integration times for each band are distributed accordingly. (Our observations will be used in conjunction with deep archival F475W and F814W data in our analysis.)
In F275W, we plan to conduct 3 orbits of exposures. These 3 exposures will be arranged in a WFC3-UVIS 3-point dither line. These observations should allow 5-sigma detection of stars down to 25.75 vegamag.
In F336W, we plan to conduct 1.6 orbits of exposure; one exposure lasting a full orbit, and a second orbit that will be partialy spent performing a further F336W exposure (followed by our F110W exposures). The two F336 exposures will be arranged in a WFC3-UVIS 2-point dither line. These observations should allow 5-sigma detection of stars down to 26.14 vegamag.
In F110W, we plan to conduct 0.4 orbits of exposures (~16 mins), performed during the same orbit as the second F336W exposure descrirbed above. The two F110W exposures will be arranged in a WFC3-IR 2-point dither line. These observations should allow 5-sigma detection of stars down to 26.05 vegamag.
In F160W, we plan to perform 1 orbit of exposures. Thsee two F160W exposures will be arranged in a WFC3-IR 2-point dither line. These observations should allow 5-sigma detection of stars down to 25.55 vegamag.The PI, Christopher Clark, is an expert in studying the resolved properties of the ISM in the local Universe, especially dust, through multiwavelength tracers. His publications feature work on mapping the physical properties of dust within nearby galaxies, on how the UV attenuation properties of dust vary in galaxies at earlier evolutionary stages, and on the contributions of evolved stars to the Galaxy's dust budget.
The team's co-investigators include specialists in resolved stellar population studies of nearby galaxies (M. Boyer, Y. Choi, K. Gilbert, K. Gordon, L. Hagen, K. McQuinn, C. Murray, B. Williams), many of whom have been leaders in prominent HST programs in the field, such as PHAT (PID 12055), LUVIT (PID 15275), Scylla (PID 15891), METAL (PID 14675), METAL-Z (PID 15880), and SMIDGE (PID 13659). Team members C. Clark, M. Boyer, S. Goldman, K. Gordon, L. Hagen, and J. Roman-Duval have all published studies on the origins of dust and its evolution in the ISM. Team members K. McQuinn, M. Boyer, and S. Goldman are foremost experts on Leo P, heaving led previous HST projects observing it in the optical and NIR. Team members J. Roman-Duval and L. Hagen have a particular background in using UV absorption to understand the dust and ISM properties of local galaxies. Also, many of the team are contributors to the BEAST software which will be central to our analysis (C. Choi, C. Clark, M. Boyer, S. Goldman, L. Hagen, K. Gordon, C. Murray, B. Williams).Stellar Populations and the Interstellar Medium6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYLSBYESJ2000J2000WFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF336WWFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF160WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falseThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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)false30According to the HST ETC (Request ID: WFC3UVIS.im.1447512), each of the exposures in this pattern should have 10 e- pixel due to background, so the post-flash of 10 e- should bring this up to the requested 20 e-.The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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)true20Becuase this exposure is long enough to exceed the old 12 e- per pixel due to background CTE threshold, the HST ETC does not give the background e- value for it. However, extrapolating from our other F336W exposure, which is a factor of 1.73 shorter and had background of 7 e-, this exposure should have 13 e- pixel due to background so the post-flash of 7 e- should bring this up to the requested 20 e-.According to the HST ETC (Request ID: WFC3UVIS.im.1447515 ), this exposure should have 7.1 e- pixel due to background, so the post-flash of 13 e- should bring this up to the requested 20 e-.The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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