0Assigned ID: 1056
----- Attempting Submission 1 (Fri Apr 10 23:38:32 GMT 2015) -----
HST Phase I Proposal 1056 (improposal.apt) successfully submitted.
Receipt: # 1056-3
----- Attempting Submission 4 (Fri Apr 10 23:50:08 GMT 2015) -----
HST Phase I Proposal 1056 (improposal.apt) successfully submitted.
Receipt: # 1056-2
----- Attempting Submission 5 (Fri Apr 10 23:54:51 GMT 2015) -----
HST Phase I Proposal 1056 (improposal.apt) successfully submitted.
Receipt: # 1056-3POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.This resubmission:
We have made small changes to visits 7-10 (all are WFC3/UVIS):
Visit 9: Exposure times were made longer for F547M at the expense of F438W to achieve
comparable S/N in both filters. Post-flash values were changed accordingly.
Visits 7-10: We choose the smaller aperture UVIS2-C1K1C-SUB instead of UVIS2 to minimize
the overheads, as our targets are compact. We changed the exposure times (~50s per
exposure) and post-flash values accordingly.
Previous resubmission:
We have made changes to UVIS filters, and to post-flash values - both approved by
Program Coordinator and Program Scientist.-594004814----- Attempting Submission 1 (Thu Jul 23 22:55:36 GMT 2015) -----
----- Attempting Submission 2 (Thu Oct 29 00:22:48 GMT 2015) -----
----- Attempting Submission 3 (Thu Jan 21 23:14:44 GMT 2016) -----I obtain warnings about careful use of POS-TARG in ACS ramp filters. We use small steps.Origin of double peaks in Lyman-alpha spectra: diffuse halos or Lyman continuum leakage?The Lyman-alpha (Lya) line of hydrogen is a tool of prominent cosmological importance. Most of the observed spectra show P-Cygni profiles, but a fraction of them are double-peaked, interpreted as radiative transfer effects in static media in the realm of the common expanding shell models. However, several studies indicate that this interpretation is inconsistent with ancillary data. We propose a new theoretical scheme for the origin of 2 types of double peaks: 1) Our simulations show that double peaks arise in Lya "halos", i.e. diffuse Lya emission in circum-galactic gas. 2) We predict that no Lya halos are expected at galaxies with escaping Lyman continuum (LyC), and in this case narrow Lya double peaks result from radiative transfer in low column density of neutral hydrogen. We propose testing these two schemes on Green Peas, a class of local, compact, low-mass, low-metallicity galaxies, which comprise some of the strongest candidates for LyC escape. Most of their HST/COS Lya spectra are double-peaked, carrying the signal from the entire galaxy and its Lya halo, thanks to the target compactness. We have selected 4 targets with very different Lya spectra: narrow and broad, strong and weak double-peaks, and one single-peak spectrum. We will image them in Lya, FUV continuum and H-alpha. We expect detecting 2 large halos (plus one available in the archive), while the other 2 targets are probable LyC leakers. We will search for connections between spatial Lya properties (halo extent, surface brightness profile, flux concentration) and spectral Lya signatures (peak separation, blue peak strength). Our results will have impact on Lya data interpretation both at low and high redshift.This program will image 4 compact dwarf galaxies with two ACS/SBC filters to synthesize a Lya bandpass (F140LP and F150LP - 2 orbits per target for z<0.2, or F150LP and F165LP - 4 orbits per target for z>0.2), with two WFC3/UVIS filters (F390W and F475W, 1 orbit per target), and with ACS/WFC (F850LP and ramp filters FR872N or FR853N, 1 orbit per target). This amounts to 18 orbits.
All SBC visits are kept to 2 orbits to prevent heatup of the detector and the associated increase in dark current. All SBC visits are safe with respect to the bright object limit. We have indicated ETC run numbers for the brightest (in FUV flux) target in all filters used, hence this is conservative and deemed safe by the BOT tool.
All SBC visits should be scheduled so that the SBC HAS NOT BEEN IN USE FOR THE PAST 24 hours to minimize the dark current.
All SBC visits use 4 dither positions per filter to improve photometric accuracy and to mitigate the effect of the detector stripe.
The WFC3/UVIS visits, 1 orbit per target, filters F390W and F475W, utilise a 3 point dither to step over droplets.
ACS/WFC is used for ramp filter imaging and F850LP, utilising SMALL pos-targs.ISM IN EXTERNAL GALAXIES12falsetruefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTThis object was generated by the targetselector and retrieved from the NED database.J2000J2000FUV = 19.3 mag ABGALAXYDWARF COMPACTSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV = 20.2 mag ABGALAXYDWARF COMPACTSTARBURSTThis object was generated by the targetselector and retrieved from the NED database.J2000J2000FUV = 19.6 mag ABGALAXYDWARF COMPACTSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV = 19.3 mag ABACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/WFCImagingNoNoF850LPACS/WFCRampFilterNoNoFR782NWFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF475WACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/WFCImagingNoNoF850LPACS/WFCRampFilterNoNoFR782NWFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF475WACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPACS/WFCImagingNoNoF850LPACS/WFCRampFilterNoNoFR853NWFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF475WACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/WFCImagingNoNoF850LPACS/WFCRampFilterNoNoFR782NWFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF475WThe scheduling data was generated by CASM 23.2.CASM was run in Phase II mode./private/var/folders/ny/y2rfgxpn4k37g754z2ph3gd00001bc/T/OPVisit5070587500479532537.xmlWe request that the SBC not be used 24 hours before this visit in order to mitigate the effects of dark current.(Tic-Visit
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