0 Assigned ID: 929 ----- Attempting Submission 1 (Fri Apr 11 22:09:53 GMT 2014) ----- HST Phase I Proposal 929 (HSTIPMLyC14.apt) successfully submitted. ----- Attempting Submission 2 (Fri Apr 11 23:48:11 GMT 2014) ----- HST Phase I Proposal 929 (HSTIPMLyC14.apt) successfully submitted. 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. There seems to be a bright star near Target 2, please check. Our targets are only a few arcsec in diameter, so the warnings about bandpass variations should not be a cnocern. We changed a couple of the continuum-band observations from 2 exposures to 3 exposures to allow for cleaner data reduction. We are able to do this with no degradation in S/N. --- Aug 19, 2014: Changed ACS MRAMPQ aperture readouts to full-frame MRAMP readouts as per Marco's email. --- Oct 7, 2014: Added FLASH = 12 e/px to all WFC3 exposures as per Sylvia's email. Also changed all non-quad filter apertures to quadrant B, as per her advice. --- Jan 21, 2015: Added ORIENT restrictions to Visits 4 and 5 as per Marco and Miranda's emails. This is to avoid diffraction spikes from nearby bright star in Tol 1247 field using ACS. -255510351 ----- Attempting Submission 1 (Tue Jul 22 17:09:48 GMT 2014) ----- HST Phase II Proposal 13702 (Oey_GO13702_PhaseII.apt) successfully submitted. ----- Attempting Submission 2 (Tue Aug 19 17:46:59 GMT 2014) ----- ----- Attempting Submission 3 (Tue Oct 07 20:55:15 GMT 2014) ----- HST Phase II Proposal 13702 (Oey_GO13702_PhaseII_2.apt) successfully submitted. ----- Attempting Submission 4 (Wed Jan 21 19:34:29 GMT 2015) ----- Our targets are only a few arcsec in diameter, so the warnings about bandpass variations should not be a concern -- unless we need to adjust the pointing. Please see comments. Mapping the LyC-Emitting Regions of Local Galaxies We propose to map the optically thin regions in the only two, known Lyman-continuum (LyC) emitting galaxies in the local universe, Haro 11 and Tol 1247-232. This will be done with the recently developed technique of ionization-parameter mapping (IPM), based on nebular emission-line imaging. We will use ACS/WFC and WFC3/UVIS to carry out narrow-band imaging in [O II] and [O III], as well as nearby continuum, where necessary. Together with existing data, our results will clarify the conditions for LyC emission and will yield more realistic estimates of the escape fraction of LyC radiation from these galaxies. We plan to carry out ionization-parameter mapping with narrow-band imaging in [Oiii] 4959,5007 and [Oii] 3727 for Haro 11 and Tol 1247-232. We will also require continuum imaging to generate continuum-subtracted, emission-line images. Haro 11 and Tol 1247-232 are redshifted to z = 0.0206 and 0.0480, respectively. The ACS ramp filters will allow us to tune the bandpasses to the necessary redshifted emission-line wavelengths, which is necessary for Tol 1247-232. Haro 11 is also accessible with WFC3 narrow-band filters, so we choose the instruments according to sensitivity. For the ACS ramp filters, FR505N is used for [Oiii] imaging, and its 2% bandpass corresponds to a width of about 100 A. This allows obtaining both [Oiii] 4959,5007 simultaneously, while centering the bandpass to avoid H-beta 4861. We will use FR388N for [Oii] imaging of Tol 1247-232, and its 2% bandpass corresponds to about 78 A width. The nearest bright emission line is [Ne iii] 3869, which is too far to be a contamination concern. For Haro 11, we use WFC3/UVIS FQ378N, which similarly excludes [Ne iii]. The angular sizes of the target galaxies are only a few arcsec, so they will easily fit within the ramp filter monochromatic regions on the order of 30 arcsec diameter, which correspond to one ACS quadrant. We will therefore only require readout of the WFC1-MRAMPQ quadrant on ACS. Haro 11 similarly fits easily within a WFC/UVIS quadrant, as necessary for using the FQ378N quadrant filter. We can estimate our exposure times by scaling directly from the existing HST H-alpha observations. Haro 11 was observed by ACS/WFC FR656N for 680 s. We need to obtain a S/N = 10 in the outer, low surface-brightness regions in each of [Oii] and [Oiii]. This corresponds to surface brightness of about 5 x 10^-15 erg s^-1 cm^-2 arcsec^-2 , according to the ACS Ramp Filter ETC. For Haro 11, the measured reddening in Knot C implies that we need an additional factor of 1.2 in depth at [Oiii] relative to H-alpha (James et al. 2013). We can obtain the corresponding depth in 3 x 800 s in FR505N centered at 5110 A (1 ACS orbit). We compared with the WFC3/UVIS F508N, but find that ACS FR505N is more efficient. For [Oii] at 3803|A, however, WFC3 FQ378N is much more efficient than ACS FR388N. At [Oii], the aggregate reddening implies a factor of 1.5 deeper exposures than at H-alpha. Since we expect the reddening to be much lower in the outer, low surface-brightness regions, we aim for a factor of 1.3 deeper than the existing H-alpha data, since the sensitivity is so much worse at this wavelength. The corresponding depth can be achieved with 6 x 1200 s in WFC3 FQ378N (3 WFC3 orbits). The redshift of Tol 1247-232 requires using the ACS ramp filters. It turns out that this galaxy has the same reddening as Haro 11, Knot C (c(H-beta)=0.3; Terlevich et al. 1993), and so we request the same depth observations as for Haro 11 in both bands. For [Oiii], we again use ACS filter FR505N, now centered at 5247 A, with the same 2400-s exposure time (1 ACS orbit). For [Oii], we observe with FR388N for an exposure time of 10 x 1200 s, centered at 3906 A (5 ACS orbits). Thus, our emission-line observations require a total of 7 ACS orbits and 3 WFC3 orbits. We will need continuum observations that are uncontaminated by line emission to obtain the best continuum subtraction for our targeted emission-line observations. Note that we also plan to make use of the existing H-alpha observations, so we need to ensure that we will have continuum observations for these, too. There are sufficient existing HST continuum observations for Haro 11 in [Oiii]: 471 s in ACS/WFC F550M, which the ACS ETC shows is perfectly matched to the depth of our total proposed [Oiii] observations in FR505N. There is also a 600-s exposure in F775W by WFC3 for Tol 1247-232, which serves as continuum for H-alpha. The remaining bands will need either new or supplementary observations. The [Oii] continuum observations need to be obtained with the more blue-sensitive WFC3, since there is no U filter on ACS. We therefore propose to obtain all the other continuum data with this instrument. For Haro 11, the existing ACS/HRC F330W data are only 1/3 as deep as we require, and so we propose to obtain about 600 s x 2 with WFC3/UVIS in F336W. There are no suitable H-alpha continuum data for this galaxy, so we also will obtain about 300 s x 2 in F763M. For Tololo 1247-232, there is no available [Oiii] continuum, so we plan to obtain 300 s x 3 in F547M. The existing F336W data are also about 25% shallower than the depth needed, so we include an additional 900-s frame to supplement this. Thus we request 1 orbit for each galaxy using WFC3 to obtain continuum data. All multiple observations will be dithered. Our request totals 7 ACS orbits and 5 WFC3 orbits. ISM IN EXTERNAL GALAXIES Default false false false false false SUPPORTED GALAXY DWARF COMPACT STARBURST This object was generated by the targetselector and retrieved from the NED database. Data confirmed and updated. Surface brightness represents desired depth for diffuse outer regions. ESO-350-IG-038 J2000 J2000 5e-15 erg s-1 cm-2 arcsec-2 GALAXY DWARF COMPACT STARBURST This object was generated by the targetselector and retrieved from the NED database. Data confirmed and updated. Surface brightness represents desired depth for diffuse outer regions. J2000 J2000 5e-15 erg s-1 cm-2 arcsec-2 ACS/WFC RampFilter No No FR505N WFC3/UVIS Imaging No No FQ378N WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F763M ACS/WFC RampFilter No No FR388N ACS/WFC RampFilter No No FR505N WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F547M POS-TARG DITHER 3.011 LINE false false 2 85.28 ACS-WFC-DITHER-LINE 1 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 3 false POS-TARG DITHER 0.265 LINE 0.187 false false 69.05 4 20.67 ACS-WFC-DITHER-BOX 4 false POS-TARG DITHER 3.011 LINE false false 3 85.28 ACS-WFC-DITHER-LINE 5 false /Volumes/Ontario2/msoey/scitex/props/HSTipmlyc14/OP-cache/Oey_GO13702_PhaseII_2-v01.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 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