0Assigned ID: 813
----- Attempting Submission 1 (Fri Apr 10 20:54:56 GMT 2015) -----
HST Phase I Proposal 813 (phase1_gpsmedium_2015.apt) successfully submitted.
Receipt: # 813-1
----- Attempting Submission 2 (Fri Apr 10 20:56:12 GMT 2015) -----
HST Phase I Proposal 813 (phase1_gpsmedium_2015.apt) successfully submitted.
Receipt: # 813-2
----- Attempting Submission 3 (Fri Apr 10 22:23:23 GMT 2015) -----
HST Phase I Proposal 813 (phase1_gpsmedium_2015.apt) successfully submitted.
Receipt: # 813-3
----- Attempting Submission 4 (Fri Apr 10 23:12:31 GMT 2015) -----
HST Phase I Proposal 813 (phase1_gpsmedium_2015.apt) successfully submitted.
Receipt: # 813-4
----- Attempting Submission 5 (Fri Apr 10 23:32:31 GMT 2015) -----
HST Phase I Proposal 813 (phase1_gpsmedium_2015.apt) successfully submitted.
Receipt: # 813-5COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
INEFFICIENT ORDERING OF FP-POS POSITIONS
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
INEFFICIENT ORDERING OF FP-POS POSITIONS
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details.As requested, I have broken visits up into <4 orbits where possible.
We previously had 9 visits with 4 or 5 orbits. Now, only 4 visits have 4 or 5 orbits.
Due to the long acquisition times required for our faint targets, we significantly reduce our exposure times any time we break up a visit and add an extra acquisition exposure. For 3 targets (4 visits), the resulting S/N estimates are below our requested S/N of 4 in the continuum. We therefore have left these 4 visits unchanged.2017010495----- Attempting Submission 1 (Mon Jul 20 20:26:15 GMT 2015) -----
----- Attempting Submission 2 (Thu Sep 10 17:59:10 GMT 2015) -----Although our sources are compact, some emission may be extended as we discuss in the Phase II proposal. I am in contact with the support staff at STScI to determine the best plan for data reductions.
Some of our visits are 5 orbits long. In these cases, we have specified the FP-POS position by hand for each orbit. Since the first exposure (at FP-POS 1) is the shortest, we return to FP-POS 1 again after going through the other positions. The orbit planner shows no difference in overhead or exposure time for this arrangement relative to the FP-POS ordering 1-2-3-4-3. However, we can easily change to another ordering if preferred. We have also broken up larger visits, and in these cases, we also specify the FP-POS positions manually. Each target uses all 4 FP-POS positions, but 2 may be in one visit and 2 in another.LyC, Ly-alpha, and Low Ions in Green Peas: Diagnostics of Optical Depth, Geometry, and OutflowsThe "Green Peas" are extreme, low-redshift starbursts that are under intense scrutiny as a possible class of Lyman continuum (LyC) emitting galaxies. Their extreme [O III]/[O II] ratios resemble those of z>2 Ly-alpha emitters (LAEs) and suggest conditions conducive to high LyC escape fractions. Our initial COS study of four extreme GPs demonstrated the diagnostic power of Ly-alpha emission plus low-ionization absorption and emission lines to simultaneously relate optical depth, neutral gas geometry, and Ly-alpha radiative transfer. We now propose to test this understanding by confirming these relationships and trends: we will combine these data with new COS spectra of 13 of the most extreme GPs, extending our analysis to a statistically significant sample. One of the targets has the highest [O III]/[O II] ratio in the entire SDSS survey. The combined 17 total spectra of these rare, highly ionized starbursts will provide the first statistics on optical depth and Ly-alpha emission within this key, extraordinary galaxy population. The proposed COS observations will confirm whether galaxies with extreme [O III]/[O II] are indeed often optically thin and will likely lead to revealing the Ly-alpha profiles characteristic of LyC-emitting galaxies. By linking optical depth, outflow geometry, and Ly-alpha profiles, these observations will provide a vital basis for interpreting high-redshift LAE spectra.For our exposure calculations, we follow the same procedure as our existing Cycle 21 observations (GO-13293). In selecting our sample, we chose 13 star-forming galaxies from SDSS with high [O III]/[O II] ratios and reliable spectra. We then selected galaxies whose GALEX FUV magnitudes allow COS spectra with a S/N>4 in the continuum to be obtained in five orbits or fewer. This S/N is comparable to previous C II absorption studies (e.g., Heckman et al. 2011) and existing Green Pea (GP) observations (Jaskot & Oey 2013). We also include the fainter, remarkable starburst J160810 due to its extraordinary [O III]/[O II].
Each COS spectrum will cover Ly-alpha and one or more of the Si II 1260 or C II 1334 doublets. We have confirmed that no Milky Way absorption lines coincide with our wavelengths of interest. The observations will use the primary science aperture, all four FP-POS positions, and the G130M grating. We require the higher resolution G130M grating to separate the closely spaced C II 1334.5,1335.7 lines and resolve the velocity structure of the Ly-alpha, C II, and Si II line profiles. We choose the central wavelength of the grating to capture all the required lines with one setting.
We calculated exposure times for the COS observations with the Spectroscopic Exposure Time Calculator (ETC) using the GALEX FUV magnitudes. In most cases, we adopt a 3 kpc diameter for each galaxy, consistent with the optical HST GP images presented in Cardamone et al. (2009). These estimates are conservative; our existing GP observations show that the NUV-emitting regions are more compact than the full optical extent of the galaxies. The assumed 3 kpc diameters are consistent with SDSS images of the galaxies, most of which are unresolved. In five cases, however, the SDSS images show that the starburst region is more compact than 3 kpc. In these cases, we assume that half of the FUV flux is contained within the SDSS g-band half-light radius. For the lowest redshift object, 1" corresponds to ~0.5 kpc, comparable to the UV half-light radii of our existing high [O III]/[O II] GP observations. We therefore expect the COS aperture to easily encompass the majority of the UV emission from these compact starbursts.
We follow the COS handbook guidelines to determine the buffer times. We first calculate the buffer time with the spectroscopic ETC and multiply by 2/3. For all our targets, this re-scaled buffer time is longer than an individual exposure and longer than 110 seconds. As recommended by the COS handbook, we therefore adopt the ETC buffer time multiplied by 2/3.
The existing COS acquisition images for four extreme GPs show that the brightest NUV emission originates from extremely compact star clusters, with FWHM of ~0.3 kpc. At the redshifts of our targets, this physical scale corresponds to FWHM < 0.6". Nevertheless, given the uncertainty in the targets' geometry and the possible presence of multiple star-forming regions, we have marked the extended flag for the targets.
Since the targets' SDSS coordinates have the required accuracy, we will obtain acquisition images in the ACQ/IMAGE mode with Mirror A. We calculated the acquisition exposure times with the ETC for a S/N of 40 and assuming a point-like source. Since the GPs may be more extended, to be conservative, we assume that this source contains only 10% of the total NUV flux. As we plan to use the NUV imaging to identify the major star-forming regions in the galaxies, we then double the required acquisition exposure times to allow us to detect fainter emission. These exposure times are similar to the acquisition exposures for the existing GP observations.
We use the acquisition imaging ETC to verify that the expected imaging count rates are below the bright object limit. Even if we assume a point source containing 100% of the NUV flux and adopt the brightest NUV magnitude within the GALEX error bars, the acquisition image count rates do not exceed the bright object limit. We have also used the bright object tool and checked the GALEX images to verify that there are no UV-bright objects within a 30" radius of our targets.ISM IN EXTERNAL GALAXIES12falsetruefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 18.0, NUV = 17.8GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 18.2, NUV = 17.8GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 18.7, NUV = 18.6GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 19.2, NUV = 19.1GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 18.7, NUV = 18.4GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 19.3, NUV = 19.6GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 20.0, NUV = 20.0GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 19.5, NUV = 19.5GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 19.9, NUV = 19.8GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 19.8, NUV = 19.7GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 20.2, NUV = 19.7GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 20.0, NUV = 19.9GALAXYDWARF COMPACTSTARBURSTYESWe give the SDSS g-band magnitude in place of the V-magnitude.J2000J2000GALEX FUV = 20.1, NUV = 20.4COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1318COS/FUVSpectroscopicNoNoG130M1327The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode./Users/ajaskot/Documents/OP-cache/hst_phase2_14080_orbitadjust-v01.xml(Tic-Visit
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