0Assigned ID: 875
----- Attempting Submission 1 (Fri Apr 08 21:39:21 GMT 2016) -----
HST Phase I Proposal 875 (HST_UVprop_C24.apt) successfully submitted.
Receipt: # 875-1For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
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.
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.
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.
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.
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.
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.
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.We changed one target of the original sample, as discussed with CS Paule Sonnentrucker
and approved by COS Team User Support Lead Andrew Fox.
We selected two central wavelength positions and two FP-POS positions.
We are using all 4 FP-POS positions, just split over 2 CENWAVES to get full spectral coverage in the G160M bandpass.
We resubmitted with target acquisition changed from MIRRORA to MIRRORB for target 04, as requested by CS P. Sonnentrucker.
Updated proper motions based on available GAIA data, on Jan 02 2017
Updated NUV imput spectra614242342----- Attempting Submission 1 (Mon Jul 18 18:50:37 GMT 2016) -----
HST Phase II Proposal 14703 (HST_UVprop_C24.apt) successfully submitted.
Receipt: # 14703-1
----- Attempting Submission 2 (Fri Dec 30 00:02:32 GMT 2016) -----
HST Phase II Proposal 14703 (HST_UVprop_C24.apt) successfully submitted.
Receipt: # 14703-2
----- Attempting Submission 3 (Mon Jan 02 17:47:09 GMT 2017) -----
HST Phase II Proposal 14703 (HST_UVprop_C24.apt) successfully submitted.
Receipt: # 14703-3
----- Attempting Submission 4 (Mon Jan 02 21:02:55 GMT 2017) -----
HST Phase II Proposal 14703 (HST_UVprop_C24.apt) successfully submitted.
Receipt: # 14703-4
----- Attempting Submission 5 (Tue Jan 03 01:07:54 GMT 2017) -----
HST Phase II Proposal 14703 (HST_UVprop_C24.apt) successfully submitted.
Receipt: # 14703-5
----- Attempting Submission 6 (Tue Jan 03 18:25:09 GMT 2017) -----We selected two central wavelength positions and two FP-POS positions.
We are using all 4 FP-POS positions, just split over 2 CENWAVES to get full spectral coverage in the G160M bandpass.Measuring residual H2 gas from small to large gaps in protoplanetary disks: different pathways to planets?We propose HST-COS far-ultraviolet (FUV) spectra of H_2 gas emission in a representative sample of 8 "transitional" disks around young stars of ~1-2 solar masses. By targeting 0.3-5 au disk gaps revealed from the analysis of infrared (IR) CO emission spectra, the proposed HST observations will allow us to measure the density of residual molecular gas from the onset of the smallest disk gaps to the development of large gaps that can be directly imaged. The sensitive measurements of H_2 residual gas vs disk gap size obtained in this program will constrain gap-formation processes and reveal if all gap sizes belong to a common, sequential evolutionary path or to different paths that affect the orbital distribution and composition of forming planets. This is essential to validate and improve current theories of planet formation in dispersing disks, extending observations to small disk radii well beyond the angular resolution limits of current imaging techniques. This program takes immediate advantage of recent results finding new gas emission tracers of disk evolution in the UV (Hoadley, France, et al. 2015) and in the IR (Banzatti & Pontoppidan 2015), and joins them together into a new, panchromatic view of gas dispersal in planet-forming regions.Our observing strategy is driven by the need to acquire high-sensitivity, moderate spectral resolution coverage at the wavelengths spanned by strongest lines of the H2 fluorescent cascade that follows Ly_alpha photoexcitation (1390-1700 Angstrom). Spectral coverage with sufficient sensitivity and spectral resolution in this range is best provided by the M-mode settings on HST-COS. COS has the highest sensitivity for spectrally resolved observations at these FUV wavelengths (more than a factor of ten more efficient than STIS E140M at these wavelengths due to the combination of larger effective area and lower background). In the G160M bandpass, there are a wealth of H2 emission lines spread throughout (e.g., France et al. 2012) and the COS medium resolution modes have proven optimal for modeling the column densities, temperatures, and radial flux distributions from these lines with a largely enough accuracy to distinguish well between the gap-formation scenarios described in the approved Phase I proposal.
To summarize, we will use the G160M grating with multiple FP-POS settings and CENWAVE = 1577 and 1611 to simultaneously provide continuous spectral coverage, mitigate the effects of detector fixed pattern noise, and support the extended lifetime of the COS MCP detector. These modes will provide high S/N spectra of our targets across the full 1390 - 1780 Angstrom bandpass.Extrasolar Planets and Planet Formation12falsetruefalsefalsefalsefalseSUPPORTEDSTARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000STARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARPRE-MAIN SEQUENCE STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode./private/var/folders/d7/y7rsy4gx4tb9k78twmqmdmsr0000gt/T/OPVisit3922694667780471149.xml(Tic-Visit
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