v2 - CO/H2 proposal, Cycle 25 medium GO. Please contact Kevin France (kevin.france@colorado.edu) with problems.
08:20 am MDT, 04/06/17.-1153297143Assigned ID: 108
----- Attempting Submission 1 (Tue Apr 04 18:21:24 GMT 2017) -----
HST Phase I Proposal 108 (COH2_abs_cy25_kf2.apt) successfully submitted.
Receipt: # 108-1
----- Attempting Submission 2 (Thu Apr 06 14:19:53 GMT 2017) -----
HST Phase I Proposal 108 (COH2_abs_cy25_kf2.apt) successfully submitted.
Receipt: # 108-2For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.Cycle 25 CO/H2 in Disks Survey - Kevin France (University of Colroado) - kevin.france@colorado.edu - (303) 492-1429
11/17/17 submission: FP-POS = all added to longer G160M exposure to mitigate fixed pattern and gain sag concerns.
This is the Phase II that can be cut to 51 minutes/orbit for visits 03-04-05 to expand visibility.
11/20/17 submission: added a second FP-POS to all COS G160M observations, per CS request & corrected ETC run number for visits 06 and 07.
01/29/18 submission: corrected typo in target acq in visit 14, exposure 3 (was BOA/MIRRORB, should have been BOA/MIRRORA)
02/27/18 submission: : corrected typo in target acq in visit 12, exposure 1 (was BOA/MIRRORB, should have been BOA/MIRRORA)
03/01/18 submission: moved COS target acq in visit 08 and 09 to BOA/MIRRORA to avoid local rate violation in scaled target template spectrum-1294754288----- Attempting Submission 1 (Wed Jul 12 16:30:01 GMT 2017) -----
----- Attempting Submission 2 (Fri Nov 17 17:52:01 GMT 2017) -----
HST Phase II Proposal 15070 (COH2_abs_cy25_kf6.apt) successfully submitted.
Receipt: # 15070-2
----- Attempting Submission 3 (Tue Nov 21 00:26:34 GMT 2017) -----
HST Phase II Proposal 15070 (COH2_abs_cy25_kf7.apt) successfully submitted.
Receipt: # 15070-3
----- Attempting Submission 4 (Tue Nov 21 14:00:12 GMT 2017) -----
----- Attempting Submission 5 (Mon Jan 29 21:26:42 GMT 2018) -----
HST Phase II Proposal 15070 (COH2_abs_cy25_kf8.apt) successfully submitted.
Receipt: # 15070-5
----- Attempting Submission 6 (Tue Feb 27 23:59:21 GMT 2018) -----
HST Phase II Proposal 15070 (COH2_abs_cy25_kf9.apt) successfully submitted.
Receipt: # 15070-6
----- Attempting Submission 7 (Fri Mar 02 00:25:15 GMT 2018) -----An HST Spectroscopic Study of Protoplanetary Disk Abundances: CO/H2 Conversion Factors and Absolute Abundances for JWSTMeasurements of the masses and physical state of protoplanetary gas disks form the basis for estimating the initial conditions of planet formation. Among the most important constraints derived from disk diagnostics are the abundances and the physical conditions of the most important gas-phase species. Towards this end, we propose to measure absolute molecular abundances of H2, CO, H2O, and OH with HST-COS and STIS to characterize disk composition, molecular excitation temperatures, and spatial (velocity) stratification within the disk environment. These measurements will constrain the CO-to-H2 conversion factor in disks and place upcoming measurements of water and organic molecules with JWST onto an absolute abundance scale. We will achieve this goal by performing three central tasks:
(1) Measure the absorption spectra of primary molecular disk species (H2, CO, H2O, and OH) along the line-of-sight to the central star to obtain a one-dimensional slice through the disk
(2) Use these spectra to measure the column density, excitation temperature, and radial velocity of these species to determine the spatial stratification (or co-spatiality) of the gas parcels
(3) Use this information to characterize the absolute abundances (that is, relative to the H2 column density) of these major molecular species to determine the CO/H2 conversion factor and prepare for upcoming JWST disk observations. We will then characterize the abundance patterns as a function of evolutionary state of the disk and the strength of the local ultraviolet, photodissociating radiation field.The target list (Table 1) includes six disk-hosting young stars with warm CO observed along
the line-of-sight, either: 1) CO fundamental band (4.7 micron) emission profiles display a
broad single component with a central self-reversal, or 2) warm CO in archival HST-COS
spectra, both indicative of a layer of warm molecular gas along the pencil-beam line-of-sight
to the central source, noting that the line-of-sight might be somewhat different between the
M-band and the FUV. We use the same geometry to conduct our molecular gas census, using
the background FUV and NUV continua generated by accretion luminosity and the stellar
photosphere in varying degrees in our sources, depending on the wavelength, the mass of the
central star, and the accretion rate.
We will use a combination of three observing modes,
covering two visits, for each target. H2 and H2O absorption spectra will be obtained with
the COS G130M setting in the first visit, while CO and OH spectra will be obtained in the
COS G160M and STIS NUV modes, respectively. The Herbig A stars are bright enough to
support higher resolution STIS E230M observations in the NUV, and we will employ those
modes where appropriate.
We propose to use the recently commissioned COS G130M 1222 mode to obtain spectra
in the 1065 - 1360 Ang bandpass, as this is the only instrument currently capable of mediumresolution,
high-sensitivity spectroscopy at wavelengths tracing warm H2 and H2O absorption
transitions. The PI of this program was a co-I on the original calibration proposal to develop
the G130M 1222 mode, created the wavelength solutions for this new mode, carried out
some of the first science with this mode, and is intimately familiar with its operation and
performance characteristics. The PI of this program was also the PI of the Cycle 20 Project
WH2IPS (#12876) demonstrating the H2 observational proof-of-concept (France et al. 2014).
We will observe the objects in this program for 3 - 5 G130M 1222 orbits per target, using
all four focal-plane split positions (FP-POS = 1, 2, 3, 4) when possible to mitigate the effects of fixedpattern
noise and detector gain-sag due to long-term exposure of the COS detector. We use
the higher resolution G130M mode instead of the lower-resolution G140L mode because line
profiles and velocity centroids of the individual H2 and CO band structures require velocity
resolution of less than 30 km/s, making the medium resolution modes essential for meeting the
science objectives of this program.
We will observe the v = 1 - 4 bands of the CO (A - X) system with COS G160M,
following the observing strategy of our previous successful programs detecting CO in this
mode (e.g., France et al. 2012; McJunkin et al. 2013). We will observe the objects listed in
here for 1 - 3 G160M orbits per target, using all four focal-plane split positions
(FP-POS = 1, 2, 3, 4) and various cenwave settings to mitigate the effects of fixed-pattern noise.
We will employ the STIS G230M and E230M to observe and characterize the OH (A - X) system, again, the resolution
of the M modes is necessary for a clean resolution of these narrow molecular features. For
T Ori and HK Ori, the NUV source flux permits us to use the STIS E230M 2707 mode for
even higher resolution (R 30,000) observations of the OH spectral region. The proposal
team was involved with the development and testing of custom software routines for coadding
CTTS spectra obtained in various central wavelength and FP-POS configurations
with COS, and we will leverage this experience to produce high-quality spectral data products
for analysis in this project.Planets and Planet FormationStellar Physics0falsefalsetruefalsetruefalsefalseSUPPORTEDEXT-STARDISKPRE-MAIN SEQUENCE STARPROTOPLANETARY DISKT TAURI STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARDISKPROTOPLANETARY DISKT TAURI STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARDISKPROTOPLANETARY DISKT TAURI STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARDISKHERBIG AE/BEPROTOPLANETARY DISKNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARDISKHERBIG AE/BET TAURI STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARDISKHERBIG AE/BEPROTOPLANETARY DISKNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1600COS/NUVSpectroscopicNoNoG230L3000COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1600COS/NUVSpectroscopicNoNoG230L3000COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1600COS/NUVSpectroscopicNoNoG230L3000COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1600STIS/NUV-MAMASpectroscopicNoNoG230M3055COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1600STIS/NUV-MAMASpectroscopicNoNoE230M2707COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1600STIS/NUV-MAMASpectroscopicNoNoE230M2707Timing link suitability includes constraints ([02 After 01 by at most 2.0 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.154933161200082.81274120163982(Tic-Visit
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Revised to take average IUE flux from 1982 - 1989,with PSA/MIRRORB per instruction of contact scientist - kf - 10/22/12Revised to take average IUE flux from 1982 - 1989,with PSA/MIRRORB per instruction of contact scientist - kf - 10/22/12Timing link suitability includes constraints ([02 After 01 by at most 2.0 days])The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.BOT checked, kf, 06/29/12. The only violation is a mis-typing of the target star, which has been observed safely with COS.154942312900082.81327697151869(Tic-Visit
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Revised to take average IUE flux from 1982 - 1989,with PSA/MIRRORB per instruction of contact scientist - kf - 10/22/12Revised to take average IUE flux from 1982 - 1989,with PSA/MIRRORB per instruction of contact scientist - kf - 10/22/12Timing link suitability includes constraints ([04 After 03 by at most 3.0 days] [05 After 03 by at most 3.0 days])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.1513357338000124.28966564700107(Tic-Visit
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