0Assigned ID: 106
----- Attempting Submission 1 (Tue Apr 04 18:14:57 GMT 2017) -----
HST Phase I Proposal 106 (TCha_Cyc25v1.apt) successfully submitted.
Receipt: # 106-1
----- Attempting Submission 2 (Thu Apr 06 22:38:25 GMT 2017) -----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.
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.
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.Previous 5 orbit visits converted to 4 COS + 1 STIS visits.
All 4 FP-POS positions now used for G160M 1600 and G140L with a roughly 6 minute loss in
exposure time sustained.
STIS ACQ reduced to 0.1 sec exposure.
Minoe changes to proper motions.
STILL USE ONLY FP-POS=4 FOR G130M 1291 BECAUSE WE NEED TO OBSERVE THE 1281-1220 A
REGION ON THE WING OF H LYMAN-ALPHA.778651916----- Attempting Submission 1 (Wed Jul 19 18:18:41 GMT 2017) -----
HST Phase II Proposal 15128 (TCha_15128-PhaseII-v3.apt) successfully submitted.
Receipt: # 15128-1
----- Attempting Submission 2 (Thu Aug 03 19:49:51 GMT 2017) -----As discussed in the Observing Description, for G130M setting 1291 only FP-POS=4 is used to provide
observations of the red wing of H Lyman alpha (1218-1220A) where we hope to detected molecular hydrogen
absorption lines. For other gratings/settings we use all four FP-POS values.Inner Disk Structure and Transport Mechanisms in the Transitional Disk around T ChaTo better understand how Earth-like planets form around low-mass stars, we propose to study the UV (HST), X-ray (XMM), and optical (LCOGT) variability of the young star T Cha. This variability is caused by obscuration of the star by clumpy material in the rim of its inner disk. Changing sight lines through the disk allow measurement of the temperature and column density of both molecular and atomic gas and the physical properties of the dust grains in the well-mixed inner disk, as well as determining the gas-to-dust ratio. The gas-to-dust ratio affects planetesimal growth and disk stability but is difficult to measure in local regions of disks. Three 5 orbit visits, separated by 3-7 days, are required for use of analysis techniques comprising both differential "pair-method" comparison of spectra with differing A_v (particularly important for determining the dust extinction curve, A_lambda, where removal of the foreground extinction requires multiple epochs) and detailed spectral fitting of gas absorption features at each epoch. The inner disk of T Cha is particularly interesting, because T Cha has a transitional disk with a large gap at 0.2-15 AU in the dust disk and allows study of the gas and dust structure in the terrestrial planet formation zone during this important rapid phase of protoplanetary disk evolution. Characterizing the high energy (UV/X-ray) radiation field is also essential for in-depth studies of the disk in other spectral regions. Results from these observations will have wide relevance to the modeling and understanding of protoplanetary disk structure and evolution, and the complex gas and dust physics and chemistry in disk surface layers.TARGET:
T Cha is a 1.5 solar-mass T Tauri star with a K0 spectral type. It is associated with the Epsilon Cha moving group at a distance of ~100 pc and has an age of ~7 Myr. The H Balmer alpha line profile varies strongly from pure emission to inverse P Cygni on a timescale of one day or less (Alcala et al. 1993, A&A, 272, 225). The extinction towards the star varies by 3 magnitudes in the V band. This variability is not periodic nor predictable, but occurs on short timescales and is seen in all studies over the last 25 years (1992-1995: Schisano et al. 2009, A&A, 501, 1013; 2000-2009: Percy et al. 2010, JAAVSO, 38,1 ; 2015: our work). Schisano et al. (2009) analyzed the optical variability of T Cha and concluded that the changes are due to clumps in the inner disk in our line-of-sight to the central star. The position and proper motions of T Cha are well determined by Hipparcos and Gaia. ETC feasibility calcuations were performed for a variety of light levels, typically for maximum light (V=11.3, A_V=1.3) and for 1 and 2 magnitudes of additional A_V. ETC calculations used the UV/optical spectrum of a very similar proxy target (GM Aur) scaled appropriately for magnitude difference and appropriate amounts of circumstellar and interstellar/cloud absorption. Scisano et al showed that the circumstellar absorption has R_V=5.5.
We expect the target to be unpredictably variable with decreases in flux throughout the UV and optical on timescales of days certainly and probably measurably on timescales of a few hours.
OBSERVING STRATEGY:
We shall use three 5 orbit visits (constructed as a 4 orbit COS visit immediately followed by a 1 orbit STIS visit) to obtain medium resolution (R~18,000) FUV spectra of T Cha using the COS G160M+G130M gratings (covering 1150-1770 A ). The three visits are to be separted by 3-7 days. G130M will be used with the 1291 setting and G160M with the 1577 and 1600 settings. These spectra will record the UV transition region and chromospheric emission line spectrum of the central star, sampling a wide range of elements and ionization states -- e.g. strong lines of H I, C I-IV, O III-IV, Si I-IV, N V, He II (plus Mg II and Fe II from STIS G230L) --- and also the strong molecular hydrogen (H_2) and CO emission produced by H Lyman alpha fluorescent excitation of warm molecular gas on the surface of the proto-planetary disk. The G130M 1291 FP-POS=4 setting is used exclusively so that as much as possible of the red wing of H Lyman alpha is recorded -- we will measure changes in circumstellar H_2 absorptions on the red wing of this emission line in the 1218-1220 A region. The COS observations end with G140L exposures that will record the full FUV spectrum at the same time; thereby allowing better linkage to the STIS low resolution spectra.
In the final orbit of each visit we shall obtain low resolution (R~500) STIS spectra using the MAMA G230L (1570-3180 A) and CCD G430L (2900-5700 A) + G750L (5399-10000 A) gratings that will allow us to measure the variable level and shape of the dust extinction (A_lambda) throughout the FUV, NUV and far into the optical. It is vital that the STIS and COS spectra be obtained in adjacent orbits. A separate orbit is needed for the STIS observations because a significant spacecraft maneuver (best hidden in Earth occultation) and new acquisition are required to change from COS to STIS. The STIS data insure that the optical status is recorded independent of weather-dependent ground-based data.
COS OBSERVATIONS:
COS target acquisition will use a 120 sec exposure NUV ACQ/IMAGE using MIRRORB+PSA, which gives S/N = 50, 25, 13 for A_V=1.3, 2.3, 3.3. For maximum light (A_V=1.3) the peak pixel count rate is 5.8 ct/s (the limit is 50 ct/s.) With this exposure time adequate signal is reached for all expected target brigthness levels.
COS FUV observations will be split between the G130M 1291 setting and the G160M 1577/1600 settings. The 1390-1430 A region is covered by both gratings providing continuous coverage of Si IV, 3 CO bandheads, and many H_2 fluorescent lines. The spectra would be interleaved in a repeated G130M 1291 -G160M 1577 -G160M 1600 sequence spread over most of the 4 orbits. The final part of the fourth orbit is used to obtain a lower resolution G140L spectrum.
STIS OBSERVATIONS:
A 0.1 sec exposure CCD ACQ with F28X50LP will be used to acquire the target. This exposure time is sufficient for all plausible target brightness levels. This will be followed G430L (100 s) and G750L (10 s) CCD ACCUMs and a much longer (850 s) G230L NUV-MAMA TIME-TAG observation. The G430L and G750L exposures are repeated to complete the orbit followed by a G750L CCDFLAT.
COORDINATED OBSERVATIONS:
75 kiloseconds (three 25 ksec observations) of XMM-Newton time was approved by the HST review to provide coordintaed (ideally simultaneous) X-ray observations at the times of the HST UV/optical observations.
We shall obtain ground-based photometric and spectroscopic monitoring of T Cha during the weeks surrounding the HST observations. The ground-based observations do not drive any scheduling requirements but do imply that the January-July time window would be the preferred season from that perspective.Stellar PhysicsPlanets and Planet Formation6falsetruefalsefalsefalse75trueSUPPORTEDSTARPROTOPLANETARY DISKT TAURI STARNOCoordinates, parallax, and proper motions from van Leeuven (2007, "Hipparcos, the New Reduction") and Gaia DR1. Proper motions confirmed by Teixeira et al (2000, A&A, 361, 1143). Gaia DR1 provides accurate sub-mas positions at epcoh 2015.0.
Typical V magnitudes for this star range from V=11.3 down to at least V=13.3.
Only BOT warnings are from the target star itself and are invalidated by ETC runs.J2000J2000COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1600COS/NUVImagingNoNoMIRRORBSTIS/CCDImagingNoNoF28X50LPSTIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG750L7751COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1600COS/NUVImagingNoNoMIRRORBSTIS/CCDImagingNoNoF28X50LPSTIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG750L7751COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1600COS/NUVImagingNoNoMIRRORBSTIS/CCDImagingNoNoF28X50LPSTIS/CCDSpectroscopicNoNoG430L4300STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG750L7751Timing link suitability includes constraints ([Sequence (01 1A) within 0.3 days] [02 After 01 by 3.0 to 7.0 days] [1A After 01] [2A After 01] [3A After 01])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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)true40NUV target acquisition with MIRRORB. Exposure time of 120 seconds to accomodate taget variability.
At maximum light (V=11.3) achieve S/N~70 with brightest pixel at 5.75 c/s (COS.ta.1009011).
At minimum light (V=13.3) achieve S/N~18 with brightest pixel at 0.40 c/s (COS.ta.1009008).All G130M observations obtained at 1291 setting to allow use of both SEGMENTS A and B.
FP-POS=4 used for all G130M 1291 exposures because of need to observe molecular hydrogen
absorption lines on the red wing of H Lyman alpha between 1218 and 1220 A.
ETC run is for maximum light conditions.ACombined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-16 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Timing link suitability includes constraints ([Sequence (01 1A) within 0.3 days] [1A After 01])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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:data-volume 414640
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(Tic-Obset
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(Tic-Orbit
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)true10ETC checks made for wide variety of source brightness: For typical current era maximum brightness (V=11.3) 0.1 sec exposure gives S/N=156 (STIS.ta.1016403). For very faint level (V=14.5) S/N=30 (STIS.ta.1016211). For unexpectedly high brightness (V=10.4 -- largest very long-term number) the S/N=238 (STIS.ta.1016210). Under all these scenarios the 0.1 second exposure has a better than factor of 5 cushion compared to the "Time to Saturation".Timing link suitability includes constraints ([Sequence (02 2A) within 0.3 days] [02 After 01 by 3.0 to 7.0 days] [03 After 02 by 3.0 to 7.0 days])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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(Tic-Orbit
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(Tic-Orbit
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)true40NUV target acquisition with MIRRORB. Exposure time of 120 seconds to accomodate taget variability.
At maximum light (V=11.3) achieve S/N~70 with brightest pixel at 5.75 c/s (COS.ta.1009011).
At minimum light (V=13.3) achieve S/N~18 with brightest pixel at 0.40 c/s (COS.ta.1009008).All G130M observations obtained at 1291 setting to allow use of both SEGMENTS A and B.
FP-POS=4 used for all G130M 1291 exposures because of need to observe molecular hydrogen
absorption lines on the red wing of H Lyman alpha between 1218 and 1220 A.
ETC run is for maximum light conditions.ACombined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Timing link suitability includes constraints ([Sequence (02 2A) within 0.3 days] [2A After 01])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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)true10Timing link suitability includes constraints ([Sequence (03 3A) within 0.3 days] [03 After 02 by 3.0 to 7.0 days])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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)true40NUV target acquisition with MIRRORB. Exposure time of 120 seconds to accomodate taget variability.
At maximum light (V=11.3) achieve S/N~70 with brightest pixel at 5.75 c/s (COS.ta.1009011).
At minimum light (V=13.3) achieve S/N~18 with brightest pixel at 0.40 c/s (COS.ta.1009008).All G130M observations obtained at 1291 setting to allow use of both SEGMENTS A and B.
FP-POS=4 used for all G130M 1291 exposures because of need to observe molecular hydrogen
absorption lines on the red wing of H Lyman alpha between 1218 and 1220 A.
ETC run is for maximum light conditions.ACombined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Combined exposures 15-18 should provide S/N~5 per res.el. in continuum for V=11.3
(COS.sp.1009024) and S/N~1.5 per res. el. in continuum for V=13.3 (COS.sp.1009023).Timing link suitability includes constraints ([Sequence (03 3A) within 0.3 days] [3A After 01])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 15128
:visit-id "3A"
:proposal-version -1
:trans-version "20170613"
:date "01-Aug-2017 15:58:03.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:si-bright-earth-limb-angle 20.0
:data-volume 414640
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:coron NIL
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(Tic-Obset
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(Tic-Orbit
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:orbit-number 1
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)true10