Footprints of the Magnetosphere: the Star- Disk Connection in T Tauri Stars

0 Assigned ID: 226 ----- Attempting Submission 1 (Thu Apr 09 18:27:36 GMT 2015) ----- HST Phase I Proposal 226 (t56_vwcha.apt) successfully submitted. Receipt: # 226-1 ----- Attempting Submission 2 (Fri Apr 10 13:45:46 GMT 2015) ----- HST Phase I Proposal 226 (t56_vwcha.apt) successfully submitted. Receipt: # 226-2 ----- Attempting Submission 3 (Fri Apr 10 22:57:15 GMT 2015) ----- HST Phase I Proposal 226 (t56_vwcha.apt) successfully submitted. Receipt: # 226-3 ----- Attempting Submission 4 (Fri Apr 10 23:14:13 GMT 2015) ----- 0 ----- Attempting Submission 1 (Thu Jul 23 13:42:39 GMT 2015) ----- Footprints of the Magnetosphere: the Star- Disk Connection in T Tauri Stars Previous Spitzer infrared observations of disks around young, low-mass pre-main sequence stars have given us an unprecedented look at dust evolution in young objects. Despite this ground-breaking progress in studying the dust in young disks, the relationship between the dust and gas properties in the inner disk remains essentially unknown. Here we propose to quantify the variability of both the dust and gas in the disks surrounding two T Tauri stars to study how or if accretion onto the star is tied to inhomogeneities in the inner disk. To do this, we will use simultaneous HST, Spitzer, and Swift observations to constrain the X-ray, far-ultraviolet, near-ultraviolet, optical, and near-infrared emission of our sample and provide a picture of the interaction between dust and gas in the inner ~0.5 AU of the disk down to the stellar surface. We will take 5 observations each for T 56 and VW Cha with HST. Each observation will be 2 orbits in length, for a total of 20 orbits. We will need MAMA FUV and NUV spectra to measure mass accretion rates and so we choose the G140L and G230L gratings which cover 1150-1730 Ang and 1570-3180 Ang, respectively. Obtaining simultaneous optical spectra is crucial in order to measure the extinction precisely and accurately measure the FUV/NUV excess above the stellar photosphere. We will use the CCD G430L grating (2900-5700 Ang) and the CCD G750L grating (5240-1027s) to do this. In addition, we will need contemporaneous fringe-flats to correct the spectra beyond 7000 Ang where severe fringing occurs. Low-resolution is sufficient for this study since we are not attempting to measure individual lines in detail. We will achieve a SNR of ~10-20 and note that each HST orbit is ~90 minutes in length. We will need two orbits (~3 hrs) per pointing to complete our observations. We have checked the brightness limits of MAMA and the saturation levels of the CCD and our targets fall within the acceptable limits for variable objects. The timing constraints are as follows. First, for the goals of the proposal, visits 1-4 (T56) and 6-9 (VW Cha) will cover roughly 1 week with each visit separated by 1.5 to 2.5 days. The final visit for each target, visit 5 (T56) and visit 10 (VW Cha), are probing variability on a monthly scale and should follow visits 4 and 9, respectively, by 30 to 60 days. An additional constraint was placed regarding the dates for observing. The initial proposal requested joint time with Spitzer to probe NIR emission related to dust in the circumstellar disk. This time was not granted and we will therefore coordinate ground based observations to coincide with HST observations. CoI's on this proposal have institutional access to the Magellan and Southern Astrophysical Research (SOAR) telescopes, both in Chile, so we will use these telescopes to observe in the NIR. Therefore we request that HST observe the targets when they are visible from Chile, between October 30, 2015 and August 1, 2016. RESOLVED STAR FORMATION 12 false true false false 6 SUPPORTED STAR T TAURI STAR This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR T TAURI STAR This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 1437658859431 Timing link suitability includes constraints ([02 After 01 by 1.5 to 2.5 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 14193 :visit-id "05" :proposal-version -1 :trans-version "20150609" :date "23-Jul-2015 08:36:13.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 339088 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14193 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14193 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3255 :al-overhead-at-end 0 :internal-dur-at-end 552 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3588 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14193 :visit-id "05" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3366 :al-overhead-at-end 239 :internal-dur-at-end 319 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3588 :pcs-gap 0 ) true 2 0 1437658587660 Timing link suitability includes constraints ([07 After 06 by 1.5 to 2.5 days]) The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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