0Assigned ID: 518
----- Attempting Submission 1 (Fri Mar 06 16:05:03 GMT 2020) -----Original visits 4-7 visits (UV visits) split into single orbit visits:
- Stripped visits 4-7 from their second orbit's exposures making them single orbit visits.
- Added visits 4B, 5B, and 6B containing the exposures from the second orbits
- No timing links added to 4B - 7B as per PC's request. Still, the B-visits shall execute close in time to the other visits
Also, shortened exposure time for visit 9.135993794----- Attempting Submission 1 (Thu Jun 18 13:57:09 GMT 2020) -----
----- Attempting Submission 2 (Thu Apr 01 15:35:35 GMT 2021) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 3 (Tue Nov 23 14:23:31 GMT 2021) -----
----- Attempting Submission 4 (Mon Oct 24 19:31:54 GMT 2022) -----
----- Attempting Submission 5 (Tue Nov 08 19:54:53 GMT 2022) -----Jets and disk scattering - Spatially resolved optical and FUV observations of AA TaudacPlanets form during the time, when the central star accretes material from the surrounding circumstellar disk and the final system architecture depends on the poorly known accretion and ejection history. Accretion tracers are particularly prominent in the UV so that the HST legacy program ULLYSES was conceived to obtain a UV atlas of accreting, young stars. In the UV, however, extinction is a severe issue and already moderate amounts of dust can completely extinguish any (accretion) signal. Accretion and extinction decline with age so that it is imperative to understand how well UV observations actually trace genuine accretion emission for higher absorption column densities or if rather other processes, namely jet emission or light scattered towards the observer by the upper disk layers, mimic accretion in spatially unresolved data such as the ULLYSES COS observations.
Our target, the classical T Tauri star AA Tau, currently experiences a long-lasting dimming event, presumably caused by inner disk dust, i.e., the star is currently hidden behind a "natural coronograph" and the direct emission is greatly reduced. Spatially unresolved HST COS data suggest that jet emission and scattering dominate the integrated FUV light during the dimming event. We propose to utilize this situation to detect UV scattering for the first time and to measure the jet's contribution to the FUV light through spatially resolving the emission with a series of STIS long-slit spectra. This experiment, right in time for ULLYSES, will uncover what fundamentally limits UV accretion studies, lack of signal due to absorption or "contaminating" emission spoiling the interpretation of the signals.The goal of this program is to spatially resolve the FUV and optical emission in
the AA Tau system through a series of STIS long-slit observations with the slit
oriented along the jet axis (perpendicular to disk's major axis).
The program has been changed to visits of max 2 orbits following the cycle 28
recommendations. The target (the jet) is variable and the different visits shall
be executed within the same visibility window.
Due to HST entering the safe mode in Oct. 2021 just before these observations
were planned to execute, the exposure times were slightly shortend
to make the program schedulable in 2022.
Reduced gyro operations
===================
This program targets only a single object and requires a certain ORIENT range
for the long-slit observations and, hence, has a limited number of observing
opportunities per year. Reduced gyro operations may make the requested
ORIENT ranges unschedulable. Increased power in the PSF wings is not
considered very relevant for this program.
FUV data
=========
6 identical 2 orbit visits with STIS-MAMA and the G140M grating (CENWAVE=1540).
During both of the two orbits, we will use the 52x0.1D1 and 52x0.5D1 slits to
cover different sky regions. We opt for this setup to mitigate issue due to
potential minor source variability.
The flux in the G140M grating with CENWAVE=1540 is dominated by C IV and H2
emission and previous observations allow us to estimate the expected count rates
(cf. ETC run STIS.sp.1345817 for the dim state and STIS.sp.1339668 for the
bright state). The 52x0.5D1 slit captures about 50% more photons than 52x0.1D1
(see STIS.sp.1345818)
Detector safety
-------------------------
Previous COS observations of AA Tau allow us to demonstrate that the expected
global (160 cts/s) and local count rates (0.01 cts/s) are well below safety
limits. In fact, the detector can tolerate 100 fold increase in FUV
flux even w.r.t. the bright state; ETC-run: STIS.sp.1339668.
BOT has been run and does not report unsafe targets.
Optical data
============
The optical data consists of a series of five long-slit exposures separated
by 0.1 arcsec using the 52x0.1 slit oriented along the jet axis. Five different
slit positions (stepped perpendicular to the jet) will cover the same spatial
region as the FUV data.
To reduce the number of orbits per visits while maintaining that each visit
covers all 5 slit positions, three different visits were constructed: one 2 orbit
visit with 3/2 slit positions per orbit, one 2 orbit visit with 2/3 slit positions per
orbit and, finally, one 1 orbit visit with all 5 slit positions. This setup balances
scheudling flexibility while simultaneously still maintining a low number of
readouts per slit position.
We use the STIS G750M grating with CENWAVE=6581 to spatially resolve key
lines (Halpha, [O I], [S II], [N II]). Line fluxes have been estimated from a
flux calibrated ESO/VLT Xshooter spectrum (Bouvier et al. 2013). We use fluxes
of 2.0e-14 erg/s/cm^2 for [O I] 6300 AA and 1.4e-15 erg/s/cm^2 for [S II]
6716 AA; see STIS.sp.1345844 where we additionally assumed that the jet's
Halpha emission is 3e-14 erg/s/cm^2.
Target Acquisition
==============
We use the same setup as previous successful aquistions (F28x50LP), but
with a slightly increased exposure time (1.2 s). We estimate that this
exposure time is sufficient to aquire the target even for the dimmest ever
observed target brightness while still avoiding saturation for bright state
conditions.
The target confirmation chart has been reviewed and shows the target well
centered.The PI (Christian Schneider) and numerous team members have extensive experience with the analysis of spatially resolved HST data (Schneider et al., 2013a, b, Guenther et al., 2013, Skinner et al., 2018). Scientifically, the proposed project targets two important features of young stellar systems, namely (a) the jet and (b) the circumstellar disk and the team includes experts from both research area.
(a) Jets: Team members pioneered some of the observational (Bacciotti et al., 2000,2002) and theoretical methods that will be used in this proposal (Bacciotti & Eisloeffel 1998). We will construct pseudo-images of the jet using the same technique as in Maurri et al. (2014) and derive jet properties like density and excitation. Specifically, we will compare tracers of cool (1e3 K) to hot (1e5 K) plasma to study intial vs in situ heating. Further, we will study the jet collimation properties in different velocity channels similar to Bacciotti et al. (2000) or Melnikov et al. (2009).
(b) Disks and circumstellar material: The PI and other team members have also studied circumstellar gas and dust using HST as well as other space and ground-based data (Schneider et al., 2015, McJunkin et al., 2014, 2016, Guenther et al., 2018). In addition, to observing and analysis expertise, the proposing team includes modelers who have the simulation tools ready for application to the anticipated data (see, e.g., Madlener et al., 2012 for an application to a comparable system). In fact, these models were used to prove the feasibility of the proposed observations (Fig. 3 left of the proposal).
The team also includes experts on the specific target, who have studied the system since 20+ years (Bouvier et al. 1998, Schneider et al. 2015).
References for Team Expertise:
Bacciotti, F., Mundt, R., Ray, T. P., Eisloeffel, J., Solf, J., Camezind, M. 2000, ApJ, 537, 49
Bacciotti, F., Ray, T. P., Mundt, R., Eisloeffel, J., Solf, J. 2002, ApJ, 576, 222
Bacciotti, F. & Eisloeffel, J. 1998, A&A, 342, 717
Guenther, H. M., Birnstiel, T., Huenemoerder, D. P., Principe, D. A., Schneider, P. C., Wolk, S. J., Dubois, F., Logie, L., Rau, S., Vanaverbeke, S. 2018, AJ, 156, 56
Madlener, D., Wolf, S., Dutrey, A., Guilloteau, S. 2012, A&A, 543, 81
Maurri, L., Bacciotti, F., Podio, L., Eisloeffel, J., Ray, T. P., Mundt, R., Locatelli, U., Coffey, D. 2014, A&A, 565, 110
McJunkin, M., France, K., Schneider, P. C., Herczeg, G. J., Brown, A., Hillenbrand, L., Schindhelm, E., Edwards, S. 2014, ApJ, 780, 150
McJunkin, M., France, K., Schindhelm, E., Herczeg, G. J., Schneider, P. C., Brown, A. 2016, ApJ, 828, 69
Melnikov, S. Yu, Eisloeffel, J., Bacciotti, F., Woitas, J., Ray, T. P. 2009, A&A, 506, 763
Schneider, P. C., Eisloeffel, J., Guedel, M., Guenther, H. M., Herczeg, G., Robrade, J., Schmitt, J. H. M. M. 2013a, A&A, 550, 1
Schneider, P. C., Eisloeffel, J., Guedel, M., Guenther, H. M., Herczeg, G., Robrade, J., Schmitt, J. H. M. M. 2013b, A&A, 557, 110
Schneider, P. C., France, K., Guenther, H. M., Herczeg, G., Robrade, J., Bouvier, J., McJunkin, M., Schmitt, J. H. M. M. 2015, A&A, 584, 51S
Skinner, S. L., Schneider, P. C., Audard, M., Guedel, M. 2018, ApJ, 855, 143Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARJETK V-IVPROTOPLANETARY DISKT TAURI STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/FUV-MAMASpectroscopicNoNoG140M1540STIS/CCDSpectroscopicNoNoG750M6581POS-TARGMOSAICDITHER0.1STIS-ALONG-SLITfalsetrue50.0POS-TARGSTIS-PERP-TO-SLIT90.01falsePOS-TARGMOSAICDITHER0.2STIS-ALONG-SLITfalsetrue30.0POS-TARGSTIS-PERP-TO-SLIT90.03falsePOS-TARGMOSAICDITHER0.2STIS-ALONG-SLITfalsetrue20.0POS-TARGSTIS-PERP-TO-SLIT90.02falseTiming link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08 09) within 30.0 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Long slit observation with two slit widths per orbit. This setup enables us to monitor variability between the two slit widths.
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)true10Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08 09) within 30.0 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Part 2/3 for the optical data
2 orbit visit with 2 slit positions in the first orbit and 3 slit positions in the second.(Tic-Visit
:proposal-id 16233
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:data-volume 221296
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(Tic-Obset
:proposal-id 16233
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(Tic-Orbit
:proposal-id 16233
:visit-id "08"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2487
:al-overhead-at-end 72
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:dark-offset NIL
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(Tic-Orbit
:proposal-id 16233
:visit-id "08"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2488
:al-overhead-at-end 75
:internal-dur-at-end 419
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3157
:pcs-gap 0
)true20/tmp/OPVisit13188927417826327773.xmlTiming link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08 09) within 30.0 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Part 3/3 for the optical data
1 orbit visit with 5slit positions(Tic-Visit
:proposal-id 16233
:visit-id "09"
:proposal-version -1
:trans-version "20220630"
:date "08-Nov-2022 20:35:28.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 202912
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16233
:visit-id "09"
:obset-id "09"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16233
:visit-id "09"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 1870
:al-overhead-at-end 75
:internal-dur-at-end 439
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3157
:pcs-gap 0
)true10