0Assigned ID: 4232
----- Attempting Submission 1 (Wed May 24 02:29:12 GMT 2023) -----Changed Phase II contact and co-PI-1945476318----- Attempting Submission 1 (Thu Sep 14 13:28:37 GMT 2023) -----
----- Attempting Submission 2 (Fri Sep 29 21:20:35 GMT 2023) -----
----- Attempting Submission 3 (Thu Feb 27 04:47:10 GMT 2025) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 4 (Wed Apr 02 17:14:52 GMT 2025) -----No changes in observations setup were performed, and all observations are already executed.Mapping the inner disk wind of RU Lup with molecular hydrogenThe evolution of gas in protoplanetary disks sets direct constraints on the formation and evolution of planets. However, the exact mechanisms of how gas in disks evolves are not yet clear. It is now thought that disk winds play an essential role in removing angular momentum from the disk and are thus driving accretion onto the star, with significant implications on the viscous state of the disk. Measuring the ratio of wind mass loss rate to stellar accretion rate allows to estimate the disk viscosity - one fundamental parameter needed in all planet formation models.
To now, winds are observationally mainly characterized through the analysis of secondary tracers, such as forbidden atomic lines, CO or dust. However, the main mass component of disks and winds is molecular hydrogen (H2), and it is not entirely clear if wind properties derived from secondary tracers directly relate to those derived from H2.
In this program, we propose to spatially and spectrally map the inner disk wind of RU Lup, which hosts one of the best characterized inner disk winds from secondary tracers. Our measurements will target multiple lines of fluorescent H2 emission in the UV, and therefore directly trace the main mass component in the wind. The comparison of H2 wind mass loss rate, as well as the wind's spatial and kinematic structure to wind properties derived from other tracers will fundamentally probe the viscous state of the disk, and reveal how the main mass component behaves with respect to other components.This program requests a spatial scan along the disk major axis of RU Lup using the E140M grating. There are 10 seperate spatial fields that are partially overlapping and are separated by 37.5 mas. Field 'NW1' and 'SE1' are identical and are centered onto the star. The fields are all slightly shifted to the SW along the slit length direction by 35 mas to allow a focus of the field on the SW part of the disk.
We request initial acquisition (incl. peak-up) of each visit on the central star itself, RU Lup, before slewing to the respective offset field. The slit is requested to a position angle (E of N) of 47 or 227 deg, corresponding to a STIS orient angle (=PA+45 deg) of 92 or 272 deg.
We insert an optical G750M spectrum at the end of the first orbit of each visit to measure the Halpha line which will allow an estimate of the instantaneous accretion rate.
The individual visits can be executed independently from each other, but a close sampling in time would be most preferable to limit any potential variability of the system.Dr. Haeun Chung is an expert in UV instrumentation, and has expertise in spectroscopic data modeling, reduction, and analysis. Dr. Erika Hamden is an expert in UV spectroscopy and data analysis. Dr. Thomas Haworth is an expert in disk evolution and disk winds. He has led papers modelling the dynamics of internally and externally driven photoevaporative winds. He also studies disk evolution under the combined actions of internal/external winds and different degrees of viscous transport. His expertise will be used to interpret the evolutionary implications for RU Lup. Dr. Keri Hoadley is expert in modeling H2 fluorescent emission from protoplanetary disks, as well as in processing and analysing HST UV observations. Her expertise will be used to model the H2 gas properties of RU Lup and to fit them to the observations obtained in this program. Dr. Miriam Keppler has expertise in multi-wavelength data analysis of protoplanetary disks from the optical to the sub-millimeter regime. She has led publications analyzing the spatial and kinematic structure of planet-forming disks. Dr. J. Serena Kim has expertise in data analysis for HST/STIS which is the prime instrument for this proposal. Dr. Kim is an expert in star formation and evolution of circumstellar disks and has conducted numerous ground-based and space observations from X-ray to infrared wavelengths. Dr. Emma Whelan is expert in spectroscopic observations of disk winds and their interpretation. She has led a recent publication constraining the extent of the MHD wind in RU Lup, and her expertise for the RU Lup system will be used to compare the observations obtained within this program to datasets containing different disk wind tracers. Dr. Azalee Bostroem has extensive experience in STIS observations and data processing and is a particular expert of the calstis pipeline. Dr Bostroem will advice and support the observation planning and the data reduction.Stellar Physics and Stellar TypesExoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalseSUPPORTEDSTARPROTOPLANETARY DISKT TAURI STARCoordinates of RU Lup were retrieved from Gaia DR3. Vmag was retrieved from Hipparcos catalogue but might be variable (Vmag=9.6 reported in Ducati et al. 2002).J2000J2000SpT=K7, G=10.7107, J=8.732, H=7.824, K=7.138STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STARPROTOPLANETARY DISKVmag reported here correponds to the central star (RU Lup) not included in this offset field. There is no emission expected to be as bright as the star in the offset fields.STIS/FUV-MAMASpectroscopicNoNoE140M1425The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1740360717000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s.RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 seconds.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1740377720000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s.RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1740542066000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s.RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1740689395000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s.RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1742388933000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s..RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1741799797000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s.RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1742128362000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s.RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.1742405926000272.0(Tic-Visit
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)true30RU LUP has V=11.1 mag. Using the F28X50LP slit and a K7 model spectrum, the ACQ ETC predicts an SNR of 243 for an exposure time of 0.1s.RU LUP has V=11.1 mag. Using the 0.2x0.06 slit, the ACQ ETC predicts an SNR of 174 for an exposure time of 0.1s.According to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 secondsAccording to the STIS ETC, we expect a count rate of ~120 counts/s for RU Lup on the entire detector. According to the STIS instrument handbook, the buffert time should be less or equal fo 1.6 x 10^6 divided by the count rate, which corresponds to about 8000 seconds