Visits 03 and 04 were reformatted to include a TARGET ACQ for each orbit since redoing the GS ACQ would wipe out any information from the previous TARGET ACQ. Shifted technical specs as needed. Merle Reinhart knows more details. Visit 03 cut each orbit to allow visit to schedule as planned. ----- Attempting Submission 1 (Fri Jun 27 17:02:47 GMT 2008) ----- ----- Attempting Submission 2 (Fri Jul 17 18:49:17 GMT 2009) ----- ----- Attempting Submission 3 (Mon Jul 20 13:53:37 GMT 2009) ----- ----- Attempting Submission 4 (Wed Aug 26 19:34:20 GMT 2009) ----- Phase II Proposal 11660 (11660_revised.apt) successfully submitted. ----- Attempting Submission 5 (Thu Aug 27 15:18:09 GMT 2009) ----- Phase II Proposal 11660 (11660_revised.apt) successfully submitted. ----- Attempting Submission 6 (Fri Aug 28 11:31:36 GMT 2009) ----- Phase II Proposal 11660 (11660_revised.apt) successfully submitted. ----- Attempting Submission 7 (Fri Aug 28 15:42:56 GMT 2009) ----- ----- Attempting Submission 8 (Wed Nov 10 15:53:19 GMT 2010) ----- ----- Attempting Submission 9 (Thu Dec 09 18:08:32 GMT 2010) ----- Will be sorted out during processing. Assigned ID: 507 ----- Attempting Submission 1 (Fri Mar 07 19:32:27 GMT 2008) ----- Investigation Jet Rotation in Young Stars via High Resolution UV Spectra In recent years we have successfully harnessed the high resolution of STIS in the optical to reveal asymmetries in Doppler shifts transverse to the flow direction in 8 T Tauri jets (Bacciotti ea 2002; Woitas ea 2005; Coffey ea 2004; 2007). We interpret the findings, just 100 AU above the disk, as signatures of jet rotation. The significance of these results is considerable. They form the only existing observational indications supporting the theory that jets extract angular momentum from star-disk systems. Furthermore, they hold the potential to discriminate between the main model contenders: X-wind and Disk-wind (Ferreira ea 2006). Although our results are encouraging, it is evident that we are only marginally resolving the effects of rotation because of the limiting resolution (spatially and spectrally) of STIS in the optical. Therefore, in Cycle 12 we proposed to extend this study into the near-ultraviolet (NUV), giving double the spatial and spectral resolution (proposal ID 9807). Unfortunately, only 3 targets in our survey were observed before the failure of STIS (Coffey ea 2007). Nevertheless, the results were very exciting. Agreement was found between the optical and NUV results in terms of the magnitude and sense of the Doppler shift gradient across the jet. Furthermore, the NUV lines indicated that the observed high velocity gas was launched from about 0.2-0.5 AU, compared to the lower velocity gas traced in optical lines which originates from as far as 2 AU. This puts a strong contraint on MHD launch models, and indeed holds the potential to differentiate between them. Given that the strength of a rotation argument lies in the survey nature of the findings, we need to resume this program in order to see if the same rotation signatures are commonly seen in the NUV, as they are in the optical. Furthermore, the higher spatial and spectral resolution of STIS in the NUV will allow us to more accurately quantify the variation in toroidal velocity as a function of distance from the jet axis. This study will provide an invaluable statistical argument to support the fact that we are indeed observing jet rotation. Such a conclusion is critical to providing observational backing to the widely accepted but untested theory of magnetocentrifugal ejection.
We will exploit the high spatial and spectral resolution of STIS in the NUV to accurately quantify the variation in toroidal velocity between the edges of several jets from T Tauri stars. We have already demonstrated that these jets are observable with STIS in the NUV, see data of Cycle 12 (proposal ID 9807; Coffey et al. 2007). With a modest survey of 5 targets, we want to establish whether jet rotation signatures are common in the NUV, as we have found in the optical (Coffey et al. 2004; 2007). We propose to use the same configuration as in Cycle 12, i.e. STIS with the long slit (6''X0.''2) and E230M echelle grating, centred on 2707 angstroms. With the slit perpendicular to the flow axis, we will be able to spatially sample the transverse velocity profile of the jet. Given the average dispersion per pixel of lambda/60 000, and even allowing for the degradation in velocity resolution which inevitably arises from using the E230M grating with the long-slit on an extended source, we achieve a velocity resolution of 30 km/s. With sufficient signal to noise, we are able to routinely measure velocities with an accuracy as low as 1/10th of the velocity resolution, using Gaussian fitting and cross-correlation techniques. Thus we will be able to detect radial velocity differences between the borders of the flow of 3 km/s. We require the long slit (6''X0.''2) as we want to observe emission from the entire cross-section of the jet in one exposure. From our Cycle 12 NUV data, we have measured jet diameters (fwhm) to be 0.''1 - 0.''2 in the NUV. Therefore, the usual aperture adopted for the E230M echelle grating, namely 0.''2X0.''2, is not appropriate. Since we used the long slit with echelle grating in Cycle 12, we know that the position of the lines in the spectra do not cause overlap on the same columns of the detector. We are aware that a disadvantage of using the long-slit with the echelle grating is that the STScI pipeline does not provide calibration of the files. As in previous projects, pointing to the star will be achieved using target acquisition exposures, with the slit rotated at right angles to the outflow. Then the aperture will be offset by a fraction of an arcsecond with respect to the source (typically 0.''3 or 0.''4 along the flow direction, depending on the target), in order to observe only the jet contributions, at less than 100 AU above the disk-plane. The position angle of the flow, which is a critical parameter, has been found either from images taken from the ground or from the HST Archive. The instrument spatial line spread function has a half-width at zero-maximum of 0."145 in the NUV. Therefore, we can be confident that our observed emission lines originate in jet material excited through low-velocity shocks, rather than any contamination from the star. Note also that any reflected continuum emission can be easily subtracted from our spectra with standard techniques. Our exposure time estimates are determined primarily by the expected fluxes of the Mg II 2800 doublet. Our observations from Cycle 12 represent the only observations in the NUV of the initial jet beam, and are ideal for deciding optimum exposure times. In order to measure the velocity profile, we require a signal-to-noise of at least 10 in the jet borders. Since DG Tau represents one of the brightest HH jets, and even here the borders grew rapidly faint in Cycle 12 data, it seems wise in further observations to increase the exposure time to ensure accurate measurements at the farthest points from the intensity peak. We expect all but one of our 5 targets to show similar emission intensity as DG Tau. For the RW Aur approaching jet (which shows signatures of rotation in Cycle 11 spectra), the lines will be fainter by about a factor of 2. Only in this one case do we require twice the integration time. To calculate our total HST orbit requirements, we have allowed 6 minutes for guide star acquisition, 6 minutes for STIS target acquisition exposures, 8 minutes for exposure overheads and 4 minutes for an additional GO-wavecal. Sufficient signal-to-noise (>10) in the jet borders can be achieved in 3 orbits. Therefore, we require 3 orbits per target, for four targets. For the faint, yet crucial, case of the RW Aur approaching jet, we require double this exposure time and hence 6 orbits. We therefore require a total of 18 orbits. STAR FORMATION 12 false 0.0 0.0 false false false false false false SUPPORTED ISM JET This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. GSC02389-00955 HIC23873 J2000 05 07 49.5679 +30 24 5.16 J2000 ISM JET This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 04 14 17.0000 +28 10 57.80 J2000 ISM JET This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 04 42 37.6900 +25 15 37.30 J2000 ISM JET This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 04 33 39.3600 +17 51 52.30 J2000 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. We require observations with the dispersion direction perpendicular to the jet position angle. The visit orientation may therefore be 85.0 degrees or 265.0 degrees, depending on available guide stars. We choose one visit at each orientation in order to isolate possible instrumental effects. 1282328797000 265.0 (Tic-Visit :proposal-id 11660 :visit-id "01" :proposal-version -1 :trans-version "20090702" :date "28-Aug-2009 15:30:12.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 539920 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11660 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11660 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2950 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 325 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) true 5 0 The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. We require observations with the dispersion direction perpendicular to the jet position angle. The visit orientation may therefore be 85.0 degrees or 265.0 degrees, depending on available guide stars. We choose one visit at each orientation in order to isolate possible instrumental effects. (Tic-Visit :proposal-id 11660 :visit-id "02" :proposal-version -1 :trans-version "20090702" :date "28-Aug-2009 16:17:07.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 435504 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11660 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11660 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2950 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 325 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3283 :pcs-gap 0 ) true 4 0 The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. /private/var/folders/U7/U7EpVZ9NHJe91f-zXie+mk++4y2/-Tmp-/OPVisit3885908944223854824.xml We require observations with the dispersion direction perpendicular to the jet position angle. The visit orientation may therefore be 110.0 degrees or 290.0 degrees, depending on available guide stars. -- PC Note: This visit will execute at the preferred ORIENT of 110.0 degrees on a slightly fainter than default single guide star as a shared-risk observation. -- (Tic-Visit :proposal-id 11660 :visit-id "03" :proposal-version -1 :trans-version "20100902" :date "09-Dec-2010 12:44:00.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 366768 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11660 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11660 :visit-id "03" :obset-id "A3" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11660 :visit-id "03" :obset-id "B3" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11660 :visit-id "03" :orbit-number 1 :pcs-time 241 :si-vis-utilization 3005 :al-overhead-at-end 325 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "03" :orbit-number 2 :pcs-time 241 :si-vis-utilization 3005 :al-overhead-at-end 325 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "03" :orbit-number 3 :pcs-time 241 :si-vis-utilization 3005 :al-overhead-at-end 325 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 3 0 The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. We require observations with the dispersion direction perpendicular to the jet position angle. The visit orientation may therefore be 175.0 degrees or 355.0 degrees (but 355.0 is not allowed by the visit planner). 1291381739000 175.0 (Tic-Visit :proposal-id 11660 :visit-id "04" :proposal-version -1 :trans-version "20100505" :date "10-Nov-2010 10:50:45.0" :trans-errors '(:WARNINGS 6 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 314544 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11660 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11660 :visit-id "04" :obset-id "A4" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11660 :visit-id "04" :obset-id "B4" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11660 :visit-id "04" :orbit-number 1 :pcs-time 241 :si-vis-utilization 2787 :al-overhead-at-end 244 :internal-dur-at-end 321 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3021 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "04" :orbit-number 2 :pcs-time 241 :si-vis-utilization 2787 :al-overhead-at-end 244 :internal-dur-at-end 321 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3021 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "04" :orbit-number 3 :pcs-time 241 :si-vis-utilization 2787 :al-overhead-at-end 244 :internal-dur-at-end 321 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3021 :pcs-gap 0 ) true 3 3 The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. Jet position angle is 171 degress. We require observations with the dispersion direction perpendicular to this. The visit orientation may therefore be 306.0 degrees (126 does not seem to work with the visit planner.) 1290887181000 304.510871718594 (Tic-Visit :proposal-id 11660 :visit-id "05" :proposal-version -1 :trans-version "20090702" :date "28-Aug-2009 16:37:58.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 313680 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11660 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11660 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2695 :al-overhead-at-end 244 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "05" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2806 :al-overhead-at-end 325 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11660 :visit-id "05" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2806 :al-overhead-at-end 325 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) true 3 0