0 Assigned ID: 198 ----- Attempting Submission 1 (Thu Apr 07 07:47:05 GMT 2016) ----- HST Phase I Proposal 198 (FUV_w_ALMA_c24.apt) successfully submitted. Receipt: # 198-1 ----- Attempting Submission 2 (Thu Apr 07 14:17:12 GMT 2016) ----- For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. Revised version following discussion with instrument scientist. -1485522014 ----- Attempting Submission 1 (Mon Jul 18 07:36:32 GMT 2016) ----- ----- Attempting Submission 2 (Fri Jan 13 09:14:50 GMT 2017) ----- We motivate the choice of using only FP-POS 1 and 2 in the proposal description. Our succesful observations of RY Lup (mid-Cycle 23) further motivate this choice. Connecting the shape of the FUV spectrum with disk morphology: a combined HST and ALMA study of young stellar objects in Lupus The physical properties of planets reflect the physical and chemical content of the disk in which they form. Direct resolved observations of disks, e.g., with ALMA, provide us with crucial information on the disk properties to verify planet formation theories. ALMA observations have now reached levels of detail that demand as much detail in the modeling. A major input for models to reproduce resolved ALMA observations of gas in disks, the shape and intensity of the FUV radiation impinging on the disk, is still poorly understood. We thus propose to observe the FUV spectrum of three almost unextincted and still accreting young stars surrounded by disks with different morphology, recently studied with our new high-resolution ALMA observations. Our proposed observations aim at: 1) characterizing the FUV flux of young stars surrounded by disks detected with resolved observations both in dust (0.89mm) and gas (13CO, C18O, and CN) emission with ALMA, 2) studying the chemical properties of their disks to model their gas content, in particular including the FUV flux in the wl<1100 AA region reachable only with HST, which is crucial for H2 and CO photodissociation, 3) determining the relation between the shape of the observed FUV spectrum, in particular the molecular emission lines, with the disk morphology, 4) obtaining simultaneous coverage of the FUV and NUV spectrum to determine the physical origin and shape of the FUV excess above the disk accretion emission. Finally, the FUV flux determined here will also be a crucial ingredient for disk evolution models, such as photoevaporation models, to test whether they can explain the observed morphology and properties of disks. Our observing strategy is driven by the aim to provide a good wavelength coverage for measuring continuum and Lyalpha fluxes. Specifically, we want to cover the wavelengths range from approx. 1000 AA up to 4000 AA, i.e., from the spectral region that drives CO and H2 photodissociation up to the Balmer continuum and jump region, that provides a direct measure for the excess continuum caused by accretion. Another important requirement is the near-simultaneity of our observations in the various bands, as young stars are known to vary on timescales of about one day. Therefore, we plan an observing strategy that includes a mixture of near-simultaneous low and high resolution gratings: we will use three COS gratings, namely G140L (at 1280 AA, two orbits), G130M (at 1291 AA, one orbit) and G160 M (at 1577 AA, one orbit) as well as two STIS gratings (G230L and G430L in one orbit). ORBIT 1: Spectral range 1700 - 5700 AA: we observe the NUV range with the G230L grating (MAMA detector). A short exposure (ca. 1min) with the STIS G430L grating to cover the Balmer jump is done before the G230L one. ORBIT 2-3: Spectral range wl <1100 AA: To measure the flux of the continuum we do not need high spectral resolution below 1100 AA, because contaminating H2 lines are rarer than at longer wavelengths. Therefore, we can use the G140L grating centered at 1280 AA to cover this region (spectral resolution about 1 AA) as it provides the highest sensitivity. At these wavelengths, the background is expected to be relevant. Binning the spectrum to large bins (~ 1 AA) free of emission lines mitigates this effect. We only use FP-POS=1 and 2 to avoid the gap at short wavelength (~1140 and 1120 AA, respectively) as this wavelength range is crucial for our science case. ORBIT 4-5: Spectral range 1200 to 1700 AA: In this region, a wealth of H2 emission lines is present so that higher resolution of the M-mode gratings is necessarily required to disentangle continuum and emission lines. To provide a good sampling of the continuum in this region, we will use the G130M centered at 1291 AA and 1318 AA, and the G160M set to 1577 AA and 1611 AA for one orbit each. The reason to use two different central wavelengths is to have a complete wavelength coverage. Similarly, we will also determine the flux of the emission lines with high S/N. In particular, Lyalpha provides the majority of the FUV flux for CTTSs and the G130M spectrum also covers the Lyalpha emission line at sufficiently high spectral resolution to reconstruct the intrinsic Lyalpha flux using the method presented in Schindhelm et al. (2012, ApJ, 756, L23). This will allow us to determine the Lyalpha to continuum ratio for our target, which is an important parameter for disk chemistry modeling. All observations for each target should be performed as close in time as possible, that is within one day at most. We think that all observations for each target can be fitted in one visit as we did for the mid- cycle 23 observation of RY Lup. If this turns out to be difficult to schedule, we can tolerate to separate the first orbit in a different visit with a maximum separation between the first and the end of the last exposure of one day, which we would implement through the WITHIN option. Detector safety: Based on the RY Lup successful observations, and on the RU Lup available spectra, we have estimated that our exposure times will not harm the detectors in any setting. These stars have fainter V mags than RY Lup. The RY Lup data were well below instrument safety limits, and we have no reason to believe these stars will be brighter in any continuum range or gas emission lines. BOT reports errors, because it misinterprets our targets as an OV star. Coordinates match exactly. Our targets are NOT and OV star. Stellar Physics Extrasolar Planets and Planet Formation 12 false true false false false false SUPPORTED STAR PRE-MAIN SEQUENCE STAR NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates are adjusted for 2016 using proper motion information from UCAC3. MYLUP J2000 J2000 STAR PRE-MAIN SEQUENCE STAR NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates are adjusted for 2016 using proper motion information from Hipparcos. SZ68 J2000 J2000 STAR PRE-MAIN SEQUENCE STAR NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates are adjusted for 2016 using proper motion information from Tycho-2. J160830.7-382827 J2000 J2000 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Spectroscopic No No G430L 4300 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1577 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Spectroscopic No No G430L 4300 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1577 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Spectroscopic No No G430L 4300 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1577 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. /Users/cmanara/work/proposals/HST/Cycle24/FUV_w_ALMA/phase2/OP-cache/FUV_w_ALMA_c24_phaseII_rev-v01.xml (Tic-Visit :proposal-id 14604 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "13-Jan-2017 10:08:32.0" :trans-errors '(:WARNINGS 0 :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 595136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14604 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 14604 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14604 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2974 :al-overhead-at-end 0 :internal-dur-at-end 375 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "01" :orbit-number 2 :pcs-time 333 :si-vis-utilization 2974 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3085 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3084 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3082 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) true 5 0 ETC is for the observed flux-calibrated optical spectrum for this target observed few months ago with VLT/X-Shooter ETC is for the observed flux-calibrated optical spectrum for this target observed few months ago with VLT/X-Shooter This ETC run is done using the IUE spectrum of this target. This target is variable within a factor of 4 in V. We are a factor of ~15 below the brightness limit. This ETC run is done using the IUE and optical spectra of this target This ETC run is done using the STIS G140L spectrum of this target. This ETC run is done using the STIS G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. We have removed the peak of the observed Lyalpha as this was due to girocoronal emission. This ETC run is done using the G140L spectrum of this target. We have removed the peak of the observed Lyalpha as this was due to girocoronal emission. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. /Users/cmanara/work/proposals/HST/Cycle24/FUV_w_ALMA/phase2/OP-cache/FUV_w_ALMA_c24_phaseII_rev-v02.xml (Tic-Visit :proposal-id 14604 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "13-Jan-2017 10:10:29.0" :trans-errors '(:WARNINGS 0 :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 586432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14604 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 14604 :visit-id "02" :obset-id "A2" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14604 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2912 :al-overhead-at-end 0 :internal-dur-at-end 375 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "02" :orbit-number 2 :pcs-time 333 :si-vis-utilization 2912 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3023 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3023 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3023 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) true 5 0 ETC is for the observed flux-calibrated optical spectrum for this target observed few months ago with VLT/X-Shooter ETC is for the observed flux-calibrated optical spectrum for this target observed few months ago with VLT/X-Shooter This ETC run is done using the IUE spectrum of this target. This target is variable within a factor of 4 in V. We are a factor of ~15 below the brightness limit. This ETC run is done using the IUE and optical spectra of this target This ETC run is done using the STIS G140L spectrum of this target. This ETC run is done using the STIS G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. We have removed the peak of the observed Lyalpha as this was due to girocoronal emission. This ETC run is done using the G140L spectrum of this target. We have removed the peak of the observed Lyalpha as this was due to girocoronal emission. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. /Users/cmanara/work/proposals/HST/Cycle24/FUV_w_ALMA/phase2/OP-cache/FUV_w_ALMA_c24_phaseII_rev-v03.xml (Tic-Visit :proposal-id 14604 :visit-id "03" :proposal-version -1 :trans-version "20160601" :date "13-Jan-2017 10:11:01.0" :trans-errors '(:WARNINGS 0 :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 586432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14604 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 14604 :visit-id "03" :obset-id "A3" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14604 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2934 :al-overhead-at-end 0 :internal-dur-at-end 375 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "03" :orbit-number 2 :pcs-time 333 :si-vis-utilization 2934 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "03" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14604 :visit-id "03" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) true 5 0 ETC is for the observed flux-calibrated optical spectrum for this target observed few months ago with VLT/X-Shooter ETC is for the observed flux-calibrated optical spectrum for this target observed few months ago with VLT/X-Shooter This ETC run is done using the IUE spectrum of this target. This target is variable within a factor of 4 in V. We are a factor of ~15 below the brightness limit. This ETC run is done using the IUE and optical spectra of this target This ETC run is done using the STIS G140L spectrum of this target. This ETC run is done using the STIS G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. We have removed the peak of the observed Lyalpha as this was due to girocoronal emission. This ETC run is done using the G140L spectrum of this target. We have removed the peak of the observed Lyalpha as this was due to girocoronal emission. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target. This ETC run is done using the G140L spectrum of this target.