0 Assigned ID: 1 ----- Attempting Submission 1 (Fri Feb 28 18:25:55 GMT 2014) ----- HST Phase I Proposal 1 (DD_2014_v3.pdf.apt) successfully submitted. ----- Attempting Submission 2 (Mon Mar 03 12:27:56 GMT 2014) ----- A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. Sensitive exposures should have an ETC run number provided. The ETC can not be run because we are using an available but unsupported mode. The brightest flux will come from the Lyman-alpha emission from the geocorona (6.1e-13 erg/s/cm2/arcsec2) There is a warning that target acquisition should be performed before doing any spectroscopy but I am not really sure about the inputs that I should give. I tried to run the BOT but I am not sure that it worked properly. -1642859922 ----- Attempting Submission 1 (Mon Mar 10 22:28:33 GMT 2014) ----- The ETC can not be run because we are using an available but unsupported mode. The brightest flux will come from the Lyman-alpha emission from the geocorona (6.1e-13 erg/s/cm2/arcsec2) There is a warning that target acquisition should be performed before doing any spectroscopy but I am not really sure about the inputs that I should give. I tried to run the BOT but I am not sure that it worked properly. Our proposal is to use the Hubble Space Telescope Imaging Spectrograph (HST /STIS) over a single orbit to make Lyman-alpha observations of the interplanetary hydrogen (IPH) during the April period of this year (2014). These measurements will provide wavelength and flux calibration, in order to support the HYPE instrument (Hydrogen Polarimetric Explorer) that is planned to make spectro-polarimetric observations in April during a suborbital flight of a NASA sounding rocket (grant NNX08AI98G). Cross-calibration will also be made with the SWAN instrument (Solar Wind Anisotropies) on the SOHO satellite (Solar and Heliospheric Observatory). SWAN can provide flux calibration but without any spectral information, so only HST/STIS can provide the wavelength calibration. Moreover the scientific controversy on the physical properties of the local interstellar medium (LISM) is still going on. The recent observations of interstellar helium atoms by IBEX (Interstellar Boundaries Explorer) suggest that the LISM velocity vector may vary over time. Such a change should impact the bulk velocity of interplanetary hydrogen and should be detected by HST /STIS. TARGET & OBSERVATION MODE We will observe the backscattering of solar Lyman-alpha photons by the interplanetary hydrogen (IPH) in the upwind direction with HST/STIS during one orbit, in order to obtain one high-resolution line profile. The IPH is a faint and diffuse source, this is why we will use the E40H echelle grating with the long slit (52" x 0.5") in order to increase the signal-to-noise ratio. We already used this available but not supported mode for previous observations (2001, 2012, 2013). SCHEDULING CONSTRAINTS We desire to obtain the maximum Doppler shift between the interplanetary and geocoronal emissions in order to reduce the overlapping between line profiles. This requires that the Earth moves toward the upwind direction, so the observation should occur in a window of 2 months centred around 1st April 2013. April will suit better than March, because of an unique opportunity of cross-calibration: the HYPE instrument (Hydrogen Polarimetric Explorer) is planned to make spectro-polarimetric observations in April during a suborbital flight of a NASA sounding rocket (grant NNX08AI98G). CONSTRAINT ON THE FIELD OF VIEW The observations should be done with no stars brighter than V-Magnitude=18 in the aperture. REQUEST ON THE FUV-MAMA DETECTORS With a signal-to-noise of about 10, the background noise is a significant issue for the data analysis. This is why it is really important and necessary to start the FUV-MAMA detectors just before the exposure, in order to reduce the background noise, especially the intermittent glow due to the dark current. (http://www.stsci.edu/hst/stis/documents/handbooks/currentIHB/c07_performance6.html#310668) SOLAR SYSTEM Default false false false false false AVAILABLE ISM WIND The observations should be done with no stars brighter than V-Magnitude=18 in the aperture. J2000 Lyman-alpha emission from the geocorona = 6.1e-13 erg/s/cm2/arsec2 STIS/FUV-MAMA Spectroscopic No No E140H 1234 1394488926370 /tmp/OPVisit5916287570290796215.xml The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. Lyman-alpha observations of the interplanetary hydrogen in the upwind direction. (Tic-Visit :proposal-id 13628 :visit-id "01" :proposal-version -1 :trans-version "20131031" :date "10-Mar-2014 23:02:04.0" :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 173968 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13628 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13628 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2597 :al-overhead-at-end 0 :internal-dur-at-end 626 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 1 0 ETC can not be run because we are using an unsupported mode: E140H grating with the 52" x 0.5" slit.