0 Assigned ID: 6 ----- Attempting Submission 1 (Wed Feb 01 03:45:20 GMT 2012) ----- HST Phase I Proposal 6 (ngc.apt) successfully submitted. ----- Attempting Submission 2 (Thu Feb 09 22:21:48 GMT 2012) ----- Target Acquisition changed to spectroscopic to allow BOP clearance. -731728043 ----- Attempting Submission 1 (Thu Jun 21 17:53:45 GMT 2012) ----- HST Phase II Proposal 12921 (ngc-phaseII.apt) successfully submitted. ----- Attempting Submission 3 (Tue Jul 03 13:34:51 GMT 2012) ----- ----- Attempting Submission 4 (Sat Apr 27 23:06:11 GMT 2013) ----- ----- Attempting Submission 5 (Wed Jul 31 15:09:02 GMT 2013) ----- ----- Attempting Submission 6 (Thu Aug 01 23:07:53 GMT 2013) ----- Visit 1 only uses two cenwaves for 1291, and Visit 2 1318 FP-POSs are 3-4, then 1-2 in the following orbit, The solar abundances have been referenced in studies of the interstellar and intergalactic media. But the recent downward revision of several light elements has broken the accordance of these abundances with helioseismological measurements. A much higher Ne/O abundance ratio may solve this problem. But due to the absence of the suitable photospheric lines of Ne, this scenario has not been tested observationally. The interstellar medium (ISM) provides a natural laboratory for testing such a hypothesis. We propose a joint program by requesting COS-HST and LETG-Chandra observations of the low mass X-ray binary 4U 0512-401. The required observations will utilize the high resolving power of the COS to resolve the kinematic velocity components of the ISM absorbers and to measure column densities of OI and HI, and then utilize LETG observations to measure column densities of OI, OII, NeI, NeII, and NeIII. The results will enable us to evaluate the depletion level of oxygen into dust grains, measure the Ne/O abundance ratio of the ISM along the line of sight, and then examine whether the ratio is substantially higher than that usually adopted. The main goal of this project is to measure the abundance ratio between Neon and Oxygen in the interstellar medium. To this end, we seek to obtain high resolution spectra of the X-ray binary 4U 0512-401 covering OI, SiII, and SII and thus to constrain kinematics and dynamics of the ISM. Detecting these lines is our fundamental requirement and also drives the requested S/N level. 4U 0512-401 is a mildly variable in UV wavelength band. We therefore use a spectrum with a typical flux obtained from one previous observation [with the Faint Object Spectrograph (FOS) in 1997 for program 6892] as the input to the Exposure Time Calculator to estimate the ACQ-target-searching and ACQ-target-imaging time and to calculate the Buffer-time. The approved 9 orbits will use COS-G130 grating to detect the OI, SiII, and SII absorption lines and we expect to obtain a spectrum with S/N of 10 around OI wavelengths, which, together with SiII and SII absorption lines, allow us to to constrain kinematics and dynamics of the ISM to be within 20% uncertainty range. To reduce COS fixed-pattern noise, we use the G130 grating at different central wevelengths in successive exposures and use the different FP-POS offsets. By doing this, we will also obtain a spectrum coving the maximal wavelength range; the gaps at different wavelengths are also filled up with nearly even exposures. ISM AND CIRCUMSTELLAR MATTER 12 false false 200.0 0.0 false false false SUPPORTED STAR LMXB X-RAY TRANSIENT X0512-401 J2000 J2000 COS/FUV Spectroscopic No No G130M 1300 1375397555479 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. /private/var/folders/31/g39_89jm8xj0fk001s7pt0x80000gn/T/OPVisit1243673710044536989.xml Roll-angle limited to 264--282 to restrict BOA BOP area to the existing ACS F140LP image. TA changed to spectroscopic. (Tic-Visit :proposal-id 12921 :visit-id "1A" :proposal-version -1 :trans-version "20130502" :date "01-Aug-2013 18:52:34.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 887520 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12921 :visit-id "1A" :obset-id "1A" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12921 :visit-id "1A" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3000 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12921 :visit-id "1A" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3111 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12921 :visit-id "1A" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3111 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12921 :visit-id "1A" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3111 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12921 :visit-id "1A" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3111 :al-overhead-at-end 0 :internal-dur-at-end 366 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) true 5 0 FUVA only S/N=40 using the FOS spectrum Y3HG0205P. Using the IUE spectrum, which includes many other stars in the aperture produces a count rate of < 600 countns on both segments (COS.sa.524368). The count rates for the FOS spectrum are Count rate Segment A 74.255 Count rate Segment B 277.983 FUVA only S/N=40 using the FOS spectrum Y3HG0205P. Using the IUE spectrum, which includes many other stars in the aperture produces a count rate of < 600 countns on both segments (COS.sa.524368). The count rates for the FOS spectrum are Count rate Segment A 74.255 Count rate Segment B 277.983 /private/var/folders/31/g39_89jm8xj0fk001s7pt0x80000gn/T/OPVisit8634651559060252004.xml 1375397659049 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. Roll-angle limited to 264--282 to restrict BOA BOP area to the existing ACS F140LP image. (Tic-Visit :proposal-id 12921 :visit-id "2A" :proposal-version -1 :trans-version "20130502" :date "01-Aug-2013 18:54:18.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 739584 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12921 :visit-id "2A" :obset-id "2A" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12921 :visit-id "2A" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3000 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12921 :visit-id "2A" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3111 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12921 :visit-id "2A" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3111 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12921 :visit-id "2A" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3111 :al-overhead-at-end 0 :internal-dur-at-end 366 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) true 4 0 FUVA only S/N=40 using the FOS spectrum Y3HG0205P. Using the IUE spectrum, which includes many other stars in the aperture produces a count rate of < 600 countns on both segments (COS.sa.524368). The count rates for the FOS spectrum are Count rate Segment A 74.255 Count rate Segment B 277.983 FUVA only S/N=40 using the FOS spectrum Y3HG0205P. Using the IUE spectrum, which includes many other stars in the aperture produces a count rate of < 600 countns on both segments (COS.sa.524368). The count rates for the FOS spectrum are Count rate Segment A 74.255 Count rate Segment B 277.983