0 Assigned ID: 1083 ----- Attempting Submission 1 (Tue Feb 26 13:36:25 GMT 2013) ----- HST Phase I Proposal 1083 (proposal_re0503.apt) successfully submitted. ----- Attempting Submission 2 (Thu Feb 28 12:51:49 GMT 2013) ----- HST Phase I Proposal 1083 (proposal_re0503.apt) successfully submitted. ----- Attempting Submission 3 (Thu Feb 28 15:31:31 GMT 2013) ----- HST Phase I Proposal 1083 (proposal_re0503.apt) successfully submitted. ----- Attempting Submission 4 (Fri Mar 01 11:21:48 GMT 2013) ----- HST Phase I Proposal 1083 (proposal_re0503.apt) successfully submitted. Hi Shelly, please see my e-mail related to this submission. Best regards, Klaus 1770293060 ----- Attempting Submission 1 (Tue Jun 04 14:57:58 GMT 2013) ----- We propose STIS-UV spectroscopy of the rather peculiar, hot helium-rich white dwarf RE 0503-289. In FUSE spectra we have recently discovered as much as ten trans-iron group elements (atomic numbers between 31-54), a phenomenon that has never been observed before in any WD. Abundance analyses of Kr, Xe, and Ge show that they are strongly overabundant (450 to 3800 times solar). We suspect that this is related to the evolutionary history of the WD. RE 0503-289 is a transition object between the PG1159 and DO spectral classes, which represent a (pre-) WD sequence of stars that suffered a late He-shell flash. As a consequence of flash-induced envelope convection, the WD exposes the H-He intershell layer of the progenitor AGB star that is enriched with trans-Fe elements resulting from s-process nucleosynthesis. The proposed UV observations shall support a precise abundance analysis of all other elements detected so far, but we mainly aim at the detection and analysis of hitherto undetected heavy elements. We want to address the question whether the observed abundance pattern is affected by diffusion or if it represents the original composition of the s-processed material. In the latter case, detailed tests of nucleosynthesis models are possible. We will perform short-slit (0.2"x0.2") medium-dispersion UV spectroscopy of RE0503-289 in the STIS/FUV-MAMA and NUV-MAMA configurations with gratings E140M and E230M (two wavelength settings), respectively, in order to cover the wavelength range 1150-3100 A. This provides the spectral resolution (~30,000) needed for the quantitative analysis of narrow metal lines. STIS ETC was used to estimate exposure times necessary to achieve the required S/N ~ 20-40. HOT STARS Default false true false false false SUPPORTED STAR WDO J2000 J2000 1.8E-12 erg/(cm2 s A) at 1360 A STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/NUV-MAMA Spectroscopic No No E230M 2707 1370357788613 C:\Users\werner\AppData\Local\Temp\OPVisit5294166192098224887.xml The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13358 :visit-id "01" :proposal-version -1 :trans-version "20130502" :date "04-Jun-2013 16:56:27.0" :trans-errors '(:WARNINGS 0 :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 365840 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13358 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13358 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2920 :al-overhead-at-end 194 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13358 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3031 :al-overhead-at-end 194 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13358 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3031 :al-overhead-at-end 0 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) true 3 0