Hi Bill, here is the revised Phase II - I've edited visit 02, and changed the 2 M-gratings against the G230L at two central wavlengths. I'll send you the ETC input, as well as the COS spectrum from visit 04 by e-mail. Boris ----- Attempting Submission 3 (Mon Feb 22 21:13:38 GMT 2010) ----- APT complains about visit overruns in visits 01, 03, and 04 - but I haven't touched those (and 04 is already done). An intensive COS spectroscopic study of the planetary debris disks around two warm white dwarfs It is very likely that the gas giants in our Solar system will survive the evolution of the Sun into a white dwarf, and the same is thought to be generally true for Jovian planets around solar-like stars if their initial orbits are wider than ~3AU. Despite this prediction, no unambiguous detection of a planet around a white dwarf has been announced so far. However, over the past few years, about a dozen white dwarfs have been identified which host metal-rich debris disks that are thought to stem from the tidal disruption of asteroids. In most cases the debris disks are observed in the form of an infrared flux excess, and offer relatively little diagnostic potential for the study of their structure. We have discovered three warm (T~20000K) white dwarfs with metal-rich debris disks in a gaseous phase which display strong double-peaked CaII emission lines in the I-band and weak Fe 5169A emission. The line profiles can be modelled in terms of Keplerian disks with an extension of ~1Rsun around the white dwarfs. Photospheric MgII 4481A absorption demonstrates that the white dwarfs are accreting from the debris disks. Besides these spectral features, the optical wavelength range is devoid of other useful metal transitions. Here, we propose an intensive spectroscopic ultraviolet study of these systems, which will provide (a) ~1000 photospheric absorption lines of 15 chemical elements, allowing an accurate abundance study of the material accreted from the debris disks, and (b) ~2 dozen additional emission lines of Mg, Cr, Ti, and Fe that will provide detailed insight into the dynamical, thermal, and density structure of these exo-planetary debris disks.
The main scientific thrust of this proposal is (1) to determine the photospheric abundances of the two white dwarfs SDSS1228+1040 and SDSS0845+2257, which reflect the abundances in the debris disks, and (2) to obtain high-quality observations of the Mg, Cr, Ti, and Fe emission line profiles predicted to be present in the near-ultraviolet. Both goals need sufficiently high spectral resolution to avoid blending of the photospheric absorption lines, which would hinder accurate abundance determinations, and to fully resolve the kinematic structure of the emission line profiles, which will have a complex structure due to the number of components. We will cover the far-ultraviolet (FUV) of the spectrum with three orbits of COS G130M/ G160M observations per target, where two different central wavelength settings (1291/1327 & 1577/1623) will be used to cover the gaps between the two FUV detector segments. Given the large degree of overlap between these settings, we decided to adopt only two different FP-POS positions for each G130M observation. The expected S/N of the G160M observations is too low to warrant FP-POS dithering, so we go for single exposures. The emission lines from the debris disk in the near-ultraviolet (NUV) will be observed with the G225M/G285M gratings, using a total of 6 central wavelengths (2339/2373/2410 & 2657/2695/2739) to get nearly continuous coverage over the range 2225-2875, requiring 5 orbits per object. No FP-POS dithering will be done as the grating seetings overlap already to a large degree. All observations will be done in TIME-TAG mode using TAG-FLASH wavelength calibrations. Both targets are GSC-II objects, and have measured GALEX FUV and NUV fluxes. N/A EXTRA-SOLAR PLANETS 12 false 0.0 0.0 false false false false false false SUPPORTED STAR DA This is a nearby white dwarf, no extinction. GALEX FUV: 2352.02 +/- 45.70 microJy, GALEX NUV: 1696.94 +/- 26.43 microJy N4W4001867 J2000 12 28 59.9300 +10 40 32.90 J2000 STAR DB This is a nearby white dwarf, no extinction GALEX FUV: 1941.27 +/- 46.05 microJy, GALEX NUV: 2475.09 +/- 31.39 microJy (looked up in GR2, as GR4 seems to be not yet completely ingested at MAST) N90T010555 J2000 08 45 39.1700 +22 57 28.00 J2000 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Spectroscopic No No G285M 2657 COS/NUV Spectroscopic No No G285M 2695 COS/NUV Spectroscopic No No G285M 2739 COS/NUV Spectroscopic No No G225M 2339 COS/NUV Spectroscopic No No G225M 2373 COS/NUV Spectroscopic No No G225M 2410 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Spectroscopic No No G285M 2657 COS/NUV Spectroscopic No No G285M 2695 COS/NUV Spectroscopic No No G285M 2739 COS/NUV Spectroscopic No No G225M 2339 COS/NUV Spectroscopic No No G225M 2373 COS/NUV Spectroscopic No No G225M 2410 The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. /home/astro/btg/tex/Proposals/hst/cycle-17/PhaseII/OP-cache/debris-v01.xml (Tic-Visit :proposal-id 11561 :visit-id "01" :proposal-version -1 :trans-version "20091209" :date "18-Feb-2010 09:12:59.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 904720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11561 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11561 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2906 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3060 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3063 :al-overhead-at-end 0 :internal-dur-at-end 371 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) true 3 2 I used a 19000K DB model spectrum scaled to an SDSS g=15.7, which reproduces within ~15% the observed GALEX fluxes of SDSS0845+2257, as input for the COS ETC to calculate the exposure time for a S/N=40s image (COS72608) I used a 19000K DB model spectrum scaled to an SDSS g=15.7, which reproduces within ~15% the observed GALEX fluxes of SDSS0845+2257, as input for the COS ETC to calculate the exposure time for a S/N=40s image (COS72608) Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is -2 step for 1291A. Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is +1 step for 1291A. Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is -2 step for 1327A. Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is +1 step for 1327A. The expected S/N with the G160M grating does not warrant the additional overhead necessary for FP-POS splitting. Two different central wavelength are observed, which should help to iron out to some extent fixed pattern noise. The expected S/N with the G160M grating does not warrant the additional overhead necessary for FP-POS splitting. Two different central wavelength are observed, which should help to iron out to some extent fixed pattern noise. The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. /tmp/OPVisit10443.xml (Tic-Visit :proposal-id 11561 :visit-id "02" :proposal-version -1 :trans-version "20091209" :date "22-Feb-2010 21:08:34.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "32" :si-bright-earth-limb-angle 20.0 :data-volume 513296 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11561 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11561 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 371 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) true 5 0 I used a 19000K DB model spectrum scaled to an SDSS g=15.7, which reproduces within ~15% the observed GALEX fluxes of SDSS0845+2257, as input for the COS ETC to calculate the exposure time for a S/N=40s image (COS72608) I used a 19000K DB model spectrum scaled to an SDSS g=15.7, which reproduces within ~15% the observed GALEX fluxes of SDSS0845+2257, as input for the COS ETC to calculate the exposure time for a S/N=40s image (COS72608) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. /home/astro/btg/tex/Proposals/hst/cycle-17/PhaseII/OP-cache/debris-v03.xml (Tic-Visit :proposal-id 11561 :visit-id "03" :proposal-version -1 :trans-version "20091209" :date "18-Feb-2010 09:13:09.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 904720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11561 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11561 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2918 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3056 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3056 :al-overhead-at-end 0 :internal-dur-at-end 371 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) true 3 3 I used a 22000 DA model spectrum scaled to an SDSS g=16.3, which reproduces the observed GALEX fluxes of SDSS1228+1040 within ~15%, as input for the COS ETC to calculate the exposure time for a S/N=40 detection -> 7.2s (COS72608) I used a 22000 DA model spectrum scaled to an SDSS g=16.3, which reproduces the observed GALEX fluxes of SDSS1228+1040 within ~15%, as input for the COS ETC to calculate the exposure time for a S/N=40 detection -> 7.2s (COS72608) Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is -2 step for 1291A. Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is +1 step for 1291A. Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is -2 step for 1327A. Because I plan to get two different wavelength settings with the G130M grating that will overlap to a large degree, I decided that two FP-POS positions per central wavelength should be enough. This is +1 step for 1327A. The expected S/N with the G160M grating does not warrant the additional overhead necessary for FP-POS splitting. Two different central wavelength are observed, which should help to iron out to some extent fixed pattern noise. The expected S/N with the G160M grating does not warrant the additional overhead necessary for FP-POS splitting. Two different central wavelength are observed, which should help to iron out to some extent fixed pattern noise. The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. /home/astro/btg/tex/Proposals/hst/cycle-17/PhaseII/OP-cache/debris-v04.xml 1266593388000 274.15526282581686 (Tic-Visit :proposal-id 11561 :visit-id "04" :proposal-version -1 :trans-version "20091209" :date "18-Feb-2010 09:13:13.0" :trans-errors '(:WARNINGS 5 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "32" :si-bright-earth-limb-angle 20.0 :data-volume 791696 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11561 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11561 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2918 :al-overhead-at-end 0 :internal-dur-at-end 126 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "04" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3056 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "04" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3054 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "04" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3051 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11561 :visit-id "04" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3050 :al-overhead-at-end 0 :internal-dur-at-end 428 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3245 :pcs-gap 0 ) true 5 5 I used a 22000 DA model spectrum scaled to an SDSS g=16.3, which reproduces the observed GALEX fluxes of SDSS1228+1040 within ~15%, as input for the COS ETC to calculate the exposure time for a S/N=40 detection -> 7.2s (COS72608) I used a 22000 DA model spectrum scaled to an SDSS g=16.3, which reproduces the observed GALEX fluxes of SDSS1228+1040 within ~15%, as input for the COS ETC to calculate the exposure time for a S/N=40 detection -> 7.2s (COS72608)