! Proposal 5859, submission 3 ! PI: Douglas Duncan ! Received Wed Jul 26 11:23:06 EDT 1995 ! From: duncan@oddjob.uchicago.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5859,v 5.1 1995/08/01 19:11:58 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Karla Peterson ! Phone: 410 338-4774, E-mail: peterson@stsci.edu ! ! This partially completed template was generated from your Phase I proposal. ! Proposal_Information ! Section 4 Title: Major NLTE Corrections to HST Boron Observations? Proposal_Category: GO Scientific_Category: Cool Stars Cycle: 5 Investigators PI_name: Douglas Duncan PI_Institution: University of Chicago CoI_Name: Dan Kiselman CoI_Institution: Nordita // Blegdamsvej 17 // DK-2100 Copenhagen 0 Contact: ! Y or N (designate at most one contact) CoI_Name: Julie Thorburn CoI_Institution: Yerkes Observatory // Williams Bay, WI 53191 Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) A theoretical study of NLTE effects in the analysis of HST boron observations indicates that all currently-reported abundances are wrong by factors of 2.5-4X. (A systematic effect much larger than any measurement error). If true, this would force major changes in the modelling of Be and B abundances as products of cosmic ray spallation plus direct production by supernovae in the early galaxy. It would help explain why no simple model of galactic chemical evolution can yet explain the evolution of the light elements Li, Be, and B at the same time as the evolution of heavier elements such as Fe and O. We can test the NLTE prediction by observing the BII line at 1362 Angstrom in the star Procyon, whose BI abundance has been extremely well determined from two groups previous HST observations of the BI 2500Angstrom line. (The repaired GHRS opens the possibility of observing the BII line). Our calculations (see figures) demonstrate we should easily see if large amounts of B are being "hidden" (from BI observations) by being in the form of BII. We will use the star Sirius as a reference for differential analysis. BII was observed in Vega and Sirius by the Copernicus satellite 20 years ago, and our re-analysis of this data (see figure) shows we have an excellent chance of success in the present proposal. Questions ! Free format text (please update) Observing_Description: Two objects will be observed: Procyon, the primary target, and Sirius, the standard. For each, a single visit will be used to obtain FP-SPLIT observations at the single wavelength 1362Angstrom. Sirius will be observed with echelle-A and G140M, and Procyon with GHRS G140M exposure. (Even a star as bright as Procyon is not bright at 1300Angstroms. Sirius is hotter, that is why it is much brighter at these wavelengths. Exposure times of 8 min (Sirius) and 160 min (Procyon; 3 orbits) are required to achieve S/N of 300 and 80 respectively. The UV fluxes of both stars at 1360Angstrom are well known, so the exposure times are quite precise. We extracted specra from the IUE archives to check each star. Real_Time_Justification: None. Fixed_Targets Target_Number:1 Target_Name:HD61421 Alternate_Names:GSC0018702180, Procyon Description:STAR,F3-F9 Position:RA=7H 39M 18.113S +/- 0.1S, DEC= 5D 13'30.1" +/- 0.5" ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox:J2000 RV_or_Z: RA_PM:-0.04755 ! Units are seconds of time per year Dec_PM:-1.023 ! Units are seconds of arc per year Epoch:J2000 Annual_Parallax:.292 Flux:V=0.38 +/- 0.02, B-V=0.42 +/- .02, TYPE=F5 IV-V, F-CONT(1360) = 1.3 +/- 1.0 E-12, F-CONT(2090) = 3.5 +/- 1.0 E-10 Comments: Target_Number:2 Target_Name:HD48915 Alternate_Names:GSC0594902767,Sirius Description:STAR,A0-A3 V-IV Position:RA=6H 45M 8.871S +/- 0.1S, DEC= -16D 42'58.0" +/- 0.5" ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox:J2000 RV_or_Z: RA_PM:-0.0385 ! Units are seconds of time per year Dec_PM:-1.205 ! Units are seconds of arc per year Epoch:J2000 Annual_Parallax:.378 Flux:V=-1.46 +/- 0.02, B-V=0.0 +/- .02, TYPE=A1V, F-CONT(1360) = 3.8 +/- 1.0 E-9 ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number:1 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number:1 ! Section 6.5 Target_Name:HD61421 Config:HRS Opmode:ACQ Aperture:2.0 Sp_Element:MIRROR-N1 Wavelength: Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1.8S Special_Requirements:ONBOARD ACQ FOR 2-3 ! Section 7.2 Comments:STEP-TIME=0.2S Exposure_Number:2 ! Section 6.5 Target_Name:HD61421 Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G140M Wavelength:1362 Optional_Parameters:FP-SPLIT=STD Number_of_Iterations:1 Time_Per_Exposure:24.85M ! 24M 51S Special_Requirements: ! Section 7.2 Comments: Exposure_Number:3 ! Section 6.5 Target_Name:HD61421 Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G140M Wavelength:1362 Optional_Parameters:FP-SPLIT=STD Number_of_Iterations:6 Time_Per_Exposure:22.45M Special_Requirements: ! Section 7.2 Visits ! Section 6 Visit_Number:2 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number:1 ! Section 6.5 Target_Name:HD48915 Config:HRS Opmode:ACQ Aperture:2.0 Sp_Element:MIRROR-A1 Wavelength: Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1.8S Special_Requirements:ONBOARD ACQ FOR 2-3 ! Section 7.2 Comments:STEP-TIME=0.2S Exposure_Number:2 ! Section 6.5 Target_Name:HD48915 Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:ECH-A Wavelength:1362 Optional_Parameters:FP-SPLIT=STD Number_of_Iterations:1 Time_Per_Exposure:544S Special_Requirements: ! Section 7.2 Comments: Exposure_Number:3 ! Section 6.5 Target_Name:HD48915 Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G140M Wavelength:1362 Optional_Parameters:FP-SPLIT=STD Number_of_Iterations:1 Time_Per_Exposure:217.6S Special_Requirements: ! Section 7.2 Comments: Data_Distribution ! Defaults indicated; change if desired Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 ! Only astronomers with very old 9- ! track tape drives should consider ! a blocking factor of 1 Ship_To: PI_Address ! STSCI or PI_Address or ! PI Address from Phase I is: ! ! Dept. of Astronomy and Astrophy ! sics , 5640 S. Ellis Ave. , ! Chicago, IL 60637 ! ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense Recipient_Email: ! Needed if Ship_To: is not PI_Address ! ! Let us know what you think of this template and software! ! Please send a list of your likes and dislikes to your Program Coordinator