! Proposal 6459, submission 1 ! PI: Eugene Magnier ! Received Wed Feb 7 15:14:58 EST 1996 ! From: gene@pikake.astro.washington.edu ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6459,v 3.1 1996/02/07 20:31:17 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6459,v 3.1 1996/02/07 20:31:17 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: Bremmer ! Phone: 410-338-4458 , E-mail: bremmer@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0188.magnier.prop ! Date generated: Fri Dec 22 15:32:52 EST 1995 ! Proposal_Information ! Section 4 Title: The disk and jet structure of Holoea Proposal_Category: GO Scientific_Category: COOL STARS Cycle: 6 Investigators PI_name: Eugene Magnier PI_Institution: Astronomy Department, University of Washington CoI_Name: L.B.F.M. Waters CoI_Institution: University of Amsterdam Contact: N ! Y or N (designate at most one contact) CoI_Name: Yi-Jehng Kuan CoI_Institution: Academia Sinica Contact: N ! Y or N (designate at most one contact) CoI_Name: Eduardo Martin CoI_Institution: Instituto de Astrofisica Contact: N ! Y or N (designate at most one contact) Abstract: We have discovered an object in the field of the Galactic open cluster M36 which exhibits a nebulous tail-like structure, a bipolar molecular outflow, a high-velocity ionized wind, and a bright central star with spectral type ~ K0 III (Magnier et al., 1995). This source, which we have nick-named ``Holoea'', most likely represents a very early stage in the evolution from embedded to naked T Tauri star. It also presents an unusual opportunity to study a stellar jet from two angles at once because of a fortuitous reflection off of the nebulous tail. For these reasons, we are vigorously pursuing a program to study this system in detail. Here, we propose to take high- resolution optical images to study the jet and accretion disk structures, both directly and through the reflection. We also hope to find HH objects or other knots in the outflow, which will allow us eventually to measure the distance to the object via proper motion. Questions ! Free format text (please update) Observing_Description: Our observations consist of 5 orbits, with 3 orbits placing the target on the PC for direct images, and the last three placing the object in the WF2 and WF3 for polarization images. Because we require good image quality and dynamic range, each image for a filter will be split into 3 exposures and dithered. This will allow us to limit the effect of cosmic rays, and also to overcome the problem of undersampling. For the three narrow band filters, we have chosen exposure times which give us ~ 5 -- 15 counts per PC pixel for most of the jet regions, while the wide-band B and V images have been chosen to give ~ 15 -- 45 counts per PC pixel. For the V images, the star itself will receive ~ 35,000 counts spread over 4 images, so there will be no danger of saturation. The other bands will have total counts for the central star of 2000 -- 8000 counts. One orbit will consist of the H-alpha and the unpolarized V images, one orbit will include the [OI] and unpolarized B images, and a third orbit will contain the [SII] images, which require somewhat longer exposure times as this line is somewhat fainter. We have also allocated 2 orbits for the polarized B and V images -- one polarization angle per orbit. For the polarized images, we will use the WF2 and WF3 CCDs to get 0 and 45 degree polarizations. We are more concerned about having the appropriate polarization angles and sufficent field of view than the relative calibration of the two CCDs -- furthermore, the direct light from the central star and neighboring stars will help us to calibrate the relative throughput of the two cameras. Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: IRAS05327+3404 Alternate_Names: Holoea Description: STAR, T Tauri Star, K V-IV, ISM, Reflection Nebula, Bipolar Outflow Position: RA=05H 36M 05.9S +/- 0.1S, DEC=34D 06' 18.1" +/- 0.1" ! position is in "tail" ! 6 arcsec north of "star" Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=16.5, B-V=1.4 Comments: Visits ! Section 6 Visit_Number: 1 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: If possible, I'd like all five orbits scheduled consecutively, to avoid major problems with rotated images. As a minimum the first pair of orbits (with V, V+pol(45), and V+pol(90)), should be consecutive, as should the second pair (orbits 3 and 4, with B, B+pol(45), B+pol(90)). Exposure_Number: 1 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F656N ! Halpha Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 400S Special_Requirements: Exposure_Number: 2 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F555W ! V Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 40S Special_Requirements: Exposure_Number: 3 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: WF2-FIX Sp_Element: F555W, POLQ ! V + Polarizer (0 degrees) Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 180S Special_Requirements: Exposure_Number: 4 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F555W, POLQ ! V + Polarizer (45 degrees) Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 180S Special_Requirements: Exposure_Number: 5 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F631N ! [OI] Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 400S Special_Requirements: Exposure_Number: 6 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F439W ! B Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 100S Special_Requirements: Exposure_Number: 7 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: WF2-FIX Sp_Element: F439W, POLQ ! B + Polarizer (45 degrees) Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 200S Special_Requirements: Exposure_Number: 8 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F439W, POLQ ! B + Polarizer (90 degrees) Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 200S Special_Requirements: Exposure_Number: 9 ! Section 6.5 Target_Name: IRAS05327+3404 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F673N ! [SII] Wavelength: Optional_Parameters: CR-SPLIT=NO, DITHER-TYPE=LINE, DITHER-LINE-STEPS=3, CLOCKS=YES Number_of_Iterations: 1 Time_Per_Exposure: 700S Special_Requirements: 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: Astronomy Dept FM-20 University of Washington Seattle, WA 98195 Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense Recipient_Email: gene@astro.washington.edu