! Proposal 6824, submission 1 ! PI: David Devine ! Received Fri Feb 16 17:46:20 EST 1996 ! From: v20@ctios3.ctio.noao.edu ! $Id: 6824,v 11.1 1997/03/31 15:27:14 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6824,v 11.1 1997/03/31 15:27:14 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: Ready ! Phone: 410-338-4546 , E-mail: ready@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-1125.devine.prop ! Date generated: Fri Dec 22 17:49:42 EST 1995 ! Proposal_Information ! Section 4 Title: PC Imaging of HH29: The Nearest Interstellar Shock Proposal_Category: GO Scientific_Category: BINARIES AND STAR FORMATION Cycle: 6 Investigators PI_name: David Devine PI_Institution: University of Colorado CoI_Name: John Bally CoI_Institution: University of Colorado Contact: ! Y or N (designate at most one contact) CoI_Name: John Stocke CoI_Institution: University of Colorado Contact: ! Y or N (designate at most one contact) CoI_Name: Jon Morse CoI_Institution: University of Colorado Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) High resolution imaging of HH objects associated with stellar jets allows us to investigate the interaction zone where the jet impacts the surrounding medium, the resulting shock structures that are formed, and the temporal behavior of the jet itself. We propose narrow band H Alpha \ and SII PC imaging of HH29, which is associated with the well studied L1551-IRS5 flow located at a distance of approximately 150 pc. HH29 is one of the closest HH objects that is bright enough for study with the PC, allowing us to investigate shock structures associated with the outflow from a forming star at the unprecedented scale of 7.5 AU. This will impact our understanding of interstellar jets, shocks, and jet driven outflow models. Questions ! Free format text (please update) Observing_Description: We propose narrow band PC imaging in the emission lines H Alpha \ (F656N) and SII (F673N) We estimate that four orbits will be needed for H Alpha \ and SII. The exposure times were estimated in two methods, published fluxes and angular sizes of HH29 and the method outlined in the WFPC2 manual for extended emission line objects, and direct scaling from ground based NTT images taken under excellent seeing conditions. H Alpha \ and SII fluxes were determined by narrow band imaging of HH29 and the bright knot HH29a under excellent seeing conditions by Fridlund et al (1993) along with angular sizes of the emitting regions. This allows for a direct determination of exposure times using the methods outlined in the WFPC2 instrument handbook for extended emission line sources. Readout noise, dark current and expected sky background were determined also via the methods in the handbook. The resulting count rates for the brightest region (HH29a) are .06 electrons per second for H Alpha \ and .02 electrons per second for SII. An exposure time of 10^4 seconds results in S/N(H Alpha \ ) ~24 and S/N(SII)~ 13.4. From the ratio of the fluxes and sizes for HH29 and HH29a, this corresponds to S/N(H Alpha \ )~5.4 and S/N(SII)~3.0 for HH29. As a consistency check we also estimated exposure times by scaling from HH47 WF images obtained in cycle 5 and the corresponding determined fluxes. The expected exposure times agreed well with the calculated estimates. We expect that the observed S/N ratios should be a bit higher, as the ground based observations are not able to resolve angular scales <=sssim .5" \ . We require orbit long integrations with no CR splitting to ensure that the read noise will not dominate the signal. We will use two pairs of exposures offset by .25 x .25 arcseconds for each filter. This should allow for cosmic ray removal as well as deconvolution techniques to maximize the resolution. Real_Time_Justification: Because of the high proper-motions of the objects it is essential that once the observations of a given object have commenced then they are completed (in both filters) within a 2 week period. The orientation range 72D to 74D will maximize the science obtained with the WF cameras, if this creates a fatal scheduling conflict then the range 80D to 100D may be used, but at a cost to the science. Wide field, narrow band images of L1551 were obtained at Cerro Tololo InterAmerican Observatory in December of 1994, and at Kitt Peak National Observatory in October, 1995. The high angular resolution images representing the limits of ground based imaging were taken in 1990 with the ESO New Technology Telescope. Optical spectra of HH29 were obtained in early January, 1996 at the KPNO 4m. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: HH29 Alternate_Names: Description: ISM,Herbig-Haro Object Position: RA= 4H 31M 27.46S +/- 0.04S, DEC=+18D 6' 24.4" +/- 0.5" Equinox: 2000 RV_or_Z: V = -40 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: SURF-LINE(6562) = 8.8 +/- .1 E-16 W-LINE(6563) = 3.8 +/- 0.1 SURF-LINE(6731) = 6.0 +/- .1 E-16 W-LINE(6731) = 3.8 +/- 0.1 Comments: THE SUFACE BRIGHTNESS REFERS TO THE ENTIRE HH29 KNOT WHICH IS ROUGHLY 12 X 18 ARCSEC SQUARE. ABOUT 20% OF THE FLUX IS CONCENTRATED INTO A SMALLER KNOT THAT IS APPROXIMATELY 2 X 2 ARCSEC SQUARE. THE SURFACE BRIGHTNESS FOR THE [SII] LINE (6731) IS THE SUM OF THE (6717,6731) DOUBLET LINES. Visits ! Section 6 Visit_Number:1 Visit_Requirements:! ORIENTation 72D TO 74D On_Hold_Comments: Visit_Comments: THE ORIENTATION RANGE 72D TO 74D MAXIMIZES THE SCIENCE. IF THIS RANGE IS FATALLY RESTRICTIVE, THEN AN ORIENTATION OF 80D TO 100D IS POSSIBLE, BUT AT A LOSS OF SCIENCE. Exposure_Number:101 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F656N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2500S Special_Requirements: ! Section 7.2 EXPAND MAXimum DURation 4000S MINimum DURation 2500S Comments:NO CR SPLITTING TO ENSURE THAT THE READ NOISE WILL NOT DOMINATE. 101,102,107 AND 108 HAVE THE SAME POINTING. Exposure_Number:102 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F656N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2700S Special_Requirements: ! Section 7.2 SAME POSition AS 101 EXPAND MAXimum DURation 4000S MINimum DURation 2600S Comments:SEE COMMENTS FOR 101 Exposure_Number:103 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F656N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2700S Special_Requirements: ! Section 7.2 POSition TARGet 0.25,0.25 EXPAND MAXimum DURation 4000S MINimum DURation 2600S Comments:SEE COMMENTS FOR 101. 103-106 HAVE THE SAME POINTING, OFFSET FROM 101 BY .25 X .25 ARCSEC FOR DECONVOLUTION !Visits ! Section 6 ! Visit_Number:2 !Visit_Requirements:! ORIENTation 72D TO 74D !PC1-FIX ! On_Hold_Comments: ! Visit_Comments: THE ORIENTATION RANGE 72D TO 74D MAXIMIZES THE SCIENCE. ! IF THIS RANGE IS FATALLY RESTRICTIVE, THEN AN ORIENTATION OF 80D TO ! 100D IS POSSIBLE, BUT AT A LOSS OF SCIENCE. Exposure_Number:104 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F656N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2700S Special_Requirements: ! Section 7.2 SAME POSition AS 103 EXPAND MAXimum DURation 4000S MINimum DURation 2600S Comments:SEE COMMENTS FOR 101,103 Exposure_Number:105 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F673N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2700S Special_Requirements: ! Section 7.2 SAME POSition AS 103 EXPAND MAXimum DURation 4000S MINimum DURation 2600S Comments:SEE COMMENTS FOR 101,103 Exposure_Number:106 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F673N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2700S Special_Requirements: ! Section 7.2 SAME POSition AS 103 EXPAND MAXimum DURation 4000S MINimum DURation 2600S Comments:SEE COMMENTS FOR 101,103 Exposure_Number:107 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F673N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2700S Special_Requirements: ! Section 7.2 SAME POSition AS 101 EXPAND MAXimum DURation 4000S MINimum DURation 2600S Comments:SEE COMMENTS FOR 101 Exposure_Number:108 ! Section 6.5 Target_Name:HH29 Config:WFPC2 Opmode:IMAGE Aperture:PC1-FIX Sp_Element:F673N Wavelength: Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:2700S Special_Requirements: ! Section 7.2 SAME POSition AS 101 EXPAND MAXimum DURation 4000S MINimum DURation 2600S Comments:SEE COMMENTS FOR 101 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: ! ! CASA ! Campus Box 389 ! Boulder ! 80309 ! ! 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