! Proposal 6693, submission 1 ! PI: Antonella Nota ! Received Wed Feb 21 16:10:58 EST 1996 ! From: nota@stsci.edu ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6693,v 9.1 1997/06/19 19:59:30 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6693,v 9.1 1997/06/19 19:59:30 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: van Orsow ! Phone: 410-338-4568 , E-mail: vanorsow@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0776.nota.prop ! Date generated: Fri Dec 22 18:57:55 EST 1995 ! Proposal_Information ! Section 4 Title: Circumstellar Nebulae as Fossil Records of the Mass Loss History in Luminous Blue Variables Proposal_Category: GO Scientific_Category: HOT STARS Cycle: 6 Investigators PI_name: Antonella Nota PI_Institution: Space Telescope Science Institute CoI_Name: Mark Clampin CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Guillermo Garcia-Segura CoI_Institution: Instituto de Astronom'\i a-UNAM Contact: ! Y or N (designate at most one contact) CoI_Name: Norbert Langer CoI_Institution: Max Planck Institut, Munich Contact: ! Y or N (designate at most one contact) CoI_Name: Claus Leitherer CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Mario Livio CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Anna Pasquali CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Regina Schulte-Ladbeck CoI_Institution: University of Pittsburgh Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to exploit the unique spatial resolution of HST to perform a detailed imaging study of three nebulae around Galactic Luminous Blue Variables, selected on the basis of their different morphologies and physical characteristics. The observations will be performed in selected lines and in the continuum, in order to derive a complete picture of the ionized gas and dust distribution within the nebulae, at the same high resolution. Extensive ground based coronographic observations of these nebulae suggest that an interacting wind scenario can explain most of the morphologies observed, both on large and small spatial scales. We want to compare the high resolution HST images with the predictions of multidimensional, hydrodynamical models to quantitatively establish 1) the wind velocity and mass loss properties of the pre outburst phase, and 2) the duration of the pre outburst phase. The large scale nebular structure will provide information on the LBV outburst mechanism and related intervening factors (rotation, binarity). The small scale features will provide information on the local instabilities, such as anisotropies of the wind. An experiment conducted on recent HST images of the galactic LBV AG Carinae has proven the method is effective and has demonstrated its potential as a diagnostic tool, to empirically investigate the mass loss history and, thereby, the evolutionary history of the central star. Questions ! Free format text (please update) Observing_Description: We propose to use the PC to obtain high spatial resolution images of the circumstellar nebulae around three galactic Luminous Blue Variables, with the objective of characterizing both their large and small scale structure. The need for the PC is justified by several reasons: 1) the high angular resolution (0.046''/pixel) of the Point Spread Function, 2) the relatively large field of view (35''*35''); 3) the good spectral response at the red wavelengths of interest; 4) the suitability of the CCD cameras for observations requiring high dynamic range, as WFPC2 CCDs have MPP architecture (see WFPC2 Handbook, 1995), and, therefore, limited blooming on saturated stars. , For each of the three nebulae, we will take PC images in the following filters: 547M - V Continuum, F656N - HAlpha, F658N - NII. Our observational strategy is to obtain two images of each object/filter combination, to properly correct for cosmic rays. The exposure time for each of the two images has been calculated in order to achieve a S/N of 10 in the nebular region, while saturating the central object. On the basis of the WWW WFPC2 exposure time estimator and the WFPC2 handbook, using the PC camera and the F547M filter for a star with V = 7 and surface brightness in the nebula of ~eq 18 magnitudes/square arcsecs, two exposures of 300 secs, for each filter, will achieve a S/N per pixel of 10. For the HAlpha emission, assuming a typical line flux of 6times10^-14 ergs/sec/cm^2/arcsec^2, we derive a S/N per pixel of 10 for two 400 sec exposures. The NII emission is comparable to HAlpha and therefore a similar exposure time will be used, with a total of 36 minutes for each target. Including the Guide Star Acquisitions and the exposure overheads, the complete set of observations for each target requires approximately one orbit. We are aware that the bright central stars will saturate columns contained within a radius of approximately 0.3 arcsecs. For all exposures we will operate the CCDs with the serial clocks running in order to remove excess charge from saturated columns and prevent charge spreading to adjacent columns. This strategy has already proven successful, allowing us to obtain the excellent image of AG Carinae that is shown in Figure 1. In addition, we are interested in the nebular features as close as possible to the central star, and therefore, we request to repeat the observation sequence for each target a second time, after at least two months, in order to apply a roll deconvolution technique. After two months or more the spacrecraft, and therefore the Point Spread Function, will be rotated by at least 60 degrees with respect to the sky and to the object observed. This technique will allow us to distinguish PSF artifacts from nebular features in the region 1-5'' from the central star, where we cannot observe from the ground. The total time required amounts therefore to 6 orbits. Real_Time_Justification: The two sets of observations must be spaced in time by at least 2 months in order to allow a roll difference of 60 degrees or more. No supporting observations will be needed for this program. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: HD168625 Alternate_Names: HEN3-1681,SAO161375,HILT756 Description: STAR,EMISSION LINE STAR,LUMINOUS BLUE VARIABLE Position: RA=18H 21M 19.69S +/- 0.5S, DEC=-16D 22' 26.5" +/- 0.5", PLATE-ID=064B Equinox: J2000 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=8.41,B-V=+1.46 Target_Number: 2 Target_Name: HR-CARINAE Alternate_Names: HD90177,SAO238005,IRAS10211-5922 Description: STAR,EMISSION LINE STAR,LUMINOUS BLUE VARIABLE Position: RA=10H 22M 54.19S +/- 0.5S, DEC=-59D 37' 28.3"+/- 0.5", PLATE-ID=0686 Equinox: J2000 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=8.55,B-V=+0.88 ! Include at least V and B-V Visit_Number:1 Visit_Requirements: Exposure_Number:100 Target_Name:HD168625 Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F547M Optional_Parameters:CLOCKS=YES ATD-GAIN=15 Number_of_Iterations:2 Time_Per_Exposure:200S Exposure_Number:101 Target_Name:HD168625 Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F656N Optional_Parameters:CLOCKS=YES ATD-GAIN=15 Number_of_Iterations:3 Time_Per_Exposure:500S Visit_Number:2 Visit_Requirements:AFTER 1 BY 66D TO 73D Exposure_Number:200 Target_Name:HD168625 Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F547M Optional_Parameters:CLOCKS=YES ATD-GAIN=15 Number_of_Iterations:2 Time_Per_Exposure:200S Exposure_Number:201 Target_Name:HD168625 Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F656N Optional_Parameters:CLOCKS=YES ATD-GAIN=15 Number_of_Iterations:3 Time_Per_Exposure:500S Visit_Number:3 Visit_Requirements:ORIENT 180D TO 180D Exposure_Number:302 Target_Name:HR-CARINAE Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F547M Optional_Parameters:CLOCKS=YES Number_of_Iterations:2 Time_Per_Exposure:120S Exposure_Number:303 Target_Name:HR-CARINAE Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F656N Optional_Parameters:CLOCKS=YES Number_of_Iterations:3 Time_Per_Exposure:600S Visit_Number:4 Visit_Requirements: Exposure_Number:402 Target_Name:HR-CARINAE Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F547M Optional_Parameters:CLOCKS=YES ATD-GAIN=15 Number_of_Iterations:2 Time_Per_Exposure:120S Exposure_Number:403 Target_Name:HR-CARINAE Config:WFPC2 Opmode:Image Aperture:PC1 Sp_Element:F656N Optional_Parameters:CLOCKS=YES ATD-GAIN=15 Number_of_Iterations:3 Time_Per_Exposure:600S Data_Distribution ! 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