1. Replaced PC polarizer exposures with WC polarizer exposures, changed filters, as per comments from STScI.
2. Changed coronagraph images to repeated sets of MULTIACCUM as per Glenn Schneider. Slightly changed
sampling mode for NIC1 POL noncoronagraphic data.
3. Added a manul dithering sequence to the non-coronagraphic NICMOS data. ----- Attempting Submission 3 (Tue Jun 12 20:25:55 GMT 2007) -----
----- Attempting Submission 4 (Thu Jun 14 20:49:58 GMT 2007) -----
----- Attempting Submission 5 (Fri Jun 15 18:40:04 GMT 2007) -----
Probing the compact dust disk of a nearby Classical T Tauri StarBP Psc is a high Galactic latitude (b = -57), bright, IRAS source that generally has been classified as a T Tauri star but little studied to date. We have carried out a multiwavelength ground-based study of this object and find that it is most likely a ~10 Myr classical T Tauri star surrounded by a gas and dust disk, and less than 100 pc from Earth, making it one of the oldest and closest such stars known. Near-IR AO images and IR photometry show it is surrounded by an compact (0.2"), almost-edge-on, optically thick disk of dust with a wide range of temperatures. We propose a multiwavelength polarimetric study of the compact disk to support quantitative modeling to recover disk and dust parameters. We also propose coronagraphic imaging to search for larger-scale dust structures invisible in ground-based images, and narrowband imaging of an outflow jet and associated Herbig-Haro objects to study their structure and determine a kinematic distance of the system. A massive compact disk surrounding an isolated 10 Myr star is a unique environment for planet formation, and its proximity to Earth allows HST to study it in detail.We will carry out the following observation sequences, designed to probe the circumstellar dust on a variety of scales.
Visit 1 (2 orbits): WFPC2 direct and polarimetric imaging of the inner disk
1a. F555W, four dither positions, two 0.7 and 2 seconds exposures per position, 8 images total
1b. F555W, four dither positions, 10 second exposure per position, 4 images total
1c. WFPC polarimetry in F815W band. 30 second exposures, 2 dither positions each, 6 images total.
1a . Unsaturated images intended to probe the inner disk. These require very short exposure times to avoid saturation. We have estimated these assuming the V=12.2 BP Psc is a point source. Since the source will be extended (~0.1?), the risk of saturation is reduced, but the precise extent at visible wavelengths is unknown and there is also historical evidence for as much as ~1 mag of variability. At large (>0.3?) separations, these short exposures will be read-noise-limited to ~15 mag/square arcsec (2-sigma per 1 pixel box.)
1b. Medium-exposure images. If BP Psc is surrounded by an extended disk similar to that of TW Hya, it would have a brightness of ~16 magnitudes/square arcsec at 60 AU (0.6?), the outer edge of the CO disk. To detect this, we will carry out a similar set of PC exposures but with 10-second integrations. This image set will moderately saturate the central source, but the ORIENT constraints have been set up so the bleeding won't interfere with the disk (which is at a PA of about 60) or the jet (PA=-30). This allows four possible
orientation ranges.
1c. Polarimetry is a powerful technique to detect extended dust envelopes near bright sources. The baseline is to use the polarization quad twice in the PC channel (angles 135 and 15 degrees) and once in WF2 (102 degrees) due to constraints on the WFPC polarization quad. The expected polarization signature is quite strong, so some detection should be possible, though we expect the NICMOS data below to be more precisely calibrated. These images will also be moderately saturated. In addition, a
small amount of unused time at the end is filled in with H-alpha observations.
This uses two orbits - in the original proposal we had estimated one, so we have
decreased the H-alpha observations in Visit 2 from 2 to 1 orbit.
Visit 3 and 4: NICMOS polarimetry of the extended envelope
3a&4a. NICMOS NIC1 polarimetry (using the POL0S, POL60S, POL120S filters) in MULTIACCUM mode to probe the polarization at separations that will be near the edge of the coronagraph occultor.
3b&4b. NICMOS NIC2 deep coronagraphic polarimetry through the POL0L, POL60L, and POL120L filters.
The NICMOS PSF has a broader core than our ground-based AO PSF, but significantly lower ?wings? and much better stability for PSF subtraction. NICMOS polarimetry will provide a quantitative probe of circumstellar dust on larger scales, determining the the star is surrounded by a diffuse disk similar to that of TW Hydrae. In the NIC1 exposures, a TW Hya-like disk would have an SNR of ~8 per pixel at small separations. The deeper coronagraphic set will have SNR=6 per pixel per polarization for a similar disk out to 1.5? (~120 AU). Orbit 3 repeats the same sequence with a change in orientation.
Visit 5: NICMOS PSF star TYC 5243-157-1
5. Same sequence as above.
TYC 5244-226-1is a PSF star, K=8.8, matching BP PSC?s colors that has been determined to be single using Keck AO observations.
Visit 2: deep H-alpha observations
2. F658N, WF and PC cameras. Four dither positions of 400 sec per position.
(original proposal called for two orbits of this mode.)
Total of 1600seconds of integration, sufficient to give SNR=0.5 per pixel on the dimmest visible portion of the jet. This will be offset from BP Psc to center on the brightest portion of the jet. Orientation selected so the jet runs along the diagonal from PC into the rest
of the WFC. Resolution will be vastly better than any available visible-light wide-field imagery from the ground, allowing the kinematic distance measurements to be completed in 1-2 years.ISM AND CIRCUMSTELLAR MATTER12false0.0falsefalsefalsefalsefalsefalseSUPPORTEDSTART TAURI STARPRE-MAIN SEQUENCE STARPROTOPLANETARY DISKThis object was generated by the targetselector and retrieved from the SIMBAD database.
RA and DEC PM come from Tycho 2; object also known as TYC5244-148-1TYC5244-148-1J200023 22 24.6900-02 13 41.40J2000STARK V-IVPSF reference star. PM 10 mas/yearJ200023 20 38.7000-02 26 42.60J2000ISMJETKNOTHERBIG-HARO OBJECT00 00 0.0000+00 00 0.00J2000WFPC2ImagingNoF555WWFPC2ImagingYesF814WNIC2ImagingYesYesNIC1ImagingNoYesNIC2ImagingYesYesWFPC2ImagingNoF656NPOS-TARGDITHER0.559017Standarf WFPC2 dither to enhance resolutionLINE0.559017falsefalse143.130096426.56505WFPC2-BOX1falsePOS-TARGDITHER0.3535LINEfalsefalse245WFPC2-LINE2falseC:\Documents and Settings\macintosh1\Local Settings\Temp\OPVisit22135.xml
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true20C:\Documents and Settings\macintosh1\Local Settings\Temp\OPVisit41160.xmlPolarization at 15 degreesC:\Documents and Settings\macintosh1\Local Settings\Temp\OPVisit22136.xmlDeep H-alpha exposures
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