The Stars and Edge-on Disks of PDS 144: An Intermediate-Mass Analog of Wide T Tauri Multiple Stars

I've tweaked the acquisition for visit 4 up to 100s, and auto-adjusted the exposures to fit within the orbit allocation. I'm getting error messages about one of the visits which executed, which makes NO sense, but will try to proceed with submission, since the only changes are to visit 4. ----- Attempting Submission 4 (Wed Apr 28 21:08:44 GMT 2010) ----- ----- Attempting Submission 5 (Mon Dec 13 14:12:26 GMT 2010) ----- I'm getting an error on visit 8, which already executed, and which I didn't modify. The Stars and Edge-on Disks of PDS 144: An Intermediate-Mass Analog of Wide T Tauri Multiple Stars High-Inclination PMS stars are optimally oriented to measure disk size, height, to detect jets, and to directly probe disk composition. Placing these data into evolutionary context requires dates for the systems and measurements of L bol, and extinction. For such stars, X-ray data provide L x, but also N(H) and the total extinction. FUV data measures L UV, and constrains the shape of the extinction curve. Recent studies have suggested that the frequency of Jovian-mass planets is higher for systems with intermediate-mass stars, due to disk mass or composition. While suitable low mass YSOs are well-represented in the Chandra and HST archives, similar data are lacking for higher mass systems. We propose joint Chandra and HST imaging of PDS 144 to fill this gap.

This proposal combines optical and FUV imagery of the Herbig Ae binary system PDS 144. In the optical, we propose obtaining ACS SBC F606W imagery at the same orientation as archival HST data to facilitate jet studies and to establish which stars in the field are co-moving with the PDS 144 binary. The proposed orientation permits inclusion of a weak T Tauri star some 80.8" from the Herbig Ae stars in the ACS WFC field of view. In the FUV, we plan SBC F165LP, F140LP, and F122M imagery. PDS 144N (A0Ve) is viewed at 83 degrees from pole-on; the star is fully occulted to 10 microns (Perrin et al. 2006), and will not be directly observed in the FUV, closely resembling T Tau S A/B. We expect to see a dark lane at the location of the star, together with light scattered from the envelope and fluorescent H2 emission. PDS 144S (A2Ve) is viewed at 70 degrees from pole-on. After PSF subtraction in the visible, we see a dark lane at F555W. We expect that for extinction by small grains (R=3.1 or 4.0), the lane will become more conspicuous at shorter wavelengths. We have estimated the count rate for PDS 144S in two ways: 1) assuming A1V Kurucz spectrum (slightly too early in type) with V=12.8 (historical average) and E(B-V)=0.5, and by comparison with VV Ser (A2Ve, i=70D, similar distance, extinction, etc.). With the first set of assumptions, we expect 10.362 c/s within 0.4" of PDS 144S (assuming the star is directly visible), with a peak pixel count rate of 1.816 c/s at F140LP, and 3.097 c/s within 0.4" and a peak pixel rate of 0.651 c/s at F165LP (ACS ETC 122730 and 122729 respectively). In both cases the peak pixel rate is well below the variable source bright limits. Photometric variability of PDS 144: All Sky Automated Survey data for PDS 144 shows that the binary has typically been within 0.3 in V of 12.8 (see http://www.astrouw.edu.pl/asas/?psect=acvs&page=details&id=154915-2600.9 ). One lone excursion to V=11.69 has been recorded in the last 3000 days of photometry. ASAS fits a nominal period of 930 days to PDS 144 (presumably PDS 144S dominates the variability): the applicable phase of the (thus far non-repeating) optical max corresponds to early April 2010, but our time constraint for the SBC observations (see below) excludes this interval. We therefore expect PDS 144S to be near V=12.8 at the epoch of the SBC observations, presenting no safety issues for SBC observations. VV Ser (SWP 48866) has a faint blue continuum (3E-15 erg/cm/cm/s/A) with superposed H2 emission and no photospheric/stellar activity features visible, similar to our observation of the classical T Tauri star AA Tau (i=75D). The continuum is a factor of 5 fainter than T Tauri N. T Tauri was successfully observed using the ACS SBC in the same imaging modes that we propose using in this study. For both PDS 144 stars, we anticipate that the bulk of signal will be starlight scattered by the circumstellar envelopes, as well as any emisison from the bipolar jets. Jets: The jets from PDS 144 N and S have similar surface brightness to the HH 409 jet associated with HD 163296 in the optical. We anticipate that in the FUV the jet will be predominantly observed in Lyman alpha (F122M), but cannot exclude some molecular hydrogen knots visible in F140LP. At Lyman alpha, HH409A had a flux of 4.7E-13 erg/cm/cm/s/arcsec^2. In 2 ksec, we anticipate 12.4 c/s/arcsec^2, for S/N=7, neglecting extinction. Given the envelope around PDS 144, we expect that the jets will be detectable when they emerge from the envelope in the FUV and not in immediate proximity to the stars. There is a faint star lying between PDS 144N and S. Optical/NIR photometry suggests that it may be a halo K giant, rather than physically associated with PDS 144. However, Goddard Fabry-Perot imagery suggests that there may be a jet component arising in the vicinity of this star. The identification of this object will be addressed by the optical imaging planned in visit 8, and also with B and V imagery planned for the 2nd quarter of 2010 at the Apache Point Observatory 3.5m telescope. Scheduling of the ACS WFC imagery prior to the FUV observations will allow us to refine exposure estimates. We have specified a 75-100 day lag for the SBC observations relative to the WFC imagery. This lag will allow us to evaluate current photometry for the system, identify all jet-driving sources in the field in time to refine plans for the SBC exposures. Chandra expects that PDS 144 may be observed either in early April or in June/July, so it is possible that we will have the X-ray data in hand prior to the SBC observation, providing an additional safety check for the SBC exposures. Bright Object Issues (other than PDS 144S): The BOT flags a source at 15 49 14.1 -26 00 59.6 as O5V. The archival ACS WFC imagery suggest that the object has V-I>1.0, which is inconsistent with this source being an unreddened O star: it is much more likely to be another halo K giant, presenting no safety risks for the SBC exposures. In the event that the F140LP is unavailable, we will obtain shorter wavelength optical/NUV imagery of PDS 144. N/A We require deep PSF imagery at F140LP and F165LP to fully analyze our imagery, and propose the ACS SBC spectrophotometric standard HS 2027+0651 (WD 2027 +068) for this purpose. This star has already been successfully used to calibrate the ACS SBC, and has archival deep PSF data with F122M. These calibration images will not only support our program, but will facilitate analysis of data from programs 11336 and 10489. STAR FORMATION 12 false 40.0 0.0 false false false false false false SUPPORTED STAR A4-A9 V-IV HERBIG AE/BE JET PRE-MAIN SEQUENCE STAR PROTOPLANETARY DISK This object was generated by the targetselector and retrieved from the SIMBAD database. Spectral type for PDS 144S updated. Keck Hires spectra show spectral type for PDS 144S is A4-A5, not the A2 listed on SIMBAD. J2000 15 49 15.4250 -26 00 52.48 J2000 B-V=0.5, TYPE=A2V STAR HERBIG AE/BE No measured proper motion in literature; coordinates duplicate archival ACS imagery of PDS 144 to minimize geometric distortion residuals. J2000 15 49 15.5200 -26 00 50.20 J2000 TYPE=A2V, B-V=0.5 STAR G V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. HD-116956 HIP-65515 J2000 00 00 0.0000 +00 00 0.00 J2000 ACS/SBC Imaging No No F165LP ACS/SBC Imaging No No F140LP ACS/SBC Imaging No No F122M ACS/WFC Imaging No No F606W ACS/SBC Imaging No No F165LP ACS/SBC Imaging No No F140LP POS-TARG DITHER 0.179 LINE 0.116 false false 63.65 4 20.02 ACS-SBC-DITHER-BOX 1

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