1. Debris Disk Imaging with HST/NICMOS: The GO/10177 Debris Disk Survey Part 2: The Resolved Disks GLENN SCHNEIDER NICMOS Project Steward Observatory 933 N. Cherry Avenue University of Arizona Tucson, Arizona 85721 Phone: 520-621-5865 FAX: 520-621-1891 e-mail: gschneider@as.arizona.edu http://nicmosis.as.arizona.edu:8000/ Glenn Schneider Steward Observatory, University of Arizona

2. Murray Silverstone Steward Observatory, University of Arizona Debris Disk Imaging with HST/NICMOS: The GO/10177 Debris Disk Survey Part 1: Targets, Technique and Limits - Target Selection - Sample Properties - Data Reduction - Upper Limits for Non-Detections See Poster - Observing Strategy

3. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) Program Goals: - Provide critically needed high resolution scattered-light imagery of protoplanetary and debris disks to assist in discriminating between proposed evolutionary scenarios in the epochs of planet-building. - Provide a legacy of cataloged morphologies for interpreting mid- and far-IR SEDs (e.g., Spitzer) and reliable, spatially resolved, photometry and flux density limits (for non-detections).

4. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) Scattered-light imagery of CS disks directly provides: - Spatial distribution of the constituent grains, which cannot be uniquely inferred from (longer- ) SEDs alone. - Constraints to break degeneracies in disk geometries and compositions in SED models of CS disks. Spatially resolved images and SEDs of CS disks, together, inform on their global structures and on the distribution and physical properties of the CS grains. (e.g., Schneider et al 2003, AJ, 125, 1467).

5. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) Disk Structures & Disk/Planet Interactions Asymmetries (e.g., warps, gaps, arc, spirals, rings, axial anisotropies, etc.) in the spatial distributions of dusty debris in evolved disks provide evidence for unseen co- orbital planetary-mass companions through their dynamical interactions with the disk grains.

6. NICMOS 1.1  m GO/10177 NICMOS Coronagraphic Imaging Survey Why NICMOS? - Probe material as close as r = 0.3”. - Probe material as close as r = 0.3”. (ACS inner working angle > 0.9”). (ACS inner working angle > 0.9”). - Sensitive to circumstellar material - Sensitive to circumstellar material with disks of scattering fractions with disks of scattering fractions of a few x 10 -5 of total starlight at 1”. of a few x 10 -5 of total starlight at 1”. (Similar to ACS at larger radii). (Similar to ACS at larger radii). - ~ 0.1” spatial resolution 1.1  m. - ~ 0.1” spatial resolution 1.1  m. (ACS ~2x better @ 0.6  m) (ACS ~2x better @ 0.6  m) 1216s

7. GO/10177 NICMOS Coronagraphic Imaging Survey Why NICMOS? ACS 0.6  m - Probe material as close as r = 0.3”. - Probe material as close as r = 0.3”. (ACS inner working angle > 0.9”). (ACS inner working angle > 0.9”). - Sensitive to circumstellar material - Sensitive to circumstellar material with disks of scattering fractions with disks of scattering fractions of a few x 10 -5 of total starlight at 1”. of a few x 10 -5 of total starlight at 1”. (Similar to ACS at larger radii). (Similar to ACS at larger radii). - ~ 0.1” spatial resolution 1.1  m. - ~ 0.1” spatial resolution 1.1  m. (ACS ~2x better @ 0.6  m) (ACS ~2x better @ 0.6  m) 4910s STIS STIS, no longer functional :-( STIS, no longer functional :-(

8. GO/10177 NICMOS Coronagraphic Imaging Survey Why NICMOS? ACS 0.6  m - Probe material as close as r = 0.3”. - Probe material as close as r = 0.3”. (ACS inner working angle > 0.9”). (ACS inner working angle > 0.9”). - Sensitive to circumstellar material - Sensitive to circumstellar material with disks of scattering fractions with disks of scattering fractions of a few x 10 -5 of total starlight at 1”. of a few x 10 -5 of total starlight at 1”. (Similar to ACS at larger radii). (Similar to ACS at larger radii). - ~ 0.1” spatial resolution 1.1  m. - ~ 0.1” spatial resolution 1.1  m. (ACS ~2x better @ 0.6  m) (ACS ~2x better @ 0.6  m) 4910s

9. GO/10177 NICMOS Coronagraphic Imaging Survey Why NICMOS? ACS 0.6  m 4910s - Probe material as close as r = 0.3”. - Probe material as close as r = 0.3”. (ACS inner working angle > 0.9”). (ACS inner working angle > 0.9”). - Sensitive to circumstellar material - Sensitive to circumstellar material with disks of scattering fractions with disks of scattering fractions of a few x 10 -5 of total starlight at 1”. of a few x 10 -5 of total starlight at 1”. (Similar to ACS at larger radii). (Similar to ACS at larger radii). - ~ 0.1” spatial resolution 1.1  m. - ~ 0.1” spatial resolution 1.1  m. (ACS ~2x better @ 0.6  m) (ACS ~2x better @ 0.6  m)

10. GO/10177 NICMOS Coronagraphic Imaging Survey Why NICMOS? ACS 0.6  m 4910s - Capable of imaging young EGP’s of ~ 2 M jup in optically thin (e.g., debris) disks at > 1”. in optically thin (e.g., debris) disks at > 1”. - Probe material as close as r = 0.3”. - Probe material as close as r = 0.3”. (ACS inner working angle > 0.9”). (ACS inner working angle > 0.9”). - Sensitive to circumstellar material - Sensitive to circumstellar material with disks of scattering fractions with disks of scattering fractions of a few x 10 -5 of total starlight at 1”. of a few x 10 -5 of total starlight at 1”. (Similar to ACS at larger radii). (Similar to ACS at larger radii). - ~ 0.1” spatial resolution 1.1  m. - ~ 0.1” spatial resolution 1.1  m. (ACS ~2x better @ 0.6  m) (ACS ~2x better @ 0.6  m)

11. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 “YSO” Disk Candidates < 10 Myr (Optically Thick) Many with Gas (+Dust) 18 T Tau Stars (d < 150 pc) Spectra Types: G-M Spectra Types: G-M mm Continuum Excesses mm Continuum Excesses and/or and/or High Optical Polarization High Optical Polarization 4 Herbig AeBes (d < 200 pc) 8 A-F Stars FIR or mm excess >> photosphere FIR or mm excess >> photosphere ~ 1/3 HST Optical Detections 2 Ground-Based NIR Detections A few Examples…

12. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 “YSO” Disk Candidates < 10 Myr (Optically Thick) Many with Gas (+Dust) 18 T Tau Stars (d < 150 pc) Spectra Types: G-M Spectra Types: G-M mm Continuum Excesses mm Continuum Excesses and/or and/or High Optical Polarization High Optical Polarization 4 Herbig AeBes (d < 200 pc) 8 A-F Stars FIR or mm excess >> photosphere FIR or mm excess >> photosphere ~ 1/3 HST Optical Detections 2 Ground-Based NIR Detections K5, H = 9.8) DM Tauri (K5, H = 9.8) ring @ 240AU, “dark” to ~ 180AU, shadowing(?) @ PA = 95d Peak 1.6  m S.B = 17  Jy/sq. arcsec

13. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 “YSO” Disk Candidates < 10 Myr (Optically Thick) Many with Gas (+Dust) 18 T Tau Stars (d < 150 pc) Spectra Types: G-M Spectra Types: G-M mm Continuum Excesses mm Continuum Excesses and/or and/or High Optical Polarization High Optical Polarization 4 Herbig AeBes (d < 200 pc) 8 A-F Stars FIR or mm excess >> photosphere FIR or mm excess >> photosphere ~ 1/3 HST Optical Detections 2 Ground-Based NIR Detections K5, H = 9.8) GO Tauri (K5, H = 9.8) r ~ 540 AU, dark zone to ~ 290 AU ring-like, strong minor axis asymmetry striated structures “above” midplane

14. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 “YSO” Disk Candidates < 10 Myr (Optically Thick) Many with Gas (+Dust) 18 T Tau Stars (d < 150 pc) Spectra Types: G-M Spectra Types: G-M mm Continuum Excesses mm Continuum Excesses and/or and/or High Optical Polarization High Optical Polarization 4 Herbig AeBes (d < 200 pc) 8 A-F Stars FIR or mm excess >> photosphere FIR or mm excess >> photosphere ~ 1/3 HST Optical Detections 2 Ground-Based NIR Detections K7, H = 8.4; ROXR1 23) Do Ar 25 (K7, H = 8.4; ROXR1 23) r ~ 380 AU (2.7”) Morphologically similar to GM Aur dark mid-plane ~ 0.7” from star In  Oph star forming region

15. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 “YSO” Disk Candidates < 10 Myr (Optically Thick) Many with Gas (+Dust) 18 T Tau Stars (d < 150 pc) Spectra Types: G-M Spectra Types: G-M mm Continuum Excesses mm Continuum Excesses and/or and/or High Optical Polarization High Optical Polarization 4 Herbig AeBes (d < 200 pc) 8 A-F Stars FIR or mm excess >> photosphere FIR or mm excess >> photosphere ~ 1/3 HST Optical Detections 2 Ground-Based NIR Detections SZ-82 (IM Lup; M0, H = 8.1) Weak Lined T Tauri Star r = 4.3” (~ 600 AU) Morphology Similar to GM Aur

16. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 “YSO” Disk Candidates < 10 Myr (Optically Thick) Many with Gas (+Dust) 18 T Tau Stars (d < 150 pc) Spectra Types: G-M Spectra Types: G-M mm Continuum Excesses mm Continuum Excesses and/or and/or High Optical Polarization High Optical Polarization 4 Herbig AeBes (d < 200 pc) 8 A-F Stars FIR or mm excess >> photosphere FIR or mm excess >> photosphere ~ 1/3 HST Optical Detections 2 Ground-Based NIR Detections DL Tau (GVe:, H = 8.68) r ~ 420AU (3.5”), Face-On Disk CO disk with r ~ 3.7” (48 NIC3 pix) Jet seen in optical (STIS) Surface Brightness ~ r -2.6

17. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 Debris Disk Candidates > 10 Myr (Optically Thin) Likely Dust Dominated Spectral Types: A0 - K2 Main Sequence Stars IRAS FIR Excesses: L 25+60 mm / L * > 3 x 10 -4 L 25+60 mm / L * > 3 x 10 -4 unconfused by background unconfused by background nebulosity @ b > 10 nebulosity @ b > 10° None Previously Imaged

18. GO/10177 NICMOS Coronagraphic Imaging Survey 52 Targets (+ 5 Calibration Orbits) 26 Debris Disk Candidates > 10 Myr (Optically Thin) Likely Dust Dominated Spectral Types: A0 - K2 Main Sequence Stars IRAS FIR Excesses: L 25+60 mm / L * > 3 x 10 -4 L 25+60 mm / L * > 3 x 10 -4 unconfused by background unconfused by background nebulosity @ b > 10 nebulosity @ b > 10° None Previously Imaged 1. Significant 60  m excess 2. Estimate T dust and R disk from 25/60 & 60/100  m color excess 25/60 & 60/100  m color excess 3. Assume small grains with 1.1  m albedos ~ 0.2-0.5 so (f scat /f * ) albedos ~ 0.2-0.5 so (f scat /f * ) comparable to absorbed starlight comparable to absorbed starlight 4. f scat /f * instrumentally detectable 5. Disk radii likely > 0.3” 6. Distance < 150 pc 7. Surface brightness sufficiently high to detect in 1 HST orbit high to detect in 1 HST orbit

19. 0 -2 -3 -4 -5 -6 Log Fractional IR Excess / arcsec 2 0.1 1 10 Log Radius (Arcseconds) DEBRIS DISK CANDIDATE SELECTION HD 32297 Anon. F5 HD 107146 HD 92945 OBSCURED BY CORONAGRAPH NICMOS 1.1  m: 1300s ACS 0.8  m: 7800s ACS 0.8  m: 7800s

20. -Spectral Type: A0 -Distance: 112 12 pc -Distance: 112 ± 12 pc -J=7.69, H=7.62, K=7.59 (2MASS) -L 25+60  m /L * ~ 0.27% (IRAS FSC) 12(Jy) 25(Jy) 60(Jy) 100(Jy) 870*(mJy) <0.14 0.2110.034 1.1220.067 <1.60 5.66.8 12(Jy) 25(Jy) 60(Jy) 100(Jy) 870*(mJy) <0.14 0.211±0.034 1.122±0.067 <1.60 5.6±6.8 -Age: Uncertain, but… HD 32297 * Silverstone, et al. 2004

21. HD 32297 Low Luminosity for its B-V Color Similar to Young A-stars at the Bottom Locus of the V vs. B-V C-M Diagram

22. F110W Coronagraphic Imaging Difference Image HD 32297 672s Integrations 29.9 deg  Orientation ORIENTATION 2 ORIENATION 1

23. F110W Coronagraphic Imaging Difference Image HD 32297 672s Integrations REFERENCE PSF ORIENATION 1

24. F110W Coronagraphic Imaging REFERENCE PSF ORIENATION 2 Difference Image HD 32297 672s Integrations

25. HD 32297 Near Edge-On (“  Pic-like”) Disk N E Inclination = 10.52.5, P.A. = 227.51 Inclination = 10.5° ± 2.5°, P.A. = 227.5° ± 1° Extent*: > 3.3” (400 AU) to NE; > 2.5” to SW *3  per resolution element lower limits *3  per resolution element lower limits

26. HD 32297 Near Edge-On (“  Pic-like”) Disk N E 1.1  m Disk Flux Density: 4.81 0.57 mJy (r > 0.3”) 1.1  m Disk Flux Density: 4.81 ± 0.57 mJy (r > 0.3”) Scattering Fraction: 0.33% 0.04% (r > 0.3”) Scattering Fraction: 0.33% ± 0.04% (r > 0.3”) “Above”: 56% 12%, “Below”: 44 12% “Above”: 56% ± 12%, “Below”: 44 ± 12% But…

27. HD 32297 AU MIC GO/10177 GO/10228 P.I.: Kalas “The {AU Mic} disk is... has a thin midplane… Within 50 AU {5”} the midplane is straight and aligned with the star, and beyond that it deviates by 3 deg, resulting in a bowed appearance…” --Krist et al 2004 AU MIC/ACS E F606W (PSF Subtracted) 9"

28. HD 32297 Radial Surface Brightness Profile DISK ASYMMETRIES SW(r>0.3”) = 3.14 0.57mJy SW(r>0.3”) = 3.14 ± 0.57mJy NE(r>0.3”) = 1.67 0.57mJy NE(r>0.3”) = 1.67 ± 0.57mJy Symmetric: 0.5” < r < 1.7” SW Brighter @ r < 0.6” NE Brighter @ r > 2.4” SB(SW;r>0.5”) =0.455 r -3.57 NW(SB;0.5”<r<1.7”) =0.51r -3.7 NW(SB;1.7”<r<3.4”) =0.27r -2.7 S.B. in mJy/sq. arcsecond S.B. in mJy/sq. arcsecond SW NE SB ~ r -3.72 SB ~ r -2.74 SB ~ r -3.57

29. -Spectral Type: G2V (solar analog) -Distance: 28.5 0.7pc -Distance: 28.5 ± 0.7pc -J=5.87, H=5.61, K=5.54 (2MASS) -L 60+100  m /L * ~ 0.10% (IRAS FSC) 12(Jy) 25(Jy) 60(Jy) 100(Jy) 870*(mJy) 0.2590.031 <0.135 0.7050.056 0.9100.155 34.210.0 12(Jy) 25(Jy) 60(Jy) 100(Jy) 870*(mJy) 0.259±0.031 <0.135 0.705±0.056 0.910±0.155 34.2±10.0 -Age: 30 - 250 Myr (Williams et al, 2004) -Also Observed With ACS (Ardila et al, 2004) HD 107146 * Silverstone, et al. 2004

30. HD 107146 2-roll combined PSF subtracted coronagraphy *“Within 2” from the star, the {ACS} image is dominated by PSF subtraction residuals”. - Ardila 2004 Broad outer ring R = 170 AU (6.0”)  peak @ ~ 115 AU (4.0”) ACS*: f 0.6  m = 6.8 +/- 0.8 x 10 -5 f 0.6  m = 6.8 +/- 0.8 x 10 -5 f 0.8  m = 1.0 +/- 0.1 x 10 -4 f 0.8  m = 1.0 +/- 0.1 x 10 -4NICMOS: f 1.1  m = 1.4 +/- 0.2 x 10 -4 f 1.1  m = 1.4 +/- 0.2 x 10 -4 Disk Flux Density (1.1  m) = 68 10  Jy (r>0.3”) = 68 ± 10  Jy (r>0.3”)

31. HD 107146 01234567 0.1 1 10 100 1000 Radial Distance (arcsec) S. B. (microJy / sq. arcsecond) 6” Undetected by NICMOS Undetected by ACS

32. HD 107146

33. STAR: Spectral Type: F5  Pic Moving Group Age: ~ 12 Myr Distance: 50 pc L 25+60  m /L * ~ 0.2% ANOTHER NEW DISK

34. OBSERVATION: -F110W (1.1  m) -NIC2 Coronagraph -Two-Orientation -PSF-Subtraction-Recombination

35. ANOTHER NEW DISK MODEL (best fit): -Inclined Ring -Intrinsic Symmetry -I(r)/I * ~ r -2 -SB(  ) ~ H-G( ,g) -SB(r) ~ SB(r peak ) e -1 -PSF Convolution

36. ANOTHER NEW DISK “Smoothed” Observation Elliptical low-pass filter (preserve radial ) (preserve radial ) 9 “Rotation” kernal ± 9 ° “Rotation” kernal (i = 31.7 (i = 31.7 °) Gaussian Weighting

37. ANOTHER NEW DISK OBSERVATION: -F110W (1.1  m) -NIC2 Coronagraph -Two-Orientation -PSF-Subtraction-Recombination

38. ANOTHER NEW DISK RESIDUALS: Observation - Model Diffuse Halo (Currently not in model)

39. ANOTHER NEW DISK RESIDUALS: Observation - Model Diffuse Halo (Currently not in model)

40. ANOTHER NEW DISK RESIDUALS: Observation - Model Diffuse Halo (Currently not in model) ACS Courtesy of J. Krist & ACS/GTO Disk Team

41. ANOTHER NEW DISK RESIDUALS: Observation - Model Diffuse Halo (Currently not in model) NICMOS + ACS

42. ANOTHER NEW DISK Steeply Truncated Inner Radius (r = 86 AU, r inner = 61AU) “Similar” to HR 4796A (r =70 AU, r inner = 62.5AU)

43. ANOTHER NEW DISK Axial & Median S. B. Profiles Bilaterally Symmetric Ring + Diffuse Outer Halo Ring Radius = 1.706”+/-0.023” = 86.3 ± 3.7 AU 70% of scattered starlight in 36 AU wide annulus F disk /F * = 0.17 ± 0.015% Flux Density: 9.6 ± 0.8 mJy (1.2”< r <5.0”) Surface Brightness (mJy/sq.”): Peak(r=86AU) 1.75 ± 0.14

44. ANOTHER NEW DISK Bilaterally Symmetric Ring + Diffuse Outer Halo Ring Radius = 1.706”+/-0.023” = 86.3 ± 3.7 AU 70% of scattered starlight in 36 AU wide annulus F disk /F * = 0.17 ± 0.015% Flux Density: 9.6 ± 0.8 mJy (1.2”< r <5.0”) Surface Brightness (mJy/sq.”): Peak(r=86AU) 1.75 ± 0.14 Directionally Pref. Scattering: g(H-G) ~ 0.3 I = 31.7° ± 1.6° No Photocentric Offset Deprojection, Major Axis Horizontal

45. New F-star Disk Is the Morphology More Like: HD 141569A HD 107146

46. Debris Rings - Angular Scales Angular scale: r(Fomalhaut) = 19”

47. AU Mic  Pic HD 32297 HR 4796 F-Star HD 141569 HD 107146  PscA M0A5A0 F5 HAeBe B9.5 G2A3 12-20 < 10 ?812530-250200 210~1600> 4007086400170140 0.0030.00330.00240.00170.00251.4 x 10 -4 10 -6 0.00040.00150.00270.0050.0020.00840.0015x10 -6 Wing Tilt many S.B. W. Tilt Azim. No, g ~ 0.3 Yes…No. Offset, g ~ 0.3 Assym L ir /L * F nir >0.3” r AU Myr Spec Image Star

48. Glenn Schneider Steward Observatory, University of Arizona (NICMOS/IDT) Debris Disk Imaging with HST/NICMOS: The GO/10177 Debris Disk Survey Part 2: The Resolved Disks GLENN SCHNEIDER NICMOS Project Steward Observatory 933 N. Cherry Avenue University of Arizona Tucson, Arizona 85721 Phone: 520-621-5865 FAX: 520-621-1891 e-mail: gschneider@as.arizona.edu http://nicmosis.as.arizona.edu:8000/