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 Phone: FAX: Glenn Schneider Steward Observatory, University of Arizona

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

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).

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).

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.

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 of total starlight at 1”. of a few x 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 0.6  m) (ACS ~2x 0.6  m) 1216s

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 of total starlight at 1”. of a few x 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 0.6  m) (ACS ~2x 0.6  m) 4910s STIS STIS, no longer functional :-( STIS, no longer functional :-(

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 of total starlight at 1”. of a few x 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 0.6  m) (ACS ~2x 0.6  m) 4910s

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 of total starlight at 1”. of a few x 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 0.6  m) (ACS ~2x 0.6  m)

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 of total starlight at 1”. of a few x 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 0.6  m) (ACS ~2x 0.6  m)

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…

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) 240AU, “dark” to ~ 180AU, PA = 95d Peak 1.6  m S.B = 17  Jy/sq. arcsec

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

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

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

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

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 mm / L * > 3 x L mm / L * > 3 x unconfused by background unconfused by background b > 10 b > 10° None Previously Imaged

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 mm / L * > 3 x L mm / L * > 3 x unconfused by background unconfused by background b > 10 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 ~ so (f scat /f * ) albedos ~ 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

Log Fractional IR Excess / arcsec Log Radius (Arcseconds) DEBRIS DISK CANDIDATE SELECTION HD Anon. F5 HD HD OBSCURED BY CORONAGRAPH NICMOS 1.1  m: 1300s ACS 0.8  m: 7800s ACS 0.8  m: 7800s

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

HD 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

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

F110W Coronagraphic Imaging Difference Image HD s Integrations REFERENCE PSF ORIENATION 1

F110W Coronagraphic Imaging REFERENCE PSF ORIENATION 2 Difference Image HD s Integrations

HD Near Edge-On (“  Pic-like”) Disk N E Inclination = , P.A. = 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

HD Near Edge-On (“  Pic-like”) Disk N E 1.1  m Disk Flux Density: 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…

HD 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"

HD Radial Surface Brightness Profile DISK ASYMMETRIES SW(r>0.3”) = mJy SW(r>0.3”) = 3.14 ± 0.57mJy NE(r>0.3”) = mJy NE(r>0.3”) = 1.67 ± 0.57mJy Symmetric: 0.5” < r < 1.7” SW r < 0.6” NE r > 2.4” SB(SW;r>0.5”) =0.455 r 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 SB ~ r SB ~ r -3.57

-Spectral Type: G2V (solar analog) -Distance: pc -Distance: 28.5 ± 0.7pc -J=5.87, H=5.61, K=5.54 (2MASS) -L  m /L * ~ 0.10% (IRAS FSC) 12(Jy) 25(Jy) 60(Jy) 100(Jy) 870*(mJy) < (Jy) 25(Jy) 60(Jy) 100(Jy) 870*(mJy) 0.259±0.031 < ± ± ±10.0 -Age: Myr (Williams et al, 2004) -Also Observed With ACS (Ardila et al, 2004) HD * Silverstone, et al. 2004

HD 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”)  ~ 115 AU (4.0”) ACS*: f 0.6  m = 6.8 +/- 0.8 x f 0.6  m = 6.8 +/- 0.8 x f 0.8  m = 1.0 +/- 0.1 x f 0.8  m = 1.0 +/- 0.1 x 10 -4NICMOS: f 1.1  m = 1.4 +/- 0.2 x f 1.1  m = 1.4 +/- 0.2 x Disk Flux Density (1.1  m) =  Jy (r>0.3”) = 68 ± 10  Jy (r>0.3”)

HD Radial Distance (arcsec) S. B. (microJy / sq. arcsecond) 6” Undetected by NICMOS Undetected by ACS

HD

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

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

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

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

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

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

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

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

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

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

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

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

New F-star Disk Is the Morphology More Like: HD A HD

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

AU Mic  Pic HD HR 4796 F-Star HD HD  PscA M0A5A0 F5 HAeBe B9.5 G2A < 10 ? ~1600> x x10 -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

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 Phone: FAX: