Debris Disk Imaging with HST/NICMOS: The GO/10177 Debris Disk Survey Part 2: The Resolved Disks GLENN SCHNEIDER NICMOS Project Steward Observatory 933

GO/10177GO/10177NICMOS Coronagraphic Imaging SurveyNICMOS Coronagraphic Imaging Survey

52 Targets (+ 5 Calibration Orbits)52 Targets (+ 5 Calibration Orbits)Program Goals:Program Goals: - Provide critically needed high resolution scattered-light - Provide critically needed high resolution scattered-light imagery of protoplanetary and debris disks to assist in imagery of protoplanetary and debris disks to assist in discriminating between proposed evolutionary scenarios discriminating between proposed evolutionary scenarios in the epochs of planet-building.in the epochs of planet-building.

- Provide a legacy of cataloged morphologies for - Provide a legacy of cataloged morphologies for interpreting mid- and far-IR SEDs (e.g., Spitzer) and interpreting mid- and far-IR SEDs (e.g., Spitzer) and reliable, spatially resolved, photometry and flux density reliable, spatially resolved, photometry and flux density limits (for non-detections).limits (for non-detections).


52 Targets (+ 5 Calibration Orbits)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).


52 Targets (+ 5 Calibration Orbits)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 1.1NICMOS 1.1mm


Why NICMOS?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 fractionswith disks of scattering fractions of a few x 10of a few x 10-5-5 of total starlight at 1”. of total starlight at 1”. (Similar to ACS at larger radii).(Similar to ACS at larger radii).

- ~ 0.1” spatial resolution 1.1 - ~ 0.1” spatial resolution 1.1 m. m. (ACS ~2x better @ 0.6 (ACS ~2x better @ 0.6 m)m)

1216s1216s


Why NICMOS?Why NICMOS? ACS 0.6ACS 0.6mm

- 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”).



4910s4910s

STISSTIS STIS, no longer functional STIS, no longer functional :-(:-(






4910s4910s



4910s4910s

1"






4910s4910s

- - Capable of imaging young EGP’s of ~ 2 MCapable of imaging young EGP’s of ~ 2 Mjupjup in optically thin (e.g., debris) disks at in optically thin (e.g., debris) disks at >> 1”. 1”.

1"





52 Targets (+ 5 Calibration Orbits)52 Targets (+ 5 Calibration Orbits)26 “YSO” Disk Candidates26 “YSO” Disk Candidates< 10 Myr (Optically Thick)< 10 Myr (Optically Thick)Many with Gas (+Dust) Many with Gas (+Dust) 18 T Tau Stars (d < 150 pc)18 T Tau Stars (d < 150 pc) Spectra Types: G-MSpectra Types: G-M mm Continuum Excessesmm Continuum Excesses and/orand/or High Optical PolarizationHigh Optical Polarization

4 Herbig AeBes (d < 200 pc)4 Herbig AeBes (d < 200 pc)8 A-F Stars 8 A-F Stars FIR or mm excess >> photosphere FIR or mm excess >> photosphere

~ 1/3 HST Optical Detections~ 1/3 HST Optical Detections2 Ground-Based NIR Detections2 Ground-Based NIR Detections

A few Examples…A few Examples…





3.5"

STIS

DM Tauri (K5, H = 9.8)K5, H = 9.8)

ring @ 240AU, “dark” to ~ 180AU, ring @ 240AU, “dark” to ~ 180AU, shadowing(?) @ PA = 95dshadowing(?) @ PA = 95d

Peak 1.6Peak 1.6m S.B = 17 m S.B = 17 Jy/sq. arcsecJy/sq. arcsec





GO Tauri (K5, H = 9.8)K5, H = 9.8)

r ~ 540 AU, dark zone to ~ 290 AUr ~ 540 AU, dark zone to ~ 290 AUring-like, strong minor axis asymmetryring-like, strong minor axis asymmetrystriated structures “above” midplanestriated structures “above” midplane

3.5"

log(10) to3.2 mJy/ sq. arcsec

linear to134 J y/ sq. arcsec





Do Ar 25 (K7, H = 8.4; ROXR1 23)K7, H = 8.4; ROXR1 23)

r ~ 380 AU (2.7”)r ~ 380 AU (2.7”)Morphologically similar to GM AurMorphologically similar to GM Aur

dark mid-plane ~ 0.7” from stardark mid-plane ~ 0.7” from star

3.5"

H =12.43

linear to 5.3 mJy/ sq. arcsec

linear to 0.53 mJy/ sq. arcsec

In

In

Oph

sta

r fo

rmin

g re

gion

Oph

sta

r fo

rmin

g re

gion





SZ-82 (IM Lup; M0, H = 8.1)

Weak Lined T Tauri StarWeak Lined T Tauri Starr = 4.3” (~ 600 AU)r = 4.3” (~ 600 AU)

Morphology Similar to GM AurMorphology Similar to GM Aur





DL Tau (GVe:, H = 8.68)1.6m Radial Surface Brightness Profile

1 ADU/s/pix = 0.267 mJy arcsec-21" = 13.2 pixels

SQRT (0 to 4 ADU/s/pix) display

93 x 93 pixels

r ~ 420AU (3.5”), Face-On Diskr ~ 420AU (3.5”), Face-On DiskCO disk with r ~ 3.7” (48 NIC3 pix)CO disk with r ~ 3.7” (48 NIC3 pix)

Jet seen in optical (STIS)Jet seen in optical (STIS)Surface Brightness ~ r Surface Brightness ~ r -2.6-2.6


52 Targets (+ 5 Calibration Orbits)52 Targets (+ 5 Calibration Orbits)26 Debris Disk Candidates26 Debris Disk Candidates>> 10 Myr (Optically Thin) 10 Myr (Optically Thin)Likely Dust Dominated Likely Dust Dominated Spectral Types: A0 - K2Spectral Types: A0 - K2Main Sequence StarsMain Sequence StarsIRAS FIR Excesses:IRAS FIR Excesses: LL25+60 mm25+60 mm / L / L** > 3 x 10 > 3 x 10-4-4

unconfused by backgroundunconfused by background nebulosity @ nebulosity @ bb > 10 > 10°

None Previously ImagedNone Previously Imaged


52 Targets (+ 5 Calibration Orbits)52 Targets (+ 5 Calibration Orbits)26 Debris Disk Candidates26 Debris Disk Candidates>> 10 Myr (Optically Thin) 10 Myr (Optically Thin)Likely Dust Dominated Likely Dust Dominated Spectral Types: A0 - K2Spectral Types: A0 - K2Main Sequence StarsMain Sequence StarsIRAS FIR Excesses:IRAS FIR Excesses: LL25+60 mm25+60 mm / L / L** > 3 x 10 > 3 x 10-4-4

unconfused by backgroundunconfused by background nebulosity @ nebulosity @ bb > 10 > 10°

None Previously ImagedNone Previously Imaged

1. Significant 60 1. Significant 60 m excessm excess2. Estimate T2. Estimate Tdustdust and R and Rdisk disk from from

25/60 & 60/10025/60 & 60/100m color excessm color excess3. Assume small grains with 1.13. Assume small grains with 1.1mm albedos ~ 0.2-0.5 so (falbedos ~ 0.2-0.5 so (fscatscat/f/f**) )

comparable to absorbed starlightcomparable to absorbed starlight4. f4. fscatscat/f/f** instrumentally detectable instrumentally detectable

5. Disk radii likely > 0.3”5. Disk radii likely > 0.3”6. Distance < 150 pc6. Distance < 150 pc7. Surface brightness sufficiently7. Surface brightness sufficiently high to detect in 1 HST orbit high to detect in 1 HST orbit

0

-1

-2

-3

-4

-5

-6

Log

Fra

ctio

nal

IR

Exc

ess

/ arc

sec2

0.1 1 10Log Radius (Arcseconds)

DEBRIS DISK CANDIDATE SELECTION

HD 32297HD 32297Anon. F5Anon. F5

HD 107146HD 107146

HD 92945HD 92945OB

SC

UR

ED

BY

CO

RO

NA

GR

AP

HO

BS

CU

RE

D B

Y C

OR

ON

AG

RA

PH

NICMOS 1.1NICMOS 1.1m: 1300sm: 1300s ACS 0.8ACS 0.8m: 7800sm: 7800s

-Spectral Type: A0Spectral Type: A0

-Distance: 112 Distance: 112 ± 12 pc 12 pc

-J=7.69, H=7.62, K=7.59 (2MASS)J=7.69, H=7.62, K=7.59 (2MASS)

-LL25+6025+60mm//LL** ~ 0.27% (IRAS FSC) ~ 0.27% (IRAS FSC) 12(Jy)12(Jy) 25(Jy) 25(Jy) 60(Jy) 60(Jy) 100(Jy)100(Jy) 870*(mJy)870*(mJy) <0.14 0.211 <0.14 0.211±0.034 1.1220.034 1.122±0.067 <1.60 5.60.067 <1.60 5.6±6.8 6.8

-Age: Uncertain, but…Age: Uncertain, but…

HD 32297HD 32297

* Silverstone, et al. 2004* Silverstone, et al. 2004

HD 32297HD 32297

Low Luminosity for itsLow Luminosity for itsB-V Color Similar to Young B-V Color Similar to Young A-stars at the Bottom LocusA-stars at the Bottom Locusof the V vs. B-V C-M Diagramof the V vs. B-V C-M Diagram

F110W Coronagraphic ImagingF110W Coronagraphic Imaging

Difference ImageDifference Image

HD 32297HD 32297

672s Integrations672s Integrations29.9 deg 29.9 deg Orientation OrientationO

RIE

NT

AT

ION

2O

RIE

NT

AT

ION

2O

RIE

NA

TIO

N 1

OR

IEN

AT

ION

1



HD 32297HD 32297

672s Integrations672s Integrations

RE

FE

RE

NC

E P

SF

RE

FE

RE

NC

E P

SF

OR

IEN

AT

ION

1O

RIE

NA

TIO

N 1


RE

FE

RE

NC

E P

SF

RE

FE

RE

NC

E P

SF

OR

IEN

AT

ION

2O

RIE

NA

TIO

N 2


HD 32297HD 32297

672s Integrations672s Integrations

HD 32297HD 32297Near Edge-On (“Near Edge-On (“ Pic-like”) Disk Pic-like”) Disk

NN

EE

Inclination = 10.5Inclination = 10.5° ± 2.52.5°, P.A. = 227.5, P.A. = 227.5° ± 11° Extent*: Extent*: >> 3.3” (400 AU) to NE; 3.3” (400 AU) to NE; >> 2.5” to SW 2.5” to SW *3*3 per resolution element lower limits per resolution element lower limits

HD 32297HD 32297Near Edge-On (“Near Edge-On (“ Pic-like”) Disk Pic-like”) Disk

NN

EE

1.11.1m Disk Flux Density: 4.81 m Disk Flux Density: 4.81 ± 0.57 mJy (r > 0.3”) 0.57 mJy (r > 0.3”)Scattering Fraction: 0.33% Scattering Fraction: 0.33% ± 0.04% (r 0.04% (r >> 0.3”) 0.3”)

““Above”: 56% Above”: 56% ± 12%, “Below”: 44 12%, “Below”: 44 ± 12% 12% But…But…

HD 32297 AU MIC 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/ACSAU MIC/ACS

EE F606W (PSF Subtracted)F606W (PSF Subtracted)

9"

HD 32297HD 32297

Radial Surface Brightness Profile Radial Surface Brightness Profile DISK ASYMMETRIESDISK ASYMMETRIESSW(r>0.3”) = 3.14 SW(r>0.3”) = 3.14 ± 0.57mJy 0.57mJyNE(r>0.3”) = 1.67 NE(r>0.3”) = 1.67 ± 0.57mJy 0.57mJy

Symmetric: 0.5” < r < 1.7”Symmetric: 0.5” < r < 1.7”

SW Brighter @ r < 0.6”SW Brighter @ r < 0.6”NE Brighter @ r > 2.4”NE Brighter @ r > 2.4”

SB(SW;r>0.5”) =0.455 rSB(SW;r>0.5”) =0.455 r-3.57-3.57

NW(SB;0.5”<r<1.7”) =0.51rNW(SB;0.5”<r<1.7”) =0.51r-3.7-3.7

NW(SB;1.7”<r<3.4”) =0.27rNW(SB;1.7”<r<3.4”) =0.27r-2.7-2.7

S.B. in mJy/sq. arcsecondS.B. in mJy/sq. arcsecond

SW SW NENE

SB ~ r -3.72

SB ~ r -2.74

SB ~ r -3.57

-Spectral Type: G2V (solar analog)Spectral Type: G2V (solar analog)

-Distance: 28.5 Distance: 28.5 ± 0.7pc 0.7pc

-J=5.87, H=5.61, K=5.54 (2MASS)J=5.87, H=5.61, K=5.54 (2MASS)

-LL60+10060+100mm//LL** ~ 0.10% (IRAS FSC) ~ 0.10% (IRAS FSC)12(Jy)12(Jy) 25(Jy)25(Jy) 60(Jy) 60(Jy) 100(Jy) 100(Jy) 870*(mJy)870*(mJy)0.2590.259±0.031 <0.135 0.7050.031 <0.135 0.705±0.056 0.9100.056 0.910±0.155 34.20.155 34.2±10.010.0

-Age: 30 - 250 Myr (Williams et al, 2004)-Age: 30 - 250 Myr (Williams et al, 2004)

-Also Observed With ACS (Ardila et al, 2004)-Also Observed With ACS (Ardila et al, 2004)

HD 107146HD 107146

* Silverstone, et al. 2004* Silverstone, et al. 2004

HD 107146HD 107146NICMOS 1.1 , 1350 ,m s linear display unbinned

2-roll combined2-roll combinedPSF subtractedPSF subtractedcoronagraphycoronagraphy

*Ardila, et al (2004) ApJ 517, L174

ACS* 0.8 , 2150 , ,m s log display 3 3 x pixel binning

*“Within 2” from the star, the {ACS} image is dominated by PSF subtraction residuals”. - Ardila 2004

Broad outer ringBroad outer ringR = 170 AU (6.0”)R = 170 AU (6.0”)peakpeak @ ~ 115 AU (4.0”) @ ~ 115 AU (4.0”)

ACS*:ACS*: ff0.60.6mm = 6.8 +/- 0.8 x 10 = 6.8 +/- 0.8 x 10-5-5

ff0.80.8mm = 1.0 +/- 0.1 x 10 = 1.0 +/- 0.1 x 10-4-4

NICMOS:NICMOS: ff1.11.1mm = 1.4 +/- 0.2 x 10 = 1.4 +/- 0.2 x 10-4-4

Disk Flux DensityDisk Flux Density(1.1 (1.1 m)m)

= 68 = 68 ± 10 10 Jy (r>0.3”)Jy (r>0.3”)

HD 107146HD 107146

0 1 2 3 4 5 6 70.1

1

10

100

1000

Radial Distance (arcsec)

S.

B.

(mic

roJy

/ s

q. a

rcse

cond

) 6”6”U

nd

etec

ted

by

NIC

MO

SU

nd

etec

ted

by

NIC

MO

S

Un

det

ecte

d b

y A

CS

Un

det

ecte

d b

y A

CS

HD 107146HD 107146

0 1 2 3 4 5 6 70.1

1

10

100

1000

Radial Distance (arcsec)

S.

B.

(mic

roJy

/ s

q. a

rcse

cond

) 6”6”U

nd

etec

ted

by

NIC

MO

SU

nd

etec

ted

by

NIC

MO

S

STAR:STAR:

Spectral Type: F5Spectral Type: F5

Pic Moving GroupPic Moving Group

Age: ~ 12 MyrAge: ~ 12 Myr

Distance: 50 pcDistance: 50 pc

LL25+6025+60mm//LL** ~ 0.2% ~ 0.2%

ANOTHER NEW DISKANOTHER NEW DISK

ANOTHER NEW DISKANOTHER NEW DISKOBSERVATION:OBSERVATION:

-F110W (1.1F110W (1.1m)m)

-NIC2 CoronagraphNIC2 Coronagraph

-Two-OrientationTwo-Orientation

-PSF-Subtraction-PSF-Subtraction

-Recombination-Recombination

ANOTHER NEW DISKANOTHER NEW DISKMODEL (best fit):MODEL (best fit):

-Inclined RingInclined Ring

-Intrinsic SymmetryIntrinsic Symmetry

-I(r)/II(r)/I** ~ r ~ r-2-2

-SB(SB() ~ H-G() ~ H-G(,g),g)

-SB(r) ~ SB(r-SB(r) ~ SB(rpeakpeak) e) e-1-1

-PSF Convolution-PSF Convolution

ANOTHER NEW DISKANOTHER NEW DISK““Smoothed” ObservationSmoothed” Observation

Elliptical low-pass filterElliptical low-pass filter (preserve radial )(preserve radial )

±99° “Rotation” kernal “Rotation” kernal

(i = 31.7(i = 31.7°)

Gaussian WeightingGaussian Weighting

ANOTHER NEW DISKANOTHER NEW DISKOBSERVATION:OBSERVATION:

-F110W (1.1F110W (1.1m)m)

-NIC2 CoronagraphNIC2 Coronagraph

-Two-OrientationTwo-Orientation

-PSF-Subtraction-PSF-Subtraction

-Recombination-Recombination

ANOTHER NEW DISKANOTHER NEW DISKRESIDUALS:RESIDUALS:

Observation - ModelObservation - Model

Diffuse HaloDiffuse Halo

(Currently not in model)(Currently not in model)









ACSACS Courtesy of J. Krist &Courtesy of J. Krist &ACS/GTO Disk TeamACS/GTO Disk Team





NICMOS NICMOS + ACS+ ACS


N

E

1 "

Steeply Truncated Inner Radius(r = 86 AU, rinner = 61AU)

“Similar” to HR 4796A(r =70 AU, rinner = 62.5AU)


.

Angular Distance (arcseconds)

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

Fdisk/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 DISKANOTHER NEW DISKBilaterally 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

Fdisk/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 DiskIs the Morphology More Like:

HD 141569A

HD 107146

Debris Rings - Angular ScalesDebris Rings - Angular Scales

Angular scale: r(Fomalhaut) = 19”Angular scale: r(Fomalhaut) = 19”

10"4" 10"

0.6"

20" 20"5"

AU

Mic Pic

HD 32297

HR

4796F-Star

HD

141569

HD

107146

PscA

M0 A5 A0 A0 F5HAeBe

B9.5G2 A3

12-20 12-20 < 10 ? 8 12 5 30-250 200

210 ~1600 > 400 70 86 400 170 140

0.003 0.0033 0.0024 0.0017 0.0025 1.4x10-4 10-6

0.0004 0.0015 0.0027 0.005 0.002 0.0084 0.001 5x10-6

WingTilt

manyS.B.

W. TiltAzim.

No,

g ~ 0.3Yes… No.

Offset,

g ~ 0.3Ass

ym L

ir/L

* Fn

ir>

0.3” r

AU

Myr

S

pec

I

mag

e

Sta

r

Documents

Debris Disk Imaging with HST/NICMOS: The GO/10177 Debris Disk Survey Part 2: The Resolved Disks GLENN SCHNEIDER NICMOS Project Steward Observatory 933