glenn schneider steward observatory, university of arizona (nicmos/idt) high contrast imaging and...

Glenn Schneider Glenn Schneider Steward Observatory, University of Arizona (NICMOS/IDT)Steward Observatory, University of Arizona (NICMOS/IDT)

High Contrast ImagingHigh Contrast Imagingand and

The Disk/Planet ConnectionThe Disk/Planet Connection

Asymmetries (radial & azimuthal):• May implicate low-mass perturbers (planets) from: Rings, Central Holes, Gaps, Clumps, Arcs, Arclets• Help Elucidate the scattering & physical properties of the grains.

Observing scattered light from circumstellar debris has been observationally challenging because of the very high Star:Disk contrast ratios in such systems.

1984 - B.A. Smith & R.J. Terrile 6" radius coronagraphic mask, Las Campanas (discovery image)

Until very recently the large, and nearly edge-on disk around Pictoris remained the only such disk imaged. Pictoris

Resolved imaging spatial distribution of dust/debris.

Direct (Scattered Light) Imaging of Dusty DebrisDirect (Scattered Light) Imaging of Dusty Debris

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are needed to see this picture.

The HUBBLE Legacy The HUBBLE Legacy Breaking the Low Contrast ParadigmBreaking the Low Contrast Paradigm

• Diffraction Limited Imaging in Optical/Near-IR•> 98% Strehl Ratios @ alls• Highly STABLE PSF• Coronagraphy: NICMOS STIS, ACS

NIR High Dynamic Range Sampling NICMOS/MA: mag=19.4 (6 x 4m)

Background RejectionBackground Rejection1.61.6m: ~10m: ~10-6-6 pix pix-1 -1 @ 1”@ 1”

1.11.1m: ~10m: ~10-5 -5 in 2”-3” annulus in 2”-3” annulus

• Intra-Orbit Field Rotation

TODAY HST Provides a Unique Venue for High Contrast ImagingTODAY HST Provides a Unique Venue for High Contrast Imaging

HST is a stepping HST is a stepping stone for super-stone for super-high contrasthigh contrast

** imagingimaging

**Background Background RejectionRejection10109—9—10101010

Terrestrialplanets

form

Clearing ofinner solar

system,formation of a

Kuipercometary

belt?

108

yrs109

yrs

Era of heavybombarment

by comets

Currentage of

the Sun:5x109 yrs.

PerseiSun

HyadesTucanaeAssoc Pleiades

Primary Dust (≤ m) Secondary Dust (≥Locked to Gas Collisional erosion

Clearing Timescales: P-R drag few 10 Rad. Pressure: ~ 10 From: R. Webb

Collapsingprotostar

forms proto-planetary disk

106

yrs

Taurus,Ophiuchus

star formingregions

m)

64

Rocky coresof giant

planets form

accretegaseous

atmospheres

TW Hydrae

ry s107

Assoc

Giant planets

Planet-Building TimelinePlanet-Building TimelineHST Vis/NIR HST Vis/NIR

High ContrastBeyond HST Vis/UV Super-High Contrast

Young Extra-Solar Planet* &Brown Dwarf Companions

* < few x 106 yr at 1”

2.5"

1"

Circumstellar Disksfdisk/f*

> few x 10-3 at 1”

> 50 mas

Scientific Areas of Investigation EnabledScientific Areas of Investigation EnabledWith Today’s Capabilities on HSTWith Today’s Capabilities on HSTvia PSF-Subtracted Coronagraphic Imagingvia PSF-Subtracted Coronagraphic Imaging

Moving Beyond HST into the Super-High Contrast RegimeMoving Beyond HST into the Super-High Contrast Regime

Exosolar Planet Imaging & Spectroscopy: few x 106 Myr at 1” > 109 yr (solar age) at 1”

Disk Imaging & Spectroscopy: fdisk/f*

> few x 10-3 at 1” ≤ 10-6 at 1” > 50 mas a few mas (sub-AU at 200pc)

OPTICAL CONFIGURATIONS

•Coronagraphy•Polarimetric Nulling•Nulling Interferometry•Wavefront Correction•Station-Keeping Occulters•Interferometric Arrays

TECHNOLOGICAL CHALLENGES

•Micro-Roughness of Optical Surfaces•Particulate/Contamination Control•Stray Light Management & Control•Pupil Apodization (and Shaping)•Metrological Tolerancing & Stability•Wavefront/Mirror Sensing & Control

The Dusty Disk/Planet ConnectionThe Dusty Disk/Planet Connection Current theories of disk/planet evolution suggest a presumed epoch of planet-building via the formation and agglomerative growth of embryonic bodies, and the subsequent accretion of gaseous atmospheres onto hot giant planets, is attendant with a significant decline in the gas-to-dust ratios in the remnant protostellar environments.

In this critical phase of newly formed (or forming) extra-solar planetary systems, posited from a few few megayears to a few tens of megayearsmegayears to a few tens of megayears, the circumstellar environments become dominated by a second-generation population of dust containing larger grains arising from the collisional erosion of planetesimals.

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are needed to see this picture.

< 1Myr< 1MyrProplydsProplydsin Orionin Orion

and…and…SubstellarSubstellarObjets toObjets to~ 10 M~ 10 Mjupjup

HH30 Obscured GM AUR UnembeddedHH30 Obscured GM AUR Unembedded

Direct ImageDirect Image

Coronagraph +Coronagraph +PSF SubtractionPSF Subtraction

~ 1— few Myr~ 1— few Myr

. .

Radius (Arcsec) from Hole Center

5 7 9 11 13 15 17 19 21 23 25 27 29 31 33 35 37

2

3

4

5

6

7

8

9

10

11

12

13

14

15

16

0.3 0.45 0.6 0.75 0.9 1.05 1.2 1.35 1.5 1.65 1.8 1.95 2.1 2.25 2.4 2.55 2.7 2.85

Azimuthal Averages, 1-Pixel Wide Annular Zones(69:69, 208:209) and (77, 205) Glint Features Excluded

Radius (Pixels) from Hole Center

0 0.075 0.15 0.225 0.3 0.375 0.45 0.525 0.6 0.675 0.75 0.825 0.9 0.975 1.0510-6

10

10-4

10-3

10-2

10-1

100 REDUCTION IN BACKGROUND FLUX FROM F160W PSF

Unocculted F160W PSFPSF + CoronagraphPSF + Coronagraph + Roll

ARCSECONDS

CoronagraphicHole

Radius = 0.3"

1pixel

-5

Coronagraph +Coronagraph +

PSF SubtractionPSF Subtraction

Collapsingprotostar


106

yrs

Taurus,Ophiuchus

star formingregions

Planet-Building TimelinePlanet-Building Timeline

HH 30

Collapsingprotostar


106

yrs

Taurus,Ophiuchus

star formingregions


QuickTime™ and aSorenson Video decompressorare needed to see this picture.

Rocky coresof giant

planets form

Collapsingprotostar


106

yrs

Taurus,Ophiuchus

star formingregions


accretegaseous

atmospheres

TW Hydrae

ry s107

Assoc

Giant planets

141569A

Terrestrialplanets

form



Kuipercometary

belt?

108

yrs109

yrs


by comets

Currentage of

the Sun:5x109 yrs.

PerseiSun



Clearing Timescales: P-R drag few 10 Rad. Pressure: ~ 10

From: R. Webb

Collapsingprotostar


106

yrs

Taurus,Ophiuchus

star formingregions

m)

64

Rocky coresof giant

planets form

accretegaseous

atmospheres

TW Hydrae

ry s107

Assoc

Giant planets


Examples of Dusty Disks with Radial and Hemispheric Brightness Examples of Dusty Disks with Radial and Hemispheric Brightness Anisotropies and Complex Morphologies, Possibly Indicative of Anisotropies and Complex Morphologies, Possibly Indicative of Dynamical Interactions with Unseen Planetary Mass Companions, Dynamical Interactions with Unseen Planetary Mass Companions, Spatially Resolved and Imaged Around Young (< 10 Myr) Stars by HST.Spatially Resolved and Imaged Around Young (< 10 Myr) Stars by HST.

N

E

1 "

HR 4796A (A0V), ~ 8 MyrA 70AU radius ring, ~ 12 AU wide ring of very red material, exhibiting strong forward scattering and ansally asymmetric hemispheric flux densities.

A 400AU radius disk, with a broad, partially filled asymmetric gap containing a “spiral” arclet.

HD 141569A(Herbig Ae/Be)~ 5 Myr


TW Hya (K7) “Old” PMS Star

Pole-on circularly symmetric disk with a break in its surface brightness profile at 120 AU (2”).


TW Hya (K7) “Old” PMS Star

Pole-on circularly symmetric disk with a break in its surface brightness profile at 120 AU (2”).

and, possibly, a radially and azimuthally confined arc-like depression.


HR 4796AHR 4796A

1.1m 0.58m

Ansal Separation (Peaks) = 2.107” ± 0.0045”

Major Axis of BFE = 2.114” ± 0.0055"

P.A. of Major Axis (E of N) = 27.06° ± 0.18°

Major:Minor Axial Length = (3.9658 ± 0.034): 1

Inclination of Pole to LOS = 75.73° ± 0.12°

Photocentric Offset from BFE(Y) = -0.0159" ± 0.0048"

Photocentric Offset from BFE(X) = +0.0031" ± 0.0028"

HR 4796A RING GEOMETRYHR 4796A RING GEOMETRY(Least-Squares Isophotal Ellipse Fit)

00.10.20.30.40.50.60.70.80.91

1.1

-1.6 -1.5 -1.4 -1.3 -1.2 -1.1 -1 -0.9 -0.8 -0.7 -0.6

NE ANSA CROSS-SECTIONAL PROFILE

Distance (Arc Seconds)

0.197"

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1

1.1

-1.6 -1.5 -1.4 -1.3 -1.2 -1.1 -1 -0.9 -0.8 -0.7 -0.6

NE ANSA CROSS-SECTIONAL PROFILE

Distance (Arc Seconds)

0.197"

Bri

ghtn

ess

(Nor

mal

ized

to N

E A

nsa)

HR 4796A Circumstellar Debris Ring - WIDTHHR 4796A Circumstellar Debris Ring - WIDTH

FWHM ring = 0.184”

FWHM: 12.3±0.7AU 8.7% Dring

1-e-1 = 0.265”

PSF point source = 0.070”Measured = 0.197”

WIDTH AT NE ANSA

1-e-1: 17.7±10.1AU 12.5% Dring

*

20% inner:outerfall-off asymmetry

*

Ansal Separation (Peaks) = 2.107” ± 0.0045”

Major Axis of BFE = 2.114” ± 0.0055"

P.A. of Major Axis (E of N) = 27.06° ± 0.18°

Major:Minor Axial Length = (3.9658 ± 0.034): 1

Inclination of Pole to LOS = 75.73° ± 0.12°

Photocentric Offset from BFE(Y) = -0.0159" ± 0.0048"

Photocentric Offset from BFE(X) = +0.0031" ± 0.0028"

RING GEOMETRY - Least-Squares Isophotal Ellipse FitRING GEOMETRY - Least-Squares Isophotal Ellipse Fit

““FACE-ON” PROJECTION - With Flux ConservationFACE-ON” PROJECTION - With Flux Conservation

Spatially Resolved Relative PHOTOMETRY of the RingSpatially Resolved Relative PHOTOMETRY of the Ring

N-S

igm

a

Bri

ghtn

ess

Rat

io (

Per

cent

)

NW:SE Surface Brightness AnisotropyNW:SE Surface Brightness Anisotropy

30

40

50

60

70

80

90

NE % Peak CountsSW % Peak Counts% SW/NE

Angle from Major Axis (Degrees)

-2

0

2

4

6

8

-60 -50 -40 -30 -20 -10 0 10 20 30 40 50 60

(%SW - %NE) : SIGMA (%SW/%NE)

100 BACK FRONT

N-S

igm

a

Bri

ghtn

ess

Rat

io (

Per

cent

)

0123456

0 10 20 30 40 50 60

(NE Front-Back) : SIGMA(Front/Back)(SW Front-Back) : SIGMA(Front/Back)(MEAN Front-Back) : SIGMA(Front/Back)

100

110

120

130

140

150

160

170 NE % FRONT:BACKSW % FRONT:BACKMEAN FRONT:BACK1 + 0.73*COS(theta)

Angle from Major Axis (Degrees)

Front:Back Surface Brightness AnisotropyFront:Back Surface Brightness Anisotropy

Broad Colors of the HR 4796A Debris RingBroad Colors of the HR 4796A Debris Ring[50CCD]-[F110W]=0.55±0.09[50CCD]-[F160W]=1.14+0.20

-0.17

Intrinsically red grains

•Consistent with collisionally evolved population of particle sizes > few microns

•Not primordial ISM grains

•Similar intrinsic colors to TNOsin our solar system [V]-[J]=+1.07*

•Consistent with laboratory* irradiation experiments on a varietyof organics to study reddening ofD & P type asteroids with distance From Sun.

*Barucci et al (1993); Andronico et al (1987)

Terrestrialplanets

form



Kuipercometary

belt?

108

yrs109

yrs


by comets

Currentage of

the Sun:5x109 yrs.

PerseiSun



Clearing Timescales: P-R drag few 10 Rad. Pressure: ~ 10

From: R. Webb

Collapsingprotostar


106

yrs

Taurus,Ophiuchus

star formingregions

m)

64

Rocky coresof giant

planets form

accretegaseous

atmospheres

TW Hydrae

ry s107

Assoc

Giant planets


0

6 7 8 9 10Log10 Age (years)

80Mjup

14Mjup

JUPITER

SATURN

STARS (Hydrogen burning)

BROWN DWARFS (Deuterium burning)

PLANETS

200Mjup

Evolution of M Dwarf Stars, Brown Dwarfsand Giant Planets (from Adam Burrows)

-10

-8

-6

-4

-2

Log

10 L

/Lsu

m

sun

Cooling Curves for Substellar ObjectsCooling Curves for Substellar Objects

CORONAGRAPHICCORONAGRAPHICCOMPANIONCOMPANIONDETECTIONDETECTION

(Multiaccum) Imagingat two S/C orientations(in a single HST visability period).

Background objectsrotate about occultedTarget. PSF structuresand optical artifactsdo not.

TWA6. Two Integrations: Median of 3 Multiaccum Each

Roll = 30° Time = 20 minutes

Above: Coronagraphic Images

Roll: 30°

Above: Coronagraphic Images

Roll: 30°

Left: Difference Image

Same display dynamic range

H “companion” = 20.1H = 13.2, =2.5”

At =2.5” background brightness is reduced by an ADDITIONAL factor of 50 over raw coronagraphic gain (ofappx 4).

Each independent image of TWA6“B” is S/N ~20 in difference frame.

Imperfections inPSF-subtractionsresult in residualsexpected from purephoton noise.

Systematics:

OTA “Breathing”

Target Re-centration

Coron. Edge Effects

Mechanical Stability

Detectability and Spatial CompletenessDetectability and Spatial Completeness

(() Dependence via Model PSF Implantation) Dependence via Model PSF Implantation

Observed Model* Nulled Implant

*TinyTim 5.0 HST+NICMOS Optical Model - Krist

Detectability: (Detectability: () Dependence via Model PSF Implantation) Dependence via Model PSF Implantation

.

4

8

12

16

20

25%

Rec

over

ed F

lux

S/ N

(Positi ve Im

plan t Onl y)

Photometric Efficacy & Statistical SignificancePhotometric Efficacy & Statistical Significance

. ..

1.0"

Detectability: Detectability: ((11””) Dependence via Model PSF Implantation) Dependence via Model PSF Implantation

0.01.02.0 1.0 2.0Arc Seconds

PSF FWHM = 0.16"

NICMOSF160W25 OCT 1998

Camera 2 (0.076"/pixel)Coronagraph (0.3" radius)Integration Time =1280s

TWA6 Image TWA6 Image Combination:Combination:S/NS/NTWA6B TWA6B = 35= 35

H-Band (F160W) Point-Source Detectability LimitsH-Band (F160W) Point-Source Detectability Limits Two-Roll Coronagraphic PSF Subtraction 22m Total Integration

H(5) = 7.14 + 3.15” - 0.286” 2 {M&K Stars}.

. .

9

10

11

12

13

14

15

16

0 1 2 3 4 5 6 7 8 9 10Rdiu(Acecond)

Normalized Intensity

-4 -2 0 2 4

4

2

0

-2

-4

0.0 0.2 0.4 0.6 0.8 1.0

7x7 Pixels71% Ensquared Energy

5σ

1σ

Rea

d N

oise

Dom

inat

edPh

oton

Noi

se D

omin

ated

H=6.9

0.01.02.0 1.0 2.0Arc Seconds

PSF FWHM = 0.16"



TW Hya AssnTW Hya AssnK7K7primaryprimary, D = 55pc, D = 55pcAge = 10 MyrAge = 10 Myr

=2.54”, 140AU=2.54”, 140AUH =13.2H =13.2(L(LB/AB/A)[H]=5 )[H]=5 xx1010-6-6

Habs = 16.6Habs = 16.6

Implies:Implies:• • Mass ~ 2Mass ~ 2JupiterJupiter

• • TTeffeff ~ 800K ~ 800K

IFIF Companion... Companion...

S/NS/NTWA6B TWA6B = 35= 35

TWA 6A/BTWA 6A/B

0.01.02.0 1.0 2.0Arc Seconds

PSF FWHM = 0.16"



Confirmation (or Rejection) by Common Proper MotionConfirmation (or Rejection) by Common Proper Motion

… … possible via ground-possible via ground-based adaptive optics based adaptive optics

imaging with a sufficiently imaging with a sufficiently long temporal baseline.long temporal baseline.

Keck II + AO imaging. Keck II + AO imaging. Courtosy of B.Macintosh, LLNLCourtosy of B.Macintosh, LLNL

Anomaly or Bias? A Jovian Planet @ Anomaly or Bias? A Jovian Planet @ >> 140 AU? 140 AU?

• RV Surveys suggest ~ 5% MS *s have 0.8—8 Mjup companions

@ d < 3AU from their primaries.

• NOT Where Giant Planets are found in our own Solar System

WHY ARE THEY THERE?

Posited*: Mutual interactions within a disk can perturb one young planet to move into a < 1AU eccentric orbit (as inferred from RV surveys), and the other…

Ejected (but bound) to very large separations, > 100AU

Cannot be observationally tested with HST-like capabilities, requires “Super-High” contrast imaging.

* e,g., Lin & Ida (ApJ, 1997); Boss (2001, IAU Symp 202)

Inner Regions of Evolved DisksInner Regions of Evolved DisksCannot yet be probed in scattered light. Yet, as inferred from mid-IR:

An inner tenuous component of warm zodi-like dust may

be confined within a few AU of HR 4796A.

12–20m thermal emission is contained completely

within the large inner “hole” of HD 141569A.

What evolutionary and dynamical interactions may be going on between What evolutionary and dynamical interactions may be going on between unseen planets and unseen dust which will shape these systems?unseen planets and unseen dust which will shape these systems?

Requires “Super-High” contrast and resolution.

0

6 7 8 9 10Log10 Age (years)

80Mjup

14Mjup

JUPITER

SATURN

STARS (Hydrogen burning)

BROWN DWARFS (Deuterium burning)

PLANETS

200Mjup

-10

-8

-6

-4

-2

Log

10 L

/Lsu

m

sun

HST Has Sampled Only the Low-Hanging Fruit HST Has Sampled Only the Low-Hanging Fruit in the in the DiskDisk//PlanetPlanet Orchard. Orchard.

GL

503.2B

GL

577B/C

CD

-33° 7795BT

WA

6B ?

HR

7329B

Anomaly or Bias? A Jovian Planet @ Anomaly or Bias? A Jovian Planet @ >> 140 AU? 140 AU?

• RV Surveys suggest ~ 5% MS *s have 0.8—8 Mjup companions

@ d < 3AU from their primaries.

• NOT Where Giant Planets are found in our own Solar System

WHY ARE THEY THERE?

Posited*: Mutual interactions within a disk can perturb one young planet to move into a < 1AU eccentric orbit (as inferred from RV surveys), and the other…

Ejected (but bound) to very large separations, > 100AU

* e,g., Lin & Ida (ApJ, 1997); Boss (2001, IAU Symp 202)

GLENN SCHNEIDERNICMOS ProjectSteward Observatory933 N. Cherry AvenueUniversity of ArizonaTucson, Arizona 85721

Phone: 520-621-5865 FAX: 520-621-1891e-mail: [email protected]://nicmosis.as.arizona.edu:8000/

HUBBLE SPACE TELESCOPE

UV/Optical imaging and spectroscopy of collisionally evolved circumstellar debris and co-orbital bodies will play a pivotal role in furthering our understanding of the formation and evolution of exosolar planetary systems. To study physical processes acting over sub-AU spatial scales and time scales comparable to the age of our solar system will require a 3—4 order of magnitude improvement in instrumental stray light rejection over the performance obtainable with HST.

Is it, or Isn’t It?Is it, or Isn’t It?• Undetected in NICMOS 0.9m Followup Observation I-H > 3• Marginally Detected in 6-Orbit Binned STIS G750L Spectrum• Colors Consistent with 2 Mjup, 10 Myr, “Hot” Giant Planet

Instrument Band Bandpass Mag NICMOS/C2 F160W 1.40—1.80 20.1NICMOS/C2 F090M 0.80—1.00 >23.1 STIS/G750L I extract 0.81—0.99 ~25.4STIS/G750L R extract 0.63—0.77 >27.2

If NOT a hot young planet, it must be aHighly exotic object!

Is it, or Isn’t It?Is it, or Isn’t It?• Undetected in NICMOS 0.9m Followup Observation I-H > 3• Marginally Detected in 6-Orbit Binned STIS G750L Spectrum• Colors Consistent with 2 Mjup, 10 Myr, “Hot” Giant Planet*

. .

1 0- 5

0 . 0 0 0 1

0 . 0 0 1

0 . 0 1

0 . 1

1

1 0S y n t h e t i c S p e c t r u m : T = 8 0 0 K , 1 0 M y r , d = 1 0 p c , g = 3 x 1 0 - 4

W a v e l e n g t h ( Å )

0 . 7 0 . 8 0 . 9 1 1 . 1 1 . 2 1 . 3 1 . 4 1 . 5 1 . 6 1 . 7 1 . 8 1 . 9

F 1 6 0 WF 0 9 0 M

R e x t r a c t

I e x t r a c t

H2O

H2O

H2O

C H4

C H4

C O

C O

C H4K

H2O

C H4

H2 - H

2H

2 - H

2

20.1>23.1

~25.4

>27.2

• Keck/AO Astrometric (PM) Follow-up Thus-Far Inconclusive

* Sudarsky et al., 2000Spectrum from A. Burrows

Is it, or Isn’t It?Is it, or Isn’t It?A differential proper motion measure will be obtained with NICMOS.

If common proper motions are confirmed we will request time for NICMOS grism spectrophotometry to obtain a near-IR spectrum.

. .

1 0- 5

0 . 0 0 0 1

0 . 0 0 1

0 . 0 1

0 . 1

1

1 0S y n t h e t i c S p e c t r u m : T = 8 0 0 K , 1 0 M y r , d = 1 0 p c , g = 3 x 1 0 - 4

W a v e l e n g t h ( Å )

0 . 7 0 . 8 0 . 9 1 1 . 1 1 . 2 1 . 3 1 . 4 1 . 5 1 . 6 1 . 7 1 . 8 1 . 9

F 1 6 0 WF 0 9 0 M

R e x t r a c t

I e x t r a c t

H2O

H2O

H2O

C H4

C H4

C O

C O

C H4K

H2O

C H4

H2 - H

2H

2 - H

2

20.1>23.1

~25.4

>27.2

glenn schneider steward observatory, university of arizona (nicmos/idt) high contrast imaging and...

Documents

secondary dust

complex morphologies

mtoday hst

stable psf coronagraphy

5x109 yrs

gas collisional erosion

lowmass perturbers planets

myr stars