HST Coronagraphic Imaging of Debris...
Transcript of HST Coronagraphic Imaging of Debris...
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HST Coronagraphic Imaging of Debris Disks
John Krist (JPL & ACS Science Team)
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Young Star Disks vs. Debris Disks
GG Tau HD 100546
HD 163296 AB Aur
Young Star Disks & Envelopes
Fomalhaut
AU Mic
HD 107146
HD 107146
HD 92945
Debris Disks
<~10 Myr, >MJup, Optically thick,Gas rich, Accreting
>~10 Myr, <~MEarth, Optically thin,Gas poor, Collisional debris
See talk by Grady
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Observed Characteristics of Debris Disks
• Ldust/Lstar < 10-2
– Beta Pic = ~2 x 10-3
– Fomalhaut = ~8 x 10-5
• No significant extinction within disk (what you see is what there is)
• Low total brightness relative to star (e.g. Fomalhaut’s integrated disk flux is 10-6 of the star’s)
• Extended (Fomalhaut disk ~190 arcsec2)
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Why Use HST to Image Debris Disks?
• Large, high-resolution field• Wide wavelength coverage (0.2 - 2.5 μm)• Only choice for high-res imaging in the
visible• Stability over time
– Residual diffracted & scattered light pattern is very stable compared to ground-based scopes and can be subtracted out using PSF subtraction (reference PSF or roll subtraction)
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HST PSF Subtraction
The stability of HST allows diffracted and scattered light to be subtracted
Beta Pictoris
Alpha Pic
Beta - Alpha Pic
ACS coronagraphGolimowski et al. (2006)
Beta PicWFPC2WFPC2 Science Team
Reference PSF Subtraction Roll Subtraction
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HST Coronagraphs
Filters & polarizersFull Lyot stopLarge occultersDead
~1”0.2 – 1.0 μmACS
No filtersIncomplete Lyot stopDead
~0.5”0.2 – 1.0 μmSTIS
Filters & polarizersStill workingMisaligned Lyot stop
~0.5”0.9 – 2.5 μmNICMOS
Advantages &Disadvantages
PracticalInner
RadiusBandpassCamera
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ACS PSF Mean Brightness Profiles (V)
Unocculted star
Coronagraph
│Coronagraph - PSF│(Roll subtraction – 24 hrs later)
7x reduction
6x reduction
1200x reduction 1500x reduction
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Debris Disks Seen in Scattered Light
ACS22K1HD 92945
Ground, ACS, NICMOS10M1AU Mic
ACS (Ardila et al.)43K8AG Tri
ACS18K1HD 53143
ACS46G5HD 202917
NICMOS (see Hines talk)35G4HD 61005
ACS, NICMOS29G2HD 107146
ACS16G0HD 207129
ACS17F9HD 10647
ACS18F5HD 139664
ACS, NICMOS51F5HD 181327
ACS, Ground45F2HD 15115
Ground, WFPC2, NICMOS, STIS, ACS19A5Beta Pic
ACS8A3Fomalhaut
NICMOS, Ground112A0HD 32297
NICMOS, STIS, Ground67A0HR 4796
NICMOS, STIS, ACS, ~Ground (Palomar)99A0HD 141569A
Disk Seen inScattered Light with
Distance(pc)
SpecTypeName
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www.circumstellardisks.org
See poster by McCabe
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HD 141569aA0V (Herbig Ae), 99 pc, ~5 Myr, Ld/L*=8 x10-3
ACS Direct (V) STIS Coronagraph (U→I)
NICMOS Coronagraph (J)ACS Coronagraph (V)
Palomar AOCoronagraph (2.2 μm)
Boccaletti et al. (2003)
HST subtractions by Krist.ACS results in Clampin et al. (2003)NICMOS results in Weinberger et al. (1999), Augereau et al. (1999)STIS results in Mouillet et al. (2001)
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HD 141569a: ACS Observations
Hard stretchDeprojectedDensity Map
DeprojectedDensity Map
ACS science results in Clampin et al. (2003)
Disk is red relative to star.g = ~0.2
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HD 141569a: Dynamical Modeling
Ardila et al. (2005):Recent fly-by of nearby binary created large spirals,while a large planet created tight spirals & inner clearing;gas drag needed to slow the blow-out of dust
Wyatt (2005)
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HR 4796A0V, 67 pc, ~8 Myr, Ld/L* = 5 x 10-3, with nearby M star
STIS (0.2 – 1 μm) NICMOS (J band)
2.2” (148 AU)
Subtractions by Krist (no additional cleaning or smoothing).NICMOS science results in Schneider et al. (1999)
Disk is red relative to star.Brightness asymmetries possibly due to influence of companion star.Sharp inner edge.May be nearly optically thick in radial direction.
Ground K’Augereau et al. (1999)
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HD 32297A0V, 112 pc, Ld/L* = 3 x 10-3
2” (224 AU)
NICMOS (J band) Ground (R band)
Schneider et al. (2005) Kalas (2005)
Inclination ~10 degDisk might be blue.~0.004 of starlight scattered by disk.
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FomalhautA3V, 8 pc, ~200 Myr, Ld/L* = 8 x 10-5
Kalas, Graham, & Clampin (2005)
Deprojected
Total light from disk is 10-6 of the star’s.Mean surface brightness = 22 mag arcsec-2.Moderate forward scattering (g ~ 0.2)
15 AU
}
140 AU18”
Quillen (2006) suggests a Neptune-Saturn mass planet at r = 119 AU
ACS (Wide V band)
350 μmMarsh et al.
(2005)
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Beta PicA5V, 19 pc, 12-20 Myr, Ld/L*=3 x 10-3
29” (550 AU)
Deconvolved
ACS (Wide V band)
Golimowski et al. (2006)
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Beta Pic Colors
Golimowski et al. (2006)
Right/Left & Top/Bottom disk color asymmetries.Disk is red and gets redder with increasing radius.
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HD 15115F2V, 45 pc, ~12 Myr?, Ld/L* = ~5 x 10-4
5” (225 AU) 5” (225 AU)
ACS (Wide V band) Keck (H band)
Possible fly-by candidate identifiedDisk is blue relative to star based on V-H colors, and becomes moreblue at larger radii
Kalas et al. (2007)
See poster by Kalas at this conference
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HD 181327F5V, 51 pc, 12 Myr, Ld/L*=2 x 10-3
175 AU
NICMOS (J) ACS (Wide V band)
Schneider et al. (2006)
Disk is red.g = 0.3
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HD 139664F5V, 18 pc, 100-1000 Myr, Ld/L*=1 x 10-4
6” (108 AU)
ACS (Wide V band)
Kalas et al. (2006)
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HD 10647(HR 506)F9V, 17 pc, 0.3-7 Gyr, Ld/L*=3 x 10-4
350 AU (20”)
Stapelfeldt et al. (in prep)
See poster by Stapelfeldt et al. at this conference.
Has R-V planet: a = 2 AU, Msini = 0.91 MJup
ACS (Wide V band)
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HD 207129G0V, 16 pc, ~6 Gyr, Ld/L*=1 x 10-4
Krist et al. (2007)
Spitzer 70 μmBryden et al. (2007)
• Seen only in roll subtractions• Faintest disk yet seen
V = 24 mag / arcsec2
ACS (Wide V band)
Smoothed,4x4 Binned
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HD 107146G2V, 29 pc, 30-250 Myr, Ld/L*=1 x 10-3
4”114 AU
Ardila et al. (2004)
ACS (Wide V band)
g = 0.2 – 0.3Slightly red relative to star
See talk by Metchev on modeling of this disk.
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HD 202917G5V, 46 pc, 30 Myr, Ld/L*=3 x 10-4
2” (92 AU)
ACS Science Team
ACS (Wide V band)
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HD 53143K1V, ~1 Gyr, 18 pc, Ld/L*=3 x 10-4
6” (108 AU)
ACS (Wide V band)
Kalas et al. (2006)
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3 4 5 6 7 8 9 10Arcsec from Star
10-8
10-7
10-6
10-5
Flux
disk
/ Fl
uxst
ar /
Arc
sec2
r-1.5
r-8
F814W
F606W
HD 92945K1V, 22 pc, ~100 Myr, Ld/L*=8 x 10-4
11” (240 AU)
ACS (Wide V band)
Golimowski et al. (in prep)
See poster by Golimowski et al. at this conference
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2”20 AU
BVI
AU MicM1V, 10 pc, 12 Myr, Ld/L*=4 x 10-4
V m
ag a
rcse
c-2
1 10Radius (arcsec)
24
22
20
18
16
NorthwestSoutheast
Radial brightness
Krist et al. (2005)
ACS (B,V,I)
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AU Mic
0 10 20 30 40 50 60 70 80 90 100
0
0
AU
AU
E N
EN
NW side
SE side
A B C
D
Galaxy
ACS (Wide V band)
Krist et al. (2005)
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AU Mic Polarization
ACS (Wide V band)
Graham, Kalas, & Matthews (2007)
• ACS R band coronagraphic imaging polarimetry• Peak polarization of 41% indicates single scattering by sub-micron
size particles• Consistent with highly porous, micron-sized dust aggregates
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Scattered-Light Debris Disk Inclinations
i
HD 107146 (65°)
HD 181327 (58°)
HD 141569A (35°)
Fomalhaut (24°)
AU Mic (0°)
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Disk Vertical Profiles
Lorentzian Gaussian
At r = 30 AU:Beta Pic FWHMvert = 12 AUAU Mic FWHMvert = 2 AU
Beta Pic & AU Mic have Lorentzian vertical profiles.
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Fractional Disk Luminosities (Ld/Lstar)
8 x 10-3
HD 141569a
8 x 10-4
HD 92945
8 x 10-5
Fomalhaut~800x more than solar zodi
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Known Colors of Debris DisksRelative to Star
Red
HD 141569A
HD 4796A
Beta Pic
HD 181327
HD 107146
Blue
HD 32297 (?)
HD 15115
AU Mic
Neutral
HD 92945
One disk color by itself doesn’t mean a whole lot
See talk by Debes
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Degree of Forward Scattering
g = 0 g = 0.2 g = 0.3 g = 0.4 (0.7?)
g = 0 Isotropic
g = 1 Full forward scattering
g = -1 Full backward scattering
By itself, degree of forward scattering doesn’t say a whole lot
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Signs of Stellar & Planetary Encounters?
StellarEncounters
Clearings,Rings
Secondary disks,Warps
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HST Rules! (for debris disks) Of the debris disks that have been imaged in scattered light:
- ~70% have been reliably seen only with HST
- ~40% have been seen only with ACS
Non-detections for ~90 debris disk candidates (15% success rate)
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The Future
• NICMOS is still operational• Only a couple of debris disk programs in Cycle 16• STIS might be repaired in next servicing mission, maybe
ACS/WFC, but ACS/HRC (which contains the coronagraph) is uncertain
• No coronagraph on new WFC3 camera• At the bottom-of-the-barrel for IRAS-derived candidates;
Spitzer is providing new targets, especially for solar & later type stars
• JWST coronagraphs will probably have lower contrast than ACS or STIS ones
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