High Contrast Imaging with NICMOS - I i (Teaching an Old Dog New Tricks With Coronagraphic Polarmetry)
Glenn Schneider Dean C. Hines p Steward Observatory Space Science Inst. University of Arizona New Mexico Office
pi
The conference will produce rare opportunities for θ synergy and cross-fertilization between -current ground-based high-contrast programs (GDPS, LYOT, & NICI) -planned extreme AO programs (GPI & VLT-SPHERE) -future telescopes (TMT, JWST, TPF).
High Contrast Imaging with NICMOS - I i (Teaching an Old Dog New Tricks With Coronagraphic Polarmetry) *
Glenn Schneider Dean C. Hines p Steward Observatory Space Science Inst. University of Arizona New Mexico Office
pi
θ
http://nicmosis.as.arizona.edu:8000 [email protected] *See Poster: Hines et al.
1 HST: Unique Venue for High Contrast Imaging 1st Generation WFPC-1 FOC 0.1% reflective spot f/288 optical channel d = 1.2” in PC8 (f/30) Lyot coronaraph 14 λ/D @ 0.5µm 7.2 mas/pix, 3.2” FOV
HST has flown 5 high contrast imaging systems.
HST: Unique Venue for High Contrast Imaging 2nd Generation STIS NICMOS 2 Focal Plane Occulting Wedges Lyot Coronagraph Width: 1” - 3” r = 0.3”, f/45, 76 mas/pix Unfiltered (CCD broad response) 3.2 λ/D @ 1.1 µm
3rd Generation ACS Abberated-beam Coronagraph r = 0.9” & 1.8” masks {21|42} λ/D @ 0.5 µm HST has flown 5 high contrast imaging systems.
2 HST/NICMOS: Unique Venue for High Contrast Imaging
• Near-IR (0.9 —2.4 µm) Diffraction Limited Imaging • > 98% Strehl Ratios @ all λs • Highly STABLE PSF • Coronagraphy • Polarimetry • Inter-Orbit Field Rotation
NIR High Dynamic Range Sampling NICMOS/MA: Δmag=20/orbit
Two-Orientation PSF Areas of Investigation in Planetary System Subtracted Coronagraphy Formation/Evolution Enabled With Today’s Capabilities on HST via NICMOS PSF- Subtracted Direct, Coronagraphic, and Polarimetric Imaging Sub-Stellar
Companion HST GTO/7227 ΔH ~– 9.7 + 2.1ρ” Candidate Detection
3 BLUE = F090M(0.9µm) Areas of Investigation in Planetary System GREEN=F110M(1.1µm) Formation/Evolution Enabled With Today’s RED=F160W(1.6µm) Capabilities on HST via NICMOS PSF- Subtracted Direct, Coronagraphic, and Polarimetric Imaging Sub-Stellar
Companion HST GO/10176 Multi-band color indices & Confirmation & Differential Astrometry Characterization
Areas of Investigation in Planetary System Formation/Evolution Enabled With Today’s Capabilities on HST via NICMOS PSF- Subtracted Direct, Coronagraphic, and Polarimetric Imaging Circumstellar Disk
Detection & HST GTO/7233 x -4 Multiband Imaging fdisk/f* > few 10 at 1” ρ > 0.3”
4 Areas of Investigation in Planetary System Formation/Evolution Enabled With Today’s Capabilities on HST via NICMOS PSF- Subtracted Direct, Coronagraphic, and Polarimetric Imaging Circumstellar Disk 2 µm Imaging HST GO/10852 Polarimetry P% > 1% ~
PSF-Subtracted Coronagraphy
IMAGING DETECTION OF EGP & BD COMPANIONS TO NEARBY STARS
by 2-Roll Image Differencing (NICMOS Camera 2: 76 mas/pixel, ρ > 0.3”)
5 NICMOS F160W (H-band) Coronagraphic Performance (G2V)
. Radius (Pixels) from Hole Center 5 7 9 11 13 15 17 19 21 23 25 27 29 31 33 35 37
100 REDUCTION IN BACKGROUND FLUX FROM F160W PSF w.r.t. central pixel F (H) = 11% F B 16 10-1 central star A Unocculted PSF 15 Coronagraph /D C /D Coronagraph & PSF Subtraction K 14 10-2 λ λ G 13 1 R pixel O 12 10-3 = 2.2 = 2.2 m U m 11 µ N µ 1.6 D 10 10-4 1.6 R 9 IWA IWA E 10-5 8 INTENSITY (AZIMUTHAL AVERAGE) Coronagraphic D Hole U 7 Radius = 0.3" C 10-6 6 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 1.05 T ARCSECONDS I 5 O N 4 3 2 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 Radius (Arcsec) from Hole Center
Coronagraphic Companion Detection Self-Referntial PSF @ 2 Field Orientations Unresolved (Point-Like) Object: H =20.1, ΔH = 13.2, ρ=2.5”
Linear Display 0—2 ADU/sec/pixel; 2.19E-6 Janskys/ADU/sec/pixel
6 Coronagraphic Companion Detection PSF “Roll Subtraction” Difference Image: H =20.1, ΔH = 13.2 (La/Lb = 200,000:1), ρ=2.5”
At ρ=2.5” background brightness is reduced by an ADDITIONAL factor of ~50 over raw coronagraphic gain (of appx 4).
Linear Display -0.4 — +0.4 ADU/sec/pixel; 2.19E-6 Janskys/ADU/sec/pixel
Coronagraphic Companion Detection PSF “Roll Subtraction” Each independent point- Geometrical Rectification source image is S/N ~ 20 And De-Spiking*
*NICMOS/IDT Post-Processing & Analysis S/W: DSKP & IDP3 ftp://nicmos.as.arizona.edu/
Linear Display -0.4 — +0.4 ADU/sec/pixel; 2.19E-6 Janskys/ADU/sec/pixel
7 HST/NICMOS: Unique Venue for High Contrast Imaging
• Near-IR (0.9 —2.4 µm) Diffraction Limited Imaging • > 98% Strehl Ratios @ all λs Background Rejection • Highly STABLE PSF 1.6µm* : ~10-6 pix-1 @ 1” • Coronagraphy *w.r.t. central pixel
Fcentral(H) = 11% Fstar • Field Rotation
NIR High Dynamic Range Sampling NICMOS/MA: Δmag=20/orbit
. Cooling Curves for Substellar Objects 0 Evolution of M Dwarf Stars, Brown Dwarfs and Giant Planets (from Adam Burrows)
-2 200M jup sum L 80M L/ -4 jup 10 Log -6 sun NICMOS H-Band Companion Detection Limit 14Mjup
-8 STARS (Hydrogen burning) BROWN DWARFS (Deuterium burning) JUPITER PLANETS ΔH(50%) = 9.7±0.3 + 2.1 x ρ SATURN -10 6 7 ””””” ” 8 9 10 Log10 Age (years)
8 BROWN DWARF COMPANIONS TO “YOUNG” STARS 45 Stars, Median Age: 150 Myrs, Average Distance: 30 pc Mass Sensitivity: 5 Mjup @ 30 AU for 36%, 1 Mjup for < 30 Myrs Lowrance et al. 2005 AJ 130 1845 CD -33° 7785B (TWA5) HR 7329B Lowrance et al. 1999 ApJ 512 L127 Lowrance et al. 2000 ApJ 541 390 HST GTO/2776 HST GTO/2776 Primary: Primary: Spec: M1.5eV Spec: A0V Age: ~ 10 Myr Age: ~ 30 Myr Companion: Companion: Mass: ~ 20 Mjup Mass: ~ 50 Mjup Teff: ~ 2600 K Teff: ~ 2600 K Proj. Sep: 100 AU Proj. Sep: 200 AU Spec: M8 - M8.5 (STIS) Spec: M7-M8 (STIS)
REPRESENTATIVE EJP CANDIDATE DETECTIONS
Age ΔH Mass Sep Dist Myr mag est. " AU A 12 13.0 ~3 1.9 80 B 30 12.0 ~5 2.8 120 C 30 12.7 2—3 2.6 100 D 50 13.4 1-2 4.1 140 From HST 10176 Survey - see J. Farihi, Wed. afternoon
9 PSF-Subtracted Direct Imaging
CHARACTERIZATION OF “NEARBY” EGP & BD COMPANIONS
by 2-Roll Image Differencing NICMOS Camera 1: 43 mas/pixel “short wavelength” diagnostic filters
GO/10176: 116 Targets Including: 2M1207 (M8.5V, ~ 8 Myr, β Pic Moving Group)
04/27/2004
VLT/NACO H,Ks,L’
Chauvin et al 2004
10 2M1207 (M8.5V, ~ 8 Myr, β Pic Moving Group) HST/NICMOS CAMERA 1 FOLLOW-UP IMAGING 08/28/2004 (4 month astrometric baseline w.r.t VLT)
04/27/2004 PSF Subtraction
VLT/NACO H,Ks,L’ F090M (0.9µm) F110M (1.1µm) F160W (1.6µm)
Chauvin et al 2004 Song et al 2006, ApJ 652, 724
2M1207 (M8.5V, ~ 8 Myr, β Pic Moving Group) HST/NICMOS CAMERA 1 FOLLOW-UP IMAGING 08/28/2004 (4 month astrometric baseline w.r.t VLT)
04/27/2004 PSF Subtraction
VLT/NACO H,Ks,L’ F090M (0.9µm) F110M (1.1µm) F160W (1.6µm) (projected on
0.774 46 AU* Giant Planet ” Companion
sky) *59 +/- 7 pc Chauvin et al 2004 Song et al 2006, ApJ 652, 724
11 At 0.9 microns the 2M1207b: - has an apparent magnitude of +22.3 (08/28/2004) - is 720 times fainter than 2M1207 (mag +15.20) - is 44 times fainter than it is at 1.6 microns F090M(0.9µm) F110M(1.1µm) F160W(1.6µm)
2M1207b is 774 mas from 2M1207A NICMOS observations exploit the stability of the HST Point Spread Function to reduce the background light from 2M1207A and improve the image contrasts.
HST/NICMOS Camera 1 Observations of 2M1207 Two Orbits at Two Field Orientations 9.9° Roll - Constrained by Available Guide Stars
F090M(0.9µm) F110M(1.1µm) F160W(1.6µm)
4-Point Dither Combined Images ROLL ORIENTATIONS 1 & 2
12 HST/NICMOS Camera 1 Observations of 2M1207
F090M(0.9µm) F110M(1.1µm) F160W(1.6µm)
4-Point Dither Combined Images TWO-ROLL DIFFERENCE IMAGE
HST/NICMOS Camera 1 Observations of 2M1207
F090M(0.9µm) F110M(1.1µm) F160W(1.6µm)
4-Point Dither Combined Images SIMULTANEOUS BEST-FIT OPTICAL MODEL
13 HST/NICMOS Camera 1 Observations of 2M1207 F090M(0.9µm) F110M(1.1µm) F160W(1.6µm)
BEST-FIT MODEL SUBTRACTIONS
HST/NICMOS Camera 1 Observations of 2M1207 F090M(0.9µm) F110M(1.1µm) F160W(1.6µm)
BEST-FIT MODEL SUBTRACTIONS
14 HST/NICMOS Camera 1 Observations of 2M1207
ROTATE TO SAME SKY ORIENTATION
HST/NICMOS Camera 1 Observations of 2M1207
F090M(0.9µm) F110M(1.1µm) F160W(1.6µm)
4-Point Dither Combined Images COMBINATION IMAGES
15 .
HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING
F145M (1.45µm) imaging in H20 absorption band
THEORETICAL EGP SPECTRA (A. Burrows) F090M F110M F160W 1 Y Teff = 1200K Age = 6.5 Myr SIT 0.8 [g] = 3.778 EN ------D 5 M F145M X jupiter 0.6 1.44 R jupiter LU F
0.000041 Lsun
ED 0.4 CLEAR
ALIZ CLOUDY
M 0.2 OR N 0.8 1 1.2 1.4 1.6 1.8 Wavelength (microns)
HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING
NICMOS F145M (1.45µm)
2M1207A/b - 26 APR 05
16 HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING
F145M (1.45µm) imaging in H20 absorption band
2M1207b APPARENT MAGNITUDES
µm 04/27/04 VLT 08/28/2004 HST 04/26/2005 HST 0.90 +22.34 ± 0.35 +22.58 ± 0.35 1.10 +20.61 ± 0.15 1.45 +19.05 ± 0.03 1.60 +18.24 ± 0.02 +18.27 ± 0.02 2.20 +16.93 ± 0.11 3.90 +15.28 ± 0.14
HST/NICMOS CAMERA 1, 2nd FOLLOW-UP IMAGING
2M1207A/B APPARENT MAGNITUDE - NICMOS & VLT
waveln 2M1207b 2M1207A Δmag 0.90µm: +22.34 ± 0.35 +14.66 ± 0.03 +7.68 ± 0.35 1.10µm: +20.61 ± 0.15 +13.44 ± 0.03 +7.17 ± 0.15 1.45µm: +19.05 ± 0.03 +13.09 ± 0.03 +6.42 ± 0.04 1.60µm: +18.24 ± 0.02 +12.60 ± 0.02 +5.63 ± 0.03 2.20µm: +16.93 ± 0.11 +11.95 ± 0.03 +4.98 ± 0.11 3.80µm: +15.28 ± 0.14 +11.38 ± 0.14 +3.90 ± 0.17
17 HST/NICMOS CAMERA 1, 2nd FOLLOW-UP IMAGING
2M1207B NEAR-IR COLOR INDICES
F110M F145M F160W Ks L’ λ1-λ2 1.10 1.45 1.60 2.20 3.90 0.90 1.86±0.29 3.42±0.25 4.21±0.25 5.54±0.27 7.19±0.28 1.10 1.56±0.15 4.21±0.25 3.68±0.19 5.33±0.21 1.45 0.79±0.03 2.12±0.11 3.77±0.14 1.60 1.33±0.16 2.98±0.18 2.20 1.65±0.02
M(1207B) = 5 ± 3 Mjup q (2M1270 B/A) ~ 0.2
Song et al 2006, ApJ 652, 724
16 σ CPM
18 PSF-Template Subtracted Coronagraphy CIRCUMSTELLAR SCATTERED-LIGHT DISK IMAGING • Resolved imaging spatial distribution of dust/debris.
• Elucidate the physical & geometrical properties of disks & grains. (Simultaneous; multi λ) Light Scattering & SED Modeling • Asymmetries (radial & azimuthal): May implicate low-mass perturbers (planets) from: Rings, Central Holes, Gaps, Warps, Clumps, Arcs, Arclets
NICMOS F110W (~ J-Band) Coronagraphic Performance
Normalized* Radial Profiles (Azimuthal Median)
*w.r.t. central pixel, F(F110W)central = 23.3% Fstar
Direct
Coronagraphic
PSF Subtracted
1” 2” Background Rejection @ 1.1µm: ~10-5 in 2”-3” annulus
19 REPRESENTATIVE SCATTERED LIGHT DISK IMAGES WITH NICMOS/F110W PSF-SUBTRACTED CORONAGRAPHY (HST GO/7233)
GM AUR TW HYA HD 141569A HR 4796A
~ 1Myr cTTS ~ 5Myr cTTS ~ 5-8 Myr HAeBe ~ 8 Myr A0/PMS
A) Schneider et al. 2003, AJ, 125, 1467 B) Weinberger et al. 2002, ApJ, 566, 409 C) Weinberger et al. 1999, ApJ, 522, L53 D) Schneider et al. 1999, ApJ, 513, L127
PSF-Template Subtracted Coronagraphy
SCATTERED-LIGHT IMAGING OF (optically thick) CIRCUMSTELLAR DISKS of Unobscured T TAURI STARS
20 HH30 Obscured T TauGM/Protoplanetary AUR Unembedded Circumstellar (Av < 0.5) Disks… Red Polar Lobes 10 µJy arcsec-2 Observing young circumstellarCoronagraph disks + With obscured central stars isPSF not Subtraction difficult.
Disk systems with unembedded, or only marginally obscured central stars are Direct Image much more observationally challenging Lower Scattering Surface and require PSF-subtracted coronagraphy. 200 µJy arcsec-2
Faint Blue Ribbon
J* = 0.33 Jy H* = 0.40 Jy
GM AUR Unembedded cTTs (K7V) Coronagraph + Age: 1.3+/-0.3 Myr PSF Subtraction
Beckwith et al 1990: Dust inferred from 1.3mm continuum
Koerner, Sargent & Beckwith 1993: 13CO(2->1) emission, Keplerian rotation.
Stapelfeldt et al 1997: WFPC-2 imaging, flared inclined disk.
21 Circumstellar Dust Inferred from Spectral Energy Distribution
GM AUR (cTTS)
SED & Spatial Dust Distribution Simultaneously Constrain Disk Models
Model as Passively Heated Disks to Determine: Geometry: Orientation, Inclination, Size Physical Characteristics: Disk Mass, Scale Height, Envelope Infall Rate Dependency of Grain Properties (λ Dependent): Dust Lane Width, Scattered Light Pattern, long-λ SED slope (Disk dust opacity, κ ~ λ-1, shallower than ISM grains, as in other disks) Simultaneously Model Scattered Light & SED: -Envelope: Tereby, Shu & Cassen (84) Rotational Collapse Geometry Curved Bipolar Evacuated Cavity (Whitney & Hartmann 93) - Dust Model & Grain Parameters per Wood (00) - Adopted Flared Disk Structure (300 AU radius, 1000 AU envelope)
ρ0 = disk density extrapolated to stellar surface ω = radial coordinate in disk midplane β h = scale height increasing with radius = h0(ω /R*) -> β = 1.25; α = 2.25; surface density Σ ~ 1/ω (D’Alessio et al 99) - Monte Carlo scattered light modeling (Whitney & Hartmann 92)
22 GM AUR Model Fitting Results OBSERVED 50° Model 55 ° Model Residuals F 1 6 0 W A B C F 1 1 0 W
-1.0 -0.5 0.0 0.5 1.0 Surface Brightness (mJy arcsec-2) LOS Inclination = 52.5° PA Major Axis = 328.5° -7 Disk Mass = 0.04 Msun Infall Rate = 1.5x10 Msun /year Envelope Mass = 0.001 Msun Scale Height = 0.008R* (z=8AU @ r=100 AU) Schneider et al. 2003, AJ, 125, 1467
Classical T-Tauri Star Disks
DoAr 25 GM AUR (cy 7) HST GO/10177 HST GTO/7233 HST GO/10177 DoAR 25 (ROXR1 23; K7V, H=8.4), in ρ Oph star forming region. Left: 0 to 5.3 mJy arcsec-2; Middle : 0 to 0.53 mJy arcsec-2)
23 Classical T-Tauri Star Disks
GO TAU (K5, H=9.6) HST GO/10177 Disk semimajor axis ~ 4.5" (490 AU). The dark zone extends to ~ 2.4" (340 AU) Stronger brightness asymmetry along the minor axis. Striated structures (nebulosity) seen the regions of high surface brightness. Left: linear 0 to 0.134 mJy arcsec-2. Right: log 0.02 to 3.2 mJy arcsec -2
Classical T-Tauri Star Disks
DM TAU (K5, H=9.8) NICMOS STIS HST GO/9136 HST GO/10177 Faint Disk - Peak Surface Brightness 17 µJy arcsec-2. Also seen in the optical (STIS, Grady). Broad Ring: ~ 320 AU in extent, 140 AU wide. Disk Interior to ~ 240 AU is dark (cleared, shadowed?) Inclination ~ 37 degrees.
24 Classical T-Tauri Star Disks
DL TAU (K5, H=9.8) HST GO/10177 HST GO/9136
PSF-Subtracted Coronagraphy
SCATTERED-LIGHT IMAGING OF (optically thin) DEBRIS DISKS
25 Debris Disks HR 4796A 70 AU Radius Debris Ring: ~10 Myr A-Type Star Multi-Band PSF-Subtracted Coronagraphic Imaging HST GO8624 HST GTO/7233 HST GO/10167
See Debes et al. Lyot Conference talk: Thu. 11:30 AM
Debris Disks HD 181327 — 86 AU Radius Ring-Like Debris Disk: ~40 Myr F-Type Star
1.1 µm Bilaterally Symmetric Ring Ring Radius = 86 ± 3.7 AU
HST GO/10177 Ring Width ~ 27 AU (FWHM) Flux Density: 9.6 ± 0.8 mJy (1.2”< r <5.0”)
Fdisk/F* = 0.17 ± 0.015% Surface Brightness (mJy/sq.”): Peak Az Med = 1.15 ± 0.09 Peak Min Axis = ~ 1.7 Directionally Pref Scattering: g(H-G) ~ 0.3 No Photocentric Offset Inclination from face-on = 37.1° ± 1.6° PA (E of N) = 332° ± 2 ° *Schneider et al. 2006, ApJ, 650, 414
26 Debris Disks HD 181327 — 86 AU Radius Ring-Like Debris Disk: ~40 Myr F-Type Star
1.1 µm HST GO/10177
*Schneider et al. 2006, ApJ, 650, 414
Debris Disks HD 181327 — 86 AU Radius Ring-Like Debris Disk: ~40 Myr F-Type Star
27 Debris Disks HD 181327 — 86 AU Radius Ring-Like Debris Disk: ~40 Myr F-Type Star
Debris Disks HD 181327 — 86 AU Radius Ring-Like Debris Disk: ~40 Myr F-Type Star
Vertical Scale Height: 6 ± 2 AU @ 87.6 AU ( radius of max. surface density)
Estimated Dust Mass: ~ 4 Mmoon of amin ~ 1 µm collionally replenished grains
*Schneider et al. 2006, ApJ, 650, 414
28 Debris Disks
HD 107416 (K5, H=9.8) HST GTO/9987 & 10330 HST GO/10177 See Metchev et al. Lyot Conference talk: Wed. 11:15 AM Two-roll combined PSF-subtracted coronagraphic images of a near face-on debris disk, r ~ 150 AU, about the Sun-like star HD 107146 (spectral type G2, J = 5.9, d = 28.5 pc). NICMOS (1350s, linear display), ACS (2150s, log display, 3x3 pixel binning).
Debris Disks HD 32297* — Near Edge-On Debris Disk Around A-Type Star HST GO/10177 1.1µm flux density = 5.28 ± 0.57 mJy (r > 0.3”) Radial (major axis) extent = 400 AU.
Fdisk/F* (1.1µm) = 0.36% ± 0.04% (similar to IRAS 25+60) Inclination = 10.5 ± 2.5 deg from edge on, PA = 236.5 ± 1deg. Radial surface brightness profiles along the disk major axis suggests azimuthal asymmetries in the dust distribution which might implicate the existence of one or more (unseen) planetary mass companions. *Schneider et al. 2005, ApJ, 639, L227
29 Debris Disks HD 32297 — Near Edge-On Debris Disk Around A-Type Star
SB ~ r
-3.72
SB ~ r SB ~ r -2.74 -3.57
TODAY HST Provides a Unique Venue for High Contrast Imaging
• UV/Optical & Near-IR (<2.4µm) Diffraction Limited Imaging • > 98% Strehl Ratios @ all λs • Highly STABLE PSF • Imaging Polarimetry: • Coronagraphy 1.9 - 2.1µm 0.2” Spatial Resolution • Intra-Orbit 75 mas/pix Field P% sensitivity > 1% Rotation
30 1 NICMOS
POLL 2MASS Ks 0.8 2MASS H Y T I V I
S 0.6 S I M S N A
R 0.4 T
R E T L I
F 0.2
0 1.4 1.6 1.8 2 2.2 2.4 WAVELENGTH (microns)
DIRECTDIRECT POLARIMETRICPOLARIMETRIC IMAGINGIMAGING OFOF (Centrally(Centrally Obscured*)Obscured*) YSOYSO DISK/ENVELOPEDISK/ENVELOPE SYSTEMSSYSTEMS
* Low Contrast
31 HST Cycle 13 - GO 10178 Imaging Polarimetry of Young Stellar Objects A Study in Dust Grain Evolution Dean C. Hines (PI), Glenn Schneider (contact co-I), Angela S. Cotera, Deborah Padgett, Karl Stapelfeldt, Dan Potter, Barbara Whitney Observed a representative sample (5 Class I and 5 Class 2) of YSOs in early evolutionary phases to investigate how the dust population evolves in size and spatial distribution during the transition from disk+envelope+protostar to disk+star systems. - L1551 IRS-5 - HH 30 - IRAS 04302+2247 - HARO 6-5B - IRAS 04016+2610 - HK Tau B - CoKu Tau-1 - HV Tau C - DG Tau B - HL Tau
I H R A B S A N 0 D 4 3 - 0 F 2 1 + 6 2 0 2 W 4 - 7
32 I T R O A T S A L 0 4 I 3 N 0 T 2 E + N 2 S 2 I 4 T 7 Y
I P R O A L S A R 0 I 4 Z 3 A 0 T 2 I + O 2 N 2 4 7
33 P O I L R A A R S I Z 0 E 4 D 3 0 I 2 N + T 2 E 2 N 4 S 7 I T Y
C H o K B u A N T D a u - F 1 6 0 W -
34 C T o O K T u A L T a I u N T E N S I T Y
C P o O K L u A R T I a Z u A T I O N
35 P O C L o A K R u I Z T E a D u I N T E N S I T Y
D H G B T A a N u D
B - F 1 6 0 W -
36 D T G O T T A a L u I B N T E N S I T Y
D P G O L T A a R u I Z B A T I O N
37 P O D L G A R T I a Z u E D B I N T E N S I T Y
Centrally Unobscured* YSO, T-Tauri, Herbig AeBe and Debris Disks Are Much More Technically Challenging…
* High Contrast
38 TODAY HST Provides a Unique Venue for High Contrast Imaging
• UV/Optical & Near-IR (<2.4µm) Diffraction Limited Imaging • > 98% Strehl Ratios @ all λs • Highly STABLE PSF • Imaging Polarimetry: • Coronagraphy 1.9 - 2.1µm 0.2” Spatial Resolution • Inter-Orbit 75 mas/pix Field P% sensitivity < 1% Rotation
See Poster: Hines et al.
CORONAGRAPHICCORONAGRAPHIC POLARIMETRICPOLARIMETRIC IMAGINGIMAGING OFOF CIRCUMSTELLARCIRCUMSTELLAR PROTOPLANETARYPROTOPLANETARY && DEBRISDEBRIS DISKSDISKS
39 Coronagraphic Polarimetry Enabing Science Demonstration (GO 9768)
TW HYA Face-On Circumstellar Disk (H=7.56, K= 7.30)
1.1 µm scattered light
Polarimetric Analysis from Coronagraphic POL0, 120, 240 Images
Coronagraphic Polarimetry Enabing Science Demonstration (GO 9768)
TW HYA Face-On Disk H=7.56 K= 7.30 UNPOL STD BD +32-3739 H=8.78 K= 8.72
TW HYA Face-On Circumstellar Disk (H=7.56, K= 7.30)
Polarimetric Analysis from Coronagraphic POL0, 120, 240 Images
40 Coronagraphic Polarimetry Enabing Science Demonstration (GO 9768)
TARGETS TYPE NAME 2MASS-H 2MASS-K FACE ON DISK TW HYA 7.558 7.297 UNPOL STD * BD +32-3739 8.775 8.721
Coronagraphic POL0, 120, 240 Scaled PSF Image Subtraction
Coronagraphic Polarimetry Enabing Science Demonstration (GO 9768)
TARGETS TYPE NAME 2MASS-H 2MASS-K FACE ON DISK TW HYA 7.558 7.297 UNPOL STD * BD +32-3739 8.775 8.721
Coronagraphic POL0, 120, 240 Scaled PSF Image Subtraction And Polarimetric Analysis
41 HST Cycle 14 HST/GO 10519 Janet Simpson (PI + 7 co-I’s) Testing the Stellar Coalescence and Accretion Disk Theories of Massive Star Formation with NICMOS
HST Cycle 15 (Execution Continuing into Cycle 16) HST/GO 10847 HST/GO 10852 G. Schneider (PI + 6 co-I’s) Dean C. Hines (PI + 14 co-I’s) Coronagraphic Coronagraphic Polarimetry with Polarimetry of NICMOS: Dust Grain HST-Resolved Evolution in T Tau Stars Debris Disks
HST Cycle 15 - Coronagraphic Polarimetry Targets T-TAURI DISKS DEBRIS DISKS GO/10852 GO/10847 GM AUR DM TAU HD 32297 HD 181327
SZ 82 GO TAU AU MIC HR 4796
GM AUR GTO/7233 DM TAU GO/10177 DoAr 25 HD 107146 HD 61005 SZ 82 GO/10177 GO TAU GO/10177 DOAR 25 GO/10177 HD 32297 GO/10177 HD 181327 GO/10177 AU MIC GO/10228 HR 4796 GTO/7233 HD 107146 GO/10177 See Hines et al. talk: HD 61005 GO/10527 Thu. 10:30 AM
42 GM AUR
2µm Total Intensity HST GO/10852 1.1 µm & 1.6 µm HST GO/10852 PSF Subtracted Coronagraphic Polarimetry HST GO/7233
43 HD 32297 HST GO/10847
PSF Subtracted Coronagraphic Polarimetry
44 HST Cycle 16 HST/GO 11155 Marshall Perrin (PI + 11 co-I’s) Dust Grain Evolution in Herbig Ae Stars: NICMOS Coronagraphic Imaging and Polarimetry
First Observations (HD 141569)… TOMORROW! (stay tuned…)
HST: Unique Venue for High Contrast Imaging SM4 (11 Sept 2008) & 4th Generation STIS ? NICMOS 2 Focal Plane Occulting Wedges Lyot Coronagraph Width: 1” - 3” r = 0.3”, f/45, 76 mas/pix Unfiltered (CCD broad response) 3.2 λ/D @ 1.1 µm
WFC-3 & COS No Coronagraphs
3rd Generation ACS ? Abberated-beam Coronagraph r = 0.9” & 1.8” masks 3.2 λ/D @ 1.1 µm
45