NICMOS & VLT Imaging of2MASSWJ 1207334-393254 (aka 2M1207)

A Planetary-Mass Companion to aYoung Brown Dwarf

Glenn Schneider (Steward Observatory, U. Arizona)

HST/GO 10176 TeamI. Song, PI (Gemini Obs.)G. Schneider (UofA)B. Zuckerman (UCLA)E. Becklin (UCLA)P. Lowrance (Caltech)B. Macintosh (LLNL)M. Bessell (ANU)

VLT CollaboratorsC. Dumas (ESO)G. Chauvin (ESO)

First imaging detection of a gravitationallybound, extrasolar, planetary-mass companion.

NICMOS CORONAGRAPHIC SURVEY OF 116NEARBY (20 - 100 pc from Earth)YOUNG (a few million to ~ 100 million years)STARS & BROWN DWARFSSTARTED JULY, 2004 (HST cycle 13)*

*see: poster # 34

HST/GO 10176 TeamI. Song, PI (Gemini Obs.)G. Schneider (UofA)B. Zuckerman (UCLA)E. Becklin (UCLA)P. Lowrance (Caltech)B. Macintosh (LLNL)M. Bessell (ANU)

NICMOS CORONAGRAPHIC SURVEY OF 116NEARBY (20 - 100 pc from Earth)YOUNG (a few million to ~ 100 million years)STARS & BROWN DWARFS STARTED JULY, 2004 (HST cycle 13)

Larger angular separations: - less challenging image contrasts - more accurate photometry

NICMOS CORONAGRAPHIC SURVEY OF 116NEARBY (20 - 100 pc from Earth)YOUNG (a few million to ~ 100 million years)STARS & BROWN DWARFS STARTED JULY, 2004 (HST cycle 13)

Thermally emissive: - INFRARED “bright” from residual heat of formation

NICMOS CORONAGRAPHIC SURVEY OF 116NEARBY (20 - 100 pc from Earth)YOUNG (a few million to ~ 100 million years)STARS & BROWN DWARFS STARTED JULY, 2004 (HST cycle 13)

Including 2MASSWJ 1207334-393254 (2M1207)

NICMOS CORONAGRAPHIC SURVEY OF 116NEARBY (20 - 100 pc from Earth)YOUNG (a few million to ~ 100 million years)STARS & BROWN DWARFS STARTED JULY, 2004 (HST cycle 13)

Program Status: 77% Completed (02 May 2005)

NICMOS CORONAGRAPHIC SURVEY OF 116NEARBY (20 - 100 pc from Earth)YOUNG (a few million to ~ 100 million years)STARS & BROWN DWARFS STARTED JULY, 2004 (HST cycle 13)

• Identifying individual EGP candidates for astrometric, photometric, spectroscopic follow-up.

• Will provide statistics on EGP population distribution at orbital distances beyond the current reach of Radial Velocity surveys.

• Will inform on minimum mass for Jeans mass fragmentation (e.g., Low & Bell 176 367 (1976), suggested at ~ 7 Mjup), with detection sensitivities in the 1 - 10 Mjup range at 10’s to 100’s of AU.

NICMOS CORONAGRAPHIC SURVEY OF 116NEARBY (20 - 100 pc from Earth)YOUNG (a few million to ~ 100 million years)STARS & BROWN DWARFS including 2M1207STARTED JULY, 2004 (HST cycle 13)

Giant Planet CompanionCandidate

May, 2004VLT CollaboratorsSuggested 2M1207:

A Giant Planet CandidateNear a Young Brown Dwarf:Direct VLT/NACO* ObservationsUsing IR Wavefront Sensing

Oct 2004: A & A, 425, L29

VLT/AO TEAM (NACO)G. Chauvin, A.-M. Lagrange, C. Dumas, B. Zuckerman,D. Mouillet, I. Song, J.-L. Beuzit, P. Lowrance

“Very faint, very red object @ ~ 780 mas”

*NACO/CONICA: (Near-IR camera) Adaptive Optics Configuration

2M1207 TW Hya Assn Member Age: 8 +4/-3 MyrsDistance: 70 ± 20 pcSpectrum: M8.525 Jupiter-Mass BD

Zuckerman et al 2001 (ApJ 562 87)Gziz 2002 (ApJ 575 484)

Ortega et al 2002 (ApJ 575 75)Song et al 2003 (ApJ 559 342)

Mohanty et al 2003 (A&A 441 517)Gizis & Bharat 2004 (ApJ 608 113)

Sterzik et al 2004 (A&A 427 245)Zuckerman & Song 2004 (ARA&A 42 685)

VLT/NACO Discovery Image (H, Ks, L’)

*

* d ~ 52 +/-8 pc Mamajek, poster 26 this symposium

(revised position & uncertainties)

VLT/AO TEAM (NACO) G. Chauvin (ESO), A.-M. Lagrange (Obs. de Grenoble) C. Dumas (ESO), B. Zuckerman (UCLA), D. Mouillet (Observatoire Midi-Pyrénées), I. Song (Gemini Observatory), J.-L. Beuzit (Observatoire de Grenoble), P. Lowrance (SSC/IPAC)

VLT/NACO OBSERVATIONS (APRIL/JUNE 2004) - IMAGING IN 3 SPECTRAL BANDS > 1.6 m (H, Ks, L’) “Colors” suggestive of Young Extra-Solar Giant Planet (EGP) - GPCC UNDETECTED IN 1.26 m J-band Source too faint for declining AO performance at short ’s - LOW RESOLUTION SPECTROSCOPY @ 1.5 - 1.8 m With broad absorption indicative of H20, expected for young EGPs

SUGGESTED:Mass = 5 ± 2 x Jupiter,

Temperature = 1250K ± 200K

* Scholz et al (2005)” (-78 +/- 11 , -24 +/ -9 ) mas/year

2M1207 Proper Motion: ~ (-55 , -24 )* mas/year

Rapid Common PM Follow-up

0.774”

54 AU

@ 70 pc

(projected on sky)

Location of 2M1207

Giant Planet CompanionCandidate

HST/NICMOS CAMERA 1 FOLLOW-UP IMAGINGEpoch 2: 08/28/2004 (4 month astrometric baseline w.r.t VLT)

PSF subtracted image F090M (0.9m) F110M (1.1m) F160W (1.6m)

40 +/- 6 AU @ 52 +/- 8 pc

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

NICMOS observations exploit the stability of the HST Point Spread Function to reduce the background light from2M1207A and improve the image contrasts.

F090M(0.9m) F110M(1.1m) F160W(1.6m)

2M1207b is 774 mas from 2M1207A

HST/NICMOS Camera 1 Observations of 2M1207Two Orbits at Two Field Orientations

9.9° Roll - Constrained by Available Guide Stars

F090M(0.9m) F110M(1.1m) F160W(1.6m)

4-Point Dither Combined ImagesROLL ORIENTATION # 1

F090M(0.9m) F110M(1.1m) F160W(1.6m)

4-Point Dither Combined ImagesROLL ORIENTATION # 2

HST/NICMOS Camera 1 Observations of 2M1207Two Orbits at Two Field Orientations

9.9° Roll - Constrained by Available Guide Stars

HST/NICMOS Camera 1 Observations of 2M1207

F090M(0.9m) F110M(1.1m) F160W(1.6m)

4-Point Dither Combined ImagesDIFFERENCE IMAGE

HST/NICMOS Camera 1 Observations of 2M1207

F090M(0.9m) F110M(1.1m) F160W(1.6m)

4-Point Dither Combined ImagesSIMULTANEOUS BEST-FIT OPTICAL MODEL

HST/NICMOS Camera 1 Observations of 2M1207

F090M(0.9m) F110M(1.1m) F160W(1.6m)

4-Point Dither Combined ImagesBEST-FIT MODEL SUBTRACTIONS - Negative Image Nulling

QuickTime™ and aPhoto - JPEG decompressor

are needed to see this picture.

F090M(0.9m) F110M(1.1m) F160W(1.6m)

HST/NICMOS Camera 1 Observations of 2M1207

BEST-FIT MODEL SUBTRACTIONS

HST/NICMOS Camera 1 Observations of 2M1207

INVERT SECOND ORIENTATION

HST/NICMOS Camera 1 Observations of 2M1207

ROTATE TO SAME SKY ORIENTATION

HST/NICMOS Camera 1 Observations of 2M1207

ROTATE TO SAME SKY ORIENTATION

HST/NICMOS Camera 1 Observations of 2M1207

F090M(0.9m) F110M(1.1m) F160W(1.6m)

4-Point Dither Combined ImagesCOMBINATION IMAGES

QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.

BLUE = F090M(0.9m)GREEN=F110M(1.1m)RED=F160W(1.6m)

Epoch 2 astrometry - NICMOS -Schneider et al 2004 AAS 205 114

QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.

BLUE = F090M(0.9m)GREEN=F110M(1.1m)RED=F160W(1.6m)

Common Proper Motion Probability*: 2.6 (99.1%) -Schneider et al 2004 AAS 205 114

*Predicated on earlier, more uncertain, PM for 2M1207

than Scholz et al 2005(shown here).

VLT/NACO & HST/NICMOS PHOTOMETRY 4/27/2004 & 8/28/2004

~Temp. < 1200 K

Temp. = 2750 K

APPARENT MAGNITUDEwaveln 2M1207b 2M1207A       mag          0.9m: +22.34 ± 0.35 +15.20 ± 0.03 +7.14 ± 0.351.1m: +20.16 ± 0.15 +13.29 ± 0.03 +7.02 ± 0.151.6m: +18.24 ± 0.02 +12.62 ± 0.02 +5.62 ± 0.032.2m: +16.93 ± 0.11 +11.95 ± 0.03 +4.98 ± 0.113.8m: +15.28 ± 0.14 +11.38 ± 0.14 +3.90 ± 0.17}

BOTH}HST

VLT

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 Objects

NICMOS Companion Detection Limit (M type primary)NICMOS Companion Detection Limit (M type primary)

2M1207A

2M1207b

HST/NICMOS CAMERA 1 OBSERVATIONS (AUGUST 2004) : - IMAGING IN 3 SPECTRAL BANDS < 1.6 m (H, 1.1 & 0.9 m) Provided short wavelength diagnostic flux densities (& color indices) - 2M1207B IMAGED & PHOTOMETERED IN ALL BANDS “Colors” and Flux Densities Consistent with Young EGP Mass Object

.

CLEARCLOUDY

Teff = 1200KAge = 6.5 Myr[g] = 3.778-----------------5 M jupiter1.44 R jupiter0.000041 Lsun

0.2

0.4

0.6

0.8

1

0.8 1 1.2 1.4 1.6 1.8Wavelength (microns)

F110M F160WF090M

THEORETICAL EGP SPECTRA (A. Burrows)

IMPLICATED: Temperature < 1200K, Mass < 5 Jupiter.~ ~

VLT/SPECTRUM

Epoch 3 & 4 astrometry - VLT(Chauvin et al 2005 astro-ph 4/29/05)

0.774”

54 AU

@ 70 pc

(projected on sky)

Location 2M1207A

2M1207b

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGINGEpoch 5: 26 APRIL 2005

12 month astrometric baseline w.r.t 1st VLT image7 month astrometric baseline w.r.t. 1st NICMOS image

PSF subtracted images F090M (0.9m) F145M (1.45m) F160W (1.6m)

.

CLEARCLOUDY

Teff = 1200KAge = 6.5 Myr[g] = 3.778-----------------5 M jupiter1.44 R jupiter0.000041 Lsun

0.2

0.4

0.6

0.8

1

0.8 1 1.2 1.4 1.6 1.8Wavelength (microns)

F110M F160WF090M

THEORETICAL EGP SPECTRA (A. Burrows)

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

F145M (1.45m) imaging in H20 absorption band

F145M

2M1207A/b - 26 APR 05 NICMOS F160W (1.6m)

-2 to +2 ADU/second/pixel

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

2M1207A/b - 26 APR 05 NICMOS F145M (1.45m)

-0.4 to + 0.4 ADU/second/pixel

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

2M1207A/b - 26 APR 05NICMOS F090M (0.9m)

-0.03 to + 0.03 ADU/second/pixel

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING2M1207A/b - 26 APR 05NICMOS F090M (0.9m)

-0.03 to + 0.03 ADU/second/pixel

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

F145M (1.45m) imaging in H20 absorption band

2M1207b APPARENT MAGNITUDES

m 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 ± 0.031.60 +18.24 ± 0.02 +18.27 ± 0.02 2.20 +16.93 ± 0.11 3.90 +15.28 ± 0.14

Epoch 5 astrometry - NICMOSUnequivocal common P.M.

The 2M1207 System

MASS(A) ~ 25 Mjup, MASS(b) < ~ 5 Mjup

Model Dependent: Burrows et al 1997, Chabrier et al 2000, Baraffe et al 2001

2M1207A mass derived from surface gravity from spectral line shapes (Mohantey et al 2003*) with distance and Teff get luminosity and radius.Distance uncertain by ~ 30% (70 ± 20 pc). Need trigonometric parallax!

How “GOOD” are Non-Dynamical Mass Estimates?(Corollary: How “good” are the models?)

*For upper Sco Baraffe may overestimate mass, so 2M1207b < 5 Mjup?

AB Dor. Models suggest BD mass. Close et al (2005) dynamical observations suggests models underestimate substellar masses.AB Dor at Stellar/BD boundary. Gabor/Mohantey suggest models will underestimate masses in that domain but may overestimate planetary masses.

The 2M1207 System

MASS(A) ~ 25 Mjup, MASS(b) < ~ 5 Mjup

Model Dependent: Burrows et al 1997, Chabrier et al 2000, Baraffe et al 2001

amin ~ 40 AU*, Pmin ~ 1500 yr * for 52 pc

HST/NICMOS differential astrometric precison ~ 2 mas.Annual measures with 1 precision w.r.t. orbital motion.

Mean Orbital Motion = 14.4’/year(circular, face on): ~ 3.5 mas of apparent motion/yr

Thinking toward the future…

(1° around the orbit in 5 years…)

It is of Planetary Mass, but is it a “PLANET”?

2MASSWJ 1207334-393254A

2MASSWJ 1207334-393254b

Field Star

2M1207b

2b

Toobe

Or… not to be?

(Trivial?)

Nomenclature: 2MASSWJ 1207334-393254b

Question in Conclusion:

(how did it form: collision, embryonic-ejection, core accretion, grav. collapse/ fragmentation, photo-evap in massive SF association?)

That is the question!

It is of Planetary Mass, but Is it a “PLANET”?

2MASSWJ 1207334-393254A

2MASSWJ 1207334-393254b

Field Star

Question in Conclusion:

(how did it form: collision, embryonic-ejection, core accretion, grav. collapse/ fragmentation, photo-evap in massive SF association?)

WHAT NEXT?0.9m 1.1m 1.6m

HST CYLE 14 - GO/10538

PSF-Subtracted Grism Spectrophotometry

0.8 – 1.2 m (40 ksec) & 1.1 – 1.8 m (10 ksec) in 18 HST Orbits

NICMOS & VLT Imaging of2MASSWJ 1207334-393254 (aka 2M1207)

A Planetary-Mass Companion to aYoung Brown Dwarf

Glenn Schneider (Steward Observatory, U. Arizona)

HST/GO 10176 TeamI. Song, PI (Gemini Obs.)G. Schneider (UofA)B. Zuckerman (UCLA)E. Becklin (UCLA)P. Lowrance (Caltech)B. Macintosh (LLNL)M. Bessell (ANU)

VLT CollaboratorsC. Dumas (ESO)G. Chauvin (ESO)