NICMOS & VLT Imaging of 2MASSWJ (aka 2M1207) A Planetary-Mass Companion to a Young Brown Dwarf Glenn Schneider (Steward Observatory, U. Arizona) HST/GO Team I. Song, PI (Gemini Obs.) G. Schneider (UofA) B. Zuckerman (UCLA) E. Becklin (UCLA) P. Lowrance (Caltech) B. Macintosh (LLNL) M. Bessell (ANU) VLT Collaborators C. Dumas (ESO) G. Chauvin (ESO) First imaging detection of a gravitationally bound, extrasolar, planetary-mass companion.

NICMOS CORONAGRAPHIC SURVEY OF 116 NEARBY ( pc from Earth) YOUNG (a few million to ~ 100 million years) STARS & BROWN DWARFS STARTED JULY, 2004 (HST cycle 13)* *see: poster # 34 HST/GO Team I. 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 116 NEARBY ( 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 116 NEARBY ( 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 116 NEARBY ( pc from Earth) YOUNG (a few million to ~ 100 million years) STARS & BROWN DWARFS STARTED JULY, 2004 (HST cycle 13) Including 2MASSWJ (2M1207)

NICMOS CORONAGRAPHIC SURVEY OF 116 NEARBY ( 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 116 NEARBY ( 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 (1976), suggested at ~ 7 M jup ), with detection sensitivities in the M jup range at 10’s to 100’s of AU.

NICMOS CORONAGRAPHIC SURVEY OF 116 NEARBY ( pc from Earth) YOUNG (a few million to ~ 100 million years) STARS & BROWN DWARFS including 2M1207 STARTED JULY, 2004 (HST cycle 13) Giant Planet Companion Candidate May, 2004 VLT Collaborators Suggested 2M1207: A Giant Planet Candidate Near a Young Brown Dwarf: Direct VLT/NACO * Observations Using 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 ~ 780 mas” *NACO/CONICA: (Near-IR camera) Adaptive Optics Configuration

2M1207 TW Hya Assn Member Age: 8 +4/-3 Myrs Distance: 70 ± 20 pc Spectrum: M Jupiter-Mass BD Zuckerman et al 2001 (ApJ ) Gziz 2002 (ApJ ) Ortega et al 2002 (ApJ ) Song et al 2003 (ApJ ) Mohanty et al 2003 (A&A ) Gizis & Bharat 2004 (ApJ ) Sterzik et al 2004 (A&A ) Zuckerman & Song 2004 (ARA&A ) 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  m With broad absorption indicative of H 2 0, 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” pc (projected on sky) Location of 2M1207 Giant Planet Companion Candidate HST/NICMOS CAMERA 1 FOLLOW-UP IMAGING Epoch 2: 08/28/2004 (4 month astrometric baseline w.r.t VLT) PSF subtracted image F090M (0.9  m) F110M (1.1  m) F160W (1.6  m) 40 +/ /- 8 pc

At 0.9 microns the 2M1207b: - has an apparent magnitude of (08/28/2004) - is 720 times fainter than 2M1207 (mag ) - 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 from 2M1207A and improve the image contrasts. F090M(0.9  m) F110M(1.1  m) F160W(1.6  m) 2M1207b is 774 mas from 2M1207A

HST/NICMOS Camera 1 Observations of 2M1207 Two Orbits at Two Field Orientations 9.9° Roll - Constrained by Available Guide Stars F090M(0.9  m) F110M(1.1  m) F160W(1.6  m) 4-Point Dither Combined Images ROLL ORIENTATION # 1

F090M(0.9  m) F110M(1.1  m) F160W(1.6  m) 4-Point Dither Combined Images ROLL ORIENTATION # 2 HST/NICMOS Camera 1 Observations of 2M1207 Two Orbits at Two Field Orientations 9.9° Roll - Constrained by Available Guide Stars

HST/NICMOS Camera 1 Observations of 2M1207 F090M(0.9  m) F110M(1.1  m) F160W(1.6  m) 4-Point Dither Combined Images DIFFERENCE IMAGE

HST/NICMOS Camera 1 Observations of 2M1207 F090M(0.9  m) F110M(1.1  m) F160W(1.6  m) 4-Point Dither Combined Images SIMULTANEOUS BEST-FIT OPTICAL MODEL

HST/NICMOS Camera 1 Observations of 2M1207 F090M(0.9  m) F110M(1.1  m) F160W(1.6  m) 4-Point Dither Combined Images BEST-FIT MODEL SUBTRACTIONS - Negative Image Nulling

F090M(0.9  m) F110M(1.1  m) F160W(1.6  m) 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(0.9  m) F110M(1.1  m) F160W(1.6  m) 4-Point Dither Combined Images COMBINATION IMAGES

BLUE = F090M(0.9  m) GREEN=F110M(1.1  m) RED=F160W(1.6  m) Epoch 2 astrometry - NICMOS -Schneider et al 2004 AAS

BLUE = F090M(0.9  m) GREEN=F110M(1.1  m) RED=F160W(1.6  m) Common Proper Motion Probability*: 2.6  (99.1%) -Schneider et al 2004 AAS *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 MAGNITUDE waveln 2M1207b 2M1207A  mag 0.9  m: ± ± ±  m: ± ± ±  m: ± ± ±  m: ± ± ±  m: ± ± ± 0.17 } BOTH } HST VLT

Log 10 Age (years) 80M jup 14M jup JUPITER SATURN STARS (Hydrogen burning) BROWN DWARFS (Deuterium burning) PLANETS 200M jup Evolution of M Dwarf Stars, Brown Dwarfs and Giant Planets (from Adam Burrows) Log 10 L/L sum sun Cooling Curves for Substellar Objects 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 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” pc (projected on sky) Location 2M1207A 2M1207b HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING Epoch 5: 26 APRIL month astrometric baseline w.r.t 1st VLT image 7 month astrometric baseline w.r.t. 1st NICMOS image PSF subtracted images F090M (0.9  m) F145M (1.45  m) F160W (1.6  m)

THEORETICAL EGP SPECTRA (A. Burrows) HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING F145M (1.45  m) imaging in H 2 0 absorption band F145M

2M1207A/b - 26 APR 05 NICMOS F160W (1.6  m) -2 to +2 ADU/second/pixel HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

2M1207A/b - 26 APR 05 NICMOS F145M (1.45  m) -0.4 to ADU/second/pixel HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

2M1207A/b - 26 APR 05 NICMOS F090M (0.9  m) to ADU/second/pixel HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING

2M1207A/b - 26 APR 05 NICMOS F090M (0.9  m) to ADU/second/pixel

HST/NICMOS CAMERA 1 2nd FOLLOW-UP IMAGING F145M (1.45  m) imaging in H 2 0 absorption band 2M1207b APPARENT MAGNITUDES  m 04/27/04 VLT 08/28/2004 HST 04/26/2005 HST ± ± ± ± ± ± ± ± 0.14

Epoch 5 astrometry - NICMOS Unequivocal common P.M.

The 2M1207 System MASS(A) ~ 25 M jup, MASS(b) < ~ 5 M jup Model Dependent: Burrows et al 1997, Chabrier et al 2000, Baraffe et al M1207A mass derived from surface gravity from spectral line shapes (Mohantey et al 2003*) with distance and T eff 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 M jup ? 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 M jup, MASS(b) < ~ 5 M jup Model Dependent: Burrows et al 1997, Chabrier et al 2000, Baraffe et al 2001 a min ~ 40 AU*, P min ~ 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 A 2MASSWJ b Field Star 2M1207b 2b Toobe Or… not to be? (Trivial?) Nomenclature: 2MASSWJ b 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 A 2MASSWJ b 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? 0.9  m 1.1  m 1.6  m 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 of 2MASSWJ (aka 2M1207) A Planetary-Mass Companion to a Young Brown Dwarf Glenn Schneider (Steward Observatory, U. Arizona) HST/GO Team I. Song, PI (Gemini Obs.) G. Schneider (UofA) B. Zuckerman (UCLA) E. Becklin (UCLA) P. Lowrance (Caltech) B. Macintosh (LLNL) M. Bessell (ANU) VLT Collaborators C. Dumas (ESO) G. Chauvin (ESO)