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Micro-Arcsecond Astrometry of the Galactic Center (Th. Paumard)

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Micro-Arcsecond Astrometry of the Galactic Center (Th. Paumard) Introduction Science Conclusions Astrometry in the Galactic Centre Thibaut Paumard GRAVITY project scientist LESIA – CNRS / Observatoire de Paris Work supported by European program FP7 OPTICON II WP4 Interferometry September 8, 2015 T. Paumard Astrometry in the GC Introduction Science Conclusions Outline 1 Introduction What is Astrometry exactly? Structure of the central parsec from classical imaging GRAVITY 2 Prospective science with GRAVITY Structure of the central parsec Binaries and multiple systems The Potential around Sgr A* Astrometry of the flares More realistic (and complex) models 3 Conclusions T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Outline 1 Introduction What is Astrometry exactly? Structure of the central parsec from classical imaging GRAVITY 2 Prospective science with GRAVITY Structure of the central parsec Binaries and multiple systems The Potential around Sgr A* Astrometry of the flares More realistic (and complex) models 3 Conclusions T. Paumard Astrometry in the GC Seemingly Measure position: in which coordinates? Position: 2D ? 3D? Movement: relative to what? Precise: what does it mean? Not addressed by the definition For what purpose? How is it done? Introduction Science Conclusions astrometry structure GRAVITY Seemingly clear and falsely simple definition According to wikipedia: Astrometry is the branch of astronomy that involves precise measurements of the positions and movements of stars and other celestial bodies. T. Paumard Astrometry in the GC Not addressed by the definition For what purpose? How is it done? Introduction Science Conclusions astrometry structure GRAVITY Seemingly clear and falsely simple definition According to wikipedia: Astrometry is the branch of astronomy that involves precise measurements of the positions and movements of stars and other celestial bodies. Seemingly Measure position: in which coordinates? Position: 2D ? 3D? Movement: relative to what? Precise: what does it mean? T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Seemingly clear and falsely simple definition According to wikipedia: Astrometry is the branch of astronomy that involves precise measurements of the positions and movements of stars and other celestial bodies. Seemingly Measure position: in which coordinates? Position: 2D ? 3D? Movement: relative to what? Precise: what does it mean? Not addressed by the definition For what purpose? How is it done? T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Dream and reality Reality Dream 3 per epoch: Real 3D position and “Movements”, i.e. ideally α, right ascension predictions for δ, declination 3D position; Usually relative to some 3D velocity; reference source; (3D acceleration...) vr , radial velocity at any past and future date. using spectroscopy, usually relative to Earth. T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Dream and reality Reality Dream 3 per epoch: Real 3D position and “Movements”, i.e. ideally α, right ascension predictions for δ, declination 3D position; Usually relative to some 3D velocity; reference source; (3D acceleration...) vr , radial velocity at any past and future date. using spectroscopy, usually relative to Earth. T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Example: orbital motion Star orbital parameters: 6 parameters, e.g. initial position and velocity, or position angle of line of nodes; inclination of orbital plane; angle yielding direction of major axis; semi-major axis; excentricity; elongation at given date. T. Paumard Astrometry in the GC Rotating black-hole Orientation of spin axis (2 angles); Spin parameter. Total: 16 in GR black-hole. More for alternative theory Introduction Science Conclusions astrometry structure GRAVITY Example: orbital motion Parameters of massive particle 3D position and velocity Star orbital parameters: (assuming isolated!); 6 parameters, e.g. initial mass. position and velocity, or position angle of line of Total 13 parameters in nodes; Newtonian case. inclination of orbital plane; angle yielding direction of major axis; semi-major axis; excentricity; elongation at given date. T. Paumard Astrometry in the GC More for alternative theory Introduction Science Conclusions astrometry structure GRAVITY Example: orbital motion Parameters of massive particle 3D position and velocity Star orbital parameters: (assuming isolated!); 6 parameters, e.g. initial mass. position and velocity, or position angle of line of Total 13 parameters in nodes; Newtonian case. inclination of orbital plane; Rotating black-hole angle yielding direction of Orientation of spin axis (2 major axis; angles); semi-major axis; Spin parameter. excentricity; Total: 16 in GR black-hole. elongation at given date. T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Example: orbital motion Parameters of massive particle 3D position and velocity Star orbital parameters: (assuming isolated!); 6 parameters, e.g. initial mass. position and velocity, or position angle of line of Total 13 parameters in nodes; Newtonian case. inclination of orbital plane; Rotating black-hole angle yielding direction of Orientation of spin axis (2 major axis; angles); semi-major axis; Spin parameter. excentricity; Total: 16 in GR black-hole. elongation at given date. More for alternative theory T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Constituents of central parsecs The CND (torus of molecular gas); Sgr A Ouest (the Minipiral, dust+ionised gas) + Sgr A* (the SMBH); The nuclear cluster of early type stars; The S cluster; Key questions Formation of massive stars mechanisms involved in Blitz et al. starburst galaxies and AGNs black-hole physics T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Constituents of central parsecs The CND (torus of molecular gas); Sgr A Ouest (the Minipiral, dust+ionised gas) + Sgr A* (the SMBH); The nuclear cluster of early type stars; The S cluster; Key questions Formation of massive stars mechanisms involved in starburst galaxies and Roberts & Goss ’93, VLA H92α AGNs black-hole physics T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Constituents of central parsecs The CND (torus of molecular gas); Sgr A Ouest (the Minipiral, dust+ionised gas) + Sgr A* (the SMBH); The nuclear cluster of early type stars; The S cluster; Key questions Formation of massive stars mechanisms involved in NACO H, K’, L starburst galaxies and AGNs black-hole physics T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY Constituents of central parsecs The CND (torus of molecular gas); Sgr A Ouest (the Minipiral, dust+ionised gas) + Sgr A* (the SMBH); The nuclear cluster of early type stars; The S cluster; Key questions NACO 3 epochs, Formation of massive stars SINFONI spectra mechanisms involved in starburst galaxies and AGNs black-hole physics T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY In the context of the Galactic Center Goal and mean Relate the components observed at various wavelength; 3D structure and kinematics; Interactions; Reference frame Sgr A* is a natural reference (everything rotates around it!), but not bright in the infrared: need intermediate references (e.g. masers, stars associated with radio emission; beware of nasty effects (image distorsions...) some instrumental effects are time-dependent. T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY ' 100 early type stars within a 0.5 pc radius About 100 early type stars detected 5 elements per star: 2D pos, 3D vel. Many stars, few elements ) statistical study T. Paumard Astrometry in the GC Introduction Science Conclusions astrometry structure GRAVITY The OB stars are mostly on projected tangential orbits Clock w is e s ys te m (CW S) Counte r-clock w is e s ys te m (CCW S) T. Paumard Astrometry in the GC ;k k k k k ;k k k k ;k k k k k k k k k k k k θ θ φ φ The early-type stars live in two disks 0 1 0 1 vx = v sin θ cos ' sin i cos Ω ~v = @ vy = v sin θ sin ' A ; ~n = @ − sin i sin Ω A vz = v cos θ − cos i ~v ? ~n , ~n · ~v = 0 = sin i cos Ω sin θ cos ' − sin i sin Ω sin θ sin ' − cos i cos θ , cotan θ = tan i cos(Ω + ' ) : ;k k k k k ;k k k k ;k k k k k k k k k k k k θ θ φ φ The early-type stars live in two disks 0 1 0 1 vx = v sin θ cos ' sin i cos Ω ~v = @ vy = v sin θ sin ' A ; ~n = @ − sin i sin Ω A vz = v cos θ − cos i ~v ? ~n , ~n · ~v = 0 = sin i cos Ω sin θ cos ' − sin i sin Ω sin θ sin ' − cos i cos θ , cotan θ = tan i cos(Ω + ' ) : ;k k k k k ;k k k k ;k k k k k k k k k k k k θ θ φ φ The early-type stars live in two disks 0 1 0 1 vx = v sin θ cos ' sin i cos Ω ~v = @ vy = v sin θ sin ' A ; ~n = @ − sin i sin Ω A vz = v cos θ − cos i ~v ? ~n , ~n · ~v = 0 = sin i cos Ω sin θ cos ' − sin i sin Ω sin θ sin ' − cos i cos θ , cotan θ = tan i cos(Ω + ' ) : θ θ φ φ The early-type stars live in two disks 0 1 0 1 vx;k = v k sin θk cos 'k sin i cos Ω ~v k = @ vy;k = v k sin θk sin 'k A ; ~n = @ − sin i sin Ω A vz;k = v k cos θk − cos i ~v k ? ~n , ~n · ~v k = 0 = sin i cos Ω sin θk cos 'k − sin i sin Ω sin θk sin 'k − cos i cos θk , cotan θk = tan i cos(Ω + 'k ) : θ θ φ φ The early-type stars live in two disks 0 1 0 1 vx;k = v k sin θk cos 'k sin i cos Ω ~v k = @ vy;k = v k sin θk sin 'k A ; ~n = @ − sin i sin Ω A vz;k = v k cos θk − cos i ~v k ? ~n , ~n · ~v k = 0 = sin i cos Ω sin θk cos 'k − sin i sin Ω sin θk sin 'k − cos i cos θk , cotan θk = tan i cos(Ω + 'k ) : confirms Genzel et al.
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