in formation Stars in motion Jessica R. Lu Institute for Astronomy University of Hawaii
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1 Stars in formation in motion Jessica R. Lu Institute for Astronomy University of Hawaii
2 Stars in formation in motion
3 105 Msun 104 Msun 103 Msun
4 Frontiers in star formation include massive young clusters in a range of environments. stellar initial mass function vs. environment cluster structure and dynamics as probe of star formation process as probe of cluster evolution/fate cluster mass function vs. galaxy properties
5 Massive young clusters are difficult to find and observe in detail. crowded (5-100 stars/arcsec^2) deeply embedded (AV = 10-30) large on the sky membership is difficult distance is uncertain high resolution infrared > 2 FOV astrometry spectroscopy
6 W51 - one of the most luminous star forming complexes in the Galaxy. JHK Mosaic from UKIDSS Galactic Plane Survey 1 degree wide
7 Current AO systems have too small FOV to properly characterize W51 and other GMCs. UKIDSS JHK 0.8 resolution
8 Current AO systems have too small FOV. Gemini MCAO - ideal system for clusters at 3-10 kpc JWST - ideal for characterizing unresolved clusters in other galaxies need bigger FOV for nearby massive clusters (especially lower metallicity outer Galaxy clusters) still need good resolution for precise astrometry moderate resolution spectroscopy for many objects
9 Stars in formation in motion
10 Proper motions are a powerful tool for identifying cluster members. Commonly used in globular clusters. High spatial resolution optical capabilities of HST. Massive young clusters require better astrometric precision. Massive young clusters require infrared astrometry. Anderson+ 2006
11 Successful pilot project for W51. Done in 1 year with Keck OA (55 mas resolution). Need bigger FOV to cover whole cluster/gmc. Need spectroscopy to calibrate masses. Lu et al. in prep
12 Membership gives precise IMF and test bed for stellar and cluster evolution. NGC 3603 Harayama no membership info
13 Currently, relative astrometry is precise; but reference frames are a problem (FOV). Existing Telescopes with AO Crowded Fields: 170 µas Sparse Fields: µas Absolute Astrometry:?? MCAO??
14 Astrometry is relevant to many additional science cases. Massive young star clusters Galactic Center - stellar populations, dynamics, structure Astrometric microlensing from isolated black holes Parallaxes - faint, red, crowded objects Binary/planetary companion orbits Gravitational lensing of galaxies Intermediate mass black holes Local group galaxies: orbits and internal kinematics for dark matter Jet proper motions Astrometric wobble from planets: crowded, faint, red = what Gaia won t do. Hypervelocity stars, runaway stars from other galaxies
15 Slides Internal dynamics are a powerful test of star formation theories. in formation Save As: jlu_gemini_ao.key.pdf _06_geminiAO 2 FAVORITES 3 Fill 4 5 Graphic Macintosh HD Desktop jlu Stars Applications in motion Documents SHARED DEVICES Stroke 6 Remote Disc 7 Install OS X 8 Shadow Title: jlu_gemini_ao.key Angle: 9 Author: Jessica Lu Offset 10 Reflection Subject: Opacity Save 64% Blur Keywords: Processing page: Opacity 12 Jessica R. Lu Institute for Astronomy University of Hawaii New Folder Security Options... Cancel Krumholz+ Cancel Save
16 Galactic center stellar population studies require high resolution imaging/spectroscopy.
17 Masses of stars, brown dwarfs, and remnants can be measured with orbits. Marois Konopacky+ 2008
18 Gravitational lensing requires good astrometry (~mas) to constrain mass distributions of the lens. Marshall & Treu 2008
19 Astrometric microlensing can probe isolated stellar mass black holes. Sahu STScI talk 2011 Ofek & Lu (in prep.)
20 Astrometric microlensing can probe isolated stellar mass black holes. Ofek & Lu (in prep.) Sahu Talk STScI 2011
21 Astrometric microlensing can probe isolated stellar mass black holes. Sahu Talk STScI 2011
22 Intermediate mass black holes in globular clusters. van der Marel+ 2009
23 Astrometry is relevant to many additional science cases. Galactic Center - stellar populations, dynamics, structure Astrometric microlensing from isolated black holes Parallaxes - faint, red, crowded objects Binary/planetary companion orbits Gravitational lensing of galaxies Intermediate mass black holes Local group galaxies: orbits and internal kinematics for dark matter Jet proper motions Astrometric wobble from planets: crowded, faint, red = what Gaia won t do. Hypervelocity stars, runaway stars from other galaxies
24 Stars in formation in motion Jessica R. Lu Institute for Astronomy University of Hawaii
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