Download Galactic science with AO

Years of Adaptive Optics at ESO
Galactic Science with ESO Adaptive
Optics
… a celebration, only ESO …
… a selection, not complete …
Frank Eisenhauer
Max-Planck-Institute for extraterrestrial Physics
27 November 2009
ESO Garching, Germany
Frank Eisenhauer
Galactic Science with ESO Adaptive Optics, ESO Garching, 27 November 2009
1
Everything becomes obvious if you see it
The four brightest moons orbiting Jupiter
Galileo Galilei 1609
Everything becomes obvious if you see it
Bright stars orbiting the Galactic Center
Galactic Center 2000+
With highest impact on …
NACO, SINFONI, LGSF
Schödel et al. 2002
Chauvin et al. 2004
COME-ON+, ADONIS
CRIRES
Genzel et al. 2006
Brandl et al. 1996
A supermassive black hole in the GC?
Not at all obvious, in contrary, there is
• no bright counterpart in Radio, X-ray, IR
• no jet
•…
For comparison: M87
VLA
Some, of course, knew all the time … (?)
University of California, Berkeley, led by C.H.Townes
Owens, Biretta, Eilek
Wollman et al. (1977)
A supermassive black hole in the GC!
A double break-through with NAOS/CONICA:
Unambiguous mass determination
Identification of its infrared counterpart
Genzel et al. 2003
Schödel et al. 2002
Dec.-offset from SgrA* (arcsec)
Dec.-offset from SgrA* (arcsec)
The wonderous20Galactic Center stars
A double break-through with SINFONI:
SINFONI
18.08.04:
mas)
The
central
lightK(75
month
0.6
21
0.4
22
15
26
S12
S08
S5
S4
S6
S14
S2
S13
0
S7
S17
8
-0.2
7
S8
-0.4
S9
S013
S1
S19
S11
-0.6
0.6
0.4
0.2
10
14.7
S10
1.6 light years
W6
9
0.2
10
The central parsec
19
16
0
-10
25
Paumard et al. 2006
23
0
-0.2
R.A.-offset from
SgrA*
(arcsec)
Eisenhauer
et al.
2005
90% of the stars are
young early type stars
on random orbits
-0.4
-0.6
-20
The missing OB
Supergiants of are
20
10
0
-10 the
finally
detected,
massive stars
R.A.-offset from SgrA* (arcsec)
indeed live in two
discs
Nayakshin et al. 2007
The state of the art of stellar orbits …
Tracking the motion more than 100 (!) stars within 1 arcsec radius
with about 300 µarcsec accuracy
The central stars are
on thermalized orbits
Gillessen et al. 2009
… and flares
Flare probe the physics in the immediate vicinity of the event horizon
Time domain analysis
Eckart et al. 2006, Trippe et al.
2006, Dodds-Eden in prep.
Polarization measurements
Broderick & Loeb 2005
Multi-wavelength campaigns
Eckart et al. 2009, Dodds Eden et al. 2009
Eckart et al. 2006,
Trippe et al. 2006
… and stellar dynamics and spectroscopy
S-stars are
main-sequence
stars
HeI
H
Martins et al. 2007, 2009
The discs are
warped and its
stars have a
very top-heavy
IMF
Bartko et al. 2009 a,b
An universal initial stellar mass function?
Not at all obvious, in contrary, the early observations of the starburst Galaxy M82
were indicating that IMF in these regions must be biased against the formation of
solar mass stars (Rieke et al. 1980, 1993)
But even nearby template are too dense to
resolve all stars
R136 in 30 Dor
NGC 3603
Arches
Melnick 1993
Brandl 1999
Figer 1999
Starting with COME-ON+ and ADONIS …
R136 in 30 Dor
NGC 3603
6“
Brandl et al. 1996
No cutoff at few to solar mass stars,
but shallow IMF = relative more massive stars in NGC 3603
Eisenhauer et al. 1998
… continued with NACO & SINFONI
Arches Cluster
NGC 3603
27“
Slightly topheavy IMF
Stolte et al. 2005
Dispute about
potential
turnover at 6-7
solar massed
Espinoza,et al. 2009
Harayama et al. 2008
The mass of the highest mass stars
Not at all trivial, because usually determined from stellar evolutionary tracks,
• which are poorly calibrated for these stars
Arches Cluster
• and require good spectral classification
Evolutionary sequence of high
mass stars
NGC 3603 A
most massive star
weighed so far
Schnurr et al. 2008
Schnurr
Martinsetetal.al.2008
2009
The mass of the lowest mass stars
Not at all trivial, because usually determined from stellar evolutionary tracks,
• which are poorly calibrated for these stars
• and require good spectral classification
SINFONI Spectral
Deconvolution
AB Dor C
Close et al. 2007
NACO Simultaneous
Differential Imager
Close et al. 2005
Thatte et al. 2007
Massive protostars formed by disc accretion
Not at all obvious, because radiation pressure from the protostar on the in-falling
material may prevent the formation of stars above ten solar masses
M17 silhouette disk
Protostar with
From K-band magnitude
Accretion disc : >110 Msun
from 13CO radio map and
rotation curve
Collimated H2 Jet
Chini et al. 2004, Nürnberger et al. 2007, Nielbock et al. 2008
Outlook for Galactic Science with AO
We will mostly benefit from
Continuity
High Strehl ratio
Spectroscopy
Proper motion ~T will finally solve
the field star subtraction problem in
many high-mass stellar cluster
(other than for
High-z science)
(like for High-z science)
Galactic Center
Next Peri 2013 (?)
Arches
Accelerations ~T2
Stolte et al. 2008
Relativisitc orbits
And don’t forget: AO is the Key to VLTI
Weigelt et al. 2007