The Galactic Centre: from SINFONI to GRAVITY

Transcription

The Galactic Centre:
from SINFONI to GRAVITY
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
The Galactic Centre: from SINFONI to GRAVITY – p.1/21
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Thibaut Paumard
(MPE)
F. Eisenhauer,
R. Genzel,
S. Rabien,
S. Gillessen,
F. Martins,
T. Müller,
G. Perrin,
A. Eckart,
W. Brandner,
et al.
Early
SPIFFI
spectra...
(Paumard et al. 2004)
120
180
3.0
100
180
34
27
2.5
57
80
2.0
46
31
46
57
60
1.5
34
40
1.0
31
20
0.5
27
0.0
2.05
2.10
2.15
2.20
20
40
60
80
100
early Wolf-Rayets (broad-line stars)
Early
SPIFFI
spectra...
120
2.0
81
100
1.5
178
1.0
80
60
81
61
40
0.5
0.0
2.05
178
20
61
2.10
2.15
2.20
20
40
60
80
100
late Wolf-Rayets (broad-line stars)
Early
SPIFFI
spectra...
120
3.0
2.5
75
100
41
48
14
80
2.0
75
13
41
17
60
1.5
17
48
40
1.0
14
0.5
13
20
0.0
2.05
2.10
2.15
2.20
20
40
60
80
100
“LBVs” (narrow-line stars)
Early
SPIFFI
spectra...
120
181
4
179
100
110
3
80
53
23
110
33
26
24 181
33
60
2
32
24
20
179
23
0
2.05
32
40
26
1
53
2.10
2.15
2.20
20
40
60
80
100
absorption line (OB) stars finally detected!
Outline of the
various
2003–2005
SPIFFI/SINFONI
H+K and
K-band cubes
superposed on
an L-band
NACO image
> 90 early-type
stars
Paumard et al.
2006 (ApJ, in
press)
1.3
average of 9 OB III/V stars
average of 10 OB I/II stars
normalized flux
1.2
1.1
NIII/CIII
HeII
NIII
NV?
1.0
HeI
HeI
HeI
0.8
HeI
> 90 early-type
stars
HeI
7-4
0.9
2.10
HI 7-4 (BrJ)
2.15
Outline of the
various
2003–2005
SPIFFI/SINFONI
H+K and
K-band cubes
superposed on
an L-band
NACO image
2.20
wavelength (Pm)
2.25
Paumard et al.
2006 (ApJ, in
press)
Early-type stars mostly
projected tangential orbits
on
j = cos α
SgrA*
ur
uϕ
α
v
The early-type stars live in two
well defined disks
~vk = (vx,k , vy,k , vz,k )
= ||~vk ||(sin θk cos ϕk , sin θk sin ϕk , cos θk ) .
assume all vk are normal to a common vector
n = (sin i cos Ω, − sin i sin Ω, − cos i), then
0 = ~n · ~vk
= sin i cos Ω sin θk cos ϕk
− sin i sin Ω sin θk sin ϕk
− cos i cos θk
sin i sin θk cos(Ω + ϕk ) = cos i cos θk
cotan θk = tan i cos(Ω + ϕk ) .
The early-type stars live in two
well defined disks
~vk = (vx,k , vy,k , vz,k )
= ||~vk ||(sin θk cos ϕk , sin θk sin ϕk , cos θk ) .
assume all vk are normal to a common vector
n = (sin i cos Ω, − sin i sin Ω, − cos i), then
0 = ~n · ~vk
= sin i cos Ω sin θk cos ϕk
− sin i sin Ω sin θk sin ϕk
− cos i cos θk
sin i sin θk cos(Ω + ϕk ) = cos i cos θk
cotan θk = tan i cos(Ω + ϕk ) .
IR HR diagram:
•
6 ± 2 Myr old population •
•
•
Flat IMF;
Total mass
< 104 M¯ ;
One disk
small e, other
disk large e;
One
disk
contains
GCIRS 13E:
an extremely
dense
star
cluster.
Star formation in
an accretion disk
(two, actually)
The “S-stars” are not part of
any disk
NAOS/CONICA + SINFONI
(Eisenhauer et al, 2005)
The “S-stars” are not part of
any disk
NAOS/CONICA + SINFONI
(Eisenhauer et al, 2005)
SINFONI caught a “good” flare
under good seeing conditions
•
•
•
' 4 h;
0.500 seeing;
coherence
3 ms;
time:
•
12 × 5 min;
32 × 4 min;
•
peak: 8 mJy;
•
redder than stars.
•
SINFONI caught a “good” flare
under good seeing conditions
•
•
•
' 4 h;
0.500 seeing;
coherence
3 ms;
time:
•
12 × 5 min;
32 × 4 min;
•
peak: 8 mJy;
•
redder than stars.
•
Intra-flare flux/colour correlation
blue
red
Gillessen et al. 2006 (astro-ph/0511302)
Intra-flare flux/colour correlation
blue
red
Gillessen et al. 2006 (astro-ph/0511302)
25 mas = 3000 RS
Down-sized S-cluster
•
•
•
•
Short orbital
periods (. 1 yr);
fast precession
(validate GR);
probe density
profile closer to
SgrA* (dark
matter?);
get
the
mass
included
within
100 RS .
PSF: 3 (V, ϕ) sets, K-band, 4 UTs
40
20
0
−20
−40
40
20
0
−20
−40
Assumed constraints:
• 3 hours per obs.;
• 5 sp. elmnts from
2.0 to 2.4 microns;
• dynamic range:
' 1 mag;
• error on visibility:
1%;
• error on phase: 2◦ .
Synthesised image
40
20
0
−20
−40
40
20
0
−20
−40
Synthesised image, “cleaned”
40
20
0
−20
−40
40
20
0
−20
−40
2 seasons proper motion
40
20
0
−20
−40
40
20
0
−20
−40
Crude measured astrometry + input orbits
2 seasons proper motion
15
10
5
0
−5
−10
15
10
5
0
−5
−10
Crude measured astrometry + input orbits
Imaging @ 1 mas, astrometry @
10 µas
PRIMA/GRAVITY
will
offer astrometry with µasaccuracy:
• B = 100-m baseline;
• reference–science
objects distance:
Θ = 1.200 ;
⇒ 1 RS = 10 µas accuracy
in t = 65 s integration
time!
(Glindemann & Lévêque 2000)
Orbitting blob model
Hot spot on the last stable orbit
Accretion disk
t0
t1
Hot spot at t0
t3
t1
t3
t2
t2
Last stable orbit seen from above
Last stable orbit seen at high inclination
Motion of the flare =
orbital motion of the clump
on average = 0
νLν ∝ ν 0
y (RS )
Luminosity
Astrometric model, i = 45
◦
x (RS )
Orbital phase
Global centroid, lensing + beaming
νLν ∝ ν 0
y (RS )
Luminosity
Astrometric model, i = 80
◦
x (RS )
Orbital phase
Global centroid, lensing + beaming
The light-curves don’t fit
•
•
•
(Overall raise and decay;)
low contrast;
time-variable contrast;
The light-curves don’t fit
(Overall raise and decay;)
• low contrast;
• time-variable contrast;
⇒ extended component.
•
On flares
•
•
•
10 µas astrometry ⇒ nature of flares;
lightcurves of flares consistent with shearing hot
spot on LSO;
in that case, astrometry ⇒
• parameters of the BH;
• physical properties of inner disk;
• constrain “BH” size to . a few RS ;
• explore a totally untested regime of gravity;
•
probe spacetime at a few RS

The Galactic Centre: from SINFONI to GRAVITY

Transcription

Similar documents

GALACTIC AT-ONE-MENT "Healing for the Heart and the Mind

Free-air gravity

The Shape of the Earth

GRAVITY

Astronomy Course of ETH Zürich at Diavolezza

Throw a ball up and it will fall down 1) The force of gravity pulls the

12.221 Field Geophysics – Lecture 2

Info Sheet - DuClaw Brewing Company

Final Presentation