Origins and Fundamental Physics of Supermassive Black Holes
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The US Extremely
Large Telescope
Program
Origins and Fundamental Physics
of Supermassive Black Holes
Jenny E Greene
GC Team:Tuan Do, Andrea Ghez, Jessica Lu, Matthew Hosek, Andrew Bellini,
Sukanya Chakrabarti, Mark Morris, Shoko Sakai
IMBH team: Tuan Do, Andrea Bellini, Jonelle Walsh, Kayhan Gultekin, Karl
Gebhardt, Aaron Barth, Matthew Hosek, Dongwon Kim, Mattia Libralato,
Jessica Lu, Matthew Malkan
01/07/2019 U.S. ELT Program - AAS #233 1
US-ELT:
Transforming Black Hole Science
Is GR the right description of black holes?
Proper motions and radial velocities of stars at the Galactic Center
How did supermassive black holes (SMBH) form?
Search for intermediate-mass black holes
Figure 3. Simulation of the central 0.5 arcsecond around the supermassive black hole Sgr A* (white cross) w
adaptive optics with the Keck Telescopes (left) compared to that with TMT (right). The greater resolving pow
How did SMBHs evolve through cosmic time?
along with better AO correction will likely allow us to detect a factor of > 10 times more stars in this region. W
how these orbit can be used simultaneously in a joint analysis to constraint tests of gravity and other science
Search for SMBHs out to z~2 (won’t cover now)
01/07/2019 U.S. ELT Program - AAS #233 2
Figure 4. Overlay of a sample orbits from the simulations described in Section 3. TMT will likely discover
Zooming Into Stellar Nuclei
Both angular resolution
and depth are key
From 17 to 120 stars to
be monitored at the GC
Reach the sphere of
Influence of 1000 Msun
Keck Today BHs in the MW and 10,000
1.1”=0.044pc Msun BHs to >5Mpc
01/07/2019 U.S. ELT Program - AAS #233 3
Zooming Into Stellar Nuclei
Both angular resolution
and depth are key
From 17 to 120 stars to
be monitored at the GC
Reach the sphere of
Influence of 1000 Msun
BHs in the MW and 10,000
1.1”=0.044pc Msun BHs to >5Mpc
01/07/2019 U.S. ELT Program - AAS #233 4
Galactic Center Experiment
Simulations: Instrumentation:
Number of stars: 121 (TMT) vs 17 TMT/IRIS for astrometry+moderate
(present-day) resolution spectroscopy
Assumes: 5x better astrometry GMTNIRS for high-resolution
10x better radial velocities spectroscopy for shortest-period
stars
Cadence: 3 RV and 3 PM
measurements/yr for three years Two-telescope system: provides
complementary instrumentation,
Total time: 360 hrs (IRIS) longer baseline modeling,
insurance against weather
01/07/2019 U.S. ELT Program - AAS #233 5
>10 sigma detection
Figure 4: The left panel shows the signal to noise ratio for the GR precession signal and the left
panel displays the uncertainty on the extended mass parameter at the
To 1000 Galactic
Msun Center. The red
precision
curve shows the evolution with Keck and TMT data. The blue curve on the other hand is with
only Keck data. The grey dashed horizontal line in the right panel is the extended mass value at
the distance of semi–major axis of S0–2.
Figure 4: The left panelToshows
2000 Msun precision
the signal To +/-
to noise ratio for the GR 5pc precision
precession signal and the left
panel displays the uncertainty on the extended mass parameter at the Galactic Center. The red
curve shows the evolution with Keck and TMT data. The blue curve on the other hand is with
only Keck data. The grey dashed horizontal line in the right panel is the extended mass value at
the distance of semi–major axis of S0–2.
U.S. ELT Program - AAS #233 6How do SMBHs Form?
????????????????????????????????????????????
106 10
10 10 76
10
10 10 1087 89 9
Direct Collapse Direct
Directcollapse?
Collapse
The Astrophysical Journal Letters, 824:L8 (7pp), 2016 June 10 Rodriguez et al.
rophysical Journal Letters, 824:L8 (7pp), 2016 June 10 Rodriguez et al.
Supermassive
Supermassive
Supermassive
Accretion Accretion
Stellar Mass
Stellar Mass
Stellar Mass
Black Holes
Black Holes
gravitational! Tidal !
gravitational
gravitational!
Rodriguez+2016 Tidal ! runaway disruption
Rodriguez+2016 runaway disruption
runaway?
Accretion
Accretion
PopIII SNe? dynamical ! Figure 2. Distribution of BBH total masses from GCs. In gray, we show the
CHE
distribution of all mergers that occur at z 0.5 (for GCs that form at z 3.5),
dynamical ! interactions
Figure 2. Distribution of BBH total masses from GCs.weIn show
gray, the
we distribution
show the of sources detectable with Advanced
CHE while in blue
distribution of all mergers that occur at z 0.5 (for GCs that form at z 3.5),
interactions while in blue we show the distribution of
LIGO during its first observing run. The median and 90% credible regions for
thesources detectable
total mass with Advanced
of GW150914 are shown in red (The LIGO Scientific
LIGO during its first observing run. The median and 90% & credible regions for
105 Msun
Collaboration The Virgo Collaboration 2016b). We also show the
the total mass of GW150914 are shown in red (The trigger,
LIGO LVT151012,
Scientific in purple (where we have computed
Collaboration & The Virgo Collaboration
gravitational-wave
2016b).
the median and We
(where
alsoregions
credible show bythe Accretion
adding the component mass median and
gravitational-wave trigger, LVT151012, in
explosion
the median and credible regions by adding
90%purple
Thethe
credible
component
Virgo Accretion
we have
interval computed
boundaries
mass median
Collaboration
from The LIGO Scientific Collaboration &
2016a). and
Note that while LVT151012 is below the
SN01/07/2019
explosion 90% credible interval boundaries from The
The Virgo Collaboration 2016a). Note that
LIGO
thresholdU.S.
while
signal
to ELTCollaboration
Scientific Program
be considered
was LVT151012
of astrophysical
& - there
a detection,
is below the
origin (Abbott
AASexists#233
a 84% chance that the
et al. 2016d).
7
threshold to be considered a detection, there exists a 84% chance that theSearch for
. ELT Key Science Program
Intermediate-mass Black Holes
Page 4 Draft
SgrA*
6
Two Experiments:
10 15 Cluster BHs = !
Proper motion measurements
More Common of 43 MW GCs
TOTAL NUMBER
i!
cle
t Nu )
entection
s 2e3 Msun limits with 3 epochs
105
?? Intermediate-mass
MBH (M )
r r Heavy BHs !
Cu de(3
100 total hrs*
Black Holes??
10 = rare
gh
t! U.S. ELT Key Science Program Page 5 NucDraft
Current GC ! li
104 (6 possible ! t. )
- in sed HST ACS/WFC 202x202 arcsec2 HST WFC3/UVIS 40 mas/pixel TMT/IRIS 4 mas/pixel
Ts propo
Integrated-light observations of 25 stellar
detections)
L
E 25 ( MWGC
ELT PM !
103
(43 proposed) nuclei in galaxies
5 with TMT/IRIS+GMTIFSSearch for
. ELT Key Science Program
Intermediate-mass Black Holes
Page 4 Draft
SgrA*
10 6
Two Experiments:
Cluster BHs = !
15
Integrated-light observations of 25
TOTAL NUMBER
i! More Common
cle
105
t Nu )
entection
s stellar nuclei inHeavy
galaxiesSolve the Seed Problem
U.S. ELT Key Science Program Page 4 Draft
SgrA*
106 15 Cluster BHs = !
TOTAL NUMBER
i! More Common
ucle
t N )
s
105 entection
?? Intermediate-mass
MBH (M )
r r Heavy BHs !
Cu de(3
Black Holes??
10 = rare
ht! Nuc
4 Current GC !
t. )lig
10 (6 possible !
- inposed
detections) s
T ro
EL 25 p
(
ELT PM ! MWGC
(43 proposed)
103 5
Nuc
MWGC
102
LIGO !
Binaries 10 3
10 2
10 1
100 0 3
10 104 105
D (Mpc) log (M /M )
01/07/2019 U.S. ELT Program - AAS #233 10US-ELT:
Transforming Black Hole Science
Is GR the right description of black holes?
Proper motions and radial velocities of stars at the Galactic Center
Extended mass distributions and GR tests: 360 hrs
How did supermassive black holes (SMBH) form?
Search for intermediate-mass black holes
Mass function and environments, first-ever detections of IMBHs: 200-300hrs
Figure 3. Simulation of the central 0.5 arcsecond around the supermassive black hole Sgr A* (white cross) w
adaptive optics with the Keck Telescopes (left) compared to that with TMT (right). The greater resolving pow
along with better AO correction will likely allow us to detect a factor of > 10 times more stars in this region. W
how these orbit can be used simultaneously in a joint analysis to constraint tests of gravity and other science
The combination of angular resolution
and sensitivity will transform BH science
01/07/2019 U.S. ELT Program - AAS #233 11
Figure 4. Overlay of a sample orbits from the simulations described in Section 3. TMT will likely discoverYou can also read
