TMT – FIRST LIGHT INSTRUMENT AND SCIENCE

IRIS [InfraRed Imaging Spectromoter]

> operating at the diffraction-limit with a near-infrared (0.84 to 2.4micron) imager and IFS

> The imager will have four 4k×4k Hawaii-4RG detectors with a 34 arcsec×34 arcsecfield of view (FoV) using a 4 mas pixel scale.

> The IFS will have one Hawaii-4RG which will have four spatialscales (lenslet:4 mas, 9 mas; slicer: 25 mas, 50 mas)

> The IFS will have 12 gratings with resolutions R=4000,8000, and 10000

> both the imager and IFS will use the same set of 68 filters

Current  measurements  of  black  hole  masses  are  predominantly  in  the  range  of  107-­‐108  M  

From  Gulteken  et  al.  2009  

MBH-­‐σ  and  MBH-­‐L  relaPonships  shows  the  evoluPon  of  the  central  black  hole  and  galaxies  as  a  whole  are  connected.  

Large  parts  of  the  parameter  space  in  galaxy  scaling  relaPonships  are  unexplored  

Current  compilaPon  black  hole  masses  measured  dynamically  from  McConnell  and  Ma  (2013)  

There  is  a  disagreement  in  the  black  hole  mass  scaling  relaPonships  at  high  masses  

M-­‐sigma  relaPonship  predict  different  black  hole  masses  than  M-­‐L  

From  Lauer  et  al.  2007  

The  two  relaPonships  predict  very  different  space  densiPes for  the  highest  mass  black  holes  

There  are  currently  very  few  confirmed  black  hole  masses  <  106  M  

Current  best  measurement  of  the  kinemaPcs  of  the  nucleus  of  M32  with  a  2x106  M  BH  (Seth  2010)  

Stellar  velocity  dispersion  measurements  for  the  globular  cluster  G1  may  indicate  a  104M  BH,  but  may  be  consistent  with  only  a  stellar  cluster.  (Gebhardt  et  al  2002,  Baumgardt  et  al.  2003)  

What  will  TMT  do?  

TMT  will  certainly  have  the  angular  resoluPon  

The  range  of  filters  are  important  to  sample  galaxies  at  mulPple  redshi[s  

0.0 0.1 0.2 0.3 0.4Redshift Range (z)

K−band

H−band

Y−band

Z−band

0

Filt

er

2.29 µm CO

1.619 µm CO

0.867 µm Ca Triplet

0.867 µm Ca Triplet

SimulaPng  galacPc  nuclei  

•  AO  K-­‐band  PSFs  from  NFIRAOS  –  Strehl  raPo  ~72%  at  zenith,  at  2  µm  

•  Detector:  0.002  e-­‐/s dark  current,  2  e-­‐  read  noise.  

•  K-­‐band  sky  background:  13.9  mag/sq.  arcsec  

•  Surface  brightness  profiles  extrapolated  from  current  high  angular  resoluPon  observaPons  (HST  &  AO)  

•  GravitaPonal  radius  of  influence  esPmated  by  using  BH  mass  predicPon  from  M-­‐L  relaPonship  

Mean  K-­‐band  SNR  for  9  mas  plate  scale,  R  =  8000,  2.5  hr.  int.  Pme  

Rinf  

Spectrograph:  extended  source  sensiPvity  

Ave.  SNR  over  K-­‐band  for  5  hours  of  integraPon  Pme  (20x900  s  exposures)  

(From  Do  et  al.  2014)  

Examples  of  IRIS  simulaPons  

−0.4 −0.2 0.0 0.2 0.4Distance from Center (")

−0.4

−0.2

0.0

0.2

0.4

Dis

tan

ce

fro

m C

en

ter

(") SNR

10. 45.

80.

115.

150.

185. 220.

NGC 3377 11.7 Mpc

−0.4 −0.2 0.0 0.2 0.4Distance from Center (")

−0.4

−0.2

0.0

0.2

0.4

Dis

tan

ce

fro

m C

en

ter

(") SNR

10. 45.

80.

115.

150.

185. 220.

NGC 4621 17.9 Mpc

−0.4 −0.2 0.0 0.2 0.4Distance from Center (")

−0.4

−0.2

0.0

0.2

0.4

Dis

tan

ce

fro

m C

en

ter

(") SNR

10. 45.

80.

115.

150.

185. 220.

NGC 7332 24.3 Mpc

−0.4 −0.2 0.0 0.2 0.4Distance from Center (")

−0.4

−0.2

0.0

0.2

0.4

Dis

tan

ce

fro

m C

en

ter

(") SNR

10. 45.

80.

115.

150.

185. 220.

ESO 378−20 47.7 Mpc

−0.4 −0.2 0.0 0.2 0.4Distance from Center (")

−0.4

−0.2

0.0

0.2

0.4

Dis

tan

ce

fro

m C

en

ter

(") SNR

10. 45.

80.

115.

150.

185. 220.

ESO 507−27 50.1 Mpc

−0.4 −0.2 0.0 0.2 0.4Distance from Center (")

−0.4

−0.2

0.0

0.2

0.4

Dis

tan

ce

fro

m C

en

ter

(") SNR

10. 45.

80.

115.

150.

185. 220.

ESO 462−15 80.3 Mpc

Simulated  average  S/N  per  spectral  channel    at  9  mas  plate  in  K  band  with  eight  observaPons  of  900  s  each  (2  hr  integraPon  Pme)  at  R  =  4000.    

Stellar  dynamical  measurement  of  black  hole  masses  rely  on  measuring  the  line-­‐of-­‐sight  velocity  distribuPon  

V  =  0  km/s,  σ=200  km/s,    h3=-­‐  0.144,  h4=0.029  

Stellar  dynamical  measurement  of  black  hole  masses  rely  on  measuring  the  line-­‐of-­‐sight  velocity  distribuPon  

Errors  in  Gauss-­‐Hermite  moments  as  a  funcPon  of  signal-­‐to-­‐noise  raPo  

0 20 40 60 80 100SNR

1

10

100

1000V

elo

city

Err

or

(km

/s)

R = 3000R = 4000R = 8000

0 20 40 60 80 100SNR

1

10

100

1000

Ve

locity

Dis

pe

r E

rro

r (k

m/s

)

0 20 40 60 80 100SNR

0.001

0.010

0.100

1.000

h3

Err

or

0 20 40 60 80 100SNR

0.01

0.10

1.00

h4

Err

or

Current    Measurements:  SNR  >=  40  

The  number  of  dynamical mass  measurements  of  107-­‐109  will  increase  dramaPcally  

SimulaPons  of  SDSS  galaxies  show  that  over  105  SMBHs  will  be  measurable  with  IRIS  out  to  z  =  0.2  

Do  et  al.  (2014)  

IRIS  will  be  able  to  detect  Milky  Way  mass  black  holes  out  to  the  Virgo  Cluster  

The  Milky  Way  nuclear  star  cluster  without  foreground  dust  exPncPon,  as  seen  at  16  Mpc  (5  hours  integraPon  Pme  at  K-­‐band).  

Velocity  dispersion  for  the  MW  nuculear  star  cluster  cluster  with  a  4x106  M  black  hole  

(From  Do  et  al.  in  prep)  

0 20 40 60 80 100SNR

0.1

1.0

10.0

100.0

Ve

locity

Err

or

(km

/s)

R = 4000R = 8000

0 20 40 60 80 100SNR

0.1

1.0

10.0

100.0

Ve

locity

Dis

pe

r E

rro

r (k

m/s

)

0 20 40 60 80 100SNR

0.01

0.10

1.00

h3

Err

or

0 20 40 60 80 100SNR

0.01

0.10

1.00

h4

Err

or

ObservaPons  at  R  =  4000  will  be  incapable  of  determining  higher-­‐order  moments  

Line  of  sight  velocity  distribuPon  

V  =  0  km/s,  σ=30  km/s,    h3=-­‐  0.144,  h4=0.029  

R=8000  spectral-­‐resoluPon  will  allow  observaPons  of  intermediate  mass  black  holes  

R=8000  spectral-­‐resoluPon  will  allow  observaPons  of  intermediate  mass  black  holes  

0.1 1.0 10.0Radius (pc)

0

10

20

30

40

Ve

locity

Dis

pe

rsio

n (

km

/s)

No BH20,000 Msun BH

Gebhardt et al. 2002IRIS

Comparison  of  the  velocity  dispersion  profile  of  the  globular  cluster  G1  in  M31,  with  and  without  a  2x104  Msun  black  hole  

Requires  both  angular  resoluPon  and  relaPvely  high  (R~8000)  spectral  resoluPon  

Red  –  simulated  IRIS  points  Black  –  HST/STIS  points  (Gebhardt  et  al.  2002)  

ACS HRC image

−0.2 −0.1 0.0 0.1 0.2RA Offset (arcsec)

−0.2

−0.1

0.0

0.1

0.2

DE

C O

ffse

t (a

rcse

c)

Black  hole  mass measurements  in  nuclear  star  clusters  will  also  provide  demography  of  lower  mass  black  holes  

WFPC2  F814W  from  Boker  et  al.  2002  

1  kpc  

Simulated  sensiPvity  at  R  =  8000,  with  5  hrs  of  integraPon  Pme