PROSPECTS FOR MEASURING SUPERMASSIVE BLACK HOLE MASSES WITH IRIS/TMT

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Garey Cameron
5 years ago
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1 PROSPECTS FOR MEASURING SUPERMASSIVE BLACK HOLE MASSES WITH IRIS/TMT Tuan Do Dunlap Fellow From Do T., Wright S. A., Barth A. J., Barton E. J., Simard L., Larkin J. E., Moore A. M., Wang L., Ellerbroek B., 2014, AJ, 143

2 Current measurements of black hole masses are predominantly in the range of M M BH - σ and M BH - L relaponships shows the evolupon of the central black hole and galaxies as a whole are connected. From Gulteken et al. 2009

3 Large parts of the parameter space in galaxy scaling relaponships are unexplored Current compilapon black hole masses measured dynamically from McConnell and Ma (2013)

4 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 The two relaponships predict very different space densipes for the highest mass black holes From Lauer et al. 2007

There are currently very few confirmed black hole masses < 10 6 M Current best measurement of the kinemapcs of the nucleus of M32 with a 2x10 6 M BH (Seth 2010) Stellar

5 There are currently very few confirmed black hole masses < 10 6 M Current best measurement of the kinemapcs of the nucleus of M32 with a 2x10 6 M BH (Seth 2010) Stellar velocity dispersion measurements for the globular cluster G1 may indicate a 10 4 M BH, but may be consistent with only a stellar cluster. (Gebhardt et al 2002, Baumgardt et al. 2003)

6 What will TMT do?

7 TMT will certainly have the angular resolupon

8 The range of filters are important to sample galaxies at mulpple redshi[s Z band µm Ca Triplet Y band µm Ca Triplet Filter H band µm CO K band 2.29 µm CO Redshift Range (z)

SimulaPng galacpc nuclei R inf AO K- band PSFs from NFIRAOS Strehl rapo ~72% at zenith, at 2 µm Detector: 0.

arcsec Surface brightness profiles extrapolated from current high angular resolupon observapons (HST & AO)

9 SimulaPng galacpc nuclei R inf AO K- band PSFs from NFIRAOS Strehl rapo ~72% at zenith, at 2 µm Detector: 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 for 9 mas plate scale, R = 8000, 2.5 hr. int. Pme

10 Spectrograph: extended source sensipvity Ave. 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 0.4 NGC 3377 11.7 Mpc 220. 185. 150. 115. 80. 45. 10. 0.4 0.2 0.0 0.2 0.4 NGC 4621 17.9 Mpc 220. 185. 150. 115. 80. 45. 10. 0.4 0.2 0.0 0.2 0.4 NGC 7332 24.

1 Mpc 220. 185. 150. 115. 80. 45. 10. 0.4 0.2 0.

11 Examples of IRIS simulapons NGC Mpc NGC Mpc NGC Mpc ESO Mpc ESO Mpc ESO 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.

12 Stellar dynamical measurement of black hole masses rely on measuring the line- of- sight velocity distribupon V = 0 km/s, σ=200 km/s, h 3 = , h 4 =0.029

13 Stellar dynamical measurement of black hole masses rely on measuring the line- of- sight velocity distribupon Velocity Error (km/s) R = 3000 R = 4000 R = 8000 Velocity Disper Error (km/s) Current Measurements: >= h3 Error h4 Error Errors in Gauss- Hermite moments as a funcpon of signal- to- noise rapo

14 The number of dynamical mass measurements of will increase dramapcally SimulaPons of SDSS galaxies show that over 10 5 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

15 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 4x10 6 M black hole (From Do et al. in prep)

16 R=8000 spectral- resolupon will allow observapons of intermediate mass black holes Line of sight velocity distribupon Velocity Error (km/s) R = 4000 R = 8000 Velocity Disper Error (km/s) V = 0 km/s, σ=30 km/s, h 3 = , h 4 =0.029 h3 Error 0.10 h4 Error ObservaPons at R = 4000 will be incapable of determining higher- order moments

R=8000 spectral- resolupon will allow observapons of intermediate mass black holes DEC Offset (arcsec) 0.2 0.1 0.

17 R=8000 spectral- resolupon will allow observapons of intermediate mass black holes DEC Offset (arcsec) ACS HRC image RA Offset (arcsec) Requires both angular resolupon and relapvely high (R~8000) spectral resolupon Velocity Dispersion (km/s) No BH 20,000 Msun BH Gebhardt et al IRIS Red simulated IRIS points Black HST/STIS points (Gebhardt et al. 2002) Radius (pc) Comparison of the velocity dispersion profile of the globular cluster G1 in M31, with and without a 2x10 4 M sun black hole

18 Black hole mass measurements in nuclear star clusters will also provide demography of lower mass black holes 1 kpc WFPC2 F814W from Boker et al Simulated sensipvity at R = 8000, with 5 hrs of integrapon Pme

Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies. Amy Reines Einstein Fellow NRAO Charlottesville

Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies Amy Reines Einstein Fellow NRAO Charlottesville Motivation: The origin of supermassive BH seeds Motivation: The origin of