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Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions 2D velocity and flux distribution maps Model 2D velocity field to estimate M BH directly I. How Good Are our MBH Estimates in Local Seyfert 1 Nuclei? Test Using Gas Kinematics Erin Hicks & Matt Malkan UCLA

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Page 1: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Keck NIRSPEC/AO spectra of nearest Seyfert 1s

Multiple slit positions 2D velocity and flux distribution maps

Model 2D velocity field to estimate MBH directly

I. How Good Are our MBH Estimates in Local Seyfert 1 Nuclei?

Test Using Gas KinematicsErin Hicks & Matt Malkan

UCLA

Page 2: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

NGC 3227: H2 2.1218m & 2.4237m

Gaussian fit to the emission line profile for each aperture Velocities measured to an accuracy of 20 km s-1

Peak 0''.5 SE

Page 3: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

NGC 7469: H2 2.1218m & 1.9576m

Rotational velocity pattern confirmed in at least one other H2 line, in 3227 and 7469 H2 velocity is measurable fairly far out

Page 4: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

NGC 4151 H2 also shows sharp velocity gradient

Page 5: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Summary of 2D Velocity Maps

Organized Velocity Gradient:

NGC 3227(150-200 k/s across central tenths of '‘,=tens of parsecs)

NGC 4051 NGC 4151 NGC 7469

No Velocity Gradient: NGC 3516 NGC 5548 (NGC 6814)

Emission too Weak to NGC 4593 Measure Reliably: Ark 120

Page 6: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

One Single slit position (angle=100o, offset=0''.09; there are 33 more) with Sérsic n=3 stellar models and disk PA=130o

CO disk has PA=158o (Schinnerer et al. 2004).

2D Modeling of H2 Rotation in NGC 3227

Each small tick is 7 parsecs

Page 7: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Explore wide range of acceptable models for molecular gas in NGC 3227

MBH of a few 107 Msun

Is better than nothing

Stellar M/LH of 0.5 to 1.0Is very astrophysically reasonable

Page 8: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Massive Black Hole also required in NGC 4151MBH =0.8—3 x 107 Msun,(Again does not reach 3 Significance)

Page 9: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Low-inclination (not far from face-on) molecular disk always fits better

Page 10: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Two data points aren’t quite enoughto settle the entire story

Page 11: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

With only two (noisy) detections and a few upper limits,All we can say is that reverberation masses are not too badly off

Page 12: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Reporter asked Chou-en-lai what he thoughtwas the significance of the French Revolution

He said: “It is too soon to tell.”

“…Why don’t you guys get OSIRIS data?”

Page 13: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

II. Remarkable Two-way Correlation:

1. Only the most luminous galaxies are Chandra sources (accreting SMBHs)

Colbert, MM, Teplitz, and some non-UCLA peopleused NICMOS in Parallel imaging mode* tomeasure NIR (starlight) from galaxies in X-Ray Deep Fields

2. Virtually all of the massive/star-forming galaxies harbor AGN (X-rays from accretion)

. Not X-ray detectionLarge Symbol: X-ray detection (40)

Colbert et al. 2005 Ap J. 621, 587*Discontinued last year

Page 14: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

So Massive Galaxies were building up central So Massive Galaxies were building up central black holes early on;black holes early on;III. III. When was current Galaxy Bulge/Central When was current Galaxy Bulge/Central Black Hole Mass correlation established?Black Hole Mass correlation established?

So Massive Galaxies were building up central So Massive Galaxies were building up central black holes early on;black holes early on;III. III. When was current Galaxy Bulge/Central When was current Galaxy Bulge/Central Black Hole Mass correlation established?Black Hole Mass correlation established?

MM, with Tommaso Treu (Hubble Fellow at UCLA, now UCSB), Jonghak Woo (UCSB), andRoger Blandford (Stanford)

Weigh them, way back (4 Gyears ago):

Is the SMBH/host galaxy correlation the same as today?

Page 15: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Measuring MBH/ in distant universe: 2 problems

1. Black hole mass: “sphere of influence” is too small to resolve

(0.1” at z=1 is ~800 pc)

2. Velocity dispersion: distant objects are faint, and heavily contaminated by AGN continuum

Solution: Broad-line AGN1) Reverberation mapping of BLR (AGNWatch, started late ‘80s)2) Empirically calibrated photo-ionization method, based on

reverberation masses (Wandel, Peterson, MM 1999).

Solution: Seyfert 1 host galaxiesintegrated spectra have enough starlight superposed on

the featureless AGN continuum, to measure

Page 16: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Testing MBH- Relation at z~0.36

Sample selection• redshift window: z=0.360.01 to avoid sky lines• 30 objects selected from SDSS, based on broad H

Observations• Keck spectra for 20 objects; sigma measured for 14• HST images for 20 objects

Page 17: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Measuring velocity dispersion All 14 determinations of

Possible emission lines are masked out

Page 18: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

The Black-Hole Mass vs Sigma relation at z~~0.37 disagrees with z=0

Treu, Malkan & Blandford 2004 + Woo, MM, TT, RB 2006first half of data gave 2 evolution; Woo et al. 2006--doubling data makes this 3

Systematic errors are not that large

overall systematic errors (from Stellar contamination, aperture correction, inclination):Δlog MBH = 0.25 dex, smaller than observed offset Δlog MBH ~ 0.6 dex

Ie, MBH/galaxy Mass ratio was about 4 times higher 4 Gyrs ago

Page 19: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Assuming this is real,We can think of too many

different possible explanations

Something in Mbh/Sigma/LbulgeWas different 4 Gyrs ago:

Maybe Fundamental Plane--not Mbh/Lbulge correlation--was the problem?

Page 20: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Check with ACS Images: these bulges do not look very impressive: their low Lbulge is consistent with modest sigmas

Page 21: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Is evolution real? Independent check that bulges are “too small” for MBH

•With HST ACS images, quantify host galaxy properties determined from 2-D fits:

They lie on the Fundamental Plane, ie, normal for z=0.4,with simple passive Luminosityevolution of stellar population

2006 TT, MM, JW

Page 22: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

The MBH- Mbulge relation, from fits to ACS images:

Δlog MBH > 0.59±0.19 dex

P(KS)=1.3%

Assuming normal passive evolution of stellar population, Evolutionary Offset from z=0 to 0.36 in MBH/Lbulge is similar to what we found from MBH/

MBH/Mbulge 4 times larger

Page 23: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

2.Near perfect one-to-one association between massive galaxies and AGN X-ray emission

3.Cosmic evolution in Galaxy/BH Relations: Although they have been correlated over most of

cosmic history, SMBH growth was “completed” ahead of

bulge assembly

Conclusion: Only 3 Figures to Remember

1. H2 rotation curves give Mbh consistent with Reverberation mapping

Page 24: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Keck NIRSPEC/AO R ~ 2000 1.9 - 2.4 m (K-band) 0.''0185/pixel Correction from optical

nucleus, gives Average FWHM = 0''.1

0''.037 x 3''.93 Slit

SCAM: Slit viewing camera Accurate slit position PSF monitoring 0.''0168/pixel 4''.4 x 4''.4 FOV

Simultaneous direct imaging

Page 25: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

NGC 3227 NGC 3516 NGC 4051

NGC 4151 NGC 4593 NGC 5548

Ark 120NGC 7469NGC 6814

6''

74 172 47

64 175 334

101 318 613pc/''

Galaxy

5.1 hr 1.8 hr 3.9 hr

4.1 hr 0.3 hr 1.3 hr

0.9 hr 1.9 hr3.1 hrTotal Exp.

Get Lots of Slit Positions

Ass

um

e H

o=

75

km

s -1

Mpc-

1

Sample of Seyfert 1s

Each thin black line is a single slit position, superposed on NICMOS images

Thicker lines are overlapping slits.

Assumed Ho = 75 km s -1 Mpc-1

Page 26: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Strongest Gas Emission Lines: H2 & Br

H2 1.9576 2.1218 2.2235 2.2477 2.4066 2.4237

Br 2.1661

Example nuclear spectra from a 0''.05 x 0''.04 aperture.

Page 27: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

The FP of Spheroids at z~0.36

• At z=0.36, all Spheroids are overluminous for their mass, as expected from passive stellar evolution.

Page 28: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

High S/N (100-1 per Angstrom) Keck LRIS Spectra

H H [OIII] MgI/FeI

Page 29: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Measuring velocity dispersion in z=0.36 Seyfert 1 galaxies: 1 example

Mg I5175A

Fe I5269A

Broadened K giant spectrum

Spectrum Zoom:

Page 30: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Black-Hole Mass in Seyfert 1 nucleus: H width estimation MBH ~ RBLR VBLR

2 /G (Wandel, Peterson, Malkan 1999)

Single epoch spectra provide a good measure of the H width (), if narrow (constant) component is removed (Vestergaard 2002) need high SNR (Keck provided it on these 19th mag Seyferts)

Treu, Malkan & Blandford 2004

[OIII]5007

[OIII]4959=[OIII]5007/ 3

NLR core of H

Page 31: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

2) Estimating BLR size:Empirically Calibrated Photo-Ionization Method

• The flux needed to ionize the broad line region scales as LIONIZING/RBLR

2.

• An empirical correlation is found, calibrated using reverberation mapping (which determines RBLR from direct measurement of light-crossing time)

BLR size R

BLR (lt-days)

L(5100A) (erg/s)

Estimating virial MBH

from BLR

RBLR

Page 32: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

The MBH- Lbulge relation

Δlog MBH > 0.42±0.14 dex

P(KS)=10%

Page 33: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

< 10% of Eddington

mass accretion rate= ~ 0.1-0.5 (solarmass/yr)

Are these BHs rapidly growing?

Page 34: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Open Questions

Theoretical studies “predict”:• No evolution (Granato et al. 2004)• Sigma increases with redshift (Robertson et al. 2005)• Stellar mass (sigma) decreases with redshift (Croton 2006) Is the ratio of growth rates constant?

• MBH- and MBH-Lbulge relations?

When were they formed? Do they evolve?• If spheroids evolve by mergers, what makes these scaling relations?

Page 35: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

A Scenario

The M-sigma relation should be already in place for larger masses!

• The characteristic mass scale decreases with time (downsizing), consistent with that of our galaxies at z=0.36

• Major mergers 1) trigger AGN &

SF, 2) quench SF by

feedback, 3) increase bulge

size

Page 36: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Updated with L5100A correction

Old New

Page 37: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

MBH: measuring L5100

Calibration of spectrophotometry on SDSS-DR4 photometry

Page 38: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Fe II subtraction Fe II fit with I zw 1 template

Measuring velocity dispersion ()

Page 39: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Evolution of M-sigma Relation

redshift

Δlog MBH = 0.62±0.10±0.25 dex for z~0.36 sample

Δlo

g M

BH

Page 40: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

ACS images of z=0.36 Seyfert 1’s

These Seyfert 1 galaxy hosts are big and brightA high proportion of them (?) appear to be undergoing close encounters

55 Kpc

Page 41: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Bulges at z~0.36 are smaller/less luminous than suggested by the local MBH-sigma relation.

Systematic error? (< 0.25 dex in log MBH )

Selection effects (possibly in the local relationship; spirals vs bulge dominated systems)?

Significant recent evolution of bulges if M-sigma relation is the final destiny of BH-galaxy co-evolution.

Conclusions

Page 42: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

1. Only the most luminous galaxies are Chandra X-ray sources

Colbert, MM, Teplitz, and some non-UCLA peopleused NICMOS in Parallel observing mode tomeasure IR (starlight) from galaxies in Chandra Deep Fields

2. Virtually all of the massive galaxies harbor AGN

Page 43: Keck NIRSPEC/AO spectra of nearest Seyfert 1s Multiple slit positions  2D velocity and flux distribution maps Model 2D velocity field to estimate M BH

Black Hole Mass vs Sigma. Feasible in special redshift windows

Seyfert 1 Galaxies selected from SDSS based on redshift z=0.35 - 0.37