Population census, a case study & how to find more

Active low-mass black holes COST/CERN Workshop March 2013 M. Valencia-S.

Population census, a case study & how to find more

Active intermediate-mass black holes (MBH<106 Msun)

Mónica Valencia-S.I. Physikalisches Institut. Universität zu Köln

In collaboration with: A. Eckart, J. Zuther, C. Iserlohe, M. Garcia-Marin, A. Zensus, S. Smajic, M. Vitale, G. Busch, S. Fisher, L. Moser, M. Bremer, C. Straubmeier


HE0450-2958 HE1239-2426 (c) NASA,ESA, F. Courbin, and P. Magain

Cen A .(c) NASA, CXC, CfA, R.Kraft+, MPIfR, ESO, WFI, APEX, A.Weis+

SDSS J092600+442736 z=0.187. (c) SDSS

NGC 6240. (c) NASA, CXC, MIT, STSc I, C. Canizares, and M. Nowak

Galactic Center. (c) NASA,CXC,MIT, F.Baganoff+

Over-classification vs. Unification


Unification?

BHAccretion Disk

BLRTorus

NLR

Geometrical Unification of Active Galactic Nuclei (AGN)

Low obscuration Broad Lines (10 000 km/s) + Narrow Lines (100 km/s)

Type 1

Type 2

Composed illustration. Originals (c) NASA/CXC/M.Weiss, K..Meisenheimer

Obscuration (NH >1022 cm-2) Narrow Lines (100

km/s)


Unification parameter 2?

Lbol/LEdd ~0.1 (BL AGN)

Lbol/LEdd ~10-2.5 (no BLR)

UV signature of SS disk “Big Blue Bump”

Advection Dominated / Radiatively Inefficient Accretion Flow

Trump + 2011. see also Nicastro 200, Elitzur &Ho 2009

High Accretion rate

Thin disk

BBB

Broad lines

Radio quietness

Low Accretion rate

Thick disk (ADAF/RIAF)

No BBB

No Broad lines

Radio loudness

QSOs

Seyferts

NLSy1s

FR I sources

LINERs

LLAGNs


IRAS 01072+4954 in brief

IRAS 01072+4954

LBT/LUCI. Infrared: K-band. Courtesy: J. Zuther

GEMINI/NIFS 3’’x3’’ Field-Of-View

Low-luminosity AGN (LLAGN)

Starburst galaxy: ~5 Msun/yr

Pseudo-bulge <--Secular evolution

Unobscured Sy2:

LX(2-10keV)= 1041.5 erg/s

NH < 4.0 x 1020 cm-2

Low-mass black hole: MBH ~ 105Msun

High accretion rate:

Lbol~1042.5 erg/s, m~0.2

FWHMbroad lines~500 km/s

No Broad lines in optical, no FeII





High Accretion rate

Thin disk

BBB

Broad lines

Radio quietness

Low Accretion rate

Thick disk (ADAF/RIAF)

No BBB

No Broad lines

Radio loudness

QSOs

Seyferts

NLSy1s

FR I sources

LINERs

LLAGNs



Brγ λ 2.164 μm

F(Brγ) = 1.0 x 10-16 erg s-1 cm-2

FWHM(Brγ) = 420 km/s

S/N~2.8

IRAS 01072+4954

BH Accretion:

Lbol/LEdd~0.2

M ~ 4.4 x 10-4 Msun/yr

Broad Line Region:

rBLR ~ 1 light-day ≈ 105 RS

F(Hα) = (1.7 - 4.8) x 10-14 erg s-1 cm-2

FWHM(Hα) = 430 – 600 km/s

F(Brγ) ≈ F(Hα) / 100





Stern & Laor 2012

Younes+ 2012

BL AGN

LINER 1s



Sy1 Sy2 Singh+,2011

TrueSy2 candidates Laor,2003

IMBH & NLSy1 Dewegan+,2008

Low Mass Sy2 Carol+,2009 L Edd



Sy1 Sy2 Singh+,2011

TrueSy2 candidates Laor,2003

IMBH & NLSy1 Dewegan+,2008

Low Mass Sy2 Carol+,2009 IRAS01072



Radio Loud NLSy1Foschini (2013)



Radio Loud NLSy1Foschini (2013)

Jet (radio) vs. disk luminosity in BHsFoschini (2012)

IRAS01072



Why are IMBHs important?


Why to study IMBHs?

IMBHs are the connection between SMBHs and stellar BHs


Why to study IMBHs?


IMBHs are fundamental to probe models of SMBH seeds

Greene 2012


Why to study IMBHs?



IMBHs are the most active population of BHs in the local universe (dowinsizing)

IMBHs seem to be in an early stage of evolution, therefore they can help on understanding how BHs grow


Why to study IMBHs?



IMBHs are the most active population of BHs in the local universe (dowinsizing)

IMBHs seem to be in an early stage of evolution, therefore they can help on understanding how BHs grow

IMBHs seem to reside in young galaxies (starbursts), therefore they are important to recognize the nature of the star formation – AGN relation

IMBHs seem to prefer spiral galaxies with bars or pseudobulges, therefore they might probe a different type of BH fueling

IMBHs show signatures that might allow to probe the metal enrichment of the BLR in AGNs


How many IMBHs have been detected?

Extracted from: Hubble Ultra Deep Field. (c) NASA/ESA/S. Beckwith(STScI) and The HUDF Team.


Population census

From optical observations

SDSS DR7 Stern & Laor 2011:

106<MBH<109.5

10-3<Lbol/LEdd<1

SDSS DR4 Dong+2012:

8x104<MBH<2x106

3% are LINER 1

3% host an AGN

3% host an AGN


Population census



106<MBH<109.5

10-3<Lbol/LEdd<1

SDSS DR4 Dong+2012:

8x104<MBH<2x106

3% are LINER 1

3% host an AGN

3% host an AGN

From X-rays:

Desroches & Ho 2009, Ghosh+ 2008

M*,gal<1010Msun 20% - 25 % Lx >2.3x1038 erg/s


Population census



106<MBH<109.5

10-3<Lbol/LEdd<1

SDSS DR4 Dong+2012:

8x104<MBH<2x106

3% are LINER 1

3% host an AGN

3% host an AGN

From multiwavelength campaigns

Foschini 2011:

From 76 NLSy1 46 radio loud

30 radio quiet

From 49 RLNLSy1 12 γ-emitters

From X-rays:

Desroches & Ho 2009, Ghosh+ 2008

M*,gal<1010Msun 20% - 25 % Lx >2.3x1038 erg/s

~ 310 low-mass BH

(z<0.35)


How to find more IMBHs?


How to find more?


Problems:

- Obscuration

- Dilution of the AGN by the stellar continuum

LAGN,B Lbol/LEdd (M*,gal / Lgal,B) B

Lhost,B 0.1 (Msun/Lsun) T

B/T : ratio stellar mass of the bulge to total stellar mass

=

LAGN/Lhost (Sa) ~ 45

LAGN/Lhost (Sc) ~ 7

For maximal accreting BHs:

NGC 4395. (c) Cord Scholz


How to find more?


Problems:

- Obscuration



Lhost,B 0.1 (Msun/Lsun) T

B/T : ratio stellar mass of the bulge to total stellar mass

=

MBH

M*,bulge

~ 0.001LAGN

Lhost

α MBH


How to find more?

MBH – M*,bulge relation

Graham+2012

log (MBH) = -1.0 (MK + 22.5) + 7.55Valencia-S+ 2012

IRAS 01072

IRAS 01072


How to find more?

log (MBH) = -1.0 (MK + 22.5) + 7.55Valencia-S+ (Jun.) 2012

log (MBH) = -1.09 (MK + 22.5) + 7.39

Graham & Scott (Dec.) 2012

MBH – LK,bulge relation

IRAS 01072


How to find more?


Problems:

- Obscuration



Lhost,B 0.1 (Msun/Lsun) T=

MBH

M*,bulge

~ 0.001

For MBH > 7x107 Msun:

MBH

M*,bulge

~ 10-5 – 10-4

For IMBHs with 105 Msun < MBH < 106 Msun:


How to find more?

From X-ray observations

A max. accreting BH with MBH=105 Msun:

LEdd = 1043 erg/s

LX(2-10kev) ~ 1042 erg/s


How to find more?


A max. accreting BH with MBH=105 Msun: Like IRAS 01072 (z=0.0236):

MBH~105 Msun

Lbol/LEdd ~ 0.2

FX(2-10keV)=3.1 x 10-13 erg s-1 cm-2

Chandra (~ 25 ks)

LEdd = 1043 erg/s

LX(2-10kev) ~ 1042 erg/s

Sensitivity limit Chandra (2-10keV):

FX~ 10-15 erg s-1 cm-2 (~ 20ks)

not detectable z > 0.2


How to find more?


A max. accreting BH with MBH=105 Msun: Like IRAS 01072 (z=0.0236):

MBH~105 Msun

Lbol/LEdd ~ 0.2

FX(2-10keV)=3.1 x 10-13 erg s-1 cm-2

Chandra (~ 25 ks)

LEdd = 1043 erg/s

LX(2-10kev) ~ 1042 erg/s

Sensitivity limit Chandra (2-10keV):

FX~ 10-15 erg s-1 cm-2 (~ 20ks)

not detectable z > 0.2IMBHs: 105 Msun < MBH < 106 Msun

Dong+2013 42/49 detections (S/N>3)

z < 0.08 (D < 350 Mpc)

FX(2-10keV) > 10-14 erg s-1 cm-2


How to find more?


Artist impression. (c)ESO/ L.Casada

Stellar BH with MBH~ 10 Msun:

LEdd = 1039 erg/s

LX(2-10kev) ~ 1038 erg/s

Threshold on the Eddington ratio of IMBHs:

For MBH = 105 Msun Lbol/LEdd ~ 0.001

LX(AGN)min ~ 1040 erg/s


There is still some hope

From Infrared observations

Volume-weighted space density of active SMBH in the local Universe Goulding+ 2010


Thanks!

Population census, a case study & how to find more

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