Growing black holes: from the first seeds to AGN Mar Mezcua Harvard-Smithsonian Center for Astrophysics T. Miyaji, F. Civano, G. Fabbiano, M. Karouzos,

Growing black holes: Growing black holes: from the first seeds to AGNfrom the first seeds to AGN

Mar MezcuaMar MezcuaHarvard-Smithsonian Center for AstrophysicsHarvard-Smithsonian Center for Astrophysics

F. Civano, G. Fabbiano, M. Karouzos, A.P. Lobanov, T. Miyaji, T. Miyaji, T.P. Roberts, H. Suh, A.D. Sutton

Picture credit: NASA

Black hole seeds Mar Mezcua

The seeds of supermassive black holes

Quasars of 1010 M when Universe was < 1 Gyr

Had to start as seed BHs of 100 – 106 M

Grow fast via accretion and mergers

Wu et al. (2015)

Volonteri (2012)Artist’s conception of z≈7 quasarESO

Merloni et al. (2003)

Falcke, Körding & Markoff (2004)

Gültekin et al. (2009, 2014)

Fundamental plane of BH accretion sub-Eddington accretion rates low/hard state core radio emission

Intermediate-mass black holesof 100 – 106 M

Accretion physics is scale invariant

1. Ultraluminous X-ray sources (ULXs)

- Extragalactic, off-nuclear, LX > LEddington for a stellar-mass BH (LX > 1039 erg/s for a 10 M BH)

- Extreme ULXs with LX > 5 x 1040 erg/s

Most are super-Eddington accreting stellar-mass BHs?

Black hole seeds: ULXs Mar Mezcua

IMBHs with MBH ~ 100 - 106 M

Where can we find IMBHs?

ESO 243-49 HLX-1

LX ~ 1042 erg/s (Farrell et al. 2009)

Transient jet radio emission

9·103 M < MBH < 9·104 M

(Webb et al. 2012; Cseh et al. 2015)

Nucleus of stripped satellite galaxy

HLX-1

HST+ATCA 5-9 GHZ

Webb et al. 2012

Extreme ULX NGC2276-3c

LX ~ 6 x 1040 erg/s (Sutton et al. 2012)

Jet radio emission: -VLA lobes: size ~ 650 pc-EVN: 1.8 pc jet

MBH ~ 3.9 x 105 M

(Mezcua et al. 2013c, 2015)

Nucleus of stripped satellite galaxy

Black hole seeds: ULXs Mar Mezcua

EVN 1.6 GHz

HST+Chandra composite

NASA/CXC/SAO/INAFMezcua et al. 2015, Wolter et al. 2015

Search for seed BHs in

satellite, low-mass galaxies

Search for seed BHs in

satellite, low-mass galaxies

2. Nucleus of dwarf, low-mass galaxies

Resemble the first galaxies formed in the early Universe (low mass, low metallicity)

- Optically-selected samples of AGN with broad emission lines MBH = 105 -106 M

~50 X-ray detected: Lx = 1041 - 1043 erg/s

Bias toward high Eddington ratios (> 10-2)

- X-ray detected low-mass galaxies, M* < 3 x 109 M

38 sources (Schramm et al. 2013, Lemons et al. 2015, Gallo et al. 2010, Miller et al. 2012, 2015)

Lx < 1041 erg/s

Edd. ratio < 10-2

z < 0.3

Greene & Ho 2004, 2007; Reines et al. 2013;Desroches et al. 2009; Dong et al. 2012

Black hole seeds: low-mass galaxies Mar Mezcua

Extend to higher z, complete samples

Derive BH occupation fraction

Extend to higher z, complete samples

Derive BH occupation fraction

Black hole seeds: low-mass galaxies Mar Mezcua

Formation & Evolution of seed BHs

Low fraction of IMBHs in local dwarf galaxies

High fraction of IMBHs in local dwarf galaxies

Greene (Nature Communications, 2012)

Black hole seeds: low-mass galaxies Mar Mezcua

Chandra COSMOS Legacy Survey2.2 deg2 covered by Chandra & HST

Largest survey with complete, deep,

multiwavelength dataset:

XMM-Newton, NuSTAR, CFHT, Galex UV,

Spitzer mid-IR, IRAC, Herschel, UKIRT NIR,

Subaru multicolor imaging, optical spectra

(Magellan, VLT, Keck), VLA radio imaging…

K-band sensitivity limit = 23.7+-0.1 mag

2-7 keV flux limit = 1.7 x 10-15 erg/s/cm2

I-band (HST/F814W) depth = 27.8 magChandra

Courtesy of F. Civano

Multiwavelength SED, galaxy templates

stellar mass, star formation rate, redshift, morphologyIlbert et al. 2009; McCracken et al. 2012

Black hole seeds: low-mass galaxies in COSMOS Mar Mezcua

Select low-mass galaxies as:

- i < 24 mag

- 107 < M* < 3 x 109 M

Low-mass galaxies in COSMOS

52,508 sources

K-band sensitivity limit ~ 23 mag

< 1% X-ray detected< 1% X-ray detected

Mezcua et al. submitted

Black hole seeds: X-ray stacked low-mass galaxies in COSMOS Mar Mezcua

1. Morphological classification

Low-mass galaxies dominated by starburst and spiral hosts

X-ray contribution from X-ray binaries and hot ISM gas

Accreting BHs in early-type galaxies knownMiller et al. 2012; Civano et al. 2014; Paggi et al. 2015

✔

Population of accreting BHs in

starburst and late-type galaxies ?

Study 50,285 starburst+spiral galaxies

Mezcua et al. submitted

Non-detections: stacking analysis

Black hole seeds: X-ray stacked low-mass galaxies in COSMOS Mar Mezcua

Select complete redshift bins stack Chandra images for each bin with CSTACK

Soft band (0.5-2 keV)

Hard band (2-8 keV)

Count rateBootstrapping error analysisSignificant: S/N > 3Flux conversion

NH= 2.6 x 1020 cm-2

Γ= 1.4

(Takamitsu Miyaji)

Mezcua et al. submitted

Black hole seeds: X-ray stacked low-mass galaxies in COSMOS Mar Mezcua

2. Contribution XRBs

LX,XRB α M*-SFR (Lehmer et al. 2010)

M* and SFR expected LX,XRB LX > LX,XRBs in all X-ray stacked redshift bins

Mezcua et al. submitted

Black hole seeds: X-ray stacked low-mass galaxies in COSMOS Mar Mezcua

3. Nuclear LX vs stellar mass

LX – LX,XRBs – LX,hot gas

X-ray excess!!!

Must be nuclear

LX – LX,XRBs – LX,hot gas

X-ray excess!!!

Must be nuclear

Mezcua et al. submitted

Black hole seeds: X-ray stacked low-mass galaxies in COSMOS Mar Mezcua

4. Eddington ratio and Mbh – M*

If LX/Ledd ≥ 10-2 low-mass galaxies off the Mbh-M*

Mbh ≤ 104 M

Greene 2012

Low-mass galaxies on the Mbh-M*

if LX/Ledd ≤ 10-6 Mbh ≤ 6 x 106 M

5. Low-mass galaxies in mergers

Mergers selected as neighbors with Δv ≤ 1000 km/s

At z < 0.05 10.1 % of minor mergers

1.6% of the low-mass galaxies are in minor mergers

150.71405 +2.786401

z = 0.0051

149.912802 +2.304003

z = 0.005

HST cutouts

Black hole seeds: X-ray stacked low-mass galaxies in COSMOS Mar Mezcua

Conclusions

At low z, extend search for IMBHs to:

- arm of spiral galaxies

- galaxies undergoing a minor merger

Black hole seeds Mar Mezcua

Population of low-mass starburst and spiral galaxies with accreting BHs:

- up to z=1.5

- more significant for z < 0.5

- MBH in the IMBH regime for Edd. ratio ≥ 10-2

- galaxies on the MBH-M* correlation if Edd. ratio ≤ 10-6 MBH ≤ 106 M

If they undergo minor mergers detected as ULXs (nucleus of stripped galaxy)

e.g. ESO 243-49 HLX-1, NGC 2276-3c

Jet radio emission!!

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