growing black holes: from the first seeds to agn mar mezcua harvard-smithsonian center for...
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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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