Searching for intermediate mass black holes
Natalie Webb
Institut de Recherche en Astrophysique et Planétologie Toulouse, France
Natalie Webb 1 ULXs and their environments, June 2016 Context • Black holes : stellar mass, ~310s M ; supermassive, 10 610 M ⊙ ⊙ • Black holes proposed : intermediate mass, 10 25 M (IMBH) ⊙ expect ~90% of ~109 M ⊙ galaxies contain ~104 M ⊙ black holes today
expect ~50% of ~109 M ⊙ galaxies contain > 105 M ⊙ black holes today (Greene, 2012)
Natalie Webb 2 ULXs and their environments, June 2016 HLX1
2XMM J011028.1460421 (Farrell, Webb et al., Nature, 2009) ~8” from nucleus of ESO 24349 (z=0.0224, ~95 Mpc) 42 1 If associated with ESO 24349 => Lx=1.1x10 erg s (0.210.0 keV)
=> from Eddington luminosity (LEdd), M = 5000 M⊙
Superceding LEdd by a factor 10 (Begelman 02) => M > 500 M⊙
Natalie Webb 3 ULXs and their environments, June 2016 HLX1
Wiersema et al. (2010)
Presence of Hα line confirmed by Soria et al. (2013)
Lasota, King & Dubus (2015) question the distance to HLX1
Does the system originate in ESO 24349 or is it due to a merger ?
Natalie Webb 4 ULXs and their environments, June 2016 HLX1
Webb et al., Science (2012)
3 σ upper limit, Servillat et al. (2011) 8.2 σ, 45 μJy 21 μJy (5+9 GHz)
Natalie Webb 5 ULXs and their environments, June 2016 HLX1
~1 yr ~1 yr ~1 yr ~1.12 yr ~1.25 yr >1.4 yr
Natalie Webb ULXs and their environments, June 2016 HLX1
2XMM J011028.1460421 ~8” from nucleus of ESO 24349 (z=0.0224, ~95 Mpc)
V ~ 25.4 min V ~ 23.6 max
R ~ 24.5 min R ~ 23.5 max
Webb et al. (2014)
Natalie Webb 7 ULXs and their environments, June 2016 HLX1
Lasota et al. (2011)
Orbital evolution . of polytropic companion, n=1.5, Γ =5/3. Initial periapsis separation X (relative to tidal radius) of 2.3 (red), 2.4 (magenta), 2.5 (blue), 2.7 (black), λ = R/0.01R⊙, (Godet et al. 2014) M =M /104 M⊙ 4 BH Natalie Webb 8 ULXs and their environments, June 2016 MUSE observations of the environment of HLX1
Crédit : CXO
Webb et al. (2016)
Natalie Webb 9 ULXs and their environments, June 2016 MUSE observations of ESO 24349
Galaxy mass ~ 8.1 x 1010 M ⊙
Supermassive black hole mass ~ 1 x 108 M ⊙
No evidence for a recent collision/merger
A rapidly spinning disc compared to slower bulge can indicate dry minor mergers in galaxy history, e.g. Arnold et al. (2014)
Minor merger scenario (Webb et al. 2010, Mapelli et al. 2013) possible
Younger, metalpoor halo, indicates little matter has been accreted & Crédit : CXO initial diskiness of galaxy is thus preserved
Webb et al. (2016)
Natalie Webb 10 ULXs and their environments, June 2016 HLX1
Observations in low/hard state
Hα line flux diminished by > factor 10
Confirms association of line with HLX1 and thus distance to HLX1
No radial velocity information due to faintness of line
No other lines from HLX1 to understand environment
Crédit : CXO
Webb et al. (2016)
Natalie Webb 11 ULXs and their environments, June 2016 Other intermediate mass black holes
From Earnshaw et al. (2016)
M51a
Spectrum : Г~1.5, L = 2.2x1038 5.1 x 1039 erg s1 Crédit : CXO x Low frequency break in power spectrum => M < 1.6 x 103 M BH ⊙ Radio & Xray fluxes (fundamental plane) => M < 3.5 x 104 M BH ⊙
Natalie Webb 12 ULXs and their environments, June 2016 Other intermediate mass black holes
CXO J122518.6+144545 Heida, Jonker & Torres (2015)
182 Mpc
Crédit : CXO
Natalie Webb ULXs and their environments, June 2016 13 Other intermediate mass black holes
Tidal disruption events (TDE)
(Rees, Nature, 1988)
Tidal radius inside black hole event horizon for masses > 108 M ~ ⊙
Observe TDE from lower mass BHs
5 4 ~10 – 10 event/gal./yr Crédit : CXO
~30 such events observed (Komossa 2015)
Natalie Webb 14 ULXs and their environments, June 2016 Tidal disruption events
Coincident with centre of IC 4765f011504 at z=0.0353
Galaxy inactive
Modelling the disc with kerrbb ⇒ M ~ 6 x 104 – 4 x106 M BH ⊙ Lin et al. (2011) N =0.74+0.70 x1021 cm-2 H -0.70 +3.9 ~ kT = 57.8 -3.9 eV +0.59 Γ = 3.71-0.59 Χ2 = 0.92 (115 dof) ν
Crédit : CXO
Natalie Webb 15 ULXs and their environments, June 2016 Tidal disruption events
2003 3.8 hr period from the galaxy J1231+11 Ho et al. (2011) estimate mass ~105 M ⊙ from narrow emisson lines 2005 No longer detectable with Swift If QPO is the low frequency type, 6 2005 M < 4 x10 M BH ⊙ Lin et al. (2013)
z=0.42 (d~2.3 Gpc) If at Eddington in X1 Crédit : CXO => M ~ 1 x 105 M BH ⊙ Lin et al. (2016)
Natalie Webb 16 ULXs and their environments, June 2016 Intermediate mass black holes in low mass galaxies Much work done by J. Greene & collaborators searching low mass tail of the SMBH massvelocity dispersion and massbulge luminosity relations.
Improvements to massspheroid luminosity relation (Graham & Scott, '13)
Red dots = (luminous) coreSérsic galaxies blue circles = (intermediateluminosity) Sérsic galaxies & bulges, open crosses = barred.
Graham & Scott (2013) identified ~50 lower luminosity spheroids with AGN that have M < 105 M BH ~ ⊙
Investigated 17 candidates with Xray/radio data and placed objects on black hole fundamental plane (Koliopanos et al. in prep.)
Natalie Webb 17 ULXs and their environments, June 2016 Intermediate mass black holes in low mass galaxies
y r a n i
m i l e r P (Koliopanos et al. in prep.)
Natalie Webb 18 ULXs and their environments, June 2016 Summary
2XMM J011028.1460421 HLX1 is an excellent intermediate mass black hole (IMBH) candidate of~8” from nucleus of ESO 24349 (z=0.0224, ~95 Mpc) ~2x104 M ⊙
HLX1 fuelled by tidal stripping of companion in a short lived, highly elliptical binary
Distance and luminosity to HLX1 confirmed by variability of Hα line contemporary wth the Xray variability
Other IMBH may also be detected if they tidally strip/disrupt a star
Tidal disruption events may offer another way to locate new IMBHs
Some low mass galaxies may well be home to IMBH
Natalie Webb 19 ULXs and their environments, June 2016 Open questions....
2XMM J011028.1460421 Can we detect radial velocity from HLX1 to understand the orbit ?~8” from nucleus of ESO 24349 (z=0.0224, ~95 Mpc)
Was HLX1 born in ESO 24349 or is it the result of a minor merger ?
What is the nature of the environment around HLX1 ?
Require observations to constrain properties
...and simulations to understand the history of the galaxy
What is the size and the distribution of the population of IMBHs ? how are IMBH formed ? how do IMBH evolve (mergers/accretion) ?
Natalie Webb 20 ULXs and their environments, June 2016 Backup slides
2XMM J011028.1460421 ~8” from nucleus of ESO 24349 (z=0.0224, ~95 Mpc)
Backup slides
Natalie Webb 21 ULXs and their environments, June 2016 MUSE observations of ESO 24349
Crédit : CXO
Natalie Webb 22 ULXs and their environments, June 2016 Scott & Graham 2013 sample of 72 galaxies with reliable supermassive black hole masses derive the M bh(host spheroid luminosity, L) relation Ks band 2MASS data gives nearlinear relation M bh∝ L 1.10 ± 0.20 Ks for the coreSérsic spheroids thought to be built in additive dry merger events, relation M bh∝ L 2.73 ± 0.55 Ks for Sérsic spheroids from gasrich processes. advocate that the nearlinear M bhL and M bhM Spheroid relations at high masses may have arisen from additive dry merging of galaxies. new Sérsic M bhL equations predict the masses of candidate intermediate mass black holes in almost 50 lowluminosity spheroids containing active galactic nuclei Crédit : CXO
Natalie Webb 23 ULXs and their environments, June 2016 Graham & Scott (2013)
(a) central velocity dispersion σ , (b) Ksband host spheroid magnitude, and (c) Bband host spheroid magnitude. The red dots represent the Crédit : CXO (luminous) coreSérsic galaxies and the blue circles represent the (intermediateluminosity) Sérsic galaxies and bulges, while the open crosses designate those which are barred. Natalie Webb 24 ULXs and their environments, June 2016 Scott & Graham 2013
Schematic showing the evolutionary path of "dry" galaxy mergers as they branch off from the steeper, near quadratic, Mbh–L relation for Sérsic galaxies built from "wet" mergers and/or gas
rich processes.
Crédit : CXO
Natalie Webb 25 ULXs and their environments, June 2016 Scott & Graham 2013
Predicted Intermediate Mass Black Holes Galaxy log M_bh/M_sun NGC 3185 -20.80 -20.94 5.3 +or- 0.9 NGC 3593 -20.70 -21.03 5.4 +or- 0.9 NGC 3600 -19.20 -19.72 4.0 +or- 1.1 NGC 3729 -20.10 -20.24 4.6 +or- 1.0 NGC 4245 -20.80 -20.93 5.3 +or- 0.9 NGC 4314 -21.00 -21.11 5.5 +or- 0.9 NGC 4369 -20.90 -21.01 5.4 +or- 0.9 NGC 4470 -20.40 -20.53 4.9 +or- 1.0 NGC 3003 -19.60 -20.09 4.4 +or- 1.0 NGC 3043 -20.80 -21.17 5.6 +or- 0.9 NGC 3162 -20.00 -20.12 4.4 +or- 1.0 NGC 3344 -19.30 -19.41 3.7 +or- 1.1 NGC 3507 -20.90 -21.01 5.4 +or- 0.9 NGC 3684 -20.60 -20.74 5.1 +or- 1.0 NGC 3686 -20.60 -20.72 5.1 +or- 1.0 NGC 3756 -18.20 -18.43 2.6 +or- 1.3 IC 467 -19.20 -19.50 3.8 +or- 1.1 NGC 514 -19.90 -20.02 4.3 +or- 1.0 NGC 628 -20.40 -20.51 4.9 +or- 1.0 NGC 864 -19.90 -20.03 4.3 +or- 1.0 NGC 2276 -20.90 -21.01 5.4 +or- 0.9 NGC 2715 -19.20 -19.56 3.8 +or- 1.1 NGC 2770 -19.10 -19.50 3.8 +or- 1.1 NGC 2776 -20.90 -21.01 5.4 +or- 0.9 NGC 2967 -20.30 -20.41 4.8 +or- 1.0 NGC 3041 -19.90 -20.05 4.4 +or- 1.0 NGC 3198 -19.80 -20.11 4.4 +or- 1.0 NGC 3359 -20.80 -20.97 5.4 +or- 0.9 NGC 3430 -20.10 -20.29 4.6 +or- 1.0 NGC 3433 -20.40 -20.51 4.9 +or- 1.0 NGC 3486 -19.90 -20.03 4.3 +or- 1.0 NGC 3596 -21.00 -21.11 5.5 +or- 0.9 NGC 3666 -18.20 -18.63 2.8 +or- 1.2 Crédit : CXO NGC 3726 -20.10 -20.24 4.6 +or- 1.0 NGC 3780 -20.20 -20.32 4.7 +or- 1.0 NGC 3938 -20.50 -20.61 5.0 +or- 1.0 NGC 4062 -18.50 -18.78 3.0 +or- 1.2 NGC 4096 -19.40 -19.84 4.1 +or- 1.1 NGC 4136 -18.00 -18.11 2.2 +or- 1.3 NGC 4152 -20.80 -20.92 5.3 +or- 0.9 NGC 4212 -20.10 -20.27 4.6 +or- 1.0 Natalie Webb 26 ULXs and their environments, June 2016