searching for intermediate mass black holes -...

1Natalie WebbULXs and their environments, June 2016

Searching for intermediate mass

black holes

Natalie Webb

Institut de Recherche en Astrophysique et PlanétologieToulouse, France

2

• Black holes : stellar mass, ~310s M⊙; supermassive, 10 610 M

⊙

• Black holes proposed : intermediate mass, 10 25 M⊙

(IMBH)

Context

Natalie WebbULXs and their environments, June 2016

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)

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HLX1

2XMM J011028.1460421 (Farrell, Webb et al., Nature, 2009)~8” from nucleus of ESO 24349 (z=0.0224, ~95 Mpc)If associated with ESO 24349 => Lx=1.1x1042 erg s1 (0.210.0 keV)

=> from Eddington luminosity (LEdd), M = 5000 M⊙

Superceding LEdd by a factor 10 (Begelman 02) => M > 500 M⊙


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Wiersema et al. (2010)

HLX1


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 ?

HLX1


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8.2 σ, 45 μJy3 σ upper limit, 21 μJy (5+9 GHz)

Webb et al., Science (2012)

Servillat et al. (2011)

HLX1


~1 yr~1 yr~1 yr ~1.25 yr~1 yr ~1 yr ~1.12 yr >1.4 yr

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2XMM J011028.1460421~8” from nucleus of ESO 24349 (z=0.0224, ~95 Mpc)

HLX1

Vmin

~ 25.4

Vmax

~ 23.6

Rmin

~ 24.5

Rmax

~ 23.5

Webb et al. (2014)


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HLX1

X(Godet et al. 2014)

Orbital evolutionof polytropic companion, n=1.5, =5/3. Γ

Initial periapsis separation

(relative to tidal radius) of 2.3 (red),

2.4 (magenta), 2.5 (blue), 2.7 (black),

λ = R/0.01R ,⊙ M4=MBH/104 M⊙


.

Lasota et al. (2011)

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MUSE observations of the environment of HLX1

Crédit : CXO

Webb et al. (2016)Natalie Webb

ULXs and their environments, June 2016

10

MUSE observations of ESO 24349

Crédit : CXO

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 & initial diskiness of galaxy is thus preserved

Webb et al. (2016)


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HLX1

Crédit : CXO

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

Webb et al. (2016)



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Other intermediate mass black holes

Crédit : CXO

From Earnshaw et al. (2016)

Spectrum : Г~1.5, Lx = 2.2x1038 5.1 x 1039 erg s1

Low frequency break in power spectrum => MBH

< 1.6 x 103 M⊙

Radio & Xray fluxes (fundamental plane) => MBH

< 3.5 x 104 M⊙

M51a

Crédit : CXO

Heida, Jonker & Torres (2015)CXO J122518.6+144545

Natalie WebbULXs and their environments, June 2016 13


182 Mpc

14

Crédit : CXO


Tidal disruption events (TDE)

(Rees, Nature, 1988)

Tidal radius inside blackhole event horizon for masses > 108 M

⊙

Observe TDE from lowermass BHs

~105 – 104 event/gal./yr

~30 such events observed (Komossa 2015)

~


15

Crédit : CXO


~

Tidal disruption events

NH

=0.74+0.70

x1021 cm-2

kT = 57.8+3.9 eVΓ = 3.71+0.59

Χ2

ν = 0.92 (115 dof)

-3.9

-0.70

-0.59

Lin et al. (2011)

Coincident with centre of IC 4765f011504 at z=0.0353

Galaxy inactive

Modelling the disc with kerrbb ⇒ M

BH ~ 6 x 104 – 4 x106 M

⊙

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Crédit : CXO

z=0.42 (d~2.3 Gpc)

If at Eddington in X1 => M

BH ~ 1 x 105 M

⊙

Lin et al. (2016)Natalie Webb

ULXs and their environments, June 2016

3.8 hr period from the galaxy J1231+11

Ho et al. (2011) estimate mass ~105 M ⊙

from narrow emisson lines

No longer detectable with Swift

If QPO is the low frequency type, M

BH < 4 x106 M

⊙ Lin et al. (2013)

Tidal disruption events2003

2005

2005


Intermediate mass black holes in low mass galaxiesMuch 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)

Graham & Scott (2013) identified ~50 lower luminosity spheroids with AGN that have M

BH < 105 M

⊙

Investigated 17 candidates with Xray/radio data and placed objects on black hole fundamental plane (Koliopanos et al. in prep.)

~

Red dots = (luminous) coreSérsic galaxies blue circles = (intermediateluminosity) Sérsic galaxies & bulges, open crosses = barred.


Intermediate mass black holes in low mass galaxiesP

re

li

mi

na

ry

(Koliopanos et al. in prep.)

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Summary

HLX1 is an excellent intermediate mass black hole (IMBH) candidate of ~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 linecontemporary 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


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Open questions....

What is the size and the distribution of the population of IMBHs ?

how are IMBH formed ?

how do IMBH evolve (mergers/accretion) ?

Can we detect radial velocity from HLX1 to understand the orbit ?

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


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Backup slides

Backup slides


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MUSE observations of ESO 24349

Crédit : CXO


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Scott & Graham 2013

Crédit : CXO

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


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Graham & Scott (2013)

Crédit : CXO(a) central velocity dispersion , (b) Ksband host spheroid magnitude, σand (c) Bband host spheroid magnitude. The red dots represent the (luminous) coreSérsic galaxies and the blue circles represent the (intermediateluminosity) Sérsic galaxies and bulges, while the open crosses designate those which are barred.


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Scott & Graham 2013

Crédit : CXO

Schematic showing the evolutionary path of "dry" galaxy mergers as they branch off from the steeper, nearquadratic, Mbh–L relation for Sérsic galaxies built from "wet" mergers and/or gasrich processes.


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Scott & Graham 2013

Crédit : CXO

Predicted Intermediate Mass Black HolesGalaxy 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 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


searching for intermediate mass black holes -...

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