S. Fabrika

Optical spectra of ULX

counterparts

Chandra

Hubble Space Telescope

M82

Ultraluminous X-ray sourcesX-ray luminosities > 1039 erg/s

IMBH SCAD

4/12/1 MMTin 4/32/1 MMTph

Huge UV luminosities yes yes

QPOs, tens of seconds yes yes

Radio source yes yes

Soft excess yes yes

Massive donor yes … yes

Nebulae, winds/jets no yes

Young population no yes

1. Supercritical accretion disks (SCADs) in close binaries with a stellar-mass black hole

(like SS433), observed close to the disk axis (≤ 50o)

Large intrinsic luminosity + geometrical collimation

2. Intermediate mass black holes (IMBHs) ~ 102 – 104 Mo with standard accretion isks.

They must be in close binaries with massive donors.

Extension of luminosity range

Spectroscopy of ULX nebulae

At least a part of the ULX-nebulae are dynamically

perturbed (~100 km/s on a spatial scale ~100 pc)

Emission line diagnostics of the gas excitation:

UV source (~105 К) luminosity is comparable

with that in X-rays (1040 erg/sec),

Shocks (~20-100 km/s, Lkin ~1039 erg/s)

The ULX nebulae are not SNRs

Pakull et al.

Lehmann et al.

Abolmasov et al.

HoII X-1NGC6946 ULX-1 HoIX X-1

J.Poutanen, A.Valeev, O.Sholukhova

Antennae 22 Mpc, 107 pc/”VIMOS/IFU, 13.5x13.5”/0.33”

4150-7400/1.9 A, 6 ULXs

HST/WFPC2/ACS

Chandra/HST

astrometry (<0.3”)

VLT/HST observations of ULX

in merging starburst galaxies

Antennae

Antennae galaxies

ULXs in Antennae

Sub-ULXs in Antennae

3 1038 - 1039 erg/s

Color-color and CM diagrams for

ULX-associated clusters in Antennae

Extinction estimates from spectra (Halpha/Hbeta/Hgamma)

Starburst99 models -> ages and masses

ULX

sub-ULX + ULX

SS433

A distance of SS433 to

nearest young clusters

is also about 200 pc

ULX-cluster displacements in Antennae

Association of the ULXs and high-mass X-ray binaries (HMXBs)

with extremely young (< 5 Myr) clusters is not occasional, < 0.0000001.

The coordinate displacements, < 200-300 pc, is a common property

of the HMXBs and ULXs.

Fainter X-ray sources (LMXB) loose a relation with parent clusters:

Kaaret et al. (2004), Rangelov et al. (2011).

Cluster age = Primary evolution + Secondary evolution

The ULX progenitors in Antennae are very massive

binary stars, М1 ~ М2 ~ 100 Mo or М1 ~ 2М2 ~ 100 Mo

ULXs are stellar-mass black holes with

supercritical accretion disks

Why the displacements?

They need ejection velocity ~80 km/s (if only transportation).

Cluster age = Primary evolution + Secondary evolution (+ Transportation time?)

Momentum loss at SN explosion in binary (Zwicky, 1957; Blaauw, 1961;

Shklovskii, 1976; van den Heuvel et al., 2000) produces a runaway speed

of ~50 km/s (no time for the pre-SN evolution).

Kick velocity from SN (Woosley, 1987; Cordes & Сhernoff, 1998)

gives ~5 km/s for a black hole. No time, no velocity.(but magneto-rotational SN-mechanism, Bisnovaty-Kogan, 1970)

Ejection of the binaries from clusters at their beginning stages of formation

(Moeckel, Bate, 2010; Pflamm-Altenburg, Kroupa, 2010; +++) due to

few-body encounters.

We confirm the current models of cluster formation

FOCAS spectrograph

spectral resolution 1000

region 3700-8000 А

seeing 0.4-0.9’’

4 nights

~10 hours per target

Holmberg IX X-1

V=22.8 3.6 Mpc

NGC5204 X-1

V=22.6 4.3 Mpc

Holmberg II X-1

V=21.9 3.05 Mpc

NGC4559 X-7

V=23.0 10.0 Mpc

Optical spectroscopy of ULX counterparts

Y. Ueda

A. Vinokurov

O. Sholukhova

Holmberg IX X-1 (3.6 Mpc)

NGC 4559 X-1 (10.0 Mpc)

Holmberg II X-1 (3.05 Mpc)

NGC 5204 X-1 (4.3 Mpc)

Results of the spectroscopy:

All studied ULX-objects have broad

emission lines.

The strongest are HeII 4686 A and Hα.

EW(HeII)/EW(Hβ) ≥ 2

FWHM(HeII)/FWHM(Hα) ≤ 0.8

Hydrogen content is nearly normal.

It is WNL or hot-state-LBV spectrum.

All studied ULX counterparts show the same spectra

This is homogeneous class of objects

Published spectroscopy:

NGC1313 X-2 Roberts et al. 2010

NGC5408 P13 Cseh et al., 2011

NGC7793 X-1 Motch et al., 2010

Mean EW(A): HeII Hβ Hα HeI5876 HeII5412

ULXs 9 4 25 ≤2.5 ≤1.1

SS433 20 50 300 25 2.5

WNLs, LBV and SS433

The OB Zoo: Walborn & Fitzpatrick, 2000

Classification diagram for WNL stars (Crowther & Smith, 1997)

Evolution of LBV stars AG Car, V532, HD5980 in the diagram (Sholukhova et al., 2011)

Crowther, Walborn, 2011:

ζ Pup

O2If*, O3If*

O2If*/WN5, O2.5If*/WN6, O3If*/WN7

WN6ha, WN7ha

WN11 WN9-10 WN9

• The WNL spectrum is formed in the donor star

• The spectrum is formed in a normal accretion disk with IMBH

• Supercritical accretion disks with stellar-mass BH

• New type of X-ray sources?

• The optical spectrum is formed in WNL donor

For the luminosity LX

~1040erg/s

we need ~2 10-6 MSUN

/y. The star must provide:

• The spectrum is formed in accretion disk (IMBH, M > 70 sun) with irradiation(adopt: temperature of HeII formationT ~ 4 104 t

40000K and velocity V ~ 900 V

900km/s)

a standard disk i < 6o

a warped disk i < 30o

• The spectrum is formed in a supercritical disk with a black hole like that in SS433

HI and HeI lines are 12 times weaker with respect to SS433

HeII lines are 2 times weaker

yMVm

pM SUNWN /0005.0

4

900

3/4

10

1

3/1

1000

12100m

pVorb

Exotic system with IMBH MX

>> 10 MSUN

and XWN MM ? but

34 RT

24 RT

km/s

We detect strong variations in

radial velocities 100 – 200 km/s

Roberts et al. 2010

Ho IX X-1

NGC1313 X-1

Conclision:

All the spectrally studied ULXs are stellar-mass black

holes with supercritical accretion disks

Why HI and HeI emission lines are much weaker than those in SS433?

Collimated optical and UV radiation?In SS433 optical and UV radiation are not collimated (Fabrika, Sholukhova, 2008) .

Optical luminosities of studied ULXs and SS433

In supercritical disks UV/optical luminosity

is sensitive to the mass accretion rate:

4/14/9 MMLV 2/14/3 MMTph

A decrease the mass accretion rate 2-3 times results in the wind luminosity

and temperature like those we found in ULXs

Tao et al., 2012; Vinokurov et al., 2013

SS433

Local Group imaging, Massey et al. 2006

M33

In result:

SS433 remains unique.

However we know better how and where to search for new SS433s:

they are bright stars of 21-22 magnitude up to10 Mps, with strong

and broad H-alpha emission

Thank you

The supercritical disk and its funnel in SS433

Mwind ~ 10-4 Mo /y

Twind ~ (5-7) 104K

Vwind ~ 1500 km/s

Lbol ~ 1040 erg/s

LX ~ 1036 erg/s

Jets: Lk ~ 1039 erg/s

2 j ~ 1.5º

Funnel: 2 f ~ 50º

˙

Intrinsic X-ray budget of 1040 erg/s