optical spectra of ulx counterparts - inaf iasf...
TRANSCRIPT
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