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ULX: Photon/mechanical luminosities Manfred W. Pakull, Observatoire de Strasbourg coll. Roberto Soria, Christian Motch, and others
Bamberg, June 18-22, 2012
Leiden, April 3, 2014
Manfred W. Pakull, Obs. de Strasbourg coll. R. Soria, C. Motch, Fabien Grisé & others
Non-nuclear sources @ non-X ls
S26 in NGC 7793
Non-nuclear sources @ non-X ls
Manfred W. Pakull Observatoire de Strasbourg coll.: R. Soria, C. Motch, F. Grisé & others
Leiden, April 2, 2014
NGC 1313 X-2
Outline
We can learn a lot about a phenomenon at wavelengths other than @ discovery
e.g. UV: 0 star winds; radio: jets and lobes from AGN; X-ray: hot gas in ClG
Here: ULXs at radio, optical, IR
Counterparts proper: see Fabien Grisé’s talk
Me: Action on – and interaction with ISM due to photoionization and winds and jets
ULX bubble IC 342 X-1
CFHT, H
Laurent Mirioni & Pakull 2002 W. H.T., Integral Field spectrograph, H T. Roberts et al. 2003
Tooth nebula; diameter 220 pc ! SNR-like spectrum
H VLT
*
bubble diameter ~ 26’’ = 400 pc (!); SNR like spectrum !
ULXB NGC 1313 X-2
Pakull & Mirioni 02, 03; Grisé et al. 08
The ‘SNR’ around HolmbergIX X-1
Holmberg IX X-1 = M81 X-9: Lx ~1040 erg/s; Grisé et al 2011 Miller (1995): X-ray superluminous SNR; but X-ray variable point source! see also Abolmasov & Moiseev 2008
SE
Subaru Ha [OIII] B
30 "
=
500 pc
Pakull & Mirioni 2002 NGC1313-X2 a rapidly expanding nebula
Size ~ 570 x 400 pc
Vex ~ 100 km/s
highly supersonic expansion !
E
W
Ramsey et al 2006
l
What makes ULXBs shine ?
Photoionisation by the X-ray source (and companion)
radiative shocks from highly supersonically expanding gas (a bit like SNRs)
NB: in many ULX bubbles, there is indication for both: photoionization
and shock-ionisation, ex. Holmberg IX, NGC 1313 X-2, N6946-MF16;
c.f. Abolmasov et al. 2007, 8
Same problem in AGNs, Liners, …
X-ray photoionization (XIN) No sharp Strömgren spheres because gas becomes optically thin for high hn photons; outer region of warm (10^4 K) nearly neutral atoms . With respect to stellar photoio: + strong low ionization lines [OI]l6300, [NI] l5200 [SII]; (but can be destroyed by O companion) With respect to stellar photoio: + very high ionization lines, HeII, [OIV] (IP = 54 eV=4Ryd) , [NeV] (IP = 97 eV) Te ~ 10,000 K; <~ 20,000 K for Z/Zsol < 0.2 (i.e. SMC) H, {HeIIl4686} ‘count ’ ionizing photons hn > 1Ryd , {>4Ryd} use Ferland’s Photoionization code Cloudy -> Possibility to derive ionizing luminosity from recomb. lines
Calibrating XIN (around M33 X-7)
Eclipsing (3.45 d MXRB, 16 Mo BH + 70 Mo O star Pietsch et al 2006, Orocz et al 2007 (48 GMOS spectra)
* Sits in HII region B0208f with HeII l4686 emission d(He++) = 4.5’’ = 20 pc * He+ -> He++ photoionisation by the X-ray source Pierre Maggi, Xian Hou & MWP 2012, 2014
Modelisation of photoionisation with Cloudy: degeneracy between models can be lifted (PowL, DiskBB, KerrBB excluded !) Brems, p-free-DiskBB (T~r-p) allowed
M33 X-7 cont
M33 X-7: L(4686)/L(0.3-10) = 2E 35 / 1E 38 ~ 0.002
LMC X-1: L(4686)/L(0.3-10) 2 E35/2 E38 ~ 0.001, Pakull&Angebault 1986
-like
Holmberg II X-1
HST ACS; Kaaret et al 2004
Ha HeII [OI]
Pakull & Mirioni 2002; Mirioni 2003 thesis; CFHT broad-slit
L4686= 2.5 1036 erg/s
Using Cloudy , one derives an integrated X-ray luminosity Lx ~ 6 10 39 erg/s
No strong beaming here !! L(4686)/L(0.3-10) ~ 0.0002
[OIV] l25.9 emission in Holmberg II X-1
Spitzer observations: Berghea et al. 2009 note: IP (O++) ~ IP(He+) ~ 54 eV Extensive Cloudy modeling: Lx = 1.2E40 erg/s
Interesting: an XRB in an IS cloud (n >10 cm-3) creates
1 HeII l4686 photon per 1 X-ray photon
L4686/hn4868 ~ Lx(0.5-10keV) /2 keV
( poor man’s X-ray telescope)
A few elements of shock physics (A) Adiabatic, non-radiative shock ( no B field) n1 = 4 n0; v1= 3/4 vs ; T1 ~ 105 K v100
2
(I) Isothermal, fully radiative shock (no B field) n2 = M2 n0; v2 = vs; T2=T0
Dopita & Sutherland 95 vs = 400 km/s
high- and low-ionization lines formed @ different Te e.g., Te[OIII] ~ 30-40 kK Te[OI] ~ 8 kK broad emission lines Dv ~ vs
precursor
[0I] 6300
Cooling & recombination
Shock diagnostics
[OIII]l5007/Hb ratio as function of shock vel. vs (Dopita et al 1984)
10 3 1
.3
5007/b
[OIII]l5007/Hb
[OI]l6300/Hb
Hb
log distance from shock uncomlete radiative shock (see Raymond et al 1988)
100
10
1
0.1
1
0
radiative shocks
For fully radiative shocks dissipated energy (shock luminosity per surface element [erg/cm2/s]) is l = ½ r vs
3, spherical shock L = l4p R2 = 2p r R2 vs3
and a certain fraction is radiated as H recombination radiation, i.e., lb (~0.003 x l) Dopita et al 96, Allen et al. 08
+ precursor emission (photoionized by X-ray/EUV emission from shock) observable spectrum depends on vs ; age (completeness)
lb = 7.4x10-6 vs2.4 n0 erg/cm2/s
Structure and Energetics of ULX Bubbles
l
self–similar solution for hydrodynamics; p = (g-1) e
Rs = (125/154p)1/5 (Lw/r)1/5 t3/5; vs = 3/5 Rs /t; g = 5/3
= (125/224p)1/5 “ “ “ ; = 4/3
Wind/jet driven bubble with power Lw and radiative outer shock (Weaver et al 1977)
Lrad = 27/77 Lw = 0.35 Lw for g = 5/3 = 27/112 Lw = 0.24 Lw = 4/3
Lw ~ 500* Lb for vs ~ 50-150 km/s
Radiative shock
Energetics of ULX Bubbles
• Bubble radii R ~200 pc (i.e. >> SNR)
• Expansion velocity vs ~ 80 – 150 km/s
• IS densities n ~ 0.1 - 1 cm-3
Age : t ~ 106 yrs;
Power Lw ~ 1039-40 erg/s ~ Lx (ULX) Total energy: Eo~ 1053 erg/s (several 100 SNe !!)
With Mdot x t = m Msol; m limited to a few; ( Lw = 1/2 x Mdot x vw2 )
vw = 0.19 c (L39 t 6 m–1)0.5 (mildly) relativistic
Estimate: ~ 25 % ULX blow observable bubbles
If ULX photon emission strongly beamed, than there
should be many ULXB with ULXs that are beamed away from us
Expect many more ULXB from apparently faint, or
presently inactive, or misaligned ULXs
Search for compact X-ray sources among
large SNRs candidates
some very large SNR candidates…
Lozinskaya & Moiseev 2007
Log - logD for SNR
S1-N5585
10 100 300 pc
IC 10: Bubble around XRB WR + 30 Mo BH (LM 2007) NGC 5585 S1: new ULX (Pakull & Grisé 2008)
very large ‘SNR’ ULX bubble
5.0
Matonick & Fesen 1997 noted huge
(200x300) pc ‘SNR’ in NGC 5585
300 pc
Later, R. Soria detected Chandra point
source (Lx~ 5 1039 cgs);
-> another case of a previously identified
‘SNR’: Ho IX, N6946X-1; M81X-6, … First case of an optically predicted/selected ULX
NGC1313: another huge ULX bubble ?
NGC1313 Ha VLT
X-2 ~1040 erg/s
H [SII]
Vexp = vs = 180 km/s -> Energetic bubble
Lw / Eo ~ 1039/1053 cgs
presently inactive ULX ?
Lx < 1037 erg/s
125x225 pc
HLX in NGC 470 (d=38 Mpc) Sutton, Roberts et al 2012: most extreme ULXs
Lx ~ 2-10 E40 erg/s
HII #46
HeII l4686
[OI ] ll6300,60
[NII] l5200
ESO VLT VM test observations 2011: ‘easy’: 1 ksec integration time
XMM/Chandra 2004 - 2009
HLX in NGC 470 (d=38 Mpc)
F4686 ~ 5 10-17 cgs L4686 = 1. 1037 erg/s ~ 4 x Holm II Mv = -11.2 like HLX1
HII #46
HeII l4686
[OI ]ll 6300, 60
[NII] l5200
Emission of NGC 470 HLX photoionizes; isotropic ! i.e. not beamed
“SNR” S26 in NGC 7793 (d=3.9 Mpc)
S26: Blair & Long 1997; faint ROSAT source: Read & Pietsch 1999
300 pc
H R
Pakull, Soria & Motch, 2010 Nature
Lx ~ 5E36 erg/s
Lx ~ 7E36 erg/s
Lx ~ 1.1E37 erg/s
~ 1.5
kT ~ 0.3-0.8 keV
kT ~ 0.3-0.8 keV
Mx ~ few 100 Mo
S26 and FR II radio galaxies similar morphologies
Soria et al. 2010 MNRAS
ATCA 9 GHz
1 : 1000
O – X-ray sources
S26 long slit along major axis incl. central star & hot spots ESO VLT 2011
HS North (blueshifted) *cont + *H em HS South (redshifted) 2 x 360 km/s
H [NII]l6584
S26 long-slit; short axis incl central star ESO VLT 2011
*H *HeI l6678
cont 23mag *
central star (B~23.0 mag) displays broad (HWZI~1000 km/s) redshifted emission in HeI l6678 and H (EW~ a few 100 A) very strong stellar wind activity (like SS433!)
Vex = vs =240 km/s
SS433 = ULX ? (see Fabrika 2006)
mechanically inflated Bubble W50 (SNR??) with ‘ears’ due to v = 0.26c jets Lmech = LJ ~ 1039 erg/s
200 pc
ASCA image (Kotani 1998)
Begelman’s ‘beambags’
radio-image
SS433 seen from far away: triple source ! Like S26
ULXs, SS433, jets, bubbles
VLBA; credit: NRAO/ AUI/NSF
Hol II: Cseh et al 2014 S26: Pakull et al. 2010 M83 MQ1 Soria et al 2014
Proposed discussion SS433, S26 = edge-on ULXs ?
Conclusions ULX interact with IS medium - photoionization and winds/jets Photoionisation allows to measure total luminosity (irresp. of beaming) Optical identification of HLX-2 (=NGC 470X-1) and of new bubbles ULX bubbles indicate mechanical power ~ 1E39 - 1E40 erg/s ~ Lx t ~ 1E6 yrs ; Etot ~ 1E53 erg S26 in NGC 7793: super-SS433/W50 system with hot spots (->jets); Lj ~ 5E40 erg/s >> Lx; 23mag counterpart with broad em. lines Propose to discuss relation between ULXs and QSOs