Mechanical versus X

Mechanical versus X-ray luminosity
Manfred W. Pakull, Observatoire de Strasbourg
coll. Roberto Soria, Christian Motch, Fabien Grisé and others
Chandra/ESO press release
S26
P13
ULXs & their environments
Strasbourg
June 13-16, 2016
NGC 7793: Home of ULX P13 (talk of C. Motch)
and of ultra - powerful jet source S26
Chandra/ESO press release
S26
P13
Outline
ULX nebulae and bubbles (ULXB)
ULXs interact with / act on the IS medium:
q Photoionization of ISM; formation of X-ray ionized
nebulae (XIN) ; measure of Lx
q Wind and jet driven bubbles -> rad. shocks;
measure of mechanical power P_wind or P_jet
q Real life: effects of both photo- and shockionisation;
not easy to disentangle
q What else can we learn from ULXB ?
The beginning: IC 342 X-1
CFHT, Hα
Laurent Mirioni & Pakull 2002
W. H.T., Integral Field spectrograph, Hα
T. Roberts et al. 2003
Tooth nebula; diameter 220 pc ! SNR-like spectrum
More Strasbourg ULXB
Holmberg IX X-1
NGC 1313X-2
26’’=400pc
30 ’’=500pc
NGC300 S10
NGC 5585 S1
some more of Strasbourg ULXB
NGC2403 X- 3 = MF14/15
Examples for close ’SNR’ doublets
really 1 extended ULX bubble
M81
N2403
MF22+MF23 = X-6
MF14+MF15 = X-3
MF: Matonick & Fesen SNR catalogs
some more of Strasbourg ULXB
NGC2403 X- 3 = MF14/15
Examples for close ’SNR doublets’
à really 1 extended ULX bubble
M81 X-6 MF22+MF23
N2403 X-3 MF14+MF15
Many ULXB appear in SNR catalogue entries !
Photoionisation of nebulae
by ULX
Holmberg II ULX
an X-ray ionized nebula
Holmberg II ULX
an X-ray ionized nebula
Broad (5 ’’) spectroscopic slit
Laurent Mirioni’s thesis
Holmberg II ULX
an X-ray ionized nebula; HeIIλ4686 emiss.)
Holmberg II ULX
an X-ray ionized nebula; HeIIλ4686 emiss.)
Holmberg II ULX
an X-ray ionized nebula; HeIIλ4686 emiss.)
Holmberg II X-1
Ha HeII [OI]
IP = 54 eV to excite 4686 recombination
radiation: must be due to photoionisation
by X-ray source (like LMC X-1)
L4686= 2.5 1036 erg/s; dia ~ 50 pc
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
HST ACS; Kaaret et al 2004
c.f. studies by Berghea et al.
and Abolmasov et al.
NGC 5408 X-1
Corbel & Kaaret 2009
detection of X-ray ionized nebula (XIN); dia ~ 30 pc
incl. HeII 4686 and [NeV] 3426
IP = 54eV
98eV
X-ray photoionization
No sharp Strömgren spheres because gas becomes optically thin for high
hν photons;
à outer region of warm (10^4 K) nearly neutral atoms .
* With respect to stellar photoionisation : + strong low-ionization lines:
[OI]λ6300, [NI] λ5200 [SII]
*
“
“
“
: + strong high-ionization lines
HeII, [OIV] (IP = 54 eV = 4Ryd) , [NeV] (IP = 97 eV)
* emission lines are narrow (FWHM < 30 km/s).
* Te ~ 10,000 K; <~ 20,000 K for Z/Zsol < 0.2 (i.e. SMC)
* Hα, {ΗeΙΙλ4686} lines ‘count ’ ionizing photons hν > 1Ryd , {>4Ryd}
* use Ferland’s Photoionization code Cloudy to derive
ionizing luminosity
A XRB in an IS cloud (n >10 cm-3) creates
1 HeII λ4686 photon per 1 X-ray photon
L4686/hν4868 ~ Lx(0.5-10keV) /2 keV
(à poor man’s X-ray telescope)
Ionization by shocks
ULXBubbles
Pakull & Mirioni 2002
NGC1313-X2
Ramsey et al 2006
a rapidly expanding nebula
Size ~ 570 x 400 pc
Vex ~ 100 km/s
highly supersonic expansion: shocks !
[ c(104K) = 10 km/s ]
E
W
λ
A few elements of shock physics
(A) Adiabatic, non-radiative shock ( no B field)
n1 = 4 n0 ;
v1= 3/4 vs ; T1 ~ 105 K v1002
(I) Isothermal, fully radiative shock (no B )
n2 = M2 n0; v2 = vs;
T2=T0
precursor
Cooling &
recombination
[0I] 6300
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
Δv ~ vs
->main difference to
XIN
Some shock diagnostics
10
1
5007/β
3
1
.3
0
[OIII]λ5007/Hβratio as function
of shock vel. vs (Dopita et al 1984)
radiative shocks
For fully radiative shocks dissipated energy
(shock luminosity per surface element [erg/cm2/s]) is
Is = ½ ρ vs3,
spherical shock: Lrad = 4π R2 Is = 2π ρ R2 vs3
Shock modeling (such as Dopita et al 96, Allen et al. 08)
will and tell you what the spectrum of this emission
is. For example what fraction comes out as X-rays, IR,
recombination radiation, such as L(Hbeta), or forbidden
lines such as [OIII], etc.
Radiative shock
Rs
Structure and Energetics
of ULX Bubbles
Wind/jet driven bubble with power Lw
and fully radiative outer shock
(Weaver+ 1977) results in self-similar
solution for hydrodynamics with
[p = (γ-1) e]
l
Rs = (125/154π)1/5 (Lw/ρ)1/5 t3/5 ; vs = 3/5 Rs /t; γ = 5/3
Combining with shock luminosity: Ls = 2π ρ R2 vs3
*** Lrad = 27/77 Lw = 0.35 Lw *** for γ = 5/3
example : Lβ = 0.005 Lrad = 0.002 Lw
for vs ~ 50-150 km/s
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 : τ ~ τ6 106 yrs;
***
Power Lw ~ 1039 erg/s ~ Lx (ULX) ***
Total energy: Eo~ 1053 erg/s (several 100 SNe !!)
With Mdot x τ = (few) *Msol; ( Lw = 1/2 x Mdot x vw2 )
vw = 0.19 c {L39 τ 6 (few–1)}0.5
(mildly) relativistic
-> agrees with recent XMM RGS results by Pinto et al. (Nature 2016);
of N1313 X-1 & N5408 X-2: vw = 0.2c
Some remarks on jets
FRII galaxy Cyg A
The first jet from ULX (proper)
Lx ~ 5E36 erg/s
kT ~ 0.3-0.8 keV
Lx ~ 7E36 erg/s
Γ ~ 1.5
Lx ~ 1.1E37 erg/s
kT ~ 0.3-0.8 keV
Mx ~ few 100 Mo
Pakull, Soria & Motch, 2010 Nature
Using formalism for ULX bubbles:
S26 long slit
along minor axis
along major axis
Hα
[NII]λ6584
HS North
(blueshifted)
*cont + Ha
HS South
(redshifted)
22 x 250 km/s
2 x 360 km/s
S26 energetics
Application of Weaver et al. wind-bubble formalism and
assuming the presence of full radiative shocks, we
estimate a jet power of
Lj ~ 3 x 1040 erg/s >> Lx ~ 7 x 1036 erg/s
GR MHD simulations (Tchekhovskoy + 14) suggest that
Lj can reach (at most) ~ 5 x L_disc (a=0.99) ; and
Ghisellini + 14 provide statistical proof for such high jet
power in a sample of BL Lacs.
à low Lx/Lj in S26 must due to X-ray absorption
(Compton-thick), or current X-ray low state of former
ULX/HLX.
Some results so far
ULX interact with IS medium – via photoionization and
through winds/jets
Photoionisation allows to measure total luminosity
(irresp. of beaming)
Optical identification of many new bubbles
ULX bubbles indicate mechanical power ~ 1039 erg/s
i.e., Lx ~ Lj t ~ 106 yrs ; Etot ~ 1053 erg
S26 in NGC 7793: super-SS433/W50 system with hot
spots (->jets); Lj ~ 3 1040 erg/s >> Lx; a ULX after all !
(presence of 23mag counterpart with broad em. lines )
Where there is one specimen,
there are probably others …
NGC1313 X-2 bis: another huge ULX bubble ?
NGC1313 Ha VLT
X-2 bis
125x225 pc Lx <1036 erg/s
Hα
broad!
X-2 ~1040 erg/s
Vexp = vs = 180 km/s
-> expanding very energetic bubble
Lw / Eo ~ 1039/1053 cgs
presently inactive ULX ?
[SII]
Where there is one specimen,
there are probably others …
The case of NGC 5408 X-2
NGC 5408
X-1
NGC 5408
« X-2 »
X-1
(also noted by Sutton+16)
VLA 4.9 GHz; Lang et al 07
0.4 mJy
X-1
3.0 mJy
X-2
NGC 5408 X-2
NGC 5408 X-1
Slit used for VLT spectroscopy
by Kaaret & Corbel (09), Cseh et al (11, 13)
NGC 5408 X-1 & X-2
[NeV] 3426
HeII 4686
X-1
X-2
[OI] 6300
X-1
SNR
X-2
Hα 6563
NGC 5408 X-1 & X-2
[NeV] 3426
HeII 4686
X-1
X-2
Two X-ray ionized nebulae (XIN), around X-1 and X2,
respectively, are only 14’’ = 340 pc apart
Note that there are only a handful known XIN
(around ULXs) in the sky.
NGC 5408 X-2
ESO-VLT
2010
log Fλ
HWZI =5000 km/s
EW = 2100 A
Hα
V=19.0
B-V=1.8
Extreme LBV-type object ?
NGC 5408 X-2
Hγ
log Fλ
P Cyg
HeIIλ4686
Hβ
P Cyg
Extreme LBV-type object ?
X-2: a Compton-thick (?) HLX
with a ‘LBV’ counterpart
•
NGC 5408 X-2 (Lx ~1037 erg/s) has a luminous (Mv = -10)
counterpart with presently (i.e. since several years) EW
(Ha) = 2000A (!) and HWZI ~ 5000 km/s.
Ha line was more narrow and weaker (EW= 400A) in 1993.
•
•
It excites a XIN suggesting HLX (~1041 erg/s);
heavily absorbed ?, now only weakly active ?
Radio luminosity ~ 8 x Cas A
•
•
Suggestion of common-envelope spiral-in phase of a MXB;
BB: RBB = 5,000 Rsol; take M = 100 -> Porb =30 yrs
X-2: evolutionary scenario
Question of timescale for
spiral-in.
here: > 20 yrs
Orbital decay timescale
depends strongly on stage of
core He burning (c.f. Taam &
Sandquist ARAA 00).
-> Key object for study of
massive binary evolution.
Belczynski+ 16
The end
Merci
&
Danke schön