Jet inflated bubbles: facts (and fiction)

Manfred W. Pakull, Observatoire de Strasbourgcoll. Roberto Soria, Christian Motch, and others

HEPROIII, Barcelona, June 27-July 1, 2011

S26 in NGC 7793: Chandra/ESO press release

Outline

-- bubble nebulae around Ultraluminous X-ray sources

-- microquasars and interaction with IS medium

-- Rosetta Stone S26 in NGC 7793: micro FRII-type source with reliably measured jet power

Ultraluminous X-ray sources (ULX)

X-2

NGC 1313

Lx > 3 1039 erg/s = Ledd (20 Mo)

Various hypotheses (XRB)

super-Eddington

beamed emission

IMBH (100 - 104 Mo)

I will show: ULX also emit winds/jets with Lmech ~ Lx

NGC 1313 X-2

H VLT

*

bubble diameter

~ 26’’ = 400 pc (!)

Optical spectra:shock ionised

Vs ~ 100 km/s

Pakull & Mirioni 2002, Pakull et al. 2006

ULX IC 342 X-1

• "Tooth" nebula situated in

spiral arm has a diameter

of 220pc (Pakull & Mirioni 2002; Roberts et

al. 2003; Grisé et al 2006)

• SNR-like spectrum:[SII]/H=1.2[OI] 6300/H=0.4

• X-ray or shock ionization ?

• see poster of D. Csehfrom Laurent Mirioni’s thesis

CFHT, H

The ‘SNR’ around HolmbergIX X-1

Holmberg IX X-1 = M81 X-9: Lx ~1040 erg/s; Grisé et al 2011Miller (1995): X-ray superluminous SNR; but X-ray variable point source!SE: shock breakout (?)

SE

Subaru

Ha [OIII] BB30 "

=

500 pc

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, are

presently inactive or have not yet been discovered

(200x300) pc ‘SNR’ #1 in NGC 5585 (Matonick & Fesen 1997) is optically selected ULX !

Chandra

ULX !

Kinematics of ULX bubbles

Holm IX NGC1313 X-2

IC 342 X-1 Holm II

H

[NII] 6584

Vexp = 80 – 150 km/s >> 10 km/s (cs for T~104 K)

NS

NS

NS

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

wind/jet driven bubble with power Lw (Weaver et al

1977)

R = 0.76 (Lw/)1/5 t3/5; t = 3/5 R/v

Lw = 5 1039 erg/s R1002 x v100

3 x nfully radiative shock with vs implies for total radiative lumisosity & H

Luminosity

Lrad = 27/77 x Lw ; L = f(vs) x Lw

t~106 yrs; Lw~1039-40 erg/s ~ Lx (ULX) ; Eo~1053

erg/s

(SS433/W50 - like; Pakull & Mirioni 2002; Pakull & Grisé 2006)

Galactic QSO: Cyg X-1

Russell et al. 2007

5pc

Gallo et al. 2005: thermal radio emission

[OIII]:

PJ ~ 4 x1036 – 1037 erg/s PJ ~ 30 – 100 % Lbol; compact source too radio faint: . ‘’dark’’ outflow

100x smaller than W50

~100xweakerjet

QSO SS433 & W50

mechanically inflatedBubble W50 (SNR??)with ‘ears’ due to v = 0.26c jets

Lmech = LJ ~ 1039 erg/s200 pc

ASCA image(Kotani 1998)

Begelman’s ‘beambags’i.e. linear triple XRS

radio-image

SS433 seen from far away…

Discovery of a 2ndS433/W50- type object

Pakull & Grisé 2008 in “Population explosion”Pakull, Soria, Motch 2010 Nature Soria, Pakull, et al 2020 MNRAS

after ~ 30 years of effortfrom many people…

“SNR” S26 in NGC 7793 (d=3.9 Mpc)

S26: Blair & Long 1997; faint ROSAT source: Read & Pietsch 1999

300 pc

HR

“SNR” S26 in NGC 7793 = triple XRS

Chandra archive; 50 ks; PI: Pannuti

X-ray

0.3- 1 .0 keV1.0 - 2.0 keV2.0 – 8.0 keVContours: H

Pakull, Soria & Motch, 2010 NaturePakull, 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: Vexp ~ Vs ~ 250 km/s >> cs

ESO VLT long-slit spectro HST H (Soria et al. in prep)night-sky night-sky

23 magcounterpart

Optical spectra: Optical spectra: complete shocksshocks fully radiative bubble with R~100 pc, vfully radiative bubble with R~100 pc, vs ~ 250 km/s ~ 250 km/s

t = 2 10t = 2 105 yrs; yrs; LJ = 5 x 1040 erg/s (>> Lx)

+ 9 GHz radio contours = 0.7; opt. thin syn.

S26: X-ray/ radio image

X-ray Hot Spots lead radio HS

S26 and FR II radio galaxiessimilar morphologyities

Soria et al. 2010 MNRAS ATCA 9 GHz

1 : 1000

O – X-ray sources

S26 and FR II radio galaxiesimportant difference

S26: highly supersonic expansion of cocoon into ISM i.e. M >> 1 radiative shock

radio galaxies: M~1 expansion into hot (kT ~ keV) IGM pdV work (4pV cavity enthalpy)

warm ISM hot IGM:cluster gas

Assume magnetic field ~ in equipartition with relativistic energy densityAssume magnetic field ~ in equipartition with relativistic energy density

In hot spots, In hot spots, jet energy transferred to: relativistic electrons (relativistic electrons (~ 1—1E5): = 1 radiating~ 1—1E5): = 1 radiating relativistic protons and He nuclei : = k non-relativistic protons and He nuclei : = k non-radiatingradiating BB2//88 thermal gas radiatingthermal gas radiating

= = E (rel + B) / E(total) (<< 1)E (rel + B) / E(total) (<< 1)

Calculate synchrotron emission and radio flux density fromCalculate synchrotron emission and radio flux density from PPJ, n, t, n, t

only a fraction { } = only a fraction { } = a few E(-3) of the jet power is of the jet power is . . transferred to relativistic electrons transferred to relativistic electrons

What about the radio lobes of S26?

Compare with observed radio flux densityCompare with observed radio flux density

predicted:predicted: S = 1020 {1.85 /(1+k)} mJy 5–0.7

(see also Heinz 2002, Bordas et al 2009)(see also Heinz 2002, Bordas et al 2009)

S26 radio flux S = 2.1 mJy 5–0.7; 5 = 5 GHz

S26 and radio galaxies

Calibration of { } = f (k, Calibration of { } = f (k, is is long-standing problem, long-standing problem,

also for AGNalso for AGN

(eg, Willott et al 1999)(eg, Willott et al 1999)

S26 is a rare object S26 is a rare object with direct estimates with direct estimates of both proxiesof both proxies

S26

Cavagnolo et al (2010): relation between radio lobe luminosity P(1.4GHz) and power injected into the bubble, for a sample of AGN

Power into relativistic electrons ~ (1/100) of the total jet powerPower into relativistic electrons ~ (1/100) of the total jet power

S26

{ } =1

ConclusionsULX bubbles indicate mechanical power ~ 1E39 - 1E40 erg/s ~ LxULX bubbles indicate mechanical power ~ 1E39 - 1E40 erg/s ~ Lx

t ~ 1E6 yrs ; Etot ~ 1E53 ergt ~ 1E6 yrs ; Etot ~ 1E53 erg

(Beware of fake jets/shocks)(Beware of fake jets/shocks)

S26 in NGC 7793: super-SS433/W50 system with hot spots (-S26 in NGC 7793: super-SS433/W50 system with hot spots (->jets)>jets)

Largest and most powerful microquasar system (160 x 290 pc)Largest and most powerful microquasar system (160 x 290 pc) Linear size ~ 2.5 x SS433Linear size ~ 2.5 x SS433 Radio luminosity ~ 3 x Cas ARadio luminosity ~ 3 x Cas A Jet power ~ a few E 40 erg/s (>> Ledd of accr. BH.)

Much of the jet power used to inflate fully radiative bubble,Much of the jet power used to inflate fully radiative bubble,(L(Lrad = 27/77 L = 27/77 LJet); only ~ 1% goes into synchrot-emitting ); only ~ 1% goes into synchrot-emitting

electrons electrons

Rare example of kinetically-dominated high state BH in the Rare example of kinetically-dominated high state BH in the local universe; local universe; analogy with recently discovered/advocated (Punsly 2007, 08, 11) analogy with recently discovered/advocated (Punsly 2007, 08, 11) sample of kinetically dominated quasars ? sample of kinetically dominated quasars ?

Thank you