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
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ULX: Photon/mechanical Non-nuclear sources @ non … · ULX: Photon/mechanical luminosities Manfred W. Pakull, Observatoire de Strasbourg coll. Roberto Soria, Christian Motch, and
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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
Holmberg II ULX an X-ray ionized nebula
Holmberg II ULX an X-ray ionized nebula
Broad (5 ’’) spectroscopic slit
Holmberg II ULX an X-ray ionized nebula; HeIIl4686 emiss.)
Holmberg II ULX an X-ray ionized nebula; HeIIl4686 emiss.)
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
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