Non-nuclear non-x ls

Transcription

1 ULX: Photon/mechanical luminosities Non-nuclear non-x ls Manfred W. Pakull, Observatoire de Strasbourg coll. Roberto Soria, Christian Motch, and others Manfred W. Pakull, Obs. de Strasbourg coll. R. Soria, C. Motch, Fabien Grisé & others S26 in NGC 7793 Bamberg, June 18-22, 2012 Leiden, April 3, 2014

2 Non-nuclear non-x ls NGC 1313 X-2 Manfred W. Pakull Observatoire de Strasbourg coll.: R. Soria, C. Motch, F. Grisé & others Leiden, April 2, 2014

3 Outline We can learn a lot about a phenomenon at wavelengths other 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

4 ULX bubble IC 342 X-1 CFHT, H Laurent Mirioni & Pakull 2002 W. H.T., Integral Field spectrograph, H T. Roberts et al Tooth nebula; diameter 220 pc! SNR-like spectrum

5 ULXB NGC 1313 X-2 * bubble diameter ~ 26 = 400 pc (!); SNR like spectrum! H VLT Pakull & Mirioni 02, 03; Grisé et al. 08

6 The SNR around HolmbergIX X-1 Subaru Ha [OIII] B 30 " = 500 pc SE Holmberg IX X-1 = M81 X-9: Lx ~10 40 erg/s; Grisé et al 2011 Miller (1995): X-ray superluminous SNR; but X-ray variable point source! see also Abolmasov & Moiseev 2008

7 Holmberg II ULX an X-ray ionized nebula

8 Holmberg II ULX an X-ray ionized nebula Broad (5 ) spectroscopic slit

9 Holmberg II ULX an X-ray ionized nebula; HeIIl4686 emiss.)

10 Holmberg II ULX an X-ray ionized nebula; HeIIl4686 emiss.)

11 Pakull & Mirioni 2002 NGC1313-X2 a rapidly expanding nebula Ramsey et al 2006 E W l Size ~ 570 x 400 pc Vex ~ 100 km/s highly supersonic expansion!

12 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,

13 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

14 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

15 M33 X-7 cont -like 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: L(4686)/L(0.3-10) = 2E 35 / 1E 38 ~ LMC X-1: L(4686)/L(0.3-10) 2 E35/2 E38 ~ 0.001, Pakull&Angebault 1986

16 Holmberg II X-1 Ha HeII [OI] Pakull & Mirioni 2002; Mirioni 2003 thesis; CFHT broad-slit L 4686 = erg/s HST ACS; Kaaret et al 2004 L(4686)/L(0.3-10) ~ Using Cloudy, one derives an integrated X-ray luminosity Lx ~ erg/s No strong beaming here!!

17 [OIV] l25.9 emission in Holmberg II X-1 Spitzer observations: Berghea et al note: IP (O++) ~ IP(He+) ~ 54 ev Extensive Cloudy modeling: Lx = 1.2E40 erg/s

18 Interesting: an XRB in an IS cloud (n >10 cm-3) creates 1 HeII l4686 photon per 1 X-ray photon L 4686 /hn 4868 ~ Lx (0.5-10keV) /2 kev ( poor man s X-ray telescope)

19 Ionization by shocks

20 A few elements of shock physics (A) Adiabatic, non-radiative shock ( no B field) n 1 = 4 n 0 ; v 1 = 3/4 v s ; T 1 ~ 10 5 K v (I) Isothermal, fully radiative shock (no B field) n 2 = M 2 n 0 ; v 2 = v s ; T 2 =T 0 Dopita & Sutherland 95 v s = 400 km/s precursor Cooling & recombination [0I] 6300 high- and low-ionization lines different Te e.g., Te[OIII] ~ kk Te[OI] ~ 8 kk broad emission lines Dv ~ v s

21 Shock diagnostics /b 100 [OIII]l5007/Hb Hb.3 1 [OI]l6300/Hb [OIII]l5007/Hb ratio as function of shock vel. v s (Dopita et al 1984) uncomlete radiative shock (see Raymond et al 1988) log distance from shock

22 radiative shocks For fully radiative shocks dissipated energy (shock luminosity per surface element [erg/cm2/s]) is l = ½ r v s3, spherical shock L = l4p R 2 = 2p r R 2 v s 3 and a certain fraction is radiated as H recombination radiation, i.e., lb (~0.003 x l) lb = 7.4x10-6 v s 2.4 n 0 erg/cm 2 /s Dopita et al 96, Allen et al precursor emission (photoionized by X-ray/EUV emission from shock) observable spectrum depends on v s ; age (completeness)

23 Radiative shock Structure and Energetics of ULX Bubbles Wind/jet driven bubble with power L w and radiative outer shock (Weaver et al 1977) l self similar solution for hydrodynamics; p = (g-1) e Rs = (125/154p) 1/5 (L w /r) 1/5 t 3/5 ; v s = 3/5 R s /t; g = 5/3 = (125/224p) 1/5 ; = 4/3 L rad = 27/77 L w = 0.35 L w for g = 5/3 = 27/112 L w = 0.24 L w = 4/3 Lw ~ 500* Lb for v s ~ km/s

24 Energetics of ULX Bubbles Bubble radii R ~200 pc (i.e. >> SNR) Expansion velocity vs ~ km/s IS densities n ~ cm -3 Age : t ~ 10 6 yrs; Power Lw ~ erg/s ~ Lx (ULX) Total energy: E o ~ erg/s (several 100 SNe!!) With Mdot x t = m Msol; m limited to a few; ( Lw = 1/2 x Mdot x v w 2 ) v w = 0.19 c (L 39 t 6 m 1 ) 0.5 (mildly) relativistic

25 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

26 some very large SNR candidates Log - logd for SNR Lozinskaya & Moiseev 2007 IC 10: Bubble around XRB ( 2007 WR + 30 Mo BH (LM S1-N5585 NGC 5585 S1: new ULX ( 2008 (Pakull & Grisé pc

27 very large SNR ULX bubble 300 pc Matonick & Fesen 1997 noted huge (200x300) pc SNR in NGC Later, R. Soria detected Chandra point source (Lx~ cgs); -> another case of a previously identified SNR : Ho IX, N6946X-1; M81X-6, First case of an optically predicted/selected ULX

28 NGC1313: another huge ULX bubble? NGC1313 Ha VLT 125x225 pc X-2 ~10 40 erg/s Lx < erg/s Vexp = v s = 180 km/s -> Energetic bubble L w / Eo ~ /10 53 cgs presently inactive ULX? H [SII]

29 Arp 227 Ngc 470/ NGC 474 NGC 470 CFHT calendar

30 HLX in NGC 470 (d=38 Mpc) Sutton, Roberts et al 2012: most extreme ULXs XMM/Chandra Lx ~ 2-10 E40 erg/s HII #46 HeII l4686 [NII] l5200 [OI ] ll6300,60 ESO VLT VM test observations 2011: easy : 1 ksec integration time

31 HLX in NGC 470 (d=38 Mpc) F4686 ~ cgs L4686 = erg/s ~ 4 x Holm II Mv = like HLX1 HII #46 HeII l4686 [NII] l5200 [OI ]ll 6300, 60 Emission of NGC 470 HLX photoionizes; isotropic! i.e. not beamed

32 some large SNR candidates Log - logd for SNR Lozinskaya & Moiseev 2007 S1-N pc

33 SNR S26 in NGC 7793 (d=3.9 Mpc) H R 300 pc S26: Blair & Long 1997; faint ROSAT source: Read & Pietsch 1999

34 SNR S26 in NGC 7793 = triple XRS X-ray Chandra archive; 50 ks; PI: Pannuti, Pakull & Grisé, 2007

35 L x ~ 5E36 erg/s kt ~ kev L x ~ 7E36 erg/s L x ~ 1.1E37 erg/s kt ~ kev Mx ~ few 100 Mo ~ 1.5 Pakull, Soria & Motch, 2010 Nature

36 + 9 GHz radio contours = 0.7; opt. thin syn. S26: X-ray/ radio image X-ray Hot Spots lead radio HS

37 Using formalism for ULX bubbles:

38 S26 and FR II radio galaxies similar morphologies 1 : 1000 O X-ray sources ATCA 9 GHz Soria et al MNRAS

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40 S26 long slit along major axis incl. central star & hot spots ESO VLT 2011 H [NII]l6584 HS North (blueshifted) *cont + *H em 2 x 360 km/s HS South (redshifted)

41 S26 long-slit; short axis incl central star ESO VLT 2011 V ex = v s =240 km/s *H cont 23mag * *HeI l6678 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!)

42 radio-image SS433 = ULX? (see Fabrika 2006) mechanically inflated Bubble W50 (SNR??) with ears due to v = 0.26c jets 200 pc L mech = L J ~ erg/s ASCA image ( 1998 (Kotani Begelman s beambags SS433 seen from far away: triple source! Like S26

43 ULXs, SS433, jets, bubbles VLBA; credit: NRAO/ AUI/NSF Proposed discussion SS433, S26 = edge-on ULXs? Hol II: Cseh et al 2014 S26: Pakull et al M83 MQ1 Soria et al 2014

44 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

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46 ULX bubbles: hypernova remnants? SNR see also: Abolmasov, Fabrika 2007 Abolmasov 2008, 2010 Abolmasov, Moiseeiv 2007, 2008 bubble Vexp ~ (L w /n) 1/3 R-2/3 bubble (E o /n) 1/2 R-3/2 SNR Abolmasov 2008 no HNR, wind/jet inflated!