Supernova Remnants and ULX bubbles Manfred Pakull Fabien

Supernova Remnants and ULX bubbles Manfred Pakull, Fabien Grisé, C. Motch, R. Soria 0 bservatoire Astronomique de Strasbourg

Outline -- Ultraluminous X-ray sources (ULXs) -- ULXs are (often) located in bubbles = ULXBs -- many (large) SNRs are really ULXBs -- Rosetta Stone S 26 in NGC 7793 -- ULXBs = jet inflated « beambags » like SS 433/W 50

Ultraluminous X-Ray sources • Bright (variable) non-nuclear X-ray sources in galaxies (Long & van Speybroeck (1983) i. e Lx ~ few 1040 erg/s: more luminous in X than Local Group of Galaxies!! • Isotropic luminosities > 1039. 5 erg/s i. e. Lx > Ledd (= 1. 3 1038 erg/s M/M ) for stellar-mass accretors ( M < 20 M ) ‘super. Eddington’ sources 1 ULX per 3 star-forming galaxies

XMM/ EPIC view of NGC 4559 (Cropper et al 2004)

2 ULXs in NGC 4559 (Sc, d = 10 Mpc) XMM Optical Monitor image (near-UV band) X-7 Cropper et al 2004, MNRAS; Soria et al 2004, MNRAS

XMM/ EPIC view of NGC 4559 (Cropper et al 2004)

Ultraluminous X-ray Sources suggested nature • • • SNe/very young SNR, but most are variable ! truly super-Eddington (Begelman 2002) beamed into our l. o. s. (King 2002, Markoff 2002) stellar pop III remnants (Madau & Rees 2001) low-metallicity (Z = 0. 1 Z ) binaries (Pakull & Mirioni 02) intermediate mass black holes, IMBH; in between the stellar and AGN variety • We need information from other wavelengths !! optical work: Pakull& Mirioni&Grisé, Roberts & Co; Abolmasov & Fabrika. . .

A few examples of our optical follow -up observatuions of ULXs

ULX IC 342 X-1 • "Tooth" nebula situated in spiral arm has a diameter of 220 pc (Pakull & Mirioni 2002; Roberts et al. 2003; Grisé et al 2006) CFHT, H from Laurent Mirioni’s thesis • SNR-like spectrum: [SII]/H =1. 2 [OI] 6300/H =0. 4 • X-ray or shock ionization ? • Detection of supersonic expansion (see later)

ULX IC 342 X-1 • "Tooth" nebula situated in spiral arm has a diameter of 220 pc 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 ? • Detection of supersonic CFHT; from Laurent Mirioni’s thesis expansion (see later)

ULX NGC 1313 X-2 Lx ~ 1039 -40 erg/s variable * H VLT, FORS * location far away (9 kpc) from nucleus of 4. 7 Mpc distant spiral NGC 1313 SNR-like optical spectrum (e. g. Grise et al. 2008) bubble diameter ~ 26’’ = 400 pc (!) vexp. ~ vshock ~ 100 km/s : He. II 4686 emission

Are there unrecognized ULXB (incl. from presently inactive, or from ULXs possibly beamed away from us) among large SNRs candidates ?

Optical [SII]/H > 0. 4 selected surveys of SNRs in large nearby galaxies (outside LG) Matonick & Fesen 1997: N 2403 Blair & Long 1997: N 5204, N 5585, N 6946, M 81, M 101; N 300, N 7793 Ha [SII]-H

some very large SNR candidates… Log S - log. D for SNR Lozinskaya & Moiseev 2007 IC 10: Bubble around XRB WR + 30 Mo BH (LM 2007) S 1 -N 5585 100 300 pc NGC 5585 S 1: new ULX (Pakull et al 2008)

very large ‘SNR’ in NGC 5585 300 pc 5. 0 Matonick & Fesen (1997) noted huge (200 x 300) pc ‘SNR’ in NGC 5585

very large ‘SNR’ ULXB ! 300 pc 5. 0 Matonick & Fesen (1997) noted huge (200 x 300) pc ‘SNR’ in NGC 5585 Chandra: point source (~ 5 1039 erg/s) as in many previously identified ‘SNRs’ Ho IX, NGC 6946 X-1; M 81 X-6 …

The ‘SNR’ MH 9 -11 in Holmberg. IX Subaru Ha [OIII] B 30 " = 500 pc SE Holmberg IX X-1: Lx ~1040 erg/s Miller (1995): X-ray superluminous SNR; but X-ray variable point source! Note small cluster incl. ULX counterpart; SE: shock breakout (? )

Kinematics of ULX bubbles Holm IX NGC 1313 X-2 H [NII] 6584 IC 342 X-1 Vexp = 80 – 250 km/s Holm II

Energetics of ULX Bubbles • Typical bubble radii ~200 pc (ie. >> SNR) • Expansion velocity ~ 80 km/s (up to 250 km/s) • if due to SN explosion; Sedov /snowplow : E 0 ~ 2 1052 erg R 1003 v 1002 n t ~ 1 106 yrs, E 0 ~ 5 1053 erg n “Hypernova” (GRB) Remnant (shock H luminosity: Ia~ vexp 2. 3 n --> n = 0. 1 -1. 0 cm-3) - Explosion of several (>20) SNe (superbubble) excluded (no massive cluster !) - Hypernova remnants (very popular 10 years ago) excluded

NGC 6946 MF 16 no HNR ! HST/ACS - brightest ‘SNR’ (1039 erg/s) - ‘colliding SNRs’ (Blair & Fesen 94, BF & Schlegel 01) ULX 30 pc - X-ray variable ULX (Roberts & Colbert 03) - vex=225 km/s; t ~3 104 yrs; (Dunne et al. 00) (Swartz, Soria, in prep) The youth of the bubble excludes nature as a remnant of SN explosion that created compact accreting star in ULX [after SN explosion nuclear timescale expansion of donor star before Roche lobe overflow mass transfer can take place]

Energetics of ULX Bubbles • Bubble radii up to ~200 pc (ie. >> SNR) • Expansion velocity ~ 80 km/s (up to 250 km/s) • if due to SN explosion; Sedov /snowplow : E 0 ~ 2 1052 erg R 1003 v 1002 n t ~ 1 106 yrs, E 0 ~ 5 1053 erg n (shock H luminosity: Ia~ vexp 2. 3 n --> n = 0. 1 -1. 0 cm-3) • if wind/jet driven bubble (Castor 1975, Weaver et al 1977): Lw ~ 5 1039 erg/s R 1002 v 1003 n t ~ 1 106 yrs (3 104 for NGC 6946 X-1); Lw ~ 1040 erg/s for all ULXB . Lw = ½ Mdot vout 2 ~ jet mechanical luminosity of SS 433; i. e. vout should be mildly relativistic (~ 0. 3 c)

m. QSO SS 433 & W 50 mechanically inflated Bubble W 50 with ‘ears’ due to v=0. 26 c jets (+SNR ? ) 200 pc radio-image ASCA image (Kotani 98) Begelman’s ‘beambags’ i. e. linear triple

ss 433 film VLBA; credit: NRAO/AUI/NSF

Problem: no large-scale jets seen in ULXB (or other m. QSO)

some very large SNR candidates… Log S - log. D for SNR NGC 7793 S 26 S 1 -N 5585 100 300 pc

NGC 7793 -S 26: discovery of an extragalactic SS 433/W 50 -type system 13’’ 250 pc H X-ray Chandra (archive) • very large optical ‘SNR’ S 26 in NGC 7793 dist=3. 4 Mpc, dia~250 pc; [SII]/Ha~0. 5 Blair & Long 1997 • radio source (> Cas. A; Pannuti et al 02) from Chandra archive: S 26 is coincident with linear X-ray triple.

H contours S 26 Chandra Lx ~ 1037 erg/s hard source = 23 mag OB star 0. 3 -1. 0 ke. V 1. 0 -2. 0 ke. V 2. 0 -8. 0 ke. V Lx ~ 1037 erg/s soft hot spot

What have we learned/open questions ü ULXs blow very energetic bubbles (ULXB) ü ULXB resemble large SNRs but they aren’t ü synchrotron/thermal bubble NGC 7793 -S 26 is jet-inflated ü (SS 433 and S 26 do show Pmech >> Lx; both are not ULX) ü connection m. QSO and ULX ? jet interaction with ISM ü all large SNR candidates are ULXBs (incl. inactive ULX) Merci !