Supernova Remnants and ULX bubbles

Supernova Remnants and ULX bubbles

Manfred Pakull,

Fabien Grisé, C. Motch, R. Soria

0bservatoire Astronomique de Strasbourg

OutlineOutline

-- Ultraluminous X-ray sources (ULXs)

-- ULXs are (often) located in bubbles = ULXBs

-- many (large) SNRs are really ULXBs

-- Rosetta Stone S26 in NGC 7793

-- ULXBs = jet inflated « beambags » like SS433/W50

Ultraluminous X-Ray sources 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 )‘superEddington’ sources 1 ULX per 3 star-forming galaxies

(Cropper et al 2004)

XMM/ EPIC view of NGC 4559XMM/ EPIC view of NGC 4559

Cropper et al 2004, MNRAS; Soria et al 2004, MNRAS

XMM Optical Monitor image(near-UV band)

2 2 ULXs in NGC 4559ULXs in NGC 4559 (Sc, (Sc, d = 10 d = 10 Mpc)Mpc)

X-7

(Cropper et al 2004)

XMM/ EPIC view of NGC 4559XMM/ EPIC view of NGC 4559

Ultraluminous X-ray SourcesUltraluminous X-ray Sources suggested naturesuggested 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 = 0.1Z) 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-1ULX 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 ?• Detection of supersonic

expansion (see later) from Laurent Mirioni’s thesis

CFHT, H

ULX IC 342 X-1ULX 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 ?• Detection of supersonic

expansion (see later) CFHT; from Laurent Mirioni’s thesis

ULX NGC 1313 X-2 Lx ~ 1039-40 erg/s variable

location far away (9kpc)from nucleus of 4.7 Mpc distant spiral NGC 1313SNR-like optical spectrum(e.g. Grise et al. 2008)

bubble diameter ~ 26’’ = 400 pc (!)

vexp.~ vshock ~ 100 km/s

H VLT

*

VLT, FORS

: HeII 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: N5204, N5585, N6946, M81, M101; N2403

Blair & Long 1997: N300, N7793

H

[SII]

[SII]-H

some very large SNR candidates…

Lozinskaya & Moiseev 2007

Log - logD for SNR

S1-N5585

10 100 300 pc

IC 10: Bubble around XRBWR + 30 Mo BH (LM2007)

NGC 5585 S1: new ULX (Pakull et al 2008)

very large ‘SNR’ in NGC 5585very large ‘SNR’ in NGC 5585

Matonick & Fesen (1997) noted huge (200x300) pc ‘SNR’ in NGC 5585

5.0

300 pc

very large ‘SNR’ very large ‘SNR’ ULXB ! ULXB !

5.0

Matonick & Fesen (1997) noted huge (200x300) pc ‘SNR’ in NGC 5585

300 pc

Chandra: point source (~ 5 1039 erg/s)as in many previously identified ‘SNRs’Ho IX, NGC 6946X-1; M81X-6 …

The ‘SNR’ MH9-11 in HolmbergIXThe ‘SNR’ MH9-11 in HolmbergIX

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 (?)

SE

Subaru

Ha [OIII] BB30 "

=

500 pc

Kinematics of ULX bubblesKinematics of ULX bubbles

Holm IX NGC1313 X-2

IC 342 X-1 Holm II

H

[NII] 6584

Vexp = 80 – 250

km/s

Energetics of ULX Bubbles 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 :

E0 ~ 2 1052 erg R1003 v100

2 n

t ~ 1 106 yrs, E0 ~ 5 1053 erg n “Hypernova” (GRB) Remnant

(shock H luminosity: I~ vexp2.3 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

ULX

(Swartz, Soria, in prep)

30 pc

HST/ACS NGC 6946 MF16 NGC 6946 MF16 no HNR !no HNR !

- brightest ‘SNR’ (1039 erg/s)

- ‘colliding SNRs’ (Blair & Fesen 94, BF & Schlegel 01)

- X-ray variable ULX (Roberts & Colbert 03)

- vex=225 km/s; t ~3 104 yrs; (Dunne et al. 00)

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 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 :

E0 ~ 2 1052 erg R1003 v100

2 n

t ~ 1 106 yrs, E0 ~ 5 1053 erg n

(shock H luminosity: I~ vexp2.3 n --> n = 0.1-1.0 cm-3)

• if wind/jet driven bubble (Castor 1975, Weaver et al 1977):

Lw ~ 5 1039 erg/s R1002 v100

3 n

t ~ 1 106 yrs (3 104 for NGC6946X-1); Lw ~ 1040 erg/s for all ULXB

Lw = ½ Mdot vout2 ~ jet mechanical luminosity of SS433;

i.e. vout should be mildly relativistic (~ 0.3 c)

.

QSO SS433 & W50

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

radio-image200 pc

ASCA image(Kotani 98)

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

ss433film

VLBA; credit: NRAO/AUI/NSF

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

some very large SNR candidates…

NGC 7793 S26

Log - logD for SNR

S1-N5585

10 100 300 pc

NGC 7793-S26: discovery of an extra-NGC 7793-S26: discovery of an extra-galactic SS433/W50-type systemgalactic SS433/W50-type system

• very large optical ‘SNR’ S26 in NGC7793 dist=3.4 Mpc, dia~250pc; [SII]/Ha~0.5 . Blair & Long 1997• radio source (> CasA; Pannuti et al 02)

X-ray Chandra (archive) H

13’’ 250pc

from Chandra archive:S26 is coincident with linear X-ray triple

S26 Chandra

0.3-1.0 keV1.0-2.0 keV2.0-8.0 keV

H contours

Lx ~ 1037 erg/s soft hot spot

Lx ~ 1037 erg/shard source= 23mag OB star

What have we learned/open questions

ULXs blow very energetic bubbles (ULXB)

ULXB resemble large SNRs but they aren’t

synchrotron/thermal bubble NGC7793-S26 is jet-

inflated

(SS433 and S26 do show Pmech >> Lx; both are not

ULX)

connection QSO and ULX ? jet interaction with ISM

all large SNR candidates are ULXBs (incl. inactive ULX) Merci !