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Supernova Remnants and ULX bubbles. Manfred Pakull, Fabien Grisé, C. Motch, R. Soria 0bservatoire Astronomique de Strasbourg. SNR & PWN in the Chandra Era, July 8-10 2009, Boston, MA. Outline. -- Ultraluminous X-ray sources (ULXs) -- ULXs are (often) located in bubbles = ULXBs - PowerPoint PPT Presentation
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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 !