ULXs @ non-X-ray wavelengths

Manfred Pakull

0bservatoire Astronomique de Strasbourg

coll: Roberto Soria, Christian Motch, Fabien Grisé

ULX and Middle Weight Black Holes, May 24-26, ESAC, Spain

OutlineOutline

-- Ultraluminous X-ray sources proper

-- ULXs and stellar environment

-- ULX feedback: photoionisation

-- ULX feedback: shocks; wind/jet inflated ULX bubbles

-- Rosetta Stone S26 in NGC 7793

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

NGC1313 X-2 (Thesis Grisé)

VLT/FORS1 : H,V,B HST/ACS : F814W,F555W, F435W

5“N

E

N

E10“

Color-magnitude diagrams of the stars around NGC 1313 X-2

Counterpart Mv ~ -4.5

(Grisé et al)

Cluster age:Ramsey et al 2006: > 10 Myrs E(B-V) = 0Liu et al 2007 < 10 Myrs = 0.33Grisé et al 2008 20 Myrs = 0.10

Optical Spectrum of X-2Pakull et al 2006

HeII λ4686

RV(4686) ~ 300 km/s, if disk emission -> no IMBH !

Photometry of N1313 X-2Photometry of N1313 X-2

Liu et al 2009:

Periodic (?) variation with P= 6 days

Not confirmed by ground-based photom(Grisé et al . 2009)

Holy grailHoly grail

Measure orbital period and radial velocity curve(s)of ULX (and companion)

Determine masses: stellar BHs or IMBH ?

We are close ! (c.f. C. Motch et al.; T. Roberts et al. this conf.)

Feedback Feedback I. X-ray photoionization I. X-ray photoionization

X-ray ionized nebula: XIN

Halpern & Grindlay 1980

Kallman&McCray1982

Different frm HII regions: no sharp Stroemgren spheres; ‘warm’ neutrals strong [OI] , [SII]‘warm’ He++ zone: HeII4686 emission‘Te ~104 K; line width < 20 km/s

Holmberg II ULX

2nd XIN after LMC X-1(Pakull & Angebault 1989)

nebular HeII 4686 emission at the position of the ULX (Pakull & Mirioni 2002)Zanstra He+ LyC photon counting

LHeII4686 LX nebula indeed “sees” LX ~ 1040 erg/s

-> no beaming here !

Foot nebula

Xray ionized nebula in Holmberg Xray ionized nebula in Holmberg IIII

From Laurent Mirioni’s thesis; nebula is density-bound (optically thin) beyond heel

Chandra position coincident withHe III regionHe III region

confirmed by Kaaret et al 04

[OIV] 25.9 emission in Holmberg II X-1

Spitzer observations: Berghea et al 2009 note: IP (O++) ~ IP(He+) ~ 54 eV

Orocz et al 2007:

70 Mo OB + 16 Mo BH in dense HII B208f: XIN

M33 X-7

Strasbourg students Maggi, Morgan and Master student Xian Hua:

Measure XUV (0.054 – ~0.1 KeV) emission of well-behaved BH X-ray binary using CLOUDY modeling; PL and TB wrong !

4686

NGC 5408NGC 5408

HeII 4686

Nebula: Pakull & Mirioni 2003

Spectra: Kaaret et al 2009: XIN!

4686: Nebular & STELLAR

H

FeedbackII. Shocks by wind/jets

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;

SNR-like spectrum:

[SII]/H=1.2[OI]6300/ H=0.4

• shock (or X-ray) ionization • Detection of supersonic

expansion (see later) Roberts et al 2003

INTEGRAL field spectrograph:Cont5000 H [OIII]-contours[OIII]-contours

ULXB NGC 1313 X-2

H VLT

*

bubble diameter ~ 26’’ = 400 pc (!)

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

ULX

(Swartz, Soria, in prep)

30 pc

HST/ACS

- brightest ‘SNR’ (1039 erg/s)

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

- X-ray variable ULX (Roberts & Colbert 03, poster Fengyun Rao !)

- 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]

NGC 6946 MF16 NGC 6946 MF16 no HNR !no HNR !

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 >> 20 km/s (T~104 K thermal v)

Energetics of ULX Bubbles Energetics of ULX Bubbles • Bubble radii up to ~200 pc (ie. >> SNR) • Expansion velocity ~ 80 – 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)

HNR nature of ULXB unlikely

• 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 yr for NGC6946X-1); Lw ~ 1039-40 erg/s for all

ULXB

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

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

Interstellar Bubble

Castor, McCray, Weaver 1975,Weaver et al. 1977

E_therm = 5/11 Lw t

E_kin = 15/77

Lw t

E_rad = 27/77 Lw t

E_i = 77/77 Lw t

(from Chu, 2009)

+ non-thermalparticles

107 - 108 K

Problem: strong winds or large-scale jets not readily seen in

ULXB

Estimate: >~ 25 % ULX blow bubbles

If ULX photon emission strongly beamed, than there should be many ULXB with ULXs that are

beamed away from us

Are there unrecognized ULXBfrom active, presently inactive, or

misaligned ULXs ?

Search for point-like XRS 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 (LM 2007)

NGC 5585 S1: new ULX (Pakull & Grisé 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’ is ULXB !very large ‘SNR’ is 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 …

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 readily seen in ULXB (or other

QSO)

…but non-thermal radio emission around some ULX

Hol II X-1 again

LR~ Cas Aextended emission i.e. not QSO-like

~ only 1% of PJ in SS433 is enough to power radio lobes(very small fractionof PJ go into relativistic electrons and B fields

Neal Miller, Mushotzky, Neff 2005

HeII 4686

some very large SNR candidates…

NGC 7793 S26

Log - logD for SNR

S1-N5585

10 100 300 pc

S26 = optical/Xray = P8

0.2-8 keV 0.2-1 keV

250pc

N7793: Chandra archive; 50 ks; PI: Pannuti

X + Ha

S26: Blair & Long 1997P8: Read and Pietsch 1999

0.3- 1 .0 keV1.0 - 2.0 keV2.0 – 8.0 keV

Pakull, Soria & Motch, Nature in pressPakull, Soria & Motch, Nature in pressHH contours from CTIO contours from CTIO

LLxx ~ 5E36 erg/s ~ 5E36 erg/s

LLxx ~ 7E36 erg/s ~ 7E36 erg/s

LLxx ~ 1.1E37 erg/s ~ 1.1E37 erg/s

~ 1.5~ 1.5

kT ~ 0.3-0.8 keVkT ~ 0.3-0.8 keV

kT ~ 0.3-0.8 keVkT ~ 0.3-0.8 keV

S26 and FR II radio galaxiesS26 and FR II radio galaxies

Soria et al 2009; 2010 submitted

ATCA 9.02 GHz

1000 : 1

compare with FRII CygA

Cyg A: Chandra high S/N NGC 7793 S26: Chandra 50ks

compare with FRII CygA

Cyg A: Chandra low S/N NGC7793-S26: Chandra 50ks

Radio galaxy basic modelRadio galaxy basic model

Heinz 2000, Thesis

AGN: hot T~107-8 K cluster gas weak cocoon shock

S26: warm 103-4 K ISM:strong cocoon shock

S26S26in in

HeIIHeII46864686

emissionemission-> ->

vvs ~ 275 ~ 275

km/s km/s

opt. counterpart ofcentral souce:Mv~-5 (WR) star

but finallybut finally ... ...

VVexp ~ V ~ Vs ~ 250 km/s ~ 250 km/s

ESO VLT Oct. 2009

S26/P8 summary S26/P8 summary Pakull, Soria & Motch 2010, Nature in pressPakull, Soria & Motch 2010, Nature in press

Morphology : FRII radio galaxy: radio and X-ray lobes, hot spots + optical lobes inflation of the lobes by a jet (power PJ)

Size: 300 x 150 pc, i.e. typical ULXBSupersonic expansion with 250 km/s (!); consistent with shock-excited 4686 emissionMV ~ -5 (WR) optical counterpart

Age = 2/5 R/v ~ 2 105 yrsE(rel. electrons) << E(thermal), E(kin)

PJ ~ 5 1040 erg/s (>> Lx ~ 2 1037 erg/s)

Similar to , but much more powerful than SS433/W50

Heinz 2002Heinz & Sunyaev, 2003

QSO and ULX

Thank you