Jets from quiescent stellar Jets from quiescent stellar black holesblack holes

Elena GalloElena GalloUCSBUCSB

Black hole X-ray binary jetsHard X-ray state:

- Persistent radio emission with flat radio-mm spectrum

- Partially self-absorbed

synchrotron from conical outflow (Blandford & Königl‘79; Hjellming & Johnston‘88; Kaiser‘06)

- Jet interpretation confirmed by VLBI in Cyg X-1 & GRS 1915+105 (1e-2 LEdd)

Cyg X-1Stirling et al.‘01

GRS 1915+105Dhawan et al.’01Fuchs et al.’03

Radio/X-ray correlation in hard state

Corbel et al. ‘03; Gallo, Fender & Pooley ‘03

radio flux density - scaled to 1 kpc (mJy)

X-ray flux density - scaled to 1 kpc (Crab)

V 404 Cyg GX339-4J1118+4804U 1543-47GS 1354-641E 1740.9J1550-564Cygnus X-1J0422+32GRS 1758-258

LradioLx0.70.1

Radio/X-ray correlation in quiescence

Simultaneous VLA/Chandra observations of A0620-00 (10 MSun BH at 10-8.5 LEdd)

F8.5GHz = 51 ± 7 mJy

Lowest radio luminosity measured for X-ray binary

Interpreted as synchrotron emission from a persistent outflow

Gallo et al. ‘06

Radio/X-ray correlation in quiescence

A0620-00

Lx=7x1030 erg/sec

Lradio=7x1026 erg/sec

Non-linear radio/X-ray correlation holds down to 10-8.5 LEdd

Quenched radio emission above 10-2 LEdd

Gallo et al. ‘06

Jet power via jet/ISM interaction

Jet-powered radio nebula around Cygnus X-1

Gallo et al. ‘05, Nature

Jet power via jet/ISM interaction

Kaiser & Alexander ’97

104< Tbow< 2x106

Jet/ISM in pressure balance

constant Pjet

Pjet > 0.2 x 1037 erg /sec= 0.2 LX,bol

Jet power via jet/ISM interaction

Follow-up optical (ING) observations confirm the shock-compressed nature of the gas in the arc

Refinement of shock velocity trough optical lines ratios gives: Pjet ~ 0.5 LX,bol

Russell, Fender & Gallo in prep.

Cyg X-1

A0620-00

Jet power in quiescence

Jets in quiescence A look with Spitzer

Hard/quiescent state jets: optically thick-to-thin break in the mid-IR, thus Spizter IRAC/MIPS

Muno & Mauerhan claim evidence for excess mid IR emission due to circumbinary material in 4 quiescent X-ray binaries

Muno & Mauerhan ‘06

Jets in quiescence A look with Spitzer

Gallo et al., in preparation

Re-analysis of the MIPS data gives higher values/lower limits

Jet interpretation for the mid-IR excess as likely (yet strictly simultaneous data required)

Confirms prediction of jet spectral break near K band (Russell et al’06)

Jet power in quiescence

A0620-00

Lacc = 6x1035 y (/0.1) erg/sec

Pjet = 4x1035 erg/sec

(derived from Lradio following Heinz & Grimm 2004)

If Pjet comparable to Lacc

then the jet must affect the dynamics of the accretion flow

pure ADAF solutions thus ruled out

Future work: quiescent super-massive black holes

Large Chandra proposal (~450 ksec; PI: Treu) approved to observe 86 spheroidals in the Virgo cluster, covering the entire HST/ACS VCS (Cote’ et al.)

Look for highly sub-Eddington accretion-powered nuclear emission (5.3 ksec/target with ACIS-S: sensitive down to Eddington for a neutron star)

Plus: Spitzer (awarded) and possibly Keck and VLA

Aim: to bridge the gap between inactive galaxies and AGN in a neat nearby sample