jets from quiescent stellar black holes elena gallo ucsb n.
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Jets from quiescent stellar black holes Elena Gallo UCSB. Black hole X-ray binary jets. Hard 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 )

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black hole x ray binary jets
Black hole X-ray binary jets

Hard 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)

GRS 1915+105

Dhawan et al.’01

Fuchs et al.’03

Cyg X-1

Stirling et al.‘01

radio x ray correlation in hard state
Radio/X-ray correlation in hard state

V 404 Cyg

GX339-4

J1118+480

4U 1543-47

GS 1354-64

1E 1740.9

J1550-564

Cygnus X-1

J0422+32

GRS 1758-258

radio flux density - scaled to 1 kpc (mJy)

LradioLx0.70.1

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

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

radio x ray correlation in quiescence
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 quiescence1
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 power via jet/ISM interaction

Jet-powered radio nebula around Cygnus X-1

Gallo et al. ‘05, Nature

jet power via jet ism interaction1
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 interaction2
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.

jets in quiescence a look with spitzer
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 spitzer1
Jets in quiescence A look with Spitzer

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)

Gallo et al., in preparation

jet power in quiescence1
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
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