JETS FROM MICROQUASARS Elena Gallo University of Michigan

JETS FROM MICROQUASARS Elena Gallo University of Michigan HEPRO III, Barcelona, June 28, 2011

OUTLINE X-RAY STATES & RADIO JETS (BLACK HOLES) Radio phenomenology vs accretion modes LUMINOSITY CORRELATIONS (BLACK HOLES) radio/X-ray NIR/X-ray dependence on X-ray binary parameters (lack thereof) Update: clustering algorithms, Bayesian analysis, linear regression BLACK HOLES VS NEUTRON STARS radio luminosity, bulk velocity BLACK HOLE SPIN & JET POWER

Broadband Energy Spectrum cf. Sera Markoff

Jets’ phenomenology Cyg X-1 Stirling et al. ‘ 01 GRS 1915+105 Mirabel et al. ‘ 94 SS 433 Blundell et al. 2004 1 E 140. 7 -2942 Mirabel et al. al ‘ 99

X-ray states: low/hard & quiescent (hard) Mc. Clintock & Remillard 2006 Radiatively inefficient inflow (ADAF, CDAF, JDAF, ADIOS. . ) Meyer, Liu & Meyer-Hofmeister 2006

X-ray states: low/hard & quiescent (hard) Mc. Clintock & Remillard 2006 Radiatively inefficient inflow (ADAF, CDAF, JDAF, ADIOS. . ) Meyer, Liu & Meyer-Hofmeister 2006 Cyg X-1 Stirling et al. ‘ 01

X-ray states: high/soft (thermal dominat)� Mc. Clintock & Remillard 2006 Radiatively efficient inflow (thin disc) Meyer, Liu & Meyer-Hofmeister 2006

X-ray states: high/soft (thermal dominat)� Mc. Clintock & Remillard 2006 Radiatively efficient inflow (thin disc) SUPPRESSED Meyer, Liu & Meyer-Hofmeister 2006

X-ray states: hard to Mc. Clintock soft transition� & Remillard 2006 JETS DURING HARD-TO-SOFT TRANSITIONS Meyer, Liu & Meyer-Hofmeister 2006 GRS 1915+105 Mirabel et al 1994

Black hole outburst: a journey Fender Belloni Gallo 2004; Fender Homan Belloni 2009

Corbel et al. 2003 4 U 1755 -33 Angelini et al. 2003 X-ray jets Corbel et al. 2005

Jet-powered nebulae Cyg X-1, WRST Gallo et al. 2005 Cygnus X-1, Isaac Newton Russell et al. 2006 SS 433 W 50, VLA, Dubner et al. 1998

Luminosity correlations I. X-ray/radio Corbel et al 2003, Gallo 2007

Luminosity correlations II. NIR/radio Russell et al 2006

(No) Orbital parameters dependence Roche lobe radius Orbital period Soleri & Fender 2010

(Weak) Inclination dependence (NIR/X-ray) Soleri & Fender 2010

2 Tracks & Accretion mode transition ? Coriat et al. 2011

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach Gallo et al. in prep.

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach Gallo et al. in prep.

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach Gallo et al. in prep.

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach Gallo et al. in prep.

Black Holes vs Neutron Stars I. • Black points: BHs • Red points: NS atoll sources • Blue points: NS Z sources after Migliari & Fender 2006

Black Holes vs Neutron Stars II. Fender et al 2004

Measuring BH spin I. Relativistic lines Cyg X-1 Stirling et al. ‘ 01 obs/ em Fabian et al 2000 GRS 1915+105 Mirabel et al. ‘ 94 SS 433 Blundell et al. 2004 1 E 140. 7 -2942 Mirabel et al. al ‘ 99

Measuring BH spin I. Relativistic lines Cyg X-1 Stirling et al. ‘ 01 Cf. Miller, Fabian, Cackett, Miniutti, Reis, Reynolds et al.

Measuring BH spin II: Thermal state continuum fitting H 1743 -322 (Kubota et al 2004) RISCO a* Cyg X-1 Stirling et al. ‘ 01 . . after color correction (cf. S. Davis) Teff 4 cf. Mc. Clintock, Shafee, Narayan, Steiner, Gou, Liu, Done, Gierlinski, Middleton

Constraints on spin powering of jets Fender Gallo Russell 2010

Fender Gallo Russell 2010

Hard state: Steady jets Reflection Disk No apparent jet/spin correlation Fender Gallo Russell 2010

State transitions: Transient jets Reflection Disk No apparent jet/spin correlation Fender Gallo Russell 2010

SUMMARY X-RAY STATES & RADIO JETS (BLACK HOLES) Phenomenology – well understood. LUMINOSITY CORRELATIONS (BLACK HOLES) No dependence on X-ray binary orbital parameters, nor outburst properties. Very weak dependence on jet axis. Statistically significant evidence for 2 separate clusters in the radio/X-ray domain. Universal correlation. . no longer such. BLACK HOLES VS NEUTRON STARS NSs factor ~30 fainter in radio However: the most relativistic jet source in the Galaxy is a neutron star BLACK HOLE SPIN & JET POWER No apparent relation: IF the measurements are robust (. . ) => Jets are not powered by BH rotational energy