SS 433 and other transients Zsolt Paragi JIVE

SS 433 and other transients Zsolt Paragi (JIVE) Presented at the Resolving The Sky conference, Manchester, 18 -20 April 2012

Outline • SS 433, an introduction • The radio jets on mas scales: compact jets and discrete ejecta • SS 433 and microquasars • Microquasars/SS 433 and AGN • Other microquasars, transients and Te. V sources with the ‘e-EVN’

SS 433: the first Galactic radio-jet system • Strong, H spectral lines (Stephenson, Sandaluek 1977) • Eclipsing binary, V 1343 Aql, mv=14 mg (Kholopov et al. 1981) • Related radio and X-ray sources • Spectral lines at unusual frequencies (Margon et al. 1979) • Doppler-shifted Balmer and He. I lines (Fabian, Rees 1979, Milgrom 1979) • “moving lines”, between -30000 and +50000 km/s, P~164 days (Margon 1979 b) RADIO • MERLIN: elongated structure on 1” scales (Spencer 1979) • ‘EVN’: compact VLBI structure, ~10 mas (Schilizzi et al. 1979) • VLA: precessing beams (Hjellming, Johnston 1981) A dozen of Nature papers in 1979 More than 2000 papers to date Hope to understand AGN

The binary stellar system: • O, B, or WR normal star, about 10 M or larger • Black hole or neutron star, Mcompact/M ~0, 25 (estimate) • 4 1012 cm (0, 27 AU) (Brinkmann, Kawai, Matsuok 1989) • 13. 081 day orbital period (Kemp et al. 1986) • d. M/dt = 10 -5 10 -4 M /yr (van den Heuvel 1981) • Lbol = 1039 1040 erg/s (e. g. Wagner 1986) • LX = 1036 erg/s (Kotani et al. 1996) • Lkin = 2 1039 erg/s (e. g. Watson et al. 1986) Hjellming, Johnston (1986)

Kinematic model parameters • inclination: i = 78, 83 0, 10 (Margon & Anderson 1989) • precession cone half opening angle: = 19, 85 0, 17 (Margon & Anderson 1989) • precession cone axis projected PA: = 100 2 (Hjellming & Johnston 1981): • sense of precession: s = 1 (Hjellming & Johnston 1981) • jet velocity: vjet = 0, 2602 0, 0013 c (Margon & Anderson 1989) • precession period P 164 = 162, 5 0, 03 day (Margon & Anderson 1989) • precession phase = 0. 0 at: t 164 = JD 2443588, 03 0, 3 (Vermeulen 1989) Hjellming, Johnston (1985)

Kinematic distance and Doppler beaming • Wb, Ef, Jb only! Mk. II/Mk. III • If v=0. 26, d=5. 0 0. 3 kpc ! • cf. HI d=3. 6 kpc Fejes (1986 a) • Unbeamed and beamed models; comparison with real data suggests beaming Is observed as expected Fejes (1986 b) István Fejes (1939 -2011)

EVN 10 -days monitoring at 5 GHz, 1987 D = 5 kpc 0, 001” = 5 AU • elongated radio core • discrete ejecta (bright flares ~400 days) • brightening zone Facts sheet (data: Ralph Spencer; RCV thesis) 1985 May, Mk. III mode E, 14 MHz LCP, EVN: Ef, Jb, On, Mc, Wb 14 1987 May/June, mode A, 56 MHz EVN+GBT 43 m; MERLIN Vermeulen et al. (1993) 1 -pass only 13 minutes Used whole EVN supply of tapes,

The compact inner jets • Optically thin ejecta • Flux ratio (core) @18 cm as expected (beaming) • Optically (partially) thick core jets: • Synchrotron self-absorption, similar to AGN cores (Blandford & Königl 1979) • In addition, anisotropic free-free absorption (cf. Stirling et al. 1997) • Optical depth (Lobanov et al. 1998): • Jet profile (cf. Hjellming and Johnston 1988) ne 1. 2× 106 cm-3 Paragi et al. 1999 VLBA

The equatorial outflow VLBA 22 GHz, 16 June 1998 * Global VLBI, 6 June 1998 Tb~108 K Various epochs/frequencies show evidence for: • free-free absorption at the base of the counterjet • ionized outflow, roughly perpendicular to the jets • radio emission from equatorial outflow detected • synchrotron/thermal origins proposed (cf. Blundell et al. 2001) • but note high Tb!

SS 433 radio polarization • Linear polarization is observed on ~100 mas – as scales (VLA, MERLIN), outside the inner depolarized zone (ionized gas in eq. outflow or in the jet) • B aligned with local velocity => continuous jet (Stirling et al. 2004) • B aligned with ballistic velocity => discrete ejecta (Miller-Jones et al. 2008) • Linear polarization not detected with VLBI yet (but Tudose et al. in prep. ) • Circular polarization is occasionally detected (ATCA; Fender et al. 2000) • Dedicated global VLBI experiment to look for CP origin: non-detection, but also WSRT data show no CP at that epoch (Paragi et al. 2004)

SS 433 with CHANDRA • Reheating of atomic nuclei in the extended X-ray jets • Evidence for very high Lorentz-factor inner flow? – as Fomalont et al. (2001) suggested for Sco X-1? ? ? • Extended emission in eq. flow as evidence for hot gas cannot be 100% confirmed, but may be real (Rob Fender, priv. comm. ) Migliari et al. (2002)

Galactic analogy of an alternative “AGN feedback” process? • Does SS 433 heat up ISM to 107 -8 K? • Mass loss in equatorial wind may reach or even exceed the transfer rate to the jets (King et al. 1999, Paragi 2000) • Ultrafast outflows observed in X-rays in 40% of a sample of 42 galaxies • Regulating BH grow as well as stripping gas from star-forming regions; would naturally explain MBH-Mbulge relation (Tombesi et al. 2012) XMM/NASA

BHXRB state transitions: X-ray HID SIMS High/Soft state discrete ejecta SS 433 as a microquasar • “compact jets” • quenched state • discrete ejecta • known distance, vjet, composition! But • BH or neutron star? • continuously in “soft state” • LX very low while LR high • X-rays from thermal jet Following e. g. Fender et al. (2004) jet suppressed Increasing Accretion rate, increasing Lx~Lr Compact jet line (? ) Low/Hard state

Flaring SS 433 • SS 433 likely has similar accretion state changes to other BHXRBs, but it is hidden from us in the X-rays • vjet is well known in SS 433 from optical lines, but also from VLBI-only measurements of transient ejecta (Vermeulen 1989) • but there may be a very high gamma inner flow (cf. “dark jet”, Miller-Jones et al. 2008) • tempting to interpret more and more assymetric core-jets at higher frequencies with increasing deeper in the jet But • low/high frequencies show discrete ejecta travel at the exact same speed, v=0. 26 c • this also seem to contradict the idea that during outburst in BHXRB there is an increase of , leading to the shocks Following up flaring microquasars with the “e-EVN” has became routine procedure with triggered e-VLBI observations. Tudose et al. (2010)

The Fundamental Plane of Black Hole Activity • Scaling between BHXRB in the hard state and AGN • Not all AGN classes fit • SS 433 is far brighter in radio than hard state BHXRB • Some LLAGN samples have very similar outliers (e. g. de Gasperin et al. 2011) • Why SS 433 is so special? ? ? Merloni et al. (2003); Falcke et al. (2003) Körding et al. (2006) etc.

SS 433 -W 50: a ULX plus radio nebula? 0. 5 deg. . Dubner et al. (1998) • SS 433 accretion disk X-ray emission is scattered along the jets • When viewed along the jets, SS 433 May be seen as a powerful ULX (Fabrika 2000) Supercritical accretion disc funnel: 1. 4 GHz VLA SS 433 Feng & Soria (2011) • A new example of BH powered ULX nebula is IC 342 X-1 (Cseh et al. 2012)

JIVE moments Richard with Queen's Commissioner in the Province of Drenthe, Relus ter Beek, official opening of the EVN correlator (1998) Farewell party @JIVE, 2002 December 17 EU Commissioner Janez Potocnik unleashes the power of e-VLBI, 2006

How we imagined e-EVN follow-up of high energy transients

A few examples…

Strongly decelerating jet in XTE J 1752 -223 • X-ray transient discovered by RXTE on 23 Oct. 2009; gradually evolved to soft state and produced radio flare • Initial EVN/e-VLBI observations on 11 Feb. 2010 one component (A) • VLBA follow-up showed proper motion with strong deceleration and a new component (B) that was initially thought to be the counter-jet. • EVN observations in March showed another ejected component (C) • After the source went back to the hard state two epochs VLBA observations detected the core in the system • Core apparently had high variability • After understanding source geometry, further analysed component B which showed high proper motion during the single experiment it was detected Yang et al. (2010, 2011) Radio core

MAXI J 1659 -152, the shortest orbital period BHXRB Peak position

dcore S 12/13 Flux density [m. Jy] X-ray lightcurve Size change [mas] Core size [mas] Compact jet interpretation Source size changes vs. flux density and core shift are in agreement with the compact jet model. dcore~1. 8 rcore Coreshift [mas] Hardness-Intensity Some core quenching is observed, but no bright, discrete ejecta through the state transition. Similar behaviour seen in Cyg X-1. (Rushton et al. 2012) Not powerful enough to produce strong shocks in the flow? Paragi et al. (2011) Paragi et al. (in prep. )

HESS J 0632+057, -ray BH binary candidate • Point like, variable Te. V source discovered by the HESS team (Aharonian et al. 2007; Acciari et al. 2009) • Variable counterparts in the X-rays and in the radio band (Hinton et al. 2009 and Skilton et al. 2009, respectively) • Proposed counterpart is the massive B 0 pe star MWC 148, d~1. 5 kpc; SED similar to LSI +61 303, but order of mag. fainter (Hinton et al. 2009) • Swift/XRT: 321 5 d periodicity (Bongiorno et al. 2011) supports binary nature, but binarity with optical spectroscopy not confirmed yet • X-ray outburst in Feb. 2011 (Falcone et al. 2011) • VERITAS and MAGIC reported increased activity at >200 Ge. V between 7 -9 Feb. 2011. (Ong 2011; Mariotti 2011) • e-EVN: first VLBI detection! Moldon, Ribo & Paredes (2011), ATel #3180

e-EVN: -ray BH binary scenario confirmed • Radio emission within 20 AU of MWC 148: confirming optical counterpart and indicating a compact object in close orbit • Tb>106 K – nonthermal radio emission • Follow-up observations during the normal EVN session, 30 days later: extended structure seen ~20 AU off the first epoch position, size ~75 AU Peak: 340 50 Jy/bm Total: 410 90 Jy Peak: 81 14 Jy/bm Total: 200 40 Jy Moldon, Ribo & Paredes (2011), A&A 533, L 7

A surprise from the Crab-nebula VLA (NRAO) HST (NASA/ESA) Radio Optical Chandra (NASA) X-rays

A gamma-ray flare detected by AGILE • A pulsar wind nebula: highly magnetized plasma of relativistic particles collide with ISM AGILE lightcurve, 2010 • Until now has thought to be very stable (at large) in the X-rays and -rays (standard candle) • Early AGILE data showed a flare – calibration or instrumental errors? HST Chandra • September 2010 another flare (~4 days), later confirmed by Fermi • Short duration small size, L ≤ 1016 cm • Wisps, knots and the anvil feature known HST to vary (days to months); interesting features, A in particular, marked to the right (HST/Chandra follow-up) • Pulsar itself did not change – where is the flaring region and what is the mechanism? Tavani et al. 2011, Science Chandra

The Crab-flare with the e-EVN Normal CLEAN, uv-tapered, restoring beam 150 mas Multi-resolution CLEAN, uv-tapered, 500 mas • e-EVN + 3 Merlin telescopes, 1. 6 GHz observations on 5 Nov. 2010 • Detected pulsar, C 1 and C 2 components plus extended emission • Bright optical knot HST-1 not detected • C 1 0. 5 0. 3 m. Jy, ~0. 2– 0. 6”; C 2 0. 4 0. 2 m. Jy, ≤ 0. 2” • SNR<4 for both, but simulations show that they are real Lobanov et al. 2011, Astron. Astrophys 533, A 10

The Crab-flare with the e-EVN HST e-EVN Chandra • e-EVN multi-scale image in contours, restored with 0. 7” beam • C 1, C 2 significant offset from jet axis (jet collimation beyond C 1? ? ? ) • C 1 close to (but not coincident with) knot A – related to –flare? • In this case the injection power generated the burst would be 0. 2% of the pulsar spin-down power Lobanov et al. 2011, Astron. Astrophys. 533, A 10

To be continued. . .

Prof Richard Schilizzi