1 / 48

New INTEGRAL High Mass X-ray Binaries

New INTEGRAL High Mass X-ray Binaries. Lara Sidoli (INAF-IASF, Milano). Simbol-X Bologna, 2007, 14-16 May. A biased introduction to the INTEGRAL discoveries in the HMXB field: highly obscured Galactic sources and... ....The mistery of the Supergiant Fast X-ray Transients

edan-stevens
Télécharger la présentation

New INTEGRAL High Mass X-ray Binaries

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. New INTEGRAL High Mass X-ray Binaries Lara Sidoli (INAF-IASF, Milano) Simbol-X Bologna, 2007, 14-16 May

  2. A biased introduction to the INTEGRAL discoveries in the HMXB field: highly obscured Galactic sources and... ....The mistery of the Supergiant Fast X-ray Transients IGR J11215-5952: a unique SFXT ! A possible solution to the SFXTs puzzle Overview

  3. Sources detected with ISGRI during the first 4 years of observations from Bodaghee et al., 2007, astro-ph/0703043

  4. Sources detected with ISGRI during the first 4 years of observations from Bodaghee et al., 2007, astro-ph/0703043

  5. X-ray pulsations (slow pulsators, with periods ~ few hundred seconds) Hard and highly absorbed X-ray spectra sometimes with strong Fe emission lines(Ph.Index ~0.5-1; absorbing column densities NH > 1E23 cm-2) the first (discovered on 2003, Jan 29) of these heavily absorbed sources was IGR J16318-4848 (Walter et al 2003, Matt & Guainazzi 2003, Ibarra et al. 2006) Optical Identification with Blue Supergiants or Be stars (e.g. Masetti et al. 2005, 2006, Reig et al. 2005) They are mainly located in the direction of the spiral arms of our galaxy About 30% of the new IGRs are HMXRBs

  6. The prototype of the highly obscured IGR sources: IGR J16318-4848 IGR J16318-4848 with XMM-Newton & INTEGRAL from Ibarra et al. 2006

  7. Simulation of a IGR J16318-4848-like spectrum with Simbol-X Simulated spectrum (50 ks) Nh = 2E24 cm-2 cutoffpl : ph. index = 1.6 Ec = 60 keV 3 gaussians at 6.4 keV, 7.099 keV and 7.45 keV

  8. An updated summary of IGR HMXBs with known Pspin or Porb, or both :

  9. Thanks to the Galactic Plane monitoring with INTEGRAL: heavily obscured sources & transients with short outburst have been discovered in the first 4 years of observations

  10. The story of the SFXTs begins with XTE J1739-302 ..... an unusual new x-ray transient Smith et al. 1998: RossiXTE obs. 1997 Aug 12 – discovery of a new transient, active only 1 day ! ~ 3E-9 erg/cm2/s (2-25 keV): the brightest source in the direction of the Galactic Center region on that one day Thermal bremsstrahlung spectrum kT ~ 21 keV => Be/XRB ???

  11. XTE J1739-302 ..... an unusual new x-ray transient Smith et al. 1998: RossiXTE obs. 1997 Aug 12 – discovery of a new transient, active only 1 day ! ~ 3E-9 erg/cm2/s (2-25 keV): the brightest source in the direction of the Galactic Center region on that one day Thermal bremsstrahlung spectrum kT ~ 21 keV => Be/XRB ??? Negueruela et al. 2005: Optical counterpart is an O-type supergiant (O8 I ) -> dist ~ 2 kpc => a new class of transient sources!?!?!

  12. INTEGRAL discoveries and observationsSupergiant Fast X-ray Transientsunusually SHORT outbursts, significantly shorter than Be/NS binaries OUTBURST DURATION: ~ few hours, less than a day RECURRENT OUTBURSTS HARD AND HIGHLY ABSORBED X-RAY SPECTRUM reminiscent of an X-ray pulsar OPTICAL COUNTERPART: highly reddened O B supergiants IGR J17391-3021/XTE J1739-302 ISGRI SWs (~2 ks) image sequence (20-30 keV) flux at peak=254 mCrab from Sguera et al. 2005

  13. A growing number of observations and a growing number of sources mainly thanks to INTEGRAL ! SFXTs and SFXT candidates initially selected because of the short outbursts, then possibly confirmed based on the optical counterpart from Negueruela et al. 2005 Sguera et al. 2005, 2006 Source Dist Sp.Type Peak flux (20-40) (kpc) ISGRI (erg/cm2/s) IGR J17391-3021/XTE J1739-302 2-3 O8Iab 6.5 E-09 IGR J17544-2619 3 O9Ib 3.0 E-09 SAX J1818.6-1703 ? supergiant earlier than B3 1.3 E-09 IGR J16479-4514 ? ? 2MASS source 2.4 E-10 IGR J18410-0535/AX J1841.0-0536 10 B0I 9.0 E-10 IGR J17407-2808 (=SBM10) ? 10 ? - 6.0 E-09 IGR J16195-4945/AXJ161929-4945 ? 5 - 3.0 E-10 AX J1749.1-2733 ? - - 3.0 E-10 XTE J1743-363 ? - - 3.0 E-10 IGR J16418-4532 ? - supergiant?? 6.0 E-10 IGRJ18450-0435/AX J1845.0-0433 3.6 O 9.5 I 6.0E-10 IGR J08408-4503 ? Ob5Ib 6.0E-09 IGR J11215-5952 Other possible candidates: IGR J10043-8702, IGR J10500-6410, IGR J15283-4443, IGR J18159-3353, IGR J18159-3353, IGR J 20188+3647, IGR J21117+3427,IGR J17354-3255

  14. A growing number of observations and a growing number of sources mainly thanks to INTEGRAL ! SFXTs and SFXT candidates initially selected because of the short outbursts, then possibly confirmed based on the optical counterpart from Negueruela et al. 2005 Sguera et al. 2005, 2006 et al. Source Dist Sp.Type Peak flux (20-40) (kpc) ISGRI (erg/cm2/s) IGR J17391-3021/XTE J1739-302 2-3 O8Iab 6.5 E-09 IGR J17544-2619 3 O9Ib 3.0 E-09 SAX J1818.6-1703 ? supergiant earlier than B3 1.3 E-09 IGR J16479-4514 ? ? 2MASS source 2.4 E-10 IGR J18410-0535/AX J1841.0-0536 10 B0I 9.0 E-10 IGR J17407-2808 (=SBM10) ? 10 ? - 6.0 E-09 IGR J16195-4945/AXJ161929-4945 ? 5 - 3.0 E-10 AX J1749.1-2733 ? - - 3.0 E-10 XTE J1743-363 ? - - 3.0 E-10 IGR J16418-4532 ? - supergiant?? 6.0 E-10 IGRJ18450-0435/AX J1845.0-0433 3.6 O 9.5 I 6.0E-10 IGR J08408-4503 ? Ob5Ib 6.0E-09 IGR J11215-5952 Other possible candidates: IGR J10043-8702, IGR J10500-6410, IGR J15283-4443, IGR J18159-3353, IGR J18159-3353, IGR J 20188+3647, IGR J21117+3427,IGR J17354-3255 Hard X-ray spectra with high energy cut off at ~ 10-30 keV L outburst / L quiesc. ~ 1E3-1E4 (from ASCA archival, or XMM or Chandra obs) but only from few sources!

  15. Flux (20-40 keV) at the peak of the outburst, together with the “quiescent” level quiescent level measured well far away from the outbursts 1997, Aug, XTE obs 2004, Aug, ISGRI obs

  16. IGR J17544-2619 in't Zand 2005 Chandra obs

  17. SFXTs properties: absorbing column density from X-ray spectra NH – NH Gal (1E22 cm-2) Total NH Galactic(1E22 cm-2) towards the sources

  18. SFXTs properties: X-ray luminosity during the short flares

  19. HMXRB classes: a summary Persistent wind fed accreting X-ray pulsars with supergiant companions “typical” HMXRBs, Vela X-1 like A new class -> Supergiant Fast X-ray Transients with supergiant companions transient emission, with short duration outbursts, typically few hours, less than Be/XRBs outbursts highly absorbed HMXRBs discovered with INTEGRAL a growing number of members have been discovered with INTEGRAL Be/X-ray binaries typically Transient X-ray sources with Be companions Bright persistent disk-fed massive X-ray binaries (Cen X-3 like) in close orbits

  20. Supergiant Fast X-ray Transients:proposed interpretations (I) Outbursts produced by short ejections from the donor stars in XRBs? or clumpy winds? (in 't Zand 2005) this suggestion is based on optical observations of the clumping nature of the wind from early type stars: Owocki et al. 1997, Lamers & Cassinelli 1999: line-driven winds from supergiant stars are highly variable

  21. Supergiant Fast X-ray Transients:proposed interpretations (II) A new kind of supergiant HMXRBs in wide eccentric orbits? (wider than “normal” supergiants HMXRBs, like Vela X-1, in nearly circular orbits) also to explain the large Lmax / Lmin (Negueruela et al. 2005) Lx expected from an eccentric orbit around a supergiant with a spherical homogeneous wind in the case: 30 Msun companion star beta wind=1 terminal wind velocity=1800 km/s Porb=200 days Wind mass loss rate=2 E-6 Msun/yr

  22. IGR J11215-5952: a unique SFXT Fast transient discovered on April 22, 2005 (Lubinski et al. 2005): detected with ISGRI in 2 consecutive pointings, reaching 75 mCrab at peak (20-60 keV) The companion is a B-type Supergiant: HD 306414 (Negueruela et al. 2005; Masetti et al. 2006)

  23. The INTEGRAL lightcurve shows a periodicity of ~ 330 days in the recurrence of the outbursts (Sidoli, Paizis & Mereghetti, 2006, A&A, 450, L9; astro-ph/0603081). ~ 330 days ! ~ 330 days ! 1st outburst 3-4 July 2003 2nd outburst 26-27 May 2004 3rd outburst 22 Apr 2005 ISGRI lightcurves (17-40 keV) 330 days = likely orbital period

  24. 4th outburst lightcurve (Smith et al. 2006, ATel 766 and ATel 773) XTE/PCA extreme variability X-ray spectrum: hard and quite constant through the outburst Ph. index ~ 1.7 +/- 0.2 (2.5-15 keV) NH ~ 11 +/- 3 E22 cm-2 (higher than Galactic) Flux at peak ~ 2 x 10-10 erg/cm2/s roughly consistent with previous outbursts from http://scipp.ucsc.edu/~dsmith/atel/atel0306/

  25. IGR J11215-5952: INTEGRAL spectra 2nd outburst 1st outburst 2004 2003 JEM-X IBIS/ISGRI IBIS/ISGRI 5 100 100 20 Energy (keV) Energy (keV) ph.index = 2.6 +1.8 -0.6 ph.index = 0.5 +0.4 -0.6 E cutoff = 15 +/-5 keV F = 6.2 E -10 erg/cm2/s (5-100 keV) F = 2.5 E -10 erg/cm2/s (20-100 keV) L = 3E36 erg/s (5-100 keV)

  26. IGR J11215-5952 is a slow X-ray pulsator in a wide orbit XTE/PCA pointings performed during the 4th outburst in 2006 showed variability which suggested a pulsation period of approximately 195 +/- 10 s (Smith et al. 2006). The pulsations have been confirmed during the 5th outburst in Feb 2007 (Swank et al. ATel # 999): Pspin=186.78+/- 0.3 s This would imply an X-ray pulsar with: Porb ~ 329 days P spin ~ 190 s thus an accreting pulsar lying in the Be\XRB region of the Corbet diagram ?? BUT the companion is a supergiant! so it is not a Be/NS system !!! Porb=329 days seem to suggest that outbursts in SFXTs might be related to wide highly eccentric orbits and not to clumpy winds

  27. The periodic nature of the outbursts from IGR J11215-5952 allowed us to plan & perform for the first time a sensitive and complete monitoring of the entire outburst from a SFXT, during the latest outburst, expected on 2007, 9th February with Swift/XRT Monitoring campaign strategy: - 2 ks / day at the beginning (starting on 4th February) - then exposure up to 10 ks / day during outburst - Monitoring end planned for 14th February (actually, IGR11215 was kindly observed up to 26th February) - Thanks to Neil Gehrels and to the Swift Team Results in Romano, Sidoli, Mangano, Mereghetti & Cusumano , 2007 (A&A in press; astro-ph/0704.0543)

  28. Final lightcurve from Swift / XRT observations of IGR J11215-5952 9th February 2007 Romano et al. 2007

  29. 1st fact: the accretion phase in SFXTs lasts longer than originally thought based on less sensitive instruments

  30. Note that INTEGRAL would have seen ONLY the bright “orange” region of the lightcurve, lasting less than 1 day and composed of several ``short flares” 9th February 2007

  31. Close-up view of the brightest part of the outburst (9th Feb) 2nd fact: a large variability is present, and the outburst event is composed of short flares, lasting few hours or less

  32. NH=1.11E22 (+0.79 -0.49) G=0.91 (+0.42 -0.32) NH=0.85E22 (+0.46 -0.32) G=0.94 (+0.31 -0.28) NH=2.02E22 (+1.01 -0.79) G=1.51 (+0.58 -0.53) NH=0.88E22 (+0.38 -0.31) G=1.03 (+0.32 -0.31) NH=0.83E22 (+0.62 -0.42) G=0.82 (+0.44 -0.40)

  33. The total Galactic absorption towards the source is 0.8 E22 cm-2

  34. How to explain the outburst? The recurrence time of 329 days is the underlying clock of the phoenomenon, which can be interpreted in a natural way as the orbital period of the binary system Model of accretion from a spherical homogeneous wind in an eccentric orbit around the HD star

  35. A sorta fairytale 3rd fact: the lightcurve is too narrow and steep to be explained within a model of Bondi accretion from a spherical and homogeneous wind in an eccentric binary (even with extreme eccentricities!)

  36. Using the neutron star as a probe of the supergiant wind, the shape of the X-ray lightcurve implies that the wind from the B supergiant is NOT spherical nor homogeneous then.....

  37. Using the neutron star as a probe of the supergiant wind, the shape of the X-ray lightcurve implies that the wind from the B supergiant is NOT spherical nor homogeneous then..... our idea is that there is a second wind component in a “thin equatorial disk” with lower wind velocity and a higher wind mass loss rate compared to the “polar wind component”

  38. Simulation of the radiatively driven outflow from a rotating hot star with a dipole magnetic field Log (wind density) from Ud-Doula, Townsend & Owocki, 2006, ApJ, 640, L191

  39. The proposed geometry to explain the short SFXT outbursts: OB supergiant ns The thin equatorial disk of the B-supergiant is inclined with respect to the orbital plane The star has also a polar wind with higher velocity and lower mass loss rate (~0.01 * Mass loss rate in the disk) thus, in order to explain the low X-ray emission level out of the outburst, we need anyway a not circular orbit Sidoli et al., 2007, in preparation

  40. The thickness “h” of the densest region of this disk orbital plane “h” can be estimated from the duration of the outburst: the duration t of the brightest part of the outburst is t ~ 1 day, the ns velocity near periatron is roughly vns ~ 100-200 km/s thus: h ~ 8E11 – 1.7 E12 cm (0.3-0.6 Ropt, if Ropt ~ 40 Rsun) h

  41. The thickness “h” of the densest region of the disk orbital plane “h” can be estimated from the duration of the outburst: the duration t of the brightest part of the outburst is t ~ 1 day, the ns velocity near periatron is roughly vns ~ 100-200 km/s thus: h ~ 8E11 – 1.7 E12 cm (0.3-0.6 Ropt, if Ropt ~ 40 Rsun) Nh galactic < 0.8 E 22 cm-2; Nh from X-ray spectra ~1-2 * 1E22 cm-2 Assuming about 1E22 cm-2 is local and mainly due to the supergiant disk, a rough estimate of the rdensity of the supergiant disk is: Nh*mH / h = r ~ 1E-14 cm-3 h

  42. variable wind density along the orbit “disk” wind “polar” wind

  43. Example of the model of wind accretion with the following parameters: B-supergiant mass = 39 Msun “polar wind” mass loss rate = 3.7 E-6 Msun/yr terminal velocity (“polar wind”) = 1800 km/s beta law exponent = 1.0 Porb = 329 days e = 0.4 Note that along the orbit, the centrifugal barrier is always open (with B ~ 1E12 G, and Pspin=187 s) “disk wind” with Mdot_wind = 100 * Mdot_polar terminal velocity = 900 km/s “disk wind” with Mdot_wind = 30 * Mdot_polar terminal velocity = 1600 km/s

  44. few further questions ....

  45. how to explain other SFXTs where a clear periodicity in the outbursts has not been found yet? probably a different eccentricity & a different geometry of the thin disk with respect to the orbital plane

  46. how to explain other SFXTs where a clear periodicity in the outbursts has not been found yet? probably a different eccentricity & a different geometry of the thin disk with respect to the orbital plane how to explain the persistent Vela X-1-like HMXBs with supergiant donors? probably the “equatorial disk” of the supergiant in the persistent systems lies on the orbital plane and the ns always moves inside the disk

  47. Conclusions • INTEGRAL observations opened a new view on High Mass X-ray Binaries • The new class of SFXTs has been discovered • The SFXT IGRJ11215-5952 is a key system to understand this new class of X-ray sources • We proposed a new hypothesis to explain the properties of the SFXTs, where the supergiant has an equatorial component of the wind, besides the “standard” “polar” high velocity wind. • The enhanced accretion rate when the neutron star cross this disk produces the short duration X-ray outburst

More Related