Gamma-ray binaries: from low frequencies to high resolution

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1 Gamma-ray binaries: from low frequencies to high resolution Benito Marcote PhD Student October 15, 2014

2 Gamma-Ray Binaries Binary systems which host a compact object orbiting a high mass star that have the non-thermal maximum of the Spectral Energy Distribution in γ-rays (Paredes et al 2013, Dubus 2013) System Main star P/ days Cygnus X-3 WR 02 Cygnus X-1?? O97Iab 56 MWC 656?? Be 604 PSR B Ve HESS J B0 Vpe 3150 LS I B0 Ve 265 1FGL J O6V 166 LS 5039 O65V 39 Green: X-ray binaries with gamma-ray emission Red: known gamma-ray binaries SED of gamma-ray binaries versus HMXRBs Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 2/14

3 Gamma-Ray Binaries Young non-accreting pulsar scenario Strong shock between both winds: Relativistic pair plasma wind from the pulsar Stellar wind from the massive companion star Originally proposed by Maraschi & Treves (1981), re-proposed by Dubus (2006) Radio flux dominated by the synchrotron emission at GHz Orbital motion Wind standoff Star Pulsar V Zabalza et al: GeV-TeV em Coriolis turnover Shocked pulsar wind Shocked stellar wind Model for LS 5039 from Zabalza et al (2012) Fig 1 Sketch of the proposed scenario at the periastron of a close-orbit system similar to LS5039 The region of the CD where significant turbulence, and therefore wind mixing, are expected to take place is indicated with a wavy line The red regions indicate the two proposed emitter locations Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 3/14 o t w e 2 a p r d e s t t e o m t t e o w b i a l u b l

4 The gamma-ray binary LS 5039 LS 5039 O65 V star (23 ± 3 M ) d = 25 ± 05 kpc e = 035 ± 004 P orb = ± d Light-curve: TeV: periodic outbursts GeV: periodic outbursts X-rays: periodic outbursts radio: not periodic Small variability AU Casares et al (2005) AU Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 4/14

5 The gamma-ray binary LS S ν / mjy S ν / mjy VLA 1998 VLA 2002 GMRT GMRT/WSRT 2013 None Averaged values SSA fit to averaged values SSA+Razin fit to averaged values ν / GHz S ν / mjy Jul Jul 21 SSA fit to Jul 19 SSA+Raz fit to Jul 21 Fit to averaged values ν / GHz Averaged spectrum explained by a synchrotron self-absorption emission Slightly differences in simultaneous spectra (WSRT+GMRT data) Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 5/14

6 The gamma-ray binary LS I LS I B0 Ve star (125 ± 25 M ) d = 20 ± 02 kpc e = 072 ± 015 P orb = ± 0003 d P super = 1667 ± 8 d Outbursts at all frequencies X-ray TeV: correlated(?) Radio TeV: correlated Optical Radio: correlated GeV TeV: anticorrelated Frail & Hjellming (1991), Casares et al (2005), Gregory (2002) Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 6/14

7 Radio emission of LS I LS I exhibits a large variability at radio frequencies Emission orbitally modulated (P orb 265 d) No 1, 1998 RELATIONSHIP BETWEEN 2CG 135]1 AND LSI ] STRICKMAN ET AL Vol 497 OSSE range than was observed The OSSE integral Ñux 100 from 50È300 kev during VP 325 is (43 ^ 11) ] 10~4 photons cm~2 s~1, while the integral of the ASCA best-ðt 10 9 June 94 (097) 26 June 94 (062) power-law models extrapolated to the same energy range are (10 ^ 04) 100 ] 10~4 and (05 ^ 02) ] 10~4 photons cm~2 s~1 for radio phases 02 and 042 respectively These are inconsistent10 11 June 94 (006) 28 June 94 (070) at the 28 p and 34 p levels, assuming that the spectrum 100 does not change (in particular, does not harden signiðcantly) from 10 to 300 kev Since the relatively June large 94 (009) OSSE Ðeld of view 1 July does 94 (079) not exclude the nearby QSO 0241]622 as a possible source of 100 emission, we have also plotted the result of EXOSAT (2È10 kev) observations of the QSO (Turner & Pounds 1989), June 94 (019) 2 July 94 (084) corrected for its position in the OSSE collimator response Note that the photon index power-law spectrum used to model the EXOSAT data is consistent with the OSSE result June 94 (028) 3 July 94 (088) When we look 100at an overall view of the spectra from this region, no clear picture emerges However, the fact that OSSE and COMPTEL June results 94 (031) fall signiðcantly 5 July above 94 (095) an extrapolation of the ASCA spectra and that the OSSE and 100 COMPTEL spectra are consistent with the X-ray spectrum of QSO 0241]622, lead to the likelihood that at least some, June 94 (035) 7 July 94 (002) and perhaps a signiðcant amount, of the Ñux observed by both OSSE and 100COMPTEL might come from the QSO rather than LSI ] Cycle-to-cycle variations in the X-ray emission June 94 (042) 8 July 94 (007) may also contribute to the observed discrepancy More contemporaneous X-ray 100 and01 c-ray data 10 are 100 required to test for the existence of cycle to cycle variability Frequency (GHz) of the LSI ] system and to better study the X-ray FIG 4ÈMultifrequency radio light curves of LSI ] observed Strickman FIG period 5ÈTime et recently evolution al of the (1998) reported LSI ] nonthermal by Paredes radio spectrum et al during (1997a) the outburst of 1994 JuneÈJuly Spectra are labeled according to the date and radio phase of the observation with the VLA corresponding to the radio outburst of 1994 JuneÈJuly Similarly, the low signiðcance of the OSSE light curves Error bars not shown are smaller than the symbol size a function shownof inorbital Figure phase 2 does Ultimately notthe allow high-energy us to usewith temporal wind optical signa- depth e ects dictating the time delay Benito Marcote bmarcote@amubes Astrolunch shock emissivity will depend on the geometrical and radiative tures characteristics to - ASTRON/JIVE between the injection of the electrons and the visibility of associate of the pulsar LSI cavity ] as the pulsar with orbits the OSSE the radiosource emission We 7/14 Flux Density (mjy)

8 Results from the GMRT observations GMRT data from Nov 2005 to Feb MHz 235 MHz 80 S º = mjy :0 0:5 1:0 1:5 2:0 Á Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 8/14

9 Results at very low frequencies With the GMRT observation at 154 MHz we detected for first time a gamma-ray binary at these very low frequencies ν = 154 MHz Bandwidth 32 MHz Beam: arcsec (J2000) Point-like source S ν = 37 ± 2 mjy m 42 m 41 m 40 m (J2000) 39 m 2 h 38 m Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 9/14

10 Results at very low frequencies 6 RSM pointings to LS I with LOFAR up to now ν = 149 MHz Bandwidth 78 MHz Beam: arcsec g 4 analyzed obs 3 detections > 3σ Point-like source Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 10/14

11 Results at very low frequencies Preliminary results from the RSM LOFAR observations Detection of LS I in three of four analyzed observations The behavior of the source is variable along the time φ LOFAR 150 MHz 80 Sν / mjy MJD Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 11/14

12 The gamma-ray binary HESS J The gamma-ray binary candidate HESS J HESS J B0 Vpe star (16 ± 3 M ) d = 14 ± 05 kpc e = 083 ± MWC 148 / HESS J Porb = 321 d φapa = 047 B A RR005, RM006 P orb = 321 ± 5 d AU 2 Variability at all frequencies TeV: periodic outbursts GeV: periodic outbursts X-rays: periodic outbursts radio:? 1 0 Toobserver φper = 097 Moldón (2012) AU Benito Marcote bmarcote@amubes Figure 81: Sketch of the orbit of MWC 148/HESS J with the position of the compact object during the observations of projects RR005 and RM006 marked as red circles The white dots are plotted every 01 orbital phases The empty squaresmarktheinferiorand superior conjunction of the compact object, which occur at orbital phases 0961 and 0063, respectively Astrolunch The - orbit ASTRON/JIVE was computed using the orbital solution reported in Casares et al 12/14

13 Radio emission of HESS J Radio flux density [µjy] Integral flux (>1 TeV) [10 12 cm 2 s 1 ] Phase-folded time [days] EVN 16 GHz WSRT 16 GHz GMRT 13 GHz Swift HESS VERITAS MAGIC Swift < 30 µjy Orbital phase Light-curve of HESS J in radio (color data, top), X-rays (gray circles) and TeV (color data, bottom) X-ray flux [10 12 erg cm 2 s 1 ] X-ray flux [10 12 erg cm 2 s 1 ] Declination (J2000) δ offset [mas] m Right Ascension (J2000) α offset [mas] 6 h 32 m EVN and WSRT observation in 2014 No detections in any case, with an EVN 3-σ upper-limit of 30 µjy Benito Marcote bmarcote@amubes Astrolunch - ASTRON/JIVE 13/14

14 Thank You! Benito Marcote Astrolunch - ASTRON/JIVE 14/14

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