Discovery of a transitional Redback millisecond pulsar J !
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1 Discovery of a transitional Redback millisecond pulsar J ! By Jayanta Roy!! JBCA, University of Manchester!! and!! National Centre for Radio Astrophysics (NCRA-TIFR) Neutron stars at the crossroads, 25 th June 2015! European Week of Astronomy and Space Science
2 Collaborators! Paul S. Ray (NRL)! Bhaswati Bhattacharyya (University of Manchester)! Ben Stappers (University of Manchester)! Jayaram N. Chengalur (NCRA-TIFR)! Julia Deneva (NRL)! Fernando Camilo (Colombia University)! Tyrel J. Johnson (George Mason University)! Michael Wolff (NRL)! Jason W. T. Hessels (ASTRON)! Cees G. Bassa (ASTRON)! Evan F. Keane (University of Manchester)! Elizabeth C. Ferrara (NASA Goddard Space Flight Center)! Alice K. Harding (NASA Goddard Space Flight Center)! Kent S. Wood (NRL)!
3 LMXB to MSP! ü The extremely short spin period of millisecond pulsars are assumed to be! outcome of accretion of the mass transferred by a low-mass (< Msun)! companion star through an accretion disk.! ü A Gyr-long mass accretion during which the system with an accretion disk appears luminous in X-ray; brighter in gamma-ray; radio continuum powered by outflow.! ü 300 known radio MSPs in our Galaxy are believed to be recycled product of accreting neutron stars in low-mass X-ray binaries.! ü Discovery of millisecond pulsation from accreting neutron stars in LMXB supports how mass accretion is able to effectively spin-up a neutron star.! ü PSR J (Archibald et al. 2009) and J I (Papitto et al. 2013) provide most convincing proof of evolutionary link shared by accreting neutron star in low-mass X-ray binary and radio millisecond pulsars.!
4 Transitional MSP systems! ü PSR J with an evidence of accretion disk in ; radio pulsar in 2009; reverse transition to LMXB in June 2013 (Stappers et al. 2014, Patruno et al. 2014) à decadal time-scale between transitions! ü In last decade ( ) IGR J has shown both rotation! powered and accretion powered activities on a time-scales of few days to months. The short timescales observed for transitions between! accretion-powered and rotation-powered states are comparable with! those for typical X-ray luminosity variations, caused by swings of the! mass inflow rate onto the neutron star.! ü It is probable that a rotation-powered pulsar switches on during the! X-ray quiescent states of other accreting millisecond pulsars!
5 LMXB XSS J ! ü A flat-spectrum radio emission possibility powered by outflow (Hill et al. 2011)! ü X-ray, UV emissions compatible with accretion powered object! (de Martino D. et al. 2013)! ü Bassa et al reported sudden! decrease in X-ray and optical flux! around November/December 2012! ü Previous sign of accretion disk also! disappeared!! ü XSS J may harbour an! active rotation-powered MSP!! ü Orbital modulation of X-ray brightness (Bogdanov et al. 2014)! Courtesy : Bassa et al. 2014
6 The GMRT! ü The Giant Metre-wave Radio Telescope (GMRT) is a radio interferometer operating at low radio frequencies (150, 244, 322, 607, 1060 to 1450 MHz)! ü Array consisting of 30 antennas of 45 metres diameter, operating at metre wavelengths -- the largest in the world at these frequencies!! ü Simultaneous dual beam search one with HPBW ~ 40 (incoherent with 0.4 mjy) other with 1 (coherent with 0.1 mjy)! ü 2048 X MHz 61 μs gives! dispersion_smear < sample_resolution for! DM up-to 100 pc cm-3! ü Synchronous time-domain and imaging! study!!
7 Discovery of PSR J ! PSR J , 1.69ms redback MSP at a DM of 43.5 pc cm -3 discovered at 607 MHz with the GMRT! (Roy, Bhattacharyya & Ray, Atel #5890, 2014)!
8 ü 500 days of phase coherent! timing combining! GMRT-607 MHz and! Parkes-1390 MHz TOAs! resulting 15 μs residuals! ü Model with four orbital period! derivatives!!! ü Companion mass of < 0.4 M sun! ü Edot/a 2 (4 x erg lt-s -2 s -1 ):! an order of magnitude! higher than other MSP binaries! Timing of PSR J !
9 Timing residuals! Post-fit residuals (µs) Year GMRT 607 MHz TOAs Parkes 1390 MHz TOAs ü ~ 322 TOAs from early 2014 to early June 2015! ü A redback! MJD ü Roche lobe radius (0.24 R sun ) smaller than opaque part of companion orbit (4.9 R sun )! ü Excess DM of seen at eclipse egress à 4 x cm -2 added electron density!
10 Synchronous radio imaging! PLot file version 1 created 23-SEP :15:21 CONT: J IPOL MHZ 19:37-20:43.ICL Declination (J2000) eclipsing binary phase Right ascension (J2000) Cont peak flux = E-04 JY/BEAM Levs = 1.000E-05 * (12, 18.78, 29.39, 46.00, 72) PLot file version 1 created 23-SEP :15:16 CONT: J IPOL MHZ 22:56-END.ICL Declination (J2000) Right ascension (J2000) Cont peak flux = E-04 JY/BEAM Levs = 1.000E-05 * (12, 18.78, 29.39, 46.00, non-eclipsing binary! phase
11 Continuum flux Vs pulsed flux! ü Interstellar effects like scatter broadening or excess dispersion are not the cause of eclipse; probably absorption of radio waves are causing radio eclipse!
12 Pre-discovery radio observations! ü Hill et al observations shows radio emission powered by outflow! ü Parkes 2012 Mar observations showed marginal detections! à rotation powered pulsed! emission active in LMXB-! state (Takata et al 2014)!! ü Parkes 2013 Nov 12 observations had few intermittent detections!
13 Pulsed gamma-ray emission using Fermi-LAT! Courtesy : Johnson et al 2015 ü > 6σ significance detections of gamma-ray! pulsations using +6months data with same! model as in Johnson et al 2015! ü > 0.1 GeV light curve using data over the! radio timing-span! ü Gamma-ray peak nearly aligned with main! peak of 1400 MHz radio profile! ü Partial co-location of radio-gamma-ray emission region! ü Considerable spectral evolution of two radio peaks!
14 Gamma-ray emission! ü Timing model with higher-order orbital period derivatives Vs Proper motion! ü Photon flux dropped by 3x at! transition! ü Flux light curve with 2-day! bins results the transition day! as 2012 Nov 30! ü Gradual decrease in! gamma-ray flux at! post-transition! ü Propeller model to explain the! gamma-ray and X-ray flux increase! in LMXB-state (Papitto et al. 2014)! Courtesy to Tyrel Johnson
15 Summary! ü Discovery of redback PSR J associated with LMXB XSS J ! ü Signature of erratic binary orbital behavior! ü Synchronous radio imaging to revel the eclipse cause!! ü Detection of post-transition gamma-ray pulsation from PSR J ! ü Gamma-ray flux monitoring suggest probable transition day! ü Significant profile evolution and gamma-ray emission model! Thank you!
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