Long-term monitoring of RRAT J HU HuiDong Urumqi Observatory, NAOC July 27, 2009 Rotating Radio Transients Observation

Introduction Rotating Radio Transients (RRATs) Rotating Radio Transients (RRATs) 11 discovered and published on Nature (M. A. McLaughlin et al. 2006) (M. A. McLaughlin et al. 2006)  Characters of the 11 RRATs Bursts duration between 2 and 30 ms Bursts duration between 2 and 30 ms Average time intervals between bursts range from 4 minutes to 3 hours Average time intervals between bursts range from 4 minutes to 3 hours Periodicities, 0.4-7s Periodicities, 0.4-7s Detectible flux duration <1s/d Detectible flux duration <1s/d Brightest radio sources after the giant pulses from the Crab pulsar and the pulsar B Brightest radio sources after the giant pulses from the Crab pulsar and the pulsar B  The number of RRATs may exceed that of regular pulsars

NamePPdotDMRaDec Burst Rate Survey s s/spc/cm^3hh:mm:ss.sdd:mm:ss.s 1/h J : GBT350 J :57-14:203.43PH J :55-44:285.14PH J :48-43:161.42PM1 J :47-58:416.86PM2 J :31-57:111.71*PM2 J :17:46.357:59: PM1 J :28-58:541.71*PM2 J :23-56: PM2 J :43-60:320.78PM1 J :23-08:46154GBT350 J :39-25:131.71*PM2 J :54-30:110.60PM1 J :19: :58: PM1 J :26-14:271.06PM1 J :39-01:360.62PM1 J :40-06: PM2 J :46-02:561.10PM1 J :48-12:471.25PM1 J :11+00:370.31PM1 J :13: :33: PM 1 J : PALFA

About RRAT J Mclaughlin et al. 2006, Nature ， 439, 817 Burst rate: 17 per hour Burst duration: 2 ms Peak flux : ~3.6 Jy Single pulses timing P: 4.26 s P-dot: s/s DM: 196 (3) pc cm -3 Age: 117 Kyr B surf : 5 × Gauss Radio observations X-ray observations The Chandra observation detected the X-ray counterpart (Reynolds et al. 2006). XMM–Newton, discovered the X-ray pulsations with the period predicted by the timing of radio bursts. Mclaughlin et al. (2007) So, what is it?

Observation system and de-dispersion method 128 channels, with bandwidth 2.5M Hz 2 polarizations, Center frequency is 1540M Hz

Observations of RRATs Giant pulses of some pulsars Search of extremely strong pulses from pulsars PSR B Weltevrede et al ， ApJ ， 645 ， 147 Small-time-scale radio transients search Monitoring of magnetars (AXP & SGRs) Based on the Filter-Bank de-dispersion system, We developed software to search rare and strong single pulses. Since March 2007: Identifying the signal

Long Term monitoring of RRAT J Timing results from 162 bursts Updated to Mar Esamdin et al ， MNRAS, 389, 1399 DM=196.0(4)

Long Term monitoring of RRAT J Timing results from 162 bursts Single pulse timing ： Updated to Mar Esamdin et al ， MNRAS, 389, 1399

Long Term monitoring of RRAT J Timing results from 162 bursts Timing position Timing residuals and pulse phases Bimodal distribution of pulse phase? In fact, there are even more… Updated to Mar Esamdin et al ， MNRAS, 389, 1399

About 350 strong bursts detected updated to June 2009 Long-Term monitoring of RRAT J Timing irregularity: First glitch detected in RRAT ？ Epoch around MJD 54580

Long-Term monitoring of RRAT J Top left: Timing residuals with 1 st glitch fitted. Bottom right: Timing residuals with both glitches fitted

Long Term monitoring of RRAT J Glitch parameters got: Glitch parameters got: Epoch of Glitch 1: MJD Epoch of Glitch 1: MJD Δν: 1.989(8)× Hz Δν: 1.989(8)× Hz ν(dot):8.11(7)× Hz s -1 ν(dot):8.11(7)× Hz s -1 Epoch of Glitch 2: MJD Epoch of Glitch 2: MJD Δν: 1.02(1) × Hz Δν: 1.02(1) × Hz ν(dot): 1.8(2) × Hz s -1 ν(dot): 1.8(2) × Hz s -1 The second glitch is too small?

Long Term monitoring of RRAT J

Summary: In observation of hundreds of hours, we detected about 350 dispersed bursts of RRAT J1819−1458 with the signal-to-noise ratios (S/Ns) above 5 σ threshold. The S/N of the strongest burst is The source’s DM measured through our data is ± 0.4 pc cm −3. Our timing position with 2σ error is consistent with the position of its X-ray counterpart CXOU J − glitches detected in observation during 800 days, with first one at MJD 54572, the other one at MJD The distribution of the timing residuals is bimodal before the first glitch, but has only one main component between the 2 glitches, and becomes bimodal again after the second glitch. Careful study of the radio bursts properties is necessary to get a more accurate parameter of the second glitch. Long Term monitoring of RRAT J

Thanks! And, Thanks to YUAN J.P. ZHAO C.S. and A. Esamdin