Name: Sangita Kumari
Affiliation: National Centre for Radio Astrophysics Pune
Conference ID : ASI2022_301
Title : A decade of a timing study of a black widow pulsar J1544+4937 with the GMRT
Authors : Sangita Kumari, Bhaswati Bhattacharyya, Devojyoti Kansabanik, Jayanta Roy
Abstract Type: Poster
Abstract Category : Stars, ISM and Galaxy
Abstract : We present results from long-term timing of a black widow millisecond pulsar (BW MSP) J1544+4937 discovered with GMRT. This is the longest duration timing study of any galactic MSP with the GMRT. BW MSPs are compact binaries (orbital period < 1 day) in special evolutionary phases with a non-degenerate main-sequence companion with mass < 0.01 Msun. Initial 1.5 years of timing indicated that PSR J1544+4937, a 2.15 ms pulsar, is in a compact orbit with an orbital period of 2.9 hours (Bhattacharyya et al. 2013). The current study extends the existing timing baseline to 11 years including multi-frequency GMRT observations combining 32 MHz and 200 MHz bandwidth systems and achieved a timing residual of 6.4 μs. We report the first detections for a significant value of proper motion, first order orbital period derivative and 1st, 2nd , 3rd order DM derivatives for this system. Although with the advent of Fermi gamma-ray telescope, a significant number of BWs are now available, it is hard to time them precisely in general, as most of them exhibit orbital variability along with dispersion measure (DM) variation. Therefore they are not considered to be suitable for Pulsar Timing Array (PTA). But Bochenek et al. 2015, using simulated data, emphasized that BW pulsars can be included in the PTA after proper modeling of the timing systematics using higher order orbital period derivatives and DM derivatives. From 4 years of timing using sensitive wide-bandwidth (200 MHz) uGMRT observations, we have achieved 2.9 μs timing residual. With such precise timing aided with simultaneous multi-frequency observations with the uGMRT we aim to measure the intra-orbit DM variation for J1544+4937, which will provide input for hydrodynamical simulations of the orbit (Tavani et al. 1991) and will allow us to explore the possibility for inclusion of J1544+4937 in PTA.