Crab pulsar Mingyu Ge HXMT Collaboration IHEP 2018
Crab pulsar Mingyu Ge HXMT Collaboration IHEP, 2018 -04 -12
Outline n n n Introduction Pulse profile Phase-resolved spectrum Flux evolution Crab Nebula HXMT observation – Dead time correction – Flux variation
Introduction Ø SN 1054 Typical double peaks (Abdo et al. 2010, Ge et al. 2012) Abdo et al. (2010)
Pulse profile vs energy n Ratio vs energy n P 1 P 2/P 1 P 2 bridge Kuiper et al. 2001 bridge/P 1 Ge et al. 2012
Phase-resolved spectrum Massaro 2006 Photo index evolves with energy
Phase-resolved spectrum Ge et al. 2012 Log-parabola
Flux evolution By Linli Yan Submitted to Ap. J – (2. 44± 0. 41)e-14 Wilson-Hodge et al. 2011 Crab Nebula
Crab Nebula n Spatial variation Mori et al. 2004
Pulsed spectrum n Nu. STAR profile Madsen et al. 2015
Pulsed spectrum n Nu. STAR Observation Madsen et al. 2015
Pulsed spectrum n RXTE observation Logpar model
Nu. STAR vs RXTE Nu. STAR
Pulsed spectrum n An accurate model Kuiper et al. 2001
Insight-HXMT observation Pulse profile n Timing results n Pulsed spectrum n Pulsed rate observed by Insight n
Pulse profile n ~1. 2 ms Crab pulsar LE pulse profile Mean Time Delay: ~800 us
HE Cs. I n Crab: HE Cs. I Rate ~2 cnts s-1 Exposure map Monitor Crab pulsar Calibration for Cs. I
Glitch n Giant Glitch 2017. 7 -2018. 1, by Xufang Li Hours
Pulsed spectrum Background
Dead time correction Pulsed flux After correctio
Dead time correction Dt
Relative flux ratio from HE +0. 2% After dead time correction Det. ID: 0 -11 -0. 2% Systematic error? Flux evolution? Assume: Conversion efficiency is constant
Relative flux ratio from ME&LE
Summary Ø Calibration information for Insight-HXMT Ø Flux measurement for Crab pulsar Thank you for your attention!
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