# PSR J1907+0602: A Radio-Faint Gamma-Ray Pulsar Powering a Bright TeV Pulsar Wind Nebula

**Authors:**  Fermi LAT Collaboration, the Fermi Pulsar Timing Consortium,  :, A. A. Abdo  
**arXiv:** [1001.0792](https://arxiv.org/abs/1001.0792)  
**Date:** 2010-01-06  
**Summary page:** https://www.summarizepaper.com/en/paper/1001.0792v1/

## Key points

- Comprehensive multiwavelength analysis of the 106.6 ms gamma-ray pulsar PSR J1907+06 near TeV source MGRO J1908+06
- Pulsed gamma-ray emission observed from 100 MeV to above 10 GeV with a power-law index of approximately 1.76 ± 0.05 and an exponential cutoff energy at E_{c} = 3.6 ± 0.5 GeV
- Radio observations detect faint radio pulsations with a flux density of approximately 3.4 microJy at 1.5 GHz and a dispersion measure DM = 82.1 ± 1.1 cm^{-3}pc, indicating a distance of about 3.2 ± 0.6 kpc
- X-ray observations reveal an absorbed compact X-ray source with non-thermal emission and a flux of (2..3^{+0..6}_{-1..4}) x10^{-14} erg cm^{-2} s^{-1}
- Distance to PSR J1907+06 aligns with that of supernova remnant G40..5-0..5 and S74 molecular cloud, potential birth sites for the system

## Summary

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 and the  present a comprehensive multiwavelength analysis of the 106.6 ms gamma-ray pulsar PSR J1907+06, located near the TeV source MGRO J1908+06. Through timing observations with Fermi, the precise position of the pulsar is determined to be R.A. = 19h07m547(2), decl. = +06:02:16(2). This places it firmly within the extent of the TeV source, suggesting that it is likely the pulsar wind nebula associated with PSR J1907+0602. The study reveals pulsed gamma-ray emission across a wide energy range, from 100 MeV to above 10 GeV. The phase-averaged power-law index in the energy range E > 0.1 GeV is approximately 1.76 ± 0.05, with an exponential cutoff energy at E_{c} = 3.6 ± 0.5 GeV. Detailed energy-dependent gamma-ray pulsed light curves are presented, along with constraints on off-pulse emission linked to the TeV source. Radio observations using the Arecibo telescope detect very faint radio pulsations from PSR J1907+06, with a flux density of approximately 3.4 microJy at 1.5 GHz and a dispersion measure DM = 82.1 ± 1.1 cm^{-3}pc indicating a distance of about 3.2 ± 0.6 kpc and a pseudo-luminosity of L_{1400} around ~0.035 mJy kpc^2. X-ray observations from Chandra ACIS reveal an absorbed compact X-ray source at R.A.=19h07m54.76, decl.=+06:02:14.6 within significant non-thermal emission and a flux of (2..3^{+0..6}_{-1..4}) x10^{-14} erg cm^{-2} s^{-1}. Upper limits on arcminute scale X-ray emissions are also established based on archival ASCA data. The implied distance to PSR J1907+06 aligns with that of supernova remnant G40..5-0..5 located opposite to the TeV nebula from PSR J1907+0602 and S74 molecular cloud situated closer, which are considered as potential birth sites for this intriguing system.