An, Hongjun10; Madsen, Kristin K.11; Reynolds, Stephen P.12; Kaspi, Victoria M.10; Harrison, Fiona A.11; Boggs, Steven E.13; Christensen, Finn Erland1; Craig, William W.13; Fryer, Chris L.14; Grefenstette, Brian W.11; Hailey, Charles J.15; Mori, Kaya15; Stern, Daniel11; Zhang, William W.16
1 National Space Institute, Technical University of Denmark2 Astrophysics, National Space Institute, Technical University of Denmark3 McGill University4 California Institute of Technology5 North Carolina State University6 University of California at Berkeley7 Los Alamos National Laboratory8 Columbia University9 NASA Goddard Space Flight Center10 McGill University11 California Institute of Technology12 North Carolina State University13 University of California at Berkeley14 Los Alamos National Laboratory15 Columbia University16 NASA Goddard Space Flight Center
We present the first images of the pulsar wind nebula (PWN) MSH 15−52 in the hard X-ray band (8 keV), as measured with the Nuclear Spectroscopic Telescope Array (NuSTAR). Overall, the morphology of the PWN as measured by NuSTAR in the 3–7 keV band is similar to that seen in Chandra high-resolution imaging. However, the spatial extent decreases with energy, which we attribute to synchrotron energy losses as the particles move away from the shock. The hard-band maps show a relative deficit of counts in the northern region toward the RCW 89 thermal remnant, with significant asymmetry.We find that the integrated PWN spectra measured with NuSTAR and Chandra suggest that there is a spectral break at 6 keV, which may be explained by a break in the synchrotron-emitting electron distribution at ∼200 TeV and/or imperfect cross calibration. We also measure spatially resolved spectra, showing that the spectrum of the PWN softens away from the central pulsar B1509−58, and that there exists a roughly sinusoidal variation of spectral hardness in the azimuthal direction. We discuss the results using particle flow models.We find non-monotonic structure in the variation with distance of spectral hardness within 50 of the pulsar moving in the jet direction, which may imply particle and magnetic-field compression by magnetic hoop stress as previously suggested for this source. We also present two-dimensional maps of spectral parameters and find an interesting shell-like structure in the NH map.We discuss possible origins of the shell-like structure and their implications.