Multi-wavelength Study of HESS J1741-302

We present the results of two Chandra X-ray Observatory (Chandra) observations of TeV γ-ray source HESS J1741-302. We investigate whether there is any connection between HESS J1741-302 and the sources seen at lower energies. One of the brightest X-ray sources in the HESS J1741-302 field, CXOU J174112.1-302908, appears to be associated with a low-mass star (possibly representing a quiescent low-mass X-ray binary or cataclysmic variable (CV)), hence, it is unlikely to be a source of TeV γ-rays. In the same field we have potentially detected X-rays from WR 98a, which is likely to be a colliding wind binary with massive stars. No TeV emission has been reported so far from such systems although predictions have been made. Finally, we found that the previously reported Suzaku source, Suzaku J1740.5-3014 (which is not covered by the Chandra observations), appears to be a hard X-ray source detected by INTERGAL ISGRI, which supports the magnetized CV classification but makes its association with the TeV emission unlikely. The young pulsar PSR B1737-30, so far undetected in X-rays and projected on the sky near the CV, may be the contributor of relativistic particles responsible for the TeV emission. Read more here.

Spitzer (Fadda et al. 2006) image (8.0 μm) of the HESS region. The green and magenta squares represent the Chandra and Suzaku observations, respectively (with the corresponding ObsIDs on top). The yellow circles show the locations and extension of the two bright regions within the HESS source (smaller circle: J1741A, larger circle: J1741B). The three pulsars (PSR B1737−30, PSR J1741−3016, and PSR J1739−3023) are shown with filled white circles.

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