Akiko Kawamura

A DETAILED STUDY OF NON-THERMAL X-RAY PROPERTIES AND INTERSTELLAR GAS TOWARD THE γ-RAY SUPERNOVA REMNANT RX J1713.7–3946

We have carried out a spectral analysis of the Suzaku X-ray data in the 0.4-12xa0keV range toward the shell-type very high-energy γ-ray supernova remnant (SNR) RX J1713.7–3946. The aims of this analysis are to estimate detailed X-rays spectral properties at a high angular resolution up to 2 arcmin and to compare them with the interstellar gas. The X-ray spectrum is non-thermal and used to calculate absorbing column density, photon index, and absorption-corrected X-ray flux. The photon index varies significantly from 2.1 to 2.9. It is shown that the X-ray intensity is well correlated with the photon index, especially in the west region, with a correlation coefficient of 0.81. The X-ray intensity tends to increase with the averaged interstellar gas density while the dispersion is relatively large. The hardest spectra, with photon indexes of less than 2.4, are found outside of the central 10 arcmin of the SNR, from the north to the southeast (~430 arcmin2) and from the southwest to the northwest (~150 arcmin2). The former region shows low interstellar gas density, while the latter shows high interstellar gas density. We present a discussion of possible scenarios that explain the distribution of the photon index and its relationship with the interstellar gas.

Molecular Clouds as Cosmic-Ray Barometers

The advent of high sensitivity, high resolution � -ray detectors, together with a knowledge of the distribution of the atomic hydrogen and especially of the molecular hydrogen in the Galaxy on a subdegree scale, creates a unique opportunity to explore the flux of cosmic rays in the Galaxy. We here present the new data on the distribution of the molecular hydrogen from a large region of the inner Galaxy obtained by the NANTEN Collaboration. We then introduce a methodology which aims to provide a test bed for current and future � -ray observatories to explore the cosmic-ray flux at various positions in our Galaxy. In particular, for a distribution of molecular clouds, as provided by the NANTEN survey, and local cosmic-ray density as measured at the Earth, we estimate the expected GeV to TeV � -ray signal, which can then be compared with observations, and use to test the cosmic-ray flux.

A Detailed Study of the Interstellar Protons toward the TeV γ-Ray SNR RX J0852.0–4622 (G266.2–1.2, Vela Jr.): The Third Case of the γ-Ray and ISM Spatial Correspondence

We present a new analysis of the interstellar protons toward the TeV

Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud - I. N159W

gamma

Dense molecular gas at 12 mm towards Galactic TeV gamma-ray sources

-ray SNR RX J0852.0

ALMA Reveals Molecular Cloud N55 in the Large Magellanic Cloud as a Site of Massive Star Formation

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Molecular Clouds Associated with the Type Ia SNR N103B in the Large Magellanic Cloud

4622 (G266.2

The ALMA Science Archive

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Detailed distributions of the CO J = (2 − 1)/J = (1 − 0) intensity ratios toward a large area of the central molecular zone

1.2, Vela Jr.). We used the NANTEN2

Evidence for triggered star formation in the Carina Flare supershell

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