The first MAXI/SSC catalog of X-ray sources in 0.7–7.0 keV

Tomida, H.; Uchida, D.; Tsunemi, H.; Imatani, R.; Kimura, Masashi; Nakahira, S.; Hanayama, T.; Yoshidome, K.

doi:10.1093/pasj/psw006

Cited by 8 publications

(8 citation statements)

References 23 publications

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“…Below, we collectively call all the other components as backgrounds, and try to construct a method to estimate and remove them. This makes a big difference from studies of point sources, in which the background can be estimated from surrounding sky regions (Hiroi et al 2013;Tomida et al 2016).…”

Section: Ssc Backgroundsmentioning

confidence: 99%

MAXI/SSC all-sky maps from 0.7 keV to 4 keV

Nakahira

Tsunemi

Tomida

et al. 2020

Publications of the Astronomical Society of Japan

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By accumulating data from the Solid-state Slit Camera (SSC) on board the MAXI mission for 2 years from 2009 to 2011, diffuse X-ray background maps were obtained in energies of 0.7-1.0, 1.0-2.0, and 2.0-4.0 keV. They are the first ones that were derived with a solid-state instrument, and to be compared with the previous ROSAT all sky survey result. While the SSC map in the highest energy band is dominated by point sources and the Galactic Diffuse X-ray emission, that in 0.7-1.0 keV reveals an extended X-ray structure, of which the brightness distribution is very similar to that observed with ROSAT about 20 years before. Like in the ROSAT result, the emission is dominated by a bright arc-like structure, which appears to be a part of a circle of ∼ 50 • radius centered at about (l, b) ∼ (340 • , 15 • ). In addition, the SSC map suggests a fainter and larger ellipse, which is elongated in the north-south direction and roughly centered at the Galactic center. The spectrum of these structures is explained as thin thermal emission from a plasma, with a temperature of ∼ 0.31 keV and an abundance of ∼ 0.3 Solar. Based on SSC observation conditions including the low Solar activity, the Solar Wind Charge Exchange signals are estimated to be negligible in the present SSC maps, as well as in the > 0.56 keV ROSAT map. A brief discussion is given to the obtained results.Key words: key word1 -key word2 -. . . -key wordn

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Section: Ssc Backgroundsmentioning

confidence: 99%

MAXI/SSC all-sky maps from 0.7 keV to 4 keV

Nakahira

Tsunemi

Tomida

et al. 2020

Publications of the Astronomical Society of Japan

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“…Figure 11 shows that Cygnus Loop is still producing nonthermal X-ray emission thanks to the residual component of non confined electrons. Such flux is much smaller than the detected Xray emission, estimated to be 56.9 × 10 −11 erg s −1 cm −2 in the [0.7-1.85] keV interval (Tomida et al 2016) which is, however, compatible with being of purely thermal origin. In this work we do not attempt to model the thermal emission because it requires to account for the different chemical abundances to fit the X-ray lines, and goes beyond our aims.…”

Section: Cygnus Loop Propertiesmentioning

confidence: 61%

New high-frequency radio observations of the Cygnus Loop supernova remnant with the Italian radio telescopes

Loru,

Pellizzoni,

Egron

et al. 2020

Preprint

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Supernova remnants (SNRs) represent a powerful laboratory to study the Cosmic-Ray acceleration processes at the shocks, and their relation to the properties of the circumstellar medium. With the aim of studying the high-frequency radio emission and investigating the energy distribution of accelerated electrons and the magnetic field conditions, we performed single-dish observations of the large and complex Cygnus Loop SNR from 7.0 to 24.8 GHz with the Medicina and the Sardinia Radio Telescope, focusing on the northern filament (NGC 6992) and the southern shell. Both regions show a spectrum well fitted by a power-law function (S ∝ ν −α ), with spectral index α = 0.45 ± 0.05 for NGC 6992 and α = 0.49 ± 0.01 for the southern shell and without any indication of a spectral break. The spectra are significantly flatter than the whole Cygnus Loop spectrum (α = 0.54 ± 0.01), suggesting a departure from the plain shock acceleration mechanisms, which for NGC6992 could be related to the ongoing transition towards a radiative shock. We model the integrated spectrum of the whole SNR considering the evolution of the maximum energy and magnetic field amplification. Through the radio spectral parameters, we infer a magnetic field at the shock of 10 µG. This value is compatible with a pure adiabatic compression of the interstellar magnetic field, suggesting that the amplification process is currently inefficient.

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“…For these sources, Ref. [94] did not mention the flux in either the soft or the hard energy band, and thus we were unable to infer the normalization and spectral index using our method outlined above. We expect that these sources will have a negligible contribution to the background counts.…”

Section: B Velocity Spectroscopy Using Simulationsmentioning

confidence: 99%

“…In order to understand the impact of point sources in our fields of view, we use the MAXI/ SSC catalog [94]. The catalog gives the time averaged flux of Xray sources in the energy range 0.7 -7 keV separated into two energy bands: soft (0.7 -1.85 keV) and hard (1.85 -7 keV).…”

Section: Synthetic Observation By Micro-xmentioning

confidence: 99%

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Doppler effect on indirect detection of dark matter using dark matter only simulations

Powell

Laha

et al. 2017

Phys. Rev. D

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Indirect detection of dark matter is a major avenue for discovery. However, baryonic backgrounds are diverse enough to mimic many possible signatures of dark matter. In this work, we study the newly proposed technique of dark matter velocity spectroscopy [1]. The non-rotating dark matter halo and the Solar motion produce a distinct longitudinal dependence of the signal which is opposite in direction to that produced by baryons. Using collisionless dark matter only simulations of Milky Way like halos, we show that this new signature is robust and holds great promise. We develop mock observations by high energy resolution X-ray spectrometer on a sounding rocket, the Micro-X experiment, to our test case, the 3.5 keV line. We show that by using six different pointings, Micro-X can exclude a constant line energy over various longitudes at ≥ 3σ. The halo triaxiality is an important effect and it will typically reduce the significance of this signal. We emphasize that this new smoking gun in motion signature of dark matter is general, and is applicable to any dark matter candidate which produces a sharp photon feature in annihilation or decay. *

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The first MAXI/SSC catalog of X-ray sources in 0.7–7.0 keV

Cited by 8 publications

References 23 publications

MAXI/SSC all-sky maps from 0.7 keV to 4 keV

MAXI/SSC all-sky maps from 0.7 keV to 4 keV

New high-frequency radio observations of the Cygnus Loop supernova remnant with the Italian radio telescopes

Doppler effect on indirect detection of dark matter using dark matter only simulations

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