K-Shell Line Distribution of Heavy Elements along the Galactic Plane Observed with Suzaku

Uchiyama, Hideki; Nobukawa, Masayoshi; Tsuru, Takeshi Go; Koyama, K.

doi:10.1093/pasj/65.1.19

Cited by 101 publications

(208 citation statements)

References 51 publications

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“…The derived temperature value is higher than that estimated by various studies of the Galactic Ridge Emission using X-rays (e.g., Yuasa et al 2012;Yamauchi et al 2014;Uchiyama et al 2013;Nobukawa et al 2016), however, within uncertainties it is consistent with that of the low temperature component of the Galactic Ridge Emission derive by e.g., Yuasa et al (2012) and Uchiyama et al (2013). We find that the properties of the VRNEI models in these fits are comparable to those in the VRNEI+POWERLAW fits (see Table 1).…”

Section: Spectral Analysissupporting

confidence: 84%

“…As discussed in more detail in Section 2.2, we find that we can produce quite a good fit (reduced χ 2 = 0.96) to our X-ray spectrum with the temperature of the APEC model ∼ 1.9 keV. While this value is much lower than 6 keV derived in previous studies (Kaneda et al 1997;Ebisawa et al 2005;Ryu et al 2009), it is comparable to the softer, coronal X-ray source contribution of the high temperature component of the GRXE derived by Yuasa et al (2012), or the low temperature component of the GRXE derived by Uchiyama et al (2013).…”

Section: Nature Of the Hard X-ray Tail Componentsupporting

confidence: 75%

“…Kaneda et al (1997) showed that in the 0.5-10.0 keV energy range, the GRXE is best described by an opticallythin thermal plasma model with a low and high temperature component of ∼1.0 keV and ∼6 keV respectively. This was later confirmed using Chandra (e.g., Ebisawa et al 2005) and Suzaku (e.g., Ryu et al 2009;Yuasa et al 2012;Uchiyama et al 2013). Yuasa et al (2012) attempted to decompose the high energy (∼6 keV) component of the GRXE into its various discrete source contributions.…”

Section: Nature Of the Hard X-ray Tail Componentmentioning

confidence: 92%

“…Second, we fit the global X-ray spectrum using an absorbed VRNEI plus a APEC model in which we fix the temperature, and abundance parameters derived by Kaneda et al (1997) or Uchiyama et al (2013) for the the GRXE. Again, we find that this produces a similar result (χ 2 r = 0.99) compared to our model listed in Table 1 and 2.…”

Section: Nature Of the Hard X-ray Tail Componentmentioning

confidence: 99%

See 3 more Smart Citations

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

Auchettl

Wong

et al. 2017

ApJ

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We present an X-ray imaging and spectroscopic study of the molecular cloud interacting mixedmorphology (MM) supernova remnant (SNR) G346.6-0.2 using XMM-Newton. The X-ray spectrum of the remnant is well described by a recombining plasma that most likely arises from adiabatic cooling, and has sub-solar abundances of Mg, Si, and S. Our fits also suggest the presence of either an additional power-law component with a photon index of ∼2, or an additional thermal component with a temperature of ∼2.0 keV. We investigate the possible origin of this component and suggest that it could arise from either the Galactic ridge X-ray emission, an unidentified pulsar wind nebula or Xray synchrotron emission from high-energy particles accelerated at the shock. However, deeper, high resolution observations of this object are needed to shed light on the presence and origin of this feature. Based on its morphology, its Galactic latitude, the density of the surrounding environment and its association with a dense molecular cloud, G346.6-0.2 most likely arises from a massive progenitor that underwent core-collapse.

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Section: Spectral Analysissupporting

confidence: 84%

Section: Nature Of the Hard X-ray Tail Componentsupporting

confidence: 75%

Section: Nature Of the Hard X-ray Tail Componentmentioning

confidence: 92%

Section: Nature Of the Hard X-ray Tail Componentmentioning

confidence: 99%

See 2 more Smart Citations

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

Auchettl

Wong

et al. 2017

ApJ

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“…They assumed that the spectrum of radioemitting electrons could be extrapolated into the region 100 keV -1 GeV, and just the electrons with E < 1 GeV ionized the GC molecular gas with the rate ζ ∼ (1−3)×10 −15 s −1 ; this about the value derived by (see Oka et al, 2005). Then the question is whether these electrons can provide the diffuse 6.4 keV emission in the GC as observed by Uchiyama et al (2012).…”

Section: Ionization By Cr Electrons In the Intercloud Medium Stationmentioning

confidence: 94%

On the origin of the 6.4keV line in the Galactic Center region

Dogiel

Chernyshov

Kiselev

et al. 2014

Astroparticle Physics

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We analyse the 6.4 keV iron line component produced in the Galactic Center (GC) region by cosmic rays in dense molecular clouds (MCs) and in the diffuse molecular gas. We showed that this component, in principle, can be seen in several years in the direction of the cloud Srg B2. If this emission is produced by low energy CRs which ionize the interstellar molecular gas the intensity of the line is quite small, < 1%. However, we cannot exclude that local sources of CRs or X-ray photons nearby the cloud may provide much higher intensity of the line from there. Production of the line emission from molecular clouds depends strongly on processes of CR penetration into them. We show that turbulent motions of neutral gas may generate strong magnetic fluctuations in the clouds which prevent free penetration of CRs into the clouds from outside. We provide a special analysis of the line production by high energy electrons. We concluded that these electrons hardly provide the diffuse 6.4 keV line emission from the GC because their density is depleted by ionization losses. We do not exclude that local sources of electrons may provide an excesses of the 6.4 keV line emission in some molecular clouds and even reproduce a relatively short time variations of the iron line emission. However, we doubt whether a single electron source provides the simultaneous short time variability of the iron line emission from clouds which are distant from each other on hundred pc as observed for the GC clouds. An alternative speculation is that local electron sources could also provide the necessary effect of the line variations in different clouds that are seen simultaneously by chance that seems, however, very unlikely.

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Discovery of new X-ray sources near the unidentified gamma-ray source HESS J1841-055

Nobukawa

Tsuru

et al. 2015

Advances in Space Research

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HESS J1841−055 is a diffuse unidentified gamma-ray source with the size of ∼ 1.3 • × 1 • . No conclusive counterpart in other wavelengths has so far detected. To search for X-rays responsible for the TeV emission, the Suzaku observations were conducted, which covered a half region of the HESS source. In the soft band (0.5-2.0 keV), we discovered a diffuse emission, Suzaku J1840.2−0552, with the size of ∼ 10 ′ . Since its spectrum was fitted by an optically thin thermal plasma model, Suzaku J1840.2−0552 is likely to be a supernova remnant. We also discovered an extended source, Suzaku J1840.2−0544, in the hard band (2.0-8.0 keV) with an emission line at 6.1 keV. From the spectral feature and large interstellar absorption, this source is likely to be a cluster of galaxies behind the Galactic plane at the red-shift of ∼0.09. The other diffuse source spatially overlaps with the SNR candidate G26.6−0.2, which shows a non-thermal dominant spectrum. Since no other candidate is found in the hard X-ray band, we infer that these largely extended sources could be possible counterparts of HESS J1841−055.

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K-Shell Line Distribution of Heavy Elements along the Galactic Plane Observed with Suzaku

Cited by 101 publications

References 51 publications

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

On the origin of the 6.4keV line in the Galactic Center region

Discovery of new X-ray sources near the unidentified gamma-ray source HESS J1841-055

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