Cord serum thyrotropin and birth weight in a normal Japanese population

Mitsuda, Naomi; Tamaki, Haruo; Amino, Nobuyuki

doi:10.1093/clinchem/36.1.168a

Cited by 8 publications

(10 citation statements)

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“…Here and in what follows we adopt a simple choice for the continuum in the HETG band: a disk blackbody spectrum as implemented in the diskbb model in xspec (Mitsuda et al 1984), with a characteristic temperature kT = 1.72 keV and a normalization which is allowed to vary in order to achieve a good fit. In addition, we find that an additional harder component is needed to fit to the spectrum in the low state.…”

Section: Gaussian Fittingmentioning

confidence: 99%

Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum

Kallman

McCollough

Koljonen

et al. 2019

ApJ

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We present model fits to the X-ray line spectrum of the well known High Mass X-ray binary Cyg X-3. The primary observational dataset is a spectrum taken with the Chandra X-ray Observatory High Energy Transmission Grating (HETG) in 2006, though we compare it to all the other observations of this source taken so far by this instrument. We show that the density must be ≥ 10 12 cm −3 in the region responsible for most of the emission. We discuss the influence of the dust scattering halo on the broad band spectrum and we argue that dust scattering and extinction is not the most likely origin for the narrow feature seen near the Si K edge. We identify the features of a wind in the profiles of the strong resonance lines and we show that the wind is more apparent in the lines from the lighter elements. We argue that this wind is most likely associated with the companion star. We show that the intensities of most lines can be fitted, crudely, by a single component photoionized model. However, the iron K lines do not fit with this model. We show that the iron K line variability as a function of orbital phase is different from the lower energy lines, which indicates that the lines arise in physically distinct regions. We discuss the interpretation of these results in the context of what is known about the system and similar systems.

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Section: Gaussian Fittingmentioning

confidence: 99%

Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum

Kallman

McCollough

Koljonen

et al. 2019

ApJ

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“…The temperature of the blackbody becomes kT = 100 ± 2 eV. Fitting the data with more realistic thermal accretion disc spectrum like diskbb (Mitsuda et al 1984) or diskpn (Gierlinski et al 1999) provides a poor fit to data (χ 2 /ν = 1780/1361 and χ 2 /ν = 1782/1360 respectively) and the temperature becomes very high (kT = 155±2 eV and 159±3 eV respectively). These results would seem to reject an origin for the soft excess in terms of unmodified thermal blackbody emission.…”

Section: Spectral Analysismentioning

confidence: 99%

Discovery of Hard X-Ray Delays in the X-Ray Emission of the Seyfert 1 Galaxy Markarian 110: Possible Evidence of Comptonization

Dasgupta

Rao

2006

ApJ

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We report the discovery of hard X-ray delays in the X-ray emission of the Seyfert 1 galaxy Mrk 110, based on a long XMM-Newton observation. Cross correlation between the X-ray light curves of different energy bands reveals an energy dependent delay ranging from a few minutes to an hour. We find that the energy spectrum can be modeled by Comptonization of disk blackbody photons. The energy dependent delay can be modeled as due to the effect of Comptonization in a hot plasma confined within 10 Schwarzschild radius of the black hole. We discuss our results in the context of inverse Comptonization of the soft photons by highly energetic plasma.

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“…Single component models, such as a BB or PL (Table 1), are less appropriate than the BB plus PL, as there are larger residuals with peculiar shapes and the χ 2 are larger. Other models are also less favored: a modified disk blackbody (Stella and Rosner 1984) and the disk model of Mitsuda et al (1984) produce large residuals at low and high energies in the PCA, and have χ 2 /ν values of 3065/259 and 12345/258 respectively. A Compton scattering model (Sunyaev and Titarchuk 1980) provides a somewhat better fit, but still yields χ 2 /ν = 2758/258.…”

Section: Observations and Spectral Analysismentioning

confidence: 99%

Energy Spectra and High-Frequency Oscillations in 4U 0614+091

Ford

Kaaret

Chen

et al. 1997

The Astrophysical Journal

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We investigate the behavior of the high-frequency quasi-periodic oscillations (QPOs) in 4U 0614ϩ091, combining timing and spectral analyses of RXTE observations. The energy spectra of the source can be described by a power law (␣ 1 2.8) and a blackbody (kT 1 1.5 keV), with the blackbody accounting for 10%-20% of the total energy flux. We find a robust correlation of the frequency, , of the higher frequency QPO near 1 kHz with the flux of the blackbody, F BB . The slope of this correlation, d log ͞d log F BB , is 0.27-0.37. The source follows the same relation even in observations separated by several months. The QPO frequency does not have a similarly unique correlation with the total flux or the flux of the power-law component. The rms fraction of the higher frequency QPO rises with energy from 6.8% H 1.5% (3-5 keV) to 21.3% H 4.0% (10 -12 keV). For the lower frequency QPO, however, it is consistent with a constant value of 5.4% H 0.9%. The results may be interpreted in terms of a beat-frequency model for the production of the high-frequency QPOs.

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Cord serum thyrotropin and birth weight in a normal Japanese population

Cited by 8 publications

References 0 publications

Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum

Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum

Discovery of Hard X-Ray Delays in the X-Ray Emission of the Seyfert 1 Galaxy Markarian 110: Possible Evidence of Comptonization

Energy Spectra and High-Frequency Oscillations in 4U 0614+091

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