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Data & statistics on Spectral energy distribution with spectral lines – 30373 results
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Residuals of the spectral energy distribution of Ton 34 after subtracting our absorbed continuum Model iv from BK07. The different spectral segments have been color-coded as follows, SWP: red, LWP orange, HST-FOS: blue, and Palomar: dark green. Color-coded fiducial marks indicate the position of observed or expected (labeled with symbol “?”) emission lines. Measurements of line intensities and upper ...

Residuals of the spectral energy distribution of Ton 34 after subtracting our absorbed continuum Model iv from BK07. The different spectral segments have been color-coded as follows, SWP: red, LWP ...

www.astroscu.unam.mx/~binette/ton34_shock

of 2000 Å, the two distributions are the same. This is because nanodiamond dust ...
Si iv λ1400, and Lyα show a clear asymmetry in the line profile, with a blue shoulder (see Fig. 2). For these lines, we included a third, broader Gaussian. The FWHM

Dec 2007 | Instituto de Astronomía UNAM
Original Url: http://www.astroscu.unam.mx/~binette/ton34_shock
Spectral energy distribution of the prompt emission. KonusWind spectra and ‘Pi of the Sky’ flux density in three 10-s time intervals centred at T0 1 3 s (green), T0 1 17 s (blue) and T0 1 32 s (red). (Detailed time intervals and c-ray spectral parameters are given in Supplementary Table 1.) The high-energy data points are from Konus-Wind, and the solid line shows the best-fit Band function50 for each ...
47 more results from this site ▶

Spectral energy distribution of the prompt emission. KonusWind spectra and ‘Pi of the Sky’ flux density in three 10-s time intervals centred at T0 1 3 s (green), T0 1 17 s (blue) and T0 1 32 s (red ...

www.physics.unlv.edu/~bzhang/racusin08.pdf

synchrotron energy. This would imply a third spectral component arising from second-order ...
radiation mechanisms must dominate in each spectral regime. The most natural ...
as the ratio of the inverse Compton to synchrotron energy losses, is Y , nFn(Ep)/nFn(Ep, syn

Jan 2008 | UNLV Department of Physics and Astronomy – 47 more results from this site
Original Url: http://www.physics.unlv.edu/~bzhang/racusin08.pdf
Low energy spectral index distribution from Ghirlanda et al. (2002). The vertical lines represent the limits of the emission models reported in Table 1 and plotted in Fig. 2. The triangles represent the maximum values found from the spectral analysis of the bursts presented in this work along with their 90% confidence interval (horizontal bars). The gray histogram shows the distribution of the low energy ...
1178 more results from this site ▶

Low energy spectral index distribution from Ghirlanda et al. (2002). The vertical lines represent the limits of the emission models reported in Table 1 and plotted in Fig. 2. The triangles represent ...

www.aanda.org/index.php?option=com_article&access=standard&Itemid=129&url=/articles/aa/pdf/2003/30/aa3251.pdf

and that The distribution of the low energy photon spectral index α obtained from the time resolved ...
E indicates the photon energy. The high energy spectral component can be described in most ...
2002) have a low energy power law spectral index −3/2 ≤ α ≤ −2/3, i.e. within

Jan 2002 | Astronomy & Astrophysics – 1178 more results from this site
Original Url: http://www.aanda.org/index.php?option=com_article&access=standard&Itemid=129&url=/articles/aa/pdf/2003/30/aa3251.pdf
Spectral energy distributions of the models with T = 2800 K; log (g [cm/s2 ]) = −0.65; M = 2 M ; Z = Z ; C/O = 1.4 (blue solid line) and T = 2800 K; log (g [cm/s2 ]) = −0.70; M = 2 M ; Z = Z ; C/O = 1.1 (red dotted line). The upper panel shows the wavelength region up to 60 µm, the lower panel shows the visible spectral range and the near infrared up to 2 µm in more detail.

Spectral energy distributions of the models with T = 2800 K; log (g [cm/s2 ]) = −0.65; M = 2 M ; Z = Z ; C/O = 1.4 (blue solid line) and T = 2800 K; log (g [cm/s2 ]) = −0.70; M = 2 M ; Z = Z ; C/O = 1 ...

othes.univie.ac.at/1627/1/2008-10-13_9940129.pdf

1 x 1 0 [e rg /s ] ν ν. F 1 x 1 0 1 x 1 0 T = 2 8 0 0 K ; M = 2 M ; Z = 1 Z ; C /O = 1 , 4 ( s o lid ) ; lo g ( g [c m /s ]) = - 0 .6 5 ] [d y n /c m g a s lo g p ...
1 x 1 0 1 x 1 0 1 x 1 0 1 x 1 0 1 x 1 0 1 x 1 0 [e rg /s ] ν ν. F T=2800K; log (g [cm/s ])=-0.65; M=2M ; Z=1Z ; C/O=1.4 2 T=2800K; log (g [cm/s ])=-0.70; M=2M ; Z=1Z ; C/O=1.1 2 wavelength [Å] 1 2 0 0 0 ...
region

Oct 2008 | Hochschulschriften-Service - E-Theses
Original Url: http://othes.univie.ac.at/1627/1/2008-10-13_9940129.pdf
Observed spectral energy distributions at two different epochs (both after the temporal break). The optical fluxes have been corrected for the Galactic extinction. The solid lines are the best fit power law models find at each epoch, where α is the best fit spectral index. The dashed lines define the expected range of values at 90% confidence level.

Observed spectral energy distributions at two different epochs (both after the temporal break). The optical fluxes have been corrected for the Galactic extinction. The solid lines are the best fit power ...

www.pa.iasf.cnr.it/~cusumano/refereed/2007AA.474.827S.pdf

these observational aspects by extracting an optical-toX-ray spectral energy distribution (SED ...
is well described by a simple power law with spectral index αopt, X, 1 = 0.5±0.1. The latter is consistent with the spectral index we find from the X-ray analysis based

Oct 2007 | IASF Palermo (formerly IFCAI)
Original Url: http://www.pa.iasf.cnr.it/~cusumano/refereed/2007AA.474.827S.pdf
Spectral energy distribution for the nucleus of NGC 4565 (see Table 3). The solid and dotted lines are the spectral energy distributions for the nuclei of NGC 4579 and M81 from Ho (1999), respectively. For the purpose of comparison, the curves have been shifted downward by À1.0 and À1.5, respectively. Upper limits are indicated by points with arrows (see x 3.3.3).

Spectral energy distribution for the nucleus of NGC 4565 (see Table 3). The solid and dotted lines are the spectral energy distributions for the nuclei of NGC 4579 and M81 from Ho (1999), respectively ...

batc.bao.ac.cn/papers/BATC-papers/2002ApJ576xue.pdf

in the bulge. All these data are presented in Table 3, and the spectral energy distribution ...
the spectral energy distribution for the low-luminosity active galactic nucleus in M81 ...
The resemblance of the spectral energy distribution for the nucleus of NGC 4565 with those

Jan 1999 | BATC
Original Url: http://batc.bao.ac.cn/papers/BATC-papers/2002ApJ576xue.pdf
Left: Spectral energy distribution of HL Tau from about 350 m to 6 cm wavelength. The solid line fits the short wavelengths (thermal emission by dust) and the dashed line fits the long wavelengths (free-free emission from ionized gas). The long-wavelength spectral index of the dust is 2.9, meaning that 0.9 with no corrections for optically thick emission (Wilner et al. 1996). Right: Distribution of ’s ...

Left: Spectral energy distribution of HL Tau from about 350 m to 6 cm wavelength. The solid line fits the short wavelengths (thermal emission by dust) and the dashed line fits the long wavelengths (free ...

www.uapress.arizona.edu/onlinebks/PPIV/chap20.pdf

of the disks contribute to the spectral energy distribution at long wavelengths. It ...
Fig. 4 shows the distribution of emissivity exponents, , determined from the observed spectral slope of disk emission near 1 mm. Many of the disks in this sample

Jan 1996 | The University of Arizona Press
Original Url: http://www.uapress.arizona.edu/onlinebks/PPIV/chap20.pdf
A) Spectral distribution at x = 0.75D, for S = 0.42, 0.71, 0.88, 1, 1.05, shown by solid lines. Experiments were repeated independently at S = 0.43, 0.5, 0.72, 0.9, 1.05, shown by dashed lines. (b) The impulsive increase of the spectral energy versus swirl number S shows the appearance of Hopf bifurcations at Sk1 and Sk2 for modes m = +1 and +2.

A) Spectral distribution at x = 0.75D, for S = 0.42, 0.71, 0.88, 1, 1.05, shown by solid lines. Experiments were repeated independently at S = 0.43, 0.5, 0.72, 0.9, 1.05, shown by dashed lines. (b) ...

ae-www.usc.edu/bio/tmax/publications/JFM525;115-159.pdf

The spectral energy distribution at the axial location x = 0.75D is shown ...
of the spectral energy of modes m = +1 and +2 is plotted in figure 14(b) by a square ...
of spectral energy versus the swirl number reveals that the saturation amplitude

Feb 2005 | USC Aerospace & Mechanical Engineering : AM
Original Url: http://ae-www.usc.edu/bio/tmax/publications/JFM525;115-159.pdf
Solid line: Spectral energy distribution, 8mm-7-mm MP studio carbons at 37 volts, 40 amperes. Dotted line: Spectral energy distribution, ...

Solid line: Spectral energy distribution, 8mm-7-mm MP studio carbons at 37 volts, 40 amperes. Dotted line: Spectral energy distribution, ...

www.mole.com/aboutus/history/smpte/1943-06p333.html

FIG. 13. Solid line: Spectral energy distribution, 8mm-7-mm MP studio carbons at 37 volts, 40 amperes. Dotted line: Spectral energy distribution, solar radiation at sea level.

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Spectral energy distribution of the Crab Nebula renormalized to the total phase interval. The fit of the synchrotron (purple dashed line) and IC (blue dash-dotted line) are represented separately with two power laws. The black curve is the best fit obtained with the sum of these two power laws. The LAT spectral points are obtained using the model-independent maximum likelihood method described in Section ...
60 more results from this site ▶

Spectral energy distribution of the Crab Nebula renormalized to the total phase interval. The fit of the synchrotron (purple dashed line) and IC (blue dash-dotted line) are represented separately with ...

people.roma2.infn.it/~glast/A185.Fermi.Crab.Pulsar.apj.pdf

component using the LAT data only. Figure 6. Spectral energy distribution of the Crab ...
spectral points at high energy indicate a lower flux in comparison to EGRET. However, it ...
The EGRET spectral points are represented on the same plot. As in the case

Jan 2001 | main – 60 more results from this site
Original Url: http://people.roma2.infn.it/~glast/A185.Fermi.Crab.Pulsar.apj.pdf
Related searches: quasars spectral energy distribution, spectral energy distribution deduced from the hst and nir, spectral energy distributions versus luminosity, spectral energy distribution of an spherically symmetric infalling envelope, multi spectral energy distribution

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