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Using the powerful Heterodyne Receiver Array (HERA) on the IRAM m telescope (9 beams, 2 polarizations, NGC NGC NGC NGC – – – LDS – – – – 3 21 23, – – – 2 6 2 6 IRAM. from wastewater by maghemite nanoparticles. Water Research, , 39(18): – Iram M, Guo C, Guan Yet al. Adsorption and magnetic removal of.

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Norma Iram Iso 9712

Indeed, the modeled and predicted abundances of c-C 3 H 2 are consistent, while the modeled abundance of 456 2 H is still one order of magnitude lower than the measured abundance cf. Molecular ions play an important role in the physics and chemistry of the insterstellar medium. Roueff 3M. The current usage metrics is available hours after online publication and is updated daily on week days. Laboratory spectroscopy is underway to confirm these results.

We wish to know to which development order we can significantly fit the frequency model to the observed data.

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Lines simultaneously observed in the cut displayed in Fig. Kram article Next article. This led us to conclude that the species is a reactive molecule with a spatial distribution similar to small hydrocarbon chains. Two positions are observed: We aim to constrain the chemical content of the Horsehead mane with a millimeter unbiased line survey at two positions, namely the photo-dissociation region PDR and the nearby shielded core.

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Belloche 6 and D.

Contour levels are shown in the grey-scale lookup tables. Current usage metrics About article metrics Return to article. Summary Acknowledgments References Appendix A: Carretera de Ajalvir, Km 4. Information on key gas-phase progenitors of these molecules sheds light on this problem. We therefore assume that the eight lines have the same line width.

List of tables List of figures. We used the Ohio State Ira osu pure gas-phase jram network upgraded for photochemical studies.

This assumption enables a quick fit convergence when we start the fit with the following initial values: Services Articles citing this article CrossRef The measured abundances are typically one and two orders of magnitude higher than the modeled abundances for C 2 H and C 3 H 2. Sievers 5F. Goicoechea 4S. The green lines are Gaussian fits. Simple hydrocarbon molecules, such as C 2 H, C 3 H, and C 3 H 2 have been detected in a wide 436 of sources from diffuse e.

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The legend at the bottom of the figure presents the line coding for the curves: Bardeau 1A. We only consider the most stable isomers to compare the measured and modeled abundances. Gerin 2J. Pure gas-phase chemistry models do not succeed in reproducing the measured abundances of small hydrocarbons in the interstellar medium. The illuminating star is positioned at the right of the plots.

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Le Petit 3J. Column densities and abundances with respect to the number of protons, i. To compute the spectroscopic parameters associated with the set of unidentified lines, we used higher order improvements to the simple model of a linear rotor. The spectra and the Gaussian fits are shown as black iarm and green curves, respectively. Displayed integrated intensities are expressed in the main beam temperature scale.

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The left column presents the profiles computed by the code, which samples the UV-illuminated gas on a finer spatial grid than the UV-shielded gas to correctly represent the steep physical and chemical gradients. Initial iran of the metrics may take a while. Janssen, Meudon Cedex, France e-mail: They trace the gas physical conditions, e.

Le Bourlot 3A.

Data correspond to usage on the plateform after Metrics Show article metrics. This iramm likely for two reasons. This is due to a combination of two effects. Gratier 1V.