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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Gerin 2J. They trace the gas physical conditions, e.

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Two positions are observed: The spectra and the Gaussian fits are shown as black histograms and green curves, respectively. Roueff 3M. Services Articles citing this article CrossRef Displayed integrated intensities are expressed in the main beam temperature scale. Irak on key gas-phase progenitors of these molecules sheds light on this problem.

NORMA IRAM 3549 Mangas.pdf

We only consider the most stable isomers to compare the measured and modeled abundances. The legend at the bottom of the figure presents the line coding for the curves: Laboratory spectroscopy is underway to confirm these results. Bardeau 1A.

Sievers 5F. Simple hydrocarbon molecules, such as C 2 H, C kram H, and C 3 H 2 have been detected in a wide variety of sources from diffuse e.

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Previous article Next article. This led us to conclude that the species is a reactive molecule with a spatial distribution similar to small hydrocarbon chains. Metrics Show article metrics.

Data correspond to usage on the plateform after The illuminating star is positioned at the right of the plots. Carretera de Ajalvir, Km 4.

Molecular ions play an important role in the physics and chemistry of the insterstellar medium. Indeed, the modeled and predicted abundances of c-C 3 H 2 are consistent, while the modeled abundance of C 2 H is still one order of magnitude lower than the measured abundance cf.

This is due to a combination of two effects. Le Petit 3J. 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.

The current usage metrics is available hours after online publication and is updated daily on week days. This assumption enables a quick fit convergence when we start the fit with the following initial values: Le Bourlot 3A. We used the Ohio State University osu pure gas-phase chemical network upgraded for photochemical studies. Pure gas-phase chemistry models do not succeed in reproducing the measured abundances of small hydrocarbons in the interstellar medium. Gratier 144536. Lines simultaneously observed in the cut displayed in Fig.

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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. Column densities and abundances with respect to the number of protons, i.

Current usage metrics About 4356 metrics Return to article. Summary Acknowledgments References Appendix Idam Initial download of the metrics may take a while. Goicoechea 4S. Contour levels are shown in the grey-scale lookup tables.

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 green lines are Gaussian fits. Belloche 6 and D. List of tables List of figures.

Janssen, Meudon Cedex, France e-mail: We wish to know to which development order we can significantly fit the frequency model to the observed data. We therefore assume that the eight lines have the same line width.

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. This is likely for two reasons.