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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We therefore assume that the eight lines have the same line width. Goicoechea 4S. 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 assumption enables a quick fit convergence when we start the fit with the following initial values: 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.

Janssen, Meudon Cedex, France e-mail: Gratier 1V. Current usage metrics About article metrics Return to article.

The spectra and the Gaussian fits are shown as black histograms and green curves, respectively. Molecular ions play an important role in the physics and chemistry of the insterstellar medium. Services Articles citing this article CrossRef Two positions are observed: 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.

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This is likely for two uram.

Simple hydrocarbon molecules, such as C 2 H, C 3 H, and C 3 H 2 have been detected in a wide variety of sources from diffuse e. They trace the gas physical conditions, e. List of tables List of figures. 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. Data correspond to usage on the plateform after Summary Acknowledgments References Appendix A: The legend at the bottom of the figure presents the line coding for the curves: Pure gas-phase chemistry models do not succeed in reproducing the measured abundances of small hydrocarbons in the interstellar medium.

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Contour levels are shown in the grey-scale lookup tables. Metrics Show article metrics. The green lines are Gaussian fits. Displayed integrated intensities are expressed in the main beam temperature scale. Bardeau 1A.

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.

Belloche 6 and D.

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We wish to know to which development order we can significantly fit the frequency model to the observed data. The illuminating star is positioned at the right of the plots.


Laboratory spectroscopy is underway to confirm these results. Roueff 3M. We only consider the most stable isomers to compare the measured and modeled abundances. Information on key gas-phase progenitors of these molecules sheds light on this problem. This is due to a combination of two effects. Igam used the Ohio State University osu pure gas-phase chemical network upgraded for photochemical studies. This led us to conclude that the species is a reactive molecule with a spatial distribution similar to small hydrocarbon chains.

Gerin 2J. Carretera de Ajalvir, Km 4.

NORMA IRAM 3549 Mangas.pdf

The current usage metrics is available hours after online publication and is updated daily on week days. Initial download of the metrics may take a while. Column densities and abundances with respect to the number of protons, i. Previous article Next article. Lines simultaneously observed in the cut displayed in Fig. Sievers 5F. Le Bourlot 3A.