The figure below shows what stellar spectra are like in this wavelength range. All stars hotter than about 3000 K effective temperature radiate like a hot blackbody at these long wavelengths, possibly with a very few atomic lines (of Hydrogen, in the A-type stars) or molecular bands (the CO band overtone near 2.25 microns for example, in K-type stars and G-type stars). ... unusual features: mixed chemistry sources, Wolf-Rayet stars, ice bands, featureless carbon-star spectra ...

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

... Observatory . ... Science . ... Science Users Information > Data Handling and Products > Data Reduction FAQ > My data shows an extended, bright feature - what can this be? ... Observing Facilities . ... Observing with ESO Telescopes . ... Science Data Products Forum . ... ESO Data . ... You might also want to check http://www.eso.org/sci/observing/PublicSurveys/useful_links/OmegaCAM_images.html where we provide a collection of example OmegaCAM images, illustrating some special data features. ...

... A concrete application is displayed step by step by the command: TUTORIAL/CLOUD . The data used for this example are CaII absorption features observed in the spectrum of SN 1986g in NGC 5128 (observer: S. d'Odorico, instrument: CASPEC). ... Sampling is 0.05? per pixel and the measured instrumental resolution, 17km/s. The final cloud model consists of 12 absorption doublets. The corresponding image includes both components K and H and has been convolved by a gaussian PSF of 0.22? (17km/s) FWHM. ...

... A detailed study of two consecutive bright points observed simultaneously with CDS, EIT and MDI is presented. The analysis of the evolution of the photospheric magnetic features and their coronal counterpart shows that there is a linear dependence between the EIT Fe XII 195? flux and the total magnetic flux of the photospheric bipolarity. ... In a follow-up study, we used wide slit (90arcsec240arcsec) movies of four EIT coronal bright points (BPs) obtained with CDS. ...

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