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High Resolution Spectroscopy with the VLT Summary of Experimental
Scientific Requirements for HighResolution Spectroscopy with the VLT
Why High Spectral Resolution Even at Low SignalNoise?
27 other sections not shown
absorption lines abundance adaptive optics AGB stars aperture array Astron astronomical Astrophys atmospheric beam camera chromospheric circumstellar collimated combined focus components coude cross-disperser detected detector diameter disk dispersion echelle grating echelle spectrometer efficiency elements emission lines equivalent widths European Southern Observatory Fe/H fibre Figure Fourier galactic galaxies high resolution spectroscopy high spectral resolution i i i i increase infrared instrument interferogram interstellar interstellar medium isotopic large telescopes limited line profiles Magellanic Clouds Maillard main sequence measured microns mirror molecular molecules mosaic Nasmyth noise objects observations Observatory obtained Pallavicini parameters photometric photospheric pixels possible postdisperser quasars radial velocity red giants region resolving power rotation S/N ratio sensitivity shows signal-to-noise slit solar sources spatial resolution spectral coverage spectral lines spectral range spectral resolution spectrometer spectrum stellar surface temperature thermal wavefront wavelength