Intermediate Resolution Near-Infrared Spectroscopy of 36 late-M Dwarfs

Far-infrared continuum data from the COBE/DIRBE instrument were com- bined with Nagoya 4-m 13 CO J = 1 → 0 spectral line data to infer the multiparsec-scale physical conditions in

For each spectrogram, the name, spectral type, and evening date (YYMMDD) are shown. The 130615 data were obtained with WHT but not with lucky spectroscopy. The top spectrogram is

In the second scenario (bottom panel), the Auger electron is ejected later, when the molecule has begun to dissociate, and transfers the recoil momentum to only one of the two

Left-hand panel: two-planet fit (model B2) to the observed data with no quadratic trend removed.. Right-hand panel: periodogram of residuals to

Here we use the spectral resolution of the high- order harmonic coherent frequency comb combined with the possibility to tune the laser wavelength, as well as a weak infrared

We observed these BCDs by using PMAS integral field spectroscopy in the optical spectral range (3700–6900 Å) and mapping the brightest emission lines, hence their interstellar

Based on optical and near-infrared spectroscopy, we classify the primary NLTT 51469A as an M3 ± 1 dwarf, estimate photometrically the spectral type of its close companion NLTT 51469B

The PUMA processing architecture, with its intermediate scenario model CSM, has been shown to be effective in two ways: (a) in its power to collect and reconcile the