(DOI: will be inserted by hand later) VLTI/AMBER and VLTI/MIDI spectro-interferometric observations of the B[e] supergiant CPD−57 ◦ 2874?

(DOI: will be inserted by hand later)

Aims. We have used mid-infrared long-baseline interferometry to resolve the circumstellar material around the Herbig Ae star HR 5999, providing the first direct measurement of its angular size, and to derive constraints on the spatial distribution of the dust. Methods. MIDI at the VLTI was used

Summary. We present interferometric observations of the Be star 51 Ophiuchi. These observations were obtained during the science demonstration phase of the MIDI instrument at the Very Large Telescope Interferometer (VLTI). Using MIDI, a Michelson 2 beam combiner that operates at the N band (8 to 13

spatial resolution of the circumstellar environment of classical Be stars. We used the VLTI/MIDI instrument with baselines up to 130 m to obtain an angular resolution of about 15 mas in the N band and compared our results with previous K band measurements obtained with the VLTI/AMBER instrument and

Summary. We studied the geometry of the inner (AU-scale) circumstellar environment around the Herbig Be star MWC 147. Combining, for the first time, near-(NIR, K band) and mid-infrared (MIR, N band) spectro-interferometry on a Herbig star, our VLTI/MIDI and AMBER data constrain not only

Summary. We present the results of the first mid-infrared interferometric observations of the Mira variable RR Sco with the VLTI/MIDI, together with K-band observations using VLTI/VINCI. The uniform-disk diameter was found to be 18 mas between 8 and 10 μm, while it gradually increases

Calibration of MIDI, the Mid-infrared Interferometer for the VLTI MIDI is the MID-infrared Interferometric Instrument at the Very Large Telescope Interferometer (VLTI). It will perform long-baseline stellar interferometry in the N band (8... 13�m). In the run-up of setting up MIDI, some preparatory

We report on observations of circumstellar disks around young stars that have been obtained with the MIDI instrument, which is mounted on the VLT Interferometer and operates in the 10µm atmospheric window. The maximum spatial resolution of 5 milli-arcsec corresponds to sub-AU scales at the distance

This investigation focuses on observational measurements of the differential interferometric phase between spectral channels in the VLTI/MIDI instrument. Measurements of target stars are compared with theoretical predictions in order to investigate the effects of dispersion in humid air