The η Car Campaign with UVES at the ESO VLT I. The dataset and a first look

Details The η Car Campaign with UVES at the ESO VLT I. The dataset and a first look The η Car Campaign with UVES at the ESO VLT I. The dataset and a first look

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..332..160w&link_type=abstract

The Fate of the Most Massive Stars, ASP Conference Series, Vol. 332, Proceedings of the conference held 23-28 May, 2004 in Grand

Astronomy and Astrophysics

Astronomy

2

Scientific paper

All observations were carried out in service observing mode between December 2002 and November 2003 with UVES at ESO's VLT UT2 (Kueyen) on Cerro Paranal, Chile. The program ID's are : 70.D-0607(A), 71.D-168(A), 72.D-052(A); the Principle Investigator K. Weis.
For all observations the standard settings DIC1, 346+580 (blue arm centered at 3460 Å, red arm at 5800 Å) and DIC2, 437+860 (blue arm centered at 4370 Å red arm at 8600 Å) were used. The observed wavelength range extends continuously from 3 100 Å to 10 200 Å except for small gaps due to the space between the two CCDs of the detector mosaic at the red channel. The primary objective was to observe the reflected stellar spectrum at the FOS4 position (about 2.6 arcsec south and 2.8 arcsec east of the star) in the Homunculus. One short and one long exposure was secured with the DIC1 (346+580 setting) to record both the extremely bright Hα emission and the fainter lines with good signal-to-noise ratio. The slit width of all observations was 0.3 arcsec and 0.4 arcsec in the red and blue range, respectively, resulting in a spectral resolution of 80 000 in the red and 110 000 in the blue arm. The pixel scales and slit lengths were, respectively, 0.246 arcsec/pixel and 7.6 arcsec in the blue and 0.182 arcsec/pixel and 11.8 arcsec in the red arm. To monitor the 2003 event, spectra were taken about every week during the event (mid May to end of July) and every month before and after the event time. No spectra could be taken between mid August and late November due to the very low elevation of η Car at Paranal during this time. The July 26 spectrum shows the minimum intensities of the changing highly excited lines, such as He I 6678 Å and therefore resembles the best ``event-spectrum''. This favors a differential light travel time of four weeks from the star to FOS4 (assuming a global disappearance of these lines).

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