2009A&A...508.1073M


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.30CEST19:01:32

2009A&A...508.1073M - Astronomy and Astrophysics, volume 508, 1073-1083 (2009/12-3)

VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance.

MOURARD D., CLAUSSE J.M., MARCOTTO A., PERRAUT K., TALLON-BOSC I., BERIO Ph., BLAZIT A., BONNEAU D., BOSIO S., BRESSON Y., CHESNEAU O., DELAA O., HENAULT F., HUGHES Y., LAGARDE S., MERLIN G., ROUSSEL A., SPANG A., STEE P., TALLON M., ANTONELLI P., FOY R., KERVELLA P., PETROV R., THIEBAUT E., VAKILI F., McALISTER H., TEN BRUMMELAAR T., STURMANN J., STURMANN L., TURNER N., FARRINGTON C. and GOLDFINGER P.J.

Abstract (from CDS):

Among optical stellar interferometers, the CHARA Array located at Mt Wilson in California offers the potential of very long baselines (up to 330m) and the prospect of coupling multiple beam combiners. This paper presents the principle and the measured performance of VEGA, Visible spEctroGraph and polArimeter installed in September 2007 at the coherent focus of the array. With 0.3ms of arc of spatial resolution and up to 30000 of spectral resolution, VEGA intends to measure fundamental parameters of stars, to study stellar activities and to image and analyze circumstellar environments. We describe the observing modes that have been implemented for this spectro-polarimeter and show actual performances measured on the sky during the first observing runs. The astrophysical programs are described in relation to the observing modes of the instrument, the presentation of the spectrograph and of the interface table is shown and finally the data is presented. We discuss the perspectives of further development in the framework of the CHARA Array. We show that VEGA/CHARA is fully operational. The current limiting magnitude is nearly 7 but the results depend on the observing conditions (seeing, spectral resolution, etc.). We have validated the stability of the instrumental visibility at the level of 1 to 2% over half an hour and of the instrumental polarization for various declinations. Some examples of squared visibility and differential visibility are presented. The spectro-polarimeter VEGA has been installed and successfully tested on CHARA. It will permit stellar physics studies at unprecedented spectral and spatial resolutions.

Abstract Copyright:

Journal keyword(s): instrumentation: high angular resolution - instrumentation: interferometers

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * zet Cas Pu* 00 36 58.2841866 +53 53 48.867311 2.58 3.47 3.66 3.74 3.95 B2IV 421 0
2 * g Per * 02 02 18.1108126001 +54 29 15.154292739 4.64 4.96 5.04 5.01 5.06 B8III 93 0
3 * psi Per Be* 03 36 29.3798227 +48 11 33.478941 3.60 4.17 4.23     B5Ve 396 0
4 * omi Her Be* 18 07 32.5507266 +28 45 44.967843 3.74 3.802 3.827     B9.5III 142 0
5 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2516 0
6 * gam Lyr * 18 58 56.6224137 +32 41 22.400295 3.140 3.200 3.250 3.27 3.28 B9III 266 0
7 * iot Cyg PM* 19 29 42.3587204 +51 43 47.205830   3.899 3.755     A5V 123 0
8 * tet Cep SB* 20 29 34.8651841062 +62 59 38.621587534 4.58 4.42 4.22 4.05 3.96 A7III 144 0
9 * alf Cyg sg* 20 41 25.91514 +45 16 49.2197 1.11 1.34 1.25 1.14 1.04 A2Ia 718 0

    Equat.    Gal    SGal    Ecl

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2020.09.30-19:01:32

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