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J/A+A/434/1201      ESO VLTI Calibrators Program             (Richichi+, 2005)

First results from the ESO VLTI Calibrators Program. Richichi A., Percheron I. <Astron. Astrophys. 434, 1201 (2005)> =2005A&A...434.1201R
ADC_Keywords: Stars, diameters ; Interferometry Keywords: techniques: high angular resolution - techniques: interferometric - catalogs - stars: fundamental parameters Abstract: The ESO Very Large Telescope Interferometer (VLTI) is one of the leading interferometric facilities. It is equiped with several 8.2 and 1.8m telescopes, a large number of baselines up to 200m, and with several subsystems designed to enable high quality measurements and to improve significantly the limits of sensitivities currently available to long-baseline interferometry. For this, a large number of observations of potential calibrators have been obtained during the commissioning phase of the VLTI. These data are publicly available. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 230 191 Candidate VLTI calibrators
See also: J/A+A/393/183 : Catalogue of calibrator stars for LBSI (Borde+, 2002) J/A+A/431/773 : CHARM2, an updated (Richichi+, 2005) Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Name used in the VLTI system 11- 12 A2 --- --- [HD] 14- 19 I6 --- HD HD number 21- 23 A3 --- --- [SAO] 25- 30 I6 --- SAO ? SAO number 32- 42 A11 --- OName Other name 44- 62 A19 --- OName2 Other name 64- 65 I2 h RAh Right ascension (J2000) 67- 68 I2 min RAm Right ascension (J2000) 70- 74 F5.2 s RAs Right ascension (J2000) 76 A1 --- DE- Declination sign (J2000) 77- 78 I2 deg DEd Declination (J2000) 80- 81 I2 arcmin DEm Declination (J2000) 83- 86 F4.1 arcsec DEs Declination (J2000) 88- 95 F8.5 arcsec/yr pmRA Proper motion in right ascension 97-104 F8.5 arcsec/yr pmDE Proper motion in declination 106-109 F4.2 mag Vmag ? V magnitude 111-115 F5.2 mag Kmag K magnitude 117-130 A14 --- SpType MK spectral Type 131-135 F5.2 mas Diam Angular diameter 137-140 F4.2 mas e_Diam ? rms uncertainty on Diam 142-162 A21 --- r_Diam Reference for angular diameter (1) 164-166 I3 --- E0-G0 Number of observations in E0-G0 (16.0m) (2) 168-170 I3 --- E0-G1 Number of observations in E0-G1 (66.0m) (2) 172-173 I2 --- U1-U3 Number of observations in U1-U3 (102.4m) (2) 175 I1 --- U1-U2 Number of observations in U1-U2 (56.6m) (2) 177 I1 --- U1-U4 Number of observations in U1-U4 (130.2m) (2) 179-180 I2 --- U2-U3 Number of observations in U2-U3 (46.6m) (2) 182 I1 --- U2-U4 Number of observations in U2-U4 (89.4m) (2) 184-186 I3 --- U3-U4 Number of observations in U3-U4 (62.4m) (2) 188-190 I3 --- M0-B3 Number of observations in M0-B3 (139.7m) (2) 192-193 I2 --- B3-C3 Number of observations in B3-C3 (8.0m) (2) 195-197 I3 --- B3-D1 Number of observations in B3-D1 (24.0m) (2) 199-200 I2 --- D0-H0 Number of observations in D0-H0 (64.0m) (2) 202-204 I3 --- Nobs Total number of observations 206-207 I2 --- Nbase Total number of baselines used
Note (1): References for the available diameters: Borde = Borde et al., 2002, Cat. J/A+A/393/183 CHARM2 = Richichi et al., 2005, Cat. J/A+A/431/773 MIDI = T. Verhoelst, priv. comm. Note (2): Number of observations (OBs) on the specified VLTI baselines, processed by the pipeline and validated according to the criteria (flags) described in the paper.
Acknowledgements: Andrea Richichi, arichich(at)eso.or
(End) Patricia Vannier [CDS] 27-Jan-2005
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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