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J/A+A/500/1027  EROS CMD towards 4 Galactic spiral arms fields    (Rahal+, 2009)

The EROS2 search for microlensing events towards the spiral arms: the complete seven season results. Rahal Y.R., Afonso C., Albert J.-N., Andersen J., Ansari R., Aubourg E., Bareyre P., Beaulieu J.-P., Charlot X., Couchot F., Coutures C., Derue F., Ferlet R., Fouque P., Glicenstein J.-F., Goldman B., Gould A., Graff D., Gros M., Haissinski J., Hamadache C., de Kat J., Lesquoy E., Loup C., Le Guillou L., Magneville C., Mansoux B., Marquette J.-B., Maurice E., Maury A., Milsztajn A., Moniez M., Palanque-Delabrouille N., Perdereau O., Rahvar S., Rich J., Spiro M., Tisserand P., Vidal-Madjar A., The EROS-2 collaboration <Astron. Astrophys. 500, 1027 (2009)> =2009A&A...500.1027R
ADC_Keywords: Surveys ; Stars, variable ; Photometry, UBVRI Keywords: cosmology: dark matter - Galaxy: disk - Galaxy: bulge - Galaxy: structure - Galaxy: spiral arms - Galaxy: microlensing Abstract: The EROS-2 project has been designed to search for microlensing events towards any dense stellar field. The densest parts of the Galactic spiral arms have been monitored to maximize the microlensing signal expected from the stars of the Galactic disk and bulge. 12.9 million stars have been monitored during 7 seasons towards 4 directions in the Galactic plane, away from the Galactic center. Description: EROS Colour-magnitude diagrams towards 4 fields of the Galactic spiral arms in the domain: 0.<(Vj-Ic)<6. 13.<Ic<22. The stellar density is represented in the colour-magnitude plane as a 2D histogram with a sampling of 0.2 in colour and 0.3 in magnitude. Uncertainties: - A systematic uncertainty of 5.3% (common to all bins) is due to the uncertainty on the effectively monitored field. - The statistical uncertainty for each bin can be deduced from the normalization factor used to obtain the diagrams from the original observations. The content of a given bin divided by this normalisation factor A is an integer that corresponds to the original count. This number follows a Poissonian statistics, which should be used to estimate statistical uncertainties. This normalisation factor A depends on the field: cmdtm (θ Musca): A = 194.9318 cmdgn (γ Normae): A = 97.46588 cmdgs (γ Scuti): A = 233.9181 cmdbs (β Scuti): A = 194.9318 File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file cmdbs.dat 24 900 CMD diagram towards θ Musca cmdgn.dat 24 900 CMD diagram towards γ Normae cmdgs.dat 24 900 CMD diagram towards γ Scuti cmdtm.dat 24 900 CMD diagram towards β Scuti
See also: J/ApJ/631/906 : MACHO Galactic Bulge microlensing events (Thomas+, 2005) J/A+A/454/185 : EROS-2 microlensing parameters (Hamadache+, 2006) J/A+A/466/157 : Bulge Microlensing Events (Soto+, 2007) Byte-by-byte Description of file: cmdbs.dat cmdgn.dat cmdgs.dat cmdtm.dat
Bytes Format Units Label Explanations
2- 4 F3.1 mag V-Ic Central value of the (Vj-Ic) bin (1) 7- 11 F5.2 mag Icmag Central value of the Ic bin 13- 24 F12.5 deg-2.mag-2 w Stellar density (2)
Note (1): V_J is the Johnson V magnitude, I_C is the Cousins I magnitude Note (2): The density is the number density of stars per square degree, per unit of magnitude and per unit of color index.
Acknowledgements: Marc Moniez, moniez(at)lal.in2p3.fr
(End) Patricia Vannier [CDS] 01-Apr-2009
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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