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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
cmdbs.dat 23 900 CMD diagram towards θ Musca
cmdgn.dat 24 900 CMD diagram towards γ Normae
cmdgs.dat 23 900 CMD diagram towards γ Scuti
cmdtm.dat 23 900 CMD diagram towards β Scuti
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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
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Bytes Format Units Label Explanations
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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)
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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.
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Acknowledgements:
Marc Moniez, moniez(at)lal.in2p3.fr
(End) Patricia Vannier [CDS] 01-Apr-2009