J/A+A/500/1027  EROS CMD towards 4 Galactic spiral arms fields    (Rahal+, 2009)
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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
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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 ({theta} Musca):  A = 194.9318
     cmdgn ({gamma} Normae): A =  97.46588
     cmdgs ({gamma} Scuti):  A = 233.9181
     cmdbs ({beta} 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 {theta} Musca
cmdgn.dat      24      900   CMD diagram towards {gamma} Normae
cmdgs.dat      23      900   CMD diagram towards {gamma} Scuti
cmdtm.dat      23      900   CMD diagram towards {beta} 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
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(End)                                        Patricia Vannier [CDS]  01-Apr-2009