TY - JOUR
T1 - The POINT-AGAPE survey - I. The variable stars in M31
AU - An, J.H.
AU - Evans, N.W.
AU - Hewett, P.
AU - Baillon, P.
AU - Novati, S.C.
AU - Carr, B.J.
AU - Creze, M.
AU - Giraud-Heraud, Y.
AU - Gould, A.
AU - Jetzer, P.
AU - Kaplan, J.
AU - Kerins, E.
AU - Paulin-Henriksson, S.
AU - Smartt, Stephen
AU - Stalin, C.S.
AU - Tsapras, Y.
PY - 2004/7/1
Y1 - 2004/7/1
N2 - For the purposes of identifying microlensing events, the POINT-AGAPE collaboration has been monitoring the Andromeda galaxy (M31) for three seasons (1999-2001) with the Wide Field Camera on the Isaac Newton Telescope. In each season, data are taken for one hour per night for roughly 60 nights during the six months that M31 is visible. The two 33 x 33 arcmin(2) fields of view straddle the central bulge, northwards and southwards. We have calculated the locations, periods and brightness of 35 414 variable stars in M31 as a by-product of the microlensing search. The variables are classified according to their period and brightness. Rough correspondences with classical types of variable star (such as Population I and II Cepheids, Miras and semiregular long-period variables) are established. The spatial distribution of Population I Cepheids is clearly associated with the spiral arms, while the central concentration of the Miras and long-period variables varies noticeably, the brighter and the shorter period Miras being much more centrally concentrated.
AB - For the purposes of identifying microlensing events, the POINT-AGAPE collaboration has been monitoring the Andromeda galaxy (M31) for three seasons (1999-2001) with the Wide Field Camera on the Isaac Newton Telescope. In each season, data are taken for one hour per night for roughly 60 nights during the six months that M31 is visible. The two 33 x 33 arcmin(2) fields of view straddle the central bulge, northwards and southwards. We have calculated the locations, periods and brightness of 35 414 variable stars in M31 as a by-product of the microlensing search. The variables are classified according to their period and brightness. Rough correspondences with classical types of variable star (such as Population I and II Cepheids, Miras and semiregular long-period variables) are established. The spatial distribution of Population I Cepheids is clearly associated with the spiral arms, while the central concentration of the Miras and long-period variables varies noticeably, the brighter and the shorter period Miras being much more centrally concentrated.
U2 - 10.1111/j.1365-2966.2004.07853.x
DO - 10.1111/j.1365-2966.2004.07853.x
M3 - Article
SN - 0035-8711
VL - 351
SP - 1071
EP - 1098
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -