INVESTIGADORES
PIATTI Andres Eduardo
congresos y reuniones científicas
Título:
A New Giant Branch Clump Structure Towards the Large Magellanic Cloud
Autor/es:
PIATTI, ANDRÉS E.; GEISLER, DOUG; BICA, EDUARDO; CLARIA OLMEDO, JUAN JOSÉ; SANTOS JR, JOÂO F.C.; SARAJEDINI, A.; DOTTORI, HORACIO
Lugar:
Estados Unidos
Reunión:
Congreso; 194th Meeting of the American Astronomical Society; 1999
Resumen:
We present Washington C,T_1 CCD photometry of 21 fields located in the
northern part of the Large Magellanic Cloud (LMC), and spread over a
region of nearly 2({Box }({o})) ( ~ 6(o) from the bar). The surveyed
areas were chosen on the basis of the presence of a secondary giant
clump in the CMDs of the fields of SL 388 and SL 509, observationally
detected by Bica et al., 1998, AJ 116, 723. From the collected data we
found that most of the observed field CMDs do not show a separate
secondary clump, but rather a vertical structure (VS). The VS also
appears in the field of NGC 2209 ( ~ 10(o) far away), but it is
negligible in the remaining observed cluster fields. Its position and
size are nearly the same throughout the surveyed regions: it lies below
the Main Giant Clump (MGC) and extends from the bottom of the MGC to ~
0.45 mag fainter, spanning the bluest color range of the MGC. Moreover,
VS stars are uniformly distributed in their corresponding fields. In two
fields, as well as in the NGC 2209 field, the MGC is slightly tilted,
following approximately the reddening vector, while the VS maintains its
verticality. Finally, assuming that there is roughly the same number of
MGC stars in each field, we found that the number of stars in the box
defined by Delta (C-T_1)=1.44-1.53 mag and Delta T_1=18.8-19.7 mag has a
strong spatial variation, reaching the highest VS star density just East
of SL 509. Further studies are required in order to determine whether
the VS is caused by the presence of an old stellar population or by an
evolutionary effect as predicted by the theoretical models of Girardi et
al. 1998 MNRAS 301, 723, or even by a layer of stars located behind the
LMC.