Open AccessRed variables in the OGLE‐II data base – III. Constraints on the three‐dimensional structures of the Large and Small Magellanic Clouds
Author(s) -
Lah P.,
Kiss L. L.,
Bedding T. R.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society: letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.067
H-Index - 122
eISSN - 1745-3933
pISSN - 1745-3925
DOI - 10.1111/j.1745-3933.2005.00033.x
Subject(s) - red clump , physics , astrophysics , large magellanic cloud , distance modulus , red giant branch , stars , line (geometry) , astronomy , population , photometry (optics) , metallicity , geometry , mathematics , demography , sociology
We present an analysis of the 3D structure of the Magellanic Clouds, using period–luminosity (P–L) relations of pulsating red giants in the OGLE‐II sample. By interpreting deviations from the mean P–L relations as distance modulus variations, we examine the 3D distributions of the sample. The results for the Large Magellanic Cloud, based solely on stars below the tip of the Red Giant Branch (LMC), confirm previous results on the inclined and possibly warped bar of the LMC. The depth variation across the OGLE‐II field is about 2.4 kpc, interpreted as the distance range of a thin but inclined structure. The inclination angle is about 29°. A comparison with OGLE‐II red clump distances revealed intriguing differences that seem to be connected to the red clump reddening correction. A spatially variable red clump population in the LMC can explain the deviations, which may have a broader impact on our understanding of the LMC formation history. For the Small Magellanic Cloud, we find a complex structure showing patchy distribution scattered within 3.2 kpc of the mean. However, the larger range of the overall depth on every line‐of‐sight is likely to smooth out significantly the real variations.