Mid-IR period-magnitude relations for AGB stars

Details Mid-IR period-magnitude relations for AGB stars Mid-IR period-magnitude relations for AGB stars

2009-01-20

arxiv.org/abs/0901.3032v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

5 pages, 4 figures

Scientific paper

10.1111/j.1745-3933.2009.00628.x

Asymptotic Giant Branch variables are found to obey period-luminosity relations in the mid-IR similar to those seen at K_S (2.14 microns), even at 24 microns where emission from circumstellar dust is expected to be dominant. Their loci in the M, logP diagrams are essentially the same for the LMC and for NGC6522 in spite of different ages and metallicities. There is no systematic trend of slope with wavelength. The offsets of the apparent magnitude vs. logP relations imply a difference between the two fields of 3.8 in distance modulus. The colours of the variables confirm that a principal period with log P > 1.75 is a necessary condition for detectable mass-loss. At the longest observed wavelength, 24 microns, many semi-regular variables have dust shells comparable in luminosity to those around Miras. There is a clear bifurcation in LMC colour-magnitude diagrams involving 24 micron magnitudes.

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