Long-period variables in the Magellanic Clouds

Abstract

Surveys for long-period variables in the MagellanicWith the advent of the IRAS satellite, many point sources were found in the Magellanic Clouds. Some of the most luminous optically visible LPVs (including objects found on I plates) were detected by IRAS, but many of the IRAS point sources have no optical counterparts. The colours of some of these IRAS sources indicate that they may be variable OH/IR stars, and a number of them have been monitored in the near infrared (JHK); some variable sources have been found by Whitelock et al (1989) in the SMC and by Wood et al (1990) in the LMC and SMC. Infrared photometryTo derive useful quantities such as M bo j and T e ff (estimates), infrared JHK photometry is required for the LPVs. Such photometry can be found in papers by Glass

Field Mycology

“…m 05 offset of the PG3 Miras translates with the theoretical period-colour relation from Wood et al (1991; assuming comparable masses between the PG3 & the field versus the LMC Miras) in a mean metallicity of the PG3 and field Miras ∼ 1.4 times as high as the LMC.…”

“…The period-colour relation for the PG3 Miras was found to be shifted significantly from the Large Magellanic Cloud (LMC) relation (Feast et al 1989). With the theoretical relation from Wood et al (1991) it was concluded that this must be due to metallicity, which could be about 1.6 times larger for the PG3 Miras (Bl92). Feast (1996) obtained similar results for the Miras in the galactic bulge versus those in the LMC.…”