Ultra-low Amplitude Variables in the LMC -- Classical Cepheids, Pop. II Cepheids, RV Tau Stars and Binary Variables

TL;DR

This study identifies ultra-low amplitude variable stars near the Cepheid instability strip in the LMC, revealing new pulsating and binary candidates with potential implications for stellar evolution understanding.

Contribution

First comprehensive search for ultra-low amplitude variables in the LMC using MACHO and OGLE data, uncovering new pulsating and binary candidates near the Cepheid instability strip.

Findings

25 singly periodic and 4 multiply periodic ULA objects identified.

ULA objects cluster near the pulsational instability strips of LMC variables.

Some ULA variables follow parallel period-magnitude relations, suggesting different evolutionary stages.

Abstract

A search for variable stars with ultra-low amplitudes (ULA), in the millimag range, has been made in the combined MACHO and OGLE data bases in the broad vicinity of the Cepheid instability strip in the HR diagram. A total of 25 singly periodic and 4 multiply periodic ULA objects has been uncovered. Our analysis does not allow us to distinguish between pulsational and ellipsoidal (binary) variability, nor between LMC and foreground objects. However, the objects are strongly clustered and appear to be associated with the pulsational instability strips of LMC Pop. I and II variables. When combined with the ULA variables of Buchler et al (2005) a total of 20 objects fall close to the classical Cepheid instability strip. However, they appear to fall on parallel period-magnitude relations that are shifted to slightly higher magnitude which would confer them a different evolutionary status. Low amplitude RV Tauri and Pop. II Cepheids have been uncovered that do not appear in the MACHO or OGLE catalogs. Interestingly, a set of binaries seem to lie on a PM relation that is essentially parallel to that of the RV Tauri/Pop. II Cepheids.