Mode identification based on time-series spectrophotometry for the bright rapid sdB pulsator EC 01541−1409^⋆,⋆⋆

¹ ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
e-mail: srandall@eso.org
² Département de Physique, Université de Montréal, CP 6128, Succ. Centre-Ville, Montréal QC H3C 3J7, Canada
³ Institut d’Astrophysique et de Géophysique de l’Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
⁴ Chargé de recherches, Fonds de la Recherche Scientifique, FNRS, rue d’Egmont 5, 1000 Bruxelles, Belgium

Received: 6 December 2013
Accepted: 28 January 2014

Abstract

We present an analysis of time-resolved spectrophotometry gathered with FORS/VLT for the rapidly pulsating hot B subdwarf EC 01541−1409 with the aim of identifying the degree index ℓ of the larger amplitude modes. This mode identification can be extremely useful in detailed searches for viable asteroseismic models in parameter space, and can be crucial for testing the validity of a solution a posteriori. To achieve it, we exploit the ℓ-dependence of the monochromatic amplitude, phase, and velocity-to-amplitude ratio of a mode as a function of wavelength. We use the ℓ-sensitive phase lag between the flux perturbation and the radial velocity as an additional diagnostic tool. On this basis, we are able to unambiguously identify the dominant 140.5 s pulsation of our target as a radial mode, and the second-highest amplitude periodicity at 145.8 s as an ℓ = 2 mode. We further exploit the exceptionally high-sensitivity data that we gathered for the dominant mode to infer modal properties that are usually quite difficult to estimate in sdB pulsators, namely the physical values of the dimensionless radius, temperature, and surface gravity perturbations.