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Astrophysics Source Code Library

Making codes discoverable since 1999

Searching for codes credited to 'Moya, A.'

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[ascl:2504.002] PBjam: Automating asteroseismology of solar-like oscillators
Nielsen, M. B.; Davies, G. R.; Ball, W. H.; Lyttle, A. J.; Li, T.; Hall, O. J.; Chaplin, W. J.; Gaulme, P.; Carboneau, L.; Ong, J. M. J.; García, R. A.; Mosser, B.; Roxburgh, I. W.; Corsaro, E.; Benomar, O.; Moya, A.; Lund, M. N.; Hatt, E.; Jones, B. P.; Logue, M.

PBjam analyzes the oscillation spectra of solar-like oscillators. The code performs two main tasks: identifying a set of modes of interest in a spectrum of oscillations, and accurately modeling those modes to measure their frequencies. Mode identification relies on a large set of previous observations of the model parameters, which are then used to construct a prior distribution to inform the sampling. PJjam models the modes using a nested sampling or MCMC algorithm, where Lorentzian profiles are fit to each of the identified modes.

[ascl:2506.004] TESS-cont: TESS contamination tool
Castro-González, A.; Lillo-Box, J.; Armstrong, D. J.; Acuña, L.; Aguichine, A.; Bourrier, V.; Gandhi, S.; Sousa, S. G.; Delgado-Mena, E.; Moya, A.; Adibekyan, V.; Correia, A. C. M.; Barrado, D.; Damasso, M.; Winn, J. N.; Santos, N. C.; Barkaoui, K.; Barros, S. C. C.; Benkhaldoun, Z.; Bouchy, F.; Briceño, C.; Caldwell, D. A.; Collins, K. A.; Essack, Z.; Ghachoui, M.; Gillon, M.; Hounsell, R.; Jehin, E.; Jenkins, J. M.; Keniger, M. A. F.; Law, N.; Mann, A. W.; Nielsen, L. D.; Pozuelos, F. J.; Schanche, N.; Seager, S.; Tan, T. -G.; Timmermans, M.; Villaseñor, J.; Watkins, C. N.; Ziegler, C.

TESS-cont quantifies the flux fraction coming from nearby stars in the TESS photometric aperture of any observed target. The package identifies the main contaminant Gaia DR2/DR3 sources, quantifies their individual and total flux contributions to the aperture, and determines whether any of these stars could be the origin of the observed transit and variability signals. Written in Python, TESS-cont is based on building the pixel response functions (PRFs) of nearby Gaia sources and computing their flux distributions across the TESS Target Pixel Files (TPFs) or Full Frame Images (FFIs).