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New low mass ratio contact binaries in the Catalina Sky Survey

Christopoulou, Panagiota-Eleftheria and Lalounta, Eleni and Papageorgiou, Athanasios and Ferreira-Lopes, C. E. and Catelan, Márcio and Drake, Andrew J. (2022) New low mass ratio contact binaries in the Catalina Sky Survey. Monthly Notices of the Royal Astronomical Society, 512 (1). pp. 1244-1261. ISSN 0035-8711. doi:10.1093/mnras/stac534. https://resolver.caltech.edu/CaltechAUTHORS:20220503-853150300

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Abstract

We present the identification and photometric analysis of 30 new low mass ratio (LMR) totally eclipsing contact binaries found in Catalina Sky Survey data. The LMR candidates are identified using Fourier coefficients and visual inspection. We perform a detailed scan in the parameter plane of mass ratio (q) versus inclination (i) using PHOEBE -0.31 scripter to derive the best (q, i) pair for the initial models. The relative physical parameters are determined from the final model of each system. A Monte Carlo approach was adopted to derive the parameter errors. The resulting parameters confirm the identification. The approximate absolute physical parameters of the systems are estimated based on the light-curve solutions and Gaia Early Data Release 3 distances. 12 out of 30 new systems have fill-out factors f>50 per cent and q ≤ 0.25 (deep contact LMR systems), and eight of them, to within errors, are extreme LMR deep systems with q ≤ 0.1. We discuss the evolutionary status of the 30 LMR systems in comparison with the most updated catalogue of LMR systems from the literature. The scenario of the LMR systems as pre-merger candidates forming fast rotating stars is investigated for all systems, new and old, based both on Hut’s stability criteria and critical instability mass ratio (q_(inst)) relation. CSS__J075848.2+125656, with q/q_(inst) = 1.23 ± 0.23, and CSS__J093010.1−021624, with q/q_(inst) = 1.25 ± 0.23, can be considered as merger candidates.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stac534DOIArticle
https://arxiv.org/abs/2202.12835arXivDiscussion Paper
ORCID:
AuthorORCID
Christopoulou, Panagiota-Eleftheria0000-0001-6002-7625
Lalounta, Eleni0000-0001-6045-5400
Papageorgiou, Athanasios0000-0002-3039-9257
Ferreira-Lopes, C. E.0000-0002-8525-7977
Catelan, Márcio0000-0001-6003-8877
Additional Information:© 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2022 February 22. Received 2022 February 22; in original form 2021 December 20. Published: 26 February 2022. AP gratefully acknowledges the support provided by the grant cofinanced by Greece and the European Union (European Social Fund – ESF) through the Operational Programme ‘Human Resources Development, Education and Lifelong Learning’ in the context of the project ‘Reinforcement of Postdoctoral Researchers – 2nd Cycle’ (MIS-5033021), implemented by the State Scholarships Foundation (IKY). CEFL acknowledges a post-doctoral fellowship from the CNPq, MCTIC/FINEP (CT-INFRA grant 0112052700), and the Embrace Space Weather Program for the computing facilities at INPE. This work made use of data products from the CSS survey. Support for MC is provided by ANID’s Millennium Science Initiative through grant ICN12_12009, awarded to the Millennium Institute of Astrophysics (MAS), and by ANID’s Basal project FB210003. The CSS survey is funded by the National Aeronautics and Space Administration under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the US National Science Foundation under grants AST-0909182, AST-1313422, AST-1413600, and AST-1518308. We would like to thank the referee for constructive comments and recommendations that have improved the paper. Data Availability: The data underlying this paper are available in the paper and in its online supplementary material.
Funders:
Funding AgencyGrant Number
European Social FundMIS-5033021
State Scholarships FoundationUNSPECIFIED
Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)UNSPECIFIED
Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC)0112052700
Financiadora de Estudos e Projetos (FINEP)UNSPECIFIED
Millenium Science InitiativeICN12_12009
Agencia Nacional de Investigación y Desarrollo (ANID)FB210003
NASANNG05GF22G
NSFAST-0909182
NSFAST-1313422
NSFAST-1413600
NSFAST-1518308
Subject Keywords:surveys, binaries: eclipsing, binaries: close, stars: evolution, stars: fundamental parameters
Issue or Number:1
DOI:10.1093/mnras/stac534
Record Number:CaltechAUTHORS:20220503-853150300
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220503-853150300
Official Citation:Panagiota-Eleftheria Christopoulou, Eleni Lalounta, Athanasios Papageorgiou, C E Ferreira Lopes, Márcio Catelan, Andrew J Drake, New low mass ratio contact binaries in the Catalina Sky Survey, Monthly Notices of the Royal Astronomical Society, Volume 512, Issue 1, May 2022, Pages 1244–1261, https://doi.org/10.1093/mnras/stac534
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:114570
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:04 May 2022 17:57
Last Modified:04 May 2022 17:57

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