Unveiling the nature of HE 0107–5240: a long period binary CEMP-no star with [Fe/H] of –5.56

Context . The vast majority of the most iron-poor stars in the Galaxy exhibit strong carbon enhancement, with C/H ratios about two orders of magnitude below solar. This unusual chemical composition likely reflects the properties of the gas cloud from which these stars formed, having been enriched by one, or at most a few, supernovae. A remarkable member of this stellar class, HE 0107 −5240 with [Fe/H]=–5.56, has been identified as part of a binary system. Aims . We aim to constrain the orbital parameters of HE 0107−5240 through radial velocity monitoring with the ESPRESSO spectrograph. Methods . We derived radial velocities using cross-correlation with a template, taking advantage of the strong G-band feature. We combined all observations to obtain a high signal-to-noise ratio spectrum, which we used to refine our understanding of the stellar chemical composition. We additionally used a co-added UVES spectrum in the blue to complement the wavelength coverage of ESPRESSO. Results . Observations of HE 0107−5240 over a span of more than four years yield a revised orbital period of about 29 years. We provide updated elemental abundances for Sc, Cr, Co, and, tentatively, Al, along with a new upper limit for Be. We derive the iron abundance from ionised Fe lines and establish significant upper limits for Li, Si, and Sr. Conclusions . We confirm that the star is a long-period binary. Iron abundances derived from neutral and ionised lines are consistent with the local thermodynamical equilibrium (LTE) assumption, which casts doubt on published deviations from LTE corrections for Fe in this star. The heavy elements Sr and Ba remain undetected, confirming the classification of HE 0107−5240 as a carbon-enhanced, metal-poor star not enhanced in heavy elements (CEMP-no), and supporting the absence of an n-capture element plateau at the lowest metallicities.

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Journal
Astronomy and Astrophysics
Published
2025-11-10
DOI
https://doi.org/10.1051/0004-6361/202556891
Citations
2
Primary Topic
Stellar, planetary, and galactic studies
Type
article
Field-Weighted Citation Impact
2.31
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article

Unveiling the nature of HE 0107–5240: a long period binary CEMP-no star with [Fe/H] of –5.56

N. J. Nunes, L. Monaco, Marco Limongi, L. Sbordone et al.
2 citations
Astronomy and Astrophysics
Stellar, planetary, and galactic studies
2.31
article

Unveiling the nature of HE 0107–5240: a long period binary CEMP-no star with [Fe/H] of –5.56

N. J. Nunes, L. Monaco, Marco Limongi, L. Sbordone, E. Caffau, N. Christlieb, M. R. Zapatero Osorio, S. Cristiani, C. J. A. P. Martins, P. Molaro, M. Spite, P. François, Lorenzo Roberti, Tobias M. Schmidt, P. Bonifacio, H.‐G. Ludwig, David S. Aguado, M. Steffen, A. J. Gallagher, R. Lallement, G. Cupani, N. C. Santos, R. Rébolo, A. Chieffi, J. I. Gónzalez Hernández, Dinko Milaković, V. D'Odorico, M. T. Murphy, C. Allende Prieto, Agnese Falla
article en
2 citations

Abstract

Context . The vast majority of the most iron-poor stars in the Galaxy exhibit strong carbon enhancement, with C/H ratios about two orders of magnitude below solar. This unusual chemical composition likely reflects the properties of the gas cloud from which these stars formed, having been enriched by one, or at most a few, supernovae. A remarkable member of this stellar class, HE 0107 −5240 with [Fe/H]=–5.56, has been identified as part of a binary system. Aims . We aim to constrain the orbital parameters of HE 0107−5240 through radial velocity monitoring with the ESPRESSO spectrograph. Methods . We derived radial velocities using cross-correlation with a template, taking advantage of the strong G-band feature. We combined all observations to obtain a high signal-to-noise ratio spectrum, which we used to refine our understanding of the stellar chemical composition. We additionally used a co-added UVES spectrum in the blue to complement the wavelength coverage of ESPRESSO. Results . Observations of HE 0107−5240 over a span of more than four years yield a revised orbital period of about 29 years. We provide updated elemental abundances for Sc, Cr, Co, and, tentatively, Al, along with a new upper limit for Be. We derive the iron abundance from ionised Fe lines and establish significant upper limits for Li, Si, and Sr. Conclusions . We confirm that the star is a long-period binary. Iron abundances derived from neutral and ionised lines are consistent with the local thermodynamical equilibrium (LTE) assumption, which casts doubt on published deviations from LTE corrections for Fe in this star. The heavy elements Sr and Ba remain undetected, confirming the classification of HE 0107−5240 as a carbon-enhanced, metal-poor star not enhanced in heavy elements (CEMP-no), and supporting the absence of an n-capture element plateau at the lowest metallicities.

Astronomy and AstrophysicsVol. 704
Goethe University Frankfurt (DE), University of Geneva (CH), Centre National de la Recherche Scientifique (FR), Goethe-Institute United Kingdom (GB), Universidad de La Laguna (ES), Universidade do Porto (PT), Université Paris Cité (FR), Heidelberg University (DE), Frankfurt Institute for Advanced Studies (DE), Konkoly Observatory (HU), Sorbonne Université (FR), Institute of Astrophysics and Space Sciences (PT), Sorbonne Paris Cité (FR), Institute for Space Astrophysics and Planetology (IT), Centro de Astrofísica da Universidade do Porto (PT), Kavli Institute for the Physics and Mathematics of the Universe (JP), Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Sud (IT), Centro de Astrobiología (ES), Instituto de Astrofísica de Canarias (ES), Institute for Fundamental Physics of the Universe (IT), Instituto de Geofísica y Astronomía (CU), Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (IT), Université de Picardie Jules Verne (FR), Monash University (AU), Swinburne University of Technology (AU), Sapienza University of Rome (IT), National Institute for Astrophysics (IT)
Openalex Percentile: Top 10%
Stellar, planetary, and galactic studies
2.31
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