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A GALEX far-ultraviolet study of quasi-coeval samples of red giants

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Abstract

Samples of red giant branch (RGB) stars have been compiled from the literature for seven moving groups, and searches made for both GALEX FUV and Johnson \(\mathit{BV}\) photometry. It has been possible to derive a colour index \((\mathit{FUV}-B)\) for many giants, which has been combined with \(B-V\) to give a two-colour diagram for each kinematic group. In addition, analogous data have been gleaned for a small number of red giants in the open cluster NGC 752.

Optical photometry has been combined with parallax and proper motion data from the Gaia DR2 data release to document the colour-magnitude diagram (CMD) positions and space motion velocities among the proposed group giants. Comparisons with isochrones confirm a range in age among the groups considered. However, none of the group samples evince RGB sequences as tight in the CMD as those typical of open clusters. Considering also the velocity dispersions found within each set of group candidates, it is concluded that the fraction of non-members included may be significant.

The RGB stars ascribed to different moving groups are largely located within overlapping regions of the FUV two-colour diagram, without any obvious systematic offsets between groups of different age. All of the RGB sequences attain a maximum \((\mathit{FUV}-B)\) colour of \(\approx 14.2\)–14.5 mag within the optical colour range of \(1.0 < B-V < 1.25\). Many of the stars in this range are in the core-helium-burning (CHB) phase of evolution. On the red side of the CHB region in the two-colour diagram, i.e., at \(B-V > 1.25\), the RGB stars from different groups largely map out a common locus.

Among CHB and other giants blueward of \(B-V = 1.25\) there are a number of stars with FUV-excesses ranging from 2-4 mag as judged by the \((\mathit{FUV}-B)\) colour. There is found evidence for a range in chromospheric activity among CHB stars. By analogy with known properties of Hyades cluster giants a range in activity among the CHB stars within a moving group may be a consequence of different degrees of spindown corresponding to different amounts of time spent in the core-helium-burning phase.

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Notes

  1. http://www.astro.ucla.edu/~drodrigu/UVWCalc.html.

  2. https://idlastro.gsfc.nasa.gov/homepage.html.

  3. An individual value of \(\sigma \) was calculated from the range between separate FUV magnitude values for each star for which multiple measurements were given by the DR6/7 search. The representative value of \(\sigma \) quoted herein is taken to be the mean of these individual values. Some variable stars and flare stars were not considered in this calculation.

  4. https://www.cosmos.esa.int/gaia.

  5. https://www.cosmos.esa.int/web/gaia/dpac/consortium.

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Acknowledgements

GHS gratefully acknowledges the support of the National Science Foundation through award AST-1517791.

This research has made use of the NASA Astrophysics Data System. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work has made use of data from the European Space Agency (ESA) mission Gaia,Footnote 4 as processed by the Gaia Data Processing and Analysis Consortium (DPACFootnote 5). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

This research also made use of the SIMBAD data base, operated at CDS, Strasbourg, France, as well as the General Catalogue of Photometric Data operated at the University of Lausanne, Switzerland, and the WEBDA database, operated at the Department of Theoretical Physics and Astrophysics of the Masaryk University.

We thank the referee for helpful comments on the manuscript.

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Smith, G.H., Cochrane, K.M. A GALEX far-ultraviolet study of quasi-coeval samples of red giants. Astrophys Space Sci 365, 95 (2020). https://doi.org/10.1007/s10509-020-03806-5

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