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Lind, Karin
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Publications (10 of 57) Show all publications
Simpson, J. D., Martell, S. L., Da Costa, G., Horner, J., Wyse, R. F. G., Ting, Y.-S., . . . Nordlander, T. (2020). The GALAH Survey: Chemically tagging the Fimbulthul stream to the globular cluster omega Centauri. Monthly notices of the Royal Astronomical Society, 491(3), 3374-3384
Open this publication in new window or tab >>The GALAH Survey: Chemically tagging the Fimbulthul stream to the globular cluster omega Centauri
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2020 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 491, no 3, p. 3374-3384Article in journal (Refereed) Published
Abstract [en]

Using kinematics from Gaia and the large elemental abundance space of the second data release of the GALAH survey, we identify two new members of the Fimbulthul stellar stream, and chemically tag them to massive, multimetallic globular cluster omega Centauri. Recent analysis of the second data release of Gaia had revealed the Fimbulthul stellar stream in the halo of the Milky Way. It had been proposed that the stream is associated with the omega Cen, but this proposition relied exclusively upon the kinematics and metallicities of the stars to make the association. In this work, we find our two new members of the stream to be metal-poor stars that are enhanced in sodium and aluminium, typical of second population globular cluster stars, but not otherwise seen in field stars. Furthermore, the stars share the s-process abundance pattern seen in omega Cen, which is rare in field stars. Apart from one star within 1.5 deg of omega Cen, we find no other stars observed by GALAH spatially near omega Cen or the Fimbulthul stream that could be kinematically and chemically linked to the cluster. Chemically tagging stars in the Fimbulthul stream to omega Cen confirms the earlier work, and further links this tidal feature in the Milky Way halo to omega Cen.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS, 2020
Keywords
globular clusters: individual: omega Cen, galaxy: halo, galaxy: kinematics and dynamics
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-406909 (URN)10.1093/mnras/stz3105 (DOI)000512306500020 ()
Available from: 2020-03-20 Created: 2020-03-20 Last updated: 2020-03-20Bibliographically approved
Xiang, M., Ting, Y.-S., Rix, H.-W., Sandford, N., Buder, S., Lind, K., . . . Zhang, H.-W. (2019). Abundance Estimates for 16 Elements in 6 Million Stars from LAMOST DR5 Low-Resolution Spectra. Astrophysical Journal Supplement Series, 245(2), Article ID 34.
Open this publication in new window or tab >>Abundance Estimates for 16 Elements in 6 Million Stars from LAMOST DR5 Low-Resolution Spectra
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2019 (English)In: Astrophysical Journal Supplement Series, ISSN 0067-0049, E-ISSN 1538-4365, Vol. 245, no 2, article id 34Article in journal (Refereed) Published
Abstract [en]

We present the determination of stellar parameters and individual elemental abundances for 6 million stars from similar to 8 million low-resolution (R similar to 1800) spectra from LAMOST DR5. This is based on a modeling approach that we dub the data-driven Payne (DD-Payne), which inherits essential ingredients from both the Payne and the Cannon. It is a data-driven model that incorporates constraints from theoretical spectral models to ensure the derived abundance estimates are physically sensible. Stars in LAMOST DR5 that are in common with either GALAH DR2 or APOGEE DR14 are used to train a model that delivers stellar parameters (T-eff, log g, V-mic) and abundances for 16 elements (C, N, O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Co, Ni, Cu, and Ba) over a metallicity range of -4.dex < [Fe/H] < 0.6 dex when applied to the LAMOST spectra. Cross-validation and repeat observations suggest that, for S/N-pixel >= 50, the typical internal abundance precision is 0.03-0.1 dex for the majority of these elements, with 0.2-0.3 dex for Cu and Ba, and the internal precision of T-eff and log g is better than 30 K and 0.07 dex, respectively. Abundance systematics at the similar to 0.1 dex level are present in these estimates but are inherited from the high-resolution surveys' training labels. For some elements, GALAH provides more robust training labels, for others, APOGEE. We provide flags to guide the quality of the label determination and identify binary/multiple stars in LAMOST DR5. An electronic version of the abundance catalog is made publicly available.

Place, publisher, year, edition, pages
IOP PUBLISHING LTD, 2019
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-408204 (URN)10.3847/1538-4365/ab5364 (DOI)000518771900011 ()
Available from: 2020-04-06 Created: 2020-04-06 Last updated: 2020-04-06Bibliographically approved
Osorio, Y., Lind, K., Barklem, P. S., Prieto, C. A. & Zatsarinny, O. (2019). Ca line formation in late-type stellar atmospheres: I. The model atom. Astronomy and Astrophysics, 623, Article ID A103.
Open this publication in new window or tab >>Ca line formation in late-type stellar atmospheres: I. The model atom
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2019 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 623, article id A103Article in journal (Refereed) Published
Abstract [en]

Context

Departures from local thermodynamic equilibrium (LTE) distort the calcium abundance derived from stellar spectra in various ways, depending on the lines used and the stellar atmospheric parameters. The collection of atomic data adopted in non-LTE (NLTE) calculations must be sufficiently complete and accurate.

Aims

We derive NLTE abundances from high-quality observations and reliable stellar parameters using a model atom built afresh for this work, and check the consistency of our results over a wide wavelength range with transitions of atomic and singly ionised calcium.

Methods

We built and tested Cat and Can model atoms with state-of-the-art radiative and collisional data, and tested their performance deriving the Ca abundance in three benchmark stars: Procyon, the Sun, and Arcturus. We have excellent-quality observations and accurate stellar parameters for these stars. Two methods to derive the LTE/NLTE abundances were used and compared. The LTE/NLTE centre-to-limb variation (CLV) of Ca lines in the Sun was also investigated.

Results

The two methods used give similar results in all three stars. Several discrepancies found in LTE do not appear in our NLTE results; in particular the agreement between abundances in the visual and infra-red (IR) and the Cat and Can ionisation balance is improved overall, although substantial line-to-line scatter remains. The CLV of the calcium lines around 6165 angstrom can be partially reproduced. We suspect differences between our modelling and CLV results are due to inhomogeneities in the atmosphere that require 3D modelling.

Keywords
line: formation, stars: abundances
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-380454 (URN)10.1051/0004-6361/201834680 (DOI)000460891400001 ()
Funder
Swedish Research Council, 2015-00415_3Knut and Alice Wallenberg FoundationSwedish Research Council
Available from: 2019-03-28 Created: 2019-03-28 Last updated: 2019-03-28Bibliographically approved
Amarsi, A. M., Nissen, P. E., Asplund, M., Lind, K. & Barklem, P. (2019). Carbon and oxygen in metal-poor halo stars. Astronomy and Astrophysics, 622, Article ID L4.
Open this publication in new window or tab >>Carbon and oxygen in metal-poor halo stars
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2019 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 622, article id L4Article in journal (Refereed) Published
Abstract [en]

Carbon and oxygen are key tracers of the Galactic chemical evolution; in particular, a reported upturn in [C/O] towards decreasing [O/H] in metal-poor halo stars could be a signature of nucleosynthesis by massive Population III stars. We reanalyse carbon, oxygen, and iron abundances in 39 metal-poor turn-off stars. For the first time, we take into account 3D hydrodynamic effects together with departures from local thermodynamic equilibrium (LTE) when determining both the stellar parameters and the elemental abundances, by deriving effective temperatures from 3D non-LTE H beta profiles, surface gravities from Gaia parallaxes, iron abundances from 3D LTE Fe ii equivalent widths, and carbon and oxygen abundances from 3D non-LTE C-I and O-I equivalent widths. We find that [C/Fe] stays flat with [Fe/H], whereas [O/Fe] increases linearly up to 0.75 dex with decreasing [Fe/H] down to -3.0 dex. Therefore [C/O] monotonically decreases towards decreasing [C/H], in contrast to previous findings, mainly because the non-LTE e ff ects for O i at low [Fe/H] are weaker with our improved calculations.

Place, publisher, year, edition, pages
EDP SCIENCES S A, 2019
Keywords
radiative transfer, stars: abundances, stars: late-type, stars: Population II
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-376813 (URN)10.1051/0004-6361/201834480 (DOI)000456967800001 ()
Funder
Swedish Research Council, 2015-004153Australian Research Council, FL110100012Australian Research Council, DP150100250Swedish Research CouncilKnut and Alice Wallenberg Foundation
Available from: 2019-02-20 Created: 2019-02-20 Last updated: 2019-02-20Bibliographically approved
Marino, A. F., Da Costa, G. S., Casey, A. R., Asplund, M., Bessell, M. S., Frebel, A., . . . Yong, D. (2019). Keck HIRES spectroscopy of SkyMapper commissioning survey candidate extremely metal-poor stars. Monthly notices of the Royal Astronomical Society, 485(4), 5153-5167
Open this publication in new window or tab >>Keck HIRES spectroscopy of SkyMapper commissioning survey candidate extremely metal-poor stars
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2019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 485, no 4, p. 5153-5167Article in journal (Refereed) Published
Abstract [en]

We present results from the analysis of high-resolution spectra obtained with the Keck HIRES spectrograph for a sample of 17 candidate extremely metal-poor (EMP) stars originally selected from commissioning data obtained with the SkyMapper telescope. Fourteen of the stars have not been observed previously at high dispersion. Three have [Fe/H] <= -3.0, while the remainder, with two more metal-rich exceptions, have -3.0 <= [Fe/H] <= -2.0 dex. Apart from Fe, we also derive abundances for the elements C, N, Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Mn, Co, Ni, and Zn, and for n-capture elements Sr, Ba, and Eu. None of the current sample of stars is found to be carbon-rich. In general, our chemical abundances follow previous trends found in the literature, although we note that two of the most metal-poor stars show very low [Ba/Fe] (similar to-1.7) coupled with low [Sr/Ba] (similar to-0.3). Such stars are relatively rare in the Galactic halo. One further star, and possibly two others, meet the criteria for classification as a r-I star. This study, together with that of Jacobson et al. (2015), completes the outcomes of the SkyMapper commissioning data survey for EMP stars.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS, 2019
Keywords
stars: abundances, stars: Population II, Galaxy: halo, Galaxy: stellar content
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-390639 (URN)10.1093/mnras/stz645 (DOI)000474880400051 ()
Funder
EU, Horizon 2020, 797100Australian Research Council
Available from: 2019-08-21 Created: 2019-08-21 Last updated: 2019-08-21Bibliographically approved
Reggiani, H., Amarsi, A. M., Lind, K., Barklem, P. S., Zatsarinny, O., Bartschat, K., . . . Melendez, J. (2019). Non-LTE analysis of K I in late-type stars. Astronomy and Astrophysics, 627, Article ID A177.
Open this publication in new window or tab >>Non-LTE analysis of K I in late-type stars
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2019 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 627, article id A177Article in journal (Refereed) Published
Abstract [en]

Context. Older models of Galactic chemical evolution (GCE) predict [K/Fe] ratios as much as 1 dex lower than those inferred from stellar observations. Abundances of potassium are mainly based on analyses of the 7698 angstrom resonance line, and the discrepancy between GCE models and observations is in part caused by the assumption of local thermodynamic equilibrium (LTE) in spectroscopic analyses. Aims. We study the statistical equilibrium of K I, focusing on the non-LTE effects on the 7698 angstrom line. We aim to determine how non-LTE abundances of potassium can improve the analysis of its chemical evolution, and help to constrain the yields of GCE models. Methods. We construct a new model K I atom that employs the most up-to-date atomic data. In particular, we calculate and present inelastic e+K collisional excitation cross-sections from the convergent close-coupling (CCC) and the B-Spline R-matrix (BSR) methods, and H+K collisions from the two-electron model (LCAO). We constructed a fine, extended grid of non-LTE abundance corrections based on 1D MARCS models that span 4000 < T-eff/K < 8000, 0.50 < log g < 5.00, -5.00 < [Fe/H] < +0.50, and applied the corrections to potassium abundances extracted from the literature. Results. In concordance with previous studies, we find severe non-LTE effects in the 7698 angstrom line. The line is stronger in non-LTE and the abundance corrections can reach approximately -0.7 dex for solar-metallicity stars such as Procyon. We determine potassium abundances in six benchmark stars, and obtain consistent results from different optical lines. We explore the effects of atmospheric inhomogeneity by computing for the first time a full 3D non-LTE stellar spectrum of K I lines for a test star. We find that 3D modeling is necessary to predict a correct shape of the resonance 7698 angstrom line, but the line strength is similar to that found in 1D non-LTE. Conclusions. Our non-LTE abundance corrections reduce the scatter and change the cosmic trends of literature potassium abundances. In the regime [Fe/H] less than or similar to -1.0 the non-LTE abundances show a good agreement with the GCE model with yields from rotating massive stars. The reduced scatter of the non-LTE corrected abundances of a sample of solar twins shows that line-by-line differential analysis techniques cannot fully compensate for systematic LTE modelling errors; the scatter introduced by such errors introduces a spurious dispersion to K evolution.

Place, publisher, year, edition, pages
EDP SCIENCES S A, 2019
Keywords
stars: abundances, stars: late-type, line: formation, Galaxy: evolution, Galaxy: abundances
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-391374 (URN)10.1051/0004-6361/201935156 (DOI)000476708200002 ()
Funder
Swedish Research Council, 2015-004153Knut and Alice Wallenberg FoundationAustralian Research Council, 170100521Swedish Research Council
Available from: 2019-09-04 Created: 2019-09-04 Last updated: 2019-09-04Bibliographically approved
Feuillet, D. K., Frankel, N., Lind, K., Frinchaboy, P. M., Garcia-Hernandez, D. A., Lane, R. R., . . . Roman-Lopes, A. (2019). Spatial variations in the Milky Way disc metallicity-age relation. Monthly notices of the Royal Astronomical Society, 489(2), 1742-1752
Open this publication in new window or tab >>Spatial variations in the Milky Way disc metallicity-age relation
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2019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 489, no 2, p. 1742-1752Article in journal (Refereed) Published
Abstract [en]

Stellar ages are a crucial component to studying the evolution of the Milky Way. Using Gaia DR2 distance estimates, it is now possible to estimate stellar ages for a larger volume of evolved stars through isochrone matching. This work presents [M/H]-age and [alpha/M]-age relations derived for different spatial locations in the Milky Way disc. These relations are derived by hierarchically modelling the star formation history of stars within a given chemical abundance bin. For the first time, we directly observe that significant variation is apparent in the [M/H]-age relation as a function of both Galactocentric radius and distance from the disc midplane. The [M/H]-age relations support claims that radial migration has a significant effect in the plane of the disc. Using the [M/H] bin with the youngest mean age at each radial zone in the plane of the disc, the present-day metallicity gradient is measured to be -0.059 +/- 0.010 dex kpc(-1), in agreement with Cepheids and young field stars. We find a vertically flared distribution of young stars in the outer disc, confirming predictions of models and previous observations. The mean age of the [M/H]-[alpha/M] distribution of the solar neighbourhood suggests that the high-[M/H] stars are not an evolutionary extension of the low-alpha sequence. Our observational results are important constraints to Galactic simulations and models of chemical evolution.

Keywords
Galaxy: abundances, Galaxy: disc, Galaxy: evolution, Galaxy: stellar content
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-396651 (URN)10.1093/mnras/stz2221 (DOI)000489298100018 ()
Funder
Swedish Research Council, 2015-00415 3
Available from: 2019-11-14 Created: 2019-11-14 Last updated: 2019-11-14Bibliographically approved
Buder, S., Lind, K., Ness, M. K., Asplund, M., Duong, L., Lin, J., . . . Wyse, R. F. (2019). The GALAH survey: An abundance, age, and kinematic inventory of the solar neighbourhood made with TGAS. Astronomy and Astrophysics, 624, Article ID A19.
Open this publication in new window or tab >>The GALAH survey: An abundance, age, and kinematic inventory of the solar neighbourhood made with TGAS
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2019 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 624, article id A19Article in journal (Refereed) Published
Abstract [en]

The overlap between the spectroscopic Galactic Archaeology with HERMES (GALAH) survey and Gaia provides a high-dimensional chemodynamical space of unprecedented size. We present a first analysis of a subset of this overlap, of 7066 dwarf, turn-off, and subgiant stars. These stars have spectra from the GALAH survey and high parallax precision from the Gaia DR1 Tycho-Gaia Astrometric Solution. We investigate correlations between chemical compositions, ages, and kinematics for this sample. Stellar parameters and elemental abundances are derived from the GALAH spectra with the spectral synthesis code SPECTROSCOPY MADE EASY. We determine kinematics and dynamics, including action angles, from the Gaia astrometry and GALAH radial velocities. Stellar masses and ages are determined with Bayesian isochrone matching, using our derived stellar parameters and absolute magnitudes. We report measurements of Li, C, O, Na, Mg, Al, Si, K, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, Zn, Y, as well as Ba and we note that we have employed non-LTE calculations for Li, O, Al, and Fe. We show that the use of astrometric and photometric data improves the accuracy of the derived spectroscopic parameters, especially log g. Focusing our investigation on the correlations between stellar age, iron abundance [Fe/H], and mean alpha-enhancement [alpha/Fe] of the magnitude-selected sample, we recover the result that stars of the high-a sequence are typically older than stars in the low-a sequence, the latter spanning iron abundances of -0.7 < [Fe/H] < +0.5. While these two sequences become indistinguishable in [alpha/Fe] vs. [Fe/H] at the metal-rich regime, we find that age can be used to separate stars from the extended high-a and the low-a sequence even in this regime. When dissecting the sample by stellar age, we find that the old stars (>8 Gyr) have lower angular momenta L-z than the Sun, which implies that they are on eccentric orbits and originate from the inner disc. Contrary to some previous smaller scale studies we find a continuous evolution in the high-alpha-sequence up to super-solar [Fe/H] rather than a gap, which has been interpreted as a separate "high-alpha metal-rich" population. Stars in our sample that are younger than 10 Gyr, are mainly found on the low alpha-sequence and show a gradient in L-z from low [Fe/H] > (L-z > L-z,L-circle dot) towards higher [Fe/H] (L-z < L-z,L-circle dot), which implies that the stars at the ends of this sequence are likely not originating from the close solar vicinity.

Place, publisher, year, edition, pages
EDP SCIENCES S A, 2019
Keywords
surveys, solar neighborhood, Galaxy: evolution, stars: fundamental parameters, stars: abundances, stars: kinematics and dynamics
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-382390 (URN)10.1051/0004-6361/201833218 (DOI)000462979700002 ()
Funder
Swedish Research Council, 2015-00415_3Australian Research Council, DE1401000598Swedish National Infrastructure for Computing (SNIC), 2015/1-309Swedish National Infrastructure for Computing (SNIC), 2016/1-400
Available from: 2019-04-26 Created: 2019-04-26 Last updated: 2019-04-26Bibliographically approved
Bland-Hawthorn, J., Sharma, S., Tepper-Garcia, T., Binney, J., Freeman, K. C., Hayden, M. R., . . . Wyse, R. F. G. (2019). The GALAH survey and Gaia DR2: dissecting the stellar disc's phase space by age, action, chemistry, and location. Monthly notices of the Royal Astronomical Society, 486(1), 1167-1191
Open this publication in new window or tab >>The GALAH survey and Gaia DR2: dissecting the stellar disc's phase space by age, action, chemistry, and location
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2019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 486, no 1, p. 1167-1191Article in journal (Refereed) Published
Abstract [en]

We use the second data releases of the European Space Agency Gaia astrometric survey and the high-resolution Galactic Archaeology with HERMES (GALAH) spectroscopic survey to analyse the structure of our Galaxy's disc components. With GALAH, we separate the alpha-rich and alpha-poor discs (with respect to Fe), which are superposed in both position and velocity space, and examine their distributions in action space. We study the distribution of stars in the zV(z) phase plane, for both V-phi and V-R, and recover the remarkable 'phase spiral' discovered by Gaia. We identify the anticipated quadrupole signature in zV(z) of a tilted velocity ellipsoid for stars above and belowtheGalactic plane. By connecting ourwork with earlier studies, we show that the phase spiral is likely to extend well beyond the narrow solar neighbourhood cylinder in which it was found. The phase spiral is a signature of corrugated waves that propagate through the disc, and the associated non-equilibrium phase mixing. The radially asymmetric distribution of stars involved in the phase spiral reveals that the corrugation, which is mostly confined to the alpha-poor disc, grows in z-amplitude with increasing radius. We present new simulations of tidal disturbance of the Galactic disc by the Sagittarius (Sgr) dwarf. The effect on the zV(z) phase plane lasts greater than or similar to 2 Gyr, but a subsequent disc crossing wipes out the coherent structure. We find that the phase spiral was excited less than or similar to 0.5 Gyr ago by an object like Sgr with total mass similar to 3 x 10(10) M-circle dot (stripped down from similar to 5 x 10(10) M-circle dot when it first entered the halo) passing through the plane.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS, 2019
Keywords
astrometry, proper motions, stars: kinematics and dynamics, Galaxy: disc, evolution, structure
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-390635 (URN)10.1093/mnras/stz217 (DOI)000474894100088 ()
Funder
Australian Research Council, DP150104667Australian Research Council, DP160103747Australian Research Council, DE140100598Swedish Research Council, 2015-00415_3
Available from: 2019-08-21 Created: 2019-08-21 Last updated: 2019-08-21Bibliographically approved
Simpson, J. D., Martell, S. L., Da Costa, G., Casey, A. R., Freeman, K. C., Horner, J., . . . Nordlander, T. (2019). The GALAH survey: co-orbiting stars and chemical tagging. Monthly notices of the Royal Astronomical Society, 482(4), 5302-5315
Open this publication in new window or tab >>The GALAH survey: co-orbiting stars and chemical tagging
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2019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 482, no 4, p. 5302-5315Article in journal (Refereed) Published
Abstract [en]

We present a study using the second data release of the GALAH survey of stellar parameters and elemental abundances of 15 pairs of stars identified by Oh et al. They identified these pairs as potentially co-moving pairs using proper motions and parallaxes from Gaia DR1. We find that 11 very wide (>1 pc) pairs of stars do in fact have similar Galactic orbits, while a further four claimed co-moving pairs are not truly co-orbiting. Eight of the 11 co-orbiting pairs have reliable stellar parameters and abundances, and we find that three of those are quite similar in their abundance patterns, while five have significant [Fe/H] differences. For the latter, this indicates that they could be co-orbiting because of the general dynamical coldness of the thin disc, or perhaps resonances induced by the Galaxy, rather than a shared formation site. Stars such as these, wide binaries, debris of past star formation episodes, and coincidental co-orbiters, are crucial for exploring the limits of chemical tagging in the Milky Way.

Keywords
stars, abundances, stars, formation, galaxy, disc
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-368651 (URN)10.1093/mnras/sty3042 (DOI)000462327300077 ()
Funder
Swedish Research Council, 2015-00415 3
Available from: 2018-12-06 Created: 2018-12-06 Last updated: 2019-04-29Bibliographically approved
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