Survey of Surveys

Tsantaki, M.; Pancino, E.; Marrese, P. M.; Marinoni, S.; Rainer, M.; Turchi, Alessio; Randich, S.; Gallart, Carme; Battaglia, G.; Masseron, T.

doi:10.1051/0004-6361/202141702

Cited by 33 publications

(35 citation statements)

References 86 publications

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“…This is obtained for the above local sample by complementing the radial velocities from Gaia EDR3 with v los measurements from GALAH DR3 (Buder et al 2021), APOGEE DR16 (Ahumada et al 2020), RAVE DR6 (Steinmetz et al 2020b,a), and LAM-OST DR6 (Liu et al 2019;Wang et al 2020). Velocity systematic shifts between surveys, although small (see Tsantaki et al 2022), have been considered. We select halo stars by requiring that |V − V LS R | > 210 km/s, where V is the total velocity vector corrected for the Solar motion and Local Standard of Rest velocity (V LS R = 232 km/s from McMillan 2017).…”

Section: Data and Sample Selectionmentioning

confidence: 99%

Unveiling the past evolution of the progenitor of the Helmi streams

Ruiz-Lara¹,

Helmi²,

Gallart³

et al. 2022

Preprint

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Aims. We aim to determine the star formation history (SFH) of the progenitor of the Helmi streams. Methods. From the 5D Gaia EDR3 data set, we extract local samples of stars dominated by the Helmi streams, and the Galactic (thick and thin) disc and halo. We do this by identifying regions in a pseudo-Cartesian velocity space (obtained by setting line-ofsight velocities to zero), where stars belonging to these components, as identified in samples with 6D phase-space information, are predominantly found. We make use of an updated absolute colour-magnitude diagram (aCMD) fitting methodology to contrast, for the first time, the SFH of a disrupted accreted system -the Helmi streams-to that of the average Milky Way inner halo. To this end, special attention is given to the correct characterisation of Gaia completeness effects and observational errors on the aCMD. Results. We find that the progenitor of the Helmi streams experienced an early star formation but which was sustained for longer (until 7-9 Gyr ago) than for the Milky Way halo (10-11 Gyr ago). As a consequence, half of its stellar mass was in place ∼ 0.7 Gyr later. The quenching of star formation in the Helmi streams progenitor, together with some hints of a star formation burst at ∼ 8 Gyr, suggest it was accreted by the Milky Way around this time, in concert with previous estimates based on the dynamics of the streams.

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Section: Data and Sample Selectionmentioning

confidence: 99%

Unveiling the past evolution of the progenitor of the Helmi streams

Ruiz-Lara¹,

Helmi²,

Gallart³

et al. 2022

Preprint

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“…This differs from the official Gaia DR2-EDR3 match in the sense that we looked backwards for EDR3 stars in the DR2 catalogue, while the official Gaia cross-match looks forward for DR2 stars in the EDR3 catalogue. This specific cross-match will be used below for the cross-match with the Survey of Surveys SoS (Tsantaki et al 2022, see also Sections 3.5 and 4.5) and for the reddening estimates (Section 4.3).…”

Section: Gaia Cross-match and Catalogue Cleaningmentioning

confidence: 99%

“…To identify spectroscopically confirmed binaries, we used the Survey of Surveys (hereafter SoS, Tsantaki et al 2022), which combines in a homogeneous way data from the major spectroscopic surveys (see Section 4.5 for more details). Among other parameters, the SoS catalogue contains a flag indicating whether Kounkel et al 2021), the others are SB2, contact binaries, radial velocity variables, or ultra-wide binaries.…”

Section: Binary Starsmentioning

confidence: 99%

“…The first method we employed is based on spectroscopy. We used data from the SoS I (Tsantaki et al 2022, see also Section 3.5), which contains homogenized, combined, and recalibrated RVs for about 11 million stars, with zero-point errors of a few hundred m/s and internal uncertainties in the range 0.5-1.5 tainty δLY is the probability that the object is indeed a young stellar object in all the WISE bands, and SY with its uncertainty δSY is the same probability, but without considering the W3 and W4 bands. We classified as "YSO:", i.e., as suspect YSO, 122 additional objects matching the less-restrictive criteria recommended by the authors.…”

Section: Spectroscopic Parameters and Radial Velocitymentioning

confidence: 99%

“…We found RV estimates for 9643 stars and stellar parameters for 6365 stars in the combined catalogue. Because only RVs are carefully re-calibrated in SoS I, to obtain the other stellar parameters for stars observed in more than one survey, we simply took the mean of the parameters presented in Table 8 by Tsantaki et al (2022), which is adequate for our present purpose. We complemented the SoS spectroscopic parameters using the white dwarfs identified in the Kong & Luo (2021) or Fusillo et al (2021) catalogues (see also Section 4.4).…”

Section: Spectroscopic Parameters and Radial Velocitymentioning

confidence: 99%

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The Gaia EDR3 view of Johnson-Kron-Cousins standard stars: the curated Landolt and Stetson collections

Pancino,

Marrese,

Marinoni

et al. 2022

Preprint

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Context. In the era of large surveys and space missions, it is necessary to rely on large samples of well-characterized stars for intercalibrating and comparing measurements from different surveys and catalogues. Among the most employed photometric systems, the Johnson-Kron-Cousins has been used for decades and for a large amount of important datasets. Aims. Our goal is to profit from the Gaia EDR3 data, Gaia official cross-match algorithm, and Gaia-derived literature catalogues, to provide a well-characterized and clean sample of secondary standards in the Johnson-Kron-Cousins system, as well as a set of transformations between the main photometric systems and the Johnson-Kron-Cousins one. Methods. Using Gaia as a reference, as well as data from reddening maps, spectroscopic surveys, and variable stars monitoring surveys, we curated and characterized the widely used Landolt and Stetson collections of more than 200 000 secondary standards, employing classical as well as machine learning techniques. In particular, our atmospheric parameters agree significantly better with spectroscopic ones, compared to other machine learning catalogues. We also cross-matched the curated collections with the major photometric surveys to provide a comprehensive set of reliable measurements in the most widely adopted photometric systems. Results. We provide a curated catalogue of secondary standards in the Johnson-Kron-Cousins system that are well-measured and as free as possible from variable and multiple sources. We characterize the collection in terms of astrophysical parameters, distance, reddening, and radial velocity. We provide a table with the magnitudes of the secondary standards in the most widely used photometric systems (ugriz, grizy, Gaia, Hipparcos, Tycho, 2MASS). We finally provide a set of 167 polynomial transformations, valid for dwarfs and giants, metal-poor and metal-rich stars, to transform U BVRI magnitudes in the above photometric systems and vice-versa.

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Assessment of [Fe/H] determinations for FGK stars in spectroscopic surveys

Soubiran

Brouillet

Casamiquela

2022

A&A

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Context. The iron abundance [Fe/H] in the atmosphere of FGK-type stars is crucial in stellar and galactic physics. The number of stars with a measured value of [Fe/H] is increasing considerably thanks to spectroscopic surveys. However, different methodologies, inputs, and assumptions used in spectral analyses lead to different precisions in [Fe/H] and possibly to systematic differences, which need to be evaluated. It is essential to understand the characteristics of each survey to fully exploit their potential, in particular if the surveys are combined to probe a larger galactic volume and to improve statistics. Aims. The purpose of this study is to compare [Fe/H] determinations from the largest spectroscopic surveys to other catalogues taken as reference. Offsets and dispersions of the residuals are examined, as are their trends with other parameters. The investigated surveys are the latest public releases of APOGEE, GALAH, RAVE, LAMOST, SEGUE, and the Gaia-ESO Survey. Methods. We use reference samples that provide independent determinations of [Fe/H], which are compared to those from the surveys for common stars. The distribution of the residuals is assessed through simple statistics that measure the offset between two catalogues and the dispersion representative of the precision of both catalogues. When relevant, linear fits are performed. A large sample of FGKtype stars with [Fe/H] based on high-resolution, high-signal-to-noise spectroscopy was built from the PASTEL catalogue to provide a reference sample. We also use FGK members in open and globular clusters to assess the internal consistency of [Fe/H] of each survey. The agreement of median [Fe/H] values for clusters observed by different surveys is discussed. Results. All the surveys overestimate the low metallicities, and some of them also underestimate the high metallicities. They perform well in the most populated intermediate metallicity range whatever the resolution. In most cases, the typical precision that we deduce from the comparisons is in good agreement with the uncertainties quoted in the catalogues. Some exceptions to this general behaviour are discussed.

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Survey of Surveys

Cited by 33 publications

References 86 publications

Unveiling the past evolution of the progenitor of the Helmi streams

Unveiling the past evolution of the progenitor of the Helmi streams

The Gaia EDR3 view of Johnson-Kron-Cousins standard stars: the curated Landolt and Stetson collections

Assessment of [Fe/H] determinations for FGK stars in spectroscopic surveys

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