Gaia Astrometric Science Performance – Post-Launch Predictions

Bruijne, J. H. J. de; Rygl, K. L. J.; Antoja, T.

doi:10.1051/eas/1567004

Cited by 54 publications

(49 citation statements)

References 21 publications

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“…2 http://www.cosmos.esa.int/web/gaia for all sources. Gaia was launched in December 2013 (de Bruijne, Rygl, & Antoja 2014), and the first data release was in September 2016 (Gaia Collaboration et al 2016b), containing positions and white-light magnitudes for the best behaved stars, and additional information like parallaxes and proper motions for 2 million stars observed previously with Tycho-2 (Høg et al 2000;Michalik, Lindegren, & Hobbs 2015;Lindegren et al 2016). …”

Section: Introductionmentioning

confidence: 99%

Globular clusters with Gaia

Pancino

Bellazzini

Giuffrida

et al. 2017

Mon. Not. R. Astron. Soc.

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The treatment of crowded fields in Gaia data will only be a reality in a few years from now. In particular, for globular clusters, only the end-of-mission data (public in 2022-2023) will have the necessary full crowding treatment and will reach sufficient quality for the faintest stars. As a consequence, the work on the deblending and decontamination pipelines is still ongoing. We describe the present status of the pipelines for different Gaia instruments, and we model the end-of-mission crowding errors on the basis of available information. We then apply the nominal post-launch Gaia performances, appropriately worsened by the estimated crowding errors, to a set of 18 simulated globular clusters with different concentration, distance, and field contamination. We conclude that there will be 10 3 -10 4 stars with astrometric performances virtually untouched by crowding (contaminated by <1 mmag) in the majoritiy of clusters. The most limiting factor will be field crowding, not cluster crowding: the most contaminated clusters will only contain 10-100 clean stars. We also conclude that: (i) the systemic proper motions and parallaxes will be determined to 1% or better up to 15 kpc, and the nearby clusters will have radial velocities to a few km s −1 ; (ii) internal kinematics will be of unprecendented quality, cluster masses will be determined to 10% up to 15 kpc and beyond, and it will be possible to identify differences of a few km s −1 or less in the kinematics (if any) of cluster sub-populations up to 10 kpc and beyond; (iii) the brightest stars (V 17 mag) will have space-quality, wide-field photometry (mmag errors), and all Gaia photometry will have 1-3% errors on the absolute photometric calibration.

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Section: Introductionmentioning

confidence: 99%

Globular clusters with Gaia

Pancino

Bellazzini

Giuffrida

et al. 2017

Mon. Not. R. Astron. Soc.

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“…Using the location of Sculptor and the precision corrections expected [7], we find an improvement in this precision of roughly 7 µas/yr (14 µas/yr) at G = 17 (G = 18) corresponding to an improvement of nearly 20% over the average precision [8] of 39 µas/yr (72 µas/yr). In our calculations below we conservatively approximate this improvement to be 15% and so the final precision with which proper motions can be measured is…”

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confidence: 63%

“…As described in the Gaia Science Performance document [7] and updated in [8] to reflect post-launch performance, Gaia can measure proper motions with an end of mission precision, in µas/yr, of …”

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confidence: 99%

What can Gaia (with Thirty Meter Telescope) say about the Sculptor Dwarf's Core?

Evslin¹

2015

Monthly Notices of the Royal Astronomical Society: Letters

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Walker et al.'s Magellan/MMFS Survey survey identified 1355 red giant candidates in the dwarf spheroidal galaxy Sculptor. We find that the Gaia satellite will be able to measure the proper motions of 139 of these with a precision of between 13 and 20 km/s. Using a Jeans analysis and 5-parameter density model we show that this allows a determination of the mass within the deprojected half-light radius to within 16% and a measurement of the dark matter density exponent γ to within 0.68 within that radius. If, even at first light, the TMT observes Sculptor then the combined observations will improve the precision on these proper motions to about 5 km/s, about 5 years earlier than would be possible without Gaia, further improving the precision of γ to 0.27. Using a bimodal stellar population model for Sculptor the precision of γ improves by about 30%. This suggests that Gaia (with TMT) is capable of excluding a cusped profile of the kind predicted by CDM simulations with 2σ (4σ) of confidence.

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“…The upcoming multi-object spectrographs, WEAVE on WHT (Dalton et al 2012) and 4MOST on VISTA (de Jong et al 2012), will play an important role in confirming more cluster white dwarfs and measuring accurate physical parameters. The ESA Gaia mission will deliver parallaxes for several hundred thousand white dwarfs down to 18-20 mag (Jordan 2007;Carrasco et al 2014;Gaensicke et al 2015), with an accuracy of ≈30 per cent (de Bruijne, Rygl & Antoja 2015). ESA Gaia will supply a crucial improvement to open clusters science, as it will determine stellar membership via the measure of parallaxes and proper motions, allowing the accurate determination of cluster distances and ages, and thus significantly improving the study of the initial-to-final mass relation…”

Section: S U M M a Ry A N D C O N C L U S I O N Smentioning

confidence: 99%

A search for white dwarfs in the Galactic plane: the field and the open cluster population

Raddi¹,

Catalán²,

Gänsicke³

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigated the prospects for systematic searches of white dwarfs at low Galactic latitudes, using the VLT Survey Telescope H α Photometric Survey of the Galactic plane and Bulge (VPHAS+). We targeted 17 white dwarf candidates along sightlines of known open clusters, aiming to identify potential cluster members. We confirmed all the 17 white dwarf candidates from blue/optical spectroscopy, and we suggest five of them to be likely cluster members. We estimated progenitor ages and masses for the candidate cluster members, and compare our findings to those for other cluster white dwarfs. A white dwarf in NGC 3532 is the most massive known cluster member (1.13 M ), likely with an oxygen-neon core, for which we estimate an 8.8 +1.2 −4.3 M progenitor, close to the mass-divide between white dwarf and neutron star progenitors. A cluster member in Ruprecht 131 is a magnetic white dwarf, whose progenitor mass exceeded 2-3 M . We stress that wider searches, and improved cluster distances and ages derived from data of the ESA Gaia mission, will advance the understanding of the mass-loss processes for low-to intermediate-mass stars.

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Gaia Astrometric Science Performance – Post-Launch Predictions

Cited by 54 publications

References 21 publications

Globular clusters with Gaia

Globular clusters with Gaia

What can Gaia (with Thirty Meter Telescope) say about the Sculptor Dwarf's Core?

A search for white dwarfs in the Galactic plane: the field and the open cluster population

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