New light on the <i>Gaia</i> DR2 parallax zero-point: influence of the asteroseismic approach, in and beyond the <i>Kepler</i> field

Khan, Saniya; Miglio, A.; Mosser, B.; Arenou, Frédéric; Belkacem, K.; Brown, A. G. A.; Katz, David; Casagrande, Luca; Chaplin, W. J.; Davies, G. R.; Rendle, B. M.; Rodrigues, Thaíse S.; Bossini, D.; Cantat-Gaudin, T.; Elsworth, Y.; Girardi, L.; North, Thomas S. H.; Vallenari, A.

doi:10.1051/0004-6361/201935304

Cited by 73 publications

(74 citation statements)

References 74 publications

(127 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Comparing Kepler first-ascent red giant branch and red clump asteroseismic parallaxes to Gaia DR2 parallaxes, Khan et al (2019) find agreement between the Gaia and asteroseismic radius scales within ∼ 5%. We note that our results are not directly comparable because they do not account for f ∆ν , and so their level of agreement between Gaia and asteroseismic radius scales is an upper bound.…”

Section: Scaling Relations For [Fe/h] < −1mentioning

confidence: 74%

Testing the Radius Scaling Relation with Gaia DR2 in the Kepler Field

Zinn

Pinsonneault

Huber

et al. 2019

ApJ

View full text Add to dashboard Cite

We compare radii based on Gaia parallaxes to asteroseismic scaling relation-based radii of ∼ 300 dwarfs & subgiants and ∼ 3600 first-ascent giants from the Kepler mission. Systematics due to temperature, bolometric correction, extinction, asteroseismic radius, and the spatially-correlated Gaia parallax zero-point, contribute to a 2% systematic uncertainty on the Gaia-asteroseismic radius agreement. We find that dwarf and giant scaling radii are on a parallactic scale at the −2.1% ± 0.5% (rand.) ± 2.0% (syst.) level (dwarfs) and +1.7% ± 0.3% (rand.) ± 2.0%(syst.) level (giants), supporting the accuracy and precision of scaling relations in this domain. In total, the 2% agreement that we find holds for stars spanning radii between 0.8R and 30R . We do, however, see evidence for relative errors in scaling radii between dwarfs and giants at the 4% ± 0.6% level, and find evidence of departures from simple scaling relations for radii above 30R . Asteroseismic masses for very metal-poor stars are still overestimated relative to astrophysical priors, but at a reduced level. We see no trend with metallicity in radius agreement for stars with −0.5 < [Fe/H] < +0.5. We quantify the spatially-correlated parallax errors in the Kepler field, which globally agree with the Gaia team's published covariance model. We provide Gaia radii, corrected for extinction and the Gaia parallax zero-point for our full sample of ∼ 3900 stars, including dwarfs, subgiants, and first-ascent giants.

show abstract

Section: Scaling Relations For [Fe/h] < −1mentioning

confidence: 74%

Testing the Radius Scaling Relation with Gaia DR2 in the Kepler Field

Zinn

Pinsonneault

Huber

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…By the study of a sample of RR-Lyrae, the parallax zero point was found to be 0.057±0.0034 mas Muraveva et al (2018) It is therefore undoubtable that there is a non-zero parallax offset in the Gaia DR2 between 0.2 and 0.8 mas. There is a significant difference in the parallax zero-points derived from fainter and bluer quasars (0.029 mas, Lindegren et al (2018)) and from brighter and redder sources like Cepheids (0.046 mas, Riess et al (2018); 0.048 mas, Groenewegen (2018)), RR Lyrae (0.057 mas, Muraveva et al (2018)), or red giants and red clump stars (0.0528 mas, Zinn et al (2019); 0.0517 mas, Khan et al (2019); and 0.03838 mas, Hall et al (2019)).…”

Section: Dmt Applicationmentioning

confidence: 99%

“…reported a parallax offset of 0.082±0.033 mas using a sample of eclipsing binaries. In 2019, many more studies dealt with the Gaia parallax zero point and the value varies between 0.030 and 0.1 mas (0.031±0.11mas,Graczyk et al (2019); 0.054±0.006mas,Schönrich et al (2019); 0.0523±0.002 mas,Leung & Bovy (2019); 0.075±0.029mas,Xu et al (2019); 0.0517±0.0008mas,Khan et al (2019); 0.03838 +0.01354 −0.01383 mas,Hall et al (2019); and 0.0528±0.0024 mas,Zinn et al (2019)).…”

mentioning

confidence: 99%

Distance mapping applied to four well-known planetary nebulae and a nova shell

Gómez-Gordillo

Akras

Gonçalves

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Accurate distance estimates of astrophysical objects such as planetary nebulae (PNe), and nova and supernova remnants, among others, allow us to constrain their physical characteristics, such as size, mass, luminosity, and age. An innovative technique based on the expansion parallax method, the so-called distance mapping technique (DMT), provides distance maps of expanding nebulae as well as an estimation of their distances. The DMT combines the tangential velocity vectors obtained from 3D morpho-kinematic models and the observed proper motion vectors to estimate the distance. We applied the DMT to four PNe (NGC 6702, NGC 6543, NGC 6302, and BD+30 3639) and one nova remnant (GK Persei) and derived new distances in good agreement with previous studies. New simple morpho-kinematic shape models were generated for NGC 6543, NGC 6302, and NGC 6702, whereas for BD+30 3639 and GK Persei published models were used. We demonstrate that the DMT is a useful tool to obtain distance values of PNe, in addition to revealing kinematically peculiar regions within the nebulae. Distances are also derived from the trigonometric Gaia parallaxes. The effect of the non-negligible parallax offset in the second Gaia data release is also discussed.

show abstract

“…The zero-point offset between the observed and asteroseismic parallaxes is considered in many papers in the literature (Sahlholdt et al 2018;Zinn et al 2018;Khan et al 2019;Hall et al 2019). Most of these studies find the observed parallax less than the asteroseismic parallax: ∆π = π obs − πsis, about -0.05 mas.…”

Section: Comparison Of the Observed And Asteroseismic Parallaxesmentioning

confidence: 99%

Fundamental properties of Kepler and CoRoT targets – IV. Masses and radii from frequencies of minimum Δν and their implications

Yıldız

Orhan

Kayhan

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Recently, by analysing the oscillation frequencies of 90 stars, Yıldız, Ç elik Orhan & Kayhan have shown that the reference frequencies (ν min0 , ν min1 and ν min2 ) derived from glitches due to He II ionization zone have very strong diagnostic potential for the determination of their effective temperatures. In this study, we continue to analyse the same stars and compute their mass, radius and age from different scaling relations including relations based on ν min0 , ν min1 and ν min2 . For most of the stars, the masses computed using ν min0 and ν min1 are very close to each other. For 38 stars, the difference between these masses is less than 0.024 M ⊙ . The radii of these stars from ν min0 and ν min1 are even closer, with differences of less than 0.007 R ⊙ . These stars may be the most well known solar-like oscillating stars and deserve to be studied in detail. The asteroseismic expressions we derive for mass and radius show slight dependence on metallicity. We therefore develop a new method for computing initial metallicity from this surface metallicity by taking into account the effect of microscopic diffusion. The time dependence of initial metallicity shows some very interesting features that may be important for our understanding of chemical enrichment of Galactic Disc. According to our findings, every epoch of the disc has its own lowest and highest values for metallicity. It seems that rotational velocity is inversely proportional to 1/2 power of age as given by the Skumanich relation.

show abstract

New light on the Gaia DR2 parallax zero-point: influence of the asteroseismic approach, in and beyond the Kepler field

Cited by 73 publications

References 74 publications

Testing the Radius Scaling Relation with Gaia DR2 in the Kepler Field

Testing the Radius Scaling Relation with Gaia DR2 in the Kepler Field

Distance mapping applied to four well-known planetary nebulae and a nova shell

Fundamental properties of Kepler and CoRoT targets – IV. Masses and radii from frequencies of minimum Δν and their implications

Contact Info

Product

Resources

About