Isochrone fitting in the Gaia era | Astronomy & Astrophysics (A&A)

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Table 4

Maximum distance modulus μ_d and a fraction of stars for which the use of parallaxes and spectrophotometric data gives at least 10% improvement in log(age) uncertainties as compared to those obtained with spectrophotometric data alone.

c rowspan="0" c>0 * [0pt]Survey	TGAS (dataset 2/dataset 3)		Gaia EoM (dataset 1/dataset 5)
	Maximum μ_d	Fraction (%)	Maximum μ_d	Fraction (%)
APOGEE DR14	9. m7	25.7	14. m4	80.4
GALAH DR1	11. m 8	85.1	∞	100.0
Gaia-ESO DR2	10. m 3	84.4	14. m4	82.7
LAMOST DR3	8. m 7	53.8	14. m9	94.4
LAMOST GAC DR2	10. m 8	76.8	13. m8	85.3
LAMOST GAC VB DR2	10. m 3	71.8	16. m9	99.7
LAMOST-Cannon	10. m 3	38.5	14. m9	94.3
RAVE DR5	11. m 3	78.9	∞	100.0
RAVE-on	10. m 8	74.3	17. m4	99.9
SEGUE	–	–	10. m 8	19.3
TESS-HERMES DR1	10. m 3	97.9	∞	100.0

Notes. Second and third columns are the result of comparing datasets 2 and 3 (without and with TGAS parallaxes used). Fourth and fifth columns are the result of comparing datasets 1 and 5 (without and with Gaia EoM parallaxes used).

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