Difference of the log-likelihoods of the warp (Yusifov 2004) and no-warp models Δ ≡ ℓWARP−ℓNOWARP for the TGAS(HIP2) sample.
|ϖ < 2 mas||(1 < ϖ < 2) mas||ϖ < 1 mas|
|Sample||Nstars||Δ||σΔ||P(Δ > 0)||N stars||Δ||σΔ||P(Δ > 0)||Nstars||Δ||σΔ||P(Δ > 0)|
|No HIP2 binaries||672||–2.75||6.81||0.34||267||15.03||3.40||1.00||405||–11.85||26.27||0.31|
|95% Conf. Int.||730||–0.86||5.94||0.44||289||10.30||3.23||1.00||444||–13.99||5.23||0.00|
|90% Conf. Int.||692||2.79||4.91||0.72||273||9.11||2.71||1.00||420||–10.85||4.13||0.00|
Notes. Results are shown for the whole sample (All, mv < 8.5) and for the bright sample (mv < 7.5). We also report the results obtained removing the objects with high ΔQ, where ΔQ is the difference between the TGAS and Hipparcos proper motion (Lindegren et al. 2016). For the Hipparcos subset in TGAS, the 95th and 90th percentiles of the ΔQ distribution are ΔQ95% = 23 and ΔQ90% = 11. We also present the results excluding the stars labeled as binaries in van Leeuwen (2008). The 95% (90%) confidence interval is obtained considering the stars with proper motions μb between the 2.5th and the 97.5th (the 5th and the 95th) percentiles of the whole μb distribution (with 767 stars), without restricting to the range (−10 <μb < 5) mas/yr (see text). The standard deviation σΔ and the probability P(Δ > 0) are calculated using bootstrap resamples (see text).
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