A white dwarf catalogue from Gaia-DR2 and the Virtual Observatory
A white dwarf catalogue from Gaia-DR2 and the Virtual Observatory
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DOI：
10.1093/mnras/sty2120
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发表时间：
2018-07
影响因子：
4.8
通讯作者：
F. Jiménez-Esteban;F. Jiménez-Esteban;S. Torres;A. Rebassa-Mansergas;G. Skorobogatov;E. Solano;C. C
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文献类型：
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作者：
F. Jiménez-Esteban;F. Jiménez-Esteban;S. Torres;A. Rebassa-Mansergas;G. Skorobogatov;E. Solano;C. C
我们提出了一个目录的73,221白色矮星候选人提取的天体测量和光度数据最近公布的盖亚DR 2目录。白色矮星是在最新的人口合成模拟器的帮助下，从盖亚赫茨伯格-罗素图中选出的。我们的分析表明，盖亚实际上已经识别出了距离太阳100 pc以内的所有白色矮星。因此，我们的子种群8,555个白色矮星在这个距离限制和考虑的颜色范围内，$-1，0.52 <（G_{\rm BP}-G_{\rm RP}）<0.80$，是迄今为止最大和最完整的体积有限的样本。从这个子样本中，我们确定了8，343个CO核心和212个ONe核心的白色矮星候选者，并推导出白色矮星的空间密度为4.9\pm0.4\times10 ^{-3}\，{\rm pc^{-3}}$。这些源的赫兹-罗素图中的分叉是清晰可见的，我们的模型没有预测到。我们使用虚拟天文台工具VOSA通过拟合其光谱能量分布来获得我们的源的有效温度和光度，我们通过虚拟天文台使用公开可用的测光从UV到NIR构建。根据这些参数，我们导出了白色矮星的半径。通过对富氢白色矮星冷却序列的半径和有效温度进行插值，得到了它们的表面重力和质量。盖亚100 pc的白色矮星人口明显占主导地位的冷（$\sim $8，000 K）的对象，并揭示了大量的人口（$M \sim 0.8 M_{\odot}$）白色矮星，其中不超过$\sim $$30 -40 \%$可以归因于氢缺乏的气氛，其起源仍然不确定。
We present a catalogue of 73,221 white dwarf candidates extracted from the astrometric and photometric data of the recently published Gaia DR2 catalogue. White dwarfs were selected from the Gaia Hertzsprung-Russell diagram with the aid of the most updated population synthesis simulator. Our analysis shows that Gaia has virtually identified all white dwarfs within 100 pc from the Sun. Hence, our sub-population of 8,555 white dwarfs within this distance limit and the colour range considered, $-\,0.52<(G_{\rm BP}-G_{\rm RP})<0.80$, is the largest and most complete volume-limited sample of such objects to date. From this sub-sample we identified 8,343 CO-core and 212 ONe-core white dwarf candidates and derived a white dwarf space density of $4.9\pm0.4\times10^{-3}\,{\rm pc^{-3}}$. A bifurcation in the Hertzsprung-Russell diagram for these sources, which our models do not predict, is clearly visible. We used the Virtual Observatory tool VOSA to derive effective temperatures and luminosities for our sources by fitting their spectral energy distributions, that we built from the UV to the NIR using publicly available photometry through the Virtual Observatory. From these parameters, we derived the white dwarf radii. Interpolating the radii and effective temperatures in hydrogen-rich white dwarf cooling sequences, we derived the surface gravities and masses. The Gaia 100 pc white dwarf population is clearly dominated by cool ($\sim$ 8,000 K) objects and reveals a significant population of massive ($M \sim 0.8 M_{\odot}$) white dwarfs, of which no more than $\sim$ $30-40 \%$ can be attributed to hydrogen-deficient atmospheres, and whose origin remains uncertain.