The end of the white dwarf cooling sequence in M 67
The end of the white dwarf cooling sequence in M 67
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DOI：
10.1051/0004-6361/200913721
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发表时间：
2010-01
影响因子：
6.5
通讯作者：
Andrea Bellini;A. Bellini;L. Bedin;G. Piotto;M. Salaris;Jay Anderson;E. Brocato;R. Ragazzoni;S. Ortolani;A. Bonanos;I. Platais;R. Gilliland;G. Raimondo;A. Bragaglia;M. Tosi;S. Gallozzi;V. Testa;C. Kochanek;E. Giallongo;A. Baruffolo;J. Farinato;E. Diolaiti;R. Speziali;Giovanni Carraro;R. Yadav
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文献类型：
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作者：
Andrea Bellini;A. Bellini;L. Bedin;G. Piotto;M. Salaris;Jay Anderson;E. Brocato;R. Ragazzoni;S. Ortolani;A. Bonanos;I. Platais;R. Gilliland;G. Raimondo;A. Bragaglia;M. Tosi;S. Gallozzi;V. Testa;C. Kochanek;E. Giallongo;A. Baruffolo;J. Farinato;E. Diolaiti;R. Speziali;Giovanni Carraro;R. Yadav
在本文中，我们首次提出了一个自行选择的老银河系疏散星团M 67的白色矮星（WD）样本，下降到WD冷却序列（CS）的底部。颜色-亮度图基于LBC-蓝色相机在LBT的主焦点处收集的数据。作为第一个时代的数据，我们使用CFHT存档图像收集10年前LBC数据。我们测量了所有确定的源的自行。然后使用自行将前景和背景物体从星团中分离出来，包括WD。最后，将V与B-I色星等图中的场-物净化后的WD CS与模型进行了比较。我们确认，从WD CS底部位置得出的年龄与关闭年龄一致。
In this paper, we present for the first time a proper-motion-selected white dwarf (WD) sample of the old Galactic open cluster M 67, down to the bottom of the WD cooling sequence (CS). The color-magnitude diagram is based on data collected with the LBC-Blue camera at the prime-focus of LBT. As first epoch data, we used CFHT-archive images collected 10 years before LBC data. We measured proper motions of all the identified sources. Proper motions are then used to separate foreground and background objects from the cluster stars, including WDs. Finally, the field-object cleaned WD CS in the V vs. B-I color-magnitude diagram is compared with the models. We confirm that the age derived from the location of the bottom of the WD CS is consistent with the turn off age.