到达恒星运动学群和非常宽的双星之间的边界。IV。盖亚DR3中rho > 1000角秒的最宽华盛顿双星系统
Reaching the boundary between stellar kinematic groups and very wide binaries. IV. The widest Washington double star systems with rho > 1000 arcsec in Gaia DR3
摘要：
目的：利用最新的盖亚DR 3数据，我们分析了华盛顿双星（WDS）星表中角距大于1000弧秒的最宽双星对，角距为$ρ$。研究方法：我们确认了这对恒星系统的成员资格，根据共同的自行，视差，（如果可用）径向速度，以及颜色-星等图中各个组成部分的loxity。我们还寻找了与超宽对更近的同伴，无论是由白龙会报告的还是我们通过新的盖亚天体测量搜索发现的。此外，我们确定了每颗恒星（和白矮星）的质量，并根据投影的物理分离计算了引力势能，|Ug*| 的系统。结果：在目前由WDS编目的155159对中，有504对$ρ$ > 1000 arcsec。其中，只有2个超宽对尚未被确认，10个没有任何可用的天体测量，339个没有通过自行或视差的保守过滤，59个是年轻恒星运动学群、星协或疏散星团的成员，只有94个仍然是银河系中真正的超宽对。考虑到补充天体测量和书目搜索中确定的较短距离的额外成员，我们在94个超宽恒星系统中发现了79颗新星（39颗报告，加上40颗未报告的WDS）。当包含具有大型盖亚DR 3 RUWE、$σ_{Vr}$或自行异常的新的近距离双星候选时，该样本将被扩展。此外，大部分的子系统和非层次结构的许多广泛的系统与三个或更多的明星是显着的。
英文摘要：
Aims: With the latest Gaia DR3 data, we analyse the widest pairs in the Washington Double Star (WDS) catalogue with angular separations, $ρ$, greater than 1000 arcsec. Methods: We confirmed the pair's membership to stellar systems based on common proper motions, parallaxes, and (when available) radial velocities, together with the locii of the individual components in colour-magnitude diagrams. We also looked for additional closer companions to the ultrawide pairs, either reported by WDS or found by us with a new Gaia astrometric search. In addition, we determined masses for each star (and white dwarf) and, with the projected physical separation, computed the gravitational potential energy, |Ug*|, of the systems. Results: Of the 155159 pairs currently catalogued by WDS, there are 504 with $ρ$ > 1000 arcsec. Of these, only 2 ultrawide pairs have not been identified, 10 do not have any available astrometry, 339 have not passed a conservative filtering in proper motion or parallax, 59 are members of young stellar kinematic groups, associations or open clusters, and only 94 remain as bona fide ultrawide pairs in the galactic field. Accounting for the additional members at shorter separations identified in a complementary astrometric and bibliographic search, we found 79 new stars (39 reported, plus 40 not reported by WDS) in 94 ultrawide stellar systems. This sample is expanded when including new close binary candidates with large Gaia DR3 RUWE, $σ_{Vr}$, or a proper motion anomaly. Furthermore, the large fraction of subsystems and the non-hierarchical configurations of many wide systems with three or more stars is remarkable.
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