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Table 5.

Suggested clusters as places of origin for runaway stars based on spatial coincidence.

HIP Num Origin p-val Tf Trel Vrel Tc Flagage Suggested Original References
(Myr) (Myr) (km s−1) (Myr) Mechanism Mechanism
3881 Cl Alessi 20 0.23 −15.19 15.68 ± 4.12 17.96 /38 Y DES/BSS DES 1,2,16,17
14514 Orion OB1a 0.77 −4.69 4.96 ± 0.72 53.06 Y BSS/DES BSS/DES 3,18
18614 Per OB2 0.69 −6.40 9.29 ± 4.09 47.9 Y DES BSS 3,19
22061 Collinder69 0.99 (a) −1.016 1.08 ± 0.11 102.6 Y DES DES 4,5,20
24575 ONC 0.96 (b) −2.5 2.58 ± 0.05 105.8 Y DES DES 6,1,21
26241 ONC None – – – – DES
27204 ONC 0.94 −2.42 2.47 ± 0.17 113.93 Y DES DES
Collinder 69 0.65 −3.2 3.35 ± 0.13 117.0 Y DES 1,2,22
29678 Collinder 69 0.98 (a) −1.19 1.32 ± 0.15 59.1 Y DES DES 4,5,20
38455 Cl Platais 3 0.306 −17.8 19.37 ± 7.87 20.76 N BSS BSS 1,7,22
38518 Cl Gulliver 9 0.76 −7.95 9.17 ± 3.61 19.26 Y BSS BSS 1,7,22
Gam Vel Subcluster 0.015 −4.92 13.00 ± 3.54 27.10 Y BSS 8,22
39429 Trumpler 10 0.84 −2.6 2.07 ± 0.37 56.20 Y BSS – 1,7,22
42038 NGC 2451A 0.996 −36.561 27.96 ± 5.82 8.37 Y BSS BSS 1,10,22
0.42 −35.8 22.73 ± 6.17 7.68 1,7
Cl VDBH 99 0.64 −34.15 18.80 ± 3.69 8.15 Y BSS – 1,7,22
Cl Platais 9 0.30 −20.2 32.58 ± 23.72 9.32 Y BSS – 1,7,22
IC 2391 0.0004 −18.78 29.93 ± 11.37 11.2 Y BSS BSS 1,7,23
46950 Gam Vel subcluster 0.73 −14.95 13.77 ± 4.10 5.99 Y DES BSS 1, 7,22
48943 NGC 6405 0.40 −24.8 20.97 ± 2.70 22.96 Y BSS BSS 1,7,23
49934 NGC3532 0.47 −4.27 3.76 ± 0.81 27.7 N BSS BSS 9,22
57669 η Cha Association 0.54 −5.46 4.93 ± 2.52 20.7 Y BSS BSS 1,10,24
Cl Alessi 13 0.10 −12.61 10.25 ± 4.88 16.32 40 Y BSS 1,10,25
69491 NGC 6475 0.20 −16 13.10 ± 1.62 12.3 N BSS BSS 1,7,22
C 1439-661 0.183 −11.44 17.25 ± 5.64 17.95 Y BSS 1,7,22
76013 Cl Platais 10 None – – – – – BSS 1,7
81377 Sco-Cen OB 2 (c) 0.81 −0.742 2.65 ± 0.21 33.15 5-6 Y BSS BSS 11,12 (d),13,19
82286 Cl VDBH 205 0.96 −0.70 1.00 ± 0.71 169 13 Y BSS – 1,7
82868 Cl Alessi 13 0.65 −12.35 14.18 ± 5.86 27.74 40 Y BSS BSS 1,10,25
91599 NGC 6883 0.92 −10.73 9.46 ± 1.50 98.75 Y BSS BSS/DES 10,14,26
102274 Alessi-Teutsch 5 0.62 −2.7 2.72 ± 0.29 61.9 Y BSS BSS 1,10 (8),27
0.97 −3.03 3.01 ± 0.23 53.09 1,7 (f)
NGC 7160 0.86 −2.77 3.11 ± 0.54 48.58 Y BSS 1,10,23
109556 Cep OB3 < 2σ −3.70 – 52.55 5–7 Y – BSS 10 (g),15,19
Cep OB3 0.11 −2.95 2.69 ± 0.87 64.37 Y BSS BSS 12 (h)

Notes. The closest approach to the cluster center is chosen to be less than 1 pc if not stated otherwise. Identifications that differ from those of Hoogerwerf et al. (2001) are highlighted in boldface. Listed are the statistical p-values for best trajectories, times of flight to the parent cluster Tf using gravitational potential, relative ejection velocities Vrel with respect to the parent cluster, the corresponding cluster’s age Tc, the time of flight Trel calculated assuming a straight trajectory with 1σ errors, flag Flagage based on whether the cluster age is in line with the suggested mechanism with ‘Y’ meaning it is and ‘N’ meaning it is not a suitable site of origin, suggested ejection mechanism by us, and suggested mechanism by Hoogerwerf et al. (2001). References are given for the relevant input parameters, occasionally alternative entries are given when published values disagree.

(a)

Closest approach to cluster center at 7 pc.

(b)

Closest approach at 2.4 pc.

(c)

Closest approach at 12 pc.

(d)

New HIPPARCOS reduction van Leeuwen (2007).

(e)

Radial velocity vrad = −42.0 km s−1.

(f)

Radial velocity vrad = −21.0 km s−1.

(g)

Distance D = 0.66 kpc; PM = −1.759, −1.445 mas yr−1; radial velocity vrad = −22.9 km s−1.

(h)

d = 0.7 Kpc; PM = −0.581, −3.434 mas yr−1; radial velocity vrad = −22.9 km s−1.

References. Kinematic of clusters/associations: (1) PM, Par (Cantat-Gaudin et al. 2018); (2) RV (Carrera et al. 2019); (3) Mel’Nik & Dambis (2017) (10% er parallax); (4) Carrera et al. (2019); (5) Cantat-Gaudin & Anders (2020); (6) Kuhn et al. (2019); (7) RV (Soubiran et al. 2018); (8) Beccari et al. (2018); (9) Gaia Collaboration (2018); (10) Conrad et al. (2017); (11) PSR PM from Fomalont et al. (1997); (12) Mel’Nik & Dambis (2009); (13) Wright & Mamajek (2018); (14) PM from Dias et al. (2014); (15) Kharchenko et al. (2005); Age estimates of Clusters: (16) Richer et al. (2021); (17) Kharchenko et al. (2016); (18) Brown et al. 1994; (19) Brown et al. (1997); (20) Swiggum et al. (2021); (21) Reggiani et al. (2011); (22) Bossini et al. (2019); (23) Liu & Pang 2019; (24) Bell et al. (2015); (25) Zuckerman et al. (2019); (26) Joshi et al. (2016); (27) Dias et al. (2019).

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