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Table 2:

Polarization results of stars in direction to NGC 5617.

Stara 		Other ids.b $P_{\rm max} \pm \epsilon_{p} $ $\sigma_{1}$c $\lambda_{\rm max} \pm \epsilon_{\lambda}$ kin. memb.d this work
    $\%$   $\mu$m    
36 L96 3.31 $\pm$ 0.10 0.63 0.63 $\pm$ 0.05   nm
55 L180, RG 2.36 $\pm$ 0.22 1.04 0.49 $\pm$ 0.07 nm(M; FM) nm
65 L98 1.87 $\pm$ 0.19 1.25 0.72 $\pm$ 0.20   nm
68* L105, BS 4.26 $\pm$ 0.08 0.78 0.61 $\pm$ 0.03   member
79 L46 4.93 $\pm$ 0.39 1.61 0.70 $\pm$ 0.12   member
80 L158 4.61 $\pm$ 0.08 0.29 0.57 $\pm$ 0.02   nm
93 L94 4.60 $\pm$ 0.22 1.02 0.54 $\pm$ 0.06   member
94 L45 4.37 $\pm$ 0.10 0.59 0.50 $\pm$ 0.02   member
100 L47 5.05 $\pm$ 0.29 1.00 0.43 $\pm$ 0.03   member
106 L91 4.56 $\pm$ 0.17 0.71 0.49 $\pm$ 0.04   member
107 L48 4.50 $\pm$ 0.22 1.32 0.55 $\pm$ 0.06   member
116* L42 4.13 $\pm$ 0.03 1.37 0.55 $\pm$ 0.01 m(M; FM) member
136 L89 3.91 $\pm$ 0.23 1.80 0.61 $\pm$ 0.11   nm
139 L39 4.36 $\pm$ 0.17 1.10 0.52 $\pm$ 0.05   member
143 L51 3.36 $\pm$ 0.33 1.78 0.55 $\pm$ 0.13   nm
146 L49 4.33 $\pm$ 0.29 1.84 0.58 $\pm$ 0.08   member
154 L52 2.49 $\pm$ 0.27 3.47 0.57 $\pm$ 0.13   nm
169 L53 4.61 $\pm$ 0.15 0.92 0.49 $\pm$ 0.03   member
175 L15 4.31 $\pm$ 0.06 0.48 0.56 $\pm$ 0.02   member
176 L114 2.57 $\pm$ 0.09 0.55 0.51 $\pm$ 0.03   nm
180 L54 4.77 $\pm$ 0.05 0.47 0.53 $\pm$ 0.01 m(FM) member
182 L86, BS 4.18 $\pm$ 0.18 0.87 0.46 $\pm$ 0.03   poss.member
184 L87 4.76 $\pm$ 0.14 0.95 0.53 $\pm$ 0.04   member
185* L31, BS 4.43 $\pm$ 0.03 0.32 0.52 $\pm$ 0.01   member
186 L115 4.75 $\pm$ 0.07 0.43 0.56 $\pm$ 0.02   member
187* L2 1.83 $\pm$ 0.26 1.52 0.63 $\pm$ 0.20   nm
188 L85 4.57 $\pm$ 0.30 1.04 0.65 $\pm$ 0.10   member
190 L16 4.07 $\pm$ 0.09 0.83 0.55 $\pm$ 0.03   member
195* L1, BS 4.42 $\pm$ 0.62 2.21 0.44 $\pm$ 0.09   poss. member
196 L55 2.80 $\pm$ 0.28 1.39 0.45 $\pm$ 0.10   nm
202* L29, BS 4.83 $\pm$ 0.10 1.33 0.50 $\pm$ 0.02 nm(FM) member
203 L56 4.53 $\pm$ 0.11 0.65 0.52 $\pm$ 0.02   member
205* L3 4.51 $\pm$ 0.30 0.93 0.44 $\pm$ 0.05   member
207* L4 3.69 $\pm$ 0.16 1.01 0.52 $\pm$ 0.05   member
214 L116 4.23 $\pm$ 0.07 0.59 0.60 $\pm$ 0.02   member
215 L84 3.46 $\pm$ 0.11 0.98 0.56 $\pm$ 0.04   poss.member
216* L5 4.33 $\pm$ 0.06 0.51 0.57 $\pm$ 0.02   member
221 L57 3.72 $\pm$ 0.11 0.95 0.49 $\pm$ 0.03   member
225* L28 4.82 $\pm$ 0.17 0.94 0.51 $\pm$ 0.03   member
226* L26 4.16 $\pm$ 0.48 1.91 0.70 $\pm$ 0.22   member
227* L17, RG 4.38 $\pm$ 0.18 2.29 0.48 $\pm$ 0.03 m(M; FM) member
238 L59 3.95 $\pm$ 0.45 1.48 0.55 $\pm$ 0.13   member
244 L23 3.86 $\pm$ 0.12 0.66 0.55 $\pm$ 0.04   member
258* L81 4.01 $\pm$ 0.17 1.69 0.54 $\pm$ 0.05   member
259 L119 4.02 $\pm$ 0.42 1.06 0.45 $\pm$ 0.06   member
260 L118 3.20 $\pm$ 0.30 2.26 0.56 $\pm$ 0.14   member
261 L20, BS 3.98 $\pm$ 0.14 2.32 0.55 $\pm$ 0.04   poss.member
269 L120 3.46 $\pm$ 0.11 0.59 0.58 $\pm$ 0.05   nm
270 L82 4.31 $\pm$ 0.26 2.36 0.49 $\pm$ 0.05   poss.member
274 L62 4.19 $\pm$ 0.39 2.39 0.59 $\pm$ 0.13   member
275 L61 4.09 $\pm$ 0.57 1.58 0.47 $\pm$ 0.11   member
276 L68 4.71 $\pm$ 0.05 0.24 0.60 $\pm$ 0.01   member
379 L64 3.25 $\pm$ 0.15 1.11 0.57 $\pm$ 0.07   nm
292 L65 4.30 $\pm$ 0.37 1.67 0.43 $\pm$ 0.05   member
294 L66 3.90 $\pm$ 0.18 0.80 0.48 $\pm$ 0.04   member
295 L121 3.78 $\pm$ 0.10 0.54 0.58 $\pm$ 0.05   member
302 L122 4.35 $\pm$ 0.11 0.75 0.65 $\pm$ 0.04   member
321 L143 2.31 $\pm$ 0.29 0.69 0.42 $\pm$ 0.08   nm
327 L144 3.05 $\pm$ 0.21 1.55 0.56 $\pm$ 0.08   nm
330 L141 4.29 $\pm$ 0.13 1.94 0.57 $\pm$ 0.04   member
331 L123 3.30 $\pm$ 0.18 1.30 0.66 $\pm$ 0.11   nm
333 L129 5.32 $\pm$ 0.40 1.88 0.62 $\pm$ 0.13   nm
334 L138 4.64 $\pm$ 0.16 1.31 0.52 $\pm$ 0.05   member
336 L142 3.73 $\pm$ 0.53 1.75 0.71 $\pm$ 0.19   nm
339* L124 3.92 $\pm$ 0.20 1.08 0.55 $\pm$ 0.06   nm
342 L126 3.08 $\pm$ 0.07 0.79 0.63 $\pm$ 0.04 nm(M; FM) nm
347 L125 2.12 $\pm$ 0.13 1.39 0.60 $\pm$ 0.09 nm(M; FM) nm

Notes.  (a) Identifications from Haug (1978); (b) identifications from Lindoff (1968); RG: Red giant, BS: Blue straggler; (*) membership according to photometric studies; (c)  ${\sigma_{1}}^{2} = \sum {(r_{\lambda}/{\epsilon_{p_\lambda}})^2}/(m-2)$; where m is the number of colors and $r_{\lambda} = P_{\lambda} - P_{\rm max}~\exp(-K~{\rm ln}^2({\lambda_{\rm max}/{\lambda}))}$; (d) membership according to Mermilliod et al. (M) (2008) and/or Frinchaboy & Majewski (FM) (2008).


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