Table 2. Open in new tab Gaia DR2...

	Parallax^*	Distance	Distance (BJ)			RV^†		Subsection
(1) IRAS 02143+5852	1.364 ± 0.289	>0.510		>0.74	3.778	−49.02 ± 14.69	18.689	3.4
(2) IRAS 05089+0459	0.754 ± 0.345	>0.684		>0.88	3.477	85.92 ± 1.49	21.908	3.4
(3) IRAS 05208−2035	0.687 ± 0.030	1.420 ± 0.064	1.403\|$^{+0.053}_{-0.059}$\|	2.91 ± 0.25	3.690	52.84 ± 3.68	2.184	3.4
(4) HD 46703	0.268 ± 0.024	3.512 ± 0.330	3.399\|$^{+0.276}_{-0.278}$\|	3.92 ± 0.26	3.778	−83.53 ± 7.71	1.622	3.2
(5) HD 56126	0.454 ± 0.024	2.124 ± 0.114	2.099\|$^{+0.108}_{-0.110}$\|	3.93 ± 0.25	3.813	93.71 ± 3.54	0.922	3.1
(6) IRAS 07140−2321	0.178 ± 0.012	5.116 ± 0.343	5.122\|$^{+0.377}_{-0.404}$\|	3.74 ± 0.26	3.845	62.38 ± 4.13	1.029	3.1
(7) IRAS 07227−1320	0.489 ± 0.021	1.975 ± 0.087	1.982\|$^{+0.068}_{-0.073}$\|	2.58 ± 0.25	3.544	70.68 ± 0.39	1.176	3.3
(8) IRAS 08187−1905	0.288 ± 0.033	3.280 ± 0.403	3.259\|$^{+0.342}_{-0.391}$\|	3.60 ± 0.12	3.789	65.44 ± 1.87	1.695	3.2
(9) HD 116745	0.177 ± 0.020	5.154 ± 0.597	4.893\|$^{+0.379}_{-0.444}$\|	3.20 ± 0.11	3.842	240.11 ± 0.54	0.933	3.1
(10) IRAS 14325−6428	0.192 ± 0.037	4.795 ± 1.033	4.883\|$^{+0.622}_{-0.928}$\|	2.77 ± 0.30	3.806	−76.54 ± 10.08	2.181	3.2
(11) IRAS 15210−6554	−0.152 ± 0.143	>6.623		>3.29	3.634	−83.90 ± 0.87	2.279	3.4
(12) HD 137569	0.752 ± 0.079	1.301 ± 0.150	1.316\|$^{+0.132}_{-0.197}$\|	3.19 ± 0.11	4.021	−45.0	2.023	3.2
(13) BD −33 2642	0.271 ± 0.032	3.474 ± 0.434	3.467\|$^{+0.308}_{-0.466}$\|	3.54 ± 0.12	4.301	−94.7 ± 2.5	1.295	3.1
(14) BD +32 2754	3.239 ± 0.014	0.307 ± 0.001	0.307\|$^{+0.001}_{-0.001}$\|	1.10 ± 0.06	3.760	−60.50 ± 0.50	1.161	3.3
(15) HD 161796	0.502 ± 0.024	1.926 ± 0.091	1.921\|$^{+0.091}_{-0.095}$\|	3.85 ± 0.07	3.813	−54.17 ± 1.78	1.216	3.1
(16) IRAS 18075−0924	−0.171 ± 0.192	>4.348				−59.68 ± 0.68	7.580	3.4
(17) BD −12 4970	0.467 ± 0.020	2.065 ± 0.090	1.984\|$^{+0.072}_{-0.101}$\|	5.50 ± 0.25	4.431	124.95 ± 9.43	0.956	3.1
(18) HD 178443	1.034 ± 0.016	0.951 ± 0.014	0.939\|$^{+0.014}_{-0.015}$\|	1.99 ± 0.06	3.714	343.55 ± 0.28	1.102	3.3
(19) PHL 1580	3.156 ± 0.018	0.315 ± 0.002	0.314\|$^{+0.001}_{-0.002}$\|	1.12 ± 0.06	4.380	−70.53 ± 0.72	0.954	3.3
(20) LS III +52 5	3.119 ± 0.011	0.319 ± 0.001	0.315\|$^{+0.001}_{-0.001}$\|	1.22 ± 0.06	4.398	−232.83 ± 0.67	0.817	3.3

Parallax^*

Distance

Distance (BJ)

RV^†

Subsection

Star

(mas)

(kpc)

log (L/|${L_{\odot}}$|⁠)^‡

log (T_eff/K)

(km s⁻¹)

RUWE

in section 3

(1) IRAS 02143+5852

1.364 ± 0.289

>0.510

>0.74

3.778

−49.02 ± 14.69

18.689

3.4

(2) IRAS 05089+0459

0.754 ± 0.345

>0.684

>0.88

3.477

85.92 ± 1.49

21.908

3.4

(3) IRAS 05208−2035

0.687 ± 0.030

1.420 ± 0.064

1.403|$^{+0.053}_{-0.059}$|

2.91 ± 0.25

3.690

52.84 ± 3.68

2.184

3.4

(4) HD 46703

0.268 ± 0.024

3.512 ± 0.330

3.399|$^{+0.276}_{-0.278}$|

3.92 ± 0.26

3.778

−83.53 ± 7.71

1.622

3.2

(5) HD 56126

0.454 ± 0.024

2.124 ± 0.114

2.099|$^{+0.108}_{-0.110}$|

3.93 ± 0.25

3.813

93.71 ± 3.54

0.922

3.1

(6) IRAS 07140−2321

0.178 ± 0.012

5.116 ± 0.343

5.122|$^{+0.377}_{-0.404}$|

3.74 ± 0.26

3.845

62.38 ± 4.13

1.029

3.1

(7) IRAS 07227−1320

0.489 ± 0.021

1.975 ± 0.087

1.982|$^{+0.068}_{-0.073}$|

2.58 ± 0.25

3.544

70.68 ± 0.39

1.176

3.3

(8) IRAS 08187−1905

0.288 ± 0.033

3.280 ± 0.403

3.259|$^{+0.342}_{-0.391}$|

3.60 ± 0.12

3.789

65.44 ± 1.87

1.695

3.2

(9) HD 116745

0.177 ± 0.020

5.154 ± 0.597

4.893|$^{+0.379}_{-0.444}$|

3.20 ± 0.11

3.842

240.11 ± 0.54

0.933

3.1

(10) IRAS 14325−6428

0.192 ± 0.037

4.795 ± 1.033

4.883|$^{+0.622}_{-0.928}$|

2.77 ± 0.30

3.806

−76.54 ± 10.08

2.181

3.2

(11) IRAS 15210−6554

−0.152 ± 0.143

>6.623

>3.29

3.634

−83.90 ± 0.87

2.279

3.4

(12) HD 137569

0.752 ± 0.079

1.301 ± 0.150

1.316|$^{+0.132}_{-0.197}$|

3.19 ± 0.11

4.021

−45.0

2.023

3.2

(13) BD −33 2642

0.271 ± 0.032

3.474 ± 0.434

3.467|$^{+0.308}_{-0.466}$|

3.54 ± 0.12

4.301

−94.7 ± 2.5

1.295

3.1

(14) BD +32 2754

3.239 ± 0.014

0.307 ± 0.001

0.307|$^{+0.001}_{-0.001}$|

1.10 ± 0.06

3.760

−60.50 ± 0.50

1.161

3.3

(15) HD 161796

0.502 ± 0.024

1.926 ± 0.091

1.921|$^{+0.091}_{-0.095}$|

3.85 ± 0.07

3.813

−54.17 ± 1.78

1.216

3.1

(16) IRAS 18075−0924

−0.171 ± 0.192

>4.348

−59.68 ± 0.68

7.580

3.4

(17) BD −12 4970

0.467 ± 0.020

2.065 ± 0.090

1.984|$^{+0.072}_{-0.101}$|

5.50 ± 0.25

4.431

124.95 ± 9.43

0.956

3.1

(18) HD 178443

1.034 ± 0.016

0.951 ± 0.014

0.939|$^{+0.014}_{-0.015}$|

1.99 ± 0.06

3.714

343.55 ± 0.28

1.102

3.3

(19) PHL 1580

3.156 ± 0.018

0.315 ± 0.002

0.314|$^{+0.001}_{-0.002}$|

1.12 ± 0.06

4.380

−70.53 ± 0.72

0.954

3.3

(20) LS III +52 5

3.119 ± 0.011

0.319 ± 0.001

0.315|$^{+0.001}_{-0.001}$|

1.22 ± 0.06

4.398

−232.83 ± 0.67

0.817

3.3

	Parallax^*	Distance	Distance (BJ)			RV^†		Subsection
(1) IRAS 02143+5852	1.364 ± 0.289	>0.510		>0.74	3.778	−49.02 ± 14.69	18.689	3.4
(2) IRAS 05089+0459	0.754 ± 0.345	>0.684		>0.88	3.477	85.92 ± 1.49	21.908	3.4
(3) IRAS 05208−2035	0.687 ± 0.030	1.420 ± 0.064	1.403\|$^{+0.053}_{-0.059}$\|	2.91 ± 0.25	3.690	52.84 ± 3.68	2.184	3.4
(4) HD 46703	0.268 ± 0.024	3.512 ± 0.330	3.399\|$^{+0.276}_{-0.278}$\|	3.92 ± 0.26	3.778	−83.53 ± 7.71	1.622	3.2
(5) HD 56126	0.454 ± 0.024	2.124 ± 0.114	2.099\|$^{+0.108}_{-0.110}$\|	3.93 ± 0.25	3.813	93.71 ± 3.54	0.922	3.1
(6) IRAS 07140−2321	0.178 ± 0.012	5.116 ± 0.343	5.122\|$^{+0.377}_{-0.404}$\|	3.74 ± 0.26	3.845	62.38 ± 4.13	1.029	3.1
(7) IRAS 07227−1320	0.489 ± 0.021	1.975 ± 0.087	1.982\|$^{+0.068}_{-0.073}$\|	2.58 ± 0.25	3.544	70.68 ± 0.39	1.176	3.3
(8) IRAS 08187−1905	0.288 ± 0.033	3.280 ± 0.403	3.259\|$^{+0.342}_{-0.391}$\|	3.60 ± 0.12	3.789	65.44 ± 1.87	1.695	3.2
(9) HD 116745	0.177 ± 0.020	5.154 ± 0.597	4.893\|$^{+0.379}_{-0.444}$\|	3.20 ± 0.11	3.842	240.11 ± 0.54	0.933	3.1
(10) IRAS 14325−6428	0.192 ± 0.037	4.795 ± 1.033	4.883\|$^{+0.622}_{-0.928}$\|	2.77 ± 0.30	3.806	−76.54 ± 10.08	2.181	3.2
(11) IRAS 15210−6554	−0.152 ± 0.143	>6.623		>3.29	3.634	−83.90 ± 0.87	2.279	3.4
(12) HD 137569	0.752 ± 0.079	1.301 ± 0.150	1.316\|$^{+0.132}_{-0.197}$\|	3.19 ± 0.11	4.021	−45.0	2.023	3.2
(13) BD −33 2642	0.271 ± 0.032	3.474 ± 0.434	3.467\|$^{+0.308}_{-0.466}$\|	3.54 ± 0.12	4.301	−94.7 ± 2.5	1.295	3.1
(14) BD +32 2754	3.239 ± 0.014	0.307 ± 0.001	0.307\|$^{+0.001}_{-0.001}$\|	1.10 ± 0.06	3.760	−60.50 ± 0.50	1.161	3.3
(15) HD 161796	0.502 ± 0.024	1.926 ± 0.091	1.921\|$^{+0.091}_{-0.095}$\|	3.85 ± 0.07	3.813	−54.17 ± 1.78	1.216	3.1
(16) IRAS 18075−0924	−0.171 ± 0.192	>4.348				−59.68 ± 0.68	7.580	3.4
(17) BD −12 4970	0.467 ± 0.020	2.065 ± 0.090	1.984\|$^{+0.072}_{-0.101}$\|	5.50 ± 0.25	4.431	124.95 ± 9.43	0.956	3.1
(18) HD 178443	1.034 ± 0.016	0.951 ± 0.014	0.939\|$^{+0.014}_{-0.015}$\|	1.99 ± 0.06	3.714	343.55 ± 0.28	1.102	3.3
(19) PHL 1580	3.156 ± 0.018	0.315 ± 0.002	0.314\|$^{+0.001}_{-0.002}$\|	1.12 ± 0.06	4.380	−70.53 ± 0.72	0.954	3.3
(20) LS III +52 5	3.119 ± 0.011	0.319 ± 0.001	0.315\|$^{+0.001}_{-0.001}$\|	1.22 ± 0.06	4.398	−232.83 ± 0.67	0.817	3.3

Parallax^*

Distance

Distance (BJ)

RV^†

Subsection

Star

(mas)

(kpc)

log (L/|${L_{\odot}}$|⁠)^‡

log (T_eff/K)

(km s⁻¹)

RUWE

in section 3

(1) IRAS 02143+5852

1.364 ± 0.289

>0.510

>0.74

3.778

−49.02 ± 14.69

18.689

3.4

(2) IRAS 05089+0459

0.754 ± 0.345

>0.684

>0.88

3.477

85.92 ± 1.49

21.908

3.4

(3) IRAS 05208−2035

0.687 ± 0.030

1.420 ± 0.064

1.403|$^{+0.053}_{-0.059}$|

2.91 ± 0.25

3.690

52.84 ± 3.68

2.184

3.4

(4) HD 46703

0.268 ± 0.024

3.512 ± 0.330

3.399|$^{+0.276}_{-0.278}$|

3.92 ± 0.26

3.778

−83.53 ± 7.71

1.622

3.2

(5) HD 56126

0.454 ± 0.024

2.124 ± 0.114

2.099|$^{+0.108}_{-0.110}$|

3.93 ± 0.25

3.813

93.71 ± 3.54

0.922

3.1

(6) IRAS 07140−2321

0.178 ± 0.012

5.116 ± 0.343

5.122|$^{+0.377}_{-0.404}$|

3.74 ± 0.26

3.845

62.38 ± 4.13

1.029

3.1

(7) IRAS 07227−1320

0.489 ± 0.021

1.975 ± 0.087

1.982|$^{+0.068}_{-0.073}$|

2.58 ± 0.25

3.544

70.68 ± 0.39

1.176

3.3

(8) IRAS 08187−1905

0.288 ± 0.033

3.280 ± 0.403

3.259|$^{+0.342}_{-0.391}$|

3.60 ± 0.12

3.789

65.44 ± 1.87

1.695

3.2

(9) HD 116745

0.177 ± 0.020

5.154 ± 0.597

4.893|$^{+0.379}_{-0.444}$|

3.20 ± 0.11

3.842

240.11 ± 0.54

0.933

3.1

(10) IRAS 14325−6428

0.192 ± 0.037

4.795 ± 1.033

4.883|$^{+0.622}_{-0.928}$|

2.77 ± 0.30

3.806

−76.54 ± 10.08

2.181

3.2

(11) IRAS 15210−6554

−0.152 ± 0.143

>6.623

>3.29

3.634

−83.90 ± 0.87

2.279

3.4

(12) HD 137569

0.752 ± 0.079

1.301 ± 0.150

1.316|$^{+0.132}_{-0.197}$|

3.19 ± 0.11

4.021

−45.0

2.023

3.2

(13) BD −33 2642

0.271 ± 0.032

3.474 ± 0.434

3.467|$^{+0.308}_{-0.466}$|

3.54 ± 0.12

4.301

−94.7 ± 2.5

1.295

3.1

(14) BD +32 2754

3.239 ± 0.014

0.307 ± 0.001

0.307|$^{+0.001}_{-0.001}$|

1.10 ± 0.06

3.760

−60.50 ± 0.50

1.161

3.3

(15) HD 161796

0.502 ± 0.024

1.926 ± 0.091

1.921|$^{+0.091}_{-0.095}$|

3.85 ± 0.07

3.813

−54.17 ± 1.78

1.216

3.1

(16) IRAS 18075−0924

−0.171 ± 0.192

>4.348

−59.68 ± 0.68

7.580

3.4

(17) BD −12 4970

0.467 ± 0.020

2.065 ± 0.090

1.984|$^{+0.072}_{-0.101}$|

5.50 ± 0.25

4.431

124.95 ± 9.43

0.956

3.1

(18) HD 178443

1.034 ± 0.016

0.951 ± 0.014

0.939|$^{+0.014}_{-0.015}$|

1.99 ± 0.06

3.714

343.55 ± 0.28

1.102

3.3

(19) PHL 1580

3.156 ± 0.018

0.315 ± 0.002

0.314|$^{+0.001}_{-0.002}$|

1.12 ± 0.06

4.380

−70.53 ± 0.72

0.954

3.3

(20) LS III +52 5

3.119 ± 0.011

0.319 ± 0.001

0.315|$^{+0.001}_{-0.001}$|

1.22 ± 0.06

4.398

−232.83 ± 0.67

0.817

3.3

Table 2.

Open in new tab

Gaia DR2 parallaxes and derived luminosities of 20 high-velocity post-AGB candidates.

	Parallax^*	Distance	Distance (BJ)			RV^†		Subsection
Star	(mas)	(kpc)	(kpc)	log (L/\|${L_{\odot}}$\|⁠)^‡	log (T_eff/K)	(km s⁻¹)	RUWE	in section 3
(1) IRAS 02143+5852	1.364 ± 0.289	>0.510		>0.74	3.778	−49.02 ± 14.69	18.689	3.4
(2) IRAS 05089+0459	0.754 ± 0.345	>0.684		>0.88	3.477	85.92 ± 1.49	21.908	3.4
(3) IRAS 05208−2035	0.687 ± 0.030	1.420 ± 0.064	1.403\|$^{+0.053}_{-0.059}$\|	2.91 ± 0.25	3.690	52.84 ± 3.68	2.184	3.4
(4) HD 46703	0.268 ± 0.024	3.512 ± 0.330	3.399\|$^{+0.276}_{-0.278}$\|	3.92 ± 0.26	3.778	−83.53 ± 7.71	1.622	3.2
(5) HD 56126	0.454 ± 0.024	2.124 ± 0.114	2.099\|$^{+0.108}_{-0.110}$\|	3.93 ± 0.25	3.813	93.71 ± 3.54	0.922	3.1
(6) IRAS 07140−2321	0.178 ± 0.012	5.116 ± 0.343	5.122\|$^{+0.377}_{-0.404}$\|	3.74 ± 0.26	3.845	62.38 ± 4.13	1.029	3.1
(7) IRAS 07227−1320	0.489 ± 0.021	1.975 ± 0.087	1.982\|$^{+0.068}_{-0.073}$\|	2.58 ± 0.25	3.544	70.68 ± 0.39	1.176	3.3
(8) IRAS 08187−1905	0.288 ± 0.033	3.280 ± 0.403	3.259\|$^{+0.342}_{-0.391}$\|	3.60 ± 0.12	3.789	65.44 ± 1.87	1.695	3.2
(9) HD 116745	0.177 ± 0.020	5.154 ± 0.597	4.893\|$^{+0.379}_{-0.444}$\|	3.20 ± 0.11	3.842	240.11 ± 0.54	0.933	3.1
(10) IRAS 14325−6428	0.192 ± 0.037	4.795 ± 1.033	4.883\|$^{+0.622}_{-0.928}$\|	2.77 ± 0.30	3.806	−76.54 ± 10.08	2.181	3.2
(11) IRAS 15210−6554	−0.152 ± 0.143	>6.623		>3.29	3.634	−83.90 ± 0.87	2.279	3.4
(12) HD 137569	0.752 ± 0.079	1.301 ± 0.150	1.316\|$^{+0.132}_{-0.197}$\|	3.19 ± 0.11	4.021	−45.0	2.023	3.2
(13) BD −33 2642	0.271 ± 0.032	3.474 ± 0.434	3.467\|$^{+0.308}_{-0.466}$\|	3.54 ± 0.12	4.301	−94.7 ± 2.5	1.295	3.1
(14) BD +32 2754	3.239 ± 0.014	0.307 ± 0.001	0.307\|$^{+0.001}_{-0.001}$\|	1.10 ± 0.06	3.760	−60.50 ± 0.50	1.161	3.3
(15) HD 161796	0.502 ± 0.024	1.926 ± 0.091	1.921\|$^{+0.091}_{-0.095}$\|	3.85 ± 0.07	3.813	−54.17 ± 1.78	1.216	3.1
(16) IRAS 18075−0924	−0.171 ± 0.192	>4.348				−59.68 ± 0.68	7.580	3.4
(17) BD −12 4970	0.467 ± 0.020	2.065 ± 0.090	1.984\|$^{+0.072}_{-0.101}$\|	5.50 ± 0.25	4.431	124.95 ± 9.43	0.956	3.1
(18) HD 178443	1.034 ± 0.016	0.951 ± 0.014	0.939\|$^{+0.014}_{-0.015}$\|	1.99 ± 0.06	3.714	343.55 ± 0.28	1.102	3.3
(19) PHL 1580	3.156 ± 0.018	0.315 ± 0.002	0.314\|$^{+0.001}_{-0.002}$\|	1.12 ± 0.06	4.380	−70.53 ± 0.72	0.954	3.3
(20) LS III +52 5	3.119 ± 0.011	0.319 ± 0.001	0.315\|$^{+0.001}_{-0.001}$\|	1.22 ± 0.06	4.398	−232.83 ± 0.67	0.817	3.3

	Parallax^*	Distance	Distance (BJ)			RV^†		Subsection
Star	(mas)	(kpc)	(kpc)	log (L/\|${L_{\odot}}$\|⁠)^‡	log (T_eff/K)	(km s⁻¹)	RUWE	in section 3
(1) IRAS 02143+5852	1.364 ± 0.289	>0.510		>0.74	3.778	−49.02 ± 14.69	18.689	3.4
(2) IRAS 05089+0459	0.754 ± 0.345	>0.684		>0.88	3.477	85.92 ± 1.49	21.908	3.4
(3) IRAS 05208−2035	0.687 ± 0.030	1.420 ± 0.064	1.403\|$^{+0.053}_{-0.059}$\|	2.91 ± 0.25	3.690	52.84 ± 3.68	2.184	3.4
(4) HD 46703	0.268 ± 0.024	3.512 ± 0.330	3.399\|$^{+0.276}_{-0.278}$\|	3.92 ± 0.26	3.778	−83.53 ± 7.71	1.622	3.2
(5) HD 56126	0.454 ± 0.024	2.124 ± 0.114	2.099\|$^{+0.108}_{-0.110}$\|	3.93 ± 0.25	3.813	93.71 ± 3.54	0.922	3.1
(6) IRAS 07140−2321	0.178 ± 0.012	5.116 ± 0.343	5.122\|$^{+0.377}_{-0.404}$\|	3.74 ± 0.26	3.845	62.38 ± 4.13	1.029	3.1
(7) IRAS 07227−1320	0.489 ± 0.021	1.975 ± 0.087	1.982\|$^{+0.068}_{-0.073}$\|	2.58 ± 0.25	3.544	70.68 ± 0.39	1.176	3.3
(8) IRAS 08187−1905	0.288 ± 0.033	3.280 ± 0.403	3.259\|$^{+0.342}_{-0.391}$\|	3.60 ± 0.12	3.789	65.44 ± 1.87	1.695	3.2
(9) HD 116745	0.177 ± 0.020	5.154 ± 0.597	4.893\|$^{+0.379}_{-0.444}$\|	3.20 ± 0.11	3.842	240.11 ± 0.54	0.933	3.1
(10) IRAS 14325−6428	0.192 ± 0.037	4.795 ± 1.033	4.883\|$^{+0.622}_{-0.928}$\|	2.77 ± 0.30	3.806	−76.54 ± 10.08	2.181	3.2
(11) IRAS 15210−6554	−0.152 ± 0.143	>6.623		>3.29	3.634	−83.90 ± 0.87	2.279	3.4
(12) HD 137569	0.752 ± 0.079	1.301 ± 0.150	1.316\|$^{+0.132}_{-0.197}$\|	3.19 ± 0.11	4.021	−45.0	2.023	3.2
(13) BD −33 2642	0.271 ± 0.032	3.474 ± 0.434	3.467\|$^{+0.308}_{-0.466}$\|	3.54 ± 0.12	4.301	−94.7 ± 2.5	1.295	3.1
(14) BD +32 2754	3.239 ± 0.014	0.307 ± 0.001	0.307\|$^{+0.001}_{-0.001}$\|	1.10 ± 0.06	3.760	−60.50 ± 0.50	1.161	3.3
(15) HD 161796	0.502 ± 0.024	1.926 ± 0.091	1.921\|$^{+0.091}_{-0.095}$\|	3.85 ± 0.07	3.813	−54.17 ± 1.78	1.216	3.1
(16) IRAS 18075−0924	−0.171 ± 0.192	>4.348				−59.68 ± 0.68	7.580	3.4
(17) BD −12 4970	0.467 ± 0.020	2.065 ± 0.090	1.984\|$^{+0.072}_{-0.101}$\|	5.50 ± 0.25	4.431	124.95 ± 9.43	0.956	3.1
(18) HD 178443	1.034 ± 0.016	0.951 ± 0.014	0.939\|$^{+0.014}_{-0.015}$\|	1.99 ± 0.06	3.714	343.55 ± 0.28	1.102	3.3
(19) PHL 1580	3.156 ± 0.018	0.315 ± 0.002	0.314\|$^{+0.001}_{-0.002}$\|	1.12 ± 0.06	4.380	−70.53 ± 0.72	0.954	3.3
(20) LS III +52 5	3.119 ± 0.011	0.319 ± 0.001	0.315\|$^{+0.001}_{-0.001}$\|	1.22 ± 0.06	4.398	−232.83 ± 0.67	0.817	3.3

From Gaia EDR3 (Lindegren et al. 2021).

†

From Gaia DR2 except for IRAS 07140−2321, HD 137569, and BD +33 2642, for which the values are respectively taken from RAVE DR6 (Steinmetz et al. 2020), Duflot, Figon, and Meyssonnier (1995), and Gontcharov (2006).

‡

The luminosity uncertainty includes the uncertainty in distance and reddening (section 2). In case the relative parallax measurement uncertainty is larger than |$20\%$|⁠, we provide 2σ lower limits.

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