Improving the surface brightness-color relation for early-type stars using optical interferometry

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Volume 570 (October 2014)

A&A, 570 (2014) A104

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Table 1

Physical parameters of the stars in our sample.


	λ Aql	γ Lyr	γ Ori	8 Cyg	ι Her	ζ Per	ζ Peg	δ Cyg
	HD 177756	HD 176437	HD 35468	HD 184171	HD 160762	HD 24398	HD 214923	HD 186882


RA	19:06:14	18:58:56	05:25:07	19:31:46	17:39:27	03:54:07	22:41:27	19:44:58
Dec	+ 04°52′57′′	+ 32°41′22′′	+ 06°20′58′′	+ 34°27′10′′	+ 46°00′22′′	+ 31°53′01′′	+ 10°49′52′′	+ 45°07′50′′
S. Type^a	B9V	A1III	B2III	B3IV	B3IV	B1Ib	B9IV	A0IV
m_V [ mag ]^b	3.430	3.248	1.637	4.740	3.794	2.850	3.406	2.868
m_K [ mag ]^b	3.670	3.240	2.340	5.114	4.228	2.670	3.565	2.810
π [ mas ] ^c	26.37 ± 0.64	5.26 ± 0.27	12.92 ± 0.52	3.79 ± 0.16	7.17 ± 0.13	4.34 ± 0.19	15.96 ± 0.19	19.77 ± 0.48
A _V ^d	0.03 ± 0.01	0.12 ± 0.03	0.00 ± 0.06	0.15 ± 0.11	0.04 ± 0.03	0.87 ± 0.05	0.05 ± 0.01	0.04 ± 0.01
E(V − K) ^e	0.03 ± 0.01	0.11 ± 0.03	0.00 ± 0.05	0.12 ± 0.10	0.03 ± 0.03	0.77 ± 0.05	0.04 ± 0.01	0.04 ± 0.01


T_eff [ K ]	11 780 ^a	10 000 ^a	21 840 ^a	16 100 ^m	17 000 ^m	22 580 ^a	11 430 ^a	10 150 ^a
M [ M_⊙ ]	2.99 ^j	5.76 ^k	7.77 ^j	6.40 ^m	6.30 ^m	15.50 ^l	3.22 ^j	2.93 ^j
R [ R_⊙ ]	2.24 ^j	15.40 ^k	5.75 ^j	6.50 ^m	5.40 ^m	26 ^f	3.98 ^j	5.13 ^j
L [ L_⊙ ]	78 ^g	2430 ^k	9211 ⁿ	2512 ^m	2138 ^m	47039 ^h	224 ^g	155 ⁿ
log g	4.22 ^j	4.06 ^o	3.84 ^o	3.62 ^m	3.77 ^m	3.27 ^o	3.75 ^j	3.49 ^j
[ Fe/H ]	−0.08 ^o	0.15 ^o	−0.07 ^o	0.25 ⁱ	−0.04 ^o	−0.08 ^o	0.06 ^o	−

Notes.

^(a)

Zorec et al. (2009);

^(b)

magnitudes from the General Catalogue of Photometric Data Mermilliod et al. (1997);

^(c)

van Leeuwen (2007);

^(d)

derived from Eq. (3) for stars with distances lower than 75 pc (λ Aql, ζ Peg, and δ Cyg), and from Eq. (4) for more distant stars;

^(e)

average value based on the literature (Wegner 1994; Pecaut & Mamajek 2013; Ducati 2002; Fitzpatrick 1999), see the text for more explanations;

^(f)

Pasinetti Fracassini et al. (2001);

^(g)

Zorec & Royer (2012);

^(h)

Hohle et al. (2010);

⁽ⁱ⁾

Gies & Lambert (1992);

^(j)

Allende Prieto & Lambert (1999);

^(k)

Maestro et al. (2013);

^(l)

Tetzlaff et al. (2011);

^(m)

Fitzpatrick & Massa (2005);

⁽ⁿ⁾

McDonald et al. (2012);

^(o)

Wu et al. (2011).

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