A mid-IR interferometric survey with MIDI/VLTI: resolving the second-generation protoplanetary disks around post-AGB binaries

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Volume 599 (March 2017)

A&A, 599 (2017) A41

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Table 3

Stellar parameters resulting from the SED fitting.

Nr.	IRAS	E(B−V)	T _eff	θ _⋆	[Fe/H]
		(mag)	(K)	(mas)	(dex)

1	04440+2605	0.5	4875	0.44	−0.5
		0.5	4550	0.31	−0.5
2	07008+1050	0.04	6050	0.270	−4.0
3	07284-0940	0.18	5050	1.2	−1.0
		0.16	5025	0.58	−1.0
4	08011-3627	0.4	5925	0.22	−1.0
		0.2	5875	0.14	−1.0
5	08544-4431	1.40	7225	0.54	−0.5
6	09256-6324	0.7	6700	0.38	−1.0
7	10158-2844	0.21	7750	0.49	−4.0
8	10174-5704	0.88	3500	1.09	0.0^b
9	10456-5712	0.34	4275	1.8	0.0^b
10	11385-5517	0.35	8350	0.26	0.0^c
11	12185-4856	0.3	5925	0.18	−1.0
		0.3	5850	0.138	−1.0
12	12222-4652	0.17	7000	0.178	0.0
13	15469-5311	1.34	7425	0.23	0.0
14	17038-4815	0.3	4375	0.29	−1.5
		0.7	4575	0.18	−1.5
15	17243-4348	0.3	5075	0.16	0.0
		0.3	4850	0.14	0.0
16	17534+2603	0.07	6850	0.52	0.0
17	18281+2149	0.26	6200	0.39	−1.5
		0.03	4800	0.318	−1.5
18	19125+0343	0.79	7275	0.140	−0.5
19	22327-1731	0.12	8275	0.085	−1.0

Notes. The pulsating sources have two entries, one for a minimum and a maximum pulsation phase. Metallicities are taken from de Ruyter et al. (2006) unless otherwise noted. ,

^(a)

H band fluxes are also included in the fit for sources 1, 8 and 17

^(b)

This metallicity is assumed.

^(c)

The spectroscopic constraints for this source come from Kipper (2005).

^(f)

We are cautious about IRAS 10174-5704, given the limited data and the limiting T_eff = 3500 K in the atmosphere grid.

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