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 2

Pulsation properties of the sample stars.

Nr.	IRAS	Type	ΔV_puls ^a	P_pulsation ^b	Ref.

1	04440+2605	RVTau	1.2	78.7	1, 2
2	07008+1050	Puls.	0.15	72 ± 3	3
3	07284-0940	RVTau	1.1	92 ± 3	4, 5
4	08011-3627	RVTau	0.5	76 ± 4	4
5	08544-4431	Puls.	0.15	~72	4, 6
6	09256-6324	Puls.	0.45	72 ± 1	4
7	10158-2844	pAGB	<0.25	−	7
8	10174-5704	pAGB	<0.10	−	4
9	10456-5712	pAGB	<0.25	−	4
10	11385-5517	pAGB	<0.10	−	8
11	12185-4856	RVTau	0.6	32.8642	9
12	12222-4652	Puls.	0.15	~60	4, 10
13	15469-5311	Puls.	0.15	~50	4
14	17038-4815	RVTau	1.50	37.9 ± 1.5	11
15	17243-4348	RVTau	0.8	100 ± 4	4, 12
16	17534+2603	Puls.	<0.25	65 ± 3	13, 14
17	18281+2149	RVTau	1.8	75 ± 2	10
18	19125+0343	pAGB	<0.15	−	4
19	22327-1731	pAGB	<0.05	−	4

Notes. Objects in which the characteristic RV Tau features have been identified in the light curve are listed as RV Tau. Otherwise, if a pulsation period has been detected it is listed as “Puls.”, and if no period is known in the literature the source is denoted as “pAGB”. The (maximum) amplitude of pulsational variability in the V band is given, as well as the main pulsation period wherever relevant.

^(a)

Peak-to-peak amplitude.

^(b)

The main pulsation period.

Reference.

⁽¹⁾

Taranova et al. (2009).

⁽²⁾

Zsoldos (1996).

⁽³⁾

Waelkens et al. (1991b).

⁽⁴⁾

Kiss et al. (2007).

⁽⁵⁾

Percy & Bakos (1998).

⁽⁶⁾

Maas et al. (2003).

⁽⁷⁾

Waelkens et al. (1991a).

⁽⁸⁾

Bakker et al. (1996).

⁽⁹⁾

Shenton et al. (1994).

⁽¹⁰⁾

Samus et al. (2009).

⁽¹¹⁾

Manick et al. (2017).

⁽¹²⁾

Maas (2003).

⁽¹³⁾

Dubath et al. (2011).

⁽¹⁴⁾

Percy et al. (2000).

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