Establishing binarity amongst Galactic RV Tauri stars with a disc

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Table 4

Pulsation periods derived from the photometric and spectroscopic time series.


	Spectroscopy		Photometry


Star	P_Puls.	P_Puls.	S/N_Puls.	Amplitude	Phot. type
	(days)	(days)		(mag)


DY Ori	30	30.4, 60.9²	7.7, 6.7	0.23, 0.11	RVa^a
EP Lyr	42, 83	41.6, 83.8²	3.8, 4.6	0.25, 0.22	RVa^b
HP Lyr	68	68.4¹	4.8	0.11	RVa^c
IRAS 17038−4815	38	37.9, 19.0, 69.3, 1356.2²^*	16.0, 5.3, 4.8, 4.9	0.44, 0.09, 0.08, 0.08	RVb^a
IRAS 09144−4933	50	1758.0^*, 85.4, 50.3²	6., 4.6, 4.0	0.12, 0.07, 0.07	RVb^a
TW Cam	43	43.5, 671.0¹^*	7.2, 5.9	0.08, 0.07	RVb^a

Notes. Column 2 shows the pulsation periods in the radial velocities with peaks in the Lomb-Scargle periodogram above a S/N of 4. Column 3 shows the pulsation periods found in the photometry. We indicate in Col. 4 the S/N in the Lomb-Scargle periodogram associated with each pulsation period in the photometry. The amplitudes of the pulsations are shown in Col. 5.

⁽¹⁾

Data from AAVSO.

⁽²⁾

Data from ASAS.

^(a)

This work.

^(b)

Zsoldos (1995).

^(c)

Graczyk et al. (2002).

^(*)

The italicised numbers in Col. 3 are the spectroscopic orbital periods found in the photometry, which confirms their RVb nature.

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