Planetary nebulae seen with TESS: New and revisited short-period binary central star candidates from Cycles 1 to 4

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Volume 690 (October 2024)

A&A, 690 (2024) A190

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Table 2

Results from the light curve analysis of those already known binary systems analysed with the parametric approach described in Sect. 3.1.

Name	BestModel	Period (days)	T₀ (2458300)	A_ref/A_1E (ppt)	A_beam (ppt)	A_ellip (ppt)
Abell30	1E	${1.06115}_{- 0.00013}^{+ 0.00013}$ $1.06115_{ - 0.00013}^{ + 0.00013}$	${55.06}_{- 0.15}^{+ 0.15}$ $55.06_{ - 0.15}^{ + 0.15}$	${14.14}_{- 0.25}^{+ 0.25}$ $14.14_{ - 0.25}^{ + 0.25}$	—	—
LoTr5	1E ⁽¹⁾	${5.8090049}_{- 0.0000036}^{+ 0.0000036}$ $5.8090049_{ - 0.0000036}^{ + 0.0000036}$	${71.35280}_{- 0.00064}^{+ 0.00064}$ $71.35280_{ - 0.00064}^{ + 0.00064}$	${13.8657}_{- 0.0033}^{+ 0.0033}$ $13.8657_{ - 0.0033}^{ + 0.0033}$	—	—
AMU1	1E ⁽²⁾	${2.9726}_{- 0.0014}^{+ 0.0013}$ $2.9726_{ - 0.0014}^{ + 0.0013}$	${57.94}_{- 0.54}^{+ 0.55}$ $57.94_{ - 0.54}^{ + 0.55}$	${0.424}_{- 0.077}^{+ 0.077}$ $0.424_{ - 0.077}^{ + 0.077}$	—	—
NGC5189	3E	${1.7151718}_{- 0.0000065}^{+ 0.0000065}$ $1.7151718_{ - 0.0000065}^{ + 0.0000065}$	${66.3145}_{- 0.0031}^{+ 0.0031}$ $66.3145_{ - 0.0031}^{ + 0.0031}$	${11.21}_{- 0.28}^{+ 0.28}$ $11.21_{ - 0.28}^{ + 0.28}$	${5.38}_{- 0.28}^{+ 0.28}$ $5.38_{ - 0.28}^{ + 0.28}$	${27.95}_{- 0.28}^{+ 0.28}$ $27.95_{ - 0.28}^{ + 0.28}$
NGC2392	3E	${2.13769}_{- 0.00016}^{+ 0.00016}$ $2.13769_{ - 0.00016}^{ + 0.00016}$	${73.949}_{- 0.091}^{+ 0.091}$ $73.949_{ - 0.091}^{ + 0.091}$	${1.310}_{- 0.011}^{+ 0.011}$ $1.310_{ - 0.011}^{ + 0.011}$	${0.913}_{- 0.013}^{+ 0.013}$ $0.913_{ - 0.013}^{ + 0.013}$	${0.7787}_{- 0.0097}^{+ 0.0097}$ $0.7787_{ - 0.0097}^{ + 0.0097}$

Notes. ⁽¹⁾This periodicity in LoTr 5 corresponds to the rotation period.⁽²⁾ Although the evidence for the flat model is larger in our analysis of AMU 1, we can recover the 1-effect model with similar evidence to the flat model by discarding the data with a high dispersion. The fit then converges to the known orbital period but still with insufficient significance (see Section 4.1).

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