J/MNRAS/498/6005 PN ETHOS 1 Bgri magnitudes & radial velocities (Munday+, 2020)
The post-common-envelope binary central star of the planetary nebula ETHOS 1.
Munday J., Jones D., Garcia-Rojas J., Boffin H.M.J., Miszalski B.,
Corradi R.L.M., Rodriguez-Gil P., Rubio-Diez M.M., Santander-Garcia M.,
Sowicka P.
<Mon. Not. R. Astron. Soc. 498, 6005-5012 (2020)>
=2020MNRAS.498.6005M 2020MNRAS.498.6005M (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; Photometry ; Optical ; Radial velocities
Keywords: stars: AGB and post-AGB - binaries: close -
planetary nebulae: individual: PN G068.1+11.0 - white dwarfs -
Abstract:
We present a detailed study of the binary central star of the
planetary nebula ETHOS 1 (PN G068.1+11.0). Simultaneous modelling of
light and radial velocity curves reveals the binary to comprise a hot
and massive pre-white-dwarf with an M-type main-sequence companion. A
good fit to the observations was found with a companion that follows
expected mass-temperature-radius relationships for low-mass stars,
indicating that despite being highly irradiated it is consistent with
not being significantly hotter or larger than a typical star of the
same mass. Previous modelling indicated that ETHOS 1 may comprise the
first case where the orbital plane of the central binary does not lie
perpendicular to the nebular symmetry axis, at odds with the
expectation that the common envelope is ejected in the orbital plane.
We find no evidence for such a discrepancy, deriving a binary
inclination in agreement with that of the nebula as determined by
spatio-kinematic modelling. This makes ETHOS 1 the ninth
post-common-envelope planetary nebula in which the binary orbital and
nebular symmetry axes have been shown to be aligned, with as yet no
known counter-examples. The probability of finding such a correlation
by chance is now less than 0.00002%.
Description:
Time-series photometry of ETHOS 1 in the i band, acquired using the
MEROPE camera mounted on the 1.2-m Flemish Mercator Telescope between
2009 August 24 and September 4, was already presented in Miszalski et
al. (2011MNRAS.413.1264M 2011MNRAS.413.1264M). The same data are reanalysed here in order
to provide a longer time baseline with which to constrain the orbital
period as well as model the photometric variability.
Time resolved photometric and radial velocity observations of the
binary central star system of the planetary nebula ETHOS 1.
Objects:
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RA (2000) DE Designation(s) (Per)
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19 16 31.50 +36 09 47.9 ETHOS 1 = PN G068.1+11.0 (0.5351263)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
bmag.dat 34 110 B-band light curve
gmag.dat 34 36 g-band light curve
rmag.dat 34 106 r-band light curve
imag.dat 34 183 i-band light curve
rv.dat 31 21 Radial velocity curve
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Byte-by-byte Description of file: bmag.dat gmag.dat rmag.dat imag.dat
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Bytes Format Units Label Explanations
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3- 15 F13.5 d JD Heliocentric Julian Date
19- 24 F6.3 mag mag Apparent magnitude in Band
28- 32 F5.3 mag e_mag Uncertainty of magnitude in Band
34 A1 --- Band [Bgri] Observed band
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Byte-by-byte Description of file: rv.dat
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Bytes Format Units Label Explanations
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3- 15 F13.5 d JD Heliocentric Julian Date
19- 24 F6.1 km/s RV Radial velocity
28- 31 F4.1 km/s e_RV Uncertainty of radial velocity measurement
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Acknowledgements:
David Jones, djones(at)iac.es
James Munday, jm01398(at)surrey.ac.uk
(End) Patricia Vannier [CDS] 11-Sep-2020