J/A+A/496/813 Binary PNe towards the Galactic bulge (Miszalski+, 2009)
Binary planetary nebulae nuclei towards the Galactic bulge.
I. Sample discovery, period distribution and, binary fraction.
Miszalski B., Acker A., Moffat A.F.J, Parker Q.A., Udalski A.
<Astron. Astrophys. 496, 813 (2009)>
=2009A&A...496..813M 2009A&A...496..813M
ADC_Keywords: Planetary nebulae ; Binaries, eclipsing
Keywords: ISM: planetary nebulae: general - stars: binaries: general -
stars: binaries: eclipsing - stars: binaries: symbiotic
Abstract:
Binarity has been hypothesised to play an important, if not
ubiquitous, role in the formation of planetary nebulae (PNe). Yet
there remains a severe paucity of known binary central stars required
to test the binary hypothesis and to place strong constraints on the
physics of the common-envelope (CE) phase of binary stellar evolution.
Large photometric surveys offer an unrivalled opportunity to
efficiently discover many binary central stars. We have combined
photometry from the OGLE microlensing survey with the largest sample
of PNe towards the Galactic bulge to systematically search for new
binaries. A total of 21 periodic binaries were found thereby more than
doubling the known sample. The orbital period distribution was found
to be best described by CE population synthesis models when no
correlation between primary and secondary masses is assumed for the
initial mass ratio distribution. A comparison with post-CE white dwarf
binaries indicates both distributions are representative of the true
post-CE period distribution with most binaries exhibiting periods less
than one day. An estimated close binary fraction of 12-21% is
derived and is the first robust and independent validation of the
prevailing 10-15% fraction estimated by Bond (2000, in Asymmetrical
Planetary Nebulae II: From Origins to Microstructures, 199, 115). This
suggests that binarity is not a precondition for the formation of PNe
and that close binaries do not play a dominant role in the shaping of
nebular morphologies. Systematic effects and biases of the survey are
discussed with implications for future photometric surveys.
Description:
Coordinates for 288 planetary nebulae searched for photometric
variations in OGLE-III. Remarks are given according to the central
star (CSPN) identification process detailed in the paper. For each
planetary nebula the OGLE-III field, PN G designation, common name,
equatorial coordinates and central star ID are given.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 65 288 Coordinates and central star ID remarks
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See also:
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Field OGLE-III field (BLGNNN)
7 A1 --- --- [,]
8- 10 I3 --- Field2 ? Second OGLE-III field number (NNN)
12- 22 A11 --- PNG PN G designation (lll.l+bb.b)
24- 36 A13 --- Name Common name of the planetary nebula
38- 39 I2 h RAh Right ascension (J2000.0)
41- 42 I2 min RAm Right ascension (J2000.0)
44- 47 F4.1 s RAs Right ascension (J2000.0)
49 A1 --- DE- Declination sign (J2000.0)
50- 51 I2 deg DEd Declination (J2000.0)
53- 54 I2 arcmin DEm Declination (J2000.0)
56- 57 I2 arcsec DEs Declination (J2000.0)
59- 65 A7 --- Rem Central star (CSPN) ID remarks (1)
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Note (1): The following remarks have been used:
P = Possible CSPN
L = Likely CSPN
T = True CSPN
B = Blue CSPN
B? = Likely Blue CSPN
S = Photometry affected by systematic effects
S? = Photometry likely affected by systematic effects
NEB = Nebular rim or other faint nebula detection not coincident with CSPN
NULL = Photometry not extracted for technical reasons (see text)
NONE = No candidate CSPN identified
BIN = Photometry Binary CSPN
BIN? = Likely Photometric Binary CSPN
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Acknowledgements:
Brent Miszalski, bmiszalski(at)gmail.com
(End) Brent Miszalski [Obs. Strasbourg], Patricia Vannier [CDS] 30-Jan-2009