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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 65 288 Coordinates and central star ID remarks
See also: V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
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)
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
Acknowledgements: Brent Miszalski, bmiszalski(at)
(End) Brent Miszalski [Obs. Strasbourg], Patricia Vannier [CDS] 30-Jan-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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