J/A+A/682/A70 Binary central stars of LMC PNe (Gladkowski+, 2024)
Binary central stars of planetary nebulae in the Large Magellanic Cloud.
Gladkowski M., Hajduk M., Smolec R., Szczerba R., Soszynski I.
<Astron. Astrophys. 682, A70 (2024)>
=2024A&A...682A..70G 2024A&A...682A..70G (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Planetary nebulae ; Stars, variable ;
Photometry ; Optical
Keywords: planetary nebulae: general - binaries: general -
galaxies: individual: Large Magellanic Cloud
Abstract:
Close binary central stars of planetary nebulae (PNe) must have formed
through a common envelope evolution during the giant phase experienced
by one of the stars. Transfer of the angular momentum from the binary
system to the envelope leads to the shortening of the binary
separations from the radius of red giant to the radius of the order of
few tenths of AU. Thus, close binary central stars of planetary
nebulae are laboratories to study the common envelope phase of
evolution. The close binary fraction in the Galaxy has been measured
in various sky surveys, but the close binary fraction is not yet well
constrained for the Magellanic Clouds, and our results may help the
study of common envelope evolution in low-metallicity environments.
This paper presents a continuation of our study of variability in the
Magellanic Cloud planetary nebulae on the basis of data from the OGLE
survey. Previously, we had analysed the OGLE data in the Small
Magellanic Cloud. Here, the study is extended to the Large Magellanic
Cloud (LMC). In this paper we search for close binary central stars
with the aim to constrain the binary fraction and period distribution
in the LMC. We identified 290 counterparts of PNe in the LMC in the
I-band images from the OGLE-III and OGLE-IV surveys. However, the
light curves of ten objects were not accessible in the OGLE database,
and thus we analysed the time series photometry of 280 PNe. In total,
32 variables were found, but 5 of them turned out to be foreground
objects. Another 18 objects show irregular or regular variability that
is not attributable to the binarity of their central stars. Their
status and the nature of their variability will be verified in the
follow-up paper. Nine binary central stars of PNe with periods between
0.24 and 23.6 days were discovered. The obtained fraction for the LMC
PNe is 3.3+2.6-1.6% without correcting for incompleteness. This
number is significantly lower than the 12-21% derived in the analogous
search in the Galactic bulge. We discuss this difference, taking into
account observational biases. The lower binary fraction suggests a
lower efficiency of the common envelope phase in producing close
binaries in the LMC compared to the Galaxy.
Description:
Table A.1 contains the full list of 280 LMC PNe listed in Reid
(2014MNRAS.438.2642R 2014MNRAS.438.2642R) identified in the OGLE-III and OGLE-IV fields
for which the I-band data are available in the OGLE database.
The table lists the names, coordinates (RA and Dec) for J2000.0,
OGLE-III mean V and I magnitudes, number of measurements in the I-band
in the OGLE-III + OGLE-IV surveys (when available), reference for
identification, notes, and other names.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 118 280 List of LMC PNe identified in the OGLE-III
and OGLE-IV fields
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See also:
J/A+A/561/A8 : Binary central stars of SMC PNe (Hajduk+, 2014)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Name of the object (1)
15 I1 h RAh Right ascension (J2000.0)
17- 18 I2 min RAm Right ascension (J2000.0)
20- 24 F5.2 s RAs Right ascension (J2000.0)
26 A1 --- DE- Declination sign (J2000.0)
27- 28 I2 deg DEd Declination (J2000.0)
30- 31 I2 arcmin DEm Declination (J2000.0)
33- 36 F4.1 arcsec DEs Declination (J2000.0)
38- 43 F6.3 mag Vmag ? V-band OGLE-III mean magnitude
45- 50 F6.3 mag Imag I-band OGLE-III mean magnitude
52- 62 A11 --- NI Number of the OGLE-III and OGLE-IV (when
available) I-band observations (2)
64 A1 --- r_Name Reference for identification (3)
66- 72 A7 --- Note Notes (4)
74-118 A45 --- OName Other names
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Note (1): Acronyms used:
[RP2006] = Reid & Parker (2006MNRAS.373..521R 2006MNRAS.373..521R)
[M94b] = Morgan (1994A&AS..103..235M 1994A&AS..103..235M)
[BE74] = Bohannan (1974A&AS...18...47B 1974A&AS...18...47B)
2MASS = Cutri et al. (2003yCat.2246....0C 2003yCat.2246....0C)
WSPN = Westerlund & Smith (1964MNRAS.127..449W 1964MNRAS.127..449W)
Jacoby LMC = Jacoby (1980ApJS...42....1J 1980ApJS...42....1J)
MGPN LMC = Morgan & Good (1992A&AS...92..571M 1992A&AS...92..571M)
SMP LMC = Sanduleak et al. (1978PASP...90..621S 1978PASP...90..621S),
Sanduleak et al. 1984IAUS..108..231S 1984IAUS..108..231S)
LHA = Henize (1956ApJS....2..315H 1956ApJS....2..315H)
LM = Lindsay & Mullan (1963IrAJ....6...51L 1963IrAJ....6...51L)
Note (2): Ten objects in the sample were observed in two OGLE-IV fields. In such
the cases the numbers of I-band observations are as follows:
(OGLE-III) + (OGLE-IV 1-st field) + (OGLE-IV 2-nd field)
Note (3): Reference as follows:
1 = Jacoby (1980ApJS...42....1J 1980ApJS...42....1J)
2 = Morgan & Good (1992A&AS...92..571M 1992A&AS...92..571M)
3 = Morgan (1994A&AS..103..235M 1994A&AS..103..235M)
4 = Leisy et al. (1997A&AS..121..407L 1997A&AS..121..407L, Cat. J/A+AS/121/407)
5 = Reid & Parker (2006MNRAS.373..521R 2006MNRAS.373..521R, Cat. J/MNRAS/373/521)
6 = Miszalski et al. (2011A&A...531A.157M 2011A&A...531A.157M, Cat. J/A+A/531/A157)
7 = Reid & Parker (2013MNRAS.436..604R 2013MNRAS.436..604R)
* = Based on the Aladin Sky Atlas
Note (4): The following remarks have been used:
bin = binary CSPNe
var = variable object, but no binary CSPNe
fo = foreground object (belonging to the Milky Way not the LMC)
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Acknowledgements:
Marcin Gladkowski, seyfert(at)ncac.torun.pl
(End) Patricia Vannier [CDS] 22-Nov-2023