New planetary nebulae in the Galactic bulge region with l &gt; 0  - I. Discovery method and first results

Boumis, P.; Paleologou, E. V.; Mavromatakis, F.; Papamastorakis, I.

doi:10.1046/j.1365-8711.2003.06233.x

Cited by 33 publications

(40 citation statements)

References 44 publications

(65 reference statements)

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“…For PTB 25, the E(B − V) value derived from the u − g colour is smaller than both values from Boumis et al (2003), who calculated E(B − V) from the Balmer decrement, and a second, larger value that accounted for higher extinction in the direction of the Galactic Bulge. The good agreement between the colour E(B − V) value and that from Frew (private communication) increases our confidence in the value.…”

Section: Interstellar Reddeningmentioning

confidence: 57%

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The binary fraction of planetary nebula central stars - III. the promise of VPHAS+

Barker

Zijlstra

Marco

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The majority of planetary nebulae (PNe) are not spherical, and current single-star models cannot adequately explain all the morphologies we observe. This has led to the Binary Hypothesis, which states that PNe are preferentially formed by binary systems. This hypothesis can be corroborated or disproved by comparing the estimated binary fraction of all PNe central stars (CS) to that of the supposed progenitor population. One way to quantify the rate of CS binarity is to detect near infra-red (IR) excess indicative of a low-mass main sequence companion. In this paper, a sample of known PNe within data release 2 of the ongoing VPHAS+ are investigated. We give details of the method used to calibrate VPHAS+ photometry, and present the expected colours of CS and main sequence stars within the survey. Objects were scrutinized to remove PN mimics from our sample and identify true CS. Within our final sample of 7 CS, 6 had previously either not been identified or confirmed. We detected an i band excess indicative of a low-mass companion star in 3 CS, including one known binary, leading us to to conclude that VPHAS+ provides the precise photometry required for the IR excess method presented here, and will likely improve as the survey completes and the calibration process finalised. Given the promising results from this trial sample, the entire VPHAS+ catalogue should be used to study PNe and extend the IR excesstested CS sample.

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Section: Interstellar Reddeningmentioning

confidence: 57%

“…This PN was discovered by Boumis et al (2003) and simultaneously catalogued in the preliminary results of the MASH catalogue (Parker et al 2006). The field of this PN is very crowded, but a particularly blue star in the centre of the PN has been identified in VPHAS+ as the CS candidate.…”

Section: Ptb 25mentioning

confidence: 91%

The binary fraction of planetary nebula central stars - III. the promise of VPHAS+

Barker

Zijlstra

Marco

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…An additional ∼450 PNe were then added from a large number of literature sources (e.g. Acker et al 1992Acker et al , 1996Kohoutek 1994Kohoutek , 2002Zanin et al 1997;Beaulieu et al 1999;Cappellaro et al 2001;Jacoby & Van de Steene 2004;Boumis et al 2003Boumis et al , 2006Górny 2006). As a further check we made use of updated coordinates provided by Kerber et al (2003) and SIMBAD to ensure no objects were missed.…”

Section: Planetary Nebulae Catalogue Constructionmentioning

confidence: 99%

Binary planetary nebulae nuclei towards the Galactic bulge

Miszalski

Acker

Moffat³

et al. 2009

A&A

215

310

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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. A close binary fraction of 12−21% is derived and is the first robust and independent validation of the previous 10−15% estimate. 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.

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“…⋆ e-mail:stavrosakras@on.br 2006; Boumis et al 2003Boumis et al , 2006Sahai et al 2011;Sabin et al 2014). …”

Section: Introductionunclassified

Multi-band polarimetry of post-asymptotic giant branch stars – I. Optical measurements

Akras

Vélez

Nanouris

et al. 2017

Mon. Not. R. Astron. Soc.

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We present new optical broad-band (UBVRI) aperture polarimetric observations of 53 post-asymptotic giant branch (AGB) stars selected to exhibit a large nearinfrared excess. 24 out of the 53 stars (45% of our sample) are presented for the first time. A statistical analysis shows four distinctive groups of polarized post-AGB stars: unpolarized or very lowly polarized (degree of polarization or DoP<1%), lowly polarized (1% < DoP< 4%), moderately polarized (4% < DoP < 8%) and highly polarized (DoP > 8%). 23 out of the 53 (66%) belong to the first group, 10 (19%) to the second, five (9%) to the third and only three (6%) to the last group. Approximately, 34% of our sample was found to be unpolarized objects, which is close to the percentage of round planetary nebulae. On average, the low and moderate groups show a wavelength-dependent polarization that increases towards shorter wavelength, implying an intrinsic origin of the polarization, which signifies a Rayleigh-like scattering spectrum typical for non-symmetrical envelopes composed principally of small dust grains. The moderately polarized stars exhibit higher K-W3 and W1-W3 colour indices compared with the group of lowly polarized stars suggesting a possible relation between DoP and mass-loss rate. Moreover, they are found to be systematically colder (redder in B-V), which may be associated with the condensation process close to these stars that results in higher degree of polarization. We also provide evidence that multiple scattering in optically thin polar outflows is the mechanism that gives high DoP in post-AGB stars with a bipolar or multi-polar envelopes.

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New planetary nebulae in the Galactic bulge region with l > 0 - I. Discovery method and first results

Cited by 33 publications

References 44 publications

The binary fraction of planetary nebula central stars - III. the promise of VPHAS+

The binary fraction of planetary nebula central stars - III. the promise of VPHAS+

Binary planetary nebulae nuclei towards the Galactic bulge

Multi-band polarimetry of post-asymptotic giant branch stars – I. Optical measurements

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