The planetary nebula systems of the Magellanic Clouds

Sanduleak, N.; MacConnell, D. J.; Philip, A. G. D.

doi:10.1086/130397

Cited by 103 publications

(77 citation statements)

References 5 publications

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“…In order to make the base list for this study we used the PN catalogue from Reid & Parker (2006a,b, 2010, collectively Sanduleak et al (1978), which have the form 'SMP LMC xx', are referred to as 'SMP Lxx'. For references to SMC PNe catalogued as 'SMP SMC xx', we use 'SMP Sxx' as a shorthand.…”

Section: Base Catalogue and Detection Methodsmentioning

confidence: 99%

Radio Planetary Nebulae in the Large Magellanic Cloud

Leverenz

Filipović

Vukotić

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present 21 new radio-continuum detections at catalogued planetary nebula (PN) positions in the Large Magellanic Cloud (LMC) using all presently available data from the Australia Telescope Online Archive at 3, 6, 13 and 20 cm. Additionally, 11 previously detected LMC radio PNe are re-examined with 7 detections confirmed and reported here. An additional three PNe from our previous surveys are also studied. The last of the 11 previous detections is now classified as a compact H ii region which makes for a total sample of 31 radio PNe in the LMC. The radio-surface brightness to diameter (Σ-D) relation is parametrised as Σ ∝ D −β . With the available 6 cm Σ-D data we construct Σ-D samples from 28 LMC PNe and 9 Small Magellanic Cloud (SMC) radio detected PNe. The results of our sampled PNe in the Magellanic Clouds (MCs) are comparable to previous measurements of the Galactic PNe. We obtain β = 2.9 ± 0.4 for the MC PNe compared to β = 3.1 ± 0.4 for the Galaxy. For a better insight into sample completeness and evolutionary features we reconstruct the Σ-D data probability density function (PDF). The PDF analysis implies that PNe are not likely to follow linear evolutionary paths. To estimate the significance of sensitivity selection effects we perform a Monte Carlo sensitivity simulation on the Σ-D data. The results suggest that selection effects are significant for values larger than β ∼ 2.6 and that a measured slope of β = 2.9 should correspond to a sensitivity-free value of ∼ 3.4.

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Section: Base Catalogue and Detection Methodsmentioning

confidence: 99%

Radio Planetary Nebulae in the Large Magellanic Cloud

Leverenz

Filipović

Vukotić

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…There are approximately 700 objects catalogued as PNe in the LMC (Leisy et al 1997;Reid & Parker 2006a,b) and 140 in the SMC (Jacoby, private communication;Sanduleak & MacConnell & Philip 1978;Jacoby 1980;Jacoby & De Marco 2002). Magellanic PNe are best known for their fundamental role in the development of the extragalactic standard candle [O III] λ5007 Planetary Nebula Luminosity Function (PNLF; Henize & Westerlund 1963;Jacoby 1980Jacoby , 1989.…”

Section: Planetary Nebulaementioning

confidence: 99%

The VMC survey

Cioni

Clementini

Girardi

et al. 2011

A&A

310

304

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Context. The new VISual and Infrared Telescope for Astronomy (VISTA) has started operations. Over its first five years it will be collecting data for six public surveys, one of which is the near-infrared Y JK s VISTA survey of the Magellanic Clouds system (VMC). This survey comprises the Large Magellanic Cloud (LMC), the Small Magellanic Cloud, the Magellanic Bridge connecting the two galaxies and two fields in the Magellanic Stream. Aims. This paper provides an overview of the VMC survey strategy and presents first science results. The main goals of the VMC survey are the determination of the spatially-resolved star-formation history and the three-dimensional structure of the Magellanic system. The VMC survey is therefore designed to reach stars as faint as the oldest main sequence turn-off point and to constrain the mean magnitude of pulsating variables such as RR Lyrae stars and Cepheids. This paper focuses on observations of VMC fields in the LMC obtained between November 2009 and March 2010. These observations correspond to a completeness of 7% of the planned LMC fields. Methods. The VMC data are comprised of multi-epoch observations which are executed following specific time constraints. The data were reduced using the VISTA Data Flow System pipeline with source catalogues, including astrometric and photometric corrections, produced and made available via the VISTA Science Archive. The VMC data will be released to the astronomical community following the European Southern Observatory's Public Survey policy. The analysis of the data shows that the sensitivity in each wave band agrees with expectations. Uncertainties and completeness of the data are also derived. Results. The first science results, aimed at assessing the scientific quality of the VMC data, include an overview of the distribution of stars in colour-magnitude and colour-colour diagrams, the detection of planetary nebulae and stellar clusters, and the K s band light-curves of variable stars. Conclusions. The VMC survey represents a tremendous improvement, in spatial resolution and sensitivity, on previous panoramic observations of the Magellanic system in the near-infrared, providing a powerful complement to deep observations at other wavelengths.

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“…In column (1) of Table 1 we list the usual name of the PN, where J, MA, MG, SMP, and SP indicate the original discovery or listing catalogs, with J referring to Jacoby (1980), MA to Meyssonnier & Azzopardi (1993), MG to Morgan & Good (1985), SMP to Sanduleak et al (1978), and SP to Sanduleak & Pesch (1981). Note that in some cases they may be listed in two or more catalogs, and we use the most commonly used names.…”

Section: Data Selection Of Smc Pnementioning

confidence: 99%

Planetary nebulae in the Small Magellanic Cloud

Ventura

Stanghellini

Criscienzo

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyse the planetary nebulae (PNe) population of the Small Magellanic Cloud (SMC), based on evolutionary models of stars with metallicities in the range 10 −3 ≤ Z ≤ 4 × 10 −3 and mass 0.9 M < M < 8 M , evolved through the asymptotic giant branch (AGB) phase. The models used account for dust formation in the circumstellar envelope. To characterise the PNe sample of the SMC, we compare the observed abundances of the various species with the final chemical composition of the AGB models: this study allows us to identify the progenitors of the PNe observed, in terms of mass and chemical composition. According to our interpretation, most of the PNe descend from low-mass (M < 2M ) stars, which become carbon rich, after experiencing repeated third dredge-up episodes, during the AGB phase. A fraction of the PNe showing the signature of advanced CNO processing are interpreted as the progeny of massive AGB stars, with mass above ∼ 6M , undergoing strong hot bottom burning. The differences with the chemical composition of the PNe population of the Large Magellanic Cloud (LMC) is explained on the basis of the diverse star formation history and age-metallicity relation of the two galaxies. The implications of the present study for some still highly debated points regarding the AGB evolution are also commented.

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The planetary nebula systems of the Magellanic Clouds

Cited by 103 publications

References 5 publications

Radio Planetary Nebulae in the Large Magellanic Cloud

Radio Planetary Nebulae in the Large Magellanic Cloud

The VMC survey

Planetary nebulae in the Small Magellanic Cloud

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