Spatially resolved kinematic observations of the planetary nebulae Hen 3-1333 and Hen 2-113

We have performed integral field spectroscopy of the planetary nebulae Hen 3-1333 (PNG332.9-09.9) and Hen 2-113 (PNG321.0+03.9), which are unusual in exhibiting dual-dust chemistry and multipolar lobes but also ionized by late-type [WC 10] central stars. The spatially resolved velocity distributions of the H$\alpha$ emission line were used to determine their primary orientations. The integrated H$\alpha$ emission profiles indicate that Hen 3-1333 and Hen 2-113 expand with velocities of ~ 32 and 23 km/s, respectively. The Hubble Space Telescope observations suggest that these planetary nebulae have two pairs of tenuous lobes extending upwardly from their bright compact cores. From three-dimensional geometric models, the primary lobes of Hen 3-1333 and Hen 2-113 were found to have inclination angles of about -30$^{\circ}$ and 40$^{\circ}$ relative to the line of sight, and position angles of -15$^{\circ}$ and 65$^{\circ}$ measured east of north in the equatorial coordinate system, respectively.Comment: 4 pages, 3 figures, accepted for publication in MNRAS Letter

Proposed nomenclature for Extragalactic Planetary Nebulae

The ability to identify and distinguish between the wide variety of celestial objects benefits from application of a systematic and logical nomenclature. This often includes value-added information within the naming convention which can aid in placing the object positionally either via an RA/DEC or l,b concatenation. All new nomenclatures should be created following IAU guidelines. However as the number density of specific object types on the sky increases, as in the case of PN in external galaxies, a useful positional identifier becomes problematic. This brief but timely paper attempts to progress the debate on this vexing issue for the case of extragalactic planetary nebulae (EPN). There is a clear need to rationalise the current ad-hoc system now that many thousands of Extragalactic PN are being discovered.Comment: 3 pages, no figures, LaTeX, to be published in Proceedings of the ESO workshop on Planetary Nebulae beyond the Milky Way held at ESO, Garching, May 19-21, 200

Extragalactic Planetary Nebulae: Observational Challenges & Future Prospects

The study of extragalactic planetary nebulae (EPN) is a rapidly expanding field. The advent of powerful new instrumentation such as the PN spectrograph has led to an avalanche of new EPN discoveries both within and between galaxies. We now have thousands of EPN detections in a heterogeneous selection of nearby galaxies and their local environments, dwarfing the combined galactic detection efforts of the last century. Key scientific motivations driving this rapid growth in EPN research and discovery have been the use of the PNLF as a standard candle, as dynamical tracers of their host galaxies and dark matter and as probes of Galactic evolution. This is coupled with the basic utility of PN as laboratories of nebula physics and the consequent comparison with theory where population differences, abundance variations and star formation history within and between stellar systems informs both stellar and galactic evolution. Here we pose some of the burning questions, discuss some of the observational challenges and outline some of the future prospects of this exciting, relatively new, research area as we strive to go fainter, image finer, see further and survey faster than ever before and over a wider wavelength regimeComment: 4 pages, no figures, LaTeX, to be published in Proceedings of the ESO workshop on Planetary Nebulae beyond the Milky Way held at ESO, Garching, May 19-21, 200

H-alpha Stacked Images Reveal Large Numbers of PNe in the LMC

Our new, deep, high resolution H-alpha and matching R-band UKST multi-exposure stack of the central 25 sq. degrees of the LMC promises to provide an unprecedented homogeneous sample of >1,000 new PNe. Our preliminary 2dF spectroscopy on the AAT has vindicated our selection process and confirmed 136 new PNe and 57 emission-line stars out of a sample of 263 candidate sources within an initial 2.5 sq. deg. area. To date approximately one third of the entire LMC has been scanned for candidates (~7.5 sq.deg.). More than 750 new emission sources have been catalogued so far along with independent re-identification of all known and possible PNe found from other surveys. Once our image analysis is complete, we plan comprehensive spectroscopic follow-up of the whole sample, not only to confirm our PN candidates but also to derive nebula temperatures and densities which, with the aid of photoionization modeling, will yield stellar parameters which are vital for constructing H-R diagrams for these objects. A prime objective of the survey is to produce a Luminosity Function which will be the most accurate and comprehensive ever derived in terms of numbers, magnitude range and evolutionary state; offering significant new insights into the LMC's evolutionary history. The observation and measurement of our newly discovered AGB halos around 60% of these PN will also assist in determining the initial- to final-mass ratios for this phase of stellar evolution.Comment: 6 pages, 3 figures, LaTeX, to be published in Proceedings of the ESO workshop on Planetary Nebulae beyond the Milky Way held at ESO, Garching, May 19-21, 200

Extending the RP survey to the outer LMC

We are extending our search for faint PNe in the LMC to include the outer 56 deg2 area not covered in the original UKST survey of the central 25 deg2 region. Candidate PNe have been selected using the Magellanic Cloud Emission Line Survey (MCELS) and the first round of observations has yielded 93 new LMC PNe while confirming the 102 previously known PNe in the outer LMC. We plan to continue our spectroscopic object identification program until we cover all our remaining candidates in the survey area. These observations, providing medium and high resolution spectra from 3650 Ang to 6900 Ang will additionally be used to measure fluxes for a series of research projects including luminosity functions, abundances and LMC kinematics.Comment: 2 pages, 1 figure, IAU283 poster contributio

A New Population of Planetary Nebulae Discovered in the Large Magellanic Cloud (I): Preliminary Sample

We report our initial discovery of 73 new planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) following confirmatory 2dF spectroscopy on the Anglo-Australian Telescope (AAT). Preliminary candidate sources come from a 10 per cent sub-area of our new deep, high resolution H-alpha map of the central 25 deg. square of the LMC obtained with the UK Schmidt Telescope (UKST). The depth of the high resolution map was extended to Requiv~22 for H-alpha (4.5 x 10-17 ergs cm-2 s-1 Ang-1) by a process of multi-exposure median co-addition of a dozen 2-hour H-alpha exposures. The resulting map is at least 1-magnitude deeper than the best wide-field narrow-band LMC images currently available. This depth, combined with our selection technique, has also led to the discovery of extended AGB halos around many new and previously known LMC PNe for the first time. Once complete, our new survey is expected to triple the LMC PN population and have significant implications for the LMC PN luminosity function, kinematics, abundance gradients chemical evolution and, via study of the AGB halos, the initial to final mass relation for low to intermediate mass stars.Comment: 14 pages, 21 figures (zipped). Accepted for publication in Mmonthly Notices of the Royal Astronomical Societ

Planetary Nebula Surveys: Past, Present and Future

In this review we cover the detection, identification and astrophysical importance of planetary nebulae (PN). The legacy of the historic Perek & Kohoutek and Acker et al. catalogues is briefly covered before highlighting the more recent but significant progress in PN discoveries in our Galaxy and the Magellanic Clouds. We place particular emphasis on the major MASH and the IPHAS catalogues, which, over the last decade alone, have essentially doubled Galactic and LMC PN numbers. We then discuss the increasing role and importance that multi-wavelength data is playing in both the detection of candidate PN and the elimination of PN mimics that have seriously biased previous PN compilations. The prospects for future surveys and current efforts and prospects for PN detections in external galaxies are briefly discussed due to their value both as cosmic distance indicators and as kinematical probes of galaxies and dark matter properties.Comment: 8 pages, 1 figure, Proceedings of the Asymmetric Planetary Nebula V Conference (Invited Review, Lake District, England, June 2010

A New Population of Planetary Nebulae Discovered in the Large Magellanic Cloud (IV): The Outer LMC

We have extended our PNe survey to the outer ~64deg^2 of the LMC using maps from the Magellanic Cloud Emission Line Survey (MCELS) and the UK Schmidt Telescope (UKST) H-alpha survey. Although the MCELS survey has poorer ~5 arcsecond resolution than both the UKST H-alpha survey and the original H-alpha median stacked map in the LMC's central 25deg^2, it has the advantage of additional narrow-band filters at H-alpha, [OIII] and [SII] providing improved diagnostic capabilities. Using these data to uncover new emission line candidates we have so far spectroscopically confirmed an extra 61 LMC PNe which we present here for the first time. We have also independently recovered and spectroscopically confirmed 107 of the 109 (98%) PNe that were previously known to exist in the outer LMC. The majority of our newly discovered and previously known PNe were confirmed using the AAOmega, multi-object fibre spectroscopy system on the 3.9-m Anglo-Australian Telescope (AAT) and the 6dF multi-object spectrograph on the UKST. These newly identified PNe were cross-checked against extant multi-wavelength imaging surveys in the near and mid-infrared in particular and against the latest emission-line ratio diagnostic plots for improved confidence in PNe identification.Comment: 24 pages, 22 figures, accepted MNRAS main journal stt 160

Observations and three-dimensional ionization structure of the planetary nebula SuWt 2

The planetary nebula SuWt 2 (PN G311.0+02.4), is an unusual object with a prominent, inclined central emission ellipse and faint bipolar extensions. It has two A-type stars in a proven binary system at the centre. However, the radiation from these two central stars is too soft to ionize the surrounding material leading to a so far fruitless search for the responsible ionizing source. Such a source is clearly required and has already been inferred to exist via an observed temporal variation of the centre-of-mass velocity of the A-type stars. Moreover, the ejected nebula is nitrogen-rich which raises question about the mass-loss process from a likely intermediate-mass progenitor. We use optical integral-field spectroscopy to study the emission lines of the inner nebula ring. This has enabled us to perform an empirical analysis of the optical collisionally excited lines, together with a fully three-dimensional photoionization modelling. Our empirical results are used to constrain the photoionization models, which determine the evolutionary stage of the responsible ionizing source and its likely progenitor. The time-scale for the evolutionary track of a hydrogen-rich model atmosphere is inconsistent with the dynamical age obtained for the ring. This suggests that the central star has undergone a very late thermal pulse. We conclude that the ionizing star could be hydrogen-deficient and compatible with what is known as a PG 1159-type star. The evolutionary tracks for the very late thermal pulse models imply a central star mass of ~ 0.64M${}_{\odot}$, which originated from a ~ 3M${}_{\odot}$ progenitor. The evolutionary time-scales suggest that the central star left the asymptotic giant branch about 25,000 years ago, which is consistent with the nebula's age.Comment: 18 pages, 11 figures, 10 tables, proof corrections applie