Wide binaries in planetary nebulae with<i>Gaia</i>DR2

González-Santamaría, I.; Manteiga, M.; Manchado, A.; Gómez-Muñoz, M. A.; Dafonte, Carlos

doi:10.1051/0004-6361/202039422

Cited by 8 publications

(5 citation statements)

References 29 publications

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“…A small number of PNe have eclipsing binary nuclei (see Section 6); astrophysical analyses of these systems provide additional distance estimates (F16, Table 3). González-Santamaría et al (2020) found eight wide binaries (including one triple system) among their good-quality Gaia DR2 distance sample described in GS19. Most recently, GS21 detected three further possible wide binary systems in their EDR3 sample, including the Ring Nebula (NGC 6720).…”

Section: Primary Methodsmentioning

confidence: 96%

Planetary Nebulae: Sources of Enlightenment

Kwitter

Henry

2022

PASP

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In this review/tutorial we explore planetary nebulae as a stage in the evolution of low-to-intermediate-mass stars, as major contributors to the mass and chemical enrichment of the interstellar medium, and as astrophysical laboratories. We discuss many observed properties of planetary nebulae, placing particular emphasis on element abundance determinations and comparisons with theoretical predictions. Dust and molecules associated with planetary nebulae are considered as well. We then examine distances, binarity, and planetary nebula morphology and evolution. We end with mention of some of the advances that will be enabled by future observing capabilities.

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Section: Primary Methodsmentioning

confidence: 96%

Planetary Nebulae: Sources of Enlightenment

Kwitter

Henry

2022

PASP

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“…We find that only with a careful examination of every PN and CSPN candidate on an individual basis and by using all the power of multi-wavelength imagery and other pertinent data in HASH can proper evaluations be made and more reliable CSPN be identified. This appears to be true for both [2] and Gaia [10][11][12][13], where our results show some potential issues with correct CSPN identification. Fuller details and work on this topic will be the subject of a paper by Parker et al, which is in preparation.…”

Section: Discussionmentioning

confidence: 56%

“…Nevertheless, unlike for [2], no astrometric problems were found. Others [10][11][12][13] have been using Gaia Early Release data to identify CSPN, with [12] reporting results for 1725 Galactic CSPN based on Gaia EDR3 data. However, from our HASH study it is clear that there may be problems with these Gaia CSPN compilations, as Figure 3 clearly shows for PN 'Outers 2 (HASH ID #10957), where the available PanSTARRs and SDSS irg imagery reveals the true blue CSPN that is also right at the geometric center of the PN.…”

Section: Comparisons With the Gaia Astrometric Surveymentioning

confidence: 99%

A Preliminary Investigation of CSPN in the HASH Database

2022

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We present some preliminary findings on the population of planetary nebula where central stars (CSPN) have been independently identified in the HASH catalogue. Many new discoveries and candidates have been found (416 at the time of this writing), adding significantly to the previously known sample of about 600. We also present results from a comparison between our own HASH measurements of CSPN and those provided in existing CSPN catalogues and those from Gaia. We show the value of a federated, multi-wavelength database of Galactic PNe like HASH in terms of not only uncovering faint, new CSPN but of assisting in correct identifications, removing PN mimics with apparent CSPN, correcting incorrect assignments and providing improved positions. HASH provides the community with a comprehensive and reliable resource for any study of the CSPN population of Galactic PNe.

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“…This article is an extension of our previous studies on the Galactic planetary nebulae (PNe) population using Gaia Data Release 2 (DR2): González-Santamaría et al (2019) (Paper I) and González-Santamaría et al (2020) (Paper II). Here, we make use of the recently published Gaia Early Data Release 3 (EDR3) archive, which provides a greater quantity of higher quality astrometric and photometric data that allow us to update and Full Tables A.1 and A.2 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http: //cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/656/A51 enlarge our PNe catalogue and analyse its results in greater detail.…”

Section: Introductionmentioning

confidence: 94%

Planetary nebulae in Gaia EDR3: Central star identification, properties, and binarity

González-Santamaría

Manteiga

Manchado

et al. 2021

A&A

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Context. The Gaia Early Data Release 3 (EDR3), published in December 2020, features improved photometry and astrometry compared to that published in the previous DR2 file and includes a substantially larger number of sources, of the order of 2000 million, making it a paradigm of big data astronomy. Many of the central stars of planetary nebulae (CSPNe) are inherently faint and difficult to identify within the field of the nebula itself. Gaia measurements may be relevant not only in identifying the ionising source of each nebula, but also in the study their physical and evolutionary properties. Aims. We demonstrate how Gaia data mining can effectively help to solve the issue of central star misidentification, a problem that has plagued the field since its origin. As we did for DR2, our objective is to present a catalogue of CSPNe with astrometric and photometric information in EDR3. From that catalogue, we selected a sample of stars with high-quality astrometric parameters, on which we carried out a more accurate analysis of CSPNe properties. Methods.GaiaGBP − GRP colours allow us to select the sources with sufficient temperatures to ionise the nebula. In order to estimate the real colour of a source, it is important to take into account interstellar extinction and, in the case of compact nebulae, nebular extinction when available. In addition, distances derived from EDR3 parallaxes (combined with consistent literature values) can be used to obtain nebular intrinsic properties from those observed. With this information, CSPNe can be plotted in an Hertzsprung-Russell diagram. From information on the spectral classification of the CS (from the literature) and evolutionary models for post-AGB stars, their evolutionary state can then be analysed. Furthermore, EDR3 high-quality astrometric data enable us to search for objects comoving with CSs in the field of each nebula by detecting sources with parallaxes and proper motions similar to those of the CS. Results. We present a catalogue of 2035 PNe with their corresponding CS identification from among Gaia EDR3 sources. We obtain the distances for those with known parallaxes in EDR3 (1725 PNe). In addition, for a sub-sample (405 PNe) with the most accurate distances, we obtain different nebular properties such as their Galactic distribution, radius, kinematic age, and morphology. Furthermore, for a set of 74 CSPNe, we present the evolutionary state (mass and age) derived from their luminosities and effective temperatures from evolutionary models. Finally, we highlight the detection of several wide binary CSPNe through an analysis of the EDR3 astrometric parameters, and we contribute to shedding some light on the relevance of close binarity in CSPNe.

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Wide binaries in planetary nebulae withGaiaDR2

Cited by 8 publications

References 29 publications

Planetary Nebulae: Sources of Enlightenment

Planetary Nebulae: Sources of Enlightenment

A Preliminary Investigation of CSPN in the HASH Database

Planetary nebulae in Gaia EDR3: Central star identification, properties, and binarity

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