New young planetary nebulae in IPHAS

Viironen, K.; Mampaso, A.; Corradi, R. L. M.; Rodríguez, Mónica; Greimel, R.; Sabin, L.; Unruh, Y. C.; Delgado-Inglada, G.; Drew, J. E.; Giammanco, C.; Groot, P.; Parker, Quentin A.; Sokoloski, J. L.; Zijlstra, A. A.

doi:10.1051/0004-6361/200811575

Cited by 34 publications

(36 citation statements)

References 46 publications

(76 reference statements)

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“…The object has a high excitation class (Parker et al 2006). However, in agreement with Viironen et al (2009b, Fig. 1) this could be a D-type symbiotic star.…”

Section: Notes On Individual Objectssupporting

confidence: 82%

Near-infrared photometry of Galactic planetary nebulae with the VVV Survey

Weidmann

Gamen

Hoof

et al. 2013

A&A

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Context. Planetary nebulae (PNe) are powerful tracers of evolved stellar populations. Among the 3000 known PNe in the Galaxy, about 600 are located within the 520 square-degree area covered by the VVV survey. The VVV photometric catalogue provides an important new dataset for the study of PNe, with high-resolution imaging in five near-infrared bands. Aims. There are various colour-colour diagrams that can be obtained from the VVV filters. We investigate the location of PNe in these diagrams and the separation from other types of objects. This includes the new Y−J vs. Z−Y diagram. Methods. Aperture photometry of known PNe in the VVV area was retrieved from source catalogues. Care was taken to minimise any confusion with field stars. The colours of the PNe we are determined for (H−K s ), (J−H), (Z−Y), and (Y−J), and compared to stars and to other types of emission line objects. Cloudy photo-ionisation models were used to predict colours for typical PNe.Results. We present near-infrared photometry for 353 known PNe. The best separation from other objects is obtained in the (H−K s ) vs. (J−H) diagram. We calculated the emission-line contribution to the in-band flux based on a model for NGC 6720: we find that this is highest in the Z and Y bands at over 50%, lower in the J band at 40%, and lowest in the H and K s bands at 20%. A new view of PNe in the wavelength domain of the Z and Y bands is shown. Photo-ionisation models are used to explore the observed colours in these bands. The Y band is shown to be dominated by He i 1.083 μm and He ii 1.012 μm, and colours involving this band are very sensitive to the temperature of the ionizing star. Conclusions. The VVV survey represents a unique dataset for studying crowded and obscured regions in the Galactic plane. The diagnostic diagrams presented here allow one to study the properties of known PNe and to uncover objects not previously classified.

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“…The object has a high excitation class (Parker et al 2006). However, in agreement with Viironen et al (2009b, Fig. 1) this could be a D-type symbiotic star.…”

Section: Notes On Individual Objectssupporting

confidence: 82%

Near-infrared photometry of Galactic planetary nebulae with the VVV Survey

Weidmann

Gamen

Hoof

et al. 2013

A&A

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“…However, the absence of both the red giant bands and the Raman scattered emission features in their optical spectra does not allow, at present, a classification as genuine symbiotic stars. In fact, they are discussed in detail by Viironen et al (2009a) and classified as young planetary nebulae. They form part of a larger sample of objects, including very well studied nebulae like M 2-9 or Mz 3, whose nature as young planetary nebulae or symbiotic stars is controversial.…”

Section: Objects Borderline Between Symbiotic Stars and Planetary Nebmentioning

confidence: 99%

IPHAS and the symbiotic stars

Corradi

Valentini

Munari

et al. 2009

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Context. Knowledge of the total population of symbiotic stars in the Galaxy is important for understanding basic aspects of stellar evolution in interacting binaries and the relevance of this class of objects in the formation of supernovae of type Ia. Aims. In a previous paper, we presented the selection criteria needed to search for symbiotic stars in IPHAS, the INT Hα survey of the Northern Galactic plane. IPHAS gives us the opportunity to make a systematic, complete search for symbiotic stars in a magnitude-limited volume. Methods. Follow-up spectroscopy at different telescopes worldwide of a sample of sixty two symbiotic star candidates is presented. Results. Seven out of nineteen S-type candidates observed spectroscopically are confirmed to be genuine symbiotic stars. The spectral type of their red giant components, as well as reddening and distance, were computed by modelling the spectra. Only one new D-type symbiotic system, out of forty-three candidates observed, was found. This was as expected (see discussion in our paper on the selection criteria). The object shows evidence for a high density outflow expanding at a speed ≥65 km s −1 . Most of the other candidates are lightly reddened classical T Tauri stars and more highly reddened young stellar objects that may be either more massive young stars of HAeBe type or classical Be stars. In addition, a few notable objects have been found, such as three new Wolf-Rayet stars and two relatively high-luminosity evolved massive stars. We also found a helium-rich source, possibly a dense ejecta hiding a WR star, which is surrounded by a large ionized nebula. Conclusions. These spectroscopic data allow us to refine the selection criteria for symbiotic stars in the IPHAS survey and, more generally, to better understand the behaviour of different Hα emitters in the IPHAS and 2MASS colour-colour diagrams.

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“…Viironen et al (2009a) published a list of 781 new IPHAS PN candidates, whereas the discovery and detailed study of five new IPHAS PNe were presented by Viironen et al (2009b).…”

Section: Introductionmentioning

confidence: 99%

A new planetary nebula in the outer reaches of the Galaxy

Viironen¹,

Mampaso²,

Corradi³

et al. 2011

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Aims. A proper determination of the abundance gradient in the Milky Way requires the observation of objects at large galactiocentric distances. With this aim, we are exploring the planetary nebula population towards the Galactic anticentre. In this article, the discovery and physico-chemical study of a new planetary nebula towards the anticentre direction, IPHASX J052531.19+281945.1 (PNG 178.1-04.0), is presented. Methods. The planetary nebula was discovered from the IPHAS survey. Long-slit follow-up spectroscopy was carried out to confirm its planetary nebula nature and to calculate its physical and chemical characteristics.Results. The newly discovered planetary nebula turned out to be located at a very large galactocentric distance (D GC = 20.8±3.8 kpc), larger than any previously known planetary nebula with measured abundances. Its relatively high oxygen abundance (12+log(O/H) = 8.36 ± 0.03) supports a flattening of the Galactic abundance gradient at large galactocentric distances rather than a linearly decreasing gradient.

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New young planetary nebulae in IPHAS

Cited by 34 publications

References 46 publications

Near-infrared photometry of Galactic planetary nebulae with the VVV Survey

Near-infrared photometry of Galactic planetary nebulae with the VVV Survey

IPHAS and the symbiotic stars

A new planetary nebula in the outer reaches of the Galaxy

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