An Optical-Infrared Study of the Young Multipolar Planetary Nebula NGC 6644

Hsia, Chin; Kwok, Sun; Zhang, Yong; Koning, Nico; Volk, Kevin

doi:10.1088/0004-637x/725/1/173

Cited by 14 publications

(21 citation statements)

References 22 publications

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“…For the objects chosen, at least three pairs are obviously seen, and the number 3 is also commonly found in literatures (NGC 7027 by Nakashima et al 2010; NGC 6644 by Hsia et al 2010;and NGC 7026 by Clark et al, this volume). It is possible that there are more than three pairs (for example, IRAS 19024+0044 by Sahai et al 2005;and NGC 5189 by Sabin et al, this volume), but adding more pairs means adding more parameters; at this stage we hope to keep the number of parameters down.…”

Section: Why We Choose the Numbersupporting

confidence: 68%

Multipolar planetary nebulae: Not as geometrically diversified as thought

Chong¹,

Kwok²,

Imai³

et al. 2011

Proc. IAU

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Abstract. We present a general three-dimensional model of multipolar planetary nebulae (PNe). By rotating to different viewing angles and adjusting the angles between the multiple lobes, we demonstrate that the model is able to reproduce HST Hα images of 20 multipolar young PNe. Though this model only considers the geometrical projection effects, it significantly unifies the selected PNe and can be considered as a first-order fundamental model of the "multipolar" morphological class. This kind of model reduces complexity and is essential to pursuing of the shaping mechanism. In addition, we illustrate that under some special conditions, i.e. in certain viewing angles, or with low sensitivity, it will be hard to imagine that the projected image originates from a multipolar-lobed model.

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Section: Why We Choose the Numbersupporting

confidence: 68%

Multipolar planetary nebulae: Not as geometrically diversified as thought

Chong¹,

Kwok²,

Imai³

et al. 2011

Proc. IAU

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“…Originally this subclass included K 3-24, M 1-75, and M 2-46, and very likely M 3-28 and M 4-14. Since then, the sample of quadrupolar PNe has increased with time up to a number of ten (Manchado et al, 1996;Guerrero & Manchado, 1998;Cuesta & Phillips, 2000;Mampaso et al, 2006;Vázquez et al, 2008;Hsia et al, 2010, this paper), but they are certainly more because some PNe are prone to be classified as quadrupolar (e.g., NGC 4361 and NGC 6072, Muthu & Anandarao, 2001;Kwok et al, 2010), whereas other morphological subclasses are closely related (e.g., the Starfish Nebulae, Sahai, 2000). To date, only one proto-PN, IRAS 19475+3119, has been reported to have a quadrupolar morphology (Sahai et al, 2007).…”

Section: Discussionmentioning

confidence: 99%

Kn 26, a new quadrupolar planetary nebula

Guerrero¹,

Miranda²,

Ramos-Larios³

et al. 2013

A&A

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Once classified as an emission line source, the planetary nebula (PN) nature of the source Kn 26 has been only recently recognized in digital sky surveys. To investigate the spectral properties and spatio-kinematical structure of Kn 26, we have obtained high spatial-resolution optical and near-IR narrow-band images, high-dispersion long-slit echelle spectra, and intermediate-resolution spectroscopic observations. The new data reveal an hourglass morphology typical of bipolar PNe. A detailed analysis of its morphology and kinematics discloses the presence of a second pair of bipolar lobes, making Kn 26 a new member of the subclass of quadrupolar PNe. The time-lap between the ejection of the two pairs of bipolar lobes is much smaller than their dynamical ages, implying a rapid change of the preferential direction of the central engine. The chemical composition of Kn 26 is particularly unusual among PNe, with a low N/O ratio (as of type II PNe) and a high helium abundance (as of type I PNe), although not atypical among symbiotic stars. Such an anomalous chemical composition may have resulted from the curtail of the time in the Asymptotic Giant Branch by the evolution of the progenitor star through a common envelope phase.

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“…The emerging flux of I19312 with extinction corrections are fitted by a three-component model using the same expression described in Hsia et al (2010). As seen in Figure 6, only the shortest wavelength component (less than roughly λ =5 µm) is affected by the interstellar extinction correction.…”

Section: Absolute Luminositymentioning

confidence: 99%

Wide Field Co Mapping in the Region of Iras 19312+1950

Nakashima

Ladeyschikov

Соболев

et al. 2016

ApJ

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We report the results of a wide field CO mapping in the region of IRAS 19312+1950. This IRAS object exhibits SiO/H 2 O/OH maser emission, and is embedded in a chemically-rich molecular component, of which the origin is still unknown. In order to reveal the entire structure and gas mass of the surrounding molecular component for the first time, we have mapped a wide region around IRAS 19312+1950 in the 12 CO J = 1-0, 13 CO J = 1-0 and C 18 O J = 1-0 lines using the Nobeyama 45m telescope. In conjunction with the archival CO maps, we investigated a region with a size up to 20 ′ × 20 ′ around this IRAS object. We calculated CO gas mass assuming the LTE condition, a stellar velocity against to the interstellar medium assuming an analytic model of a bow shock, and absolute luminosity using the latest archival data and trigonometric parallax distance. The derived gas-mass (225 M ⊙ -478 M ⊙ ) of the molecular component and the relatively large luminosity (2.63 × 10 4 L ⊙ ) suggest that the central SiO/H 2 O/OH maser source seems to be a red supergiant (RSG) rather than an asymptotic giant branch (AGB) star or post-AGB star.

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An Optical-Infrared Study of the Young Multipolar Planetary Nebula NGC 6644

Cited by 14 publications

References 22 publications

Multipolar planetary nebulae: Not as geometrically diversified as thought

Multipolar planetary nebulae: Not as geometrically diversified as thought

Kn 26, a new quadrupolar planetary nebula

Wide Field Co Mapping in the Region of Iras 19312+1950

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