Unravelling the chemical inhomogeneity of PNe with VLT FLAMES integral-field unit spectroscopy

Tsamis, Y. G.; Walsh, J. R.; Pequignot, D.; Barlow, M. J.; Liu, Xw-W.; Danziger, I.J.

doi:10.1017/s1743921306003036

Cited by 22 publications

(34 citation statements)

References 7 publications

(9 reference statements)

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“…In particular, the O ii flux map seems to peak at the position of the apex of HH 202, the zone also known as HH 202‐S – spaxels (−5.5, −6.5) and (−6.5, −4.5). A similar spatial distribution of both kinds of lines was already observed using long‐slit spectra in the Orion Nebula by Mesa‐Delgado et al (2008), as well as in the three PNe observed by Tsamis et al (2008). Fig.…”

Section: Line Measurements and Reddening Correctionsupporting

confidence: 83%

“…This apparent trend is mainly produced by the behaviour observed at HH 202‐S and HH 202‐N, which are precisely the zones where the O 2+ and C 2+ abundances obtained from RLs are lower and T e ([O iii ]) is higher. From integral field spectroscopy, Tsamis et al (2008) have found rather clear positive correlations between ionic abundances obtained from RLs and T e in three PNe, exactly the opposite trend we observe in this FOV of the Orion Nebula. These authors argue that their results provide evidence for the existence of two distinct components of highly ionized gas at very different temperatures.…”

Section: Discussionsupporting

confidence: 61%

“…The use of the integral field spectroscopy is still in its infancy in the study of ionized nebulae and the number of works available is still rather small. In the case of PNe, Tsamis et al (2008) have carried out the first deep study using this technique with Fibre Large Array Multi Element Spectrograph (FLAMES) at the Very Large Telescope (VLT) taking spectra of three PNe of the Galactic disc and covering the spectral range from 3964 to 5078 Å. For the Orion Nebula, Tsamis, Walsh & Péquignot (2009) have presented preliminary results of integral field spectroscopy with FLAMES for several proplyds with the aim of studying the behaviour of the physical conditions, chemical abundances and the ADF in and outside these kinds of objects.…”

Section: Introductionmentioning

confidence: 99%

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Properties of the ionized gas in HH 202 - I. Results from integral field spectroscopy with PMAS

Mesa‐Delgado¹,

López‐Martín²,

Esteban³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We present results from integral field spectroscopy with the Potsdam Multi‐Aperture Spectrograph of the head of the Herbig–Haro (HH) object HH 202 with a spatial sampling of 1 × 1 arcsec2. We have obtained maps of different emission lines, physical conditions – such as electron temperature and density – and ionic abundances from recombination and collisionally excited lines. We present the first map of the Balmer temperature and of the temperature fluctuation parameter, t2. We have calculated the t2 in the plane of the sky, which is substantially smaller than that determined along the line of sight. We have mapped the abundance discrepancy factor (ADF) of O2+, ADF(O2+), finding its maximum value at the HH 202‐S position. We have explored the relations between the ADF(O2+) and the electron density, the Balmer and [O iii] temperatures, the ionization degree as well as the t2 parameter. We do not find clear correlations between these properties and the results seem to support that the ADF and t2 are independent phenomena. We have found a weak negative correlation between the O2+ abundance determined from recombination lines and the temperature, which is the expected behaviour in an ionized nebula, hence it seems that there is no evidence for the presence of supermetal‐rich droplets in H ii regions.

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Section: Line Measurements and Reddening Correctionsupporting

confidence: 83%

Section: Discussionsupporting

confidence: 61%

Section: Introductionmentioning

confidence: 99%

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Properties of the ionized gas in HH 202 - I. Results from integral field spectroscopy with PMAS

Mesa‐Delgado¹,

López‐Martín²,

Esteban³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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“…However, only a small number of PNe have been studied using a spectroscopic mapping technique. Some examples are NGC 6369 (Monteiro et al 2004), NGC 40 (Leal-Ferreira et al 2011, NGC 5882 (Tsamis et al 2008), NGC 6153 (Tsamis et al 2008), and NGC 7009 (Tsamis et al 2008;Phillips et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic mapping of the planetary nebula NGC 6302

Rauber

Copetti

Krabbe

2014

A&A

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Context. Most spectroscopic studies of planetary nebulae (PNe) are based on data from specific parts of the objects. Considering the high complexity of their morphological structures, integrated or average values across an observed region can only provide limited information of their ionic, density, and temperature structures. Aims. We investigate the spatial variation of the physical and chemical properties of NGC 6302, a high-ionization PNe, with a complex bipolar structure. Methods. Spatially resolved long-slit spectroscopic data were obtained from 11 parallel and equally spaced directions over the nebula. Integrated spectra were also obtained and 142 lines were identified. Results. The electron density maps show a peaked distribution, with the densest area at the circumstellar region, reaching N e ≈ 40 000 cm −3 , and decreasing to N e ≤ 1000 cm −3 at the lobes. Knots were observed in the N e (S ii) map, with 2000 cm −3 < N e < 3000 cm −3 . The N e (Ar iv) map suggests the presence of an inner region with N e ≈ 20 000 cm −3 that extends from the center through the east lobe. A homogeneous temperature distribution was found for both T e (O iii) and T e (N ii). Small temperature fluctuations on the plane of the sky of t 2 s (N ii) = 0.0071 and t 2 s (O iii) = 0.0043 were estimated.Conclusions. In general, the total abundances obtained are similar to the maximum found in the ionic abundance maps of the dominant ionic species. This demonstrates the potential of spatially resolved abundance studies for establishing lower limits of the total abundances based on ionic abundances, for checking the ionization correlation factors, and in some cases, for determining the total abundances directly from maps of ionic abundances.

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“…Spectral H 2 imaging in the infrared has been applied mostly to map the morphology of post-AGB stars and the AGB remnant halo of Planetary Nebulae (Hrivnak et al 2008(Hrivnak et al , 2006Sahai & Trauger 1998;Kastner et al 2001;Cox et al 2003;Davis et al 2005; Van de Steene et al 2008). The novel technique of Integral Field Spectroscopy has been applied for these evolved objects to obtain higher spatial and spectral resolution in molecular hydrogen and other lines (Tsamis et al 2008;Sandin et al 2008;Santander-García et al 2007Sharp et al 2006;Lowe & Gledhill 2006;Monreal-Ibero et al 2005).…”

Section: The Molecular Envelopesmentioning

confidence: 99%