The offset dependent behavior of narrow optical emission features in the Red Rectangle proto-planetary nebula

Wehres, Nadine; Linnartz, H.; Winckel, H. Van; Tielens, A. G. G. M.

doi:10.1051/0004-6361/201116587

Cited by 9 publications

(11 citation statements)

References 34 publications

(97 reference statements)

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“…Sarre et al 1995, Glinsky et al 2002, Wehres et al 2011. These spatially resolved spectra show that most, but not all, narrow features show typical molecular rotational contours and a decrease of rotationally excited states at larger distances from the central engine (Figure 3).…”

Section: The Red Rectanglementioning

confidence: 85%

Why is the Red Rectangle Unique?

Winckel¹

2013

Proc. IAU

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Abstract. The Red Rectangle is a spectacular bipolar nebula centred around the eccentric evolved binary HD 44179. The nebula is rich in spectral signatures: it is the brightest source of the Extended Red Emission (ERE), of the Blue Luminescence (BL) as well as one of the brightest sources of mid-IR PAH bands. Moreover, and unique to this source, a plethora of narrow emission lines is detected on top of the diffuse ERE. Some of these molecular features show rotational contours which become narrower at larger angular separation from the central engine. Some converge to wavelengths and profiles of narrow DIBs. All these observations show that the Red Rectangle is a very rich laboratory to study active astrochemical processes within the nebula. We also address, but fail to answer, the question why this source is so unique among the many observed post-AGB binary analogues.

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Section: The Red Rectanglementioning

confidence: 85%

Why is the Red Rectangle Unique?

Winckel¹

2013

Proc. IAU

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“…Some of these emission bands were also compared to the diffuse interstellar bands (DIBs), molecular features which are usually seen in absorption in diffuse interstellar clouds. The Red Rectangle seems unique in this respect as it shows the same molecular features (DIBs) seen in emission (Sarre 1991;Scarrott et al 1992;Sarre et al 1995;Van Winckel et al 2002;Wehres et al 2011 of the Red Square, although one particular IR DIB has been argued to arise from circumstellar material in the nebula itself (Zasowski et al 2015). An overview of the X-shooter spectrum is given in Fig.…”

Section: The Optical Spectrum: Molecules and Atomic Ionsmentioning

confidence: 97%

Medium-resolution échelle spectroscopy of the Red Square Nebula, MWC 922

Wehres

Ochsendorf

Tielens

et al. 2017

A&A

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Context. Medium-resolution échelle spectra of the Red Square Nebula surrounding the star MWC 922 are presented. The spectra have been obtained in 2010 and 2012 using the X-shooter spectrograph mounted on the Very Large Telescope (VLT) in Paranal, Chile. The spectrum covers a wavelength range between 300 nm−2.5 µm and shows that the nebula is rich in emission lines. Aims. We aim to identify the emission lines and use them as a tool to determine the physical and chemical characteristics of the nebula. The emission lines are also used to put constraints on the structure of the nebula and on the nature of the central stars. Results. These findings put constraints on the evolution of the central objects in MWC 922. The Red Square shows strong similarities to the Red Rectangle Nebula, both in morphology and in its mid-IR spectroscopic characteristics. As for the Red Rectangle, the observed morphology of the nebula reflects mass-loss in a binary system. Specifically, we attribute the biconical morphology and the associated rung-like structure to the action of intermittent jets blown by the accreting companion in a dense shell, which has been created by the primary. We stress, though, that despite the morphological similarities, these two objects represent very different classes of stellar objects.

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“…W. W. Duley drew our attention to Wehres et al [57], in which they assumed a carbon chain and estimated the number of carbon atom to be 7 to 8. This is for an emission band at 6615 Å from the Red Rectangle whose carrier is perhaps the same as that for λ6613.6 DIB.…”

Section: N = 7 − 8 By Wehres Et Almentioning

confidence: 99%

Constraining the size of the carrier of the λ5797.1 diffuse interstellar band

Huang

Oka

2015

Molecular Physics

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The diffuse interstellar band (DIB) at 5797.1Å is simulated based on three premises: (1) The carrier of the DIB is polar as concluded by T. Oka et al. from the anomalous spectrum toward Herschel 36. (2) The sharp central feature observed by P. J. Sarre's group is the Qbranch of a parallel band of a prolate top. (3) The radiative temperature of the environment is Tr = 2.73 K.A 2 Π ← 2 Π transition of a linear radical is simulated. Results depend on 10 parameters, with the rotational constant B being the most critical. Comparisons of calculated spectra with observed data constrain B, which in turn constrains the number of heavy atoms to 5 ≤ n ≤ 7. Upper limits based on the Her 36 spectrum and lower limits based on stability against photodissociation are also discussed. The latter is based on the assumption that the DIB molecules are produced top-down from the breakdown of dust rather than bottom-up by chemical reactions.A difficulty with this limit is that J. P. Maier's laboratory has observed many molecules within this size range, some of which have been tested astronomically. Candidates are discussed in light of many prolate tops observed by the P. Thaddeus and M. C. McCarthy microwave group.

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The offset dependent behavior of narrow optical emission features in the Red Rectangle proto-planetary nebula

Cited by 9 publications

References 34 publications

Why is the Red Rectangle Unique?

Why is the Red Rectangle Unique?

Medium-resolution échelle spectroscopy of the Red Square Nebula, MWC 922

Constraining the size of the carrier of the λ5797.1 diffuse interstellar band

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