A molecular line survey of a sample of AGB stars and planetary nebulae

Smith, C. L.; Zijlstra, A. A.; Fuller, G. A.

doi:10.1093/mnras/stv1934

Cited by 8 publications

(5 citation statements)

References 39 publications

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“…The twocomponent line profile could be associated with an expanding ring, or a disc in rotation. This object has previously been detected in CO (J = 2 − 1) and CO (J = 1 − 0) (Cox et al 1991;Sahai et al 1991;Cox et al 1992;Smith et al 2015).…”

Section: Ic 4406mentioning

confidence: 55%

Opening PANDORA’s box: APEX observations of CO in PNe

Guzmán-Ramírez

Gómez-Ruiz

Boffin

et al. 2018

A&A

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Context. Observations of molecular gas have played a key role in developing the current understanding of the late stages of stellar evolution. Aims. The survey Planetary nebulae AND their cO Reservoir with APEX (PANDORA) was designed to study the circumstellar shells of evolved stars with the aim to estimate their physical parameters. Methods. Millimetre carbon monoxide (CO) emission is the most useful probe of the warm molecular component ejected by low-to intermediate-mass stars. CO is the second-most abundant molecule in the Universe, and the millimetre transitions are easily excited, thus making it particularly useful to study the mass, structure, and kinematics of the molecular gas. We present a large survey of the CO (J = 3−2) line using the Atacama Pathfinder EXperiment (APEX) telescope in a sample of 93 proto-planetary nebulae and planetary nebulae. Results. CO (J = 3−2) was detected in 21 of the 93 objects. Only two objects (IRC+10216 and PN M2-9) had previous CO (J = 3−2) detections, therefore we present the first detection of CO (J = 3−2) in the following 19 objects: Frosty Conclusions. CO (J = 3−2) was detected in all 4 observed pPNe (100%), 15 of the 75 PNe (20%), one of the 4 wide binaries (25%), and in 1 of the 10 close binaries (10%). Using the CO (J = 3−2) line, we estimated the column density and mass of each source. The H 2 column density ranges from 1.7 × 10 18 to 4.2 × 10 21 cm −2 and the molecular mass ranges from 2.7 × 10 −4 to 1.7 × 10 −1 M .

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Section: Ic 4406mentioning

confidence: 55%

Opening PANDORA’s box: APEX observations of CO in PNe

Guzmán-Ramírez

Gómez-Ruiz

Boffin

et al. 2018

A&A

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“…The abundances of HNC in these objects ranged from (0.2-3.3)×10 −7 . In contrast, Smith et al (2015) found f(HNC/H 2 )(0.5-2.9)×10 −8 for the envelopes of C-stars II Lup, RAFGL 4211, and AI Vol. HNC has also been identified in a number of proto-planetary nebulae (PPNe).…”

Section: Hnc Abundance and Distribution In Planetary Nebulaementioning

confidence: 84%

New Detections of HNC in Planetary Nebulae: Evolution of the [Hcn]/[Hnc] Ratio

Schmidt

Ziurys

2017

ApJ

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“…These studies have been mostly focused on C-rich CSEs given that carbon is more chemically active than oxygen and, therefore, C-rich envelopes are expected and observed to display a large variety of different molecular species (e.g. Cernicharo et al, 2000, Smith et al, 2015). However, the number of studies in the millimeter wavelength range has increased in the last years, and these studies have evidenced that O-rich CSEs do also host a rich variety of molecules (Ziurys et al, 2007, Kim et al, 2010, De Beck et al, 2013, Sánchez Contreras et al, 2015, and references therein).…”

Section: Introductionmentioning

confidence: 99%

The millimeter IRAM-30 m line survey toward IK Tauri

Velilla-Prieto

Contreras

Cernicharo

et al. 2016

A&A

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With a total of ~350 lines detected of 34 different molecular species (including different isotopologues), IK Tau displays a rich chemistry for an oxygen-rich circumstellar envelope. The detection of carbon bearing molecules like HCO, as well as the discrepancies found between our derived abundances and the predictions from chemical models for some molecules, highlight the need for a revision of standard chemical models. We were able to identify at least two different emission components in terms of rotational temperatures. The warm component, which is mainly traced out by SO, is probably arising from the inner regions of the envelope (at ≲8) where SO has a fractional abundance of (SO)~10. This result should be considered for future investigation of the main formation channels of this, and other, parent species in the inner winds of O-rich AGB stars, which at present are not well reproduced by current chemistry models.

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A molecular line survey of a sample of AGB stars and planetary nebulae

Cited by 8 publications

References 39 publications

Opening PANDORA’s box: APEX observations of CO in PNe

Opening PANDORA’s box: APEX observations of CO in PNe

New Detections of HNC in Planetary Nebulae: Evolution of the [Hcn]/[Hnc] Ratio

The millimeter IRAM-30 m line survey toward IK Tauri

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