ETHYL CYANIDE ON TITAN: SPECTROSCOPIC DETECTION AND MAPPING USING ALMA

M. A. Cordiner; M. Y. Palmer; C. A. Nixon; P. G. J. Irwin; N. A. Teanby; S. B. Charnley; M. J. Mumma; Z. Kisiel; J. Serigano; Y. -J. Kuan; Y. -L. Chuang; K. -S. Wang

doi:10.1088/2041-8205/800/1/L14

ETHYL CYANIDE ON TITAN: SPECTROSCOPIC DETECTION AND MAPPING USING ALMA

M. A. Cordiner, M. Y. Palmer, C. A. Nixon, P. G. J. Irwin, N. A. Teanby, S. B. Charnley, M. J. Mumma, Z. Kisiel, J. Serigano, Y. -J. Kuan, Y. -L. Chuang, K. -S. Wang

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Abstract

We report the first spectroscopic detection of ethyl cyanide (C2H5CN) in Titan's atmosphere, obtained using spectrally and spatially resolved observations of multiple emission lines with the Atacama Large Millimeter/submillimeter Array (ALMA). The presence of C2H5CN in Titan's ionosphere was previously inferred from Cassini ion mass spectrometry measurements of C2H5CNH+. Here we report the detection of 27 rotational lines from C2H5CN (in 19 separate emission features detected at confidence) in the frequency range 222–241 GHz. Simultaneous detections of multiple emission lines from HC3N, CH3CN, and CH3CCH were also obtained. In contrast to HC3N, CH3CN, and CH3CCH, which peak in Titan's northern (spring) hemisphere, the emission from C2H5CN is found to be concentrated in the southern (autumn) hemisphere, suggesting a distinctly different chemistry for this species, consistent with a relatively short chemical lifetime for C2H5CN. Radiative transfer models show that C2H5CN is most concentrated at altitudes km, suggesting production predominantly in the stratosphere and above. Vertical column densities are found to be in the range (1–5) × 1014 cm−2.

Original language	Undefined/Unknown
Pages (from-to)	1-7
Number of pages	7
Journal	Astrophysical Journal Letters
Volume	800
Issue number	1
DOIs	https://doi.org/10.1088/2041-8205/800/1/L14
Publication status	Published - 11 Feb 2015

Keywords

astro-ph.EP
planets and satellites: individual (Titan)
techniques: interferometric
planets and satellites: atmospheres
– techniques: imaging spectroscopy

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10.1088/2041-8205/800/1/L14

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© 2015. The American Astronomical Society. All rights reserved.
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3 Finished

Research into planetary formation at Bristol.
Elliott, T. R.
1/04/15 → 28/02/19
Project: Research
Nick Teanby's Leverhulme Prize
Teanby, N. A.
1/03/11 → 1/03/14
Project: Research
Mars and Titan's atmosphere and interior
Teanby, N. A.
1/07/10 → 1/10/13
Project: Research

Cite this

@article{0a16260bf1cb4ec68d49cd4f7871f9ed,

title = "ETHYL CYANIDE ON TITAN: SPECTROSCOPIC DETECTION AND MAPPING USING ALMA",

abstract = "We report the first spectroscopic detection of ethyl cyanide (C2H5CN) in Titan's atmosphere, obtained using spectrally and spatially resolved observations of multiple emission lines with the Atacama Large Millimeter/submillimeter Array (ALMA). The presence of C2H5CN in Titan's ionosphere was previously inferred from Cassini ion mass spectrometry measurements of C2H5CNH+. Here we report the detection of 27 rotational lines from C2H5CN (in 19 separate emission features detected at confidence) in the frequency range 222–241 GHz. Simultaneous detections of multiple emission lines from HC3N, CH3CN, and CH3CCH were also obtained. In contrast to HC3N, CH3CN, and CH3CCH, which peak in Titan's northern (spring) hemisphere, the emission from C2H5CN is found to be concentrated in the southern (autumn) hemisphere, suggesting a distinctly different chemistry for this species, consistent with a relatively short chemical lifetime for C2H5CN. Radiative transfer models show that C2H5CN is most concentrated at altitudes km, suggesting production predominantly in the stratosphere and above. Vertical column densities are found to be in the range (1–5) × 1014 cm−2.",

keywords = "astro-ph.EP, planets and satellites: individual (Titan), techniques: interferometric, planets and satellites: atmospheres, – techniques: imaging spectroscopy",

author = "Cordiner, {M. A.} and Palmer, {M. Y.} and Nixon, {C. A.} and Irwin, {P. G. J.} and Teanby, {N. A.} and Charnley, {S. B.} and Mumma, {M. J.} and Z. Kisiel and J. Serigano and Kuan, {Y. -J.} and Chuang, {Y. -L.} and Wang, {K. -S.}",

year = "2015",

month = feb,

day = "11",

doi = "10.1088/2041-8205/800/1/L14",

language = "Undefined/Unknown",

volume = "800",

pages = "1--7",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "IOP Publishing",

number = "1",

}

ETHYL CYANIDE ON TITAN : SPECTROSCOPIC DETECTION AND MAPPING USING ALMA. / Cordiner, M. A.; Palmer, M. Y.; Nixon, C. A.; Irwin, P. G. J.; Teanby, N. A.; Charnley, S. B.; Mumma, M. J.; Kisiel, Z.; Serigano, J.; Kuan, Y. -J.; Chuang, Y. -L.; Wang, K. -S.

In: Astrophysical Journal Letters, Vol. 800, No. 1, 11.02.2015, p. 1-7.

Research output: Contribution to journal › Article (Academic Journal) › peer-review

TY - JOUR

T1 - ETHYL CYANIDE ON TITAN

T2 - SPECTROSCOPIC DETECTION AND MAPPING USING ALMA

AU - Cordiner, M. A.

AU - Palmer, M. Y.

AU - Nixon, C. A.

AU - Irwin, P. G. J.

AU - Teanby, N. A.

AU - Charnley, S. B.

AU - Mumma, M. J.

AU - Kisiel, Z.

AU - Serigano, J.

AU - Kuan, Y. -J.

AU - Chuang, Y. -L.

AU - Wang, K. -S.

PY - 2015/2/11

Y1 - 2015/2/11

N2 - We report the first spectroscopic detection of ethyl cyanide (C2H5CN) in Titan's atmosphere, obtained using spectrally and spatially resolved observations of multiple emission lines with the Atacama Large Millimeter/submillimeter Array (ALMA). The presence of C2H5CN in Titan's ionosphere was previously inferred from Cassini ion mass spectrometry measurements of C2H5CNH+. Here we report the detection of 27 rotational lines from C2H5CN (in 19 separate emission features detected at confidence) in the frequency range 222–241 GHz. Simultaneous detections of multiple emission lines from HC3N, CH3CN, and CH3CCH were also obtained. In contrast to HC3N, CH3CN, and CH3CCH, which peak in Titan's northern (spring) hemisphere, the emission from C2H5CN is found to be concentrated in the southern (autumn) hemisphere, suggesting a distinctly different chemistry for this species, consistent with a relatively short chemical lifetime for C2H5CN. Radiative transfer models show that C2H5CN is most concentrated at altitudes km, suggesting production predominantly in the stratosphere and above. Vertical column densities are found to be in the range (1–5) × 1014 cm−2.

AB - We report the first spectroscopic detection of ethyl cyanide (C2H5CN) in Titan's atmosphere, obtained using spectrally and spatially resolved observations of multiple emission lines with the Atacama Large Millimeter/submillimeter Array (ALMA). The presence of C2H5CN in Titan's ionosphere was previously inferred from Cassini ion mass spectrometry measurements of C2H5CNH+. Here we report the detection of 27 rotational lines from C2H5CN (in 19 separate emission features detected at confidence) in the frequency range 222–241 GHz. Simultaneous detections of multiple emission lines from HC3N, CH3CN, and CH3CCH were also obtained. In contrast to HC3N, CH3CN, and CH3CCH, which peak in Titan's northern (spring) hemisphere, the emission from C2H5CN is found to be concentrated in the southern (autumn) hemisphere, suggesting a distinctly different chemistry for this species, consistent with a relatively short chemical lifetime for C2H5CN. Radiative transfer models show that C2H5CN is most concentrated at altitudes km, suggesting production predominantly in the stratosphere and above. Vertical column densities are found to be in the range (1–5) × 1014 cm−2.

KW - astro-ph.EP

KW - planets and satellites: individual (Titan)

KW - techniques: interferometric

KW - planets and satellites: atmospheres

KW - – techniques: imaging spectroscopy

U2 - 10.1088/2041-8205/800/1/L14

DO - 10.1088/2041-8205/800/1/L14

M3 - Article (Academic Journal)

VL - 800

SP - 1

EP - 7

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

SN - 2041-8205

IS - 1

ER -

ETHYL CYANIDE ON TITAN: SPECTROSCOPIC DETECTION AND MAPPING USING ALMA

Abstract

Keywords

Access to Document

Projects

Research into planetary formation at Bristol.

Nick Teanby's Leverhulme Prize

Mars and Titan's atmosphere and interior

Cite this