CO ice mixed with CH3OH: the answer to the non-detection of the 2152 cm−1 band?

Cuppen, H. M.; Penteado, Eduardo Monfardini; Isokoski, K.; Marel, Nienke van der; Linnartz, H.

doi:10.1111/j.1365-2966.2011.19443.x

Cited by 68 publications

(90 citation statements)

References 31 publications

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“…According to Pontoppidan et al (2003), solid CO exists (at least) in three different configurations, in which remarkably water ices are excludedand CO:CH 3 OH interactions favored (Cuppen et al 2011).…”

Section: Implications For Space Chemistrymentioning

confidence: 99%

Chemical Evolution of a Co Ice Induced by Soft X-Rays

Ciaravella

Chen

Cecchi‐Pestellini

et al. 2016

ApJ

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We irradiated a pure carbon monoxide ice with soft X-rays of energies up to 1.2 keV. The experiments were performed using the spherical grating monochromator beamline at the National Synchrotron Radiation Research Center in Taiwan, exploiting both monochromatic (at 0.3 and 0.55 keV) and broader energy (0.25-1.2 keV) fluxes. The infrared spectra of the irradiated ices showed the formation of a number of products such as polycarbon monoand dioxides C n O m , and chains containing up to 10 carbon atoms. While a gentle increase in the energy absorbed by the ice sample is reflected by an increase in the column densities of newly born species, such correlation breaks down at very high fluxes. In this regime the production yield falls down sharply by about a factor of 100. The refractory residue obtained in the broad energy irradiation is a "compromise" between those obtained with proton irradiation of C 3 O 2 and CO ices in previous experiments. Finally, we discuss the possible implications for space chemistry

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Section: Implications For Space Chemistrymentioning

confidence: 99%

Chemical Evolution of a Co Ice Induced by Soft X-Rays

Ciaravella

Chen

Cecchi‐Pestellini

et al. 2016

ApJ

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“…Experiments with all mixtures were performed at the Sackler Laboratory for Astrophysics, Leiden University, Netherlands, except for CO:O 2 :N 2 :CO 2 = 1:5:1:0.5, which was performed at the NASA Ames Research Center, CA, USA. The CO:CH 3 OH spectra are taken from Cuppen et al (2011). The mixtures CO:CH 3 OH = 9:1 and 4:1 are saturated.…”

Section: E X P E R I M E N Ta L S P E C T R Amentioning

confidence: 99%

“…Moreover, since methanol has been shown to be the final product of the hydrogenation of CO ice, methanol could potentially be a good candidate for the red component. With this in mind, we recently published a study (Cuppen et al 2011) in which the widths and positions of infrared laboratory spectra of CO:CH 3 OH ice mixtures were compared with those of the red component of the aforementioned survey by Pontoppidan et al (2003). This comparison showed that the observed spectral characteristics correspond to the characteristics of laboratory spectra of CO:CH 3 OH mixtures with ratios between 1:9 and 9:1.…”

Section: Introductionmentioning

confidence: 99%

“…Furthermore, H 2 O:CO:CO 2 mixtures of different ratios and temperatures were also tested by Cuppen et al (2011) and the conclusion was that such mixtures can indeed suppress the 2152 cm −1 feature, but (1) the amount of CO 2 needed for that is unrealistic, and the spectral characteristics of the red component cannot be properly reproduced, and (2) more realistic ratios can make the 2152 cm −1 feature weaker only for annealed ices. However, Cuppen et al (2011) did not consider the shape and depths of the CH 3 OH and H 2 O bands, nor did they consider grain shape effects. As pointed out by Tielens et al (1991), grain shape can induce changes in the profiles of ice mixtures which contain CO in a high concentration.…”

Section: Introductionmentioning

confidence: 99%

“…This source also shows a salience at long wavelengths of the CO feature, and the detection of CH 3 OH has also been reported (Boogert, Hogerheijde & Blake 2002a;Boogert et al 2008), but with lower abundance. Although we work with a smaller sample than Cuppen et al (2011), the present study includes new details, such as grain shape corrections and direct comparison between laboratory and observed spectra. The latter are taken at much higher resolution than the observations used in the earlier study.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Spectroscopic constraints on CH₃OH formation: CO mixed with CH₃OH ices towards young stellar objects

Penteado

Boogert

Pontoppidan

et al. 2015

Mon. Not. R. Astron. Soc.

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The prominent infrared absorption band of solid CO -commonly observed towards young stellar objects (YSOs) -consists of three empirically determined components. The broad 'red component' (2136 cm −1 , 4.681 μm) is generally attributed to solid CO mixed in a hydrogenbonded environment. Usually, CO embedded in the abundantly present water is considered. However, CO:H 2 O mixtures cannot reproduce the width and position of the observed red component without producing a shoulder at 2152 cm −1 , which is not observed in astronomical spectra. Cuppen et al. showed that CO:CH 3 OH mixtures do not suffer from this problem. Here, this proposition is expanded by comparing literature laboratory spectra of different CO-containing ice mixtures to high-resolution (R = λ/ λ = 25 000) spectra of the massive YSO AFGL 7009S and of the low-mass YSO L1489 IRS. The previously unpublished spectrum of AFGL 7009S shows a wide band of solid 13 CO, the first detection of 13 CO ice in the polar phase. In this source, both the 12 CO and 13 CO ice bands are well fitted with CO:CH 3 OH mixtures, while respecting the profiles and depths of the methanol bands at other wavelengths, whereas mixtures with H 2 O cannot. The presence of a gradient in the CO:CH 3 OH mixing ratio in the grain mantles is also suggested. Towards L1489 IRS, the profile of the 12 CO band is also better fitted with CH 3 OH-containing ices, although the CH 3 OH abundance needed is a factor of 2.4 above previous measurements. Overall, however, the results are reasonably consistent with models and experiments about formation of CH 3 OH by the hydrogenation of CO ices.

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