Observations of Solid Carbon Dioxide in Molecular Clouds with the<i>Infrared Space Observatory</i>

Gerakines, Perry A.; Whittet, D. C. B.; Ehrenfreund, P.; Boogert, A. C. A.; Tielens, A. G. G. M.; Schütte, W. A.; Chiar, J. E.; Dishoeck, E. F. van; Prusti, T.; Helmich, Frank; Graauw, Th. de

doi:10.1086/307611

Cited by 270 publications

(468 citation statements)

References 41 publications

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“…Support for this expectation comes from infrared observations of ubiquitous solid CO 2 (Gerakines et al 1999). …”

Section: Solid Phase Processesmentioning

confidence: 97%

The chemistry of high-mass star formation

Tak¹,

Floris²

2005

Proc. IAU

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Abstract. This paper reviews the chemistry of star-forming regions, with an emphasis on the formation of high-mass stars. We first outline the basic molecular processes in dense clouds, their implementation in chemical models, and techniques to measure molecular abundances. Then, recent observational, theoretical and laboratory developments are reviewed on the subjects of hot molecular cores, cosmic-ray ionization, depletion and deuteration, and oxygen chemistry. The paper concludes with a summary of outstanding problems and future opportunities.

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“…Support for this expectation comes from infrared observations of ubiquitous solid CO 2 (Gerakines et al 1999). …”

Section: Solid Phase Processesmentioning

confidence: 97%

The chemistry of high-mass star formation

Tak¹,

Floris²

2005

Proc. IAU

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“…In many cases, the ices were subsequently warmed, or warmed and cooled, and additional spectra were taken at higher temperatures. Temperatures where spectra were measured were selected based on where ice segregation is known to occur (e.g., Blake et al, 1991;Jenniskens and Blake, 1996;Ehrenfreund et al, 1997Gerakines et al, 1999). The temperature of the sample window inside the chamber was adjusted from 15 K up to 170 K at a rate of 2 K min À1 and cooled at a rate of $10 K min À1 in order to observe effects on the ice sample when the temperature is cycled.…”

Section: Methodsmentioning

confidence: 99%

“…Infrared (IR) absorption spectroscopy in the near-IR (k = $0.9-2.5 lm) and mid-IR (k = 2.5-25 lm) are powerful methods by which these icy components can be detected and studied. IR absorption band positions and profiles are used for identification of physical properties such as composition, and temperature Allamandola et al (1992), Salama et al (1994), Chiar et al (1995), , Gerakines et al (1999), Gibb et al (2000), Bernstein et al (2005), White et al (2009), andÖberg et al (2009). Temperatures of H 2 O-dominated ice mixtures can range from 10 to 15 K in quiescent interstellar dust cloud environments to as high as 100-150 K around protostellar disks.…”

Section: Introductionmentioning

confidence: 99%

“…Temperatures of H 2 O-dominated ice mixtures typically found on outer Solar System surfaces typically range from 50 to 160 K. These temperatures can vary with time and location, depending on sunlight exposure, local geological activity, etc. CO 2 is important in studies of icy surfaces on planetary bodies in the Solar System because the IR absorption profiles of CO 2 -containing ices created in the laboratory have been shown to be sensitive to conditions of the ice such as temperature, temperature history, ice composition, and radiation exposure (Sandford and Allamandola, 1990a;Ehrenfreund et al, 1998Gerakines et al, 1999;Dartois et al, 1999;Moore et al, 2001;Moore, 2000, 2001;van Broekhuizen et al, 2006;Hodyss et al, 2008;White et al, 2009;Öberg et al, 2007. These investigations provide a relevant database indispensable to spectral analysis from remote measurements (e.g., Sandford and Allamandola, 1990a;Ehrenfreund et al, 1998;Gálvez et al, 2007;Gerakines et al, 2005;Cook et al, 2011).…”

Section: Introductionmentioning

confidence: 99%

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Laboratory spectra of CO2 vibrational modes in planetary ice analogs

White

Mastrapa

Sandford

2012

Icarus

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a b s t r a c tLaboratory spectra have shown that CO 2 is a powerful diagnostic tool for analyzing infrared data from remote observations, as it has been detected on icy moons in the outer Solar System as well as dust grain surfaces in the interstellar medium (ISM). IR absorption band profiles of CO 2 within ice mixtures containing H 2 O and CH 3 OH change with respect to temperature and mixture ratios. In this particular study, the m 3 CO 2 asymmetric stretch mode near 4.3 lm (2350 cm À1 ), overtone mode near 1.97 lm (5080 cm À1 ), and the combination bands near 2.7 lm (3700 cm À1 ), 2.8 lm (3600 cm À1 ), and 2.02 lm (4960 cm À1 ), are systematically observed in different mixtures with H 2 O and CH 3 OH in temperature ranges from 15 K to 150 K. Additionally, some high-temperature deposits (T > 50 K) of H 2 O, CH 3 OH, and CO 2 ice mixtures were performed and it was discovered that CO 2 may deposit out at higher temperatures than previously recorded. These data may then be used to interpret infrared observational data obtained from icy surfaces in the outer Solar System and beyond.

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“…The ISO spectra combined with extensive laboratory studies focusing on both the CO stretching and bending modes of this molecule have provided great insight into the various forms of mixed molecular ices present in dense clouds. [118,143,152,[196][197][198][199][200] …”

Section: Co 2 (Carbon Dioxide)mentioning

confidence: 99%

From Interstellar Polycyclic Aromatic Hydrocarbons and Ice to Astrobiology

Allamandola

Hudgins

2003

Solid State Astrochemistry

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Tremendous strides have been made in our understanding of interstellar material over the past twenty years thanks to significant, parallel developments in observational astronomy and laboratory astrophysics. Twenty years ago the composition of interstellar dust was largely guessed at, the concept of ices in dense molecular clouds ignored, and the notion of large, abundant, gas phase, carbon rich molecules widespread throughout the interstellar medium (ISM) considered impossible.Today the composition of dust in the diffuse ISM is reasonably well constrained to micron-sized cold refractory materials comprised of amorphous and crystalline silicates mixed with an amorphous carbonaceous material containing aromatic structural units and short, branched aliphatic chains. In dense molecular clouds, the birthplace of stars and planets, these cold dust particles are coated with mixed molecular ices whose major components are is very well constrained. Lastly, the signature of carbon-rich polycyclic aromatic hydrocarbons (PAHs), shockingly large molecules by earlier interstellar chemistry standards, is widespread throughout the Universe. This paper presents a detailed summary of these disparate interstellar components and ends by considering both of them as important feedstock to the chemical inventory of the primordial Earth. Particular attention is paid to their possible role in the chemistry that led to the origin of life. An extensive reference list is given to allow the student entry into the full depth of the literature.The first part of this paper focuses on interstellar PAHs. The laboratory and theoretical underpinning which supports the PAH model is reviewed in some detail. This is followed by a few specific examples which demonstrate how these data can be used to analyze the interstellar spectra and probe local conditions in different emission zones. These examples include tracing the evolution of carbon as it passes from its birthsite in circumstellar shells through the ISM, determining specifics about the cosmic PAH population in many different environments including PAH size and structure, and probing local conditions in the different emission zones.The second part of this paper summarizes the laboratory and observational background leading to our current understanding of interstellar/precometary ices. Although the most abundant interstellar ice components are the very simple molecules such as H 2 O, CH 3 OH, CO, CO 2 , and NH 3 , more complex species including accreted PAHs and those formed by UV and cosmic ray processing within the ice must also be present. Here we give a detailed summary of the photochemical evolution on those ices 2 found in the densest regions of molecular clouds, the regions where stars and planetary systems are formed. Ultraviolet photolysis of these ices produces a host of new compounds, some of which show intriguing prebiotic behavior.The last part of this paper draws all this information together and considers the possible roles these compounds might have played in early Earth...

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Observations of Solid Carbon Dioxide in Molecular Clouds with theInfrared Space Observatory

Cited by 270 publications

References 41 publications

The chemistry of high-mass star formation

The chemistry of high-mass star formation

Laboratory spectra of CO2 vibrational modes in planetary ice analogs

From Interstellar Polycyclic Aromatic Hydrocarbons and Ice to Astrobiology

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