Near-Arcsecond Resolution Observations of the Hot Corino of the Solar-Type Protostar IRAS 16293–2422

By S. Bottinelli, C. Ceccarelli, R. Neri, Jonathan P. Williams, E. Caux, S. Cazaux, Bertrand Lefloch, S. Maret, A. F. L. D. D. Grenoble, Institute for Astronomy and 5 more. 2004

159 citations recorded by the source corpus.

Complex organic molecules have previously been discovered in solar-type protostars, raising the questions of where and how they form in the envelope. Possible formation mechanisms include grain mantle evaporation, the interaction of the outflow with its surroundings, and/or the impact of UV/X-rays inside the cavities. In this Letter we present the first interferometric observations of two complex molecules, CH3CN and HCOOCH3, toward the solar-type protostar IRAS 16293-2422. The images show that the emission originates from two compact regions centered on the two components of the binary system. We discuss how these results favor the grain mantle evaporation scenario, and we investigate the implications of these observations for the chemical composition and physical and dynamical state of the two components.

Subfields: Astronomy and Astrophysics, Organic Chemistry

View Paper: https://www.semanticscholar.org/paper/ded64fdaa77604cfcdf94f205a0a88ea1504310e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Caselli
2. E. Herbst
3. Cecilia Ceccarelli
4. R. Garrod
5. E. Dishoeck
6. V. Wakelam
7. E. V. van Dishoeck
8. A. Tielens

In Organic Chemistry

1. A. Tielens
2. R. Garrod
3. E. V. van Dishoeck
4. P. Caselli
5. E. Herbst
6. V. Wakelam
7. Cecilia Ceccarelli
8. I. Jiménez-Serra

Citations in the corpus

• DETECTION OF THE SIMPLEST SUGAR, GLYCOLALDEHYDE, IN A SOLAR-TYPE PROTOSTAR WITH ALMA (2012, background): “…studies of its chemistry have revealed strong differentiation among different species toward the two components in the binary (IRAS16293A and IRAS16293B; Wootten 1989) including complex organic molecules (Bottinelli et al. 2004; Schöier et al. 2004; Bisschop et al. 2008; Jørgensen et al. 2011).”
• Our astrochemical heritage (2012, background): “Since then, more low-mass hot cores have been discovered and, to distinguish them from the high-mass hot cores, they were called hot corinos ([60]; [61]; [62]; [256]; [230]; see also the review by [203]).”
• Formation of Complex Molecules in Prestellar Cores: A Multilayer Approach (2017, background): “Formation of COMs in hot cores and corinos is reasonably well explained by the “warm-up scenario” (Garrod & Herbst 2006; Garrod et al. 2008), in which complex organic molecules first form via surface radical-radical reactions at 30– 40 K and then evaporate to the gas at higher temperatures reaching ”
• Molecular Evolution and Star Formation: From Prestellar Cores to Protostellar Cores (2007, background): “We are dealing here with the formation of a low-mass protostar, so the hot-core stage is more aptly referred to as a “hot corino”, and short time scales have previously been discussed for such regions (Wakelam et al. 2004; Bottinelli et al. 2004a).”
• The Molecular Universe (2011, background): “In recent years, regions with similar characteristics as hot cores – but much smaller and therefore labeled hot corino’s – have also been discovered around solar-type protostars (Bottinelli et al. 2004).”
• Complex Chemistry in Star-forming Regions: An Expanded Gas-Grain Warm-up Chemical Model (2008, background): “The low-mass protostellar analogs of hot cores, the so-called ‘hot corinos’, also show strong signatures of complex molecules (Cazaux et al. 2003; Bottinelli et al. 2004a,b).”
• Hot corinos in NGC 1333-IRAS4B and IRAS2A (2006, background): “We also have a possible detection for C2H5OH at 226.661 GHz in IRAS4B2.”
• PROSAC: A Submillimeter Array Survey of Low-Mass Protostars. I. Overview of Program: Envelopes, Disks, Outflows, and Hot Cores (2007, background): “More recently, Bottinelli et al. (2004) resolved the emission of complex organic species, CH3CN andHCOOCH3, toward this source and derived a size of 100AU, comparable to the expected size of the hot corino.”
• Organic molecules in the Galactic center - Hot core chemistry without hot cores (2006, methodology): “In this case the molecular abundances were derived by assuming a source size of 0.5′′ for IRAS 4A (Bottinelli et al. 2004a), 0.25′′ for IRAS 4B, 0.43′′ for IRAS 2A (Maret et al. 2004), and 2′′ for IRAS 16293-2422 (Cazaux et al. 2003).”