The Hot Core around the Low-Mass Protostar IRAS 16293–2422: Scoundrels Rule!

By S. Cazaux, A. Tielens, C. Ceccarelli, A. Castets, V. Wakelam, E. Caux, B. Parise, D. Teyssier. 2003

401 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/5c8d6237eb4159ea5b1a8e55e2684f5aa7f25b40

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

In Atmospheric Science

In Spectroscopy

Citations in the corpus

Formation of complex organic molecules in cold objects: the role of gas-phase reactions (2015, background): “…Cecilia.Ceccarelli@obs.ujf-grenoble.fr ‡ E-mail: vianney.taquet@nasa.gov paradigm has lasted for almost two decades, until new observations (e.g. Cazaux et al. 2003; Bottinelli et al. 2007; Requena-Torres et al. 2006), laboratory experiments (Geppert et al. 2007) and theoretical studies…”
Formation rates of complex organics in UV irradiated CH3OH-rich ices I: Experiments (2009, background): “…complexity are being detect d in star-forming regions (Blake et al. 1987; Nummelin et al. 2000; Bisschop et al. 2007b; van Dishoeck et al. 1995; Cazaux et al. 2003; Bottinelli et al. 2004, 2007; Belloche et al. 2009); however, the origins of these complex molecules are the subject of debate.”
Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores (2006, background): “…observed abundances at temperatures of ∼100 K. Numerous allusions have been made (e.g. Charnley et al. 1995; Ehrenfreund & Charnley 2000; Cazaux et al. 2003; Peeters et al. 2006) to the possibility that methyl formate is produced on dust-grain surfaces at some point in the evolution of…”
A COLD COMPLEX CHEMISTRY TOWARD THE LOW-MASS PROTOSTAR B1-b: EVIDENCE FOR COMPLEX MOLECULE PRODUCTION IN ICES (2010, background): “Complex organic molecules have been detected toward a range of astrophysical environments, including low-mass protostars (van Dishoeck et al. 1995; Cazaux et al. 2003; Bottinelli et al. 2007); however, the origins of these complex molecules as well as their fates are uncertain.”
Testing grain surface chemistry : a survey of deuterated formaldehyde and methanol in low-mass Class 0 protostars (2006, background): “Indeed Bottinelli et al.(2004) observed complex molecules in the Hot Core of IRAS4A, molecules that were detected for the first time in a low-mass protostar towards IRAS16293 (Cazaux et al. 2003).”
Complex Molecules in the Hot Core of the Low-Mass Protostar NGC 1333 IRAS 4A (2004, methodology): “The most important result of the present work is the detection of complex molecules in the hot corino of IRAS4A, the second Class 0 in which those molecules have been searched for, after IRAS16293 (Cazaux et al. 2003).”
THE ORIGIN OF COMPLEX ORGANIC MOLECULES IN PRESTELLAR CORES (2014, background): “Since then, they have been discovered in a variety of environments such as low-mass hot corinos (Cazaux et al. 2003; Bottinelli et al. 2004; Ceccarelli 2005) and cold envelopes (Jaber et al. 2014), Galactic Center cold clouds (Requena-Torrelles et al. 2006), and prestellar cores (Öberg et al.…”
Hot corinos in NGC 1333-IRAS4B and IRAS2A (2006, background): “Indeed, in the two sources where hot corinos have been detected so far, IRAS 16293 (Cazaux et al. 2003) and IRAS4A (Bottinelli et al. 2004a), similar jumps in the formaldehyde and/or methanol abundances have also been claimed (Maret et al. 2004, 2005), supporting the choice of our targets.”
Complex Molecules in the L1157 Molecular Outflow (2008, methodology): “Even so, similar low temperatures have also been derived for the same complex molecules in the gas immediately surrounding low-mass protostars (Cazaux et al. 2003; Bottinelli et al. 2004; 2007).”
On the Formation of Glycolaldehyde (HCOCH2OH) and Methyl Formate (HCOOCH3) in Interstellar Ice Analogs (2007, background): “Since then it has also been observed in several other hot molecular cores (Remijan et al. 2002, 2003), in high-mass starforming regions (Remijan et al. 2004), in the low-mass protostar IRAS 16293 2422 (Cazaux et al. 2003), and also toward the protoYplanetary nebula CRL 618 (Remijan et al. 2005).”
Our astrochemical heritage (2012, background): “…evaporate and all species trapped in them are released in the gas phase, giving rise to a rich chemistry, first discovered in high-mass protostellar envelopes and called hot core chemistry (e.g., Blake et al. 1987), and successively unveiled in low-mass protostellar envelopes (Cazaux et al. 2003).”
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).”
Organic molecules in protoplanetary disks around T Tauri and Herbig Ae stars (2004, background): “…protoplanetary disks studied here, only a few ×104 yr, and its chemistry is particularly rich as shown by the number of species found in surveys in the (sub)millimeter range (e.g., van Dishoeck et al. 1995; Ceccarelli et al. 2001; Schöier et al. 2002, Cazaux et al. 2003 and references therein).”
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).”
Near-Arcsecond Resolution Observations of the Hot Corino of the Solar-Type Protostar IRAS 16293–2422 (2004, background): “The proof that the complex organic molecules detected by Cazaux et al. (2003) and Bottinelli et al. (2004) originate from the inner warm regions (envelope or disk), called hot corinos (Ceccarelli 2004; Bottinelli et al. 2004), was still missing until today.”
The c2d Spitzer Spectroscopic Survey of Ices around Low-Mass Young Stellar Objects. I. H2O and the 5-8 μm Bands (2007, background): “The relative abundances of N-, C-, and O-bearing species coming from the ices determine directly the type of chemistry in hot cores (or ‘hot corinos’ for low mass objects; e.g. Cazaux et al. 2003).”