Seeds of Life in Space (SOLIS)

Codella, C.; Ceccarelli, C.; Caselli, P.; Balucani, Nadia; Barone, Vincenzo; Fontani, F.; Leflóch, B.; Podio, L.; Viti, S.; Feng, Siyi; Bachiller, R.; Bianchi, E.; Dulieu, F.; Jiménez-Serra, Izaskun; Holdship, Jonathan; Neri, R.; Pineda, Jaime E.; Pon, Andy; Sims, Ian; Spezzano, S.; Vasyunin, A. I.; Alves, F. O.; Bizzocchi, L.; Bottinelli, S.; Caux, E.; Chacón-Tanarro, A.; Choudhury, R.; Coutens, A.; Favre, Cécile; Hily-Blant, Pierre; Kahane, C.; Al-Edhari, A. Jaber; Laas, J.; López-Sepulcre, A.; Ospina, Juan Felipe Orozco; Oya, Yoko; Punanova, A.; Puzzarini, Cristina; Quénard, D.; Rimola, Albert; Sakai, Nami; Skouteris, Dimitrios; Taquet, V.; Testi, L.; Theulé, Patrice; Ugliengo, Piero; Vastel, C.; Vazart, Fanny; Wiesenfeld, Laurent; Yamamoto, Satoshi

doi:10.1051/0004-6361/201731249

Cited by 108 publications

(73 citation statements)

References 46 publications

(78 reference statements)

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“…In recent years, formamide has been observed in low-mass star formation environments such as shocked regions by protostellar jets (e.g., Codella et al 2017). Protostellar shocks produced by episodic jets of matter propagate at supersonic velocity through dense gas surrounding the star.…”

Section: Astrophysical Context and The Importance Of Temperature-progmentioning

confidence: 99%

“…Protostellar shocks produced by episodic jets of matter propagate at supersonic velocity through dense gas surrounding the star. In these shocked regions, the presence of a large number of molecules is due to mechanical release by gas-grain collisions and grain-grain collisions (López-Sepulcre et al 2019;Codella et al 2017). Aside from protostellar shocks, the other low-mass star for-mation environments where formamide has been detected are hot corinos (Kahane et al 2013;López-Sepulcre et al 2015;Marcelino et al 2018;Imai et al 2016;Oya et al 2017;Lee et al 2017).…”

Section: Astrophysical Context and The Importance Of Temperature-progmentioning

confidence: 99%

“…Furthermore, during landing of Philae aboard Rosetta mission, in situ mass spectrometer data inferred the presence of formamide in the comet nucleus with the highest abundance after water (Goesmann et al 2015). In recent years, formamide was also observed in two types of low-mass star forming environment: shocked regions by protostellar jets (e.g., Codella et al 2017) and hot corinos (Kahane et al 2013;López-Sepulcre et al 2015;Marcelino et al 2018;Imai et al 2016;Oya et al 2017;Lee et al 2017). In hightemperature regions (>100 K) such as hot corinos, thermal desorption is responsible for sublimation of frozen mantles into the gas phase.…”

Section: Introductionmentioning

confidence: 99%

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Photoprocessing of formamide ice: route towards prebiotic chemistry in space

Corazzi

Fedele

Poggiali

et al. 2020

A&A

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Aims. Formamide (HCONH 2 ) is the simplest molecule containing the peptide bond first detected in the gas phase in Orion-KL and SgrB 2 . In recent years, it has been observed in high temperature regions such as hot corinos, where thermal desorption is responsible for the sublimation of frozen mantles into the gas phase. The interpretation of observations can benefit from information gathered in the laboratory, where it is possible to simulate the thermal desorption process and to study formamide under simulated space conditions such as UV irradiation. Methods. Here, two laboratory analyses are reported: we studied formamide photo-stability under UV irradiation when it is adsorbed by space relevant minerals at 63 K and in the vacuum regime. We also investigated temperature programmed desorption of pure formamide ice in the presence of TiO 2 dust before and after UV irradiation. Results. Through these analyses, the effects of UV degradation and the interaction between formamide and different minerals are compared. We find that silicates, both hydrates and anhydrates, offer molecules a higher level of protection from UV degradation than mineral oxides. The desorption temperature found for pure formamide is 220 K. The desorption temperature increases to 250 K when the formamide desorbs from the surface of TiO 2 grains. Conclusions. Through the experiments outlined here, it is possible to follow the desorption of formamide and its fragments, simulate the desorption process in star forming regions and hot corinos, and constrain parameters such as the thermal desorption temperature of formamide and its fragments and the binding energies involved. Our results offer support to observational data and improve our understanding of the role of the grain surface in enriching the chemistry in space.

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Section: Astrophysical Context and The Importance Of Temperature-progmentioning

confidence: 99%

Section: Astrophysical Context and The Importance Of Temperature-progmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Photoprocessing of formamide ice: route towards prebiotic chemistry in space

Corazzi

Fedele

Poggiali

et al. 2020

A&A

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“…On the other hand, interferometry is the way to image the small (down to ∼ 1 ) regions chemically enriched due to the passage of a shock. In this context, a large number of studies have revealed bow shocks and cavities opened by protostellar jets (Gueth et al 1998;Bachiller et al 1998;Benedettini et al 2007Benedettini et al , 2013Codella et al 2009Codella et al , 2017Persson et al 2012;Santangelo et al 2015;Lefèvre et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Seeds of Life in Space (SOLIS)

Taquet

Codella

Simone

et al. 2020

A&A

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Context. Low-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows.Aims. The evolution of sulfur chemistry is studied along the outflows driven by the NGC1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. Methods. We observed various transitions from OCS, CS, SO, and SO 2 towards NGC1333-IRAS4A in the 1.3, 2, and 3mm bands using the IRAM NOrthern Extended Millimeter Array (NOEMA) and we interpreted the observations through the use of the Paris-Durham shock model. Results. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO 2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east -south west (NE-SW) direction. SO is detected at extremely high radial velocity up to +25 km s −1 relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO 2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO 2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 10 5 cm −3 and relatively warm (T > 100 K) temperatures in most cases. Conclusions. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputtered into the shock gas. In contrast, the longer and likely older outflow triggered by IRAS4A2 is more enriched in species that have a gas phase origin, such as SO 2 .

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“…Atacama Large Millimeter/submillimeter Array (ALMA) observations by Coutens et al (2016) of IRAS 16293-2422 show that the deuterium fractions in HNCO and NH 2 CHO are very similar, implying a chemical link. On the other hand, Codella et al (2017) observed a shock near L1157-B1 using interferometric observations. Through these observations and follow-up chemical modeling, they concluded that NH 2 CHO is made efficiently in the gas phase from H 2 CO, at least in this source.…”

Section: Introductionmentioning

confidence: 99%

Exploring the formation pathways of formamide

Allen

Tak

López-Sepulcre

et al. 2020

A&A

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Context. As a building block for amino acids, formamide (NH 2 CHO) is an important molecule in astrobiology and astrochemistry, but its formation path in the interstellar medium is not understood well. Aims. We aim to find empirical evidence to support the chemical relationships of formamide to HNCO and H 2 CO. Methods. We examine high angular resolution (∼ 0.2 ) Atacama Large Millimeter/submillimeter Array (ALMA) maps of six sources in three high-mass star-forming regions and compare the spatial extent, integrated emission peak position, and velocity structure of HNCO and H 2 CO line emission with that of NH 2 CHO by using moment maps. Through spectral modeling, we compare the abundances of these three species.Results. In these sources, the emission peak separation and velocity dispersion of formamide emission is most often similar to HNCO emission, while the velocity structure is generally just as similar to H 2 CO and HNCO (within errors). From the spectral modeling, we see that the abundances between all three of our focus species are correlated, and the relationship between NH 2 CHO and HNCO reproduces the previously demonstrated abundance relationship. Conclusions. In this first interferometric study, which compares two potential parent species to NH 2 CHO, we find that all moment maps for HNCO are more similar to NH 2 CHO than H 2 CO in one of our six sources (G24 A1). For the other five sources, the relationship between NH 2 CHO, HNCO, and H 2 CO is unclear as the different moment maps for each source are not consistently more similar to one species as opposed to the other.

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Seeds of Life in Space (SOLIS)

Cited by 108 publications

References 46 publications

Photoprocessing of formamide ice: route towards prebiotic chemistry in space

Photoprocessing of formamide ice: route towards prebiotic chemistry in space

Seeds of Life in Space (SOLIS)

Exploring the formation pathways of formamide

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