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Your search keyword '"Cosentino, G."' showing total 11 results
Start Over Author "Cosentino, G." Journal monthly notices of the royal astronomical society
11 results on '"Cosentino, G."'

2. The complex organic molecular content in the L1517B starless core.

Author

Megías, A, Jiménez-Serra, I, Martín-Pintado, J, Vasyunin, A I, Spezzano, S, Caselli, P, Cosentino, G, and Viti, S

Subjects
METHANOL, MOLECULES, ASTROCHEMISTRY
Abstract

Recent observations of the pre-stellar core L1544 and the younger starless core L1498 have revealed that complex organic molecules (COMs) are enhanced in the gas phase towards their outer and intermediate-density shells. Our goal is to determine the level of chemical complexity towards the starless core L1517B, which seems younger than L1498, and compare it with the other two previously studied cores to see if there is a chemical evolution within the cores. We have carried out 3 mm high-sensitivity observations towards two positions in the L1517B starless core: the core's centre and the position where the methanol emission peaks (at a distance of ∼5000 au from the core's centre). Our observations reveal that a lower number of COMs and COM precursors are detected in L1517B with respect to L1498 and L1544, and also show lower abundances. Besides methanol, we only detected CH3O, H2CCO, CH3CHO, CH3CN, CH3NC, HCCCN, and HCCNC. Their measured abundances are ∼3 times larger towards the methanol peak than towards the core's centre, mimicking the behaviour found towards the more evolved cores L1544 and L1498. We propose that the differences in the chemical complexity observed between the three studied starless cores are a consequence of their evolution, with L1517B being the less evolved one, followed by L1498 and L1544. Chemical complexity in these cores seems to increase over time, with N-bearing molecules forming first and O-bearing COMs forming at a later stage as a result of the catastrophic depletion of CO. [ABSTRACT FROM AUTHOR]

Published
2023
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3. Negative and positive feedback from a supernova remnant with SHREC: a detailed study of the shocked gas in IC443

Author

Cosentino, G, primary, Jiménez-Serra, I, additional, Tan, J C, additional, Henshaw, J D, additional, Barnes, A T, additional, Law, C-Y, additional, Zeng, S, additional, Fontani, F, additional, Caselli, P, additional, Viti, S, additional, Zahorecz, S, additional, Rico-Villas, F, additional, Megías, A, additional, Miceli, M, additional, Orlando, S, additional, Ustamujic, S, additional, Greco, E, additional, Peres, G, additional, Bocchino, F, additional, Fedriani, R, additional, Gorai, P, additional, Testi, L, additional, and Martín-Pintado, J, additional

Published
2022
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5. ALMA–IRDC: dense gas mass distribution from cloud to core scales

Author

Barnes, A T, primary, Henshaw, J D, additional, Fontani, F, additional, Pineda, J E, additional, Cosentino, G, additional, Tan, J C, additional, Caselli, P, additional, Jiménez-Serra, I, additional, Law, C Y, additional, Avison, A, additional, Bigiel, F, additional, Feng, S, additional, Kong, S, additional, Longmore, S N, additional, Moser, L, additional, Parker, R J, additional, Sánchez-Monge, Á, additional, and Wang, K, additional

Published
2021
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7. ALMA–IRDC – II. First high-angular resolution measurements of the 14N/15N ratio in a large sample of infrared-dark cloud cores.

Author

Fontani, F, Barnes, A T, Caselli, P, Henshaw, J D, Cosentino, G, Jiménez-Serra, I, Tan, J C, Pineda, J E, and Law, C Y

Subjects
CLOUD computing, ISOTOPOLOGUES, STAR formation, MEASUREMENT
Abstract

The 14N/15N ratio in molecules exhibits a large variation in star-forming regions, especially when measured from N2H+ isotopologues. However, there are only a few studies performed at high-angular resolution. We present the first interferometric survey of the 14N/15N ratio in N2H+ obtained with Atacama Large Millimeter Array observations towards four infrared-dark clouds harbouring 3 mm continuum cores associated with different physical properties. We detect N15NH+ (1–0) in |$\sim 20\!-\!40{{\ \rm per\ cent}}$| of the cores, depending on the host cloud. The 14N/15N values measured towards the millimetre continuum cores range from a minimum of ∼80 up to a maximum of ∼400. The spread of values is narrower than that found in any previous single-dish survey of high-mass star-forming regions and than that obtained using the total power data only. This suggests that the 14N/15N ratio is on average higher in the diffuse gaseous envelope of the cores and stresses the need for high-angular resolution maps to measure correctly the 14N/15N ratio in dense cores embedded in IRDCs. The average 14N/15N ratio of ∼210 is also lower than the interstellar value at the Galactocentric distance of the clouds (∼300–330), although the sensitivity of our observations does not allow us to unveil 14N/15N ratios higher than ∼400. No clear trend is found between the 14N/15N ratio and the core physical properties. We find only a tentative positive trend between 14N/15N and H2 column density. However, firmer conclusions can be drawn only with higher sensitivity measurements. [ABSTRACT FROM AUTHOR]

Published
2021
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8. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution – survey description and compact source catalogue

Author

Eden, D J, primary, Liu, Tie, additional, Kim, Kee-Tae, additional, Juvela, M, additional, Liu, S-Y, additional, Tatematsu, K, additional, Francesco, J. Di, additional, Wang, K, additional, Wu, Y, additional, Thompson, M A, additional, Fuller, G A, additional, Li, Di, additional, Ristorcelli, I, additional, Kang, Sung-ju, additional, Hirano, N, additional, Johnstone, D, additional, Lin, Y, additional, He, J H, additional, Koch, P M, additional, Sanhueza, Patricio, additional, Qin, S-L, additional, Zhang, Q, additional, Goldsmith, P F, additional, Evans, N J, additional, Yuan, J, additional, Zhang, C-P, additional, White, G J, additional, Choi, Minho, additional, Lee, Chang Won, additional, Toth, L V, additional, Mairs, S, additional, Yi, H-W, additional, Tang, M, additional, Soam, A, additional, Peretto, N, additional, Samal, M R, additional, Fich, M, additional, Parsons, H, additional, Malinen, J, additional, Bendo, G J, additional, Rivera-Ingraham, A, additional, Liu, H-L, additional, Wouterloot, J, additional, Li, P S, additional, Qian, L, additional, Rawlings, J, additional, Rawlings, M G, additional, Feng, S, additional, Wang, B, additional, Li, Dalei, additional, Liu, M, additional, Luo, G, additional, Marston, A P, additional, Pattle, K M, additional, Pelkonen, V-M, additional, Rigby, A J, additional, Zahorecz, S, additional, Zhang, G, additional, Bőgner, R, additional, Aikawa, Y, additional, Akhter, S, additional, Alina, D, additional, Bell, G, additional, Bernard, J-P, additional, Blain, A, additional, Bronfman, L, additional, Byun, D-Y, additional, Chapman, S, additional, Chen, H-R, additional, Chen, M, additional, Chen, W-P, additional, Chen, X, additional, Chen, Xuepeng, additional, Chrysostomou, A, additional, Chu, Y-H, additional, Chung, E J, additional, Cornu, D, additional, Cosentino, G, additional, Cunningham, M R, additional, Demyk, K, additional, Drabek-Maunder, E, additional, Doi, Y, additional, Eswaraiah, C, additional, Falgarone, E, additional, Fehér, O, additional, Fraser, H, additional, Friberg, P, additional, Garay, G, additional, Ge, J X, additional, Gear, W K, additional, Greaves, J, additional, Guan, X, additional, Harvey-Smith, L, additional, Hasegawa, T, additional, He, Y, additional, Henkel, C, additional, Hirota, T, additional, Holland, W, additional, Hughes, A, additional, Jarken, E, additional, Ji, T-G, additional, Jimenez-Serra, I, additional, Kang, M, additional, Kawabata, K S, additional, Kim, Gwanjeong, additional, Kim, Jungha, additional, Kim, Jongsoo, additional, Kim, S, additional, Koo, B-C, additional, Kwon, Woojin, additional, Kuan, Y-J, additional, Lacaille, K M, additional, Lai, S-P, additional, Lee, C F, additional, Lee, J-E, additional, Lee, Y-U, additional, Li, H, additional, Lo, N, additional, Lopez, J A P, additional, Lu, X, additional, Lyo, A-R, additional, Mardones, D, additional, McGehee, P, additional, Meng, F, additional, Montier, L, additional, Montillaud, J, additional, Moore, T J T, additional, Morata, O, additional, Moriarty-Schieven, G H, additional, Ohashi, S, additional, Pak, S, additional, Park, Geumsook, additional, Paladini, R, additional, Pech, G, additional, Qiu, K, additional, Ren, Z-Y, additional, Richer, J, additional, Sakai, T, additional, Shang, H, additional, Shinnaga, H, additional, Stamatellos, D, additional, Tang, Y-W, additional, Traficante, A, additional, Vastel, C, additional, Viti, S, additional, Walsh, A, additional, Wang, H, additional, Wang, J, additional, Ward-Thompson, D, additional, Whitworth, A, additional, Wilson, C D, additional, Xu, Y, additional, Yang, J, additional, Yuan, Y-L, additional, Yuan, L, additional, Zavagno, A, additional, Zhang, C, additional, Zhang, H-W, additional, Zhou, C, additional, Zhou, J, additional, Zhu, L, additional, and Zuo, P, additional

Published
2019
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11. Widespread SiO and CH3OH emission in filamentary infrared dark clouds.

Author

Cosentino, G., Jiménez-Serra, I., Henshaw, J. D., Caselli, P., Viti, S., Barnes, A. T., Fontani, F., Tan, J. C., and Pon, A.

Subjects
*HIGH mass stars, *STAR formation, *STAR clusters, *DARK matter, *SILICON oxide, *CRYSTAL whiskers, *METHANOL
Abstract

Infrared dark clouds (IRDCs) are cold, dense regions of high (optical and infrared) extinction, believed to be the birthplace of high-mass stars and stellar clusters. The physical mechanisms leading to the formation of these IRDCs are not completely understood and it is thus important to study their molecular gas kinematics and chemical content to search for any signature of the IRDCs formation process. Using the 30-m-diameter antenna at the Instituto de Radioastronomía Milimétrica (IRAM), we have obtained emission maps of dense gas tracers (H13CO+ and HN13C) and typical shock tracers (SiO and CH3OH) towards three IRDCs, G028.37+00.07, G034.43+00.24, and G034.77-00.55 (clouds C, F, and G, respectively).We have studied the molecular gas kinematics in these clouds and, consistent with previous works towards other IRDCs, the clouds show complex gas kinematics with several velocity-coherent substructures separated in velocity space by a few km s-1. Correlated with these complex kinematic structures, widespread (parsec-scale) emission of SiO and CH3OH is present in all the three clouds. For clouds C and F, known to be actively forming stars, widespread SiO and CH3OH is likely associated with on-going star formation activity. However, for cloud G, which lacks either 8 or 24 μm sources and 4.5 μm H2 shock-excited emission, the detected widespread SiO and CH3OH emission may have originated in a large-scale shock interaction, although a scenario involving a population of low-mass stars driving molecular outflows cannot be fully ruled out. [ABSTRACT FROM AUTHOR]

Published
2018
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