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95 results on '"SERRA I."'

1. Disruption of a massive molecular cloud by a supernova in the Galactic Centre: Initial results from the ACES project.

Author

Nonhebel, M., Barnes, A. T., Immer, K., Armijos-Abendaño, J., Bally, J., Battersby, C., Burton, M. G., Butterfield, N., Colzi, L., García, P., Ginsburg, A., Henshaw, J. D., Hu, Y., Jiménez-Serra, I., Klessen, R. S., Kruijssen, J. M. D., Liang, F.-H., Longmore, S. N., Lu, X., and Martín, S.

Subjects
SUPERNOVA remnants, INTERSTELLAR medium, MILKY Way, AUTOMATIC test equipment, KINETIC energy
Abstract

The Milky Way's Central Molecular Zone (CMZ) differs dramatically from our local solar neighbourhood, both in the extreme interstellar medium conditions it exhibits (e.g. high gas, stellar, and feedback density) and in the strong dynamics at play (e.g. due to shear and gas influx along the bar). Consequently, it is likely that there are large-scale physical structures within the CMZ that cannot form elsewhere in the Milky Way. In this paper, we present new results from the Atacama Large Millimeter/submillimeter Array (ALMA) large programme ACES (ALMA CMZ Exploration Survey) and conduct a multi-wavelength and kinematic analysis to determine the origin of the M0.8–0.2 ring, a molecular cloud with a distinct ring-like morphology. We estimate the projected inner and outer radii of the M0.8–0.2 ring to be 79″ and 154″, respectively (3.1 pc and 6.1 pc at an assumed Galactic Centre distance of 8.2 kpc) and calculate a mean gas density >104 cm−3, a mass of ~106 M⊙, and an expansion speed of ~20 km s−1, resulting in a high estimated kinetic energy (>1051 erg) and momentum (>107 M⊙ km s−1). We discuss several possible causes for the existence and expansion of the structure, including stellar feedback and large-scale dynamics. We propose that the most likely cause of the M0.8–0.2 ring is a single high-energy hypernova explosion. To viably explain the observed morphology and kinematics, such an explosion would need to have taken place inside a dense, very massive molecular cloud, the remnants of which we now see as the M0.8–0.2 ring. In this case, the structure provides an extreme example of how supernovae can affect molecular clouds. [ABSTRACT FROM AUTHOR]

Published
2024
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3. FAUST

Author

Sabatini, G., primary, Podio, L., additional, Codella, C., additional, Watanabe, Y., additional, De Simone, M., additional, Bianchi, E., additional, Ceccarelli, C., additional, Chandler, C. J., additional, Sakai, N., additional, Svoboda, B., additional, Testi, L., additional, Aikawa, Y., additional, Balucani, N., additional, Bouvier, M., additional, Caselli, P., additional, Caux, E., additional, Chahine, L., additional, Charnley, S., additional, Cuello, N., additional, Dulieu, F., additional, Evans, L., additional, Fedele, D., additional, Feng, S., additional, Fontani, F., additional, Hama, T., additional, Hanawa, T., additional, Herbst, E., additional, Hirota, T., additional, Isella, A., additional, Jímenez-Serra, I., additional, Johnstone, D., additional, Lefloch, B., additional, Le Gal, R., additional, Loinard, L., additional, Liu, H. B., additional, López-Sepulcre, A., additional, Maud, L. T., additional, Maureira, M. J., additional, Menard, F., additional, Miotello, A., additional, Moellenbrock, G., additional, Nomura, H., additional, Oba, Y., additional, Ohashi, S., additional, Okoda, Y., additional, Oya, Y., additional, Pineda, J., additional, Rimola, A., additional, Sakai, T., additional, Segura-Cox, D., additional, Shirley, Y., additional, Vastel, C., additional, Viti, S., additional, Watanabe, N., additional, Zhang, Y., additional, Zhang, Z. E., additional, and Yamamoto, S., additional

Published
2024
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4. Excitation and spatial study of a prestellar cluster towards G+0.693-0.027 in the Galactic centre.

Author

Colzi, L., Martín-Pintado, J., Zeng, S., Jiménez-Serra, I., Rivilla, V. M., Sanz-Novo, M., Martín, S., Zhang, Q., and Lu, X.

Subjects
LOCAL thermodynamic equilibrium, MOLECULAR structure, RADIO lines, CONDENSATION (Meteorology), ASTROCHEMISTRY
Abstract

Context. Star formation in the central molecular zone (CMZ) is suppressed with respect to that of the Galactic disk, and this is likely related to its high turbulent environment. This turbulence impedes the potential detection of prestellar cores. Aims. We present the temperature, density, and spatial structure of the CMZ molecular cloud G+0.693-0.027, which has been proposed to host a prestellar cluster in the Sgr B2 region. Methods. We analysed multiple HC3N rotational transitions that were observed with the IRAM 30m, APEX, Yebes 40m, and GBT radio telescopes, together with SMA+APEX spatially resolved maps. Results. The spectral shape of HC3N lines shows three distinct velocity components: a broad component with a line width of 23 km s−1 (C1), and two narrow components with line widths of 7.2 and 8.8 km s−1 (C2 and C3). This suggests that a fraction of the molecular gas in this cloud is undergoing turbulence dissipation. From an initial local thermodynamic equilibrium analysis, we found column densities of N = (6.54 ± 0.07) × 1014 cm−2, (9 ± 3) × 1014 cm−2, and (3.6 ± 0.7) × 1013 cm−2 for C1, C2, and C3, respectively. These values were used as input for a subsequent non-local thermodynamic equilibrium analysis, in which we found H2 densities of 2 × 104 cm−3, 5 × 104 cm−3, and 4 × 105 cm−3 and kinetic temperatures of 140 K, 30 K, and 80 K for C1, C2, and C3, respectively. The spatially resolved maps confirm that the colder and high-density condensations C2 and C3, which peak in the 70–85 km s−1 velocity range, have deconvolved sizes of 9″ (0.36 pc) and 7.6″ (0.3 pc), respectively, and are embedded in a more diffuse and warmer gas (C1). Conclusions. The larger-scale structure of the Sgr B2 region, consistently with previous works, shows a hole at 40–50 km s−1 that is likely due to a small cloud that shocked the Sgr B2 region and is spatially related with a massive cloud at 60–80 km s−1. We propose that the impacting small cloud sequentially triggered the formation of Sgr B2(M), (N), and (S) and the condensations in G+0.693-0.027 during its passage. The two condensations are in a post-shocked environment that has undergone internal fragmentation. Based on the analysis of their masses and the virial parameters, C2 might expand, while C3 might further fragment or collapse. [ABSTRACT FROM AUTHOR]

Published
2024
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5. FAUST. XI. Enhancement of the complex organic material in the shocked matter surrounding the [BHB2007] 11 protobinary system

Author

Vastel, C., primary, Sakai, T., additional, Ceccarelli, C., additional, Jimenez-Serra, I., additional, Alves, F., additional, Balucani, N., additional, Bianchi, E., additional, Bouvier, M., additional, Caselli, P., additional, Chandler, C.J., additional, Charnley, S., additional, Codella, C., additional, De Simone, M., additional, Dulieu, F., additional, Evans, L., additional, Fontani, F., additional, Lefloch, B., additional, Loinard, L., additional, Menard, F., additional, Podio, L., additional, Sabatini, G., additional, Sakai, N., additional, and Yamamoto, S., additional

Published
2024
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6. The abundance and excitation of molecular anions in interstellar clouds

Author

Ministerio de Ciencia e Innovación (España), Agúndez, Marcelino [0000-0003-3248-3564], Marcelino, Nuria [0000-0001-7236-4047], Tercero, Belén [0000-0002-4782-5259], Jimenez-Serra, I. [0000-0003-4493-8714], Cernicharo, José [0000-0002-3518-2524], Agúndez, Marcelino, Marcelino, Nuria, Tercero, Belén, Jimenez-Serra, I., Cernicharo, José, Ministerio de Ciencia e Innovación (España), Agúndez, Marcelino [0000-0003-3248-3564], Marcelino, Nuria [0000-0001-7236-4047], Tercero, Belén [0000-0002-4782-5259], Jimenez-Serra, I. [0000-0003-4493-8714], Cernicharo, José [0000-0002-3518-2524], Agúndez, Marcelino, Marcelino, Nuria, Tercero, Belén, Jimenez-Serra, I., and Cernicharo, José

Abstract

We report new observations of molecular anions with the Yebes 40m and IRAM 30m telescopes toward the cold dense clouds TMC-1 CP, Lupus-1A, L1527, L483, L1495B, and L1544. We detected for the first time C3N- and C5N- in Lupus-1A and C4H- and C6H- in L483. In addition, we report new lines of C6H- toward the six targeted sources, of C4H- toward TMC-1 CP, Lupus-1A, and L1527, and of C8H- and C3N- in TMC-1 CP. Excitation calculations indicate that the lines of anions accessible to radiotelescopes run from subthermally excited to thermalized as the size of the anion increases, with the degree of departure from thermalization depending on the H2 volume density and the line frequency. We noticed that the collision rate coefficients available for the radical C6H cannot explain various observational facts, which advises for a revisitation of the collision data for this species. The observations presented here, together with observational data from the literature, are used to model the excitation of interstellar anions and to constrain their abundances. In general, the anion-to-neutral ratios derived here agree within 50 % (a factor of two at most) with literature values, when available, except for the C4H-/C4H ratio, which shows higher differences due to a revision of the dipole moment of C4H. From the set of anion-to-neutral abundance ratios derived two conclusions can be drawn. First, the C6H-/C6H ratio shows a tentative trend in which it increases with increasing H2 density, as expected from theoretical grounds. And second, it is incontestable that the higher the molecular size the higher the anion-to-neutral ratio, which supports a formation mechanism based on radiative electron attachment. Nonetheless, calculated rate coefficients for electron attachment to the medium size species C4H and C3N are probably too high and too low, respectively, by more than one order of magnitude.

Published
2023

7. Gas phase Elemental abundances in Molecular cloudS (GEMS). IX. Deuterated compounds of H2S in starless cores.

Author

Rodríguez-Baras, M., primary, Esplugues, G., additional, Fuente, A., additional, Spezzano, S., additional, Caselli, P., additional, Loison, J.C., additional, Roueff, E., additional, Navarro-Almaida, D., additional, Bachiller, R., additional, Martín-Doménech, R., additional, Jiménez-Serra, I., additional, Beitia-Antero, L., additional, and Le Gal, R., additional

Published
2023
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8. FAUST. X. Formaldehyde in the protobinary system [BHB2007] 11: Small-scale deuteration

Author

Evans, L., primary, Vastel, C., additional, Fontani, F., additional, Pineda, J. E., additional, Jiménez-Serra, I., additional, Alves, F., additional, Sakai, T., additional, Bouvier, M., additional, Caselli, P., additional, Ceccarelli, C., additional, Chandler, C., additional, Svoboda, B., additional, Maud, L., additional, Codella, C., additional, Sakai, N., additional, Le Gal, R., additional, López-Sepulcre, A., additional, Moellenbrock, G., additional, and Yamamoto, S., additional

Published
2023
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9. The first detection of SiC2 in the interstellar medium

Author

Massalkhi, S., primary, Jiménez-Serra, I., additional, Martín-Pintado, J., additional, Rivilla, V. M., additional, Colzi, L., additional, Zeng, S., additional, Martín, S., additional, Tercero, B., additional, de Vicente, P., additional, and Requena-Torres, M. A., additional

Published
2023
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13. The GUAPOS project: G31.41+0.31 Unbiased ALMA sPectral Observational Survey: IV. Phosphorus-bearing molecules and their relation to shock tracers.

Author

Fontani, F., Mininni, C., Beltrán, M. T., Rivilla, V. M., Colzi, L., Jiménez-Serra, I., López-Gallifa, Á., Sánchez-Monge, Á., and Viti, S.

Subjects
MOLECULES, SPECTRAL lines, ASTROCHEMISTRY, STAR formation
Abstract

Context. The astrochemistry of the important biogenic element phosphorus (P) is still poorly understood, but observational evidence indicates that P-bearing molecules are likely associated with shocks. Aims. We study P-bearing molecules and some shock tracers towards one of the chemically richest hot molecular cores, G31.41+0.31, in the framework of the project "G31.41+0.31 Unbiased ALMA sPectral Observational Survey" (GUAPOS), which is being carried out with the Atacama Large Millimeter Array (ALMA). Methods. We observed the molecules PN, PO, SO, SO2, SiO, and SiS through their rotational lines in the spectral range 84.05– 115.91 GHz covered by the GUAPOS project. Results. PN is clearly detected, while PO is tentatively detected. The PN emission arises from two regions southwest of the hot core peak, named regions 1 and 2 here, and is undetected or tentatively detected towards the hot core peak. The PN and SiO lines are very similar both in spatial emission morphology and spectral shape. Region 1 is partly overlapping with the hot core and is warmer than region 2, which is well separated from the hot core and located along the outflows identified in previous studies. The SO, SO2, and SiS emissions are also detected towards the PN-emitting regions 1 and 2, but arise mostly from the hot core. Moreover, the column density ratio SiO/PN remains constant in regions 1 and 2, while SO/PN, SiS/PN, and SO2/PN decrease by about an order of magnitude from region 1 to region 2, indicating that SiO and PN have a common origin even in regions with different physical conditions. The PO/PN ratio in region 2, where PO is tentatively detected, is ~0.6–0.9, which is in line with the predictions of pure shock models. Conclusions. Our study provides robust confirmation of previous observational evidence that PN emission is tightly associated with SiO and is likely a product of shock chemistry, as the lack of a clear detection of PN towards the hot core allows us to rule out relevant formation pathways in hot gas. We propose the PN-emitting region 2 as a new astrophysical laboratory for shock-chemistry studies. [ABSTRACT FROM AUTHOR]

Published
2024
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14. Mother of dragons

Author

Barnes, A. T., primary, Liu, J., additional, Zhang, Q., additional, Tan, J. C., additional, Bigiel, F., additional, Caselli, P., additional, Cosentino, G., additional, Fontani, F., additional, Henshaw, J. D., additional, Jiménez-Serra, I., additional, Kalb, D.-S., additional, Law, C. Y., additional, Longmore, S. N., additional, Parker, R. J., additional, Pineda, J. E., additional, Sánchez-Monge, A., additional, Lim, W., additional, and Wang, K., additional

Published
2023
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15. Gas phase Elemental abundances in Molecular cloudS (GEMS) VII. Sulfur elemental abundance

Author

Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Universidad Complutense de Madrid, Fundación Ramón Areces, Ministerio de Universidades (España), Fuente, A. [0000-0001-6317-6343], Rivière-Marichalar, P. [0000-0003-0969-8137], Navarro-Almaida, D. [0000-0002-8499-7447], Kramer; C. [0000-0002-4908-4925], Bachiller, R. [0000-0002-5331-5386], Goicoechea, Javier R. [0000-0001-7046-4319], Jiménez-Serra, I. [0000-0003-4493-8714], Martín-Doménech, R. [0000-0001-6496-9791], Spezzano, S. [0000-0002-6787-5245], Muñoz-Caro, G. [0000-0001-7003-7368], Fuente, A., Rivière-Marichalar, P., Beitia-Antero, L., Caselli, P., Wakelam, V., Esplugues, G., Rodríguez-Baras, M., Navarro-Almaida, D., Gerin, M., Kramer; C., Bachiller, R., Goicoechea, Javier R., Jiménez-Serra, Izaskun, Loison, J. C., Ivlev, A., Martín-Doménech, R., Spezzano, S., Roncero, Octavio, Muñoz-Caro, G., Cazaux, S., Marcelino, Nuria, Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Universidad Complutense de Madrid, Fundación Ramón Areces, Ministerio de Universidades (España), Fuente, A. [0000-0001-6317-6343], Rivière-Marichalar, P. [0000-0003-0969-8137], Navarro-Almaida, D. [0000-0002-8499-7447], Kramer; C. [0000-0002-4908-4925], Bachiller, R. [0000-0002-5331-5386], Goicoechea, Javier R. [0000-0001-7046-4319], Jiménez-Serra, I. [0000-0003-4493-8714], Martín-Doménech, R. [0000-0001-6496-9791], Spezzano, S. [0000-0002-6787-5245], Muñoz-Caro, G. [0000-0001-7003-7368], Fuente, A., Rivière-Marichalar, P., Beitia-Antero, L., Caselli, P., Wakelam, V., Esplugues, G., Rodríguez-Baras, M., Navarro-Almaida, D., Gerin, M., Kramer; C., Bachiller, R., Goicoechea, Javier R., Jiménez-Serra, Izaskun, Loison, J. C., Ivlev, A., Martín-Doménech, R., Spezzano, S., Roncero, Octavio, Muñoz-Caro, G., Cazaux, S., and Marcelino, Nuria

Abstract

Gas phase Elemental abundances in molecular CloudS (GEMS) is an IRAM 30m large program aimed at determining the elemental abundances of carbon (C), oxygen (O), nitrogen (N), and sulfur (S) in a selected set of prototypical star-forming filaments. In particular, the elemental abundance of S remains uncertain by several orders of magnitude and its determination is one of the most challenging goals of this program. We have carried out an extensive chemical modeling of the fractional abundances of CO, HCO$^+$, HCN, HNC, CS, SO, H$_2$S, OCS, and HCS$^+$ to determine the sulfur depletion toward the 244 positions in the GEMS database. These positions sample visual extinctions from A$_V$ $\sim$ 3 mag to $>$50 mag, molecular hydrogen densities ranging from a few 10$^3$~cm$^{-3}$ to 3$\times$10$^6$~cm$^{-3}$, and T$_k$ $\sim$ 10$-$35 K. Most of the positions in Taurus and Perseus are best fitted assuming early-time chemistry, t=0.1 Myr, $\zeta_{H_2}$$\sim$ (0.5$-$1)$\times$10$^{-16}$ s$^{-1}$, and [S/H]$\sim$1.5$\times$10$^{-6}$. On the contrary, most of the positions in Orion are fitted with t=1~Myr and $\zeta_{H_2}$$\sim$ 10$^{-17}$ s$^{-1}$. Moreover, $\sim$40% of the positions in Orion are best fitted assuming the undepleted sulfur abundance, [S/H]$\sim$1.5$\times$10$^{-5}$. Our results suggest that sulfur depletion depends on the environment. While the abundances of sulfur-bearing species are consistent with undepleted sulfur in Orion, a depletion factor of $\sim$20 is required to explain those observed in Taurus and Perseus. We propose that differences in the grain charge distribution in the envelopes of the studied clouds might explain these variations. The shocks associated with past and ongoing star formation could also contribute to enhance [S/H] in Orion.

Published
2023

16. Deuterium fractionation across the infrared-dark cloud G034.77-00.55 interacting with the supernova remnant W44

Author

Swedish Research Council, European Research Council, Ministerio de Ciencia e Innovación (España), Royal Society (UK), Cosentino, G., Tan, J. C., Jiménez-Serra, I., Fontani, F., Caselli, P., Henshaw, J. D., Barnes, A. T., Law, C. -Y., Viti, S., Fedriani, R., Hsu, C. -J., Gorai, P., Zeng, S., Swedish Research Council, European Research Council, Ministerio de Ciencia e Innovación (España), Royal Society (UK), Cosentino, G., Tan, J. C., Jiménez-Serra, I., Fontani, F., Caselli, P., Henshaw, J. D., Barnes, A. T., Law, C. -Y., Viti, S., Fedriani, R., Hsu, C. -J., Gorai, P., and Zeng, S.

Abstract

Supernova remnants (SNRs) may regulate star formation in galaxies. For example, SNR-driven shocks may form new molecular gas or compress pre-existing clouds and trigger the formation of new stars. Aims. To test this scenario, we measured the deuteration of N2H+, DNfrac 2H+- a well-studied tracer of pre-stellar cores - across the infrared-dark cloud (IRDC) G034.77-00.55, which is known to be experiencing a shock interaction with the SNR W44. Methods. We use N2H+ and N2D+ J = 1-0 single pointing observations obtained with the 30m antenna at the Instituto de Radioastronomia Millimetrica to infer DN2H+ frac towards five positions across the cloud, namely a massive core, different regions across the shock front, a dense clump, and ambient gas. Results. We find DN2H+ frac in the range 0.03-0.1, which is several orders of magnitude larger than the cosmic D/H ratio (∼10-5). The DN2H+ frac across the shock front is enhanced by more than a factor of 2 (DNfrac 2H+∼ 0.05-0.07) with respect to the ambient gas (=0.03) and similar to that measured generally in pre-stellar cores. Indeed, in the massive core and dense clump regions of this IRDC we measure DN2H+ frac ∼ 0.1. © The Authors 2023

Published
2023

18. Laboratory spectroscopy of allylimine and tentative detection towards the G+0.693-0.027 molecular cloud

Author

Alberton, D., primary, Bizzocchi, L., additional, Jiang, N., additional, Melosso, M., additional, Rivilla, V. M., additional, Charmet, A. Pietropolli, additional, Giuliano, B. M., additional, Caselli, P., additional, Puzzarini, C., additional, Alessandrini, S., additional, Dore, L., additional, Jiménez-Serra, I., additional, and Martín-Pintado, J., additional

Published
2023
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19. Gas phase Elemental abundances in Molecular cloudS (GEMS). VII. Sulfur elemental abundance

Author

Fuente, A., primary, Riviere-Marichalar, P., additional, Beitia-Antero, L., additional, Caselli, P., additional, Wakelam, V., additional, Esplugues, G., additional, Rodriguez-Baras, M., additional, Navarro-Almaida, D., additional, Gerin, M., additional, Kramer, C., additional, Bachiller, R., additional, Goicoechea, J.R., additional, Jimenez-Serra, I., additional, Loison, J. C., additional, Ivlev, A., additional, Martin-Domenech, R., additional, and al, et, additional

Published
2022
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20. PRODIGE – envelope to disk with NOEMA

Author

Valdivia-Mena, M. T., primary, Pineda, J. E., additional, Segura-Cox, D. M., additional, Caselli, P., additional, Neri, R., additional, López-Sepulcre, A., additional, Cunningham, N., additional, Bouscasse, L., additional, Semenov, D., additional, Henning, Th., additional, Piétu, V., additional, Chapillon, E., additional, Dutrey, A., additional, Fuente, A., additional, Guilloteau, S., additional, Hsieh, T. H., additional, Jiménez-Serra, I., additional, Marino, S., additional, Maureira, M. J., additional, Smirnov-Pinchukov, G. V., additional, Tafalla, M., additional, and Zhao, B., additional

Published
2022
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21. Toward the limits of complexity of interstellar chemistry: Rotational spectroscopy and astronomical search for n- and i-butanal

Author

Sanz-Novo, M., primary, Belloche, A., additional, Rivilla, V. M., additional, Garrod, R. T., additional, Alonso, J. L., additional, Redondo, P., additional, Barrientos, C., additional, Kolesniková, L., additional, Valle, J. C., additional, Rodríguez-Almeida, L., additional, Jimenez-Serra, I., additional, Martín-Pintado, J., additional, Müller, H. S. P., additional, and Menten, K. M., additional

Published
2022
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23. FAUST

Author

Vastel, C., primary, Alves, F., additional, Ceccarelli, C., additional, Bouvier, M., additional, Jiménez-Serra, I., additional, Sakai, T., additional, Caselli, P., additional, Evans, L., additional, Fontani, F., additional, Le Gal, R., additional, Chandler, C. J., additional, Svoboda, B., additional, Maud, L., additional, Codella, C., additional, Sakai, N., additional, Lόpez-Sepulcre, A., additional, Moellenbrock, G., additional, Aikawa, Y., additional, Balucani, N., additional, Bianchi, E., additional, Busquet, G., additional, Caux, E., additional, Charnley, S., additional, Cuello, N., additional, De Simone, M., additional, Dulieu, F., additional, Durân, A., additional, Fedele, D., additional, Feng, S., additional, Francis, L., additional, Hama, T., additional, Hanawa, T., additional, Herbst, E., additional, Hirota, T., additional, Imai, M., additional, Isella, A., additional, Johnstone, D., additional, Lefloch, B., additional, Loinard, L., additional, Maureira, M., additional, Murillo, N. M., additional, Mercimek, S., additional, Mori, S., additional, Menard, F., additional, Miotello, A., additional, Nakatani, R., additional, Nomura, H., additional, Oba, Y., additional, Ohashi, S., additional, Okoda, Y., additional, Ospina-Zamudio, J., additional, Oya, Y., additional, Pineda, J. E., additional, Podio, L., additional, Rimola, A., additional, Cox, D. Segura, additional, Shirley, Y., additional, Testi, L., additional, Viti, S., additional, Watanabe, N., additional, Watanabe, Y., additional, Witzel, A., additional, Xue, C., additional, Zhang, Y., additional, Zhao, B., additional, and Yamamoto, S., additional

Published
2022
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25. SOLIS

Author

de A. Schutzer, A., primary, Rivera-Ortiz, P. R., additional, Lefloch, B., additional, Gusdorf, A., additional, Favre, C., additional, Segura-Cox, D., additional, López-Sepulcre, A., additional, Neri, R., additional, Ospina-Zamudio, J., additional, De Simone, M., additional, Codella, C., additional, Viti, S., additional, Podio, L., additional, Pineda, J., additional, O’Donoghue, R., additional, Ceccarelli, C., additional, Caselli, P., additional, Alves, F., additional, Bachiller, R., additional, Balucani, N., additional, Bianchi, E., additional, Bizzocchi, L., additional, Bottinelli, S., additional, Caux, E., additional, Chacón-Tanarro, A., additional, Dulieu, F., additional, Enrique-Romero, J., additional, Fontani, F., additional, Feng, S., additional, Holdship, J., additional, Jiménez-Serra, I., additional, Jaber Al-Edhari, A., additional, Kahane, C., additional, Lattanzi, V., additional, Oya, Y., additional, Punanova, A., additional, Rimola, A., additional, Sakai, N., additional, Spezzano, S., additional, Sims, I. R., additional, Taquet, V., additional, Testi, L., additional, Theulé, P., additional, Ugliengo, P., additional, Vastel, C., additional, Vasyunin, A. I., additional, Vazart, F., additional, Yamamoto, S., additional, and Witzel, A., additional

Published
2022
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26. Astrochemical modelling of infrared dark clouds

Author

Entekhabi, N., primary, Tan, J. C., additional, Cosentino, G., additional, Hsu, C-J., additional, Caselli, P., additional, Walsh, C., additional, Lim, W., additional, Henshaw, J. D., additional, Barnes, A. T., additional, Fontani, F., additional, and Jiménez-Serra, I., additional

Published
2022
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28. First detection of C2H5NCO in the ISM and search of other isocyanates towards the G+0.693-0.027 molecular cloud

Author

Rodríguez-Almeida, L. F., primary, Rivilla, V. M., additional, Jiménez-Serra, I., additional, Melosso, M., additional, Colzi, L., additional, Zeng, S., additional, Tercero, B., additional, de Vicente, P., additional, Martín, S., additional, Requena-Torres, M. A., additional, Rico-Villas, F., additional, and Martín-Pintado, J., additional

Published
2021
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30. The GUAPOS project

Author

Colzi, L., primary, Rivilla, V. M., additional, Beltrán, M. T., additional, Jiménez-Serra, I., additional, Mininni, C., additional, Melosso, M., additional, Cesaroni, R., additional, Fontani, F., additional, Lorenzani, A., additional, Sánchez-Monge, A., additional, Viti, S., additional, Schilke, P., additional, Testi, L., additional, Alonso, E. R., additional, and Kolesniková, L., additional

Published
2021
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31. Evolutionary view through the starless cores in Taurus

Author

Navarro-Almaida, D., primary, Fuente, A., additional, Majumdar, L., additional, Wakelam, V., additional, Caselli, P., additional, Rivière-Marichalar, P., additional, Treviño-Morales, S. P., additional, Cazaux, S., additional, Jiménez-Serra, I., additional, Kramer, C., additional, Chacón-Tanarro, A., additional, Kirk, J. M., additional, Ward-Thompson, D., additional, and Tafalla, M., additional

Published
2021
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32. Water and methanol ice in L 1544

Author

Goto, M., primary, Vasyunin, A. I., additional, Giuliano, B. M., additional, Jiménez-Serra, I., additional, Caselli, P., additional, Román-Zúñiga, C. G., additional, and Alves, J., additional

Published
2021
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33. Water and Methanol Ice in L 1544

Author

Goto, M., Vasyunin, A. I., Giuliano, B. M., Jiménez-Serra, I., Caselli, P., Román-Zúñiga, C. G., and Alves, J.

Subjects
ISM [INFRARED], ASTROCHEMISTRY, DUST, EXTINCTION, CHEMICAL MODEL, HEAT SOURCES, COMPLEX ORGANIC MOLECULES, ICE, INDIVIDUAL OBJECTS: L 1544 [ISM], EVOLUTION, CHEMICAL DESORPTION, LOW TEMPERATURES, CLOUDS [ISM], MODEL PREDICTION, METHANOL, MODEL CALCULATIONS, COLD CLOUDS, STARS
Abstract

Context. Methanol and complex organic molecules have been found in cold starless cores, where a standard warm-up scenario would not work because of the absence of heat sources. A recent chemical model attributed the presence of methanol and large organics to the efficient chemical desorption and a class of neutral-neutral reactions that proceed fast at low temperatures in the gas phase. Aims. The model calls for a high abundance of methanol ice at the edge of the CO freeze-out zone in cold cloud cores. Methods. We performed medium-resolution spectroscopy toward three field stars behind the starless core L 1544 at 3 μm to constrain the methanol ice abundance and compare it with the model predictions. Results. One of the field stars shows a methanol ice abundance of 11% with respect to water ice. This is higher than the typical methanol abundance previously found in cold cloud cores (4%), but is 4.5 times lower than predicted. The reason for the disagreement between the observations and the model calculations is not yet understood. © ESO 2021. Acknlwo edgemen. M.G. thanks all the staff and crew of the IRTF, in particular, Mike Connelley, Brian Cabreira, Dave Griep, Miranda Hawarden-Ogata and Bobby Bus who kindly helped conducting the observation from Munich. We would like to thank the hospitality of the Hawaiian community that made the research presented here possible. My sincere appreciation goes to Jorma Harju and Viktor Zivkov who gave me thorough instructions how to construct dust emission / color temperature maps, and a color extinction map, respectively. We thank Wing-Fai Thi for the fruitful discussion about the influence of dust grain size on the shape of methanol ice absorption feature. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. The optical spectra of the ice was taken from Sackler Laboratory Ice Database. This research has made use of NASA’s Astrophysics Data System. This research has made use of the SIM-BAD database, operated at CDS, Strasbourg, France. M.G. is supported by the German Research Foundation (DFG) grant GO 1927/6-1. The work of A.I.V. is supported by the Russian Ministry of Science and Higher Education via the State Assignment project FEUZ-2020-0038. A.I.V. is a head of the Max Planck Partner Group at the Ural Federal University. I.J.-S. has received partial support from the Spanish FEDER (ESP2017-86582-C4-1-R) and the State Research Agency (AEI; PID2019-105552RB-C41). C.R.-Z. acknowledges support from program UNAM-DGAPA IN112620, Mexico. The authors thank the anonymous referee for the valuable suggestions that have significantly improved the manuscript.

Published
2021

34. Gas phase Elemental abundances in Molecular cloudS (GEMS)

Author

Rodríguez-Baras, M., primary, Fuente, A., additional, Riviére-Marichalar, P., additional, Navarro-Almaida, D., additional, Caselli, P., additional, Gerin, M., additional, Kramer, C., additional, Roueff, E., additional, Wakelam, V., additional, Esplugues, G., additional, García-Burillo, S., additional, Le Gal, R., additional, Spezzano, S., additional, Alonso-Albi, T., additional, Bachiller, R., additional, Cazaux, S., additional, Commercon, B., additional, Goicoechea, J. R., additional, Loison, J. C., additional, Treviño-Morales, S. P., additional, Roncero, O., additional, Jiménez-Serra, I., additional, Laas, J., additional, Hacar, A., additional, Kirk, J., additional, Lattanzi, V., additional, Martín-Doménech, R., additional, Muñoz-Caro, G., additional, Pineda, J. E., additional, Tercero, B., additional, Ward-Thompson, D., additional, Tafalla, M., additional, Marcelino, N., additional, Malinen, J., additional, Friesen, R., additional, and Giuliano, B. M., additional

Published
2021
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35. Seeds of Life in Space (SOLIS): VI. Chemical evolution of sulfuretted species along the outflows driven by the low-mass protostellar binary NGC 1333-IRAS4A

Author

Taquet, V., Codella, C., De Simone, M., López-Sepulcre, A., Pineda, J. E., Segura-Cox, D., Ceccarelli, C., Caselli, P., Gusdorf, A., Persson, M. V., Alves, F., Caux, E., Favre, C., Fontani, F., Neri, R., Oya, Y., Sakai, N., Vastel, C., Yamamoto, S., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Feng, S., Holdship, J., Lefloch, B., Jaber, Al-Edhari, A., Jiménez-Serra, I., Kahane, C., Lattanzi, V., Ospina-Zamudio, J., Podio, L., Punanova, A., Rimola, A., Sims, I. R., Spezzano, S., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., Witzel, A., Taquet, V., Codella, C., De Simone, M., López-Sepulcre, A., Pineda, J. E., Segura-Cox, D., Ceccarelli, C., Caselli, P., Gusdorf, A., Persson, M. V., Alves, F., Caux, E., Favre, C., Fontani, F., Neri, R., Oya, Y., Sakai, N., Vastel, C., Yamamoto, S., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Feng, S., Holdship, J., Lefloch, B., Jaber, Al-Edhari, A., Jiménez-Serra, I., Kahane, C., Lattanzi, V., Ospina-Zamudio, J., Podio, L., Punanova, A., Rimola, A., Sims, I. R., Spezzano, S., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., and Witzel, A.

Abstract

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 NGC 1333-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 SO2 towards NGC 1333-IRAS4A in the 1.3, 2, and 3 mm bands using the IRAM NOrthern Extended Millimeter Array 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 SO2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east-south west 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/SO2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 105 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 sputter

Published
2020

36. Seeds of Life in Space (SOLIS): VII. Discovery of a cold dense methanol blob toward the L1521F VeLLO system

Author

Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De, Simone, M., Enrique, Romero, J., Dulieu, F., Feng, S., Jaber, Al-Edhari, A., Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., Witzel, A., Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De, Simone, M., Enrique, Romero, J., Dulieu, F., Feng, S., Jaber, Al-Edhari, A., Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., and Witzel, A.

Abstract

Aims. The Seeds Of Life In Space IRAM/NOEMA large program aims at studying a set of crucial complex organic molecules in a sample of sources with a well-known physical structure that covers the various phases of solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the very low luminosity object (VeLLO) L1521F. This type of source is important to study to link prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Methods. Two frequency windows (81.6-82.6 GHz and 96.65-97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. These setups cover transitions of ketene (H2CCO), propyne (CH3CCH), formamide (NH2CHO), methoxy (CH3O), methanol (CH3OH), dimethyl ether (CH3OCH3), and methyl formate (HCOOCH3). Results. Only two transitions of methanol (A+, E2) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E1) in a very compact emission blob (∼7″ corresponding to ∼1000 au) toward the northeast of the L1521F protostar. The CS 2-1 transition is also detected within theWideX bandwidth. Consistently with what has been found in prestellar cores, the methanol emission appears ∼1000 au away from the dust peak. The location of the methanol blob coincides with one of the filaments that have previously been reported in the literature. The excitation temperature of the gas inferred from methanol is (10 ± 2) K, while the H2 gas density (estimated from the detected CS 2-1 emission and previous CS 5-4 ALMA observations) is a factor >25 higher than the density in the surrounding environment (n(H2) ≥ 107 cm-3). Conclusions. Based on its compactness, low excitation temperature, and high gas density, we suggest that the methanol emission detected with NOEMA is (i) either a cold and dense shock-induced blob that formed recently (≤ a few hundred years) by infal

Published
2020

37. Gas phase Elemental abundances in Molecular cloudS (GEMS) II. On the quest for the sulphur reservoir in molecular clouds: the H2S case

Author

Navarro-Almaida, D, Le Gal, R, Fuente, A, Rivière-Marichalar, P, Wakelam, V, Cazaux, S, Caselli, P, Laas, Jacob C, Alonso-Albi, T, Loison, J C, Gerin, M, Kramer, C, Roueff, E, Bachiller, R, Commerçon, B, Friesen, R, García-Burillo, S, Goicoechea, J R, Giuliano, B M, Jiménez-Serra, I, Kirk, Jason Matthew, Lattanzi, V, Malinen, J, Marcelino, N, Martín-Domènech, R, Muñoz Caro, G M, Pineda, J, Tercero, B, Treviño-Morales, S P, Roncero, O, Hacar, A, Tafalla, M, Ward-Thompson, Derek, Navarro-Almaida, D, Le Gal, R, Fuente, A, Rivière-Marichalar, P, Wakelam, V, Cazaux, S, Caselli, P, Laas, Jacob C, Alonso-Albi, T, Loison, J C, Gerin, M, Kramer, C, Roueff, E, Bachiller, R, Commerçon, B, Friesen, R, García-Burillo, S, Goicoechea, J R, Giuliano, B M, Jiménez-Serra, I, Kirk, Jason Matthew, Lattanzi, V, Malinen, J, Marcelino, N, Martín-Domènech, R, Muñoz Caro, G M, Pineda, J, Tercero, B, Treviño-Morales, S P, Roncero, O, Hacar, A, Tafalla, M, and Ward-Thompson, Derek

Abstract

Sulphur is one of the most abundant elements in the Universe. Surprisingly, sulphuretted molecules are not as abundant as expected in the interstellar medium and the identity of the main sulphur reservoir is still an open question. Our goal is to investigate the H S chemistry in dark clouds, as this stable molecule is a potential sulphur reservoir. Using millimeter observations of CS, SO, H S, and their isotopologues, we determine the physical conditions and H S abundances along the cores TMC 1-C, TMC 1-CP, and Barnard 1b. The gas-grain model Nautilus is used to model the sulphur chemistry and explore the impact of photo-desorption and chemical desorption on the H S abundance. Our modeling shows that chemical desorption is the main source of gas-phase H S in dark cores. The measured H S abundance can only be fitted if we assume that the chemical desorption rate decreases by more than a factor of 10 when > 2 × 10 . This change in the desorption rate is consistent with the formation of thick H O and CO ice mantles on grain surfaces. The observed SO and H S abundances are in good agreement with our predictions adopting an undepleted value of the sulphur abundance. However, the CS abundance is overestimated by a factor of 5 - 10. Along the three cores, atomic S is predicted to be the main sulphur reservoir. The gaseous H S abundance is well reproduced, assuming undepleted sulphur abundance and chemical desorption as the main source of H S. The behavior of the observed H S abundance suggests a changing desorption efficiency, which would probe the snowline in these cold cores. Our model, however, highly overestimates the observed gas-phase CS abundance. Given the uncertainty in the sulphur chemistry, we can only conclude that our data are consistent with a cosmic elemental S abundance with an uncertainty of a factor of 10.

Published
2020

38. Gas phase Elemental abundances in Molecular cloudS (GEMS)

Author

Bulut, N., primary, Roncero, O., additional, Aguado, A., additional, Loison, J.-C., additional, Navarro-Almaida, D., additional, Wakelam, V., additional, Fuente, A., additional, Roueff, E., additional, Le Gal, R., additional, Caselli, P., additional, Gerin, M., additional, Hickson, K. M., additional, Spezzano, S., additional, Riviére-Marichalar, P., additional, Alonso-Albi, T., additional, Bachiller, R., additional, Jiménez-Serra, I., additional, Kramer, C., additional, Tercero, B., additional, Rodriguez-Baras, M., additional, García-Burillo, S., additional, Goicoechea, J. R., additional, Treviño-Morales, S. P., additional, Esplugues, G., additional, Cazaux, S., additional, Commercon, B., additional, Laas, J., additional, Kirk, J., additional, Lattanzi, V., additional, Martín-Doménech, R., additional, Muñoz-Caro, G., additional, Pineda, J., additional, Ward-Thompson, D., additional, Tafalla, M., additional, Marcelino, N., additional, Malinen, J., additional, Friesen, R., additional, Giuliano, B. M., additional, Agúndez, M., additional, and Hacar, A., additional

Published
2021
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39. The GUAPOS project: G31.41+0.31 Unbiased ALMA sPectral Observational Survey

Author

Mininni, C., primary, Beltrán, M. T., additional, Rivilla, V. M., additional, Sánchez-Monge, A., additional, Fontani, F., additional, Möller, T., additional, Cesaroni, R., additional, Schilke, P., additional, Viti, S., additional, Jiménez-Serra, I., additional, Colzi, L., additional, Lorenzani, A., additional, and Testi, L., additional

Published
2020
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40. Propargylimine in the laboratory and in space: millimetre-wave spectroscopy and its first detection in the ISM

Author

Bizzocchi, L., primary, Prudenzano, D., additional, Rivilla, V. M., additional, Pietropolli-Charmet, A., additional, Giuliano, B. M., additional, Caselli, P., additional, Martín-Pintado, J., additional, Jiménez-Serra, I., additional, Martín, S., additional, Requena-Torres, M. A., additional, Rico-Villas, F., additional, Zeng, S., additional, and Guillemin, J.-C., additional

Published
2020
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41. Seeds of Life in Space (SOLIS)

Author

Taquet, V., primary, Codella, C., additional, De Simone, M., additional, López-Sepulcre, A., additional, Pineda, J. E., additional, Segura-Cox, D., additional, Ceccarelli, C., additional, Caselli, P., additional, Gusdorf, A., additional, Persson, M. V., additional, Alves, F., additional, Caux, E., additional, Favre, C., additional, Fontani, F., additional, Neri, R., additional, Oya, Y., additional, Sakai, N., additional, Vastel, C., additional, Yamamoto, S., additional, Bachiller, R., additional, Balucani, N., additional, Bianchi, E., additional, Bizzocchi, L., additional, Chacón-Tanarro, A., additional, Dulieu, F., additional, Enrique-Romero, J., additional, Feng, S., additional, Holdship, J., additional, Lefloch, B., additional, Jaber Al-Edhari, A., additional, Jiménez-Serra, I., additional, Kahane, C., additional, Lattanzi, V., additional, Ospina-Zamudio, J., additional, Podio, L., additional, Punanova, A., additional, Rimola, A., additional, Sims, I. R., additional, Spezzano, S., additional, Testi, L., additional, Theulé, P., additional, Ugliengo, P., additional, Vasyunin, A. I., additional, Vazart, F., additional, Viti, S., additional, and Witzel, A., additional

Published
2020
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42. Gas phase Elemental abundances in Molecular cloudS (GEMS)

Author

Navarro-Almaida, D., primary, Le Gal, R., additional, Fuente, A., additional, Rivière-Marichalar, P., additional, Wakelam, V., additional, Cazaux, S., additional, Caselli, P., additional, Laas, J. C., additional, Alonso-Albi, T., additional, Loison, J. C., additional, Gerin, M., additional, Kramer, C., additional, Roueff, E., additional, Bachiller, R., additional, Commerçon, B., additional, Friesen, R., additional, García-Burillo, S., additional, Goicoechea, J. R., additional, Giuliano, B. M., additional, Jiménez-Serra, I., additional, Kirk, J. M., additional, Lattanzi, V., additional, Malinen, J., additional, Marcelino, N., additional, Martín-Domènech, R., additional, Muñoz Caro, G. M., additional, Pineda, J., additional, Tercero, B., additional, Treviño-Morales, S. P., additional, Roncero, O., additional, Hacar, A., additional, Tafalla, M., additional, and Ward-Thompson, D., additional

Published
2020
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43. Seeds of Life in Space (SOLIS)

Author

Favre, C., primary, Vastel, C., additional, Jimenez-Serra, I., additional, Quénard, D., additional, Caselli, P., additional, Ceccarelli, C., additional, Chacón-Tanarro, A., additional, Fontani, F., additional, Holdship, J., additional, Oya, Y., additional, Punanova, A., additional, Sakai, N., additional, Spezzano, S., additional, Yamamoto, S., additional, Neri, R., additional, López-Sepulcre, A., additional, Alves, F., additional, Bachiller, R., additional, Balucani, N., additional, Bianchi, E., additional, Bizzocchi, L., additional, Codella, C., additional, Caux, E., additional, De Simone, M., additional, Enrique Romero, J., additional, Dulieu, F., additional, Feng, S., additional, Jaber Al-Edhari, A., additional, Lefloch, B., additional, Ospina-Zamudio, J., additional, Pineda, J., additional, Podio, L., additional, Rimola, A., additional, Segura-Cox, D., additional, Sims, I. R., additional, Taquet, V., additional, Testi, L., additional, Theulé, P., additional, Ugliengo, P., additional, Vasyunin, A. I., additional, Vazart, F., additional, Viti, S., additional, and Witzel, A., additional

Published
2020
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45. A pathfinder for Square Kilometre Array studies

Author

Coutens, A, Liu, HB, Jiménez-Serra, I, Bourke, TL, Forbrich, J, Hoare, M, Loinard, L, Testi, L, Audard, M, Caselli, P, Chacón-Tanarro, A, Codella, C, Di Francesco, J, Fontani, F, Hogerheijde, M, Johansen, A, Johnstone, D, Maddison, S, Panić, O, Pérez, LM, Podio, L, Punanova, A, Rawlings, JMC, Semenov, D, Tazzari, M, Tobin, JJ, van der Wiel, MHD, van Langevelde, HJ, Vlemmings, W, Walsh, C, and Wilner, D

Abstract

Observations of young stellar objects (YSOs) in centimeter bands can probe the continuum emission from growing dust grains, ionized winds, and magnetospheric activity that are intimately connected to the evolution of protoplanetary disks and the formation of planets. We carried out sensitive continuum observations toward the Ophiuchus A star-forming region, using the Karl G. Jansky Very Large Array (VLA) at 10 GHz over a field-of-view of 6′ and with a spatial resolution of θmaj ×θmin ~ 0.′′4 × 0.′′2. We achieved a 5 μJy beam−1 rms noise level at the center of our mosaic field of view. Among the 18 sources we detected, 16 were YSOs (three Class 0, five Class I, six Class II, and two Class III) and two were extragalactic candidates. We find that thermal dust emission generally contributed less than 30% of the emission at 10 GHz. The radio emission is dominated by other types of emission, such as gyro-synchrotron radiation from active magnetospheres, free–free emission from thermal jets, free–free emission from the outflowing photoevaporated disk material, and synchrotron emission from accelerated cosmic-rays in jet or protostellar surface shocks. These different types of emission could not be clearly disentangled. Our non-detections for Class II/III disks suggest that extreme UV-driven photoevaporation is insufficient to explain disk dispersal, assuming that the contribution of UV photoevaporating stellar winds to radio flux does not evolve over time. The sensitivity of our data cannot exclude photoevaporation due to the role of X-ray photons as an efficient mechanism for disk dispersal. Deeper surveys using the Square Kilometre Array (SKA) will have the capacity to provide significant constraints to disk photoevaporation.

Published
2019

46. VLA cm-wave survey of young stellar objects in the Oph A cluster: Constraining extreme UV- And X-ray-driven disk photoevaporation: A pathfinder for Square Kilometre Array studies

Author

Coutens, A., Liu, H. B., Jiménez-Serra, I., Bourke, T. L., Forbrich, J., Hoare, M., Loinard, L., Testi, L., Audard, M., Caselli, P., Chacón-Tanarro, A., Codella, C., Di, Francesco, J., Fontani, F., Hogerheijde, M., Johansen, A., Johnstone, D., Maddison, S., Panić, O., Pérez, L. M., Podio, L., Punanova, A., Rawlings, J. M. C., Semenov, D., Tazzari, M., Tobin, J. J., Van, Der, Wiel, M. H. D., Van, Langevelde, H. J., Vlemmings, W., Walsh, C., Wilner, D., Coutens, A., Liu, H. B., Jiménez-Serra, I., Bourke, T. L., Forbrich, J., Hoare, M., Loinard, L., Testi, L., Audard, M., Caselli, P., Chacón-Tanarro, A., Codella, C., Di, Francesco, J., Fontani, F., Hogerheijde, M., Johansen, A., Johnstone, D., Maddison, S., Panić, O., Pérez, L. M., Podio, L., Punanova, A., Rawlings, J. M. C., Semenov, D., Tazzari, M., Tobin, J. J., Van, Der, Wiel, M. H. D., Van, Langevelde, H. J., Vlemmings, W., Walsh, C., and Wilner, D.

Abstract

Observations of young stellar objects (YSOs) in centimeter bands can probe the continuum emission from growing dust grains, ionized winds, and magnetospheric activity that are intimately connected to the evolution of protoplanetary disks and the formation of planets. We carried out sensitive continuum observations toward the Ophiuchus A star-forming region, using the Karl G. Jansky Very Large Array (VLA) at 10 GHz over a field-of-view of 6′ and with a spatial resolution of θmaj ×θmin ∼ 0.′′4 × 0.′′2. We achieved a 5 μJy beam-1 rms noise level at the center of our mosaic field of view. Among the 18 sources we detected, 16 were YSOs (three Class 0, five Class I, six Class II, and two Class III) and two were extragalactic candidates. We find that thermal dust emission generally contributed less than 30% of the emission at 10 GHz. The radio emission is dominated by other types of emission, such as gyro-synchrotron radiation from active magnetospheres, free-free emission from thermal jets, free-free emission from the outflowing photoevaporated disk material, and synchrotron emission from accelerated cosmic-rays in jet or protostellar surface shocks. These different types of emission could not be clearly disentangled. Our non-detections for Class II/III disks suggest that extreme UV-driven photoevaporation is insufficient to explain disk dispersal, assuming that the contribution of UV photoevaporating stellar winds to radio flux does not evolve over time. The sensitivity of our data cannot exclude photoevaporation due to the role of X-ray photons as an efficient mechanism for disk dispersal. Deeper surveys using the Square Kilometre Array (SKA) will have the capacity to provide significant constraints to disk photoevaporation. © A. Coutens et al..

Published
2019

47. Chemical complexity in high-mass star formation

Author

Gieser, C., primary, Semenov, D., additional, Beuther, H., additional, Ahmadi, A., additional, Mottram, J. C., additional, Henning, Th., additional, Beltran, M., additional, Maud, L. T., additional, Bosco, F., additional, Leurini, S., additional, Peters, T., additional, Klaassen, P., additional, Kuiper, R., additional, Feng, S., additional, Urquhart, J. S., additional, Moscadelli, L., additional, Csengeri, T., additional, Lumsden, S., additional, Winters, J. M., additional, Suri, S., additional, Zhang, Q., additional, Pudritz, R., additional, Palau, A., additional, Menten, K. M., additional, Galvan-Madrid, R., additional, Wyrowski, F., additional, Schilke, P., additional, Sánchez-Monge, Á., additional, Linz, H., additional, Johnston, K. G., additional, Jiménez-Serra, I., additional, Longmore, S., additional, and Möller, T., additional

Published
2019
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49. VLA cm-wave survey of young stellar objects in the Oph A cluster: constraining extreme UV- and X-ray-driven disk photoevaporation

Author

Coutens, A., primary, Liu, H. B., additional, Jiménez-Serra, I., additional, Bourke, T. L., additional, Forbrich, J., additional, Hoare, M., additional, Loinard, L., additional, Testi, L., additional, Audard, M., additional, Caselli, P., additional, Chacón-Tanarro, A., additional, Codella, C., additional, Di Francesco, J., additional, Fontani, F., additional, Hogerheijde, M., additional, Johansen, A., additional, Johnstone, D., additional, Maddison, S., additional, Panić, O., additional, Pérez, L. M., additional, Podio, L., additional, Punanova, A., additional, Rawlings, J. M. C., additional, Semenov, D., additional, Tazzari, M., additional, Tobin, J. J., additional, van der Wiel, M. H. D., additional, van Langevelde, H. J., additional, Vlemmings, W., additional, Walsh, C., additional, and Wilner, D., additional

Published
2019
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50. Gas phase Elemental abundances in Molecular cloudS (GEMS)

Author

Fuente, A., primary, Navarro, D. G., additional, Caselli, P., additional, Gerin, M., additional, Kramer, C., additional, Roueff, E., additional, Alonso-Albi, T., additional, Bachiller, R., additional, Cazaux, S., additional, Commercon, B., additional, Friesen, R., additional, García-Burillo, S., additional, Giuliano, B. M., additional, Goicoechea, J. R., additional, Gratier, P., additional, Hacar, A., additional, Jiménez-Serra, I., additional, Kirk, J., additional, Lattanzi, V., additional, Loison, J. C., additional, Malinen, J., additional, Marcelino, N., additional, Martín-Doménech, R., additional, Muñoz-Caro, G., additional, Pineda, J., additional, Tafalla, M., additional, Tercero, B., additional, Ward-Thompson, D., additional, Treviño-Morales, S. P., additional, Riviére-Marichalar, P., additional, Roncero, O., additional, Vidal, T., additional, and Ballester, M. Y., additional

Published
2019
Full Text
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