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Start Over Author "SCHILKE, P." Publisher edp sciences
252 results on '"SCHILKE, P."'

5. A Survey of SiO J = 1 – 0 emission toward massive star-forming regions

Author

Kim, W.-J., Urquhart, J.S., Veena, V.S., Fuller, G.A., Schilke, P., Kim, K-T, Kim, W.-J., Urquhart, J.S., Veena, V.S., Fuller, G.A., Schilke, P., and Kim, K-T

Abstract

Aims. The application of silicon monoxide (SiO) as a shock tracer arises from its propensity to occur in the gas phase as a result of shock-induced phenomena, including outflow activity and interactions between molecular clouds and expanding Hii regions or supernova remnants. Here we search for indications of shocks toward 366 massive star-forming regions by observing the ground rotational transition of SiO (v = 0, J = 1 − 0) at 43 GHz with the Korean VLBI Network (KVN) 21 m telescopes to extend our understanding on the origins of SiO in star-forming regions. Methods. We analyze the thermal SiO 1 – 0 emission and compare the properties of SiO emission with the physical parameters of associated massive dense clumps as well as 22 GHz H2O and Class I 44 GHz CH3OH maser emission. Results. We detect SiO emission toward 104 regions which consist of 57 IRDCs, 21 HMPOs, and 26 UCHiis. Out of 104 sources, 71 and 80 sources have 22 GHz H2O and 44 GHz Class I CH3OH maser counterparts, respectively. The determined median SiO column density, N(SiO), and abundance, X(SiO), relative to N(H2) are 8.12 × 1012 cm−2 and 1.28 × 10−10, respectively. These values are similar to those obtained toward other star-forming regions and also consistent with predicted values from shock models with low-velocity shocks (≲10 – 15 km s−1). For sources with dust temperatures (Tdust) ≲ 20 K, we find that N(SiO) and X(SiO) derived with the J = 1 − 0 transition are a factor ∼ 3 larger than those from the previous studies obtained with SiO 2 – 1. While the X(SiO) does not exhibit any strong correlation with the evolutionary stages of their host clumps, LSiO is highly correlated with dust clump mass, and LSiO/Lbol also has a strong negative correlation with Tdust. This shows that colder and younger clumps have high LSiO/Lbol suggestive of an evolutionary trend. This trend is not due to excess emission at higher velocities, such as SiO wing features, as the colder sources with high LSiO/Lbol ratios lack wi

Published
2023

6. HyGAL: Characterizing the Galactic ISM with observations of hydrides and other small molecules

Author

Kim, W.-J., primary, Schilke, P., additional, Neufeld, D. A., additional, Jacob, A. M., additional, Sánchez-Monge, Á., additional, Seifried, D., additional, Godard, B., additional, Menten, K. M., additional, Walch, S., additional, Falgarone, E., additional, Veena, V. S., additional, Bialy, S., additional, Möller, T., additional, and Wyrowski, F., additional

Published
2023
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7. N-bearing complex organics toward high-mass protostars

Author

Nazari, P., primary, Meijerhof, J. D., additional, van Gelder, M. L., additional, Ahmadi, A., additional, van Dishoeck, E. F., additional, Tabone, B., additional, Langeroodi, D., additional, Ligterink, N. F. W., additional, Jaspers, J., additional, Beltrán, M. T., additional, Fuller, G. A., additional, Sánchez-Monge, Á., additional, and Schilke, P., additional

Published
2022
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8. Methanol deuteration in high-mass protostars

Author

van Gelder, M. L., primary, Jaspers, J., additional, Nazari, P., additional, Ahmadi, A., additional, van Dishoeck, E. F., additional, Beltrán, M. T., additional, Fuller, G. A., additional, Sánchez-Monge, Á., additional, and Schilke, P., additional

Published
2022
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9. The physical and chemical structure of Sagittarius B2

Author

Meng, F., primary, Sánchez-Monge, Á., additional, Schilke, P., additional, Ginsburg, A., additional, DePree, C., additional, Budaiev, N., additional, Jeff, D., additional, Schmiedeke, A., additional, Schwörer, A., additional, Veena, V. S., additional, and Möller, Th., additional

Published
2022
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10. Importance of source structure on complex organics emission

Author

van Gelder, M. L., primary, Nazari, P., additional, Tabone, B., additional, Ahmadi, A., additional, van Dishoeck, E. F., additional, Beltrán, M. T., additional, Fuller, G. A., additional, Sakai, N., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, Yang, Y.-L., additional, and Zhang, Y., additional

Published
2022
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11. The sharp ALMA view of infall and outflow in the massive protocluster G31.41+0.31

Author

Beltrán, M. T., primary, Rivilla, V. M., additional, Cesaroni, R., additional, Galli, D., additional, Moscadelli, L., additional, Ahmadi, A., additional, Beuther, H., additional, Etoka, S., additional, Goddi, C., additional, Klaassen, P. D., additional, Kuiper, R., additional, Kumar, M. S. N., additional, Lorenzani, A., additional, Peters, T., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, van der Tak, F., additional, and Vig, S., additional

Published
2022
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12. Disk fragmentation in high-mass star formation

Author

Suri, S., primary, Beuther, H., additional, Gieser, C., additional, Ahmadi, A., additional, Sánchez-Monge, Á., additional, Winters, J. M., additional, Linz, H., additional, Henning, Th., additional, Beltrán, M. T., additional, Bosco, F., additional, Cesaroni, R., additional, Csengeri, T., additional, Feng, S., additional, Hoare, M. G., additional, Johnston, K. G., additional, Klaassen, P., additional, Kuiper, R., additional, Leurini, S., additional, Longmore, S., additional, Lumsden, S., additional, Maud, L., additional, Moscadelli, L., additional, Möller, T., additional, Palau, A., additional, Peters, T., additional, Pudritz, R. E., additional, Ragan, S. E., additional, Semenov, D., additional, Schilke, P., additional, Urquhart, J. S., additional, Wyrowski, F., additional, and Zinnecker, H., additional

Published
2021
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13. Physical and chemical structure of high-mass star-forming regions

Author

Gieser, C, Beuther, H, Semenov, D, Ahmadi, A, Suri, S, Möller, T, Beltrán, MT, Klaassen, P, Zhang, Q, Urquhart, JS, Henning, T, Feng, S, Galván-Madrid, R, de Souza Magalhães, V, Moscadelli, L, Longmore, S, Leurini, S, Kuiper, R, Peters, T, Menten, KM, Csengeri, T, Fuller, G, Wyrowski, F, Lumsden, S, Sánchez-Monge, Á, Maud, L, Linz, H, Palau, A, Schilke, P, Pety, J, Pudritz, R, Winters, JM, Piétu, V, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Ludwig-Maximilians-Universität München (LMU), Leiden University, Universität zu Köln, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Royal Observatory Edinburgh (ROE), University of Edinburgh, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), University of Kent [Canterbury], Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Chinese Academy of Sciences [Beijing] (CAS), National Astronomical Observatory of Japan (NAOJ), Universidad Nacional Autónoma de México (UNAM), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), INAF - Osservatorio Astronomico di Cagliari (OAC), University of Tübingen, Max-Planck-Institut für Astrophysik (MPA), Max Planck Institute for Radio Astronomy, FEMIS 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Leeds, European Southern Observatory (ESO), Instituto de Matematicas (UNAM), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and McMaster University [Hamilton, Ontario]

Subjects
[PHYS]Physics [physics], stars: formation, astrochemistry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ISM: molecules
Abstract

International audience; Aims. Current star formation research centers the characterization of the physical and chemical properties of massive stars, which are in the process of formation, at the spatial resolution of individual high-mass cores.Methods. We use sub-arcsecond resolution (~0.′′4) observations with the NOrthern Extended Millimeter Array at 1.37 mm to study the dust emission and molecular gas of 18 high-mass star-forming regions. With distances in the range of 0.7−5.5 kpc, this corresponds to spatial scales down to 300−2300 au that are resolved by our observations. We combined the derived physical and chemical properties of individual cores in these regions to estimate their ages. The temperature structures of these regions are determined by fitting the H2CO and CH3CN line emission. The density profiles are inferred from the 1.37 mm continuum visibilities. The column densities of 11 different species are determined by fitting the emission lines with XCLASS.Results. Within the 18 observed regions, we identified 22 individual cores with associated 1.37 mm continuum emission and with a radially decreasing temperature profile. We find an average temperature power-law index of q = 0.4 ± 0.1 and an average density power-law index of p = 2.0 ± 0.2 on scales that are on the order of several 1000 au. Comparing these results with values of p derived from the literature presumes that the density profiles remain unchanged from clump to core scales. The column densities relative to N(C18O) between pairs of dense gas tracers show tight correlations. We applied the physical-chemical model MUlti Stage ChemicaL codE to the derived column densities of each core and find a mean chemical age of ~60 000 yr and an age spread of 20 000−100 000 yr. With this paper, we release all data products of the CORE project.Conclusions. The CORE sample reveals well-constrained density and temperature power-law distributions. Furthermore, we characterized a large variety in molecular richness that can be explained by an age spread that is then confirmed by our physical-chemical modeling. The hot molecular cores show the greatest number of emission lines, but we also find evolved cores at an evolutionary stage in which most molecules are destroyed and, thus, the spectra appear line-poor once again.

Published
2021

14. 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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15. Disk fragmentation in high-mass star formation: High-resolution observations towards AFGL 2591-VLA 3

Author

Suri, S., Beuther, H., Geiser, C., Ahmadi, A., Sanchez-Monge, A., Winters, J.M., Linz, H., Henning, Th., Bletran, M.T., Bosco, F., Cesaroni, R., Csengeri, T., Feng, S., Hoare, M.G., Johnston, K.G., Klaassen, P., Kuiper, R., Leurini, S., Longmore, S., Lumsden, S., Maud, L., Moscadelli, L., Möller, T., Palau, A., Peters, T., Pudritz, R.E., Ragan, S.E., Semenov, D., Schilke, P., Urquhart, J.S., Wyrowski, F., Zinnecker, H., Suri, S., Beuther, H., Geiser, C., Ahmadi, A., Sanchez-Monge, A., Winters, J.M., Linz, H., Henning, Th., Bletran, M.T., Bosco, F., Cesaroni, R., Csengeri, T., Feng, S., Hoare, M.G., Johnston, K.G., Klaassen, P., Kuiper, R., Leurini, S., Longmore, S., Lumsden, S., Maud, L., Moscadelli, L., Möller, T., Palau, A., Peters, T., Pudritz, R.E., Ragan, S.E., Semenov, D., Schilke, P., Urquhart, J.S., Wyrowski, F., and Zinnecker, H.

Abstract

Context: Increasing evidence suggests that, similar to their low-mass counterparts, high-mass stars form through a disk-mediated accretion process. At the same time, formation of high-mass stars still necessitates high accretion rates, and hence, high gas densities, which in turn can cause disks to become unstable against gravitational fragmentation. Aims: We study the kinematics and fragmentation of the disk around the high-mass star forming region AFGL 2591-VLA 3 which was hypothesized to be fragmenting based on the observations that show multiple outflow directions. Methods: We use a new set of high-resolution (0".19) IRAM/NOEMA observations at 843 µm towards VLA 3 which allow us to resolve its disk, characterize the fragmentation, and study its kinematics. In addition to the 843 µm continuum emission, our spectral setup targets warm dense gas and outflow tracers such as HCN, HC\(_3\)N and SO\(_2\), as well as vibrationally excited HCN lines. Results: The high resolution continuum and line emission maps reveal multiple fragments with subsolar masses within the inner ∼1000 AU of VLA 3. Furthermore, the velocity field of the inner disk observed at 843 µm shows a similar behavior to that of the larger scale velocity field studied in the CORE project at 1.37 mm. Conclusions: We present the first observational evidence for disk fragmentation towards AFGL 2591-VLA 3, a source that was thought to be a single high-mass core. While the fragments themselves are low-mass, the rotation of the disk is dominated by the protostar with a mass of 10.3±1.8 M\(_⊙\). These data also show that NOEMA Band 4 can obtain the highest currently achievable spatial resolution at (sub-)mm wavelengths in observations of strong northern sources.

Published
2021

17. Fragmentation and kinematics in high-mass star formation

Author

Beuther, H., primary, Gieser, C., additional, Suri, S., additional, Linz, H., additional, Klaassen, P., additional, Semenov, D., additional, Winters, J. M., additional, Henning, Th., additional, Soler, J. D., additional, Urquhart, J. S., additional, Syed, J., additional, Feng, S., additional, Möller, T., additional, Beltrán, M. T., additional, Sánchez-Monge, Á., additional, Longmore, S. N., additional, Peters, T., additional, Ballesteros-Paredes, J., additional, Schilke, P., additional, Moscadelli, L., additional, Palau, A., additional, Cesaroni, R., additional, Lumsden, S., additional, Pudritz, R., additional, Wyrowski, F., additional, Kuiper, R., additional, and Ahmadi, A., additional

Published
2021
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18. Fragmentation in the massive G31.41+0.31 protocluster

Author

Beltrán, M. T., primary, Rivilla, V. M., additional, Cesaroni, R., additional, Maud, L. T., additional, Galli, D., additional, Moscadelli, L., additional, Lorenzani, A., additional, Ahmadi, A., additional, Beuther, H., additional, Csengeri, T., additional, Etoka, S., additional, Goddi, C., additional, Klaassen, P. D., additional, Kuiper, R., additional, Kumar, M. S. N., additional, Peters, T., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, van der Tak, F., additional, Vig, S., additional, and Zinnecker, H., additional

Published
2021
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20. 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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21. Physical properties of the star-forming clusters in NGC 6334

Author

Sadaghiani, M., primary, Sánchez-Monge, Á., additional, Schilke, P., additional, Liu, H. B., additional, Clarke, S. D., additional, Zhang, Q., additional, Girart, J. M., additional, Seifried, D., additional, Aghababaei, A., additional, Li, H., additional, Juárez, C., additional, and Tang, K. S., additional

Published
2020
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22. 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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23. ALMA evidence for an SiO disc and disc wind from G17.64+0.16

Author

Maud, L. T., Cesaroni, R., Kumar, M. S. N., van der Tak, F. F. S., Allen, V., Hoare, M. G., Klaassen, P. D., Harsono, D., Hogerheijde, M. R., Sánchez-Monge, Á., Schilke, P., Ahmadi, A., Beltrán, M. T., Beuther, H., Csengeri, T., Etoka, S., Fuller, G., Galván-Madrid, R., Goddi, C., Henning, Th., Johnston, K. G., Kuiper, R., Lumsden, S., Moscadelli, L., Mottram, J. C., Peters, T., Rivilla, V. M., Testi, L., Vig, S., de Wit, W. J., Zinnecker, H., FORMATION STELLAIRE 2020, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Astronomy

Subjects
stars: winds, outflows, stars: formation, stars: protostars, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], EARLY EVOLUTION, INFRARED REFLECTION NEBULA, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, IMAGING POLARIMETRY, submillimeter: stars, stars: massive, SUBMILLIMETER ARRAY OBSERVATIONS, DISTANCE-LIMITED SAMPLE, LINE-DRIVEN ABLATION, RADIO-EMISSION, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, MASSIVE STAR-FORMATION, CIRCUMSTELLAR DISCS, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, RADIATION PRESSURE
Abstract

We present high angular resolution (similar to 0.2 '') continuum and molecular emission line Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of G17.64+0.16 in Band 6 (220-230 GHz) taken as part of a campaign in search of circumstellar discs around (proto)-O-stars. At a resolution of similar to 400 au the main continuum core is essentially unresolved and isolated from other strong and compact emission peaks. We detect SiO (5-4) emission that is marginally resolved and elongated in a direction perpendicular to the large-scale outflow seen in the (CO)-C-13 (2-1) line using the main ALMA array in conjunction with the Atacama Compact Array (ACA). Morphologically, the SiO appears to represent a disc-like structure. Using parametric models we show that the position-velocity profile of the SiO is consistent with the Keplerian rotation of a disc around an object between 10 and 30M(circle dot) in mass, only if there is also radial expansion from a separate structure. The radial motion component can be interpreted as a disc wind from the disc surface. Models with a central stellar object mass between 20 and 30 M-circle dot are the most consistent with the stellar luminosity (1 x 10(5) L-circle dot) and indicative of an O-type star. The H30 alpha millimetre recombination line (231.9 GHz) is also detected, but spatially unresolved, and is indicative of a very compact, hot, ionised region co-spatial with the dust continuum core. The broad line-width of the H30 alpha emission (full-width-half-maximum = 81.9 km s(-1)) is not dominated by pressure-broadening but is consistent with underlying bulk motions. These velocities match those required for shocks to release silicon from dust grains into the gas phase. CH3CN and CH3OH thermal emission also shows two arc shaped plumes that curve away from the disc plane. Their coincidence with OH maser emission suggests that they could trace the inner working surfaces of a wide-angle wind driven by G17.64 which impacts the diffuse remnant natal cloud before being redirected into the large-scale outflow direction. Accounting for all observables, we suggest that G17.64 is consistent with a O-type young stellar object in the final stages of protostellar assembly, driving a wind, but that has not yet developed into a compact HII region. The existance and detection of the disc in G17.64 is likely related to its isolated and possibly more evolved nature, traits which may underpin discs in similar sources.

Published
2018

24. Core fragmentation and Toomre stability analysis of W3(H₂O): A case study of the IRAM NOEMA large program CORE

Author

Ahmadi, A, Beuther, H, Mottram, JC, Bosco, F, Linz, H, Henning, T, Winters, JM, Kuiper, R, Pudritz, R, Sánchez-Monge, Á, Keto, E, Beltran, M, Bontemps, S, Cesaroni, R, Csengeri, T, Feng, S, Galvan-Madrid, R, Johnston, KG, Klaassen, P, Leurini, S, Longmore, SN, Lumsden, S, Maud, LT, Menten, KM, Moscadelli, L, Motte, F, Palau, A, Peters, T, Ragan, SE, Schilke, P, Urquhart, JS, Wyrowski, F, and Zinnecker, H

Subjects
Physik (inkl. Astronomie)
Abstract

Context. The fragmentation mode of high-mass molecular clumps and the properties of the central rotating structures surrounding the most luminous objects have yet to be comprehensively characterised. Aims. We study the fragmentation and kinematics of the high-mass star-forming region W3(H₂O), as part of the IRAM NOrthern Extended Millimeter Array (NOEMA) large programme CORE. Methods. Using the IRAM NOEMA and the IRAM 30 m telescope, the CORE survey has obtained high-resolution observations of 20 well-known highly luminous star-forming regions in the 1.37 mm wavelength regime in both line and dust continuum emission. Results. We present the spectral line setup of the CORE survey and a case study for W3(H₂O). At ~0.′′35 (700 AU at 2.0 kpc) resolution, the W3(H₂O) clump fragments into two cores (west and east), separated by ~2300 AU. Velocity shifts of a few km s⁻¹ are observed in the dense-gas tracer, CH₃CN, across both cores, consistent with rotation and perpendicular to the directions of two bipolar outflows, one emanating from each core. The kinematics of the rotating structure about W3(H₂O) W shows signs of differential rotation of material, possibly in a disk-like object. The observed rotational signature around W3(H₂O) E may be due to a disk-like object, an unresolved binary (or multiple) system, or a combination of both. We fit the emission of CH₃CN (12K-11K), K = 4-6 and derive a gas temperature map with a median temperature of ~165 K across W3(H₂O). We create a Toomre Q map to study thestability of the rotating structures against gravitational instability. The rotating structures appear to be Toomre unstable close to their outer boundaries, with a possibility of further fragmentation in the differentially rotating core, W3(H₂O) W. Rapid cooling in the Toomre unstable regions supports the fragmentation scenario. Conclusions. Combining millimetre dust continuum and spectral line data toward the famous high-mass star-forming region W3(H₂O), we identify core fragmentation on large scales, and indications for possible disk fragmentation on smaller spatial scales.

Published
2018

25. IRAS 23385+6053: An embedded massive cluster in the making

Author

Cesaroni, R., Beuther, H., Ahmadi, A., Beltran, M.T., Csengeri, T., Galvan-Madrid, R., Gieser, C., Henning, T., Johnston, K.G., Klaassen, P. D., Kuiper, R., Leurini, S., Linz, H., Longmore, S., Lumsden, S.L., Maud, L.T., Moscadelli, L., Mottram, J.C., Palau, A., Peters, T., Pudritz, R.E., Sanchez-Monge, A., Schilke, P., Semenov, D., Suri, S., Urquhart, J.S., Winters, J.M., Zhang, Q., Zinnecker, H., Cesaroni, R., Beuther, H., Ahmadi, A., Beltran, M.T., Csengeri, T., Galvan-Madrid, R., Gieser, C., Henning, T., Johnston, K.G., Klaassen, P. D., Kuiper, R., Leurini, S., Linz, H., Longmore, S., Lumsden, S.L., Maud, L.T., Moscadelli, L., Mottram, J.C., Palau, A., Peters, T., Pudritz, R.E., Sanchez-Monge, A., Schilke, P., Semenov, D., Suri, S., Urquhart, J.S., Winters, J.M., Zhang, Q., and Zinnecker, H.

Abstract

Context. This study is part of the project “CORE”, an IRAM/NOEMA large program consisting of observations of the millimeter continuum and molecular line emission towards 20 selected high-mass star forming regions. The goal of the program is to search for circumstellar accretion disks, study the fragmentation process of molecular clumps, and investigate the chemical composition of the gas in these regions. Aims. We focus on IRAS 23385+6053, which is believed to be the least evolved source of the CORE sample. This object is characterized by a compact molecular clump that is IR dark shortward of 24 µm and is surrounded by a stellar cluster detected in the near-IR. Our aim is to study the structure and velocity field of the clump. Methods. The observations were performed at ∼1.4 mm and employed three configurations of NOEMA and additional single-dish maps, merged with the interferometric data to recover the extended emission. Our correlator setup covered a number of lines from well-known hot core tracers and a few outflow tracers. The angular (∼0.′′45–0.′′9) and spectral (0.5 km s−1) resolutions were sufficient to resolve the clump in IRAS 23385+6053 and investigate the existence of large-scale motions due to rotation, infall, or expansion. Results. We find that the clump splits into six distinct cores when observed at sub-arcsecond resolution. These are identified through their 1.4 mm continuum and molecular line emission. We produce maps of the velocity, line width, and rotational temperature from the methanol and methyl cyanide lines, which allow us to investigate the cores and reveal a velocity and temperature gradient in the most massive core. We also find evidence of a bipolar outflow, possibly powered by a low-mass star. Conclusions. We present the tentative detection of a circumstellar self-gravitating disk lying in the most massive core and powering a largescale outflow previously known in the literature. In our scenario, the star powering the flow is responsib

Published
2019

26. The physical and chemical structure of Sagittarius B2

Author

Meng, F., primary, Sánchez-Monge, Á., additional, Schilke, P., additional, Padovani, M., additional, Marcowith, A., additional, Ginsburg, A., additional, Schmiedeke, A., additional, Schwörer, A., additional, DePree, C., additional, Veena, V. S., additional, and Möller, Th., additional

Published
2019
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27. Fragmentation, rotation, and outflows in the high-mass star-forming region IRAS 23033+5951

Author

Bosco, F., primary, Beuther, H., additional, Ahmadi, A., additional, Mottram, J. C., additional, Kuiper, R., additional, Linz, H., additional, Maud, L., additional, Winters, J. M., additional, Henning, T., additional, Feng, S., additional, Peters, T., additional, Semenov, D., additional, Klaassen, P. D., additional, Schilke, P., additional, Urquhart, J. S., additional, Beltrán, M. T., additional, Lumsden, S. L., additional, Leurini, S., additional, Moscadelli, L., additional, Cesaroni, R., additional, Sánchez-Monge, Á., additional, Palau, A., additional, Pudritz, R., additional, Wyrowski, F., additional, and Longmore, S., additional

Published
2019
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28. The physical and chemical structure of Sagittarius B2

Author

Schwörer, A., primary, Sánchez-Monge, Á., additional, Schilke, P., additional, Möller, T., additional, Ginsburg, A., additional, Meng, F., additional, Schmiedeke, A., additional, Müller, H. S. P., additional, Lis, D., additional, and Qin, S.-L., additional

Published
2019
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29. IRAS 23385+6053: an embedded massive cluster in the making

Author

Cesaroni, R., primary, Beuther, H., additional, Ahmadi, A., additional, Beltrán, M. T., additional, Csengeri, T., additional, Galván-Madrid, R., additional, Gieser, C., additional, Henning, T., additional, Johnston, K. G., additional, Klaassen, P. D., additional, Kuiper, R., additional, Leurini, S., additional, Linz, H., additional, Longmore, S., additional, Lumsden, S. L., additional, Maud, L. T., additional, Moscadelli, L., additional, Mottram, J. C., additional, Palau, A., additional, Peters, T., additional, Pudritz, R. E., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, Semenov, D., additional, Suri, S., additional, Urquhart, J. S., additional, Winters, J. M., additional, Zhang, Q., additional, and Zinnecker, H., additional

Published
2019
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30. Histogram of oriented gradients: a technique for the study of molecular cloud formation

Author

Soler, J. D., primary, Beuther, H., additional, Rugel, M., additional, Wang, Y., additional, Clark, P. C., additional, Glover, S. C. O., additional, Goldsmith, P. F., additional, Heyer, M., additional, Anderson, L. D., additional, Goodman, A., additional, Henning, Th., additional, Kainulainen, J., additional, Klessen, R. S., additional, Longmore, S. N., additional, McClure-Griffiths, N. M., additional, Menten, K. M., additional, Mottram, J. C., additional, Ott, J., additional, Ragan, S. E., additional, Smith, R. J., additional, Urquhart, J. S., additional, Bigiel, F., additional, Hennebelle, P., additional, Roy, N., additional, and Schilke, P., additional

Published
2019
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31. Chasing discs around O-type (proto)stars

Author

Maud, L. T., primary, Cesaroni, R., additional, Kumar, M. S. N., additional, van der Tak, F. F. S., additional, Allen, V., additional, Hoare, M. G., additional, Klaassen, P. D., additional, Harsono, D., additional, Hogerheijde, M. R., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, Ahmadi, A., additional, Beltrán, M. T., additional, Beuther, H., additional, Csengeri, T., additional, Etoka, S., additional, Fuller, G., additional, Galván-Madrid, R., additional, Goddi, C., additional, Henning, Th., additional, Johnston, K. G., additional, Kuiper, R., additional, Lumsden, S., additional, Moscadelli, L., additional, Mottram, J. C., additional, Peters, T., additional, Rivilla, V. M., additional, Testi, L., additional, Vig, S., additional, de Wit, W. J., additional, and Zinnecker, H., additional

Published
2018
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32. Core fragmentation and Toomre stability analysis of W3(H2O) A case study of the IRAM NOEMA large program CORE

Author

Ahmadi, A., Beuther, H., Mottram, J.C., Bosco, F., Linz, H., Henning, Th., Winters, J.M., Kuiper, R., Pudritz, R., Sanchez-Monge, A., Keto, E., Beltran, M., Bontemps, S., Cesaroni, R., Csengeri, T., Feng, S., Galvan-Madrid, R., Johnston, K.G., Klaassen, P., Leurini, S., Longmore, S.N., Lumsden, S., Maud, L.T., Menten, K.M., Moscadelli, l., Motte, F., Palau, A., Peters, T., Ragan, S.E., Schilke, P., Urquhart, J.S., Wyrowski, F., Zinnecker, H., Ahmadi, A., Beuther, H., Mottram, J.C., Bosco, F., Linz, H., Henning, Th., Winters, J.M., Kuiper, R., Pudritz, R., Sanchez-Monge, A., Keto, E., Beltran, M., Bontemps, S., Cesaroni, R., Csengeri, T., Feng, S., Galvan-Madrid, R., Johnston, K.G., Klaassen, P., Leurini, S., Longmore, S.N., Lumsden, S., Maud, L.T., Menten, K.M., Moscadelli, l., Motte, F., Palau, A., Peters, T., Ragan, S.E., Schilke, P., Urquhart, J.S., Wyrowski, F., and Zinnecker, H.

Abstract

The fragmentation mode of high-mass molecular clumps and the properties of the central rotating structures surrounding the most luminous objects have yet to be comprehensively characterised. Using the IRAM NOrthern Extended Millimeter Array (NOEMA) and the IRAM 30-m telescope, the CORE survey has obtained high-resolution observations of 20 well-known highly luminous star-forming regions in the 1.37 mm wavelength regime in both line and dust continuum emission. We present the spectral line setup of the CORE survey and a case study for W3(H2O). At ~0.35" (700 AU at 2 kpc) resolution, the W3(H2O) clump fragments into two cores (West and East), separated by ~2300 AU. Velocity shifts of a few km/s are observed in the dense-gas tracer, CH3CN, across both cores, consistent with rotation and perpendicular to the directions of two bipolar outflows, one emanating from each core. The kinematics of the rotating structure about W3(H2O) W shows signs of differential rotation of material, possibly in a disk-like object. The observed rotational signature around W3(H2O) E may be due to a disk-like object, an unresolved binary (or multiple) system, or a combination of both. We fit the emission of CH3CN (12-11) K = 4-6 and derive a gas temperature map with a median temperature of ~165 K across W3(H2O). We create a Toomre Q map to study the stability of the rotating structures against gravitational instability. The rotating structures appear to be Toomre unstable close to their outer boundaries, with a possibility of further fragmentation in the differentially-rotating core W3(H2O) W. Rapid cooling in the Toomre-unstable regions supports the fragmentation scenario. Combining millimeter dust continuum and spectral line data toward the famous high-mass star-forming region W3(H2O), we identify core fragmentation on large scales, and indications for possible disk fragmentation on smaller spatial scales.

Published
2018

33. Physical properties of the star-forming clusters in NGC6334 A study of the continuum dust emission with ALMA.

Author

Sadaghiani, M., Sánchez-Monge, Á., Schilke, P., Liu, H. B., Clarke, S. D., Zhang, Q., Girart, J. M., Seifried, D., Aghababaei, A., Li, H., Juárez, C., and Tang, K. S.

Subjects
STELLAR initial mass function, NUCLEOSYNTHESIS, DUST, GAS reservoirs, GAMMA ray bursts, STELLAR evolution, MOLECULAR clouds
Abstract

Aims. We aim to characterise certain physical properties of high-mass star-forming sites in the NGC6334 molecular cloud, such as the core mass function (CMF), spatial distribution of cores, and mass segregation. Methods. We used the Atacama Large Millimeter/sub-millimeter Array (ALMA) to image the embedded clusters NGC6334-I and NGC6334-I(N) in the continuum emission at 87.6 GHz. We achieved a spatial resolution of 1300 au, enough to resolve different compact cores and fragments, and to study the properties of the clusters. Results. We detected 142 compact sources distributed over the whole surveyed area. The ALMA compact sources are clustered in different regions. We used different machine-learning algorithms to identify four main clusters: NGC6334-I, NGC6334-I(N), NGC6334-I(NW), and NGC6334-E. The typical separations between cluster members range from 4000 au to 12 000 au. These separations, together with the core masses (0.1-100 M), are in agreement with the fragmentation being controlled by turbulence at scales of 0.1 pc. We find that the CMFs show an apparent excess of high-mass cores compared to the stellar initial mass function. We evaluated the effects of temperature and unresolved multiplicity on the derived slope of the CMF. Based on this, we conclude that the excess of high-mass cores might be spurious and due to inaccurate temperature determinations and/or resolution limitations. We searched for evidence of mass segregation in the clusters and we find that clusters NGC6334-I and NGC6334-I(N) show hints of segregation with the most massive cores located in the centre of the clusters. Conclusions. We searched for correlations between the physical properties of the four embedded clusters and their evolutionary stage (based on the presence of H II regions and infrared sources). NGC6334-E appears as the most evolved cluster, already harbouring a well-developed H II region. NGC6334-I is the second-most evolved cluster with an ultra-compact H II region. NGC6334-I(N) contains the largest population of dust cores distributed in two filamentary structures and no dominant H II region. Finally, NGC6334-I(NW) is a cluster of mainly low-mass dust cores with no clear signs of massive cores or H II regions. We find a larger separation between cluster members in the more evolved clusters favouring the role of gas expulsion and stellar ejection with evolution. The mass segregation, seen in the NGC6334-I and NGC6334-I(N) clusters, suggests a primordial origin for NGC6334-I(N). In contrast, the segregation in NGC6334-I might be due to dynamical effects. Finally, the lack of massive cores in the most evolved cluster suggests that the gas reservoir is already exhausted, while the less evolved clusters still have a large gas reservoir along with the presence of massive cores. In general, the fragmentation process of NGC6334 at large scales (from filament to clump, i.e. at about 1 pc) is likely governed by turbulent pressure, while at smaller scales (scale of cores and sub-fragments, i.e. a few hundred au) thermal pressure starts to be more significant. [ABSTRACT FROM AUTHOR]

Published
2020
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34. Fragmentation and disk formation during high-mass star formation

Author

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

Published
2018
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36. The feedback of an HC HII region on its parental molecular core

Author

Moscadelli, L., primary, Rivilla, V. M., additional, Cesaroni, R., additional, Beltrán, M. T., additional, Sánchez-Monge, Á, additional, Schilke, P., additional, Mottram, J. C., additional, Ahmadi, A., additional, Allen, V., additional, Beuther, H., additional, Csengeri, T., additional, Etoka, S., additional, Galli, D., additional, Goddi, C., additional, Johnston, K. G., additional, Klaassen, P. D., additional, Kuiper, R., additional, Kumar, M. S. N., additional, Maud, L. T., additional, Möller, T., additional, Peters, T., additional, Van der Tak, F., additional, and Vig, S., additional

Published
2018
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37. Accelerating infall and rotational spin-up in the hot molecular core G31.41+0.31

Author

Beltrán, M. T., primary, Cesaroni, R., additional, Rivilla, V. M., additional, Sánchez-Monge, Á., additional, Moscadelli, L., additional, Ahmadi, A., additional, Allen, V., additional, Beuther, H., additional, Etoka, S., additional, Galli, D., additional, Galván-Madrid, R., additional, Goddi, C., additional, Johnston, K. G., additional, Klaassen, P. D., additional, Kölligan, A., additional, Kuiper, R., additional, Kumar, M. S. N., additional, Maud, L. T., additional, Mottram, J. C., additional, Peters, T., additional, Schilke, P., additional, Testi, L., additional, van der Tak, F, additional, and Walmsley, C. M., additional

Published
2018
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40. Continuum radiative transfer Modeling of Sagittarius B2

Author

Schmiedeke, A., Schilke, P., Möller, Th., Sánchez-Monge, Á., Bergin, E., Comito, C., Csengeri, T., Lis, D. C., Molinari, S., Qin, S. L., Rolffs, R., Simon, Robert, Schaaf, Reinhold, and Stutzki, Jürgen

Abstract

We present results from radiative transfer modeling of the continuum emission towards Sagittarius B2 (hereafter Sgr B2). We have developed a radiative transfer framework – Pandora – that employs RADMC-3D (Dullemond 2012) for a self-consistent determination of the dust temperature. With this pipeline, we have set-up a single model that consistently reproduces the thermal dust and free-free continuum emission of Sgr B2 spanning four orders of magnitude in spatial scales (0.02–45 pc) and two orders of magnitude in frequency (20–4000 GHz).

Published
2016

41. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues First data release for the inner Milky Way:+68 degrees >= l >=-70 degrees

Author

Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., Benedettini, M., Calzoletti, L., Faustini, F., Natoli, Paolo, Piacentini, F., Merello, M., Palmese, A., Del Grande, R., Polychroni, D., Ryg, K. L. J., Polenta, G., Barlow, M. J., Bernard, J. P., Martin, P. G., Testi, L., Ali, B., Andre, P., Beltran, M. T., Billot, N., Carey, S., Cesaroni, R., Compiegne, M., Eden, D., Fukui, Y., Garcia Lario, P., Hoare, M. G., Huang, M., Joncas, G., Lim, T. L., Lord, . D., Martinavarro Armengol, S., Motte, F., Paladini, R., Paradis, D., Peretto, N., Robitaille, T., Schilke, P., Schneider, N., Schulz, B., Sibthorpe, B., Strafella, F., Thompson, M. A., Umana, G., Ward Thompson, D., and Wyrowski, F.

Subjects
infrared: ISM, techniques: photometric, stars: formation, extinction, dust, extinction, infrared: ISM, stars: formation, Galaxy: disk, methods: data analysis , techniques: photometric, dust, methods: data analysis, NO, Galaxy: disk, QB
Abstract

Aims. We present the first public release of high-quality data products (DR1) from Hi-GAL, the Herschel infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic plane surveys from the near-IR to the radio and covers five wavebands at 70, 160, 250, 350 and 500 μm, encompassing the peak of the spectral energy distribution of cold dust for 8 ≲ T ≲ 50 K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68° ≳ ℓ ≳ −70° in a | b | ≤ 1° latitude strip.\ud Methods. Photometric maps have been produced with the ROMAGAL pipeline, which optimally capitalizes on the excellent sensitivity and stability of the bolometer arrays of the Herschel PACS and SPIRE photometric cameras. It delivers images of exquisite quality and dynamical range, absolutely calibrated with Planck and IRAS, and recovers extended emission at all wavelengths and all spatial scales, from the point-spread function to the size of an entire 2°× 2° “tile” that is the unit observing block of the survey. The compact source catalogues were generated with the CuTEx algorithm, which was specifically developed to optimise source detection and extraction in the extreme conditions of intense and spatially varying background that are found in the Galactic plane in the thermal infrared.\ud Results. Hi-GAL DR1 images are cirrus noise limited and reach the 1σ-rms predicted by the Herschel Time Estimators for parallel-mode observations at 60′′ s-1 scanning speed in relatively low cirrus emission regions. Hi-GAL DR1 images will be accessible through a dedicated web-based image cutout service. The DR1 Compact Source Catalogues are delivered as single-band photometric lists containing, in addition to source position, peak, and integrated flux and source sizes, a variety of parameters useful to assess the quality and reliability of the extracted sources. Caveats and hints to help in this assessment are provided. Flux completeness limits in all bands are determined from extensive synthetic source experiments and greatly depend on the specific line of sight along the Galactic plane because the background strongly varies as a function of Galactic longitude. Hi-GAL DR1 catalogues contain 123210, 308509, 280685, 160972, and 85460 compact sources in the five bands.

Published
2016

42. The physical and chemical structure of Sagittarius B2

Author

Sánchez-Monge, Á., primary, Schilke, P., additional, Schmiedeke, A., additional, Ginsburg, A., additional, Cesaroni, R., additional, Lis, D. C., additional, Qin, S.-L., additional, Müller, H. S. P., additional, Bergin, E., additional, Comito, C., additional, and Möller, Th., additional

Published
2017
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43. Chasing discs around O-type (proto)stars: Evidence from ALMA observations

Author

Cesaroni, R., primary, Sánchez-Monge, Á., additional, Beltrán, M. T., additional, Johnston, K. G., additional, Maud, L. T., additional, Moscadelli, L., additional, Mottram, J. C., additional, Ahmadi, A., additional, Allen, V., additional, Beuther, H., additional, Csengeri, T., additional, Etoka, S., additional, Fuller, G. A., additional, Galli, D., additional, Galván-Madrid, R., additional, Goddi, C., additional, Henning, T., additional, Hoare, M. G., additional, Klaassen, P. D., additional, Kuiper, R., additional, Kumar, M. S. N., additional, Lumsden, S., additional, Peters, T., additional, Rivilla, V. M., additional, Schilke, P., additional, Testi, L., additional, van der Tak, F., additional, Vig, S., additional, Walmsley, C. M., additional, and Zinnecker, H., additional

Published
2017
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44. SEDIGISM: Structure, excitation, and dynamics of the inner Galactic interstellar medium

Author

Schuller, F., primary, Csengeri, T., additional, Urquhart, J. S., additional, Duarte-Cabral, A., additional, Barnes, P. J., additional, Giannetti, A., additional, Hernandez, A. K., additional, Leurini, S., additional, Mattern, M., additional, Medina, S.-N. X., additional, Agurto, C., additional, Azagra, F., additional, Anderson, L. D., additional, Beltrán, M. T., additional, Beuther, H., additional, Bontemps, S., additional, Bronfman, L., additional, Dobbs, C. L., additional, Dumke, M., additional, Finger, R., additional, Ginsburg, A., additional, Gonzalez, E., additional, Henning, T., additional, Kauffmann, J., additional, Mac-Auliffe, F., additional, Menten, K. M., additional, Montenegro-Montes, F. M., additional, Moore, T. J. T., additional, Muller, E., additional, Parra, R., additional, Perez-Beaupuits, J.-P., additional, Pettitt, A., additional, Russeil, D., additional, Sánchez-Monge, Á., additional, Schilke, P., additional, Schisano, E., additional, Suri, S., additional, Testi, L., additional, Torstensson, K., additional, Venegas, P., additional, Wang, K., additional, Wienen, M., additional, Wyrowski, F., additional, and Zavagno, A., additional

Published
2017
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46. OH+and H2O+absorption toward PKS 1830–211

Author

Muller, S., primary, Müller, H. S. P., additional, Black, J. H., additional, Beelen, A., additional, Combes, F., additional, Curran, S., additional, Gérin, M., additional, Guélin, M., additional, Henkel, C., additional, Martín, S., additional, Aalto, S., additional, Falgarone, E., additional, Menten, K. M., additional, Schilke, P., additional, Wiklind, T., additional, and Zwaan, M. A., additional

Published
2016
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47. Tracing extended low-velocity shocks through SiO emission

Author

Louvet, F., primary, Motte, F., additional, Gusdorf, A., additional, Nguyên Luong, Q., additional, Lesaffre, P., additional, Duarte-Cabral, A., additional, Maury, A., additional, Schneider, N., additional, Hill, T., additional, Schilke, P., additional, and Gueth, F., additional

Published
2016
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49. Hi-GAL, theHerschelinfrared Galactic Plane Survey: photometric maps and compact source catalogues

Author

Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega-Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., Benedettini, M., Calzoletti, L., Faustini, F., Natoli, P., Piacentini, F., Merello, M., Palmese, A., Del Grande, R., Polychroni, D., Rygl, K. L. J., Polenta, G., Barlow, M. J., Bernard, J.-P., Martin, P. G., Testi, L., Ali, B., André, P., Beltrán, M. T., Billot, N., Carey, S., Cesaroni, R., Compiègne, M., Eden, D., Fukui, Y., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Lim, T. L., Lord, S. D., Martinavarro-Armengol, S., Motte, F., Paladini, R., Paradis, D., Peretto, N., Robitaille, T., Schilke, P., Schneider, N., Schulz, B., Sibthorpe, B., Strafella, F., Thompson, M. A., Umana, G., Ward-Thompson, Derek, Wyrowski, F., Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega-Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., Benedettini, M., Calzoletti, L., Faustini, F., Natoli, P., Piacentini, F., Merello, M., Palmese, A., Del Grande, R., Polychroni, D., Rygl, K. L. J., Polenta, G., Barlow, M. J., Bernard, J.-P., Martin, P. G., Testi, L., Ali, B., André, P., Beltrán, M. T., Billot, N., Carey, S., Cesaroni, R., Compiègne, M., Eden, D., Fukui, Y., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Lim, T. L., Lord, S. D., Martinavarro-Armengol, S., Motte, F., Paladini, R., Paradis, D., Peretto, N., Robitaille, T., Schilke, P., Schneider, N., Schulz, B., Sibthorpe, B., Strafella, F., Thompson, M. A., Umana, G., Ward-Thompson, Derek, and Wyrowski, F.

Abstract

Aims. We present the first public release of high-quality data products (DR1) from Hi-GAL, the Herschel infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic plane surveys from the near-IR to the radio and covers five wavebands at 70, 160, 250, 350 and 500 µm, encompassing the peak of the spectral energy distribution of cold dust for 8 < T < 50 K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68◦ > t > −70◦ in a |b| ≤ 1◦ latitude strip. ∼ ∼ ∼ ∼ Methods. Photometric maps have been produced with the ROMAGAL pipeline, which optimally capitalizes on the excellent sensitivity and stability of the bolometer arrays of the Herschel PACS and SPIRE photometric cameras. It delivers images of exquisite quality and dynamical range, absolutely calibrated with Planck and IRAS, and recovers extended emission at all wavelengths and all spatial scales, from the point-spread function to the size of an entire 2◦ × 2◦ “tile” that is the unit observing block of the survey. The compact source catalogues were generated with the CuTEx algorithm, which was specifically developed to optimise source detection and extraction in the extreme conditions of intense and spatially varying background that are found in the Galactic plane in the thermal infrared. Results. Hi-GAL DR1 images are cirrus noise limited and reach the 1σ-rms predicted by the Herschel Time Estimators for parallel-mode obser- vations at 6011 s−1 scanning speed in relatively low cirrus emission regions. Hi-GAL DR1 images will be accessible through a dedicated web-based image cutout service. The DR1 Compact Source Catalogues are delivered as single-band photometric lists containing, in addition to source posi- tion, peak, and integrated flux and source sizes, a variety of parameters useful to assess the quality and reliability of the extracted sources. Caveats and hints to help in this assessment are provided. Flux completeness limits in all bands are determined

Published
2016

50. Continuum radiative transfer Modeling of Sagittarius B2

Author

Simon, Robert, Schaaf, Reinhold, Stutzki, Jürgen, Schmiedeke, A., Schilke, P., Möller, Th., Sánchez-Monge, Á., Bergin, E., Comito, C., Csengeri, T., Lis, D. C., Molinari, S., Qin, S. L., Rolffs, R., Simon, Robert, Schaaf, Reinhold, Stutzki, Jürgen, Schmiedeke, A., Schilke, P., Möller, Th., Sánchez-Monge, Á., Bergin, E., Comito, C., Csengeri, T., Lis, D. C., Molinari, S., Qin, S. L., and Rolffs, R.

Abstract

We present results from radiative transfer modeling of the continuum emission towards Sagittarius B2 (hereafter Sgr B2). We have developed a radiative transfer framework – Pandora – that employs RADMC-3D (Dullemond 2012) for a self-consistent determination of the dust temperature. With this pipeline, we have set-up a single model that consistently reproduces the thermal dust and free-free continuum emission of Sgr B2 spanning four orders of magnitude in spatial scales (0.02–45 pc) and two orders of magnitude in frequency (20–4000 GHz).

Published
2016

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