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2. Kinematics and stability of high-mass protostellar disk candidates at sub-arcsecond resolution -- Insights from the IRAM NOEMA large program CORE

Author

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

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The fragmentation mode of high-mass molecular clumps and the accretion processes that form the most massive stars ($M\gtrsim 8M_\odot$) are still not well understood. To this end, we have undertaken a large observational program (CORE) making use of interferometric observations from the Northern Extended Millimetre Array (NOEMA) for a sample of 20 luminous ($L>10^4L_\odot$) protostellar objects in the 1.37 mm wavelength regime in both continuum and line emission, reaching $\sim$0.4" resolution (800 au at 2 kpc). Using the dense gas tracer CH$_3$CN, we find velocity gradients across 13 cores perpendicular to the directions of bipolar molecular outflows, making them excellent disk candidates. Specific angular momentum ($j$) radial profiles are on average $\sim10^{-3}$ km /s pc and follow $j \propto r^{1.7}$, consistent with a poorly resolved rotating and infalling envelope/disk model. Fitting the velocity profiles with a Keplerian model, we find protostellar masses in the range of $\sim 10-25$ $M_\odot$. Modelling the level population of CH$_3$CN lines, we present temperature maps and find median gas temperatures in the range $70-210$ K. We create Toomre $Q$ maps to study the stability of the disks and find almost all (11 of 13) disk candidates to be prone to fragmentation due to gravitational instabilities at the scales probed by our observations. In particular, disks with masses greater than $\sim10-20\%$ of the mass of their host (proto)stars are Toomre unstable, and more luminous protostellar objects tend to have disks that are more massive and hence more prone to fragmentation. Our finings show that most disks around high-mass protostars are prone to disk fragmentation early in their formation due to their high disk to stellar mass ratio. This impacts the accretion evolution of high-mass protostars which will have significant implications for the formation of the most massive stars., 27 pages, 12 figures, 6 appendices - accepted for publication in Astronomy and Astrophysics

Published
2023

3. Kinematics and stability of high-mass protostellar disk candidates at sub-arcsecond resolution: Insights from the IRAM NOEMA large programme CORE.

Author

Ahmadi, A., Beuther, H., Bosco, F., Gieser, C., Suri, S., Mottram, J. C., Kuiper, R., Henning, T., Sánchez-Monge, Á., Linz, H., Pudritz, R. E., Semenov, D., Winters, J. M., Möller, T., Beltrán, M. T., Csengeri, T., Galván-Madrid, R., Johnston, K. G., Keto, E., and Klaassen, P. D.

Subjects
CIRCUMSTELLAR matter, HIGH mass stars, STELLAR mass, SUPERGIANT stars, KINEMATICS, PROTOSTARS, PROTOPLANETARY disks
Abstract

Context. The fragmentation mode of high-mass molecular clumps and the accretion processes that form the most massive stars (M ≳ 8 M⊙) are still not well understood. A growing number of case studies have found massive young stellar objects (MYSOs) to harbour disk-like structures, painting a picture that the formation of high-mass stars may proceed through disk accretion, similar to that of lower-mass stars. However, the properties of such structures have yet to be uniformly and systematically characterised. Aims. The aim of this work is to uniformly study the kinematic properties of a large sample of MYSOs and characterise the stability of possible circumstellar disks against gravitational fragmentation. Methods. We have undertaken a large observational programme (CORE) making use of interferometric observations from the Northern Extended Millimetre Array (NOEMA) for a sample of 20 luminous (L > 104L⊙) protostellar objects in the 1.37 mm wavelength regime in both continuum and spectral line emission, reaching 0.4″ resolution (800 au at 2 kpc). Results. We present the gas kinematics of the full sample and detect dense gas emission surrounding 15 regions within the CORE sample. Using the dense gas tracer CH3CN, we find velocity gradients across 13 cores perpendicular to the directions of bipolar molecular outflows, making them excellent disk candidates. The extent of the CH3CN emission tracing the disk candidates varies from 1800 to 8500 au. Analysing the free-fall to rotational timescales, we find that the sources are rotationally supported. The rotation profiles of some disk candidates are well described by differential rotation while for others the profiles are poorly resolved. Fitting the velocity profiles with a Keplerian model, we find protostellar masses in the range of ~ 10–25 M⊙. Modelling the level population of CH3CN (12K–11K) K = 0–6 lines, we present temperature maps and find median temperature in the range 70–210 K with a diversity in distributions. Radial profiles of the specific angular momentum (j) for the best disk candidates span a range of 1–2 orders of magnitude, on average ~10−3 km s−1 pc, and they follow j ∝ r1.7, which is consistent with a poorly resolved rotating and infalling envelope-disk model. Studying the Toomre stability of the disk candidates, we find almost all (11 out of 13) disk candidates to be prone to fragmentation due to gravitational instabilities at the scales probed by our observations, as a result of their high disk to stellar mass ratio. In particular, disks with masses greater than ~ 10–20% of the mass of their host (proto)stars are Toomre unstable, and more luminous YSOs tend to have disks that are more massive compared to their host star and hence more prone to fragmentation. Conclusions. In this work, we show that most disk structures around high-mass YSOs are prone to disk fragmentation early in their formation due to their high disk to stellar mass ratio. This impacts the accretion evolution of high-mass protostars which will have significant implications for the formation of the most massive stars. [ABSTRACT FROM AUTHOR]

Published
2023
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4. Water in star-forming regions: Physics and chemistry from clouds to disks as probed by Herschel spectroscopy

Author

van Dishoeck, E. F., Kristensen, L. E., Mottram, J. C., Benz, A. O., Bergin, E. A., Caselli, P., Herpin, F., Hogerheijde, M. R., Johnstone, D., Liseau, R., NISINI, Brunella, Tafalla, M., van der Tak, F. F. S., Wyrowski, F., Baudry, A., BENEDETTINI, Milena, Bjerkeli, P., Blake, G. A., Braine, J., Bruderer, S., Cabrit, S., Cernicharo, J., Choi, Y., Coutens, A., de Graauw, Th., Dominik, C., FEDELE , DAVIDE, Fich, M., Fuente, A., Furuya, K., Goicoechea, J. R., Harsono, D., Helmich, F. P., Herczeg, G. J., Jacq, T., Karska, A., Kaufman, M., Keto, E., Lamberts, T., Larsson, B., Leurini, Silvia, Lis, D. C., Melnick, G., Neufeld, D., Pagani, L., Persson, M., Shipman, R., TAQUET, VIANNEY DANIEL FRANCOIS, van Kempen, T. A., Walsh, C., Wampfler, S. F., Yıldız, U., WISH Team, Astronomy, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Low Energy Astrophysics (API, FNWI)

Subjects
Protoplanetary disks, 010504 meteorology & atmospheric sciences, 530 Physics, Astrophysics - astrophysics of galaxies, Stars: formation, FOS: Physical sciences, Astrophysics, Astrophysics - Earth and planetary astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Protostar, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, molecules [ISM], Physics::Atmospheric and Oceanic Physics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation), Astrochemistry, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], Infrared: ISM, formation [stars], astrochemistry, jets and outflows [ISM], 520 Astronomy, protoplanetary disks, Water gas, ISM [infrared], Astronomy and Astrophysics, ISM: molecules, ISM: jets and outflows, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Excited state, Outflow, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Water vapor
Abstract

(abridged) Data and results from the WISH key program are summarized, designed to provide a legacy data set to address its physics and chemistry. WISH targeted ~80 sources along the two axes of luminosity and evolutionary stage: from low- to high-mass protostars and from pre-stellar cores to protoplanetary disks. Lines of H2O, HDO, OH, CO and [O I] were observed with the HIFI and PACS instruments, complemented by molecules that probe UV, X-ray or grain chemistry. Most of the far-infrared water emission from protostars is found to be compact, originating from warm outflowing and shocked gas at high density and temperature in at least two physical components. This gas is not probed by low-J CO lines, only by J>14. Water is a significant, but not dominant, coolant. Its abundance is universally low, of order H2O/H2=2E-6, pointing to shock and outflow cavity models that include UV radiation at 100-1000 times the ISRF. In cold quiescent pre-stellar cores and envelopes, the water abundance structure is accurately probed through velocity-resolved line profiles, confirming basic chemistry networks. The gaseous HDO/H2O ratio of 0.025, much higher than that of bulk ice, is representative of the outer photodesorbed ice layers and cold chemistry. Water abundances in the inner hot cores are high, but with variations from 5E-6 to 2E-4. Combined analyses of water gas and ice show that up to 50% of the oxygen budget may be missing, with possible explanations discussed. Water vapor emission from disks is weak, indicating that water ice is locked up in larger pebbles early on and that these pebbles have settled and drifted inward by the Class II stage. Quantitatively, many oceans of water ice are available. Extragalactic low-J H2O emission is mostly compact and collisionally excited. Prospects for future mid- to far-infrared missions are given., 58 pages, 39 figures, accepted for publication in A&A

Published
2021

10. 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

11. The Planck Submillimeter Properties of Galactic High-mass Star-forming Regions: Dust Temperatures, Luminosities, Masses, and Star Formation Efficiency.

Author

Paladini, R., Mottram, J. C., Veneziani, M., Traficante, A., Schisano, E., Giardino, G., Falgarone, E., Urquhart, J. S., Harrison, D. L., Joncas, G., Umana, G., and Molinari, S.

Subjects
*STAR formation, *MOLECULAR clouds, *SPECTRAL energy distribution, *DUST, *LUMINOSITY
Abstract

Massive star formation occurs in the interior of giant molecular clouds and proceeds through many stages. In this work, we focus on massive young stellar objects (MYSOs) and ultracompact H ii regions (UCH ii), where the former are enshrouded in dense envelopes of dust and gas, the latter of which has begun dispersing. By selecting a complete sample of MYSOs and UCH ii from the Red MSX Source (RMS) survey database, we combine Planck and IRAS data and build their spectral energy distributions. With these, we estimate the physical properties (dust temperatures, mass, luminosity) of the sample. Because the RMS database provides unique solar distances, it also allows the instantaneous star formation efficiency (SFE) to be investigated as a function of Galactocentric radius. We find that the SFE increases between 2 and 4.5 kpc, where it reaches a peak, likely in correspondence with the accumulation of molecular material at the end of the Galactic bar. It then stays approximately constant up to 9 kpc, after which it linearly declines, in agreement with predictions from extragalactic studies. This behavior suggests the presence of a significant amount of undetected molecular gas at RG > 8 kpc. Finally, we present diagnostic colors that can be used to identify sites of massive star formation. [ABSTRACT FROM AUTHOR]

Published
2021
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12. Multiwavelength modelling of the circumstellar environment of the massive protostar AFGL 2591 VLA 3.

Author

Olguin, F A, Hoare, M G, Johnston, K G, Motte, F, Chen, H-R V, Beuther, H, Mottram, J C, Ahmadi, A, Gieser, C, Semenov, D, Peters, T, Palau, A, Klaassen, P D, Kuiper, R, Sánchez-Monge, Á, and Henning, Th

Subjects
STELLAR mass, RADIATIVE transfer, PROTOSTARS, DUST, CIRCUMSTELLAR matter, STAR formation
Abstract

We have studied the dust density, temperature, and velocity distributions of the archetypal massive young stellar object (MYSO) AFGL 2591. Given its high luminosity (⁠|$L=2\times 10^5\, \mbox{L$_{\odot}$}$|⁠) and distance (d  = 3.3 kpc), AFGL 2591 has one of the highest |$\sqrt{L}/d$| ratio, giving better resolved dust emission than any other MYSO. As such, this paper provides a template on how to use resolved multiwavelength data and radiative transfer to obtain a well-constrained 2D axisymmetric analytic rotating infall model. We show for the first time that the resolved dust continuum emission from Herschel 70-  μ m observations is extended along the outflow direction, whose origin is explained in part from warm dust in the outflow cavity walls. However, the model can only explain the kinematic features from CH3CN observations with unrealistically low stellar masses (<15 M⊙), indicating that additional physical processes may be playing a role in slowing down the envelope rotation. As part of our three-step continuum and line fitting, we have identified model parameters that can be further constrained by specific observations. High-resolution mm visibilities were fitted to obtain the disc mass (6 M⊙) and radius (2200 au). A combination of SED and near-infrared observations were used to estimate the luminosity and envelope mass together with the outflow cavity inclination and opening angles. [ABSTRACT FROM AUTHOR]

Published
2020
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13. The Hi-GAL compact source catalogue.\ud I. The physical properties of the clumps in the inner\ud Galaxy (−71.0 ◦ < ' < 67.0◦)

Author

Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, Sarah, Jaffa, Sarah, Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmerim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltran, M. T., Billot, N., Cambresy, L., Cesaroni, R., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mege, P., Peretto, Nicolas, Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., and Whitworth, Anthony Peter

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QB
Abstract

Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 μm. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane −71∘.0 < ℓ < 67∘.0. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-μm counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between ‘on-arm’ and ‘interarm’ positions.

Published
2017

14. Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ}< \ell < 67.0^{\circ}$)

Author

Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmerim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltrán, M. T., Billot, N., Cambrésy, L., Cesaroni, R., García-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mège, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Causi, G. Li, Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., and Yamamoto, H.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $\mu$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the portion of Galactic plane $-71.0^{\circ}< \ell < 67.0^{\circ}$. The band-merged catalogue contains 100922 sources with a regular SED, 24584 of which show a 70 $\mu$m counterpart and are thus considered proto-stellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterise different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in proto-stellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to proto-stellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between "on-arm" and "inter-arm" positions., Comment: Accepted by MNRAS

Published
2017

15. Outflows, infall and evolution of a sample of embedded low-mass protostars. The William Herschel Line Legacy (WILL) survey

Author

Mottram, J. C., van Dishoeck, E. F., Kristensen, L. E., Karska, A., San José-García, I., Khanna, S., Herczeg, G. J., Andr, Ph., Bontemps, Sylvain, Cabrit, S., Carney, T., Drozdovskaya, N., Dunham, M., Evans, J., Fedele, D., Green, J. D., Harsono, D., Johnstone, D., Jørgensen, J. K., Könyves, V., Nisini, B., Persson, M. V., Tafalla, M., Visser, R., Yildiz, U. A., Leiden Observatory [Leiden], Universiteit Leiden, Bergen University College, foreign laboratories (FL), CERN [Genève], University of Pennsylvania, FORMATION STELLAIRE 2017, 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Department of Genome Sciences [Seattle] (GS), University of Washington [Seattle], University of Glasgow, Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada, Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Universiteit Leiden [Leiden], University of Pennsylvania [Philadelphia], École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Osservatorio di Astrofisica di Roma (OAR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and École normale supérieure - Paris (ENS Paris)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Accretion rate, 0103 physical sciences, Protostar, Astrophysics::Solar and Stellar Astrophysics, Isotopologue, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Low Mass
Abstract

[Abridged] We present spectroscopic observations in H$_{2}$O, CO and related species with \textit{Herschel} HIFI and PACS, as well as ground-based follow-up with the JCMT and APEX in CO, HCO$^{+}$ and isotopologues, of a sample of 49 nearby ($d, Comment: Accepted to A&A, version after language editor corrections. 47 pages, 18 figures, 15 tables. The figures have been converted to pdf due to file-size considerations, which may lead to some degradation

Published
2017

16. The Hi-GAL compact source catalogue - I. The physical properties of the clumps in the inner Galaxy (-71.0° < ℓ < 67.0°)

Author

ELIA, Davide Quintino, MOLINARI, Sergio, SCHISANO, EUGENIO, Pestalozzi, M., PEZZUTO, Stefano, Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., BENEDETTINI, Milena, Bernard, J. P., DI GIORGIO, Anna Maria, Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., OLMI, LUCA, Schneider, N., TESTI, Leonardo, Wyrowski, F., Zavagno, A., Calzoletti, L., FAUSTINI, Fabiana, Natoli, P., Palmeirim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltrán, M. T., Billot, N., Cambrésy, L., CESARONI, Riccardo, García-Lario, P., Hoare, M. G., Huang, M., Joncas, G., LIU, Scige' John, Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mège, P., Peretto, N., RYGL, Kazi Lucie Jessica, Schilke, P., Thompson, M. A., TRAFICANTE, ALESSIO, UMANA, Grazia Maria Gloria, Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., BECCIANI, Ugo, BRESCIA, Massimo, BUEMI, CARLA SIMONA, BUFANO, FILOMENA, Butora, Robert, CAVUOTI, STEFANO, COSTA, Alessandro, Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., LETO, PAOLO, LI CAUSI, Gianluca, MARCHILI, Nicola, Martinavarro-Armengol, S., MERCURIO, AMATA, MOLINARO, Marco, RICCIO, GIUSEPPE, Sano, H., SCIACCA, Eva, Tachihara, K., Torii, K., TRIGILIO, CORRADO, VITELLO, FABIO ROBERTO, Yamamoto, H., ITA, GBR, FRA, DEU, BEL, and HUN

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

https://www.media.inaf.it/2017/07/27/herschel-la-carica-dei-101mila/ Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 μm. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane -71.0° < ℓ < 67.0°. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-μm counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between 'on-arm' and 'interarm' positions.

Published
2017

17. The Hi‐GAL compact source catalogue ‐ I. The physical properties of the clumps in the inner Galaxy (‐71.degrees 0 < l < 67.degrees 0)

Author

Elia, Davide, Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega‐Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Galaxy Astrophysics
Abstract

International audience; Hi‐GAL (Herschel InfraRed Galactic Plane Survey) is a large‐scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 mu m. We present a band‐merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane ‐71.degrees 0 < l < 67.degrees 0. The band‐merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70‐mu m counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre‐stellar ones. The surface density of sources follows an increasing trend as they evolve from pre‐stellar to protostellar, but then it is found to decrease again in themajority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between `on‐arm' and `interarm' positions.

Published
2017

18. The Hi-GAL compact source catalogue I. The physical properties of the clumps in the inner Galaxy (-71. < l < 67 )

Author

Elia, Davide, Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, Ruggero, Strafella, F., Benedettini, MARIA GILDA, Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmeirim, P., Piacentini, Francesco, Piazzo, Lorenzo, Pilbratt, G. L., Polychroni, D., Baldeschi, Adriano, Beltrã¡n, M. T., Billot, N., Cambrã©sy, L., Cesaroni, R., Garcã­a lario, P., Hoare, M. G., Huang, Meiling, Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mãge, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, Marcella, Ward thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, Eleonora, Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Li Causi, G., Marchili, N., Martinavarro armengol, S., Mercurio, A., Molinaro, Mario, Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., and Yamamoto, H.

Subjects
Infrared: ISM, extinction, Space and Planetary Science, Dust, Astronomy and Astrophysics, Catalogues, Dust, extinction, ISM: clouds, Local interstellar matter, Submillimetre: ISM
Published
2017

19. Carina's pillars of destruction: the view from ALMA.

Author

Klaassen, P D, Reiter, M R, McLeod, A F, Mottram, J C, Dale, J E, and Gritschneder, M

Subjects
PROTOSTARS, IONIZING radiation, KINEMATICS
Abstract

Forming high-mass stars have a significant effect on their natal environment. Their feedback pathways, including winds, outflows, and ionizing radiation, shape the evolution of their surroundings which impacts the formation of the next generation of stars. They create or reveal dense pillars of gas and dust towards the edges of the cavities they clear. They are modelled in feedback simulations, and the sizes and shapes of the pillars produced are consistent with those observed. However, these models predict measurably different kinematics which provides testable discriminants. Here we present the first ALMA Compact Array (ACA) survey of 13 pillars in Carina, observed in 12CO, 13CO, and C18O J = 2–1, and the 230 GHz continuum. The pillars in this survey were chosen to cover a wide range in properties relating to the amount and direction of incident radiation, proximity to nearby irradiating clusters and cloud rims, and whether they are detached from the cloud. With these data, we are able to discriminate between models. We generally find pillar velocity dispersions of <1 km s−1 and that the outer few layers of molecular emission in these pillars show no significant offsets from each other, suggesting little bulk internal motions within the pillars. There are instances where the pillars are offset in velocity from their parental cloud rim, and some with no offset, hinting at a stochastic development of these motions. [ABSTRACT FROM AUTHOR]

Published
2020
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20. Chemical complexity in high-mass star formation: An observational and modeling case study of the AFGL 2591 VLA 3 hot core.

Author

Gieser, C., Semenov, D., Beuther, H., Ahmadi, A., Mottram, J. C., Henning, Th., Beltran, M., Maud, L. T., Bosco, F., Leurini, S., Peters, T., Klaassen, P., Kuiper, R., Feng, S., Urquhart, J. S., Moscadelli, L., Csengeri, T., Lumsden, S., Winters, J. M., and Suri, S.

Subjects
STAR formation, PROTOSTARS, ASTROCHEMISTRY, ANALYTICAL chemistry, CHEMICAL models, CHEMICAL structure, TEMPERATURE distribution
Abstract

Aims. In order to understand the observed molecular diversity in high-mass star-forming regions, we have to determine the underlying physical and chemical structure of those regions at high angular resolution and over a range of evolutionary stages. Methods. We present a detailed observational and modeling study of the hot core VLA 3 in the high-mass star-forming region AFGL 2591, which is a target region of the NOrthern Extended Millimeter Array (NOEMA) large program CORE. Using NOEMA observations at 1.37 mm with an angular resolution of ~0″. 42 (1400 au at 3.33 kpc), we derived the physical and chemical structure of the source. We modeled the observed molecular abundances with the chemical evolution code MUSCLE (MUlti Stage ChemicaL codE). Results. With the kinetic temperature tracers CH3CN and H2CO we observe a temperature distribution with a power-law index of q = 0.41 ± 0.08. Using the visibilities of the continuum emission we derive a density structure with a power-law index of p = 1.7 ± 0.1. The hot core spectra reveal high molecular abundances and a rich diversity in complex molecules. The majority of the molecules have an asymmetric spatial distribution around the forming protostar(s), which indicates a complex physical structure on scales <1400 au. Using MUSCLE, we are able to explain the observed molecular abundance of 10 out of 14 modeled species at an estimated hot core chemical age of ~21 100 yr. In contrast to the observational analysis, our chemical modeling predicts a lower density power-law index of p < 1.4. Reasons for this discrepancy are discussed. Conclusions. Combining high spatial resolution observations with detailed chemical modeling allows us to derive a concise picture of the physical and chemical structure of the famous AFGL 2591 hot core. The next steps are to conduct a similar analysis for the whole CORE sample, and then use this analysis to constrain the chemical diversity in high-mass star formation to a much greater depth. [ABSTRACT FROM AUTHOR]

Published
2019
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21. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues First data release for the inner Milky Way:+68 degrees \textgreater= l \textgreater=-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, Annie, 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., RYG, K. L. J., POLENTA, G., BARLOW, M. J., BERNARD, J. -P., MARTIN, P. G., TESTI, L., ALI, B., ANDRÉ, P., BELTRAN, 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, . 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., WYROWSKI, F., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Faculty of Informatics [Lugano], Università della Svizzera italiana = University of Italian Switzerland (USI), Space Telescope Science Institute (STSci), Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Department of Physics and Astronomy [Calgary], University of Calgary, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), École Nationale Supérieure d’Agronomie [Alger] (ENSA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysics [Nagoya], Nagoya University, ISO Data Centre (ESA - Espagne), Herschel Science Centre (ESA Espagne), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, University Hospital of Cologne [Cologne], FORMATION STELLAIRE 2016, 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), SRON Netherlands Institute for Space Research (SRON), AUTRES, Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Max-Planck-Institut für Radioastronomie (MPIFR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), European Space Agency (ESA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universität zu Köln, Università della Svizzera italiana (USI), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; 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 mu m, encompassing the peak of the spectral energy distribution of cold dust for 8 less than or similar to T less than or similar to 50 K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68 degrees greater than or similar to l greater than or similar to -70 degrees in a vertical bar b vertical bar \textless= 1 degrees 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 degrees x 2 degrees “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 1 sigma-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

32. Water in star-forming regions with Herschel(WISH)

Author

Benz, A. O., Bruderer, S., van Dishoeck, E. F., Melchior, M., Wampfler, S. F., van der Tak, F., Goicoechea, J. R., Indriolo, N., Kristensen, L. E., Lis, D. C., Mottram, J. C., Bergin, E. A., Caselli, P., Herpin, F., Hogerheijde, M. R., Johnstone, D., Liseau, R., Nisini, B., Tafalla, M., Visser, R., and Wyrowski, F.

Subjects
ISM ultraviolet, ISM molecules, Massive stars, Astrophysics::High Energy Astrophysical Phenomena, Star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Low-mass stars, Astrophysics::Galaxy Astrophysics, Astrochemistry
Abstract

CONTEXT: Hydrides are simple compounds containing one or a few hydrogen atoms bonded to a heavier atom. They are fundamental precursor molecules in cosmic chemistry and many hydride ions have become observable in high quality for the first time thanks to the Herschel Space Observatory. Ionized hydrides such as CH⁺ and OH⁺ (and also HCO⁺), which affect the chemistry of molecules such as water, provide complementary information on irradiation by far-UV (FUV) or X-rays and gas temperature. AIMS: We explore hydrides of the most abundant heavier elements in an observational survey covering young stellar objects (YSOs) with different mass and evolutionary state. The focus is on hydrides associated with the dense protostellar envelope and outflows, contrary to previous work that focused on hydrides in diffuse foreground clouds. METHODS: Twelve YSOs were observed with HIFI on Herschel in six spectral settings providing fully velocity-resolved line profiles as part of the Water in star-forming regions with Herschel (WISH) program. The YSOs include objects of low (Class 0 and I), intermediate, and high mass, with luminosities ranging from 4 L⊙ to 2 × 105 L⊙. RESULTS: The targeted lines of CH⁺, OH⁺, H₂O⁺+, C⁺, and CH are detected mostly in blue-shifted absorption. H₃O⁺ and SH⁺ are detected in emission and only toward some high-mass objects. The observed line parameters and correlations suggest two different origins related to gas entrained by the outflows and to the circumstellar envelope. The derived column densities correlate with bolometric luminosity and envelope mass for all molecules, best for CH, CH⁺, and HCO⁺. The column density ratios of CH⁺/OH⁺ are estimated from chemical slab models, assuming that the H₂ density is given by the specific density model of each object at the beam radius. For the low-mass YSOs the observed ratio can be reproduced for an FUV flux of 2–400 times the interstellar radiation field (ISRF) at the location of the molecules. In two high-mass objects, the UV flux is 20–200 times the ISRF derived from absorption lines, and 300–600 ISRF using emission lines. Upper limits for the X-ray luminosity can be derived from H₃O⁺ observations for some low-mass objects. CONCLUSIONS: If the FUV flux required for low-mass objects originates at the central protostar, a substantial FUV luminosity, up to 1.5 L⊙, is required. There is no molecular evidence for X-ray induced chemistry in the low-mass objects on the observed scales of a few 1000 AU. For high-mass regions, the FUV flux required to produce the observed molecular ratios is smaller than the unattenuated flux expected from the central object(s) at the Herschel beam radius. This is consistent with an FUV flux reduced by circumstellar extinction or by bloating of the protostar.

Published
2016

33. CHIMPS: the13CO/C18O (J = 3 ? 2) Heterodyne Inner Milky Way Plane Survey

Author

Rigby, A. J., Moore, T. J. T., Plume, R., Eden, D. J., Urquhart, J. S., Thompson, M. A., Mottram, J. C., Brunt, C. M., Butner, H. M., Dempsey, J. T., Gibson, S. J., Hatchell, J., Jenness, T., Kuno, N., Longmore, S. N., Morgan, L. K., Polychroni, D., Thomas, H., White, G. J., and Zhu, M.

Subjects
QB460, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present the 13CO/C18O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey (CHIMPS) which has been carried out using the Heterodyne Array Receiver Program on the 15 m James Clerk Maxwell Telescope (JCMT) in Hawaii. The high-resolution spectral survey currently covers |b| ≤ 0.5° and 28° ≲ l ≲ 46°, with an angular resolution of 15 arcsec in 0.5 km s-1 velocity channels. The spectra have a median rms of ˜0.6 K at this resolution, and for optically thin gas at an excitation temperature of 10 K, this sensitivity corresponds to column densities of NH2 ˜ 3 × 1020 cm-2 and NH2 ˜ 4 × 1021 cm-2 for 13CO and C18O, respectively. The molecular gas that CHIMPS traces is at higher column densities and is also more optically thin than in other publicly available CO surveys due to its rarer isotopologues, and thus more representative of the three-dimensional structure of the clouds. The critical density of the J = 3 → 2 transition of CO is ≳104 cm-3 at temperatures of ≤20 K, and so the higher density gas associated with star formation is well traced. These data complement other existing Galactic plane surveys, especially the JCMT Galactic Plane Survey which has similar spatial resolution and column density sensitivity, and the Herschel infrared Galactic Plane Survey. In this paper, we discuss the observations, data reduction and characteristics of the survey, presenting integrated-emission maps for the region covered. Position-velocity diagrams allow comparison with Galactic structure models of the Milky Way, and while we find good agreement with a particular four-arm model, there are some significant deviations.

Published
2016

34. 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

35. Linking low- to high-mass YSOs with Herschel-HIFI observations of water

Author

Jose-Garcia, I. San, Mottram, J. C., van Dishoeck, E. F., Kristensen, L. E., van der Tak, F. F. S., Braine, J., Herpin, F., Johnstone, D., van Kempen, T. A., Wyrowski, F., Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Max-Planck-Institut für Extraterrestrische Physik (MPE), Danish Meat Research Institute (DMRI), SRON Netherlands Institute for Space Research (SRON), FORMATION STELLAIRE 2016, 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), Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada, Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, foreign laboratories (FL), and CERN [Genève]

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Water probes the dynamics in young stellar objects (YSOs) effectively, especially shocks in molecular outflows. It is a key molecule for exploring whether the physical properties of low-mass protostars can be extrapolated to massive YSOs. As part of the WISH key programme, we investigate the dynamics and the excitation conditions of shocks along the outflow cavity wall as function of source luminosity. Velocity-resolved Herschel-HIFI spectra of the H2O 988, 752, 1097 GHz and 12CO J=10-9, 16-15 lines were analysed for 52 YSOs with bolometric luminosities (L_bol) ranging from 10^5 L_sun. The profiles of the H2O lines are similar, indicating that they probe the same gas. We see two main Gaussian emission components in all YSOs: a broad component associated with non-dissociative shocks in the outflow cavity wall (cavity shocks) and a narrow component associated with quiescent envelope material. More than 60% of the total integrated intensity of the H2O lines (L_H2O) comes from the cavity shock component. The H2O line widths are similar for all YSOs, whereas those of 12CO 10-9 increase slightly with L_bol. The excitation analysis of the cavity shock component, performed with the non-LTE radiative transfer code RADEX, shows stronger 752 GHz emission for high-mass YSOs, likely due to pumping by an infrared radiation field. As previously found for CO, a strong correlation with slope unity is measured between log(L_H2O) and log(L_bol), which can be extrapolated to extragalactic sources. We conclude that the broad component of H2O and high-J CO lines originate in shocks in the outflow cavity walls for all YSOs, whereas lower-J CO transitions mostly trace entrained outflow gas. The higher UV field and turbulent motions in high-mass objects compared to their low-mass counterparts may explain the slightly different kinematical properties of 12CO 10-9 and H2O lines from low- to high-mass YSOs., Abridged abstract, 31 pages, 18 figures, 12 tables, accepted in Astronomy & Astrophysics

Published
2016

36. Erratum to: Guidelines for the use and interpretation of assays for monitoring autophagy (3rd edition) (Autophagy, 12, 1, 1-222, 10.1080/15548627.2015.1100356

Author

Klionsky, D. J., Abdelmohsen, K., Abe, A., Abedin, M. J., Abeliovich, H., Arozena, A. A., Adachi, H., Adams, C. M., Adams, P. D., Adeli, K., Adhihetty, P. J., Adler, S. G., Agam, G., Agarwal, R., Aghi, M. K., Agnello, M., Agostinis, P., Aguilar, P. V., Aguirre-Ghiso, J., Airoldi, E. M., Ait-Si-Ali, S., Akematsu, T., Akporiaye, E. T., Al-Rubeai, M., Albaiceta, G. M., Albanese, C., Albani, D., Albert, M. L., Aldudo, J., Algül, H., Alirezaei, M., Alloza, I., Almasan, A., Almonte-Beceril, M., Alnemri, E. S., Alonso, C., Altan-Bonnet, N., Altieri, D. C., Alvarez, S., Alvarez-Erviti, L., Alves, S., Amadoro, G., Amano, A., Amantini, C., Ambrosio, S., Amelio, I., Amer, A. O., Amessou, M., Amon, A., An, Z., Anania, F. A., Andersen, S. U., Andley, U. P., Andreadi, C. K., Andrieu-Abadie, N., Anel, A., Ann, D. K., Anoopkumar-Dukie, S., Antonioli, M., Aoki, H., Apostolova, N., Aquila, S., Aquilano, K., Araki, K., Arama, E., Aranda, A., Araya, J., Arcaro, A., Arias, E., Arimoto, H., Ariosa, A. R., Armstrong, J. L., Arnould, T., Arsov, I., Asanuma, K., Askanas, V., Asselin, E., Atarashi, R., Atherton, S. S., Atkin, J. D., Attardi, L. D., Auberger, P., Auburger, G., Aurelian, L., Autelli, R., Avagliano, L., Avantaggiati, M. L., Avrahami, L., Azad, N., Awale, S., Bachetti, T., Backer, J. M., Bae, D. -H., Bae, J. -S., Bae, O. -N., Bae, S. H., Baehrecke, E. H., Baek, S. -H., Baghdiguian, S., Bagniewska-Zadworna, A., Bai, H., Bai, J., Bai, X. -Y., Bailly, Y., Balaji, K. N., Balduini, W., Ballabio, A., Balzan, R., Banerjee, R., Bánhegyi, G., Bao, H., Barbeau, B., Barrachina, M. D., Barreiro, E., Bartel, B., Bartolomé, A., Bassham, D. C., Bassi, M. T., Bast, R. C., J, R., Basu, A., Batista, M. T., Batoko, H., Battino, M., Bauckman, K., Baumgarner, B. L., Bayer, K. U., Beale, R., Beaulieu, J. -F., Beck, G. R., Becker, C., Beckham, J. D., Bédard, P. -A., Bednarski, P. J., Begley, T. J., Behl, C., Behrends, C., Behrens, G. M. N., Behrns, K. E., Bejarano, E., Belaid, A., Belleudi, F., Bénard, G., Berchem, G., Bergamaschi, D., Bergami, M., Berkhout, B., Berliocchi, L., Bernard, A., Bernard, M., Bernassola, F., Bertolotti, A., Bess, A. S., Besteiro, S., Bettuzzi, S., Bhalla, S., Bhattacharyya, S., Bhutia, S. K., Biagosch, C., Bianchi, M. W., Biard-Piechaczyk, M., Billes, V., Bincoletto, C., Bingol, B., Bird, S. W., Bitoun, M., Bjedov, I., Blackstone, C., Blanc, L., Blanco, G. A., Blomhoff, H. K., Boada-Romero, E., Böckler, S., Boes, M., Boesze-Battaglia, K., Boise, L. H., Bolino, A., Boman, A., Bonaldo, P., Bordi, M., Bosch, J., Botana, L. M., Botti, J., Bou, G., Bouché, M., Bouchecareilh, M., Boucher, M. -J., Boulton, M. E., Bouret, S. G., Boya, P., Boyer-Guittaut, M., Bozhkov, P. V., Brady, N., Braga, V. M. M., Brancolini, C., Braus, G. H., Bravo-San-Pedro, J. M., Brennan, L. A., Bresnick, E. H., Brest, P., Bridges, D., Bringer, M. -A., Brini, M., Brito, G. C., Brodin, B., Brookes, P. S., Brown, E. J., Brown, K., Broxmeyer, H. E., Bruhat, A., Brum, P. C., Brumell, J. H., Brunetti-Pierri, N., Bryson-Richardson, R. J., Buch, S., Buchan, A. M., Budak, H., Bulavin, D. V., Bultman, S. J., Bultynck, G., Bumbasirevic, V., Burelle, Y., Burke, R. E., Burmeister, M., Bütikofer, P., Caberlotto, L., Cadwell, K., Cahova, M., Cai, D., Cai, J., Cai, Q., Calatayud, S., Camougrand, N., Campanella, M., Campbell, G. R., Campbell, M., Campello, S., Candau, R., Caniggia, I., Cantoni, L., Cao, L., Caplan, A. B., Caraglia, M., Cardinali, C., Cardoso, S. M., Carew, J. S., Carleton, L. A., Carlin, C. R., Carloni, S., Carlsson, S. R., Carmona-Gutierrez, D., Carneiro, L. A. M., Carnevali, O., Carra, S., Carrier, A., Carroll, B., Casas, C., Casas, J., Cassinelli, G., Castets, P., Castro-Obregon, S., Cavallini, G., Ceccherini, I., Cecconi, F., Cederbaum, A. I., Ceña, V., Cenci, S., Cerella, C., Cervia, D., Cetrullo, S., Chaachouay, H., Chae, H. -J., Chagin, A. S., Chai, C. -Y., Chakrabarti, G., Chamilos, G., Chan, E. Y. W., Chan, M. T. V., Chandra, D., Chandra, P., Chang, C. -P., Chang, R. C. -C., Chang, T. Y., Chatham, J. C., Chatterjee, S., Chauhan, S., Che, Y., Cheetham, M. E., Cheluvappa, R., Chen, C. -J., Chen, G., Chen, G. -C., Chen, H., Chen, J. W., Chen, J. -K., Chen, M., Chen, P., Chen, Q., Chen, S. -D., Chen, S., Chen, S. S. -L., Chen, W., Chen, W. -J., Chen, W. Q., Chen, X., Chen, Y. -H., Chen, Y. -G., Chen, Y., Chen, Y. -J., Chen, Y. -Q., Chen, Z., Cheng, A., Cheng, C. H. K., Cheng, H., Cheong, H., Cherry, S., Chesney, J., Cheung, C. H. A., Chevet, E., Chi, H. C., Chi, S. -G., Chiacchiera, F., Chiang, H. -L., Chiarelli, R., Chiariello, M., Chieppa, M., Chin, L. -S., Chiong, M., Chiu, G. N. C., Cho, D. -H., Cho, S. -G., Cho, W. C., Cho, Y. -Y., Cho, Y. -S., Choi, A. M. K., Choi, E. -J., Choi, E. -K., Choi, J., Choi, M. E., Choi, S. -I., Chou, T. -F., Chouaib, S., Choubey, D., Choubey, V., Chow, K. -C., Chowdhury, K., Chu, C. T., Chuang, T. -H., Chun, T., Chung, H., Chung, T., Chung, Y. -L., Chwae, Y. -J., Cianfanelli, V., Ciarcia, R., Ciechomska, I. A., Ciriolo, M. R., Cirone, M., Claerhout, S., Clague, M. J., Cl� ria, J., Clarke, P. G. H., Clarke, R., Clementi, E., Cleyrat, C., Cnop, M., Coccia, E. M., Cocco, T., Codogno, P., Coers, J., Cohen, E. E. W., Colecchia, D., Coletto, L., Coll, N. S., Colucci-Guyon, E., Comincini, S., Condello, M., Cook, K. L., Coombs, G. H., Cooper, C. D., Cooper, J. M., Coppens, I., Corasaniti, M. T., Corazzari, M., Corbalan, R., Corcelle-Termeau, E., Cordero, M. D., Corral-Ramos, C., Corti, O., Cossarizza, A., Costelli, P., Costes, S., Cotman, S. L., Coto-Montes, A., Cottet, S., Couve, E., Covey, L. R., Cowart, L. A., Cox, J. S., Coxon, F. P., Coyne, C. B., Cragg, M. S., Craven, R. J., Crepaldi, T., Crespo, J. L., Criollo, A., Crippa, V., Cruz, M. T., Cuervo, A. M., Cuezva, J. M., Cui, T., Cutillas, P. R., Czaja, M. J., Czyzyk-Krzeska, M. F., Dagda, R. K., Dahmen, U., Dai, C., Dai, W., Dai, Y., Dalby, K. N., Valle, L. D., Dalmasso, G., D'Amelio, M., Damme, M., Darfeuille-Michaud, A., Dargemont, C., Darley-Usmar, V. M., Dasarathy, S., Dasgupta, B., Dash, S., Dass, C. R., Davey, H. M., Davids, L. M., Dávila, D., Davis, R. J., Dawson, T. M., Dawson, V. L., Daza, P., de Belleroche, J., de Figueiredo, P., de Figueiredo, R. C. B. Q., de la Fuente, J., De Martino, L., De Matteis, A., De Meyer, G. R. Y., De Milito, A., De Santi, M., de Souza, W., De Tata, V., De Zio, D., Debnath, J., Dechant, R., Decuypere, J. -P., Deegan, S., Dehay, B., Del Bello, B., Del Re, D. P., Delage-Mourroux, R., Delbridge, L. M. D., Deldicque, L., Delorme-Axford, E., Deng, Y., Dengjel, J., Denizot, M., Dent, P., Der, C. J., Deretic, V., Derrien, B., Deutsch, E., Devarenne, T. P., Devenish, R. J., Di Bartolomeo, S., Di Daniele, N., Di Domenico, F., Di Nardo, A., Di Paola, S., Di Pietro, A., Di Renzo, L., Di Antonio, A., Díaz-Araya, G., Díaz-Laviada, I., Diaz-Meco, M. T., Diaz-Nido, J., Dickey, C. A., Dickson, R. C., Diederich, M., Digard, P., Dikic, I., Dinesh-Kumar, S. P., Ding, C., Ding, W. -X., Ding, Z., Dini, L., Distler, J. H. W., Diwan, A., Djavaheri-Mergny, M., Dmytruk, K., Dobson, R. C. J., Doetsch, V., Dokladny, K., Dokudovskaya, S., Donadelli, M., Dong, X. C., Dong, X., Dong, Z., Donohue, T. M., Donohue-Jr, T. M., Doran, K. S., D'Orazi, G., Dorn, G. W., Dosenko, V., Dridi, S., Drucker, L., Du, J., L. -L., Du, Du, L., du Toit, A., Dua, P., Duan, L., Duann, P., Dubey, V. K., Duchen, M. R., Duchosal, M. A., Duez, H., Dugail, I., Dumit, V. I., Duncan, M. C., Dunlop, E. A., Dunn, W. A., Dupont, N., Dupuis, L., Durán, R. V., Durcan, T. M., Duvezin-Caubet, S., Duvvuri, U., Eapen, V., Ebrahimi-Fakhari, D., Echard, A., Eckhart, L., Edelstein, C. L., Edinger, A. L., Eichinger, L., Eisenberg, T., Eisenberg-Lerner, A., Eissa, N. T., El-Deiry, W. S., El-Khoury, V., Elazar, Z., Eldar-Finkelman, H., Elliott, C. J. H., Emanuele, E., Emmenegger, U., Engedal, N., Engelbrecht, A. -M., Engelender, S., Enserink, J. M., Erdmann, R., Erenpreisa, J., Eri, R., Eriksen, J. L., Erman, A., Escalante, R., Eskelinen, E. -L., Espert, L., Esteban-Martínez, L., Evans, T. J., Fabri, M., Fabrias, G., Fabrizi, C., Facchiano, A., Færgeman, N. J., Faggioni, A., Fairlie, W. D., Fan, C., Fan, D., Fan, J., Fang, S., Fanto, M., Fanzani, A., Farkas, T., Faure, M., Favier, F. B., Fearnhead, H., Federici, M., Fei, E., Felizardo, T. C., Feng, H., Feng, Y., Ferguson, T. A., Fernández, Á. F., Fernandez-Barrena, M. G., Fernandez-Checa, J. C., Fernández-López, A., Fernandez-Zapico, M. E., Feron, O., Ferraro, E., Ferreira-Halder, C. V., Fesus, L., Feuer, R., Fiesel, F. C., Filippi-Chiela, E. C., Filomeni, G., Fimia, G. M., Fingert, J. 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Robin, Higaki, Katsumi, Hilfiker, Sabine, Hill, Bradford G., Hill, Joseph A., Hill, William D., Hino, Keisuke, Hofius, Daniel, Hofman, Paul, Höglinger, Günter U., Höhfeld, Jörg, Holz, Marina K., Hong, Yonggeun, Hood, David A., Hoozemans, Jeroen J.M., Hoppe, Thorsten, Hsu, Chin, Hsu, Chin-Yuan, Hsu, Li-Chung, Hu, Dong, Hu, Guochang, Hu, Hong-Ming, Hu, Hongbo, Hu, Ming Chang, Hu, Yu-Chen, Hu, Zhuo-Wei, Hua, Fang, Hua, Ya, Huang, Canhua, Huang, Huey-Lan, Huang, Kuo-How, Huang, Kuo-Yang, Huang, Shile, Huang, Shiqian, Huang, Wei-Pang, Huang, Yi-Ran, Huang, Yong, Huang, Yunfei, Huber, Tobias B., Huebbe, Patricia, Huh, Won-Ki, Hulmi, Juha J., Hur, Gang Min, Hurley, James H., Husak, Zvenyslava, Hussain, Sabah N.A., Hussain, Salik, Hwang, Jung Jin, Hwang, Seungmin, Hwang, Thomas I.S., Ichihara, Atsuhiro, Imai, Yuzuru, Imbriano, Carol, Inomata, Megumi, Into, Takeshi, Iovane, Valentina, Iovanna, Juan L., Iozzo, Renato V., Ip, Nancy Y., Irazoqui, Javier E., Iribarren, Pablo, Isaka, Yoshitaka, Isakovic, Aleksandra J., Ischiropoulos, Harry, Isenberg, Jeffrey S., Ishaq, Mohammad, Ishida, Hiroyuki, Ishii, Isao, Ishmael, Jane E., Isidoro, Ciro, Isobe, Ken-Ichi, Isono, Erika, Issazadeh-Navikas, Shohreh, Itahana, Koji, Itakura, Eisuke, Ivanov, Andrei I., Iyer, Anand Krishnan V., Izquierdo, José M., Izumi, Yotaro, Izzo, Valentina, Jäättelä, Marja, Jaber, Nadia, Jackson, Daniel John, Jackson, William T., Jacob, Tony George, Jacques, Thomas S., Jagannath, Chinnaswamy, Jain, Ashish, Jana, Nihar Ranjan, Jang, Byoung Kuk, Jani, Alkesh, Janji, Bassam, Jannig, Paulo Roberto, Jansson, Patric J., Jean, Steve, Jendrach, Marina, Jeon, Ju-Hong, Jessen, Niel, Jeung, Eui-Bae, Jia, Kailiang, Jia, Lijun, Jiang, Hong, Jiang, Hongchi, Jiang, Liwen, Jiang, Teng, Jiang, Xiaoyan, Jiang, Xuejun, Jiang, Ying, Jiang, Yongjun, Jiménez, Alberto, Jin, Cheng, Jin, Hongchuan, Jin, Lei, Jin, Meiyan, Jin, Shengkan, Jinwal, Umesh Kumar, Jo, Eun-Kyeong, Johansen, Terje, Johnson, Daniel E., Johnson, Gail V.W., Johnson, James D., Jonasch, Eric, Jones, Chri, Joosten, Leo A.B., Jordan, Joaquin, Joseph, Anna-Maria, Joseph, Bertrand, Joubert, Annie M., Ju, Dianwen, Ju, Jingfang, Juan, Hsueh-Fen, Juenemann, Katrin, Juhász, Gábor, Jung, Hye Seung, Jung, Jae U., Jung, Yong-Keun, Jungbluth, Heinz, Justice, Matthew J., Jutten, Barry, Kaakoush, Nadeem O., Kaarniranta, Kai, Kaasik, Allen, Kabuta, Tomohiro, Kaeffer, Bertrand, Kågedal, Katarina, Kahana, Alon, Kajimura, Shingo, Kakhlon, Or, Kalia, Manjula, Kalvakolanu, Dhan V., Kamada, Yoshiaki, Kambas, Konstantino, Kaminskyy, Vitaliy O., Kampinga, Harm H., Kandouz, Mustapha, Kang, Chanhee, Kang, Rui, Kang, Tae-Cheon, Kanki, Tomotake, Kanneganti, Thirumala-Devi, Kanno, Haruo, Kanthasamy, Anumantha G., Kantorow, Marc, Kaparakis-Liaskos, Maria, Kapuy, Orsolya, Karantza, Vassiliki, Karim, Md Razaul, Karmakar, Parimal, Kaser, Arthur, Kaushik, Susmita, Kawula, Thoma, Kaynar, A. 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Sue, Menna-Barreto, Rubem F.S., Menon, Manoj B., Meraz-Ríos, Marco A., Merla, Giuseppe, Merlini, Luciano, Merlot, Angelica M., Meryk, Andrea, Meschini, Stefania, Meyer, Joel N., Mi, Man-Tian, Miao, Chao-Yu, Micale, Lucia, Michaeli, Simon, Michiels, Carine, Migliaccio, Anna Rita, Mihailidou, Anastasia Susie, Mijaljica, Dalibor, Mikoshiba, Katsuhiko, Milan, Enrico, Miller-Fleming, Leonor, Mills, Gordon B., Mills, Ian G., Minakaki, Georgia, Minassian, Berge A., Ming, Xiu-Fen, Minibayeva, Farida, Minina, Elena A., Mintern, Justine D., Minucci, Saverio, Miranda-Vizuete, Antonio, Mitchell, Claire H., Miyamoto, Shigeki, Miyazawa, Keisuke, Mizushima, Noboru, Mnich, Katarzyna, Mograbi, Baharia, Mohseni, Simin, Moita, Luis Ferreira, Molinari, Marco, Molinari, Maurizio, Møller, Andreas Buch, Mollereau, Bertrand, Mollinedo, Faustino, Mongillo, Marco, Monick, Martha M., Montagnaro, Serena, Montell, Craig, Moore, Darren J., Moore, Michael N., Mora-Rodriguez, Rodrigo, Moreira, Paula I., Morel, Etienne, Morelli, Maria Beatrice, Moreno, Sandra, Morgan, Michael J., Moris, Arnaud, Moriyasu, Yuji, Morrison, Janna L., Morrison, Lynda A., Morselli, Eugenia, Moscat, Jorge, Moseley, Pope L., Mostowy, Serge, Motori, Elisa, Mottet, Deni, Mottram, Jeremy C., Moussa, Charbel E.-H., Mpakou, Vassiliki E., Mukhtar, Hasan, Levy, Jean M. Mulcahy, Muller, Sylviane, Muñoz-Moreno, Raquel, Muñoz-Pinedo, Cristina, Münz, Christian, Murphy, Maureen E., Murray, James T., Murthy, Aditya, Mysorekar, Indira U., Nabi, Ivan R., Nabissi, Massimo, Nader, Gustavo A., Nagahara, Yukitoshi, Nagai, Yoshitaka, Nagata, Kazuhiro, Nagelkerke, Anika, Nagy, Péter, Naidu, Samisubbu R., Nair, Sreejayan, Nakano, Hiroyasu, Nakatogawa, Hitoshi, Nanjundan, Meera, Napolitano, Gennaro, Naqvi, Naweed I., Nardacci, Roberta, Narendra, Derek P., Narita, Masashi, Nascimbeni, Anna Chiara, Natarajan, Ramesh, Navegantes, Luiz C., Nawrocki, Steffan T., Nazarko, Taras Y., Nazarko, Volodymyr Y., Neill, Thoma, Neri, Luca M., Netea, Mihai G., Netea-Maier, Romana T., Neves, Bruno M., Ney, Paul A., Nezis, Ioannis P., Nguyen, Hang T.T., Nguyen, Huu Phuc, Nicot, Anne-Sophie, Nilsen, Hilde, Nilsson, Per, Nishimura, Mikio, Nishino, Ichizo, Niso-Santano, Mireia, Niu, Hua, Nixon, Ralph A., Njar, Vincent C.O., Noda, Takeshi, Noegel, Angelika A., Nolte, Elsie Magdalena, Norberg, Erik, Norga, Koenraad K., Noureini, Sakineh Kazemi, Notomi, Shoji, Notterpek, Lucia, Nowikovsky, Karin, Nukina, Nobuyuki, Nürnberger, Thorsten, O'donnell, Valerie B., O'donovan, Tracey, O'dwyer, Peter J., Oehme, Ina, Oeste, Clara L., Ogawa, Michinaga, Ogretmen, Besim, Ogura, Yuji, Oh, Young J., Ohmuraya, Masaki, Ohshima, Takayuki, Ojha, Rani, Okamoto, Koji, Okazaki, Toshiro, Oliver, F. Javier, Ollinger, Karin, Olsson, Stefan, Orban, Daniel P., Ordonez, Paulina, Orhon, Idil, Orosz, Laszlo, O'rourke, Eyleen J., Orozco, Helena, Ortega, Angel L., Ortona, Elena, Osellame, Laura D., Oshima, Junko, Oshima, Shigeru, Osiewacz, Heinz D., Otomo, Takanobu, Otsu, Kinya, Ou, Jing-Hsiung Jame, Outeiro, Tiago F., Ouyang, Dong-Yun, Ouyang, Hongjiao, Overholtzer, Michael, Ozbun, Michelle A., Ozdinler, P. Hande, Ozpolat, Bulent, Pacelli, Consiglia, Paganetti, Paolo, Page, Guyléne, Pages, Gille, Pagnini, Ugo, Pajak, Beata, Pak, Stephen C., Pakos-Zebrucka, Karolina, Pakpour, Nazzy, Palková, Zdena, Palladino, Francesca, Pallauf, Kathrin, Pallet, Nicola, Palmieri, Marta, Paludan, Søren R., Palumbo, Camilla, Palumbo, Silvia, Pampliega, Olatz, Pan, Hongming, Pan, Wei, Panaretakis, Theochari, Pandey, Aseem, Pantazopoulou, Areti, Papackova, Zuzana, Papademetrio, Daniela L., Papassideri, Issidora, Papini, Alessio, Parajuli, Nirmala, Pardo, Julian, Parekh, Vrajesh V., Parenti, Giancarlo, Park, Jong-In, Park, Junsoo, Park, Ohkmae K., Parker, Roy, Parlato, Rosanna, Parys, Jan B., Parzych, Katherine R., Pasquet, Jean-Max, Pasquier, Benoit, Pasumarthi, Kishore B.S., Patschan, Daniel, Pattingre, Sophie, Pattison, Scott, Pause, Arnim, Pavenstädt, Hermann, Pavone, Flaminia, Pedrozo, Zully, Peña, Fernando J., Peñalva, Miguel A., Pende, Mario, Peng, Jianxin, Penna, Fabio, Penninger, Josef M., Pensalfini, Anna, Pepe, Salvatore, Pereira, Gustavo J.S., Pereira, Paulo C., de la Cruz, Verónica Pérez, Pérez-Pérez, María Esther, Pérez-Rodríguez, Diego, Pérez-Sala, Dolore, Perier, Celine, Perl, Andra, Perlmutter, David H., Perrotta, Ida, Pervaiz, Shazib, Pesonen, Maija, Pessin, Jeffrey E., Peters, Godefridus J., Petersen, Morten, Petrache, Irina, Petrof, Basil J., Petrovski, Goran, Phang, James M., Piacentini, Mauro, Pierdominici, Marina, Pierre, Philippe, Pierrefite-Carle, Valérie, Pietrocola, Federico, Pimentel-Muiños, Felipe X., Pinar, Mario, Pineda, Benjamin, Pinkas-Kramarski, Ronit, Pinti, Marcello, Pinton, Paolo, Piperdi, Bilal, Piret, James M., Platanias, Leonidas C., Platta, Harald W., Plowey, Edward D., Pöggeler, Stefanie, Poirot, Marc, Polčic, Peter, Poletti, Angelo, Poon, Audrey H., Popelka, Hana, Popova, Blagovesta, Poprawa, Izabela, Poulose, Shibu M., Poulton, Joanna, Powers, Scott K., Powers, Ted, Pozuelo-Rubio, Mercede, Prak, Krisna, Prange, Reinhild, Prescott, Mark, Priault, Muriel, Prince, Sharon, Proia, Richard L., Proikas-Cezanne, Tassula, Prokisch, Holger, Promponas, Vasilis J., Przyklenk, Karin, Puertollano, Rosa, Pugazhenthi, Subbiah, Puglielli, Luigi, Pujol, Aurora, Puyal, Julien, Pyeon, Dohun, Qi, Xin, Qian, Wen-Bin, Qin, Zheng-Hong, Qiu, Yu, Qu, Ziwei, Quadrilatero, Joe, Quinn, Frederick, Raben, Nina, Rabinowich, Hannah, Radogna, Flavia, Ragusa, Michael J., Rahmani, Mohamed, Raina, Komal, Ramanadham, Sasanka, Ramesh, Rajagopal, Rami, Abdelhaq, Randall-Demllo, Sarron, Randow, Felix, Rao, Hai, Rao, V. Ashutosh, Rasmussen, Blake B., Rasse, Tobias M., Ratovitski, Edward A., Rautou, Pierre-Emmanuel, Ray, Swapan K., Razani, Babak, Reed, Bruce H., Reggiori, Fulvio, Rehm, Marku, Reichert, Andreas S., Rein, Theo, Reiner, David J., Reits, Eric, Ren, Jun, Ren, Xingcong, Renna, Maurizio, Reusch, Jane E.B., Revuelta, Jose L., Reyes, Leticia, Rezaie, Alireza R., Richards, Robert I., Richardson, Des R., Richetta, Clémence, Riehle, Michael A., Rihn, Bertrand H., Rikihisa, Yasuko, Riley, Brigit E., Rimbach, Gerald, Rippo, Maria Rita, Ritis, Konstantino, Rizzi, Federica, Rizzo, Elizete, Roach, Peter J., Robbins, Jeffrey, Roberge, Michel, Roca, Gabriela, Roccheri, Maria Carmela, Rocha, Sonia, Rodrigues, Cecilia M.P., Rodríguez, Clara I., de Cordoba, Santiago Rodriguez, Rodriguez-Muela, Natalia, Roelofs, Jeroen, Rogov, Vladimir V., Rohn, Troy T., Rohrer, Bärbel, Romanelli, Davide, Romani, Luigina, Romano, Patricia Silvia, Roncero, M. Isabel G., Rosa, Jose Lui, Rosello, Alicia, Rosen, Kirill V., Rosenstiel, Philip, Rost-Roszkowska, Magdalena, Roth, Kevin A., Roué, Gael, Rouis, Mustapha, Rouschop, Kasper M., Ruan, Daniel T., Ruano, Diego, Rubinsztein, David C., Rucker, Edmund B., Rudich, Assaf, Rudolf, Emil, Rudolf, Ruediger, Ruegg, Markus A., Ruiz-Roldan, Carmen, Ruparelia, Avnika Ashok, Rusmini, Paola, Russ, David W., Russo, Gian Luigi, Russo, Giuseppe, Russo, Rossella, Rusten, Tor Erik, Ryabovol, Victoria, Ryan, Kevin M., Ryter, Stefan W., Sabatini, David M., Sacher, Michael, Sachse, Carsten, Sack, Michael N., Sadoshima, Junichi, Saftig, Paul, Sagi-Eisenberg, Ronit, Sahni, Sumit, Saikumar, Pothana, Saito, Tsunenori, Saitoh, Tatsuya, Sakakura, Koichi, Sakoh-Nakatogawa, Machiko, Sakuraba, Yasuhito, Salazar-Roa, María, Salomoni, Paolo, Saluja, Ashok K., Salvaterra, Paul M., Salvioli, Rosa, Samali, Afshin, Sanchez, Anthony M.J., Sánchez-Alcázar, José A., Sanchez-Prieto, Ricardo, Sandri, Marco, Sanjuan, Miguel A., Santaguida, Stefano, Santambrogio, Laura, Santoni, Giorgio, Dos Santos, Claudia Nune, Saran, Shweta, Sardiello, Marco, Sargent, Graeme, Sarkar, Pallabi, Sarkar, Sovan, Sarrias, Maria Rosa, Sarwal, Minnie M., Sasakawa, Chihiro, Sasaki, Motoko, Sass, Miklo, Sato, Ken, Sato, Miyuki, Satriano, Joseph, Savaraj, Niramol, Saveljeva, Svetlana, Schaefer, Liliana, Schaible, Ulrich E., Scharl, Michael, Schatzl, Hermann M., Schekman, Randy, Scheper, Wiep, Schiavi, Alfonso, Schipper, Hyman M., Schmeisser, Hana, Schmidt, Jen, Schmitz, Ingo, Schneider, Bianca E., Schneider, E. Marion, Schneider, Jaime L., Schon, Eric A., Schönenberger, Miriam J., Schönthal, Axel H., Schorderet, Daniel F., Schröder, Bernd, Schuck, Sebastian, Schulze, Ryan J., Schwarten, Melanie, Schwarz, Thomas L., Sciarretta, Sebastiano, Scotto, Kathleen, Scovassi, A. Ivana, Screaton, Robert A., Screen, Mark, Seca, Hugo, Sedej, Simon, Segatori, Laura, Segev, Nava, Seglen, Per O., Seguí-Simarro, Jose M., Segura-Aguilar, Juan, Seiliez, Iban, Seki, Ekihiro, Sell, Christian, Semenkovich, Clay F., Semenza, Gregg L., Sen, Utpal, Serra, Andreas L., Serrano-Puebla, Ana, Sesaki, Hiromi, Setoguchi, Takao, Settembre, Carmine, Shacka, John J., Shajahan-Haq, Ayesha N., Shapiro, Irving M., Sharma, Shweta, She, Hua, Shen, C.-K. Jame, Shen, Chiung-Chyi, Shen, Han-Ming, Shen, Sanbing, Shen, Weili, Sheng, Rui, Sheng, Xianyong, Sheng, Zu-Hang, Shepherd, Trevor G., Shi, Junyan, Shi, Qiang, Shi, Qinghua, Shi, Yuguang, Shibutani, Shusaku, Shibuya, Kenichi, Shidoji, Yoshihiro, Shieh, Jeng-Jer, Shih, Chwen-Ming, Shimada, Yohta, Shimizu, Shigeomi, Shin, Dong Wook, Shinohara, Mari L., Shintani, Michiko, Shintani, Takahiro, Shioi, Tetsuo, Shirabe, Ken, Shiri-Sverdlov, Ronit, Shirihai, Orian, Shore, Gordon C., Shu, Chih-Wen, Shukla, Deepak, Sibirny, Andriy A., Sica, Valentina, Sigurdson, Christina J., Sigurdsson, Einar M., Sijwali, Puran Singh, Sikorska, Beata, Silveira, Wilian A., Silvente-Poirot, Sandrine, Silverman, Gary A., Simak, Jan, Simmet, Thoma, Simon, Anna Katharina, Simon, Hans-Uwe, Simone, Cristiano, Simons, Matia, Simonsen, Anne, Singh, Rajat, Singh, Shivendra V., Singh, Shrawan K., Sinha, Debasish, Sinha, Sangita, Sinicrope, Frank A., Sirko, Agnieszka, Sirohi, Kapil, Sishi, Balindiwe J.N., Sittler, Annie, Siu, Parco M., Sivridis, Efthimio, Skwarska, Anna, Slack, Ruth, Slaninová, Iva, Slavov, Nikolai, Smaili, Soraya S., Smalley, Keiran S.M., Smith, Duncan R., Soenen, Stefaan J., Soleimanpour, Scott A., Solhaug, Anita, Somasundaram, Kumaravel, Son, Jin H., Sonawane, Avinash, Song, Chunjuan, Song, Fuyong, Song, Hyun Kyu, Song, Ju-Xian, Song, Wei, Soo, Kai Y., Sood, Anil K., Soong, Tuck Wah, Soontornniyomkij, Virawudh, Sorice, Maurizio, Sotgia, Federica, Soto-Pantoja, David R., Sotthibundhu, Areechun, Sousa, Maria João, Spaink, Herman P., Span, Paul N., Spang, Anne, Sparks, Janet D., Speck, Peter G., Spector, Stephen A., Spies, Claudia D., Springer, Wolfdieter, Clair, Daret St, Stacchiotti, Alessandra, Staels, Bart, Stang, Michael T., Starczynowski, Daniel T., Starokadomskyy, Petro, Steegborn, Clemen, Steele, John W., Stefanis, Leonida, Steffan, Joan, Stellrecht, Christine M., Stenmark, Harald, Stepkowski, Tomasz M., Stern, Stęphan T., Stevens, Craig, Stockwell, Brent R., Stoka, Veronika, Storchova, Zuzana, Stork, Björn, Stratoulias, Vassili, Stravopodis, Dimitrios J., Strnad, Pavel, Strohecker, Anne Marie, Ström, Anna-Lena, Stromhaug, Per, Stulik, Jiri, Su, Yu-Xiong, Su, Zhaoliang, Subauste, Carlos S., Subramaniam, Srinivasa, Sue, Carolyn M., Suh, Sang Won, Sui, Xinbing, Sukseree, Supawadee, Sulzer, David, Sun, Fang-Lin, Sun, Jiaren, Sun, Jun, Sun, Shi-Yong, Sun, Yang, Sun, Yi, Sun, Yingjie, Sundaramoorthy, Vinod, Sung, Joseph, Suzuki, Hidekazu, Suzuki, Kuninori, Suzuki, Naoki, Suzuki, Tadashi, Suzuki, Yuichiro J., Swanson, Michele S., Swanton, Charle, Swärd, Karl, Swarup, Ghanshyam, Sweeney, Sean T., Sylvester, Paul W., Szatmari, Zsuzsanna, Szegezdi, Eva, Szlosarek, Peter W., Taegtmeyer, Heinrich, Tafani, Marco, Taillebourg, Emmanuel, Tait, Stephen W.G., Takacs-Vellai, Krisztina, Takahashi, Yoshinori, Takáts, Szabolc, Takemura, Genzou, Takigawa, Nagio, Talbot, Nicholas J., Tamagno, Elena, Tamburini, Jerome, Tan, Cai-Ping, Tan, Lan, Tan, Mei Lan, Tan, Ming, Tan, Yee-Joo, Tanaka, Keiji, Tanaka, Masaki, Tang, Daolin, Tang, Dingzhong, Tang, Guomei, Tanida, Isei, Tanji, Kunikazu, Tannous, Bakhos A., Tapia, Jose A., Tasset-Cuevas, Inmaculada, Tatar, Marc, Tavassoly, Iman, Tavernarakis, Nektario, Taylor, Allen, Taylor, Graham S., Taylor, Gregory A., Taylor, J. Paul, Taylor, Mark J., Tchetina, Elena V., Tee, Andrew R., Teixeira-Clerc, Fatima, Telang, Sucheta, Tencomnao, Tewin, Teng, Ba-Bie, Teng, Ru-Jeng, Terro, Faraj, Tettamanti, Gianluca, Theiss, Arianne L., Theron, Anne E., Thomas, Kelly Jean, Thomé, Marcos P., Thomes, Paul G., Thorburn, Andrew, Thorner, Jeremy, Thum, Thoma, Thumm, Michael, Thurston, Teresa L.M., Tian, Ling, Till, Andrea, Ting, Jenny Pan-Yun, Ting, Jenny Pan Yun, Titorenko, Vladimir I., Toker, Lilach, Toldo, Stefano, Tooze, Sharon A., Topisirovic, Ivan, Torgersen, Maria Lyngaa, Torosantucci, Liliana, Torriglia, Alicia, Torrisi, Maria Rosaria, Tournier, Cathy, Towns, Roberto, Trajkovic, Vladimir, Travassos, Leonardo H., Triola, Gemma, Tripathi, Durga Nand, Trisciuoglio, Daniela, Troncoso, Rodrigo, Trougakos, Ioannis P., Truttmann, Anita C., Tsai, Kuen-Jer, Tschan, Mario P., Tseng, Yi-Hsin, Tsukuba, Takayuki, Tsung, Allan, Tsvetkov, Andrey S., Tu, Shuiping, Tuan, Hsing-Yu, Tucci, Marco, Tumbarello, David A., Turk, Bori, Turk, Vito, Turner, Robin F.B., Tveita, Anders A., Tyagi, Suresh C., Ubukata, Makoto, Uchiyama, Yasuo, Udelnow, Andrej, Ueno, Takashi, Umekawa, Midori, Umemiya-Shirafuji, Rika, Underwood, Benjamin R., Ungermann, Christian, Ureshino, Rodrigo P., Ushioda, Ryo, Uversky, Vladimir N., Uzcátegui, Néstor L., Vaccari, Thoma, Vaccaro, Maria I., Váchová, Libuše, Vakifahmetoglu-Norberg, Helin, Valdor, Rut, Valente, Enza Maria, Vallette, Francoi, Valverde, Angela M., Van den Berghe, Greet, Van Den Bosch, Ludo, van den Brink, Gijs R., van der Goot, F. Gisou, van der Klei, Ida J., van der Laan, Luc J.W., van Doorn, Wouter G., van Egmond, Marjolein, van Golen, Kenneth L., Van Kaer, Luc, Campagne, Menno van Lookeren, Vandenabeele, Peter, Vandenberghe, Wim, Vanhorebeek, Ilse, Varela-Nieto, Isabel, Vasconcelos, M. Helena, Vasko, Radovan, Vavvas, Demetrios G., Vega-Naredo, Ignacio, Velasco, Guillermo, Velentzas, Athanassios D., Velentzas, Panagiotis D., Vellai, Tibor, Vellenga, Edo, Vendelbo, Mikkel Holm, Venkatachalam, Kartik, Ventura, Natascia, Ventura, Salvador, Veras, Patrícia S.T., Verdier, Mireille, Vertessy, Beata G., Viale, Andrea, Vidal, Michel, Vieira, Helena L.A., Vierstra, Richard D., Vigneswaran, Nadarajah, Vij, Neeraj, Vila, Miquel, Villar, Margarita, Villar, Victor H., Villarroya, Joan, Vindis, Cécile, Viola, Giampietro, Viscomi, Maria Teresa, Vitale, Giovanni, Vogl, Dan T., Voitsekhovskaja, Olga V., von Haefen, Clarissa, von Schwarzenberg, Karin, Voth, Daniel E., Vouret-Craviari, Valérie, Vuori, Kristina, Vyas, Jatin M., Waeber, Christian, Walker, Cheryl Lyn, Walker, Mark J., Walter, Jochen, Wan, Lei, Wan, Xiangbo, Wang, Bo, Wang, Caihong, Wang, Chao-Yung, Wang, Chengshu, Wang, Chenran, Wang, Chuangui, Wang, Dong, Wang, Fen, Wang, Fuxin, Wang, Guanghui, Wang, Hai-Jie, Wang, Haichao, Wang, Hong-Gang, Wang, Hongmin, Wang, Horng-Dar, Wang, Jing, Wang, Junjun, Wang, Mei, Wang, Mei-Qing, Wang, Pei-Yu, Wang, Peng, Wang, Richard C., Wang, Shuo, Wang, Ting-Fang, Wang, Xian, Wang, Xiao-Jia, Wang, Xiao-Wei, Wang, Xin, Wang, Xuejun, Wang, Yan, Wang, Yanming, Wang, Ying, Wang, Ying-Jan, Wang, Yipeng, Wang, Yu, Wang, Yu Tian, Wang, Yuqing, Wang, Zhi-Nong, Wappner, Pablo, Ward, Carl, Ward, Diane McVey, Warnes, Gary, Watada, Hirotaka, Watanabe, Yoshihisa, Watase, Kei, Weaver, Timothy E., Weekes, Colin D., Wei, Jiwu, Weide, Thoma, Weihl, Conrad C., Weindl, Günther, Weis, Simone Nardin, Wen, Longping, Wen, Xin, Wen, Yunfei, Westermann, Benedikt, Weyand, Cornelia M., White, Anthony R., White, Eileen, Whitton, J. Lindsay, Whitworth, Alexander J., Wiels, Joëlle, Wild, Franziska, Wildenberg, Manon E., Wileman, Tom, Wilkinson, Deepti Sriniva, Wilkinson, Simon, Willbold, Dieter, Williams, Chri, Williams, Katherine, Williamson, Peter R., Winklhofer, Konstanze F., Witkin, Steven S., Wohlgemuth, Stephanie E., Wollert, Thoma, Wolvetang, Ernst J., Wong, Esther, Wong, G. William, Wong, Richard W., Wong, Vincent Kam Wai, Woodcock, Elizabeth A., Wright, Karen L., Wu, Chunlai, Wu, Defeng, Wu, Gen Sheng, Wu, Jian, Wu, Junfang, Wu, Mian, Wu, Min, Wu, Shengzhou, Wu, William K.K., Wu, Yaohua, Wu, Zhenlong, Xavier, Cristina P.R., Xavier, Ramnik J., Xia, Gui-Xian, Xia, Tian, Xia, Weiliang, Xia, Yong, Xiao, Hengyi, Xiao, Jian, Xiao, Shi, Xiao, Wuhan, Xie, Chuan-Ming, Xie, Zhiping, Xie, Zhonglin, Xilouri, Maria, Xiong, Yuyan, Xu, Chuanshan, Xu, Congfeng, Xu, Feng, Xu, Haoxing, Xu, Hongwei, Xu, Jian, Xu, Jianzhen, Xu, Jinxian, Xu, Liang, Xu, Xiaolei, Xu, Yangqing, Xu, Ye, Xu, Zhi-Xiang, Xu, Ziheng, Xue, Yu, Yamada, Takahiro, Yamamoto, Ai, Yamanaka, Koji, Yamashina, Shunhei, Yamashiro, Shigeko, Yan, Bing, Yan, Bo, Yan, Xianghua, Yan, Zhen, Yanagi, Yasuo, Yang, Dun-Sheng, Yang, Jin-Ming, Yang, Liu, Yang, Minghua, Yang, Pei-Ming, Yang, Peixin, Yang, Qian, Yang, Wannian, Yang, Wei Yuan, Yang, Xuesong, Yang, Yi, Yang, Ying, Yang, Zhifen, Yang, Zhihong, Yao, Meng-Chao, Yao, Pamela J., Yao, Xiaofeng, Yao, Zhenyu, Yao, Zhiyuan, Yasui, Linda S., Ye, Mingxiang, Yedvobnick, Barry, Yeganeh, Behzad, Yeh, Elizabeth S., Yeyati, Patricia L., Yi, Fan, Yi, Long, Yin, Xiao-Ming, Yip, Calvin K., Yoo, Yeong-Min, Yoo, Young Hyun, Yoon, Seung-Yong, Yoshida, Ken-Ichi, Yoshimori, Tamotsu, Young, Ken H., Yu, Huixin, Yu, Jane J., Yu, Jin-Tai, Yu, Jun, Yu, Li, Yu, W. Haung, Yu, Xiao-Fang, Yu, Zhengping, Yuan, Junying, Yuan, Zhi-Min, Yue, Beatrice Y.J.T., Yue, Jianbo, Yue, Zhenyu, Zacks, David N., Zacksenhaus, Eldad, Zaffaroni, Nadia, Zaglia, Tania, Zakeri, Zahra, Zecchini, Vincent, Zeng, Jinsheng, Zeng, Min, Zeng, Qi, Zervos, Antonis S., Zhang, Donna D., Zhang, Fan, Zhang, Guo, Zhang, Guo-Chang, Zhang, Hao, Zhang, Hong, Zhang, Hongbing, Zhang, Jian, Zhang, Jiangwei, Zhang, Jianhua, Zhang, Jing-Pu, Zhang, Li, Zhang, Lin, Zhang, Long, Zhang, Ming-Yong, Zhang, Xiangnan, Zhang, Xu Dong, Zhang, Yan, Zhang, Yang, Zhang, Yanjin, Zhang, Yingmei, Zhang, Yunjiao, Zhao, Mei, Zhao, Wei-Li, Zhao, Xiaonan, Zhao, Yan G., Zhao, Ying, Zhao, Yongchao, Zhao, Yu-Xia, Zhao, Zhendong, Zhao, Zhizhuang J., Zheng, Dexian, Zheng, Xi-Long, Zheng, Xiaoxiang, Zhivotovsky, Bori, Zhong, Qing, Zhou, Guang-Zhou, Zhou, Guofei, Zhou, Huiping, Zhou, Shu-Feng, Zhou, Xu-Jie, Zhu, Hongxin, Zhu, Hua, Zhu, Wei-Guo, Zhu, Wenhua, Zhu, Xiao-Feng, Zhu, Yuhua, Zhuang, Shi-Mei, Zhuang, Xiaohong, Ziparo, Elio, Zois, Christos E., Zoladek, Teresa, Zong, Wei-Xing, Zorzano, Antonio, and Zughaier, Susu M.

Subjects
Molecular Biology, Cell Biology, Settore BIO/06 - Anatomia Comparata E Citologia
Abstract

non presente

Published
2016

37. The JCMT Gould Belt Survey: a quantitative comparison between SCUBA-2 data reduction methods

Author

Mairs, S., Johnstone, D., Kirk, H., Graves, S., Buckle, J., Beaulieu, S. F., Berry, D. S., Broekhoven-Fiene, H., Currie, M. J., Fich, M., Hatchell, J., Jenness, T., Mottram, J. C., Nutter, D., Pattle, K., Pineda, J. E., Salji, C., Di Francesco, J., Hogerheijde, M. R., Ward-Thompson, D., and team, the JCMT Gould Belt survey

Subjects
Physics, Brightness, Point source, Noise (signal processing), Bolometer, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, F500, Stability (probability), law.invention, Reduction (complexity), 13. Climate action, Space and Planetary Science, law, 14. Life underwater, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), James Clerk Maxwell Telescope, Data reduction
Abstract

Performing ground-based submillimetre observations is a difficult task as the measurements are subject to absorption and emission from water vapour in the Earth's atmosphere and time variation in weather and instrument stability. Removing these features and other artifacts from the data is a vital process which affects the characteristics of the recovered astronomical structure we seek to study. In this paper, we explore two data reduction methods for data taken with the Submillimetre Common-User Bolometer Array-2 (SCUBA-2) at the James Clerk Maxwell Telescope (JCMT). The JCMT Legacy Reduction 1 (JCMT LR1) and The Gould Belt Legacy Survey Legacy Release 1 (GBS LR1) reduction both use the same software, Starlink, but differ in their choice of data reduction parameters. We find that the JCMT LR1 reduction is suitable for determining whether or not compact emission is present in a given region and the GBS LR1 reduction is tuned in a robust way to uncover more extended emission, which better serves more in-depth physical analyses of star-forming regions. Using the GBS LR1 method, we find that compact sources are recovered well, even at a peak brightness of only 3 times the noise, whereas the reconstruction of larger objects requires much care when drawing boundaries around the expected astronomical signal in the data reduction process. Incorrect boundaries can lead to false structure identification or it can cause structure to be missed. In the JCMT LR1 reduction, the extent of the true structure of objects larger than a point source is never fully recovered., Comment: 26 Pages, 16 Figures, Accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS)

Published
2015

38. Synthetic CO, H2 and HI surveys of the Galactic 2nd Quadrant, and the properties of molecular gas

Author

Duarte-Cabral, A., Acreman, D. M., Dobbs, C. L., Mottram, J. C., Gibson, S. J., Brunt, C. M., and Douglas, K. A.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We present CO, H2, HI and HISA distributions from a set of simulations of grand design spirals including stellar feedback, self-gravity, heating and cooling. We replicate the emission of the 2nd Galactic Quadrant by placing the observer inside the modelled galaxies and post process the simulations using a radiative transfer code, so as to create synthetic observations. We compare the synthetic datacubes to observations of the 2nd Quadrant of the Milky Way to test the ability of the current models to reproduce the basic chemistry of the Galactic ISM, as well as to test how sensitive such galaxy models are to different recipes of chemistry and/or feedback. We find that models which include feedback and self-gravity can reproduce the production of CO with respect to H2 as observed in our Galaxy, as well as the distribution of the material perpendicular to the Galactic plane. While changes in the chemistry/feedback recipes do not have a huge impact on the statistical properties of the chemistry in the simulated galaxies, we find that the inclusion of both feedback and self-gravity are crucial ingredients, as our test without feedback failed to reproduce all of the observables. Finally, even though the transition from H2 to CO seems to be robust, we find that all models seem to underproduce molecular gas, and have a lower molecular to atomic gas fraction than is observed. Nevertheless, our fiducial model with feedback and self-gravity has shown to be robust in reproducing the statistical properties of the basic molecular gas components of the ISM in our Galaxy., Accepted for publication in MNRAS

Published
2014

39. Fragmentation, rotation, and outflows in the high-mass star-forming region IRAS 23033+5951: A case study of the IRAM NOEMA large program CORE.

Author

Bosco, F., Beuther, H., Ahmadi, A., Mottram, J. C., Kuiper, R., Linz, H., Maud, L., Winters, J. M., Henning, T., Feng, S., Peters, T., Semenov, D., Klaassen, P. D., Schilke, P., Urquhart, J. S., Beltrán, M. T., Lumsden, S. L., Leurini, S., Moscadelli, L., and Cesaroni, R.

Subjects
PROTOSTARS, ROTATIONAL motion, STELLAR evolution, GRAVITATIONAL instability, MOLECULAR structure, SIGNAL-to-noise ratio
Abstract

Context. The formation process of high-mass stars (>8 M⊙) is poorly constrained, particularly the effects of clump fragmentation creating multiple systems and the mechanism of mass accretion onto the cores. Aims. We study the fragmentation of dense gas clumps, and trace the circumstellar rotation and outflows by analyzing observations of the high-mass (~500 M⊙) star-forming region IRAS 23033+5951. Methods. Using the Northern Extended Millimeter Array (NOEMA) in three configurations and the IRAM 30 m single-dish telescope at 220 GHz, we probe the gas and dust emission at an angular resolution of ~0.45′′, corresponding to 1900 au. Results. In the millimeter (mm) continuum emission, we identify a protostellar cluster with at least four mm-sources, where three of them show a significantly higher peak intensity well above a signal-to-noise ratio of 100. Hierarchical fragmentation from large to small spatial scales is discussed. Two fragments are embedded in rotating structures and drive molecular outflows, traced by 13CO (2–1) emission. The velocity profiles across two of the cores are similar to Keplerian but are missing the highest-velocity components close to the center of rotation, which is a common phenomena from observations like these, and other rotation scenarios are not excluded entirely. Position–velocity diagrams suggest protostellar masses of ~6 and 19 M⊙. Rotational temperatures from fitting CH3CN (12K− 11K) spectra are used for estimating the gas temperature and thereby also the disk stability against gravitational fragmentation, utilizing Toomre's Q parameter. Assuming that the candidate disk is in Keplerian rotation about the central stellar object and considering different disk inclination angles, we identify only one candidate disk as being unstable against gravitational instability caused by axisymmetric perturbations. Conclusions. The dominant sources cover different evolutionary stages within the same maternal gas clump. The appearance of rotation and outflows of the cores are similar to those found in low-mass star-forming regions. [ABSTRACT FROM AUTHOR]

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

Author

Cesaroni, R., Beuther, H., Ahmadi, A., Beltrán, M. T., Csengeri, T., Galván-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., and Peters, T.

Subjects
ACETONITRILE, SUPERGIANT stars, ACCRETION disks, STAR clusters, BIPOLAR outflows (Astrophysics), DRILL core analysis
Abstract

Context. This study is part of the CORE project, 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. 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 large-scale outflow previously known in the literature. In our scenario, the star powering the flow is responsible for most of the luminosity of IRAS 23385+6053 (~3000 L⊙). The other cores, albeit with masses below the corresponding virial masses, appear to be accreting material from their molecular surroundings and are possibly collapsing or on the verge of collapse. We conclude that we are observing a sample of star-forming cores that is bound to turn into a cluster of massive stars. [ABSTRACT FROM AUTHOR]

Published
2019
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41. Feedback in W49A diagnosed with radio recombination lines and models.

Author

Rugel, M. R., Rahner, D., Beuther, H., Pellegrini, E. W., Wang, Y., Soler, J. D., Ott, J., Brunthaler, A., Anderson, L. D., Mottram, J. C., Henning, T., Goldsmith, P. F., Heyer, M., Klessen, R. S., Bihr, S., Menten, K. M., Smith, R. J., Urquhart, J. S., Ragan, S. E., and Glover, S. C. O.

Subjects
SEYFERT galaxies, RADIO lines, CLOUD feedback
Abstract

We present images of radio recombination lines (RRLs) at wavelengths around 17 cm from the star-forming region W49A to determine the kinematics of ionized gas in the THOR survey (The H I/OH/Recombination line survey of the inner Milky Way) at an angular resolution of 16.′′8 × 13.′′8. The distribution of ionized gas appears to be affected by feedback processes from the star clusters in W49A. The velocity structure of the RRLs shows a complex behavior with respect to the molecular gas. We find a shell-like distribution of ionized gas as traced by RRL emission surrounding the central cluster of OB stars in W49A. We describe the evolution of the shell with the recent feedback model code WARPFIELD that includes the important physical processes and has previously been applied to the 30 Doradus region in the Large Magellanic Cloud. The cloud structure and dynamics of W49A are in agreement with a feedback-driven shell that is re-collapsing. The shell may have triggered star formation in other parts of W49A. We suggest that W49A is a potential candidate for star formation regulated by feedback-driven and re-collapsing shells. [ABSTRACT FROM AUTHOR]

Published
2019
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42. High-mass star formation at sub-50 au scales.

Author

Beuther, H., Ahmadi, A., Mottram, J. C., Linz, H., Maud, L. T., Henning, Th., Kuiper, R., Walsh, A. J., Johnston, K. G., and Longmore, S. N.

Subjects
STAR formation, PROPERTIES of matter, VELOCITY, MOLECULAR gas lasers
Abstract

Context. The hierarchical process of star formation has so far mostly been studied on scales from thousands of au to parsecs, but the smaller sub-1000 au scales of high-mass star formation are still largely unexplored in the submillimeter regime. Aims. We aim to resolve the dust and gas emission at the highest spatial resolution to study the physical properties of the densest structures during high-mass star formation. Methods. We observed the high-mass hot core region G351.77-0.54 with the Atacama Large Millimeter Array with baselines extending out to more than 16 km. This allowed us to dissect the region at sub-50 au spatial scales. Results. At a spatial resolution of 18/40 au (depending on the distance), we identify twelve sub-structures within the inner few thousand au of the region. The brightness temperatures are high, reaching values greater 1000 K, signposting high optical depth toward the peak positions. Core separations vary between sub-100 au to several 100 and 1000 au. The core separations and approximate masses are largely consistent with thermal Jeans fragmentation of a dense gas core. Due to the high continuum optical depth, most spectral lines are seen in absorption. However, a few exceptional emission lines are found that most likely stem from transitions with excitation conditions above 1000 K. Toward the main continuum source, these emission lines exhibit a velocity gradient across scales of 100–200 au aligned with the molecular outflow and perpendicular to the previously inferred disk orientation. While we cannot exclude that these observational features stem from an inner hot accretion disk, the alignment with the outflow rather suggests that it stems from the inner jet and outflow region. The highest-velocity features are found toward the peak position, and no Hubble-like velocity structure can be identified. Therefore, these data are consistent with steady-state turbulent entrainment of the hot molecular gas via Kelvin–Helmholtz instabilities at the interface between the jet and the outflow. Conclusions. Resolving this high-mass star-forming region at sub-50 au scales indicates that the hierarchical fragmentation process in the framework of thermal Jeans fragmentation can continue down to the smallest accessible spatial scales. Velocity gradients on these small scales have to be treated cautiously and do not necessarily stem from disks, but may be better explained with outflow emission. Studying these small scales is very powerful, but covering all spatial scales and deriving a global picture from large to small scales are the next steps to investigate. [ABSTRACT FROM AUTHOR]

Published
2019
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43. Fragmentation and disk formation during high-mass star formation.

Author

Beuther, H., Mottram, J. C., Ahmadi, A., Bosco, F., Linz, H., Henning, Th., Klaassen, P., Winters, J. M., Maud, L. T., Kuiper, R., Semenov, D., Gieser, C., Peters, T., Urquhart, J. S., Pudritz, R., Ragan, S. E., Feng, S., Keto, E., Leurini, S., and Cesaroni, R.

Subjects
*STAR formation, *SUPERGIANT stars, *MILLIMETER astronomy, *CHEMICAL processes, *NUCLEAR fragmentation
Abstract

Context. High-mass stars form in clusters, but neither the early fragmentation processes nor the detailed physical processes leading to the most massive stars are well understood. Aims. We aim to understand the fragmentation, as well as the disk formation, outflow generation, and chemical processes during high-mass star formation on spatial scales of individual cores. Methods. Using the IRAM Northern Extended Millimeter Array (NOEMA) in combination with the 30 m telescope, we have observed in the IRAM large program CORE the 1.37 mm continuum and spectral line emission at high angular resolution (~0.4″) for a sample of 20 well-known high-mass star-forming regions with distances below 5.5 kpc and luminosities larger than 104L⊙. Results. We present the overall survey scope, the selected sample, the observational setup, and the main goals of CORE. Scientifically, we concentrated on the mm continuum emission on scales on the order of 1000 AU. We detect strong mm continuum emission from all regions, mostly due to the emission from cold dust. The fragmentation properties of the sample are diverse. We see extremes where some regions are dominated by a single high-mass core whereas others fragment into as many as 20 cores. A minimum-spanning-tree analysis finds fragmentation at scales on the order of the thermal Jeans length or smaller suggesting that turbulent fragmentation is less important than thermal gravitational fragmentation. The diversity of highly fragmented vs. singular regions can be explained by varying initial density structures and/or different initial magnetic field strengths. Conclusions. A large sample of high-mass star-forming regions at high spatial resolution allows us to study the fragmentation properties of young cluster-forming regions. The smallest observed separations between cores are found around the angular resolution limit which indicates that further fragmentation likely takes place on even smaller spatial scales. The CORE project with its numerous spectral line detections will address a diverse set of important physical and chemical questions in the field of high-mass star formation. [ABSTRACT FROM AUTHOR]

Published
2018
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44. Isolated starless cores in IRDCs in the Hi-GAL survey

Author

Wilcock, L. A., Ward-Thompson, D., Kirk, J. M., Stamatellos, D., Whitworth, A., Battersby, C., Elia, D., Fuller, G. A., DiGiorgio, A., Griffin, M. J., Molinari, S., Martin, P., Mottram, J. C., Peretto, N., Pestalozzi, M., Schisano, E., Smith, H. A., and Thompson, M. A.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

In a previous paper we identified cores within infrared dark clouds (IRDCs). We regarded those without embedded sources as the least evolved, and labelled them starless. Here we identify the most isolated starless cores and model them using a three-dimensional, multi-wavelength, Monte Carlo, radiative transfer code. We derive the cores' physical parameters and discuss the relation between the mass, temperature, density, size and the surrounding interstellar radiation field (ISRF) for the cores. The masses of the cores were found not to correlate with their radial size or central density. The temperature at the surface of a core was seen to depend almost entirely on the level of the ISRF surrounding the core. No correlation was found between the temperature at the centre of a core and its local ISRF. This was seen to depend, instead, on the density and mass of the core., 12 pages + appendix, 12 figures, 4 tables. Only a sample of images in Appendix A is given due to size restrictions. Accepted by MNRAS

Published
2012

45. Cores in Infra-Red Dark Clouds (IRDCs) seen in the Hi-GAL survey between l = 300{\deg} and l = 330{\deg}

Author

Wilcock, L. A., Ward-Thompson, D., Kirk, J. M., Stamatellos, D., Whitworth, A., Elia, D., Fuller, G. A., DiGiorgio, A., Griffin, M. J., Molinari, S., Martin, P., Mottram, J. C., Peretto, N., Pestalozzi, M., Schisano, E., Plume, R., Smith, H. A., and Thompson, M. A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have used data taken as part of the Herschel infrared Galactic Plane survey (Hi-GAL) to study 3171 infrared-dark cloud (IRDC) candidates that were identified in the mid-infrared (8 {\mu}m) by Spitzer (we refer to these as 'Spitzer-dark' regions). They all lie in the range l=300 - 330 \circ and |b| 6 1 \circ. Of these, only 1205 were seen in emission in the far-infrared (250-500 {\mu}m) by Herschel (we call these 'Herschel-bright' clouds). It is predicted that a dense cloud will not only be seen in absorption in the mid-infrared, but will also be seen in emission in the far-infrared at the longest Herschel wavebands (250-500 {\mu}m). If a region is dark at all wavelengths throughout the mid-infrared and far-infrared, then it is most likely to be simply a region of lower background infrared emission (a 'hole in the sky'). Hence, it appears that previous surveys, based on Spitzer and other mid-infrared data alone, may have over-estimated the total IRDC population by a factor of 2. This has implications for estimates of the star formation rate in IRDCs in the Galaxy.We studied the 1205 Herschel-bright IRDCs at 250 {\mu}m, and found that 972 of them had at least one clearly defined 250-{\mu}m peak, indicating that they contained one or more dense cores. Of these, 653 (67 per cent) contained an 8-{\mu}m point source somewhere within the cloud, 149 (15 per cent) contained a 24-{\mu}m point source but no 8-{\mu}m source, and 170 (18 per cent) contained no 24-{\mu}m or 8-{\mu}m point sources. We use these statistics to make inferences about the lifetimes of the various evolutionary stages of IRDCs., Comment: 7 pages (+26 in appendices). Accepted for publication in MNRAS

Published
2012

46. A cluster of outflows in the Vulpecula Rift

Author

Mottram, J. C. and Brunt, C. M.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present $^{12}$CO, $^{13}$CO and C$^{18}$O (J=3$-$2) observations of a new cluster of outflows in the Vulpecula Rift with HARP-B on the JCMT. The mass associated with the outflows, measured using the $^{12}$CO HARP-B observations and assuming a distance to the region of 2.3 kpc, is 129 \msol{}, while the mass associated with the dense gas from C$^{18}$O observations is 458 \msol{} and the associated sub-millimeter core has a mass of 327 $\pm$ 112 \msol{} independently determined from Bolocam 1.1mm data. The outflow-to-core mass ratio is therefore $\sim$0.4, making this region one of the most efficient observed thus far with more than an order of magnitude more mass in the outflow than would be expected based on previous results. The kinetic energy associated with the flows, 94$\times10^{45}$ ergs, is enough to drive the turbulence in the local clump, and potentially unbind the local region altogether. The detection of SiO (J=8$-$7) emission toward the outflows indicates that the flow is still active, and not simply a fossil flow. We also model the SEDs of the four YSOs associated with the molecular material, finding them all to be of mid to early B spectral type. The energetic nature of the outflows and significant reservoir of cold dust detected in the sub-mm suggest that these intermediate mass YSOs will continue to accrete and become massive, rather than reach the main sequence at their current mass., 11 pages, 8 figures and 3 tables. Accepted to MNRAS. A higher-resolution version of figure 1 will be included in the published version and is available from the authors upon request. Updated with red and blue wings swapped to match doppler shift

Published
2011

47. The RMS Survey: Ammonia and water maser analysis of massive star forming regions

Author

Urquhart, J. S., Morgan, L. K., Figura, C. C., Moore, T. J. T., Lumsden, S. L., Hoare, M. G., Oudmaijer, R. D., Mottram, J. C., Davies, B., and Dunham, M. K.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

The Red MSX Source (RMS) survey has identified a sample of ~1200 massive young stellar objects (MYSOs), compact and ultra compact HII regions from a sample of ~2000 MSX and 2MASS colour selected sources. We have used the 100 m Green Bank telescope to search for 22-24 GHz water maser and ammonia (1,1), (2,2) and (3,3) emission towards ~600 RMS sources located within the northern Galactic plane. We have identified 308 H2O masers which corresponds to an overall detection rate of ~50%. Abridged: We detect ammonia emission towards 479 of these massive young stars, which corresponds to ~80%. Ammonia is an excellent probe of high density gas allowing us to measure key parameters such as gas temperatures, opacities, and column densities, as well as providing an insight into the gas kinematics. The average kinetic temperature, FWHM line width and total NH3 column density for the sample are approximately 22 K, 2 km/s and 2x10^{15} cm^{-2}, respectively. We find that the NH3 (1,1) line width and kinetic temperature are correlated with luminosity and finding no underlying dependence of these parameters on the evolutionary phase of the embedded sources, we conclude that the observed trends in the derived parameters are more likely to be due to the energy output of the central source and/or the line width-clump mass relationship. The velocities of the peak H2O masers and the NH3 emission are in excellent agreement with each other, which would strongly suggest an association between the dense gas and the maser emission. Moreover, we find the bolometric luminosity of the embedded source and the isotropic luminosity of the H2O maser are also correlated. We conclude from the correlations of the cloud and water maser velocities and the bolometric and maser luminosity that there is a strong dynamical relationship between the embedded young massive star and the H2O maser., 17 pages and 17 figures and 8 tables. Tables\,2 and 5 and full versions of Figs. 3 and 7 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.125.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/

Published
2011

48. Star formation triggered by H II regions in our Galaxy [Letter]

Author

Zavagno, A., Anderson, L. D., Russeil, D., Morgan, L., Stringfellow, G. S., Deharveng, L., Rodón, J. A., Robitaille, T. P., Mottram, J. C., Schuller, F., Testi, L., Billot, N., Molinari, S., di Gorgio, A., Kirk, Jason M., Brunt, C., Ward-Thompson, Derek, Traficante, A., Veneziani, M., Faustini, F., and Calzoletti, L.

Subjects
QB
Abstract

Context. It has been shown that by means of different physical mechanisms the expansion of H ii regions can trigger the formation of new stars of all masses. This process may be important to the formation of massive stars but has never been quantified in the Galaxy.\ud \ud Aims. We use Herschel-PACS and -SPIRE images from the Herschel infrared survey of the Galactic plane, Hi-GAL, to perform this study.\ud \ud Methods. We combine the Spitzer-GLIMPSE and -MIPSGAL, radio-continuum and submillimeter surveys such as ATLASGAL with Hi-GAL to study young stellar objects (YSOs) observed towards Galactic H ii regions. We select a representative H ii region, N49, located in the field centered on l = 30°observed as part of the Hi-GAL science demonstration phase, to demonstrate the importance Hi-GAL will have to this field of research.\ud \ud Results. Hi-GAL PACS and SPIRE images reveal a new population of embedded young stars, coincident with bright ATLASGAL condensations. The Hi-GAL images also allow us, for the first time, to constrain the physical properties of the newly formed stars by means of fits to their spectral energy distribution. Massive young stellar objects are observed at the borders of the N49 region and represent second generation massive stars whose formation has been triggered by the expansion of the ionized region.\ud \ud Conclusions. The first Hi-GAL images obtained using PACS and SPIRE have demonstrated the capability to investigate star formation triggered by H ii regions. With radio, submillimeter, and shorter wavelength infrared data from other surveys, the Hi-GAL images reveal young massive star-forming clumps surrounding the perimeter of the N49 H ii generated bubble. Hi-GAL enables us to detect a population of young stars at different evolutionary stages, cold condensations only being detected in the SPIRE wavelength range. The far IR coverage of Hi-GAL strongly constrains the physical properties of the YSOs. The large and unbiased spatial coverage of this survey offers us a unique opportunity to lead, for the first time, a global study of star formation triggered by H ii regions in our Galaxy.

Published
2010

49. Clouds, filaments, and protostars: the Herschel/Hi-GAL Milky Way [Letter]

Author

Molinari, S., Swinyard, B., Bally, J., Barlow, M., Bernard, J.-P., Martin, P., Moore, T., Noriega-Crespo, A., Plume, R., Testi, L., Zavagno, A., Abergel, A., Ali, B., Anderson, L., André, P., Baluteau, J.-P., Battersby, C., Beltrán, M. T., Benedettini, M., Billot, N., Blommaert, J., Bontemps, S., Boulanger, F., Brand, J., Brunt, C., Burton, M., Calzoletti, L., Carey, S., Caselli, P., Cesaroni, R., Cernicharo, J., Chakrabarti, S., Chrysostomou, A., Cohen, M., Compiegne, M., de Bernardis, P., de Gasperis, G., di Giorgio, A. M., Elia, D., Faustini, F., Flagey, N., Fukui, Y., Fuller, G. A., Ganga, K., Garcia-Lario, P., Glenn, J., Goldsmith, P. F., Griffin, Matthew Joseph, Hoare, M., Huang, M., Ikhenaode, D., Joblin, C., Joncas, G., Juvela, M., Kirk, Jason M., Lagache, G., Li, J. Z., Lim, T. L., Lord, S. D., Marengo, M., Marshall, D. J., Masi, S., Massi, F., Matsuura, Mikako, Minier, V., Miville-Deschênes, M.-A., Montier, L. A., Morgan, L., Motte, F., Mottram, J. C., Müller, T. G., Natoli, P., Neves, J., Olmi, L., Paladini, R., Paradis, D., Parsons, H., Peretto, Nicolas, Pestalozzi, M., Pezzuto, S., Piacentini, F., Piazzo, L., Polychroni, D., Pomarès, M., Popescu, C. C., Reach, W. T., Ristorcelli, I., Robitaille, J.-F., Robitaille, T., Rodón, J. A., Roy, A., Royer, P., Russeil, D., Saraceno, P., Sauvage, M., Schilke, P., Schisano, E., Schneider, N., Schuller, F., Schulz, B., Sibthorpe, Bruce, Smith, H. A., Smith, M. D., Spinoglio, L., Stamatelos, Dimitrios, Strafella, F., Stringfellow, G. S., Sturm, E., Taylor, R., Thompson, M. A., Traficante, A., Tuffs, R. J., Umana, G., Valenziano, L., Vavrek, R., Veneziani, M., Viti, S., Waelkens, C., Ward-Thompson, Derek, White, G., Wilcock, Lucy Ann, Wyrowski, F., Yorke, H. W., and Zhang, Q.

Abstract

We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key program that will map the inner Galactic plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2° × 2° tiles approximately centered at l = 30° and l = 59°. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around AV ~ 1 is exceeded for the regions in the l = 59° field; a AV value between 5 and 10 is found for the l = 30° field, likely due to the relatively higher distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.

Published
2010

50. The RMS Survey: Radio and mid-IR observations of candidate massive YSOs

Author

Mottram, J. C., Urquhart, J. S., Hoare, M. G., Lumsden, S. L., and Oudmaijer, R. D.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

The Red MSX Source (RMS) survey is a multi-wavelength programme of follow-up observations designed to distinguish between genuine massive young stellar objects (MYSOs) and other embedded or dusty objects, such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe), from a sample of ~2000 MYSOs candidates. These were identified by comparing the colours of objects from the MSX and 2MASS point source catalogues to those of known MYSOs, in order to develop colour selection criteria which have been used to produced the RMS sample of MYSOs candidates. Our ultimate aim is to produce a large unbiased sample of MYSOs (~500) with complementary multi-wavelength data with which to study their properties. Here we report the results of 826 radio continuum and 346 mid-IR imaging observations carried out using the Australia Telescope Compact Array and TIMMI2 on the ESO 3.6 m telescope respectively. These observations are aimed at identifying and removing contaminating sources., 5 pages, 2 figures, to be published in the proceedings of Interactions of Stars with their Environments III 2006

Published
2006

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