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1. A panoptic view of the Taurus molecular cloud I. The cloud dynamics revealed by gas emission and 3D dust

Author

Soler, J. D., Zucker, C., Peek, J. E. G., Heyer, M., Goldsmith, P. F., Glover, S. C. O., Molinari, S., Klessen, R. S., Hennebelle, P., Testi, L., Colman, T., Benedettini, M., Elia, D., Mininni, C., Pezzuto, S., Schisano, E., and Traficante, A.

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present a study of the three-dimensional (3D) distribution of interstellar dust derived from stellar extinction observations toward the Taurus molecular cloud (MC) and its relation with the neutral atomic hydrogen (HI) emission at 21 cm wavelength and the carbon monoxide $^{12}$CO and $^{13}$CO emission in the $J=1\rightarrow0$ transition. We used the histogram of oriented gradients (HOG) method to match the morphology in a 3D reconstruction of the dust density (3D dust) and the distribution of the gas tracers' emission. The result of the HOG analysis is a map of the relationship between the distances and radial velocities. The HOG comparison between the 3D dust and the HI emission indicates a morphological match at the distance of Taurus but an anti-correlation between the dust density and the HI emission, which uncovers a significant amount of cold HI within the Taurus MC. The HOG between the 3D dust and $^{12}$CO reveals a pattern in radial velocities and distances that is consistent with converging motions of the gas in the Taurus MC, with the near side of the cloud moving at higher velocities and the far side moving at lower velocities. This convergence of flows is likely triggered by the large-scale gas compression caused by the interaction of the Local Bubble and the Per-Tau shell, with Taurus lying at the intersection of the two bubble surfaces., 18 pages, 21 figures. Accepted for publication in Astronomy & Astrophysics (22MAY2023)

Published
2023

2. The GUAPOS project:III. Characterization of the O- and N-bearing complex organic molecules content and search for chemical differentiation

Author

Mininni, C., Beltrán, M. T., Colzi, L., Rivilla, V. M., Fontani, F., Lorenzani, A., López-Gallifa, Á., Viti, S., Sánchez-Monge, Á., Schilke, P., and Testi, L.

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 G31.41+0.31 Unbiased ALMA sPectral Observational Survey (GUAPOS) project targets the hot molecular core (HMC) G31.41+0.31 (G31), to unveil the complex chemistry of one of the most chemically rich high-mass star-forming regions outside the Galactic Center (GC). In the third paper of the project, we present a study of nine O-bearing (CH$_3$OH, $^{13}$CH$_3$OH, CH$_3^{18}$OH, CH$_3$CHO, CH$_3$OCH$_3$, CH$_3$COCH$_3$ , C$_2$H$_5$OH, aGg'-(CH$_2$OH)$_2$, and gGg'-(CH$_2$OH)$_2$) and six N-bearing (CH$_3$CN, $^{13}$CH$_3$CN, CH$_3^{13}$CN, C$_2$H$_3$CN, C$_2$H$_5$CN, and C$_2$H$_5^{13}$CN) complex organic molecules toward G31. The aim of this work is to characterize the abundances in one of the most chemically-rich hot molecular cores outside the GC and to search for a possible chemical segregation between O-bearing and N-bearing species in G31, which hosts four compact sources as seen with higher angular resolution data. Observations were carried out with the interferometer ALMA and covered the entire Band 3 from 84 to 116 GHz ($\sim 32$ GHz bandwidth) with an angular resolution of $1.2''$ ($\sim4400\,\mathrm{au}$). The spectrum has been analyzed with the tool SLIM of MADCUBA to determine the physical parameters of the emitting gas. Moreover, we have analyzed the morphology of the emission of the molecular species. We have compared the abundances w.r.t methanol of COMs in G31 with other twenty-seven sources, including other hot molecular cores inside and outside the Galactic Center, hot corinos, shocked regions, envelopes around young stellar objects, and quiescent molecular clouds, and with chemical models. Different species peak at slightly different positions, and this, together with the different central velocities of the lines obtained from the spectral fitting, point to chemical differentiation of selected O-bearing species., Comment: accepted for publication in A&A, 39 pages

Published
2023
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3. FAUST X. Multi-band, multi-scale dust study of L1527 IRS. Evidence for dust properties variations within the envelope of a Class 0/I YSO

Author

Cacciapuoti, L., Macias, E., Maury, A. J., Chandler, C. J., Sakai, N., Tychoniec, Ł., Viti, S., Natta, A., De Simone, M., Miotello, A., Codella, C., Ceccarelli, C., Podio, L., Fedele, D., Johnstone, D., Shirley, Y., Liu, B. J., Bianchi, E., Zhang, Z. E., Pineda, J., Loinard, L., Ménard, F., Lebreuilly, U., Klessen, R. S., Hennebelle, P., Molinari, S., Testi, L., and Yamamoto, S.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), 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), Astrophysics - Earth and Planetary Astrophysics
Abstract

Early dust grain growth in protostellar envelopes infalling on young discs has been suggested in recent studies, supporting the hypothesis that dust particles start to agglomerate already during the Class 0/I phase of young stellar objects (YSOs). If this early evolution were confirmed, it would impact the usually assumed initial conditions of planet formation, where only particles with sizes $\lesssim 0.25 \mu$m are usually considered for protostellar envelopes. We aim to determine the maximum grain size of the dust population in the envelope of the Class 0/I protostar L1527 IRS, located in the Taurus star-forming region (140 pc). We use Atacama Large millimetre/sub-millimetre Array (ALMA) and Atacama Compact Array (ACA) archival data and present new observations, in an effort to both enhance the signal-to-noise ratio of the faint extended continuum emission and properly account for the compact emission from the inner disc. Using observations performed in four wavelength bands and extending the spatial range of previous studies, we aim to place tight constraints on the spectral ($\alpha$) and dust emissivity ($\beta$) indices in the envelope of L1527 IRS. We find a rather flat $\alpha \sim$ 3.0 profile in the range 50-2000 au. Accounting for the envelope temperature profile, we derive values for the dust emissivity index, 0.9 < $\beta$ < 1.6, and reveal a tentative, positive outward gradient. This could be interpreted as a distribution of mainly ISM-like grains at 2000 au, gradually progressing to (sub-)millimetre-sized dust grains in the inner envelope, where at R=300 au, $\beta$ = 1.1 +/- 0.1. Our study supports a variation of the dust properties in the envelope of L1527 IRS. We discuss how this can be the result of in-situ grain growth, dust differential collapse from the parent core, or upward transport of disc large grains., Comment: Accepted for publication in A&A. Contains 18 pages, 21 figures, 5 tables

Published
2023
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4. Synthetic dust polarization emission maps at 353 GHz for an observer placed inside a Local Bubble-like cavity

Author

Maconi, E., Soler, J. D., Reissl, S., Girichidis, P., Klessen, R. S., Hennebelle, P., Molinari, S., Testi, L., Smith, R. J., Sormani, M. C., Teh, J. W., and Traficante, A.

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

We present a study of synthetic observations of polarized dust emission at 353 GHz as seen by an observer within a cavity in the interstellar medium (ISM). The cavity is selected from a magnetohydrodynamic simulation of the local ISM with time-dependent chemistry, star formation, and stellar feedback in form of supernova explosions with physical properties comparable to the Local Bubble ones. We find that the local density enhancement together with the coherent magnetic field in the cavity walls makes the selected candidate a translucent polarization filter to the emission coming from beyond its domains. This underlines the importance of studying the Local Bubble in further detail. The magnetic field lines inferred from synthetic dust polarization data are qualitatively in agreement with the all-sky maps of polarized emission at 353 GHz from the Planck satellite in the latitudes interval 15deg 65deg. We show that from our synthetic polarization maps, it is difficult to distinguish between an open and a closed Galactic cap using the inferred magnetic field morphology alone.

Published
2022

5. Mass ejection and time variability in protostellar outflows: Cep E. SOLIS XVI

Author

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

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

Protostellar jets are an important agent of star formation feedback, tightly connected with the mass-accretion process. The history of jet formation and mass-ejection provides constraints on the mass accretion history and the nature of the driving source. We want to characterize the time-variability of the mass-ejection phenomena at work in the Class 0 protostellar phase, in order to better understand the dynamics of the outflowing gas and bring more constraints on the origin of the jet chemical composition and the mass-accretion history. We have observed the emission of the CO 2-1 and SO N_J=5_4-4_3 rotational transitions with NOEMA, towards the intermediate-mass Class 0 protostellar system Cep E. The CO high-velocity jet emission reveals a central component associated with high-velocity molecular knots, also detected in SO, surrounded by a collimated layer of entrained gas. The gas layer appears to accelerate along the main axis over a length scale delta_0 ~700 au, while its diameter gradually increases up to several 1000au at 2000au from the protostar. The jet is fragmented into 18 knots of mass ~10^-3 Msun, unevenly distributed between the northern and southern lobes, with velocity variations up to 15 km/s close to the protostar, well below the jet terminal velocities. The knot interval distribution is approximately bimodal with a scale of ~50-80yr close to the protostar and ~150-200yr at larger distances >12". The mass-loss rates derived from knot masses are overall steady, with values of 2.7x10^-5 Msun/yr (8.9x10^-6 Msun/yr) in the northern (southern) lobe. The interaction of the ambient protostellar material with high-velocity knots drives the formation of a molecular layer around the jet, which accounts for the higher mass-loss rate in the north. The jet dynamics are well accounted for by a simple precession model with a period of 2000yr and a mass-ejection period of 55yr., 13 pages, 9 figures, 3 table. Accepted in A&A

Published
2022

6. Hot methanol in the [BHB2007] 11 protobinary system: hot corino versus shock origin? : FAUST V

Author

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

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

Methanol is a ubiquitous species commonly found in the molecular interstellar medium. It is also a crucial seed species for the building-up of the chemical complexity in star forming regions. Thus, understanding how its abundance evolves during the star formation process and whether it enriches the emerging planetary system is of paramount importance. We used new data from the ALMA Large Program FAUST (Fifty AU STudy of the chemistry in the disk/envelope system of Solar-like protostars) to study the methanol line emission towards the [BHB2007] 11 protobinary system (sources A and B), where a complex structure of filaments connecting the two sources with a larger circumbinary disk has been previously detected. Twelve methanol lines have been detected with upper energies in the range [45-537] K along with one 13CH3OH transition. The methanol emission is compact and encompasses both protostars, separated by only 28 au and presents three velocity components, not spatially resolved by our observations, associated with three different spatial regions, with two of them close to 11B and the third one associated with 11A. A non-LTE radiative transfer analysis of the methanol lines concludes that the gas is hot and dense and highly enriched in methanol with an abundance as high as 1e-5. Using previous continuum data, we show that dust opacity can potentially completely absorb the methanol line emission from the two binary objects. Although we cannot firmly exclude other possibilities, we suggest that the detected hot methanol is resulting from the shocked gas from the incoming filaments streaming towards [BHB2007] 11 A and B, respectively. Higher spatial resolution observations are necessary to confirm this hypothesis., Comment: 17 pages, accepted in A&A

Published
2022
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7. CHEMOUT: CHEMical complexity in star-forming regions of the OUTer Galaxy. I. Organic molecules and tracers of star-formation activity

Author

Fontani, F., Colzi, L., Bizzocchi, L., Rivilla, V. M., Elia, D., Beltrán, M. T., Caselli, P., Magrini, L., Sánchez-Monge, A., Testi, L., Romano, D., F. Fontani, L. Colzi, L. Bizzocchi, V. M. Rivilla, D. Elia, M. T. Beltrán, P. Caselli, L. Magrini, A. Sánchez-Monge, L. Testi, and D. Romano

Subjects
radio lines: ISM, stars: formation, Space and Planetary Science, ISM: cloud, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, ISM: molecule, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

The outer Galaxy is an environment with metallicity lower than the Solar one. Because of this, the formation and survival of molecules in star-forming regions located in the inner and outer Galaxy is expected to be different. To gain understanding on how chemistry changes throughout the Milky Way, it is crucial to observe outer Galaxy star-forming regions to constrain models adapted for lower metallicity environments. In this paper we present a new observational project: chemical complexity in star-forming regions of the outer Galaxy (CHEMOUT). The goal is to unveil the chemical composition in 35 dense molecular clouds associated with star-forming regions of the outer Galaxy through observations obtained with the IRAM 30m telescope. In this first paper, we present the sample, and report the detection at 3~mm of simple organic species HCO+, H13CO+, HCN, c-C3H2, HCO, C4H, and HCS+, of the complex hydrocarbon CH3CCH, and of SiO, CCS and SO. From c-C3H2, we estimate new kinematic heliocentric and Galactocentric distances based on an updated rotation curve of the Galaxy. The detection of the molecular tracers does not seem to have a clear dependence on the Galactocentric distance. We also analyse the HCO+ line profiles. We find high velocity wings in ~71% of the targets, and their occurrence does not depend on the Galactocentric distance. Our results, confirmed by a statistical analysis, show that the presence of organic molecules and tracers of protostellar activity is ubiquitous in the low-metallicity environment of the outer Galaxy. Based on this, and on the additional evidence that small, terrestrial planets are omnipresent in the Galaxy, we support previous claims that the definition of Galactic Habitable Zone should be rediscussed in view of the ubiquitous capacity of the interstellar medium to form organic molecules., Comment: 11 pages, 5 figures, 3 appendices, accepted for publication in A&A

Published
2022
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8. PENELLOPE: the ESO data legacy program to complement the Hubble UV Legacy Library of Young Stars (ULLYSES) I. Survey presentation and accretion properties of Orion OB1 and $��$-Orionis

Author

Manara, C. F., Frasca, A., Venuti, L., Siwak, M., Herczeg, G. J., Calvet, N., Hernandez, J., Tychoniec, ��., Gangi, M., Alcal��, J. M., Boffin, H. M. J., Nisini, B., Robberto, M., Briceno, C., Campbell-White, J., Sicilia-Aguilar, A., McGinnis, P., Fedele, D., K��sp��l, ��., ��brah��m, P., Alonso-Santiago, J., Antoniucci, S., Arulanantham, N., Bacciotti, F., Banzatti, A., Beccari, G., Benisty, M., Biazzo, K., Bouvier, J., Cabrit, S., Garatti, A. Caratti o, Coffey, D., Covino, E., Dougados, C., Eisl��ffel, J., Ercolano, B., Espaillat, C. C., Erkal, J., Facchini, S., Fang, M., Fiorellino, E., Fischer, W. J., France, K., Gameiro, J. F., Lopez, R. Garcia, Giannini, T., Ginski, C., Grankin, K., G��nther, H. M., Hartmann, L., Hillenbrand, L. A., Hussain, G. A. J., James, M. M., Koutoulaki, M., Lodato, G., Mauc��, K., Mendigut��a, I., Mentel, R., Miotello, A., Oudmaijer, R. D., Rigliaco, E., Rosotti, G. P., Sanchis, E., Schneider, P. C., Spina, L., Stelzer, B., Testi, L., Thanathibodee, T., Vink, J. S., Walter, F. M., Williams, J. P., and Zsidi, G.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The evolution of young stars and disks is driven by the interplay of several processes, notably accretion and ejection of material. Critical to correctly describe the conditions of planet formation, these processes are best probed spectroscopically. About five-hundred orbits of the Hubble Space Telescope (HST) are being devoted in 2020-2022 to the ULLYSES public survey of about 70 low-mass (M, Accepted for publication on Astronomy & Astrophysics. 15 pages + appendix, language edited version

Published
2021
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9. X-Shooter survey of disk accretion in Upper Scorpius I. Very high accretion rates at age>5 Myr

Author

Manara, C. F., Natta, A., Rosotti, G. P., Alcala, J. M., Nisini, B., Lodato, G., Testi, L., Pascucci, I., Hillenbrand, L., Carpenter, J., Scholz, A., Fedele, D., Frasca, A., Mulders, G., Rigliaco, E., Scardoni, C., and Zari, E.

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

Determining the mechanisms that drive the evolution of protoplanetary disks is a necessary step to understand how planets form. Here we measured the mass accretion rate for young stellar objects at age >5 Myr, a critical test for the current models of disk evolution. We present the analysis of the spectra of 36 targets in the ~5-10 Myr old Upper Scorpius region for which disk masses were measured with ALMA. We find that the mass accretion rates in this sample of old but still survived disks are similarly high as those of the younger (10^-9 Msun/yr while having low disk masses. Furthermore, the median values of the measured mass accretion rates in the disk mass ranges where our sample is complete at a level ~60-80% are compatible in these three regions. At the same time, the spread of mass accretion rates at any given disk mass is still >0.9 dex even at age>5 Myr. These results are in contrast with simple models of viscous evolution, which would predict that the values of the mass accretion rate diminish with time, and a tighter correlation with disk mass at age>5 Myr. Similarly, simple models of internal photoevaporation cannot reproduce the observed mass accretion rates, while external photoevaporation might explain the low disk masses and high accretion rates. A partial possible solution to the discrepancy with the viscous models is that the gas-to-dust ratio of the disks at >5 Myr is significantly different and higher than the canonical 100, as suggested by some dust and gas disk evolution models. The results shown here require the presence of several inter-playing processes, such as detailed dust evolution, external photoevaporation and possibly MHD winds, to explain the secular evolution of protoplanetary disks., Accepted on Astronomy & Astrophysics. Language edited version

Published
2020
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10. Bipolar molecular outflow of the very low-mass star Par-Lup3-4

Author

Santamaría-Miranda, A., de Gregorio-Monsalvo, I., Huélamo, N., Plunkett, A. L., Ribas, Á., Comerón, F., Schreiber, M. R., López, C., Mužić, K., and Testi, L.

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

Very low-mass stars are known to have jets and outflows, which is indicative of a scaled-down version of low-mass star formation. However, only very few outflows in very low-mass sources are well characterized. We characterize the bipolar molecular outflow of the very low-mass star Par-Lup3-4, a 0.12 M$_{\odot}$ object known to power an optical jet. We observed Par-Lup3-4 with ALMA in Bands 6 and 7, detecting both the continuum and CO molecular gas. In particular, we studied three main emission lines: CO(2-1), CO(3-2), and $^{13}$CO(3-2). Our observations reveal for the first time the base of a bipolar molecular outflow in a very low-mass star, as well as a stream of material moving perpendicular to the primary outflow of this source. The primary outflow morphology is consistent with the previously determined jet orientation and disk inclination. The outflow mass is $9.5\times10^{-7}\mathrm{M}_{\odot}$ , with an outflow rate of $4.3\times10^{-9}\mathrm{M}_{\odot}\mathrm{yr}^{-1}$ A new fitting to the spectral energy distribution suggests that Par-Lup3-4 may be a binary system. We have characterized Par-Lup3-4 in detail, and its properties are consistent with those reported in other very low-mass sources. This source provides further evidence that very low-mass sources form as a scaled-down version of low-mass stars., Comment: 20 pages, 11 figures, 5 tables. Accepted in A&A

Published
2020
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11. The ALMA Development Roadmap

Author

Carpenter, J., Iono, D., Testi, L., Whyborn, N., Wootten, A., and Evans, N.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The present document outlines a roadmap for future developments that will significantly expand ALMA's capabilities and enable it to produce even more exciting science in the coming decades. The proposed developments are motivated by the groundbreaking results achieved by ALMA during its first five years of operation. The roadmap described here is based on input on new scientific directions and technical feasibility of future developments from the ALMA Science Advisory Committee (ASAC), the community, and technical documents. The Working Group recommends that the top development priority, based on scientific merit and technical feasibility, is to broaden the receiver IF bandwidth by at least a factor two, and to upgrade the associated electronics and correlator. These developments will advance a wide range of scientific studies by significantly reducing the time required for blind redshift surveys, chemical spectral scans, and deep continuum surveys. In order of scientific priority, receiver upgrades are recommended for intermediate (200-425 GHz), low (< 200 GHz), and high (> 425 GHz) frequencies. The Working Group recommends that the receiver and throughput developments proceed as soon as fiscally and technically feasible. As a first step, a technical and scientific group should be formed to formalize the top-level requirements. A team of systems engineers should then be charged with flowing these requirements down to the subsystems to form a consistent new set of minimum requirements, which future development projects would have to meet. Given that upgrading the throughput will impact many ALMA subsystems, the Working Group recommends that a team within ALMA be charged with coordinating and monitoring these developments. (Abbreviated), Approved by the ALMA Board by written procedure pursuant Article 11 of the Board's Rules of Procedure Abstract abbreviated to fit arXiv constraints

Published
2019

12. The Forgotten Quadrant Survey. $^{12}$CO and $^{13}$CO (1-0) survey of the Galactic Plane in the range 220��$

Author

Benedettini, M., Molinari, S., Baldeschi, A., Beltran, M. T., Brand, J., Cesaroni, R., Elia, D., Fontani, F., Merello, M., Olmi, L., Pezzuto, S., Rygl, K. L. J., Schisano, E., Testi, L., and Traficante, A.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present the Forgotten Quadrant Survey (FQS), an ESO large project that used the 12m antenna of the Arizona Radio Observatory to map the Galactic Plane in the range 220��$, 16 pages, 17 figures, accepted for publication in Astronomy and Astrophysics

Published
2019
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13. Bright C2H emission in protoplanetary disks in Lupus: high volatile C/O>1 ratios

Author

Miotello, A., Facchini, S., van Dishoeck, E. F., Cazzoletti, P., Testi, L., Williams, J. P., Ansdell, M., van Terwisga, S., and van der Marel, N.

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

ALMA surveys have shown that CO emission in protoplanetary disks is much fainter than expected. Accordingly, CO-based gas masses and gas/dust ratios are orders of magnitude lower than previously thought. This may be explained either as fast gas dispersal, or as chemical evolution and locking up of volatiles in larger bodies leading to the low observed CO fluxes. The latter processes lead to enhanced C/O ratios in the gas, which may be reflected in enhanced abundances of molecules like C2H. The goal of this work is to employ C2H observations to understand whether low CO fluxes are caused by volatile depletion, or by fast gas dissipation. We present ALMA Cycle 4 C2H observations of a subsample of nine sources in Lupus. The integrated C2H emission is determined and compared to previous CO observations and model predictions. Seven out of nine disks are detected in C2H, whose line emission is almost as bright as 13CO. All detections are significantly brighter than the typical sensitivity of the observations, hinting at a bimodal distribution of the C2H line intensities. When compared with DALI models, the observed C2H fluxes can be reproduced only if some level of volatile carbon and oxygen depletion is allowed and C/O>1 in the gas. Models with reduced gas/dust ratios fail instead to reproduce the observations. A steeper than linear correlation between C2H and CN emission line is found. This is linked to the fact that C2H emission lines are affected more strongly by C/O variations than CN lines. Ring-like structures are detected both in C2H and in continuum emission but, as for CN, they do not seem to be connected. Sz 71 shows ring shaped emission in both C2H and CN with the location of the peak intensity coinciding. Our new ALMA C2H observations favour volatile carbon and oxygen depletion rather than fast gas dispersal to explain the faint CO observations for most of the disks., 11 pages, 12 figures, accepted for publication on A&A

Published
2019
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14. SOLIS II. Carbon-chain growth in the Solar-type protocluster OMC2-FIR4

Author

Fontani, F., Ceccarelli, C., Favre, C., Caselli, P., Neri, R., Sims, I. R., Kahane, C., Alves, F., Balucani, N., Bianchi, E., Caux, E., Al-Edhari, A. Jaber, Lopez-Sepulcre, A., Pineda, J. E., Bachiller, R., Bizzocchi, L., Bottinelli, S., Chacon-Tanarro, A., Choudhury, R., Codella, C., Coutens, A., Dulieu, F., Feng, S., Rimola, A., Hily-Blant, P., Holdship, J., Jimenez-Serra, I., Laas, J., Lefloch, B., Oya, Y., Podio, L., Pon, A., Punanova, A., Quenard, D., Sakai, N., Spezzano, S., Taquet, V., Testi, L., Theul��, P., Ugliengo, P., Vastel, C., Vasyunin, A. I., Viti, S., Yamamoto, S., and Wiesenfeld, L.

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 interstellar delivery of carbon atoms locked into molecules might be one of the key ingredients for the emergence of life. Cyanopolyynes are carbon chains delimited at their two extremities by an atom of hydrogen and a cyano group, so that they might be excellent reservoirs of carbon. The simplest member, HC3N, is ubiquitous in the galactic interstellar medium and found also in external galaxies. Thus, understanding the growth of cyanopolyynes in regions forming stars similar to our Sun, and what affects it, is particularly relevant. In the framework of the IRAM/NOEMA Large Program SOLIS (Seeds Of Life In Space), we have obtained a map of two cyanopolyynes, HC3N and HC5N, in the protocluster OMC2-FIR4. Because our Sun is thought to be born in a rich cluster, OMC2-FIR4 is one of the closest and best known representatives of the environment in which the Sun may have been born. We find a HC3N/HC5N abundance ratio across the source in the range ~ 1 - 30, with the smallest values (< 10) in FIR5 and in the Eastern region of FIR4. The ratios < 10 can be reproduced by chemical models only if: (1) the cosmic-ray ionisation rate $��$ is ~ $4 \times 10^{-14}$ s$^{-1}$; (2) the gaseous elemental ratio C/O is close to unity; (3) O and C are largely depleted. The large $��$ is comparable to that measured in FIR4 by previous works and was interpreted as due to a flux of energetic (> 10 MeV) particles from embedded sources. We suggest that these sources could lie East of FIR4 and FIR5. A temperature gradient across FIR4, with T decreasing by about 10 K, could also explain the observed change in the HC3N/HC5N line ratio, without the need of a cosmic ray ionisation rate gradient. However, even in this case, a high constant cosmic-ray ionisation rate (of the order of $10^{-14}$ s$^{-1}$) is necessary to reproduce the observations., 12 pages, 8 figures, accepted for publication in A&A

Published
2017

15. SEDIGISM: Structure, excitation, and dynamics of the inner Galactic interstellar medium

Author

Schuller, F., Csengeri, T., Urquhart, S., Duarte-Cabral, A., Barnes, P. J., Giannetti, A., Hernandez, A. K., Leurini, S., Mattern, M., Medina, S.-N. X., Agurto, C., Azagra, F., Anderson, L. D., Beltrán, M. T., Beuther, H., Bontemps, Sylvain, Bronfman, L., Dobbs, L., Dumke, M., Finger, R., Ginsburg, A., Gonzalez, E., Henning, T., Kauffmann, J., Mac-Auliffe, F., Menten, M., Montenegro-Montes, F. M., Moore, T. J. T., Muller, E., Parra, R., Perez-Beaupuits, P., Pettitt, A., Russeil, D., Sánchez-Monge, Á., Schilke, P., Schisano, E., Suri, S., Testi, L., Torstensson, K., Venegas, P., Wang, K., Wienen, M., Wyrowski, F., Zavagno, Annie, Urquhart, J. S., Dobbs, C. L., Menten, K. M., Perez-Beaupuits, J.-P., Max-Planck-Institut für Radioastronomie (MPIFR), Institut de Veille Sanitaire (INVS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), European Southern Observatory (ESO), Laboratoire de recherche en Electronique, Electrotechnique et Systèmes (L2ES), Institut National de Recherche sur les Transports et leur Sécurité (INRETS)-Université de Technologie de Belfort-Montbeliard (UTBM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), NASA Goddard Space Flight Center (GSFC), Laboratoire Dynamique de la Biodiversité (LADYBIO), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Haemophilia Unit, Vall d'Hebron University Hospital [Barcelona], Laboratoire d'Astrophysique de Marseille (LAM), 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), Physikalisches Institut [Köln], Universität zu Köln, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), University of Oxford [Oxford], School of Physics and Astronomy, University of Exceter, University of Exceter, Millimeter and Submillimeter Astronomy, Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), 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), Universität zu Köln = University of Cologne, and University of Oxford

Subjects
Infrared, ISM: structure, Rotational transition, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM: clouds, surveys, 0103 physical sciences, Isotopologue, 010303 astronomy & astrophysics, Galaxy: structure, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, radio lines: ISM, 010308 nuclear & particles physics, Molecular cloud, Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Data reduction
Abstract

The origin and life-cycle of molecular clouds are still poorly constrained, despite their importance for understanding the evolution of the interstellar medium. We have carried out a systematic, homogeneous, spectroscopic survey of the inner Galactic plane, in order to complement the many continuum Galactic surveys available with crucial distance and gas-kinematic information. Our aim is to combine this data set with recent infrared to sub-millimetre surveys at similar angular resolutions. The SEDIGISM survey covers 78 deg^2 of the inner Galaxy (-60 deg < l < +18 deg, |b| < 0.5 deg) in the J=2-1 rotational transition of 13CO. This isotopologue of CO is less abundant than 12CO by factors up to 100. Therefore, its emission has low to moderate optical depths, and higher critical density, making it an ideal tracer of the cold, dense interstellar medium. The data have been observed with the SHFI single-pixel instrument at APEX. The observational setup covers the 13CO(2-1) and C18O(2-1) lines, plus several transitions from other molecules. The observations have been completed. Data reduction is in progress, and the final data products will be made available in the near future. Here we give a detailed description of the survey and the dedicated data reduction pipeline. Preliminary results based on a science demonstration field covering -20 deg < l < -18.5 deg are presented. Analysis of the 13CO(2-1) data in this field reveals compact clumps, diffuse clouds, and filamentary structures at a range of heliocentric distances. By combining our data with data in the (1-0) transition of CO isotopologues from the ThrUMMS survey, we are able to compute a 3D realization of the excitation temperature and optical depth in the interstellar medium. Ultimately, this survey will provide a detailed, global view of the inner Galactic interstellar medium at an unprecedented angular resolution of ~30"., 30 pages. Accepted for publication in A&A. Abstract slightly shortened due to arXiv requirements

Published
2017
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16. 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., Beltr��n, M. T., Billot, N., Cambr��sy, L., Cesaroni, R., Garc��a-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., M��ge, 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 of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 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 $��$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 $��$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., Accepted by MNRAS

Published
2017
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17. ALMA Cycle 0 Publication Statistics

Author

Stoehr, F., Uta Grothkopf, Meakins, S., Bishop, M., Uchida, A., Testi, L., Iono, D., Tatematsu, K., and Wootten, A.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The scientific impact of a facility is the most important measure of its success. Monitoring and analysing the scientific return can help to modify and optimise operations and adapt to the changing needs of scientific research. The methodology that we have developed to monitor the scientific productivity of the ALMA Observatory, as well as the first results, are described. We focus on the outcome of the first cycle (Cycle 0) of ALMA Early Science operations. Despite the fact that only two years have passed since the completion of Cycle 0 and operations have already changed substantially, this analysisconfirms the effectiveness of the underlying concepts. We find that ALMA is fulfilling its promise as a transformational facility for the observation of the Universe in the submillimetre., 5 pages, 9 figures

Published
2016

18. The Science Case for ALMA Band 2 and Band 2+3

Author

Fuller, G. A., Avison, A., Beltran, M., Casasola, V., Caselli, P., Cicone, C., Costagliola, F., Breuck, C., Hunt, L., Jimenez-Serra, I., Laing, R., Longmore, S., Massardi, M., Tony Mroczkowski, Paladino, R., Ramstedt, S., Richards, A., Testi, L., Vergani, D., Viti, S., and Wagg, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We discuss the science drivers for ALMA Band 2 which spans the frequency range from 67 to 90 GHz. The key science in this frequency range are the study of the deuterated molecules in cold, dense, quiescent gas and the study of redshifted emission from galaxies in CO and other species. However, Band 2 has a range of other applications which are also presented. The science enabled by a single receiver system which would combine ALMA Bands 2 and 3 covering the frequency range 67 to 116 GHz, as well as the possible doubling of the IF bandwidth of ALMA to 16 GHz, are also considered., Comment: 27 pages, Report submitted to ESO; 3rd version includes updates to the Band 2+3 science, including adding a new section on observations of variable solar system objects

Published
2016
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19. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues. First data release for Inner Milky Way: +68��> l > -70��

Author

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

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

(Abridged) We present the first public release of high-quality data products (DR1) from Hi-GAL, the {\em 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 micron, encompassing the peak of the spectral energy distribution of cold dust for 8 < T < 50K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68�� > l > -70�� in a |b, Astronomy & Astrophysics, accepted

Published
2016
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20. A nebular analysis of the central Orion Nebula with MUSE

Author

Leod, A. F. Mc, Weilbacher, P. M., Ginsburg, A., Dale, J. E., Ramsay, S., and Testi, L.

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

A nebular analysis of the central Orion Nebula and its main structures is presented. We exploit MUSE integral field observations in the wavelength range 4595-9366 \r{A} to produce the first O, S and N ionic and total abundance maps of a region spanning 6' x 5' with a spatial resolution of 0.2". We use the S$_{23}$ ( = ([SII]$\lambda$6717,31+[SIII]$\lambda$9068)/H$\beta$) parameter, together with [OII]/[OIII] as an indicator of the degree of ionisation, to distinguish between the various small-scale structures. The only Orion Bullet covered by MUSE is HH 201, which shows a double component in the [FeII]$\lambda$8617 line throughout indicating an expansion, and we discuss a scenario in which this object is undergoing a disruptive event. We separate the proplyds located south of the Bright Bar into four categories depending on their S$_{23}$ values, propose the utility of the S$_{23}$ parameter as an indicator of the shock-contribution to the excitation of line-emitting atoms, and show that the MUSE data is able to identify the proplyds associated with disks and microjets. We compute the second order structure function for the H$\alpha$, [OIII]$\lambda$5007, [SII]$\lambda$6731 and [OI]$\lambda$6300 emission lines to analyse the turbulent velocity field of the region covered with MUSE. We find that the spectral and spatial resolution of MUSE is not able to faithfully reproduce the structure functions of previous works., Comment: 34 pages, 31 figures, published in MNRAS, added missing citation

Published
2015

21. An Overview of the 2014 ALMA Long Baseline Campaign

Author

Partnership, ALMA, Fomalont, E. B., Vlahakis, C., Corder, S., Remijan, A., Barkats, D., Lucas, R., Hunter, T. R., Brogan, C. L., Asaki, Y., Matsushita, S., Dent, W. R. F., Hills, R. E., Phillips, N., Richards, A. M. S., Cox, P., Amestica, R., Broguiere, D., Cotton, W., Hales, A. S., Hiriart, R., Hirota, A., Hodge, J. A., Impellizzeri, C. M. V., Kern, J., Kneissl, R., Liuzzo, E., Marcelino, N., Marson, R., Mignano, A., Nakanishi, K., Nikolic, B., Perez, J. E., P��rez, L. M., Toledo, I., Aladro, R., Butler, B., Cortes, J., Cortes, P., Dhawan, V., Di Francesco, J., Espada, D., Galarza, F., Garcia-Appadoo, D., Guzman-Ramirez, L., Humphreys, E. M., Jung, T., Kameno, S., Laing, R. A., Leon, S., Mangum, J., Marconi, G., Nagai, H., Nyman, L. -A., Radiszcz, M., Rod��n, J. A., Sawada, T., Takahashi, S., Tilanus, R. P. J., van Kempen, T., Vilaro, B. Vila, Watson, L. C., Wiklind, T., Gueth, F., Tatematsu, K., Wootten, A., Castro-Carrizo, A., Chapillon, E., Dumas, G., de Gregorio-Monsalvo, I., Francke, H., Gallardo, J., Garcia, J., Gonzalez, S., Hibbard, J. E., Hill, T., Kaminski, T., Karim, A., Krips, M., Kurono, Y., Lopez, C., Martin, S., Maud, L., Morales, F., Pietu, V., Plarre, K., Schieven, G., Testi, L., Videla, L., Villard, E., Whyborn, N., Zwaan, M. A., Alves, F., Andreani, P., Avison, A., Barta, M., Bedosti, F., Bendo, G. J., Bertoldi, F., Bethermin, M., Biggs, A., Boissier, J., Brand, J., Burkutean, S., Casasola, V., Conway, J., Cortese, L., Dabrowski, B., Davis, T. A., Trigo, M. Diaz, Fontani, F., Franco-Hernandez, R., Fuller, G., Madrid, R. Galvan, Giannetti, A., Ginsburg, A., Graves, S. F., Hatziminaoglou, E., Hogerheijde, M., Jachym, P., Serra, I. Jimenez, Karlicky, M., Klaasen, P., Kraus, M., Kunneriath, D., Lagos, C., Longmore, S., Leurini, S., Maercker, M., Magnelli, B., Vidal, I. Marti, Massardi, M., Maury, A., Muehle, S., Muller, S., Muxlow, T., O'Gorman, E., Paladino, R., Petry, D., Pineda, J., Randall, S., Richer, J. S., Rossetti, A., Rushton, A., Rygl, K., Monge, A. Sanchez, Schaaf, R., Schilke, P., Stanke, T., Schmalzl, M., Stoehr, F., Urban, S., van Kampen, E., Vlemmings, W., Wang, K., Wild, W., Yang, Y., Iguchi, S., Hasegawa, T., Saito, M., Inatani, J., Mizuno, N., Asayama, S., Kosugi, G., Morita, K. -I., Chiba, K., Kawashima, S., Okumura, S. K., Ohashi, N., Ogasawara, R., Sakamoto, S., Noguchi, T., Huang, Y. -D., Liu, S. -Y., Kemper, F., Koch, P. M., Chen, M. -T., Chikada, Y., Hiramatsu, M., Iono, D., Shimojo, M., Komugi, S., Kim, J., Lyo, A. -R., Muller, E., Herrera, C., Miura, R. E., Ueda, J., Chibueze, J., Su, Y. -N., Trejo-Cruz, A., Wang, K. -S., Kiuchi, H., Ukita, N., Sugimoto, M., Kawabe, R., Hayashi, M., Miyama, S., Ho, P. T. P., Kaifu, N., Ishiguro, M., Beasley, A. J., Bhatnagar, S., Braatz, J. A., Brisbin, D. G., Brunetti, N., Carilli, C., Crossley, J. H., D'Addario, L., Meyer, J. L. Donovan, Emerson, D. T., Evans, A. S., Fisher, P., Golap, K., Griffith, D. M., Hale, A. E., Halstead, D., Hardy, E. J., Hatz, M. C., Holdaway, M., Indebetouw, R., Jewell, P. R., Kepley, A. A., Kim, D. -C., Lacy, M. D., Leroy, A. K., Liszt, H. S., Lonsdale, C. J., Matthews, B., McKinnon, M., Mason, B. S., Moellenbrock, G., Moullet, A., Myers, S. T., Ott, J., Peck, A. B., Pisano, J., Radford, S. J. E., Randolph, W. T., Venkata, U. Rao, Rawlings, M. G., Rosen, R., Schnee, S. L., Scott, K. S., Sharp, N. K., Sheth, K., Simon, R. S., Tsutsumi, T., and Wood, S. J.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

A major goal of the Atacama Large Millimeter/submillimeter Array (ALMA) is to make accurate images with resolutions of tens of milliarcseconds, which at submillimeter (submm) wavelengths requires baselines up to ~15 km. To develop and test this capability, a Long Baseline Campaign (LBC) was carried out from September to late November 2014, culminating in end-to-end observations, calibrations, and imaging of selected Science Verification (SV) targets. This paper presents an overview of the campaign and its main results, including an investigation of the short-term coherence properties and systematic phase errors over the long baselines at the ALMA site, a summary of the SV targets and observations, and recommendations for science observing strategies at long baselines. Deep ALMA images of the quasar 3C138 at 97 and 241 GHz are also compared to VLA 43 GHz results, demonstrating an agreement at a level of a few percent. As a result of the extensive program of LBC testing, the highly successful SV imaging at long baselines achieved angular resolutions as fine as 19 mas at ~350 GHz. Observing with ALMA on baselines of up to 15 km is now possible, and opens up new parameter space for submm astronomy., 11 pages, 7 figures, 2 tables; accepted for publication in the Astrophysical Journal Letters; this version with small changes to affiliations

Published
2015

22. First Results from High Angular Resolution ALMA Observations Toward the HL Tau Region

Author

Partnership, ALMA, Brogan, C. L., Perez, L. M., Hunter, T. R., Dent, W. R. F., Hales, A. S., Hills, R., Corder, S., Fomalont, E. B., Vlahakis, C., Asaki, Y., Barkats, D., Hirota, A., Hodge, J. A., Impellizzeri, C. M. V., Kneissl, R., Liuzzo, E., Lucas, R., Marcelino, N., Matsushita, S., Nakanishi, K., Phillips, N., Richards, A. M. S., Toledo, I., Aladro, R., Broguiere, D., Cortes, J. R., Cortes, P. C., Espada, D., Galarza, F., Garcia-Appadoo, D., Guzman-Ramirez, L., Humphreys, E. M., Jung, T., Kameno, S., Laing, R. A., Leon, S., Marconi, G., Mignano, A., Nikolic, B., Nyman, L. -A., Radiszcz, M., Remijan, A., Rodon, J. A., Sawada, T., Takahashi, S., Tilanus, R. P. J., Vilaro, B. Vila, Watson, L. C., Wiklind, T., Akiyama, E., Chapillon, E., de Gregorio-Monsalvo, I., Di Francesco, J., Gueth, F., Kawamura, A., Lee, C. -F., Luong, Q. Nguyen, Mangum, J., Pietu, V., Sanhueza, P., Saigo, K., Takakuwa, S., Ubach, C., van Kempen, T., Wootten, A., Castro-Carrizo, A., Francke, H., Gallardo, J., Garcia, J., Gonzalez, S., Hill, T., Kaminski, T., Kurono, Y., Liu, H. -Y., Lopez, C., Morales, F., Plarre, K., Schieven, G., Testi, L., Videla, L., Villard, E., Andreani, P., Hibbard, J. E., and Tatematsu, K.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

We present Atacama Large Millimeter/submillimeter Array (ALMA) observations from the 2014 Long Baseline Campaign in dust continuum and spectral line emission from the HL Tau region. The continuum images at wavelengths of 2.9, 1.3, and 0.87 mm have unprecedented angular resolutions of 0.075 arcseconds (10 AU) to 0.025 arcseconds (3.5 AU), revealing an astonishing level of detail in the circumstellar disk surrounding the young solar analogue HL Tau, with a pattern of bright and dark rings observed at all wavelengths. By fitting ellipses to the most distinct rings, we measure precise values for the disk inclination (46.72pm0.05 degrees) and position angle (+138.02pm0.07 degrees). We obtain a high-fidelity image of the 1.0 mm spectral index ($\alpha$), which ranges from $\alpha\sim2.0$ in the optically-thick central peak and two brightest rings, increasing to 2.3-3.0 in the dark rings. The dark rings are not devoid of emission, we estimate a grain emissivity index of 0.8 for the innermost dark ring and lower for subsequent dark rings, consistent with some degree of grain growth and evolution. Additional clues that the rings arise from planet formation include an increase in their central offsets with radius and the presence of numerous orbital resonances. At a resolution of 35 AU, we resolve the molecular component of the disk in HCO+ (1-0) which exhibits a pattern over LSR velocities from 2-12 km/s consistent with Keplerian motion around a ~1.3 solar mass star, although complicated by absorption at low blue-shifted velocities. We also serendipitously detect and resolve the nearby protostars XZ Tau (A/B) and LkHa358 at 2.9 mm., Comment: 11 pages, 5 figures, 2 tables, accepted for publication in the Astrophysical Journal Letters

Published
2015

23. The EChO science case

Author

Tinetti, G., Drossart, P., Eccleston, P., Hartogh, P., Isaak, K., Linder, M., Lovis, C., Micela, G., Olliver, M., Puig, L., Ribas, I., De Sio, A., Frith, J., Justtanot, K., Showman, A., Alard, C., Yurchenko, S. N., Parviainen, H., Fouqué, P., Oliva, E., Bordé, P., Balado, A., Varley, R., Di Giorgio, A., Griffin, M., Maillard, J. P., Maggio, A., Lellouch, E., Strazzulla, G., Villaver, E., Griffith, C., Stamper, R., Amado, P. J., Rezac, L., Laken, B., Hargrave, P., Orton, G., Thompson, S., Morales, J. C., Wright, G., Massi, F., Lundgaard Rasmussen, I., Altieri, F., Covino, E., Coustenis, A., Moses, J., Lithgow Bertelloni, C., Demangeon, O., Fletcher, L., Morales Calderón, M., Lo Cicero, U., López Puertas, M., Capria, M. T., Danielski, C., Luntzer, A., Bulgarelli, A., González Hernández, J., Jacquemoud, S., MacTavish, C., Mall, U., Christian Jessen, N., Sanromá, E., Femenía Castella, B., Rocchetto, M., Miles Paez, P., Allard, F., Aylward, A., Leconte, J., Palla, F., White, G., Malaguti, G., Cavarroc, C., Lammer, H., Leto, G., Batista, V., Adybekian, V., Readorn, K., Polichtchouk, I., Petrov, R., García Piquer, A., Pancrazzi, M., Gómez Leal, I., Israelian, G., Rebolo López, R., Peralta, J., Giro, E., Tecsa, M., Haigh, J., Moro Martín, A., Pezzuto, S., Piskunov, N., Agnor, C., Hollis, M., Radioti, A., De Kok, R., Gear, W., Eymet, V., Achilleos, N., Koskinen, T., Maurin, A. S., Rank Lüftinger, T., Barlow, M., Figueira, P., Affer, L., Viti, S., Machado, P., Vakili, F., Burston, R., González Merino, B., Dominic, C., Dorfi, E., Smith, A., Sitek, P., Sánchez Lavega, A., Kerschbaum, F., Hoogeeven, R., Ballerini, P., Filacchione, G., Rodler, F., Stixrude, L., Parmentier, V., Del Val Borro, M., Vandenbussche, B., Tingley, B. W., Deeg, H. J., Tabernero, H. M., Shore, S., Fossey, S., Alonso Floriano, F. J., Santos, N., Tozzi, A., Kipping, D., Maruquette, J. B., Trifoglio, M., Scandaratio, G., Scuderi, S., Hébrard, E., Lodieu, N., Forget, F., Gustin, J., Poretti, E., Murgas Alcaino, F., Sicardy, B., Stiepen, A., Hubert, B., Grodent, D., Magnes, W., Tennyson, J., Temple, J., Galand, M., Barton, E. J., Winter, B., Valdivieso, M. L., Cordier, D., Heredero, R. L., Barrado, D., Mueller Wodarg, I., Giani, E., Correira, A., Widemann, T., Ward Thompson, D., Montañés Rodríguez, P., Moya Bedon, A., Venot, O., Prinja, R., Pinfield, D., Waldmann, I., Morello, G., Lim, T., Pallé, E., Waters, R., Wawer, P., Lognonné, P., Pietrzak, R., Fernández Hernández, Maite, Winek, W., Andersen, A., Monteiro, M., Liu, S. J., Rengel, M., Tanga, P., Yelle, R., Barstow, J. K., Maldonado, J., Irshad, R., Nelson, R., Colomé, J., De Witt, J., Lanza, N., Glasse, A., Coudé du Foresto, V., Branduardi Raymont, G., Beaulieu, J. P., Claudi, R., García López, Ramón, Eales, S., López Valverde, M. A., Turrini, D., Vinatier, S., Crook, J., Damasso, M., Ramos Zapata, G., Kovács, G., Banaszkiewicz, M., Focardi, M., Mauskopf, P., Guedel, M., Rebordao, J., Stolarski, M., Adriani, A., Norgaard Nielsen, H. U., Selig, A., Peña Ramírez, K. Y., Schmider, F. X., Baffa, C., Piccioni, G., Pantin, E., Bowles, N., Hornstrup, A., Pilat Lohinger, E., Buchhave, L. A., Soret, L., Börne, P., López Morales, M., Medvedev, A., Gesa, L., Jones, H., Pérez Hoyos, S., Gerard, J. C., Bellucci, G., Morais, H., Álvarez Iglesias, C. A., Abe, L., Pinsard, F., Tessenyi, M., Blecka, M., Wawrzaszk, A., Middleton, K., Martín Torres, J., Cho, J., Berry, D., Rataj, M., Schrader, J. R., Scholz, A., Watkins, C., Abreu, M., Testi, L., Decin, L., Sánz Forcada, J., Sozzetti, A., Lagage, P. O., Ade, P., Alcala, J., Sousa, S., Espinoza Contreras, M., Swinyard, B., Dobrijévic, M., Sánchez Béjar, V. J., Krupp, N., Bakos, G., Chamberlain, S., Chadney, J., Brown, L., Iro, N., Montalto, M., Sethenadh, J., Bouy, H., Ottensamer, R., Kehoe, T., Doel, P., Delgado Mena, E., Read, P., Coates, A., Cecchi Pestellini, C., Guillot, T., Budaj, J., Selsis, F., Jarchow, C., Del Vecchio, C., Cassan, A., Burleigh, M. R., Pagano, I., Ray, T., Gambicorti, L., Biondi, D., Cerulli, R., Ciaravella, A., Watson, D., Deroo, P., Collura, A., Graczyk, R., North, C., Ramos, A. A., Waltham, D., Montes, D., Gianotti, F., Thrastarson, H., Cockell, C., Pace, E., Bryson, I., Gómez, H., Esposito, M., Azzollini, R., Allende Prieto, C., Gillon, M., Fabrizio, N., Rickman, H., Rees, J. M., Pascale, E., Luzzi, D., Bonford, B., Cole, R., Gizon, L., Licandro Goldaracena, J., Agundez, M., Lahav, O., Zapatero Osorio, M. R., Gaulme, P., Encrenaz, T., Heyrovsky, D., Guàrdia, J., Prisinzano, L., Terenzi, L., Swain, M., Grassi, D., Eiroa, C., Maxted, P., Kerins, E., Yung, Y., Irwin, P., Herrero, E., Guio, P., Boisse, I., Claret, A., Kervella, P., Heiter, U., Bézard, B., Cabral, A., Michaut, C., Giuranna, M., Hersant, F., Hueso, R., Savini, G., Snellen, I. A., Charnoz, S., Jones, G., Belmonte Avilés, J. A., Barber, R. J., Wisniowski, T., Morgante, G., University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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 Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Laboratoire des technologies de la microélectronique (LTM), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Leicester], University of Leicester, U.S. Army Research Laboratory [Adelphi, MD] (ARL), United States Army (U.S. Army), Royal Observatory Edinburgh (ROE), University of Edinburgh, Departamento de Fisica [Aveiro], Universidade de Aveiro, SRON Netherlands Institute for Space Research (SRON), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Planetary Sciences [Tucson], University of Arizona, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 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CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [UCL London], Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), University of Stuttgart, Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, Mullard Space Science Laboratory (MSSL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Curie [Paris], Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Centre for Behaviour and Evolution, Institute of Neuroscience, Newcastle University [Newcastle], foreign laboratories (FL), CERN [Genève], STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Estrutura de Missão para a Extensão da Plataforma Continental, Estrutura de Missão para a Extensão para a Extensão da Plataforma Continental, Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Queen Mary University of London (QMUL), 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), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, Department of Geoscience, Nelson Mandela University [Port Elizabeth], African Earth Observatory Network - Earth Stewardship Science Research Institute (AEON-ESSRI), Animal Genetics, Teagasc - The Agriculture and Food Development Authority (Teagasc), 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Instituto Nacional de Engenharia, Tecnologia e Inovacao (INETI), Université Pierre et Marie Curie - Paris 6 (UPMC), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Università di Salerno - Dipartimento di Matematica, Università degli Studi di Salerno = University of Salerno (UNISA), Department of Genetics, University of North Carolina [Chapel Hill] (UNC), University of North Carolina System (UNC)-University of North Carolina System (UNC)-Carolina Center for the Genome Sciences, Institut de Recerca i Tecnologia Agroalimentàries = Institute of Agrifood Research and Technology (IRTA), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - 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Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-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), Institute for Astronomy [Vienna], University of Vienna [Vienna], Institut de génétique et microbiologie [Orsay] (IGM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH = German Research Center for Artificial Intelligence (DFKI), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Dipartimento di Matematica 'Ulisse Dini', Università degli Studi di Firenze = University of Florence (UniFI), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Université de Rennes (UR), Imperial College London, Laboratoire Hippolyte Fizeau (FIZEAU), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'Astrophysique et de Géophysique [Liège], Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Bradford, Instituto Universitario de Electroquimica, Universidad de Alicante, Centre de recherche en éducation de Nantes (CREN), Le Mans Université (UM)-Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN), Departamento de Fisica Aplicada [Bilbao], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), NASA Goddard Space Flight Center (GSFC), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Los Alamos National Laboratory (LANL), Osserv Astrofis Catania, Ist Nazl Astrofis, Centre d'Etude de l'Energie Nucléaire (SCK-CEN), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Super Invest Cient, Inst Astrofis Andalucia, ES-18080 Granada, Spain, Department of Rheumatology (LEIDEN - 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CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Instituto Nacional de Engenharia, Tecnologia e Inovacco (INETI), Physiologie de la reproduction et des comportements [Nouzilly] (PRC), Centre National de la Recherche Scientifique (CNRS)-Université de Tours-Institut Français du Cheval et de l'Equitation [Saumur]-Institut National de la Recherche Agronomique (INRA), Université Francois Rabelais [Tours], Institut Français du Cheval et de l'Equitation, Università degli Studi di Salerno (UNISA), IRTA, Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH (DFKI), Universidade do Porto [Porto], Università degli Studi di Firenze [Firenze], Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Department of Earth Sciences, University College London, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre interdisciplinaire de recherche, culture, éducation, formation, travail (CIRCEFT), Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Station biologique, Centre National de la Recherche Scientifique (CNRS), Dipartimento di Informatica [Verona], Università degli Studi di Verona, Departamento de Física e Astronomia [Porto], UMR5116, Centre Émile Durkheim (CED), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Clinica Neurologica, Università degli Studi di Perugia (UNIPG), Rebordao, J. [0000-0002-7418-0345], Kerschbaum, F. [0000-0001-6320-0980], Abreu, M. [0000-0002-0716-9568], Tabernero, H. [0000-0002-8087-4298], López Puertas, M. [0000-0003-2941-7734], Jacquemoud, S. [0000-0002-1500-5256], Tennyson, J. [0000-0002-4994-5238], Focardi, M. [0000-0002-3806-4283], Leto, G. [0000-0002-0040-5011], Lodieu, N. [0000-0002-3612-8968], Tinetti, G. [0000-0001-6058-6654], Sanroma, E. [0000-0001-8859-7937], Poretti, E. [0000-0003-1200-0473], Deeg, H. [0000-0003-0047-4241], Grassi, D. [0000-0003-1653-3066], Piccioni, G. [0000-0002-7893-6808], Ribas, I. [0000-0002-6689-0312], Coates, A. [0000-0002-6185-3125], García Ramón, J. [0000-0002-8204-6832], Bouy, H. [0000-0002-7084-487X[, Lognonne, P. [0000-0002-1014-920X], Demangeon, O. [0000-0001-7918-0355], Morales, J. C. [0000-0003-0061-518X], Ray, T. [0000-0002-2110-1068], Guio, P. [0000-0002-1607-5862], Tanga, P. [0000-0002-2718-997X], Prisinzano, L. [0000-0002-8893-2210], Barstow, J. [0000-0003-3726-5419], Balado, A. [0000-0003-4268-2516], Lithgow Bertelloni, C. [0000-0003-0924-6587], Barton, E. [0000-0001-5945-9244], Delgado, M. E. [0000-0003-4434-2195], Affer, L. [0000-0001-5600-3778], Ciaravella, A. [0000-0002-3127-8078], Barrado Navascues, D. [0000-0002-5971-9242], Figueira, P. [0000-0001-8504-283X], Covino, E. [0000-0002-6187-6685], Venot, O. [0000-0003-2854-765X], Cabral, A. [0000-0002-9433-871X], Watson, D. [0000-0002-4465-8264], Morales Calderon, M. [0000-0001-9526-9499], Ward Thompson, D. [0000-0003-1140-2761], Rebolo, R. [0000-0003-3767-7085], López Valverde, M. A. [0000-0002-7989-4267], Gillon, M. [0000-0003-1462-7739], Morgante, G. [0000-0001-9234-7412], Zapatero Osorio, M. R. [0000-0001-5664-2852], Bulgarelli, A. [0000-0001-6347-0649], Pena Ramírez, K. [0000-0002-5855-401X], Galand, M. [0000-0001-5797-914X], Pancrazzi, M. [0000-0002-3789-2482], Malaguti, G. [0000-0001-9872-3378], Sánchez Lavega, A. [0000-0001-7234-7634], Waldmann, I. [0000-0002-4205-5267], Kovacs, G. [0000-0002-2365-2330], Guillot, T. [0000-0002-7188-8428], Turrini, D. [0000-0002-1923-7740], Altieri, F. [0000-0002-6338-8300], Bellucci, G. [0000-0003-0867-8679], Baffa, C. [0000-0002-4935-100X], Olivia, E. [0000-0002-9123-0412], Selsis, F. [0000-0001-9619-5356], Scuderi, Salvatore [0000-0002-8637-2109], Hersant, F. [0000-0002-2687-7500], Gear, W. [0000-0001-6789-6196], Damasso, M. [0000-0001-9984-4278], Tizzi, A. [0000-0002-6725-3825], Pinfield, D. [0000-0002-7804-4260], Kipping, D. [0000-0002-4365-7366], Maldonado, J. [0000-0002-4282-1072], Pace, E. [0000-0001-5870-1772], Burleigh, M. [0000-0003-0684-7803], Monteiro, M. [0000-0001-5644-0898], Pilat Lohinger, E. [0000-0002-5292-1923], Chadney, J. [0000-0002-5174-2114], Moro Martín, A. [0000-0001-9504-8426], Claret, A. [0000-0002-4045-8134], Gómez, H. [0000-0003-3398-0052], Maldonado, J. [0000-0002-2218-5689], Michaut, C. [0000-0002-2578-0117], Hornstrup, A. [0000-0002-3363-0936], Scholz, A. [0000-0001-8993-5053], Irwin, P. [0000-0002-6772-384X], Bezard, B. [0000-0002-5433-5661], López Heredero, R. [0000-0002-2197-8388], Sanz Forcada, J. [0000-0002-1600-7835], Danielski, C. [0000-0002-3729-2663], Sousa, S. [0000-0001-9047-2965], Medved, A. [0000-0003-2713-8977], Bakos, G. [0000-0001-7204-6727], Ade, P. [0000-0002-5127-0401], Vandenbussche, B. [0000-0002-1368-3109], Martín Torres, J. [0000-0001-6479-2236], Correira, A. [0000-0002-8946-8579], Haigh, J. [0000-0001-5504-4754], Scandariato, G. [0000-0003-2029-0626], Guedel, M. [0000-0001-9818-0588], Sánchez Bejar, V. [0000-0002-5086-4232], Rodríguez, P. [0000-0002-6855-9682], Piskunov, N. [0000-0001-5742-7767], Adibekyan, V. [0000-0002-0601-6199], Pérez Hoyos, S. [0000-0001-9797-4917], Kervella, P. [0000-0003-0626-1749], Pascale, E. [0000-0002-3242-8154], Claudi, R. [0000-0001-7707-5105], Filacchione, G. [0000-0001-9567-0055], Rickman, H. [0000-0002-9603-6619], Amado, P. J. [0000-0002-8388-6040], Maggio, A. [0000-0001-5154-6108], Agundez, M. [0000-0003-3248-3564], Montes, D. [0000-0002-7779-238X], Fletcher, L. [0000-0001-5834-9588], Stixrude, L. [0000-0003-3778-2432], Morais, M. H. [0000-0001-5333-2736], Hueso, R. [0000-0003-0169-123X], Yurchenko, S. [0000-0001-9286-9501], Rataj, M. [0000-0002-2978-9629], Pérez Hoyos, S. [0000-0002-2587-4682], Santos, N. [0000-0003-4422-2919], Peralta, J. [0000-0002-6823-1695], Budaj, J. [0000-0002-9125-7340], Barlow, M. [0000-0002-3875-1171], Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - 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Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH ( DFKI ), Consejo Nacional de Investigaciones Científicas y Técnicas ( CONICET ), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut Universitaire de France ( IUF ), Ministère de l'Éducation nationale, de l’Enseignement supérieur et de la Recherche ( M.E.N.E.S.R. ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ), Laboratoire Hippolyte Fizeau ( FIZEAU ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Istituto di Fisica dello Spazio Interplanetario CNR (IFSI), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de recherche en éducation de Nantes ( CREN ), Université de Nantes ( UN ), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea ( UPV/EHU ), NASA Goddard Space Flight Center ( GSFC ), Onsala Space Observatory ( OSO ), Los Alamos National Laboratory ( LANL ), Centre d'Etude de l'Energie Nucléaire ( SCK-CEN ), Institut de Physique du Globe de Paris ( IPGP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Department of Rheumatology ( LEIDEN - Rhumato ), Department of Rheumatology ( COIMBRA - Rhumato ), Centre Scientifique et Technique du Bâtiment ( CSTB ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Centre interdisciplinaire de recherche, culture, éducation, formation, travail ( CIRCEFT ), Université Paris 8 Vincennes-Saint-Denis ( UP8 ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique des gaz et des plasmas ( LPGP ), Pontificia Universidad Católica de Chile, Thüringer Landessternwarte Tautenburg ( TLS ), BIBA Bremer Institut für Produktion und Logistik GmbH, Centre Émile Durkheim ( CED ), Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Catania ( OACT ), Institut de Ciencies Fotoniques [Castelldefels] ( ICFO ), Università di Perugia, Royal Holloway [University of London] ( RHUL ), and Low Energy Astrophysics (API, FNWI)

Subjects
Astrofísica, Solar System, Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], HOT-JUPITER ATMOSPHERES, 7. Clean energy, Space missions, law.invention, Astronomi, astrofysik och kosmologi, Planet, law, Observatory, Astronomy, Astrophysics and Cosmology, Transit (astronomy), Atmospheric science, Exoplanets, IR astronomy, Spectroscopy, Astronomy and Astrophysics, Space and Planetary Science, QC, QB, Eclipse, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanet, GIANT PLANETS, Physical Sciences, ENERGY-BALANCE, Astrophysics::Earth and Planetary Astrophysics, Population, MU-M, FOS: Physical sciences, F500, Astronomy & Astrophysics, Telescope, INFRARED-EMISSION-SPECTRUM, education, [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], EXTRASOLAR PLANET ATMOSPHERE, Science & Technology, Astronomy, EXOPLANET HD 189733B, HUBBLE-SPACE-TELESCOPE, Astronomía, TRANSMISSION SPECTROSCOPY, 0201 Astronomical And Space Sciences, 13. Climate action, WATER-VAPOR, astro-ph.EP, Astrophysics - Earth and Planetary Astrophysics
Abstract

The discovery of almost 2000 exoplanets has revealed an unexpectedly diverse planet population. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? What causes the exceptional diversity observed as compared to the Solar System? EChO (Exoplanet Characterisation Observatory) has been designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large and diverse planet sample within its four-year mission lifetime. EChO can target the atmospheres of super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300K-3000K) of F to M-type host stars. Over the next ten years, several new ground- and space-based transit surveys will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets. Placing the satellite at L2 provides a cold and stable thermal environment, as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. A 1m class telescope is sufficiently large to achieve the necessary spectro-photometric precision. The spectral coverage (0.5-11 micron, goal 16 micron) and SNR to be achieved by EChO, thanks to its high stability and dedicated design, would enable a very accurate measurement of the atmospheric composition and structure of hundreds of exoplanets., Comment: 50 pages, 30 figures. Experimental Astronomy

Published
2015
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24. The first Galaxy scale hunt for the youngest high-mass protostars

Author

Simon, R., Csengeri, T., Bontemps, S., Wyrowski, F., Menten, K.M., Leurini, S., Urquhart, J.S., Motte, F., Schuller, F., Testi, L., Bronfman, L., Beuther, H., Longmore, S., Commerçon, B., Henning, Th., Palau, A., Tan, J.C., Fuller, G., Peretto, N., Duarte-Cabral, A., Traficante, A., Schaaf, R., Stutzki, J., 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), Max-Planck-Institut für Radioastronomie (MPIFR), Mars Desert Research Station (MDRS), Procédés, Matériaux et Energie Solaire (PROMES), Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Departamento de Astronomia (DAS), Swinburne University of Technology (Hawthorn campus), Observatoire de Paris, Université Paris sciences et lettres (PSL), Centro de Radioastronomia y Astrofisica (CRyA), Universidad Nacional Autónoma de México (UNAM), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], 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, 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), Universidad de Santiago de Chile [Santiago] (USACH), School of Physics, PSL Research University (PSL), Centro de Radioastronomia y Astrofisica, Jodrell Bank Centre for Astrophysics, Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)

Subjects
Physics, General Engineering, FOS: Physical sciences, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), High mass, Protostar, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Solar and Stellar Astrophysics (astro-ph.SR), O-type star, QB
Abstract

The origin of massive stars is a fundamental open issue in modern astrophysics. Pre-ALMA interferometric studies reveal precursors to early B to late O type stars with collapsing envelopes of 15-20 M$_\odot$ on 1000-3000 AU size-scales. To search for more massive envelopes we selected the most massive nearby young clumps from the ATLASGAL survey to study their protostellar content with ALMA. Our first results using the intermediate scales revealed by the ALMA ACA array providing 3-5" angular resolution, corresponding to $\sim$0.05-0.1 pc size-scales, reveals a sample of compact objects. These massive dense cores are on average two-times more massive than previous studies of similar types of objects. We expect that once the full survey is completed, it will provide a comprehensive view on the origin of the most massive stars., Comment: 4 pages, 1 figure, to appear in proceedings of The 6th Zermatt ISM Symposium: Conditions and Impact of Star Formation From Lab to Space, eds. R. Simon, M. Rollig

Published
2015
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25. X-Shooter study of accretion in $��$-Ophiucus: very low-mass stars and brown dwarfs

Author

Manara, C. F., Testi, L., Natta, A., and Alcal��, J. M.

Subjects
Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present new VLT/X-Shooter optical and NIR spectra of a sample of 17 candidate young low-mass stars and BDs in the rho-Ophiucus cluster. We derived SpT and Av for all the targets, and then we determined their physical parameters. All the objects but one have M*, accepted for publication in Astronomy & Astrophysics. Abstract shortened to fit arXiv constraints

Published
2015
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26. ALMA and CARMA observations of Brown Dwarfs disks: testing the models of dust evolution

Author

Ricci, L., Testi, L., Natta, A., Aleks Scholz, Gregorio-Monsalvo, I., Isella, A., and Carpenter, J. M.

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

The first steps toward planet formation involve the coagulation of small microscopic grains into larger and larger pebbles and rocks in gas-rich disks around young stars and brown dwarfs. Observations in the sub-millimeter can trace mm/cm-sized pebbles in the outer disks, and investigate the mechanisms of coagulation/fragmentation and radial migration of these solids. These represent key, yet not fully understood ingredients for our understanding of the formation of planetesimals, the building blocks of planets. Here we present the first results from an observational program using the ALMA and CARMA sub-mm/mm interferometers aimed at characterizing the dust properties and disk structure of young disks around brown dwarfs and very low mass stars. Given the physical conditions expected for these disks, they represent critical test beds for the models of the early stages of planet formation in proto-planetary disks., Comment: 5 pages, 3 figures, proceedings for the conference 'Brown dwarfs come of age', May 20-24 2013, to be published in Memorie della Societa Astronomica Italiana

Published
2013
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27. Silicon isotopic abundance toward evolved stars and its application for presolar grains

Author

De Breuck, C., Gray, M., Nyman, L., Vlemmings, W., De Gregorio-Monsalvo, I., Wittkowski, M., Rawlings, M., Peng, T., Baudry, Alain, Testi, L., Humphreys, E., Peng, T.-C., Baudry, A., European Southern Observatory (ESO), FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-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), ESO, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Stellar mass, Metallicity, FOS: Physical sciences, Natural abundance, Astrophysics, 01 natural sciences, 0103 physical sciences, Red supergiant, Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Presolar grains, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Carbon star, Interstellar medium, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy Astrophysics
Abstract

Galactic chemical evolution (GCE) is important for understanding the composition of the present-day interstellar medium (ISM) and of our solar system. In this paper, we aim to track the GCE by using the 29Si/30Si ratios in evolved stars and tentatively relate this to presolar grain composition. We used the APEX telescope to detect thermal SiO isotopologue emission toward four oxygen-rich M-type stars. Together with the data retrieved from the Herschel science archive and from the literature, we were able to obtain the 29Si/30Si ratios for a total of 15 evolved stars inferred from their optically thin 29SiO and 30SiO emission. These stars cover a range of masses and ages, and because they do not significantly alter 29Si/30Si during their lifetimes, they provide excellent probes of the ISM metallicity (or 29Si/30Si ratio) as a function of time. The 29Si/30Si ratios inferred from the thermal SiO emission tend to be lower toward low-mass oxygen-rich stars (e.g., down to about unity for W Hya), and close to an interstellar or solar value of 1.5 for the higher-mass carbon star IRC+10216 and two red supergiants. There is a tentative correlation between the 29Si/30Si ratios and the mass-loss rates of evolved stars, where we take the mass-loss rate as a proxy for the initial stellar mass or current stellar age. This is consistent with the different abundance ratios found in presolar grains. We found that older objects (up to possibly 10 Gyr old) in our sample trace a previous, lower 29Si/30Si value of about 1. Material with this isotopic ratio is present in two subclasses of presolar grains, providing independent evidence of the lower ratio. Therefore, the 29Si/30Si ratio derived from the SiO emission of evolved stars is a useful diagnostic tool for the study of the GCE and presolar grains., Comment: 7 pages, 4 figures

Published
2013
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28. On the shape of the mass-function of dense clumps in the Hi-GAL fields. I. SED determination and global properties of the mass-functions

Author

Olmi, L., Angles-Alcazar, D., Elia, D., Molinari, S., Montier, L., Pestalozzi, M., Pezzuto, S., Polychroni, D., Ristorcelli, I., Rodon, J., Schisano, E., Smith, M. D., Testi, L., and Thompson, M.

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

Stars form in dense, dusty clumps of molecular clouds, but little is known about their origin and evolution. In particular, the relationship between the mass distribution of these clumps (also known as the "clump mass function", or CMF) and the stellar initial mass function (IMF), is still poorly understood. In order to discern the "true" shape of the CMF and to better understand how the CMF may evolve toward the IMF, large samples of bona-fide pre- and proto-stellar clumps are required. The sensitive observations of the Herschel Space Observatory (HSO) are now allowing us to look at large clump populations in various clouds with different physical conditions. We analyse two fields in the Galactic plane mapped by HSO during its science demonstration phase, as part of the more complete and unbiased Herschel infrared GALactic Plane Survey (Hi-GAL). These fields undergo a source-extraction and flux-estimation pipeline, which allows us to obtain a sample with thousands of clumps. Starless and proto-stellar clumps are separated using both color and positional criteria to find those coincident with MIPS 24 micron sources. We describe the probability density functions of the power-law and lognormal models that are used to fit the CMFs, and we then find their best-fit parameters. For the lognormal model we apply several statistical techniques to the data and compare their results. The CMFs of the two SDP fields show very similar shapes, but very different mass scales. This similarity is confirmed by the values of the best-fit parameters of either the power-law or lognormal model. The power-law model leads to almost identical CMF slopes, whereas the lognormal model shows that the CMFs have similar widths. The similar CMF shape but different mass scale represents an evidence that the overall process of star formation in the two regions is very different., Comment: This article is composed of 14 pages, 5 figures and is based on Hi-GAL data. Submitted for publication to Astronomy & Astrophysics on 19 sept. 2012

Published
2012
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29. U-band study of the accretion properties in the sigma Ori star-forming region

Author

Rigliaco, E., Natta, A., Randich, S., Testi, L., and Biazzo, K.

Subjects
Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

This paper presents the results of an U band survey with FORS1/VLT of a large area in the sigma Orionis star-forming region. We combine the U-band photometry with literature data to compute accretion luminosity and mass accretion rates from the U-band excess emission for all objects (187) detected by Spitzer in the FORS1 field and classified by Hernandez et al. (2007) as likely members of the cluster. The sample stars range in mass from ~0.06 to ~1.2 Msun; 72 of them show evidence of disks and we measure mass accretion rates Macc between, 19 pages, 17 figures, accepted by A&A

Published
2010

30. Resolved images of self-gravitating circumstellar discs with ALMA

Author

Cossins, P., Lodato, G., and Testi, L.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

In this paper we present simulated observations of massive self-gravitating circumstellar discs using the Atacama Large Millimetre/sub-millimetre Array (ALMA). Using a smoothed particle hydrodynamics model of a $0.2M_{\odot}$ disc orbiting a $1M_{\odot}$ protostar, with a cooling model appropriate for discs at temperatures below $\sim 160$K and representative dust opacities, we have constructed maps of the expected emission at sub-mm wavelengths. We have then used the CASA ALMA simulator to generate simulated images and visibilities with various array configurations and observation frequencies, taking into account the expected thermal noise and atmospheric opacities. We find that at 345 GHz (870 $\mu$m) spiral structures at a resolution of a few AU should be readily detectable in approximately face-on discs out to distances of the Taurus-Auriga star-forming complex., Comment: 8 pages, 6 figures, accepted to MNRAS. Figure quality degraded. Full paper with higher quality figures available at http://www2.fisica.unimi.it/lodato/CossinsLodatoTesti1.pdf

Published
2010

31. ATLASGAL - The APEX Telescope Large Area Survey of the Galaxy at 870 microns

Author

Schuller, F., Menten, K. M., Contreras, Y., Wyrowski, F., Schilke, P., Bronfman, L., Henning, T., Walmsley, C. M., Beuther, H., Bontemps, Sylvain, Cesaroni, R., Deharveng, L., Garay, G., Herpin, Fabrice, Lefloch, B., Linz, H., Mardones, D., Minier, V., Molinari, S., Motte, F., Nyman, L. -A., Reveret, V., Risacher, C., Russeil, D., Schneider, N., Testi, L., Troost, T., Vasyunina, T., Wienen, M., Zavagno, Annie, Kovacs, A., Kreysa, E., Siringo, G., Weiss, A., Max-Planck-Institut für Radioastronomie (MPIFR), Departamento de Astronomia (DAS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), 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), Laboratoire d'Astrophysique de Marseille (LAM), 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), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Istituto Fisica Spazio Interplanetario, ESO, European Southern Observatory (ESO), 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), 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), and Universidad de Santiago de Chile [Santiago] (USACH)

Subjects
[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, 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, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Galaxy Astrophysics
Abstract

(Abridged) Studying continuum emission from interstellar dust is essential to locating and characterizing the highest density regions in the interstellar medium. In particular, the early stages of massive star formation remain poorly understood. Our goal is to produce a large-scale, systematic database of massive pre- and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. A well characterized sample of star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submm wavelengths also represents a preparatory work for Herschel and ALMA. The APEX telescope is ideally located to observe the inner Milky Way. The Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer array observing at 870 microns, with a beam size of 19". Taking advantage of its large field of view (11.4') and excellent sensitivity, we started an unbiased survey of the Galactic Plane, with a noise level of 50-70 mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). As a first step, we covered 95 sq. deg. These data reveal 6000 compact sources brighter than 0.25 Jy, as well as extended structures, many of them filamentary. About two thirds of the compact sources have no bright infrared counterpart, and some of them are likely to correspond to the precursors of (high-mass) proto-stars or proto-clusters. Other compact sources harbor hot cores, compact HII regions or young embedded clusters. Assuming a typical distance of 5 kpc, most sources are clumps smaller than 1 pc with masses from a few 10 to a few 100 M_sun. In this introductory paper, we show preliminary results from these ongoing observations, and discuss the perspectives of the survey., Accepted for publication in A&A, 13 pages, 14 figures. Final version after language editing

Published
2009
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32. Accretion properties of T Tauri stars in sigma Ori

Author

Gatti, T., Natta, A., Randich, S., Testi, L., and Sacco, G.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Accretion disks around young stars evolve in time with time scales of few million years. We present here a study of the accretion properties of a sample of 35 stars in the ~3 million year old star-forming region sigma Ori. Of these, 31 are objects with evidence of disks, based on their IR excess emission. We use near-IR hydrogen recombination lines (Pa_gamma) to measure their mass accretion rate. We find that the accretion rates are significantly lower in sigma Ori than in younger regions, such as rho-Oph, consistently with viscous disk evolution. The He I 1.083 micron line is detected (either in absorption or in emission) in 72% of the stars with disks, providing evidence of accretion-powered activity also in very low accretors, where other accretion indicators dissapear., Astronomy and Astrophysics, accepted

Published
2008

33. Spitzer IRAC and MIPS Imaging of Clusters and Outflows in 9 High-mass Star Forming Regions

Author

Qiu, Keping, Zhang, Qizhou, Megeath, S. Thomas, Gutermuth, Robert A., Beuther, Henrik, Shepherd, Debra S., Sridharan, T. K., Testi, L., and De Pree, C. G.

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

We present Spitzer Space Telescope IRAC and MIPS observations toward a sample of nine high-mass star forming regions at a distance of around 2 kpc. Based on IRAC and MIPS 24 $\mu$m photometric results and 2MASS JHKs data, we carry out a census of young stellar objects (YSOs) in a 5' by 5' field toward each region. Toward seven out of the nine regions, we detect parsec sized clusters with around 20 YSOs surrounded by a more extended and sparse distribution of young stars and protostars. For the other two regions, IRAS 20126+4104 and IRAS 22172+5549, the former has the lowest number of YSOs in the sample and shows no obvious cluster, and the latter appears to be part of a larger, potentially more evolved cluster. The deep IRAC imaging reveals at least twelve outflows in eight out of the nine regions, with nine outflows prominent in the 4.5 $\mu$m band most probably attributed to shocked H$_2$ emission, two outflows dominated by scattered light in the 3.6 and 4.5 $\mu$m bands, and one outflow standing out from its hydrocarbon emission in the 8.0 $\mu$m band. In comparison with previous ground-based observations, our IRAC observations reveal new outflow structures in five regions. The dramatically different morphologies of detected outflows can be tentatively interpreted in terms of possible evolution of massive outflows. The driving sources of these outflows are deeply embedded in dense dusty cores revealed by previous millimeter interferometric observations. We detect infrared counterparts of these dusty cores in the IRAC or MIPS 24 $\mu$m bands. Reflection nebulae dominated by the emission from UV heated hydrocarbons in the 8 $\mu$m band can be found in most regions and they may imply the presence of young B stars., Comment: 76 pages, 25 figures and 5 tables, ApJ in press, a full resolution version available at http://www.cfa.harvard.edu/~kqiu/spitzer.pdf

Published
2008
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34. The dusty disk around VV Ser

Author

Alonso-Albi, T., Fuente, A., Bachiller, R., Neri, R., Planesas, P., and Testi, L.

Subjects
Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We have carried out observations at millimeter and centimeter wavelengths towards VV Ser using the Plateau de Bure Interferometer and the Very Large Array. This allows us to compute the SED from near infrared to centimeter wavelengths. The modeling of the full SED has provided insight into the dust properties and a more accurate value of the disk mass. The mass of dust in the disk around VV Ser is found to be about 4 10^(-5) Msun, i.e. 400 times larger than previous estimates. Moreoever, the SED can only be accounted for assuming dust stratification in the vertical direction across the disk. The existence of small grains (0.25--1 micron) in the disk surface is required to explain the emission at near- and mid-infrared wavelengths. The fluxes measured at millimeter wavelengths imply that the dust grains in the midplane have grown up to very large sizes, at least to some centimeters., Comment: To appear in ApJ

Published
2008
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35. Discovery of a Bipolar Outflow from 2MASSW J1207334-393254, A 24 Jupiter Mass Brown Dwarf

Author

Whelan, E. T., Ray, T. P., Randich, S., Baciotti, F., Jayawardhana, R., Testi, L., Natta, A., and Mohanty, S.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The 24 M Jupiter mass brown dwarf 2MASS1207-3932 has for some time been known to show clear signs of classical T Tauri-like accretion. Through analysis of its oxygen forbidden emission we have discovered that it is driving a bipolar outflow. Blue and red-shifted components to the [OI] 6300 forbidden emission line are seen at velocities of - 8 km/s and +4 km/s. Spectro-astrometry recovers the position of both components relative to the BD, at ~ 0.08 arcseconds(in opposing directions). A position velocity diagram of the line region supports the spectro-astrometric results. The H-alpha and HeI 6678 lines were also analysed. These line regions are not offset with respect to the continuum ruling out the presence of spectro-astrometric artifacts and underlining the validity of the [OI] 6300 results. The low radial velocity of the outflow, and relatively large offsets, are consistent with 2MASS1207-3932 having a near edge-on disk, as proposed by Scholz et al. 2MASS1207-3932 is now the smallest mass galactic object known to drive an outflow. The age of the TW Hydrae Association (~ 8 Myr) also makes this one of the oldest objects with a resolved jet. This discovery not only highlights the robustness of the outflow mechanism over an enormous range of masses but also suggests that it may even be feasible for young giant planets with accretion disks to drive outflows., 12 pages, 2 figures

Published
2007

36. New 13CO observations towards the Keplerian gaseous disk around R Mon

Author

Alonso-Albi, T., Fuente, A., Bachiller, R., Natta, A., Testi, L., Neri, R., and Planesas, P.

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

We present new high angular resolution observations of the 13CO 1-0 rotational line towards the HBe star R Mon, obtained with the IRAM Bure Interferometer, along with the previous results in the observed transitions 12CO 1-0 and 2-1. We have used a flat disk model to fit the 12CO 1-0 and 2-1, and 13CO 1-0 emission, in a strip perpendicular to the outflow axis. The model assumes standard abundances (X(12CO) = 8x10^-5, X(13CO) = 9x10^7), radial potential temperature and density laws (T (K) = T0 r^-q, rho (cm^-3) = rho0 r^-p), and Local Thermodynamic Equilibrium. The 13CO and 12CO emission is consistent with a flat disk at an inclination angle of 20 degrees in Keplerian rotation around the star. The gaseous disk is fitted with a mass of 0.014 Msun, an outer radius of 1500 AU, a temperature of 4500 K at the inner radius (1 AU), and values of q=0.62 and p=1.3 for the indexes of the temperature and density laws. This new 13CO observations allow us to conclude that the disk around R Mon is flat. Our result confirms previous works suggesting a predominant flat geometry in disks around early Be stars., 4 pages, 5 figure. Proceedings of the conference "Science with ALMA: a new era for Astrophysics" hold in Madrid in November, 13-17, 2006

Published
2007

37. An asymmetry detected in the disk of Kappa CMa with the AMBER/VLTI

Author

Meilland, Anthony, Millour, Florentin, Stee, Philippe, Domiciano De Souza, Armando, Petrov, Romain, Mourard, Denis, Jankov, Slobodan, Robbe-Dubois, Sylvie, Spang, Alain, Arisitidi, Eric, Antonelli, P., Beckmann, U., Bresson, Y., Chelli, A., Dugué, M., Duvert, G., Glück, L., Kern, P., Lagarde, S., Le Coarer, E., Lisi, F., Malbet, F., Perraut, K., Puget, P., Robbe-Dubois, S., Weigelt, G., Zins, G., Accardo, M., Acke, B., Agabi, K., Arezki, B., Altariba, E., Baffa, C., Behrend, J., Blöcker, T., Bonhomme, S., Busoni, S., Cassaing, F., Clausse, J.-M., Connot, C., Delboulbé, A., Domicinano De Souza, A., Driebe, T., Feautrier, P., Ferruzzi, D., Forveille, T., Fossat, E., Foy, R., Fraix-Burnet, D., Gallardo, A., Gennari, S., Glentzlin, A., Giani, E., Gilinst, C., Heiden, M., Heininger, M., Hernandez, O., Hofmann, K.-H., Kamm, D., Kraus, S., Le Contel, D., Le Contel, J.-M., Lopez, B., Magnard, Y., Marconi, A., Mars, G., Martinot-Lagarde, G., Mathias, P., Millour, F., Monin, J.-L., Mouillet, D., Mourard, D., Mège, P., Nussbaum, E., Ohnaka, K., Pacini, F., Perrier, C., Rabbia, Y., Rebattu, S., Reynaud, F., Richichi, A., Roussel, A., Sacchettini, M., Salinari, P., Schertl, D., Solscheid, W., Stee, P., Stefanini, P., Tallon, M., Tallon-Bosc, I., Tasso, D., Tatulli, E., Testi, L., Valtier, J.-C., Vannier, M., Ventura, N., Kiekebusch, M., Schöller, M., Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars: emission-line, Astrophysics (astro-ph), Stars: individual (kappa CMa), FOS: Physical sciences, Be, Astrophysics, Techniques: high angular resolution, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars: Keplerian rotation, Techniques: interferometric, Stars: circumstellar matter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; Aims. We study the geometry and kinematics of the circumstellar environment of the Be star Kappa CMa in the Br gamma emission line and its nearby continuum. Methods. We use the VLTI/AMBER instrument operating in the K band which provides a spatial resolution of about 6 mas with a spectral resolution of 1500 to study the kinematics within the disk and to infer its rotation law. In order to obtain more kinematical constraints we also use an high spectral resolution Pa beta line profile obtain in December 2005 at the Observatorio do Pico do Dios, Brazil and we compile V/R line profile variations and spectral energy distribution data points from the literature. Results. Using differential visibilities and differential phases across the Br gamma line we detect an asymmetry in the disk. Moreover, we found that kappa CMa seems difficult to fit within the classical scenario for Be stars, illustrated recently by alpha Arae observations, i.e. a fast rotating B star close to its breakup velocity surrounded by a Keplerian circumstellar disk with an enhanced polar wind. Finally we discuss the possibility for kappa CMa to be a critical rotator with a Keplerian rotating disk and try to see if the detected asymmetry can be interpreted within the "one-armed" viscous disk framework.

Published
2006
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38. Accretion in rho-Ophiuchi brown dwarfs: infrared hydrogen line ratios

Author

Gatti, T., Testi, L., Natta, A., Randich, S., and Muzerolle, J.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Mass accretion rate determinations are fundamental for an understanding of the evolution of pre-main sequence star circumstellar disks. Magnetospheric accretion models are used to derive values of the mass accretion rates in objects of very different properties, from brown dwarfs to intermediate-mass stars; we test the validity of these models in the brown dwarf regime, where the stellar mass and luminosity, as well as the mass accretion rate, are much lower than in T Tauri stars. We have measured simultaneously two infrared hydrogen lines, Pab and Brg, in a sample of 16 objects in the star-forming region rho-Oph. The sample inc ludes 7 very low mass objects and brown dwarfs and 9 T Tauri stars. Brown dwarfs where both lines are detected have a ratio Pab/Brg of ~2. Larger values, >=3.5, are only found among the T Tauri stars. The low line ratios in brown dwarfs indicate that the lines cannot originate in the column of gas accreting from the disk onto the star along the magnetic field lines, and we suggest that they form instead in the shocked photosphere, heated to temperatures of ~3500 K. If so, in analogy to veiling estimates in T Tauri stars, the hydrogen infrared line fluxes may provide a reliable measure of the accretion rate in brown dwarfs., 11 pages, 9 figures, accepted by A&A

Published
2006

39. Searching for massive pre--stellar cores through observations of N2H+ and N2D+

Author

Fontani, F., Caselli, P., Crapsi, A., Cesaroni, R., Molinari, S., Testi, L., and Brand, J.

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

We have measured the deuterium fractionation (through the column density ratio N(N2D+)/N(N2H+)) and the CO depletion factor (ratio between expected and observed CO abundance) in a sample of 10 high-mass protostellar candidates, in order to understand whether the earliest evolutionary stages of high-mass stars have chemical characteristics similar to those of low-mass ones. The observations were carried out with the IRAM-30m telescope and the JCMT. We have detected N2D+ emission in 7 of the 10 sources of our sample, and found an average value N(N2D+)/N(N2H+)~0.015. This value is 3 orders of magnitude larger than the interstellar D/H ratio, indicating the presence of cold and dense gas, in which the physical-chemical conditions are similar to those observed in low-mass pre-stellar cores. Also, the integrated CO depletion factors show that in the majority of the sources the expected CO abundances are larger than the observed values, with a median ratio of 3.2. In principle, the cold gas that gives origin to the N2D+ emission can be the remnant of the massive molecular core in which the high-mass (proto-)star was born, not yet heated up by the central object. If so, our results indicate that the chemical properties of the clouds in which high-mass stars are born are similar to their low-mass counterparts. Alternatively, this cold gas can be located into one (or more) starless core (cores) near the protostellar object. Due to the poor angular resolution of our data, we cannot decide which is the correct scenario., 27 pages, 15 figures, accepted by Astronomy and Astrophysics

Published
2006

40. A Keplerian gaseous disk around the B0 star R Mon

Author

Fuente, A., Alonso-Albi, T., Bachiller, R., Natta, A., Testi, L., Neri, R., and Planesas, P.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, General Relativity and Quantum Cosmology
Abstract

We present high-angular resolution observations of the circumstellar disk around the massive Herbig Be star R Mon (M~8 Msun) in the continuum at 2.7mm and 1.3mm and the CO 1->0 and 2->1 rotational lines. Based on the new 1.3mm continuum image we estimate a disk mass (gas+dust) of 0.007 Msun and an outer radius of, 5 pages

Published
2006

41. Dust in Proto-Planetary Disks: Properties and Evolution

Author

Natta, A., Testi, L., Calvet, N., Henning, Th., Waters, R., and Wilner, D.

Subjects
Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We review the properties of dust in protoplanetary disks around optically visible pre-main sequence stars obtained with a variety of observational techniques, from measurements of scattered light at visual and infrared wavelengths to mid-infrared spectroscopy and millimeter interferometry. A general result is that grains in disks are on average much larger than in the diffuse interstellar medium (ISM). In many disks, there is evidence that a large mass of dust is in grains with millimeter and centimeter sizes, more similar to "sand and pebbles" than to grains. Smaller grains (with micron-sizes) exist closer to the disk surface, which also contains much smaller particles, e.g., polycyclic aromatic hydrocarbons. There is some evidence of a vertical stratification, with smaller grains closer to the surface. Another difference with ISM is the higher fraction of crystalline relative to amorphous silicates found in disk surfaces. There is a large scatter in dust properties among different sources, but no evidence of correlation with the stellar properties, for samples that include objects from intermediate to solar mass stars and brown dwarfs. There is also no apparent correlation with the age of the central object, over a range roughly between 1 and 10 Myr. This suggests a scenario where significant grain processing may occur very early in the disk evolution, possibly when it is accreting matter from the parental molecular core. Further evolution may occur, but not necessarily rapidly, since we have evidence that large amounts of grains, from micron to centimeter size, can survive for periods as long as 10 Myr., Comment: Protostars and Planets V in press, 16 pages, 7 figures

Published
2006
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42. Disentangling the wind and the disk in the close surrounding of the young stellar object MWC297 with AMBER/VLTI

Author

Fabien Malbet, Benisty, M., Wit, W. J., Kraus, S., Meilland, A., Millour, F., Tatulli, E., P Berger, J., Chesneau, O., H Hofmann, K., Isella, A., Romain Petrov, Preibisch, T., Stee, P., Testi, L., Weigelt, G., Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), F. Paresce, A. Richichi, A. Chelli, and F. Delplancke

Subjects
Accretion, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], accretion disks, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, individual: MWC297, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Planetary systems: protoplanetary disks, Infrared: stars, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Be stars, technique: interferometric, Astrophysics::Solar and Stellar Astrophysics, late-type, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Stars: pre-main-sequence
Abstract

The young stellar object MWC297 is a B1.5Ve star exhibiting strong hydrogen emission lines. This object has been observed by the AMBER/VLTI instrument in 2-telescope mode in a sub-region of the K spectral band centered around the Br gamma line at 2.1656 microns. The object has not only been resolved in the continuum with a visibility of 0.50+/-0.10, but also in the Br gamma line, where the flux is about twice larger, with a visibility about twice smaller (0.33+/-0.06). The continuum emission is consistent with the expectation of an optically thick thermal emission from dust in a circumstellar disk. The hydrogen emission can be understood by the emission of a halo above the disk surface. It can be modelled as a latitudinal-dependant wind model and it explains the width, the strength and the visibibility through the emission lines. The AMBER data associated with a high resolution ISAAC spectrum constrains the apparent size of the wind but also its kinematics., In "The Power of Optical/IR Interferometry: Recent Scientific Results and 2nd Generation VLTI Instrumentation, Allemagne (2005) in press"

Published
2005

43. First AMBER/VLTI Observations of Hot Massive Stars

Author

Romain Petrov, Millour, F., Chesneau, O., Weigelt, G., Bonneau, D., Ph. Stee, Kraus, S., Mourard, D., Meilland, A., Vannier, M., Malbet, F., Lisi, F., Antonelli, P., Kern, P., Beckmann, U., Lagarde, S., Perraut, K., Gennari, S., Le Coarer, E., Th. Driebe, Accardo, M., Robbe-Dubois, S., Ohnaka, K., Busoni, S., Roussel, A., Zins, G., Behrend, J., Ferruzi, D., Bresson, Y., Duvert, G., Nussbaum, E., Marconi, A., Ph. Feautrier, Dugué, M., Chelli, A., Tatulli, E., Heininger, M., Delboulbe, A., Bonhomme, S., Schertl, D., Testi, L., Ph. Mathias, L Monin, J., Gluck, L., Hofmann, K. H., Salinari, P., Puget, P., Clausse, J. M., Didier Fraix-Burnet, D., Renaud Foy, Isella, A., Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), European Southern Observatory (ESO), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

8 pages; International audience; AMBER is the first near infrared focal instrument of the VLTI. It combines three telescopes and produces spectrally resolved interferometric measures. This paper discusses some preliminary results of the first scientific observations of AMBER with three Unit Telescopes at medium (1500) and high (12000) spectral resolution. We derive a first set of constraints on the structure of the circumstellar material around the Wolf Rayet gamma2 Velorum and the LBV eta Carinae.

Published
2005

44. Disk and wind interaction in the young stellar object MWC 297 spatially resolved with VLTI/AMBER

Author

Malbet, F., Benisty, M., de Wit, W.J., Kraus, S., Meilland, A., Millour, F., Tatulli, E., Berger, J.P., Chesneau, O., Hofmann, K.H., Isella, A., Natta, A., Petrov, R., Preibisch, T., Stee, P., Testi, L., Weigelt, G., Antonelli, P., Beckmann, U., Bresson, Y., Chelli, A., Duvert, G., Glück, L., Kern, P., Lagarde, S., Le Coarer, E., Lisi, F., Perraut, K., Robbe-Dubois, S., Roussel, A., Zins, G., Accardo, M., Acke, B., Agabi, K., Arezki, B., Aristidi, E., Baffa, C., Behrend, J., Blöcker, T., Bonhomme, S., Busoni, S., Cassaing, F., Clausse, J.-M., Colin, J., Connot, C., Delboulbé, A., Driebe, T., Dugué, M., Feautrier, P., Ferruzzi, D., Forveille, T., Fossat, E., Foy, Renaud, Fraix-Burnet, D., Gallardo, A., Gennari, S., Glentzlin, A., Giani, E., Gil, C., Heiden, M., Heininger, M., Kamm, D., Le Contel, D., Le Contel, J.-M., Lopez, B., Magnard, Y., Marconi, A., Mars, G., Martinot-Lagarde, G., Mathias, P., Monin, J.-L., Mouillet, D., Mourard, D., Mège, P., Nussbaum, E., Ohnaka, K., Pacheco, J., Pacini, F., Perrier, C., Puget, P., Rabbia, Y., Rebattu, S., Reynaud, François, Richichi, A., Sacchettini, M., Salinari, P., Schertl, D., Solscheid, W., Stefanini, P., Tallon, Michel, Tallon-Bosc, Isabelle, Tasso, D., Valtier, J.-C., Vannier, M., Ventura, N., Kiekebusch, M., Rantakyrö, F., Schöller, M., Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), ONERA - The French Aerospace Lab [Châtillon], ONERA, Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Division technique INSU/SDU (DTI), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PHOTONIQUE, XLIM (XLIM), Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), AMBER, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ONERA-Université Paris Saclay (COmUE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Protoplanetary disks, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Pre-main-sequence stars, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Planetary systems, Early-type stars, Emission-line stars, Accretion disks, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Infrared, Interferometric Techniques, Astrophysics::Galaxy Astrophysics
Abstract

The young stellar object MWC 297 has been observed with the VLT interferometer equipped with the AMBER instrument. MWC 297 has been spatially resolved in the continuum with a visibility of 0.50 as well as in the Br gamma emission line where the visibility decrease to a lower value of 0.33. This change in the visibility with the wavelength can be interpreted by the presence of an optically thick disk responsible for the visibility in the continuum and of a stellar wind traced by Br gamma and whose apparent size is 40% larger. We validate this interpretation by building a model of the stellar environment that combines a geometrically thin, optically thick accretion disk model consisting of gas and dust, and a latitude-dependent stellar wind outflowing above the disk surface. The continuum emission and visibilities obtained from this model are fully consistent with the interferometric AMBER data. They agree also with existing optical, near-infrared spectra and other broad-band near-infrared interferometric visibilities. A picture emerges in which MWC 297 is surrounded by an equatorial flat disk that is possibly still accreting and an outflowing wind which has a much higher velocity in the polar region than at the equator. [abridged], Comment: 13 pages; to be published in A&A; Acceptance day: 11/10/2005

Published
2005
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45. Exploring Brown Dwarf Disks in rho Oph

Author

Natta, A., Testi, L., Comeron, F., Oliva, E., D'Antona, F., Baffa, C., Comoretto, G., and Gennari, S.

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

This paper discusses evidence for and properties of disks associated to brown dwarfs in the star-forming region rho-Oph. We selected nine objects fr om the ISOCAM survey of Bontemps et al. (2001) that have detections in the two mid-infrared bands (6.7 and 14.3 um), relatively low extinction and low luminosity. We present low-resolution near-infrared spectra in the J, H and K bands, and determine for each source spectral type, extinction, effective temperature a nd luminosity by comparing the spectra to those of field dwarfs and to the most recent model stellar atmospheres. The results indicate that eight objects have spectral types M6-M7.5, effective temperature of 2600-2700 K, one has a later spectral type (M8.5) and lower temperature (about 2400 K). The derived extinctions range between Av~2 and 8 mag. The location of the objects on the HR diagram, in spite of the uncertainties of the evolutionary tracks for young objects of substellar mass, indicates that all the objects are very young and have masses below about 0.08 Msun. The coolest object in our sample has mass in the range 8-12 Mjup (0.008-0.012 Msun). In all cases, the mid-infrared excess is consistent with the predictions of mode ls of disks irradiated by the central object, showing that circumstellar disks are commonly associated to young brown dwarfs and plan etary-mass objects. Finally, we discuss possible variations of the disk geometry among different objects, as well as the possibility of using these data to discriminate between various f ormation scenarios., Comment: 15 pages, A&A in press, full resolution color figures for appendix A and B are available at http://www.arcetri.astro.it/~lt/preprints/preprints.html

Published
2002
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46. The TNG Near Infrared Camera Spectrometer

Author

Baffa, C., Comoretto, G., Gennari, S., Lisi, F., Oliva, E., Biliotti, V., Checcucci, A., Gavrioussev, V., Giani, E., Ghinassi, F., Hunt, L. K., Maiolino, R., Mannuci, F., Marcucci, G., Sozzi, M., Stefanini, P., and Testi, L.

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

NICS (acronym for Near Infrared Camera Spectrometer) is the near-infrared cooled camera-spectrometer that has been developed by the Arcetri Infrared Group at the Arcetri Astrophysical Observatory, in collaboration with the CAISMI-CNR for the TNG (the Italian National Telescope Galileo at La Palma, Canary Islands, Spain). As NICS is in its scientific commissioning phase, we report its observing capabilities in the near-infrared bands at the TNG, along with the measured performance and the limiting magnitudes. We also describe some technical details of the project, such as cryogenics, mechanics, and the system which executes data acquisition and control, along with the related software., 7 pages, 5 figures, compiled with A&A macros. A&A in press

Published
2001

47. Northern JHK Standard Stars for Array Detectors

Author

Hunt, L. K., filippo mannucci, Testi, L., Migliorini, S., Stanga, R. M., Baffa, C., Lisi, F., and Vanzi, L.

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

We report J, H and K photometry of 86 stars in 40 fields in the northern hemisphere. The fields are smaller than or comparable to a 4x4 arcmin field-of-view, and are roughly uniformly distributed over the sky, making them suitable for a homogeneous broadband calibration network for near-infrared panoramic detectors. K magnitudes range from 8.5 to 14, and J-K colors from -0.1 to 1.2. The photometry is derived from a total of 3899 reduced images; each star has been measured, on average, 26.0 times per filter on 5.5 nights. Typical errors on the photometry are about 0.012., Comment: 10 pages including 3 figures, one separate figure on four pages. The finding chart of the AS-30 field and a few coordinates have been corrected. GIF finding charts can also be found at http://www.arcetri.astro.it/~hunt/std.html

Published
1998
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48. Near Infrared Spectra of the Orion Bar

Author

Alessandro Marconi, Testi, L., Natta, A., and Walmsley, C. M.

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

We have used the LONGSP spectrometer on the 1.5-m TIRGO telescope to obtain long slit spectra in the J, H, and K wavelength bands towards two positions along the Orion bar. These data have been supplemented with images made using the ARNICA camera mounted on TIRGO as well as with an ESO NTT observation carried out by Dr A. Moorwood. We detect a variety of transitions of hydrogen, helium, OI, FeII, FeIII, and H_2 . From our molecular hydrogen data, we conclude that densities are moderate (3-6 10^4 cm^-3) in the layer responsible for the molecular hydrogen emission and give no evidence for the presence of dense neutral clumps. We also find that the molecular hydrogen bar is likely to be tilted by ~10 degrees relative to the line of sight. We discuss the relative merits of several models of the structure of the bar and conclude that it may be split into two structures separated by 0.2-0.3 parsec along the line of sight. It also seems likely to us that in both structures, density increases along a line perpendicular to the ionization front which penetrates into the neutral gas. We have used the 1.317um OI line to estimate the FUV radiation field incident at the ionization front and find values of 1-3x10^4 greater than the average interstellar field. From [FeII] line measurements, we conclude that the electron density in the ionized layer associated with the ionization front is of order 10^4 cm^-3. Finally, our analysis of the helium and hydrogen recombination lines implies essential coincidence of the helium and hydrogen Stromgren spheres., Comment: 17 pages with 17 figures included. Accepted for publication by Astronomy and Astrophysics

Published
1997
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49. Complex organic molecules in protostellar environments in the SKA era

Author

Codella, C., Podio, L., Fontani, F., Jiménez-Serra, I., Caselli, P., Ceccarelli, C., Palumbo, M. E., López-Sepulcre, A., Beltrán, M. T., Lefloch, B., John Robert Brucato, Viti, S., and Testi, L.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Molecular complexity builds up at each step of the Sun-like star formation process, starting from simple molecules and ending up in large polyatomic species. Complex organic molecules (COMs; such as methyl formate, HCOOCH$_3$, dymethyl ether, CH$_3$OCH$_3$, formamide, NH$_2$CHO, or glycoaldehyde, HCOCH$_2$OH) are formed in all the components of the star formation recipe (e.g. pre-stellar cores, hot-corinos, circumstellar disks, shocks induced by fast jets), due to ice grain mantle sublimation or sputtering as well as gas-phase reactions. Understanding in great detail the involved processes is likely the only way to predict the ultimate molecular complexity reached in the ISM, as the detection of large molecules is increasingly more difficult with the increase of the number of atoms constituting them. Thanks to the recent spectacular progress of astronomical observations, due to the Herschel (sub-mm and IR), IRAM and SMA (mm and sub-mm), and NRAO (cm) telescopes, an enormous activity is being developed in the field of Astrochemistry, extending from astronomical observatories to chemical laboratories. We are involved in several observational projects providing unbiased spectral surveys (in the 80-300 and 500-2000 GHz ranges) with unprecedented sensitivity of templates of dense cores and protostars. Forests of COM lines have been detected. In this chapter we will focus on the chemistry of both cold prestellar cores and hot shocked regions, (i) reviewing results and open questions provided by mm-FIR observations, and (ii) showing the need of carrying on the observations of COMs at lower frequencies, where SKA will operate. We will also emphasize the importance of analysing the spectra by the light of the experimental studies performed by our team, who is investigating the chemical effects induced by ionising radiation bombarding astrophysically relevant ices., Comment: 18 pages, 8 figures

50. ESO-Athena Synergy White Paper

Author

Padovani, P., Combes, F., Diaz Trigo, M., Ettori, S., Hatziminaoglou, E., Jonker, P., Salvato, M., Viti, S., Adami, C., Aird, J., Alexander, D., Casella, P., Ceccarelli, C., Churazov, E., Cirasuolo, M., Daddi, E., Edge, A., Feruglio, C., Mainieri, V., Markoff, S., Merloni, A., Nicastro, F., O Brien, P., Oskinova, L., Panessa, F., Pointecouteau, E., Rau, A., Robrade, J., Joop Schaye, Stoehr, F., Testi, L., Tombesi, F., 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), and bibliotheque, la.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Advanced Telescope for High ENergy Astrophysics (Athena) is the X-ray observatory mission selected by ESA within its Cosmic Vision 2015-2025 programme to address the Hot and Energetic Universe scientific theme. The ESO-Athena Synergy Team (EAST) has been tasked to single out the potential scientific synergies between Athena and optical/near-infrared (NIR) and sub/mm ground based facilities, in particular those of ESO (i.e., the VLT and ELT, ALMA and APEX), by producing a White Paper to identify and develop the: 1. needs to access ESO ground-based facilities to achieve the formulated Athena science objectives; 2. needs to access Athena to achieve the formulated science objectives of ESO facilities contemporary to Athena; 3. science areas where the synergetic use of Athena and ESO facilities in the late 2020s will result in scientific added value. Community input to the process happened primarily via a dedicated ESO - Athena Synergy Workshop that took place on Sept. 14 - 16, 2016 at ESO, Garching. This White Paper presents the results of the EAST's work, sorted by synergy area, and deals with the following topics: 1. the Hot Universe: Early groups and clusters and their evolution, Physics of the Intracluster medium, Missing baryons in cosmic filaments; 2. the Energetic Universe: Supermassive black hole (SMBH) history, SMBH accretion disks, Active Galactic Nuclei feedback - Molecular outflows, Ultra-fast outflows, Accretion Physics, Transient Science; 3. Observatory Science: Star Formation, Stars. It then discusses the optical-NIR-sub-mm perspective by providing details on VLT/MOONS, the E-ELT instruments, in particular the MOS, VISTA/4MOST, the ESO and ALMA archives, future ALMA and ESO developments, and finally the (likely) ESO - Athena astronomical scene in the 2020s. (abridged), Comment: 70 pages, 16 figures

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