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20 results on '"Polychroni, D."'

1. The GAPS Programme at TNG: LXI. Atmospheric parameters and elemental abundances of TESS young exoplanet host stars.

Author

Filomeno, S., Biazzo, K., Baratella, M., Benatti, S., D'Orazi, V., Desidera, S., Mancini, L., Messina, S., Polychroni, D., Turrini, D., Cabona, L., Carleo, I., Damasso, M., Malavolta, L., Mantovan, G., Nardiello, D., Scandariato, G., Sozzetti, A., Zingales, T., and Andreuzzi, G.

Subjects
STELLAR atmospheres, HOT Jupiters, PLANETARY mass, HEAVY elements, PLANETARY systems
Abstract

Context. The study of exoplanets at different evolutionary stages can shed light on their formation, migration, and evolution. The determination of exoplanet properties depends on the properties of their host stars. It is therefore important to characterise the host stars for accurate knowledge on their planets. Aims. Our final goal is to derive, in a homogeneous and accurate way, the stellar atmospheric parameters and elemental abundances of ten young TESS (Transiting Exoplanet Survey Satellite) transiting planet-hosting GK stars followed up with the HARPS-N (High Accuracy Radial velocity Planet Searcher for the Northern hemisphere) at TNG (Telescopio Nazionale Galileo) spectrograph within the Global Architecture of Planetary Systems (GAPS) programme. Methods. We derived stellar kinematic properties, atmospheric parameters, and abundances of 18 elements. Depending on stellar parameters and chemical elements, we used methods based on line equivalent widths and spectral synthesis. Lithium line measurements were used as approximate age estimations. We exploited chemical abundances and their ratios to derive information on planetary composition. Results. Elemental abundances and kinematic properties are consistent with the nearby Galactic thin disk. All targets show C/O<0.8 and 1.0

Published
2024
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2. The GAPS programme at TNG

Author

Mantovan, G., primary, Malavolta, L., additional, Desidera, S., additional, Zingales, T., additional, Borsato, L., additional, Piotto, G., additional, Maggio, A., additional, Locci, D., additional, Polychroni, D., additional, Turrini, D., additional, Baratella, M., additional, Biazzo, K., additional, Nardiello, D., additional, Stassun, K., additional, Nascimbeni, V., additional, Benatti, S., additional, Anna John, A., additional, Watkins, C., additional, Bieryla, A., additional, Lissauer, J. J., additional, Twicken, J. D., additional, Lanza, A. F., additional, Winn, J. N., additional, Messina, S., additional, Montalto, M., additional, Sozzetti, A., additional, Boffin, H., additional, Cheryasov, D., additional, Strakhov, I., additional, Murgas, F., additional, D’Arpa, M., additional, Barkaoui, K., additional, Benni, P., additional, Bignamini, A., additional, Bonomo, A. S., additional, Borsa, F., additional, Cabona, L., additional, Cameron, A. C., additional, Claudi, R., additional, Cochran, W., additional, Collins, K. A., additional, Damasso, M., additional, Dong, J., additional, Endl, M., additional, Fukui, A., additional, Fűrész, G., additional, Gandolfi, D., additional, Ghedina, A., additional, Jenkins, J., additional, Kabáth, P., additional, Latham, D. W., additional, Lorenzi, V., additional, Luque, R., additional, Maldonado, J., additional, McLeod, K., additional, Molinaro, M., additional, Narita, N., additional, Nowak, G., additional, Orell-Miquel, J., additional, Pallé, E., additional, Parviainen, H., additional, Pedani, M., additional, Quinn, S. N., additional, Relles, H., additional, Rowden, P., additional, Scandariato, G., additional, Schwarz, R., additional, Seager, S., additional, Shporer, A., additional, Vanderburg, A., additional, and Wilson, T. G., additional

Published
2024
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3. The GAPS program at TNG. XLVIII. The unusual formation history of V1298 Tau

Author

Turrini, D., primary, Marzari, F., additional, Claudi, R., additional, Polychroni, D., additional, Desidera, S., additional, Mesa, D., additional, Sozzetti, A., additional, Benatti, S., additional, Damasso, M., additional, Malavolta, L., additional, Micela, G., additional, Zinzi, A., additional, Suárez Mascareño;, A., additional, Béjar;, V. J. S., additional, Biazzo, K., additional, Bignamini, A., additional, Bonavita; ;, M., additional, Borsa, F., additional, and Chauvin, G., additional

Published
2023
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4. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues First data release for the inner Milky Way:+68 degrees >= l >=-70 degrees

Author

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

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

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

Published
2016

5. The earliest phases of high-mass star formation, as seen in NGC 6334 by Herschel-HOBYS

Author

Tigé, J., primary, Motte, F., additional, Russeil, D., additional, Zavagno, A., additional, Hennemann, M., additional, Schneider, N., additional, Hill, T., additional, Nguyen Luong, Q., additional, Di Francesco, J., additional, Bontemps, S., additional, Louvet, F., additional, Didelon, P., additional, Könyves, V., additional, André, Ph., additional, Leuleu, G., additional, Bardagi, J., additional, Anderson, L. D., additional, Arzoumanian, D., additional, Benedettini, M., additional, Bernard, J.-P., additional, Elia, D., additional, Figueira, M., additional, Kirk, J., additional, Martin, P. G., additional, Minier, V., additional, Molinari, S., additional, Nony, T., additional, Persi, P., additional, Pezzuto, S., additional, Polychroni, D., additional, Rayner, T., additional, Rivera-Ingraham, A., additional, Roussel, H., additional, Rygl, K., additional, Spinoglio, L., additional, and White, G. J., additional

Published
2017
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6. Hi-GAL, theHerschelinfrared Galactic Plane Survey: photometric maps and compact source catalogues

Author

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

Abstract

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

Published
2016

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

Author

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

Published
2016
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8. Recent star formation in the Lupus clouds as seen by Herschel [Letter]

Author

Rygl, K. L. J., Benedettini, M., Schisano, E., Elia, D., Molinari, S., Pezzuto, S., Andre, Ph., Bernard, J. P., White, G. J., Polychroni, D., Bontemps, S., Cox, N. L. J., Di Francesco, J., Facchini, A., Fallscheer, C., di Giorgio, A. M., Hennemann, M., Hill, T., Koenyves, V., Minier, V., Motte, F., Nguyen-Luong, Q., Peretto, Nicolas, Pestalozzi, M., Sadavoy, S., Schneider, N., Spinoglio, L., Testi, L., and Ward-Thompson, Derek

Subjects
endocrine system, QB
Abstract

We present a study of the star formation histories of the Lupus I, III, and IV clouds using the Herschel 70–500 μm maps obtained by the Herschel Gould Belt Survey Key Project. By combining the new Herschel data with the existing Spitzer catalog we obtained an unprecedented census of prestellar sources and young stellar objects in the Lupus clouds, which allowed us to study the overall star formation rate (SFR) and efficiency (SFE). The high SFE of Lupus III, its decreasing SFR, and its large number of pre-main sequence stars with respect to proto- and prestellar sources, suggest that Lupus III is the most evolved cloud, and after having experienced a major star formation event in the past, is now approaching the end of its current star-forming cycle. Lupus I is currently undergoing a large star formation event, apparent by the increasing SFR, the large number of prestellar objects with respect to more evolved objects, and the high percentage of material at high extinction (e.g., above AV ≈ 8 mag). Also Lupus IV has an increasing SFR; however, the relative number of prestellar sources is much lower, suggesting that its star formation has not yet reached its peak.

Published
2013

9. Recent star formation in the Lupus clouds as seen byHerschel

Author

Rygl, K. L. J., Benedettini, M., Schisano, E., Elia, D., Molinari, S., Pezzuto, S., André, Ph., Bernard, J. P., White, G. J., Polychroni, D., Bontemps, S., Cox, N. L. J., Di Francesco, J., Facchini, A., Fallscheer, C., di Giorgio, A. M., Hennemann, M., Hill, T., Könyves, V., Minier, V., Motte, F., Nguyen-Luong, Q., Peretto, N., Pestalozzi, M., Sadavoy, S., Schneider, N., Spinoglio, L., Testi, L., Ward-Thompson, Derek, Rygl, K. L. J., Benedettini, M., Schisano, E., Elia, D., Molinari, S., Pezzuto, S., André, Ph., Bernard, J. P., White, G. J., Polychroni, D., Bontemps, S., Cox, N. L. J., Di Francesco, J., Facchini, A., Fallscheer, C., di Giorgio, A. M., Hennemann, M., Hill, T., Könyves, V., Minier, V., Motte, F., Nguyen-Luong, Q., Peretto, N., Pestalozzi, M., Sadavoy, S., Schneider, N., Spinoglio, L., Testi, L., and Ward-Thompson, Derek

Abstract

We present a study of the star formation histories of the Lupus I, III, and IV clouds using the Herschel 70-500μm maps obtained by the Herschel Gould Belt Survey Key Project. By combining the new Herschel data with the existing Spitzer catalog we obtained an unprecedented census of prestellar sources and young stellar objects in the Lupus clouds, which allowed us to study the overall star formation rate (SFR) and efficiency (SFE). The high SFE of Lupus III, its decreasing SFR, and its large number of pre-main sequence stars with respect to proto-and prestellar sources, suggest that Lupus III is the most evolved cloud, and after having experienced a major star formation event in the past, is now approaching the end of its current star-forming cycle. Lupus I is currently undergoing a large star formation event, apparent by the increasing SFR, the large number of prestellar objects with respect to more evolved objects, and the high percentage of material at high extinction (e.g., above AVA ≈ A 8A mag). Also Lupus IV has an increasing SFR; however, the relative number of prestellar sources is much lower, suggesting that its star formation has not yet reached its peak. © 2012 ESO.

Published
2013

10. The Herschel view of the massive star-forming region NGC 6334

Author

Russeil, D., Schneider, N., Anderson, L. D., Zavagno, A., Molinari, S., Persi, P., Bontemps, S., Motte, F., Ossenkopf, V., André, Ph., Arzoumanian, D., Bernard, J.-Ph., Deharveng, L., Didelon, P., Di Francesco, J., Elia, D., Hennemann, M., Hill, T., Könyves, V., Li, J. Z., Martin, P. G., Nguyen Luong, Q., Peretto, N., Pezzuto, S., Polychroni, D., Roussel, H., Rygl, K. L. J., Spinoglio, L., Testi, L., Tigé, J., Vavrek, R., Ward-Thompson, Derek, White, G., Russeil, D., Schneider, N., Anderson, L. D., Zavagno, A., Molinari, S., Persi, P., Bontemps, S., Motte, F., Ossenkopf, V., André, Ph., Arzoumanian, D., Bernard, J.-Ph., Deharveng, L., Didelon, P., Di Francesco, J., Elia, D., Hennemann, M., Hill, T., Könyves, V., Li, J. Z., Martin, P. G., Nguyen Luong, Q., Peretto, N., Pezzuto, S., Polychroni, D., Roussel, H., Rygl, K. L. J., Spinoglio, L., Testi, L., Tigé, J., Vavrek, R., Ward-Thompson, Derek, and White, G.

Abstract

Aims. Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the contributions of turbulence and gravity. Methods. We used Herschel PACS and SPIRE imaging observations from the HOBYS key programme at wavelengths of 160, 250, 350, and 500 μm to construct dust temperature and column density maps. Using probability distribution functions (PDFs) of the column density determined for the whole complex and for four distinct sub-regions (distinguished on the basis of differences in the column density, temperature, and radiation field), we characterize the density structure of the complex. We investigate the spatial structure using the Δ-variance, which probes the relative amount of structure on different size scales and traces possible energy injection mechanisms into the molecular cloud. Results. The Δ-variance analysis suggests that the significant scales of a few parsec that were found are caused by energy injection due to expanding H ii regions, which are numerous, and by the lengths of filaments seen everywhere in the complex. The column density PDFs have a lognormal shape at low densities and a clearly defined power law at high densities for all sub-regions whose slope is linked to the exponent α of an equivalent spherical density distribution. In particular with α = 2.37, the central sub-region is largly dominated by gravity, caused by individual collapsing dense cores and global collapse of a larger region. The collapse is faster than free-fall (which would lead only to α = 2) and thus requires a more dynamic scenario (external compression, flows). The column density PDFs suggest that the different sub-regions are at different evolutionary stages, especially the central sub-region, which seems to be in a more evolved stage. © 2013 ESO.

Published
2013

11. TheHerschelview of the massive star-forming region NGC 6334

Author

Russeil, D., primary, Schneider, N., additional, Anderson, L. D., additional, Zavagno, A., additional, Molinari, S., additional, Persi, P., additional, Bontemps, S., additional, Motte, F., additional, Ossenkopf, V., additional, André, Ph., additional, Arzoumanian, D., additional, Bernard, J.-Ph., additional, Deharveng, L., additional, Didelon, P., additional, Di Francesco, J., additional, Elia, D., additional, Hennemann, M., additional, Hill, T., additional, Könyves, V., additional, Li, J. Z., additional, Martin, P. G., additional, Nguyen Luong, Q., additional, Peretto, N., additional, Pezzuto, S., additional, Polychroni, D., additional, Roussel, H., additional, Rygl, K. L. J., additional, Spinoglio, L., additional, Testi, L., additional, Tigé, J., additional, Vavrek, R., additional, Ward-Thompson, D., additional, and White, G., additional

Published
2013
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12. On the shape of the mass-function of dense clumps in the Hi-GAL fields

Author

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

Published
2013
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13. Recent star formation in the Lupus clouds as seen byHerschel

Author

Rygl, K. L. J., primary, Benedettini, M., additional, Schisano, E., additional, Elia, D., additional, Molinari, S., additional, Pezzuto, S., additional, André, Ph., additional, Bernard, J. P., additional, White, G. J., additional, Polychroni, D., additional, Bontemps, S., additional, Cox, N. L. J., additional, Di Francesco, J., additional, Facchini, A., additional, Fallscheer, C., additional, di Giorgio, A. M., additional, Hennemann, M., additional, Hill, T., additional, Könyves, V., additional, Minier, V., additional, Motte, F., additional, Nguyen-Luong, Q., additional, Peretto, N., additional, Pestalozzi, M., additional, Sadavoy, S., additional, Schneider, N., additional, Spinoglio, L., additional, Testi, L., additional, and Ward-Thompson, D., additional

Published
2012
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14. Herschelobservations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud

Author

Pezzuto, S., primary, Elia, D., additional, Schisano, E., additional, Strafella, F., additional, Di Francesco, J., additional, Sadavoy, S., additional, André, P., additional, Benedettini, M., additional, Bernard, J. P., additional, di Giorgio, A. M., additional, Facchini, A., additional, Hennemann, M., additional, Hill, T., additional, Könyves, V., additional, Molinari, S., additional, Motte, F., additional, Nguyen-Luong, Q., additional, Peretto, N., additional, Pestalozzi, M., additional, Polychroni, D., additional, Rygl, K. L. J., additional, Saraceno, P., additional, Schneider, N., additional, Spinoglio, L., additional, Testi, L., additional, Ward-Thompson, D., additional, and White, G. J., additional

Published
2012
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15. The M 16 molecular complex under the influence of NGC 6611

Author

Hill, T., primary, Motte, F., additional, Didelon, P., additional, White, G. J., additional, Marston, A. P., additional, Nguyên Luong, Q., additional, Bontemps, S., additional, André, Ph., additional, Schneider, N., additional, Hennemann, M., additional, Sauvage, M., additional, Di Francesco, J., additional, Minier, V., additional, Anderson, L. D., additional, Bernard, J. P., additional, Elia, D., additional, Griffin, M. J., additional, Li, J. Z., additional, Peretto, N., additional, Pezzuto, S., additional, Polychroni, D., additional, Roussel, H., additional, Rygl, K. L. J., additional, Schisano, E., additional, Sousbie, T., additional, Testi, L., additional, Ward Thompson, D., additional, and Zavagno, A., additional

Published
2012
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16. TheHerschelview of the on-going star formation in the Vela-C molecular cloud

Author

Giannini, T., primary, Elia, D., additional, Lorenzetti, D., additional, Molinari, S., additional, Motte, F., additional, Schisano, E., additional, Pezzuto, S., additional, Pestalozzi, M., additional, Di Giorgio, A. M., additional, André, P., additional, Hill, T., additional, Benedettini, M., additional, Bontemps, S., additional, Di Francesco, J., additional, Fallscheer, C., additional, Hennemann, M., additional, Kirk, J., additional, Minier, V., additional, Nguyen Luong, Q., additional, Polychroni, D., additional, Rygl, K. L. J., additional, Saraceno, P., additional, Schneider, N., additional, Spinoglio, L., additional, Testi, L., additional, Ward-Thompson, D., additional, and White, G. J., additional

Published
2012
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17. AHerschelstudy of YSO evolutionary stages and formation timelines in two fields of the Hi-GAL survey

Author

Elia, D., primary, Schisano, E., additional, Molinari, S., additional, Robitaille, T., additional, Anglés-Alcázar, D., additional, Bally, J., additional, Battersby, C., additional, Benedettini, M., additional, Billot, N., additional, Calzoletti, L., additional, Di Giorgio, A. M., additional, Faustini, F., additional, Li, J. Z., additional, Martin, P., additional, Morgan, L., additional, Motte, F., additional, Mottram, J. C., additional, Natoli, P., additional, Olmi, L., additional, Paladini, R., additional, Piacentini, F., additional, Pestalozzi, M., additional, Pezzuto, S., additional, Polychroni, D., additional, Smith, M. D., additional, Strafella, F., additional, Stringfellow, G. S., additional, Testi, L., additional, Thompson, M. A., additional, Traficante, A., additional, and Veneziani, M., additional

Published
2010
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18. Clouds, filaments, and protostars: TheHerschel Hi-GAL Milky Way

Author

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

Published
2010
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19. Herschel observations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud.

Author

Pezzuto, S., Elia, D., Schisano, E., Strafella, F., Di Francesco, J., Sadavoy, S., André, P., Benedettini, M., Bernard, J. P., di Giorgio, A. M., Facchini, A., Hennemann, M., Hill, T., Könyves, V., Molinari, S., Motte, F., Nguyen-Luong, Q., Peretto, N., Pestalozzi, M., and Polychroni, D.

Subjects
HYDROSTATICS, STAR formation, ASTRONOMICAL photometry, SPECTRAL energy distribution, ASTRONOMY, ASTROPHYSICS
Abstract

We report far-infrared Herschel observations obtained between 70 μm and 500 μm of two star-forming dusty condensations, [HKM99] B1-bS and [HKM99] B1-bN, in the B1 region of the Perseus star-forming cloud. In the western part of the Perseus cloud, B1-bS is the only source detected in all six PACS and SPIRE photometric bands, but it is not visible in the Spitzer map at 24 μm. B1-bN is clearly detected between 100 μm and 250 μm. We have fitted the spectral energy distributions of these sources to derive their physical properties, and find that a simple greybody model fails to reproduce the observed spectral energy distributions. At least a two-component model is required, consisting of a central source surrounded by a dusty envelope. The properties derived from the fit, however, suggest that the central source is not a Class 0 object. We then conclude that while B1-bS and B1-bN appear to be more evolved than a pre-stellar core, the best-fit models suggest that their central objects are younger than a Class 0 source. Hence, they may be good candidates to be examples of the first hydrostatic core phase. The projected distance between B1-bS and B1-bN is a few Jeans lengths. If their physical separation is close to this value, this pair would allow studying the mutual interactions between two forming stars at a very early stage of their evolution [ABSTRACT FROM AUTHOR]

Published
2012
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20. The Herschel view of the on-going star formation in the Vela-C molecular cloud.

Author

Giannini, T., Elia, D., Lorenzetti, D., Molinari, S., Motte, F., Schisano, E., Pezzuto, S., Pestalozzi, M., Di Giorgio, A. M., André, P., Hill, T., Benedettini, M., Bontemps, S., Di Francesco, J., Fallscheer, C., Hennemann, M., Kirk, J., Minier, V., Nguyên Lu'o'ng, Q., and Polychroni, D.

Subjects
STAR formation, ASTRONOMICAL photometry, MOLECULAR clouds, PROTOSTARS, CIRCUMSTELLAR matter
Abstract

Aims. As part of the Herschel guaranteed time key programme "HOBYS", we present the PACS and SPIRE photometric survey of the star-forming region Vela-C, one of the nearest sites of low-to-high-mass star formation in the Galactic plane. Our main objectives are to take a census of the cold sources and to derive their mass distribution down to a few solar masses. Methods. Vela-C was observed with PACS and SPIRE in parallel mode at five wavelengths between 70 μm and 500 μm over an area of about 3 square degrees. A photometric catalogue was extracted from the detections in each of the five bands, using a threshold of 5σ over the local background. Out of this catalogue we selected a robust sub-sample of 268 sources, of which ∼75% are cloud clumps (diameter between 0.05 pc and 0.13 pc) and 25% are cores (diameter between 0.025 pc and 0.05 pc). Their spectral energy distributions (SEDs) were fitted with a modified black body function. We classify 48 sources as protostellar, based on their detection at 70 μm or at shorther wavelengths, and 218 as starless, because of non-detections at 70 μm. For two other sources, we do not provide a secure classification, but suggest they are Class 0 protostars. Results. From the SED fitting we derived key physical parameters (i.e.mass, temperature, bolometric luminosity). Protostellar sources are in general warmer ([T] = 12.8K) and more compact ([diameter] = 0.040 pc) than starless sources ([T] = 10.3K, [diameter] = 0.067 pc). Both these findings can be ascribed to the presence of an internal source(s) of moderate heating, which also causes a temperature gradient and hence a more peaked intensity distribution. Moreover, the reduced dimensions of protostellar sources may indicate that they will not fragment further. A virial analysis of the starless sources gives an upper limit of 90% probability for the sources to be gravitationally bound and therefore prestellar in nature. A luminosity vs. mass diagram of the two populations shows that protostellar sources are in the early accretion phase, while prestellar sources populate a region of the diagram where mass accretion has not started yet. We fitted a power law N(log M) α M-1.1±0.2 to the linear portion of the mass distribution of prestellar sources. This is in between that typical of CO clumps and those of cores in nearby star-forming regions. We interpret this as a result of the inhomogeneity of our sample, which is composed of comparable fractions of clumps and cores. [ABSTRACT FROM AUTHOR]

Published
2012
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