Search

Your search keyword '"Schisano, E."' showing total 278 results
Start Over Author "Schisano, E."
278 results on '"Schisano, E."'

251. 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., Nguyn Lu’o’ng, Q., Polychroni, D., Rygl, K. L. J., Saraceno, P., Schneider, N., Spinoglio, L., Testi, L., Ward-Thompson, D., White, G. J., 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., Nguyn Lu’o’ng, Q., Polychroni, D., Rygl, K. L. J., Saraceno, P., Schneider, N., Spinoglio, L., Testi, L., Ward-Thompson, D., and White, G. J.

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 shorter 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 ( = 12.8 K) and more compact ( = 0.040 pc) than starless sources ( = 10.3 K, = 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 gravita

252. Recent star formation in the Lupus clouds as seen by Herschel

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, D., 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, D.

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.

253. A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey

Author

Könyves, V., André, Ph., Men’shchikov, A., Palmeirim, P., Arzoumanian, D., Schneider, N., Roy, A., Didelon, P., Maury, A., Shimajiri, Y., Di Francesco, J., Bontemps, S., Peretto, N., Benedettini, M., Bernard, J.-Ph., Elia, D., Griffin, M. J., Hill, T., Kirk, J., Ladjelate, B., Marsh, K., Martin, P. G., Motte, F., Nguyên Luong, Q., Pezzuto, S., Roussel, H., Rygl, K. L. J., Sadavoy, S. I., Schisano, E., Spinoglio, L., Ward-Thompson, D., White, G. J., Könyves, V., André, Ph., Men’shchikov, A., Palmeirim, P., Arzoumanian, D., Schneider, N., Roy, A., Didelon, P., Maury, A., Shimajiri, Y., Di Francesco, J., Bontemps, S., Peretto, N., Benedettini, M., Bernard, J.-Ph., Elia, D., Griffin, M. J., Hill, T., Kirk, J., Ladjelate, B., Marsh, K., Martin, P. G., Motte, F., Nguyên Luong, Q., Pezzuto, S., Roussel, H., Rygl, K. L. J., Sadavoy, S. I., Schisano, E., Spinoglio, L., Ward-Thompson, D., and White, G. J.

Abstract

We present and discuss the results of the $Herschel$ Gould Belt survey (HGBS) observations in an ~11 $deg^2$ area of the Aquila molecular cloud complex at $d$ ~ 260 pc, imaged with the SPIRE and PACS photometric cameras in parallel mode from $70\mu m$ to $500\mu m$. Using the multi-scale, multi-wavelength source extraction algorithm $getsources$, we identify a complete sample of starless dense cores and embedded (Class 0-I) protostars in this region, and analyze their global properties and spatial distributions. We find a total of 651 starless cores, ~60% ± 10% of which are gravitationally bound prestellar cores, and they will likely form stars in the future. We also detect 58 protostellar cores. The core mass function (CMF) derived for the large population of prestellar cores is very similar in shape to the stellar initial mass function (IMF), confirming earlier findings on a much stronger statistical basis and supporting the view that there is a close physical link between the stellar IMF and the prestellar CMF. The global shift in mass scale observed between the CMF and the IMF is consistent with a typical star formation efficiency of ~40% at the level of an individual core. By comparing the numbers of starless cores in various density bins to the number of young stellar objects (YSOs), we estimate that the lifetime of prestellar cores is ~1 Myr, which is typically ~4 times longer than the core free-fall time, and that it decreases with average core density. We find a strong correlation between the spatial distribution of prestellar cores and the densest filaments observed in the Aquila complex. About 90% of the $Herschel$-identified prestellar cores are located above a background column density corresponding to $A_V$ ~ 7, and ~75% of them lie within filamentary structures with supercritical masses per unit length ≳16 $M_{\odot}/pc$. These findings support a picture wherein the cores making up the peak of the CMF (and probably responsible for the base of the IMF)

254. Two mass distributions in the L 1641 molecular clouds: the Herschel connection of dense cores and filaments in Orion A

Author

Polychroni, D., Schisano, E., Elia, D., Roy, A., Molinari, S., Martin, P., André, Ph., Turrini, D., Rygl, K. L. J., Di Francesco, J., Benedettini, M., Busquet, G., di Giorgio, A. M., Pestalozzi, M., Pezzuto, S., Arzoumanian, D., Bontemps, S., Hennemann, M., Hill, T., Könyves, V., Men'shchikov, A., Motte, F., Nguyen-Luong, Q., Peretto, N., Schneider, N., White, Glenn, Polychroni, D., Schisano, E., Elia, D., Roy, A., Molinari, S., Martin, P., André, Ph., Turrini, D., Rygl, K. L. J., Di Francesco, J., Benedettini, M., Busquet, G., di Giorgio, A. M., Pestalozzi, M., Pezzuto, S., Arzoumanian, D., Bontemps, S., Hennemann, M., Hill, T., Könyves, V., Men'shchikov, A., Motte, F., Nguyen-Luong, Q., Peretto, N., Schneider, N., and White, Glenn

Abstract

We present Herschel survey maps of the L 1641 molecular clouds in Orion A. We extracted both the filaments and dense cores in the region. We identified which of the dense sources are proto- or pre-stellar, and studied their association with the identified filaments. We find that although most (71%) of the pre-stellar sources are located on filaments there, is still a significant fraction of sources not associated with such structures. We find that these two populations (on and off the identified filaments) have distinctly different mass distributions. The mass distribution of the sources on the filaments is found to peak at 4 M ⊙ and drives the shape of the core mass function (CMF) at higher masses, which we fit with a power law of the form dN/dlogM∝M -1.4 ± 0.4. The mass distribution of the sources off the filaments, on the other hand, peaks at 0.8 M ⊙ and leads to a flattening of the CMF at masses lower than ~4 M ⊙. We postulate that this difference between the mass distributions is due to the higher proportion of gas that is available in the filaments, rather than in the diffuse cloud. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

255. A Herschel and BIMA study of the sequential star formation near the W 48A H II region

Author

Rygl, K. L. J., Goedhart, S., Polychroni, D., Wyrowski, F., Motte, F., Elia, D., Nguyen-Luong, Q., Didelon, P., Pestalozzi, M., Benedettini, M., Molinari, S., André, Ph., Fallscheer, C., Gibb, A., di Giorgio, A. M., Hill, T., Könyves, V., Marston, A., Pezzuto, S., Rivera-Ingraham, A., Schisano, E., Schneider, N., Spinoglio, L., Ward-Thompson, D., White, G. J., Rygl, K. L. J., Goedhart, S., Polychroni, D., Wyrowski, F., Motte, F., Elia, D., Nguyen-Luong, Q., Didelon, P., Pestalozzi, M., Benedettini, M., Molinari, S., André, Ph., Fallscheer, C., Gibb, A., di Giorgio, A. M., Hill, T., Könyves, V., Marston, A., Pezzuto, S., Rivera-Ingraham, A., Schisano, E., Schneider, N., Spinoglio, L., Ward-Thompson, D., and White, G. J.

Abstract

We present the results of Herschel HOBYS (Herschel imaging survey of OB Young Stellar objects) photometric mapping combined with Berkeley Illinois Maryland Association (BIMA) observations and additional archival data, and perform an in-depth study of the evolutionary phases of the star-forming clumps in W 48A and their surroundings. Age estimates for the compact sources were derived from bolometric luminosities and envelope masses, which were obtained from the dust continuum emission, and agree within an order of magnitude with age estimates from molecular line and radio data. The clumps in W 48A are linearly aligned by age (east-old to west-young): we find a ultra-compact (UC) H II region, a young stellar object (YSO) with class II methanol maser emission, a YSO with a massive outflow and finally the NH2D prestellar cores from Pillai et al. This remarkable positioning reflects the (star) formation history of the region. We find that it is unlikely that the star formation in the W 48A molecular cloud was triggered by the UC H II region and discuss the Aquila supershell expansion as a major influence on the evolution of W 48A. We conclude that the combination of Herschel continuum data with interferometric molecular line and radio continuum data is important to derive trustworthy age estimates and interpret the origin of large-scale structures through kinematic information.

256. The spine of the swan: a Herschel study of the DR21 ridge and filaments in Cygnus X

Author

Hennemann, M., Motte, F., Schneider, N., Didelon, P., Hill, T., Arzoumanian, D., Bontemps, S., Csengeri, T., André, Ph., Konyves, V., Louvet, F., Marston, A., Men’shchikov, A., Minier, V., Nguyen Luong, Q., Palmeirim, P., Peretto, N., Sauvage, M., Zavagno, A., Anderson, L. D., Bernard, J.-Ph., Di Francesco, J., Elia, D., Li, J. Z., Martin, P. G., Molinari, S., Pezzuto, S., Russeil, D., Rygl, K. L. J., Schisano, E., Spinoglio, L., Sousbie, T., Ward-Thompson, D., White, G. J., Hennemann, M., Motte, F., Schneider, N., Didelon, P., Hill, T., Arzoumanian, D., Bontemps, S., Csengeri, T., André, Ph., Konyves, V., Louvet, F., Marston, A., Men’shchikov, A., Minier, V., Nguyen Luong, Q., Palmeirim, P., Peretto, N., Sauvage, M., Zavagno, A., Anderson, L. D., Bernard, J.-Ph., Di Francesco, J., Elia, D., Li, J. Z., Martin, P. G., Molinari, S., Pezzuto, S., Russeil, D., Rygl, K. L. J., Schisano, E., Spinoglio, L., Sousbie, T., Ward-Thompson, D., and White, G. J.

Abstract

In order to characterise the cloud structures responsible for the formation of high-mass stars, we present Herschel observations of the DR21 environment. Maps of the column density and dust temperature unveil the structure of the DR21 ridge and several connected filaments. The ridge has column densities higher than 1023 cm-2 over a region of 2.3 pc2. It shows substructured column density profiles and branches into two major filaments in the north. The masses in the filaments range between 130 and 1400 M⊙, whereas the mass in the ridge is 15000 M⊙. The accretion of these filaments onto the DR21 ridge, suggested by a previous molecular line study, could provide a continuous mass inflow to the ridge. In contrast to the striations seen in, e.g., the Taurus region, these filaments are gravitationally unstable and form cores and protostars. These cores formed in the filaments potentially fall into the ridge. Both inflow and collisions of cores could be important to drive the observed high-mass star formation. The evolutionary gradient of star formation running from DR21 in the south to the northern branching is traced by decreasing dust temperature. This evolution and the ridge structure can be explained by two main filamentary components of the ridge that merged first in the south.

257. Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way

Author

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

Abstract

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

258. Filaments in the Lupus molecular clouds

Author

Benedettini, M., Schisano, E., Pezzuto, S., Elia, D., André, P., Könyves, V., Schneider, N., Tremblin, P., Arzoumanian, D., di Giorgio, A. M., Di Francesco, J., Hill, T., Molinari, S., Motte, F., Nguyen-Luong, Q., Palmeirim, P., Rivera-Ingraham, A., Roy, A., Rygl, K. L. J., Spinoglio, L., Ward-Thompson, D., White, G. J., Benedettini, M., Schisano, E., Pezzuto, S., Elia, D., André, P., Könyves, V., Schneider, N., Tremblin, P., Arzoumanian, D., di Giorgio, A. M., Di Francesco, J., Hill, T., Molinari, S., Motte, F., Nguyen-Luong, Q., Palmeirim, P., Rivera-Ingraham, A., Roy, A., Rygl, K. L. J., Spinoglio, L., Ward-Thompson, D., and White, G. J.

Abstract

We have studied the filaments extracted from the column density maps of the nearby Lupus 1, 3, and 4 molecular clouds, derived from photometric maps observed with the Herschel satellite. Filaments in the Lupus clouds have quite low column densities, with a median value of ∼1.5 × 1021 cm-2 and most have masses per unit length lower than the maximum critical value for radial gravitational collapse. Indeed, no evidence of filament contraction has been seen in the gas kinematics. We find that some filaments, that on average are thermally subcritical, contain dense cores that may eventually form stars. This is an indication that in the low column density regime, the critical condition for the formation of stars may be reached only locally and this condition is not a global property of the filament. Finally, in Lupus we find multiple observational evidences of the key role that the magnetic field plays in forming filaments, and determining their confinement and dynamical evolution.

259. A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey

Author

Könyves, V., André, Ph., Men’shchikov, A., Palmeirim, P., Arzoumanian, D., Schneider, N., Roy, A., Didelon, P., Maury, A., Shimajiri, Y., Di Francesco, J., Bontemps, S., Peretto, N., Benedettini, M., Bernard, J.-Ph., Elia, D., Griffin, M. J., Hill, T., Kirk, J., Ladjelate, B., Marsh, K., Martin, P. G., Motte, F., Nguyên Luong, Q., Pezzuto, S., Roussel, H., Rygl, K. L. J., Sadavoy, S. I., Schisano, E., Spinoglio, L., Ward-Thompson, D., White, G. J., Könyves, V., André, Ph., Men’shchikov, A., Palmeirim, P., Arzoumanian, D., Schneider, N., Roy, A., Didelon, P., Maury, A., Shimajiri, Y., Di Francesco, J., Bontemps, S., Peretto, N., Benedettini, M., Bernard, J.-Ph., Elia, D., Griffin, M. J., Hill, T., Kirk, J., Ladjelate, B., Marsh, K., Martin, P. G., Motte, F., Nguyên Luong, Q., Pezzuto, S., Roussel, H., Rygl, K. L. J., Sadavoy, S. I., Schisano, E., Spinoglio, L., Ward-Thompson, D., and White, G. J.

Abstract

We present and discuss the results of the $Herschel$ Gould Belt survey (HGBS) observations in an ~11 $deg^2$ area of the Aquila molecular cloud complex at $d$ ~ 260 pc, imaged with the SPIRE and PACS photometric cameras in parallel mode from $70\mu m$ to $500\mu m$. Using the multi-scale, multi-wavelength source extraction algorithm $getsources$, we identify a complete sample of starless dense cores and embedded (Class 0-I) protostars in this region, and analyze their global properties and spatial distributions. We find a total of 651 starless cores, ~60% ± 10% of which are gravitationally bound prestellar cores, and they will likely form stars in the future. We also detect 58 protostellar cores. The core mass function (CMF) derived for the large population of prestellar cores is very similar in shape to the stellar initial mass function (IMF), confirming earlier findings on a much stronger statistical basis and supporting the view that there is a close physical link between the stellar IMF and the prestellar CMF. The global shift in mass scale observed between the CMF and the IMF is consistent with a typical star formation efficiency of ~40% at the level of an individual core. By comparing the numbers of starless cores in various density bins to the number of young stellar objects (YSOs), we estimate that the lifetime of prestellar cores is ~1 Myr, which is typically ~4 times longer than the core free-fall time, and that it decreases with average core density. We find a strong correlation between the spatial distribution of prestellar cores and the densest filaments observed in the Aquila complex. About 90% of the $Herschel$-identified prestellar cores are located above a background column density corresponding to $A_V$ ~ 7, and ~75% of them lie within filamentary structures with supercritical masses per unit length ≳16 $M_{\odot}/pc$. These findings support a picture wherein the cores making up the peak of the CMF (and probably responsible for the base of the IMF)

260. Filaments in the Lupus molecular clouds

Author

Benedettini, M., Schisano, E., Pezzuto, S., Elia, D., André, P., Könyves, V., Schneider, N., Tremblin, P., Arzoumanian, D., di Giorgio, A. M., Di Francesco, J., Hill, T., Molinari, S., Motte, F., Nguyen-Luong, Q., Palmeirim, P., Rivera-Ingraham, A., Roy, A., Rygl, K. L. J., Spinoglio, L., Ward-Thompson, D., White, G. J., Benedettini, M., Schisano, E., Pezzuto, S., Elia, D., André, P., Könyves, V., Schneider, N., Tremblin, P., Arzoumanian, D., di Giorgio, A. M., Di Francesco, J., Hill, T., Molinari, S., Motte, F., Nguyen-Luong, Q., Palmeirim, P., Rivera-Ingraham, A., Roy, A., Rygl, K. L. J., Spinoglio, L., Ward-Thompson, D., and White, G. J.

Abstract

We have studied the filaments extracted from the column density maps of the nearby Lupus 1, 3, and 4 molecular clouds, derived from photometric maps observed with the Herschel satellite. Filaments in the Lupus clouds have quite low column densities, with a median value of ∼1.5 × 1021 cm-2 and most have masses per unit length lower than the maximum critical value for radial gravitational collapse. Indeed, no evidence of filament contraction has been seen in the gas kinematics. We find that some filaments, that on average are thermally subcritical, contain dense cores that may eventually form stars. This is an indication that in the low column density regime, the critical condition for the formation of stars may be reached only locally and this condition is not a global property of the filament. Finally, in Lupus we find multiple observational evidences of the key role that the magnetic field plays in forming filaments, and determining their confinement and dynamical evolution.

261. A Herschel and BIMA study of the sequential star formation near the W 48A H II region

Author

Rygl, K. L. J., Goedhart, S., Polychroni, D., Wyrowski, F., Motte, F., Elia, D., Nguyen-Luong, Q., Didelon, P., Pestalozzi, M., Benedettini, M., Molinari, S., André, Ph., Fallscheer, C., Gibb, A., di Giorgio, A. M., Hill, T., Könyves, V., Marston, A., Pezzuto, S., Rivera-Ingraham, A., Schisano, E., Schneider, N., Spinoglio, L., Ward-Thompson, D., White, G. J., Rygl, K. L. J., Goedhart, S., Polychroni, D., Wyrowski, F., Motte, F., Elia, D., Nguyen-Luong, Q., Didelon, P., Pestalozzi, M., Benedettini, M., Molinari, S., André, Ph., Fallscheer, C., Gibb, A., di Giorgio, A. M., Hill, T., Könyves, V., Marston, A., Pezzuto, S., Rivera-Ingraham, A., Schisano, E., Schneider, N., Spinoglio, L., Ward-Thompson, D., and White, G. J.

Abstract

We present the results of Herschel HOBYS (Herschel imaging survey of OB Young Stellar objects) photometric mapping combined with Berkeley Illinois Maryland Association (BIMA) observations and additional archival data, and perform an in-depth study of the evolutionary phases of the star-forming clumps in W 48A and their surroundings. Age estimates for the compact sources were derived from bolometric luminosities and envelope masses, which were obtained from the dust continuum emission, and agree within an order of magnitude with age estimates from molecular line and radio data. The clumps in W 48A are linearly aligned by age (east-old to west-young): we find a ultra-compact (UC) H II region, a young stellar object (YSO) with class II methanol maser emission, a YSO with a massive outflow and finally the NH2D prestellar cores from Pillai et al. This remarkable positioning reflects the (star) formation history of the region. We find that it is unlikely that the star formation in the W 48A molecular cloud was triggered by the UC H II region and discuss the Aquila supershell expansion as a major influence on the evolution of W 48A. We conclude that the combination of Herschel continuum data with interferometric molecular line and radio continuum data is important to derive trustworthy age estimates and interpret the origin of large-scale structures through kinematic information.

262. Two mass distributions in the L 1641 molecular clouds: the Herschel connection of dense cores and filaments in Orion A

Author

Polychroni, D., Schisano, E., Elia, D., Roy, A., Molinari, S., Martin, P., André, Ph., Turrini, D., Rygl, K. L. J., Di Francesco, J., Benedettini, M., Busquet, G., di Giorgio, A. M., Pestalozzi, M., Pezzuto, S., Arzoumanian, D., Bontemps, S., Hennemann, M., Hill, T., Könyves, V., Men'shchikov, A., Motte, F., Nguyen-Luong, Q., Peretto, N., Schneider, N., White, Glenn, Polychroni, D., Schisano, E., Elia, D., Roy, A., Molinari, S., Martin, P., André, Ph., Turrini, D., Rygl, K. L. J., Di Francesco, J., Benedettini, M., Busquet, G., di Giorgio, A. M., Pestalozzi, M., Pezzuto, S., Arzoumanian, D., Bontemps, S., Hennemann, M., Hill, T., Könyves, V., Men'shchikov, A., Motte, F., Nguyen-Luong, Q., Peretto, N., Schneider, N., and White, Glenn

Abstract

We present Herschel survey maps of the L 1641 molecular clouds in Orion A. We extracted both the filaments and dense cores in the region. We identified which of the dense sources are proto- or pre-stellar, and studied their association with the identified filaments. We find that although most (71%) of the pre-stellar sources are located on filaments there, is still a significant fraction of sources not associated with such structures. We find that these two populations (on and off the identified filaments) have distinctly different mass distributions. The mass distribution of the sources on the filaments is found to peak at 4 M ⊙ and drives the shape of the core mass function (CMF) at higher masses, which we fit with a power law of the form dN/dlogM∝M -1.4 ± 0.4. The mass distribution of the sources off the filaments, on the other hand, peaks at 0.8 M ⊙ and leads to a flattening of the CMF at masses lower than ~4 M ⊙. We postulate that this difference between the mass distributions is due to the higher proportion of gas that is available in the filaments, rather than in the diffuse cloud. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

263. From Clouds to Young Stellar Objects and back again: the all-in-one view from the Herschel infrared Galactic Plane Survey

Author

Molinari, S., Abergel, A., Rivera-Ingraham, A., Noriega-Crespo, A., Traficante, A., di Giorgio, A., Zavagno, A., Chrysostomou, A., Roy, A., Babar, A., Maiolo, B., Schulz, B., Jiang, B., Sibthorpe, B., Swinyard, B., Battersby, C., Burigana, C., Brunt, C., Davis, C., Joblin, C., Waelkens, C., Meny, C., Codella, C., Popescu, C., Polychroni, D., Eden, D., Ikhenaode, D., Elia, D., Paradis, D., Shepherd, D., Russeil, D., Ward-Thompson, Derek, Stamatellos, Dimitris, Marshall, D. J., Sturm, E., Rosolowsky, E., Schisano, E., Faustini, F., Agostini, F., Massi, F., La Morgia, F., Piacentini, F., Strafella, F., Boulanger, F., Schuller, F., Motte, F., Wyrowski, F., Fuller, G., de Gasperis, G., Joncas, G., Giardino, G., White, G., Umana, G., Lagache, G., Rivest, G., Stringfellow, G., Yorke, H., Ristorcelli, I., Difrancesco, J., Brand, J., Glenn, J., Kirk, J., Rodon, J., Baluteau, J.-P., Bernard, J.-P., Li, J., Neves, J., Mottram, J., Fischera, J., Bally, J., Richer, J., Blommaert, J., Cernicharo, J., Ganga, K., Morgan, L., Testi, L., Anderson, L., Piazzo, L., Campeggio, L., Conversi, L., Olmi, L., Valenziano, L., Montier, L., Spinoglio, L., Beltran, M., Huang, M., Miville-Deschenes, M.-A., Sauvage, M., Veneziani, M., Thompson, M., Cohen, M., Giard, M., Marengo, M., Compiegne, M., Griffin, Matthew Joseph, Pomares, M., Hoare, M., Barlow, M. J., Burton, M., Reid et al., M., Molinari, S., Abergel, A., Rivera-Ingraham, A., Noriega-Crespo, A., Traficante, A., di Giorgio, A., Zavagno, A., Chrysostomou, A., Roy, A., Babar, A., Maiolo, B., Schulz, B., Jiang, B., Sibthorpe, B., Swinyard, B., Battersby, C., Burigana, C., Brunt, C., Davis, C., Joblin, C., Waelkens, C., Meny, C., Codella, C., Popescu, C., Polychroni, D., Eden, D., Ikhenaode, D., Elia, D., Paradis, D., Shepherd, D., Russeil, D., Ward-Thompson, Derek, Stamatellos, Dimitris, Marshall, D. J., Sturm, E., Rosolowsky, E., Schisano, E., Faustini, F., Agostini, F., Massi, F., La Morgia, F., Piacentini, F., Strafella, F., Boulanger, F., Schuller, F., Motte, F., Wyrowski, F., Fuller, G., de Gasperis, G., Joncas, G., Giardino, G., White, G., Umana, G., Lagache, G., Rivest, G., Stringfellow, G., Yorke, H., Ristorcelli, I., Difrancesco, J., Brand, J., Glenn, J., Kirk, J., Rodon, J., Baluteau, J.-P., Bernard, J.-P., Li, J., Neves, J., Mottram, J., Fischera, J., Bally, J., Richer, J., Blommaert, J., Cernicharo, J., Ganga, K., Morgan, L., Testi, L., Anderson, L., Piazzo, L., Campeggio, L., Conversi, L., Olmi, L., Valenziano, L., Montier, L., Spinoglio, L., Beltran, M., Huang, M., Miville-Deschenes, M.-A., Sauvage, M., Veneziani, M., Thompson, M., Cohen, M., Giard, M., Marengo, M., Compiegne, M., Griffin, Matthew Joseph, Pomares, M., Hoare, M., Barlow, M. J., Burton, M., and Reid et al., M.

Abstract

From diffuse interstellar cirrus to dense atomic and molecular clouds, from protostellar to post-AGB envelopes, from super-shells to supernovae remnants, the Herschel Hi-GAL survey offer an unprecedented snapshot of all the different phases of the Galactic ISM, its evolution and interactions. I will present early results on a variety of topics including the lifetime of massive pre-stellar phases, the fragmentation and collapse of extended structures, the timeline for massive star formation, dust properties in cirrus and molecular clouds.

264. A Herschelstudy of YSO evolutionary stages and formation timelines in two fields of the Hi-GAL survey*

Author

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

Abstract

We present a first study of the star-forming compact dust condensations revealed by Herschelin the two 2° × 2° Galactic Plane fields centered at [$\ell$, b] = [30°, 0°] and [$\ell$, b] =[59°, 0°] , respectively, and observed during the science demonstration phase for the HerschelInfrared GALactic plane survey (Hi-GAL) key-project. Compact source catalogs extracted for the two fields in the five Hi-GAL bands (70, 160, 250, 350 and 500 μm) were merged based on simple criteria of positional association and spectral energy distribution (SED) consistency into a final catalog which contains only coherent SEDs with counterparts in at least three adjacent Herschelbands. These final source lists contain 528 entries for the $\ell$= 30° field, and 444 entries for the $\ell$= 59° field. The SED coverage has been augmented with ancillary data at 24 μm and 1.1 mm. SED modeling for the subset of 318 and 101 sources (in the two fields, respectively) for which the distance is known was carried out using both a structured star/disk/envelope radiative transfer model and a simple isothermal grey-body. Global parameters like mass, luminosity, temperature and dust properties have been estimated. The Lbol/Menvratio spans four orders of magnitudes from values compatible with the pre-protostellar phase to embedded massive zero-age main sequence stars. Sources in the $\ell$= 59° field have on average lower L/M, possibly outlining an overall earlier evolutionary stage with respect to the sources in the $\ell$= 30° field. Many of these cores are actively forming high-mass stars, although the estimated core surface densities appear to be an order of magnitude below the 1 g cm-2critical threshold for high-mass star formation.

Published
2010

265. VIALACTEA science gateway for Milky Way analysis

Author

Stefano Cavuoti, Sergio Molinari, Massimo Brescia, Davide Elia, S. J. Liu, Zoltan Farkas, István Márton, Fabio Vitello, Ugo Becciani, Giuseppe Riccio, Péter Kacsuk, Eva Sciacca, Eugenio Schisano, Alessandro Costa, Anna Maria Di Giorgio, Ákos Hajnal, Sciacca, E., Vitello, F., Becciani, U., Costa, A., Hajnal, A., Kacsuk, P., Farkas, Z., Marton, I., Molinari, S., Di Giorgio, A. M., Schisano, E., Liu, S. J., Elia, D., Cavuoti, S., Riccio, G., and Brescia, M.

Subjects
Computer Networks and Communications, Process (engineering), Star formation, Computer science, Embarrassingly parallel, Context (language use), 02 engineering and technology, Gateway (computer program), Galactic plane, 01 natural sciences, Data science, Galaxy, Workflow, Resource (project management), Workflow systems, Science gateways, Collaborative environments, Astrophysics, DCIs, Milky way analysis, Infrastructure tests, Monitoring, Hardware and Architecture, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, 020201 artificial intelligence & image processing, 010303 astronomy & astrophysics, Software, Workflow management system
Abstract

This paper presents the latest developments on the VIALACTEA Science Gateway in the context of the FP7 VIALACTEA project. The science gateway operates as a central workbench for the VIALACTEA community in order to allow astronomers to process the new-generation surveys (from Infrared to Radio) of the Galactic Plane to build and deliver a quantitative 3D model of our Milky Way Galaxy. The final model will be used as a template for external galaxies to study star formation across the cosmic time. The adopted agile software development process allowed to fulfill the community needs in terms of required workflows and underlying resource monitoring. Scientific requirements arose during the process highlighted the needs for easy parameter setting, fully embarrassingly parallel computations and large-scale input dataset processing. Therefore the science gateway based on the WS-PGRADE/gUSE framework has been able to fulfill the requirements mainly exploiting the parameter sweep paradigm and parallel job execution of the workflow management system. Moving from development to production environment an efficient resource monitoring system has been implemented to easily analyze and debug sources of potential failures occurred during workflow computations. The results of the resource monitoring system are exploitable not only for IT experts, administrators and workflow developers but also for the end-users of the gateway. The affiliation to the STARnet Gateway Federation ensures the sustainability of the presented products after the end of the project, allowing the usage of the VIALACTEA Science Gateway to all the stakeholders, not only to the community members. © 2017 Elsevier B.V.

Published
2019
Full Text
View/download PDF

268. The Hi-GAL catalogue of dusty filamentary structures in the Galactic Plane

Author

Stefano Pezzuto, Alberto Noriega-Crespo, Manuel Merello, David Eden, Giuseppe Riccio, Luca Olmi, Fabio Vitello, Nicolas Peretto, Sergio Molinari, Eva Sciacca, Eugenio Schisano, G. Li Causi, P. Palmeirim, Annie Zavagno, M. T. Beltrán, A. M. di Giorgio, M. Benedettini, Anthony Peter Whitworth, Toby J. T. Moore, Massimo Brescia, Davide Elia, Marco Molinaro, Leonardo Testi, Ugo Becciani, L. Cambresy, G. Umana, A. Baldeschi, S. J. Liu, Alessio Traficante, Stefano Cavuoti, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Capodimonte (OAC), University of Naples Federico II, Liverpool John Moores University (LJMU), Space Telescope Science Institute (STSci), INAF - Osservatorio Astrofisico di Catania (OACT), School of Physics and Astronomy [Cardiff], Cardiff University, Departamento de Astronomia (DAS), 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), INAF - Osservatorio Astronomico di Trieste (OAT), Instituto de Astrofísica e Ciências do Espaço (IASTRO), European Southern Observatory (ESO), Schisano, E., Molinari, S., Elia, D., Benedettini, M., Olmi, L., Pezzuto, S., Traficante, A., Brescia, M., Cavuoti, S., di Giorgio, A. M., Liu, S. J., Moore, T. J. T., Noriega-Crespo, A., Riccio, G., Baldeschi, A., Becciani, U., Peretto, N., Merello, M., Vitello, F., Zavagno, A., Beltran, M. T., Cambresy, L., Eden, D. J., Li Causi, G., Molinaro, M., Palmeirim, P., Sciacca, E., Testi, L., Umana, G., Whitworth, A. P., and University of Naples Federico II = Università degli studi di Napoli Federico II

Subjects
Milky Way, Stars: formation, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Protein filament, ISM: cloud, 0103 physical sciences, Submillimeter: ISM, 010303 astronomy & astrophysics, Galaxy: structure, Solar and Stellar Astrophysics (astro-ph.SR), ISM, Astrophysics::Galaxy Astrophysics, QC, ISM: general, QB, Physics, Infrared: ISM, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Molecular cloud, SM: clouds, Astronomy and Astrophysics, Dust, Extinction, Galactic plane, Galaxy: local interstellar matter, Astrophysics - Astrophysics of Galaxies, Galaxy, ISM: dust, Galaxy:structure, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

The recent data collected by {\it Herschel} have confirmed that interstellar structures with filamentary shape are ubiquitously present in the Milky Way. Filaments are thought to be formed by several physical mechanisms acting from the large Galactic scales down to the sub-pc fractions of molecular clouds, and they might represent a possible link between star formation and the large-scale structure of the Galaxy. In order to study this potential link, a statistically significant sample of filaments spread throughout the Galaxy is required. In this work we present the first catalogue of $32,059$ candidate filaments automatically identified in the Hi-GAL survey of the entire Galactic Plane. For these objects we determined morphological (length, $l^{a}$, and geometrical shape) and physical (average column density, $N_{\rm H_{2}}$, and average temperature, $T$) properties. We identified filaments with a wide range of properties: 2$'$\,$\leq l^{a}\leq$\, 100$'$, $10^{20} \leq N_{\rm H_{2}} \leq 10^{23}$\,cm$^{-2}$ and $10 \leq T\leq$ 35\,K. We discuss their association with the Hi-GAL compact sources, finding that the most tenuous (and stable) structures do not host any major condensation and we also assign a distance to $\sim 18,400$ filaments for which we determine mass, physical size, stability conditions and Galactic distribution. When compared to the spiral arms structure, we find no significant difference between the physical properties of on-arm and inter-arm filaments. We compared our sample with previous studies, finding that our Hi-GAL filament catalogue represents a significant extension in terms of Galactic coverage and sensitivity. This catalogue represents an unique and important tool for future studies devoted to understanding the filament life-cycle., 38 pages, 29 figures, 3 appendices

Published
2020
Full Text
View/download PDF

269. Dense cores and star formation in the giant molecular cloud Vela C

Author

Frederic Schuller, Fabrizio Massi, Davide Elia, T. Hill, Frédérique Motte, Achim Weiss, Timea Csengeri, E. Schisano, Friedrich Wyrowski, M. De Luca, Luca Olmi, Francesco Strafella, Dario Lorenzetti, Teresa Giannini, Karl M. Menten, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Max Planck Institute for Radio Astronomy, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institute of Hydrology, INAF - Osservatorio Astronomico di Roma (OAR), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), 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), Sciences pour l'environnement (SPE), Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Max-Planck-Institut für Radioastronomie (MPIFR), ITA, FRA, DEU, FORMATION STELLAIRE 2020, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Massi, F., Weiss, A., Elia, D., Csengeri, T., Schisano, E., Giannini, T., Hill, T., Lorenzetti, D., Menten, K., Olmi, L., Schuller, F., Strafella, F., De Luca, M., Motte, F., Wyrowski, F., Università degli Studi di Roma 'La Sapienza' [Rome], Osservatorio di Astrofisica di Roma (OAR), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), and École normale supérieure - Paris (ENS-PSL)

Subjects
Initial mass function, FOS: Physical sciences, Context (language use), Astrophysics, Vela, 01 natural sciences, 0103 physical sciences, protostar [Stars], individual objects: Vela Molecular Ridge [ISM], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), formation [Stars], ComputingMilieux_MISCELLANEOUS, O-type star, Physics, [PHYS]Physics [physics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Molecular cloud, ISM [Submillimeter], Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), structure [ISM], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Context The Vela Molecular Ridge is one of the nearest (700 pc) giant molecular cloud (GMC) complexes hosting intermediate-mass (up to early B, late O stars) star formation, and is located in the outer Galaxy, inside the Galactic plane. Vela C is one of the GMCs making up the Vela Molecular Ridge, and exhibits both sub-regions of robust and sub-regions of more quiescent star formation activity, with both low- and intermediate(high)-mass star formation in progress. Aims We aim to study the individual and global properties of dense dust cores in Vela C, and aim to search for spatial variations in these properties which could be related to different environmental properties and/or evolutionary stages in the various sub-regions of Vela C. Methods We mapped the submillimetre (345 GHz) emission from vela C with LABOCA (beam size 19.2", spatial resolution ~0.07 pc at 700 pc) at the APEX telescope. We used the clump-finding algorithm CuTEx to identify the compact submillimetre sources. We also used SIMBA (250 GHz) observations, and Herschel and WISE ancillary data. The association with WISE red sources allowed the protostellar and starless cores to be separated, whereas the Herschel dataset allowed the dust temperature to be derived for a fraction of cores. The protostellar and starless core mass functions (CMFs) were constructed following two different approaches, achieving a mass completeness limit of 3.7 Msun. Results We retrieved 549 submillimetre cores, 316 of which are starless and mostly gravitationally bound (therefore prestellar in nature). Both the protostellar and the starless CMFs are consistent with the shape of a Salpeter initial mass function in the high-mass part of the distribution. Clustering of cores at scales of 1--6 pc is also found, hinting at fractionation of magnetised, turbulent gas., Comment: 21 pages, 19 figures, to be published in Astronomy & Astrophysics

Published
2019
Full Text
View/download PDF

270. Vialactea Visual Analytics Tool for Star Formation Studies of the Galactic Plane

Author

Stefano Cavuoti, Marco Molinaro, Robert Butora, Fabio Vitello, Ugo Becciani, Riccardo Smareglia, A. Di Giorgio, Marilena Bandieramonte, E. Schisano, Massimo Brescia, S. J. Liu, Davide Elia, Eva Sciacca, Milena Benedettini, Sergio Molinari, Alessandro Costa, Giuseppe Riccio, ITA, Vitello, F., Sciacca, E., Becciani, U., Costa, A., Bandieramonte, M., Benedettini, M., Brescia, M., Butora, R., Cavuoti, S., Di Giorgio, A. M., Elia, D., Liu, S. J., Molinari, S., Molinaro, M., Riccio, G., Schisano, E., and Smareglia, R.

Subjects
Visual analytics, Exploit, Computer science, Milky Way, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 02 engineering and technology, 01 natural sciences, Space exploration, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, media_common.cataloged_instance, European union, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Star formation, Suite, Astronomy and Astrophysics, Galactic plane, Data science, Galaxy: structure, methods: data analysis, stars: formation, surveys, techniques: image processing, Online material: color figures, Space and Planetary Science, 020201 artificial intelligence & image processing, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 607380 (VIALACTEA) and from the European Commissions Horizon 2020 research and innovation programme under the grant agreement No. 739563 (EOSCPilot.eu) We present a visual analytics tool, based on the VisIVO suite, to exploit a combination of all new-generation surveys of the Galactic Plane to study the star formation process of the Milky Way. The tool has been developed within the VIALACTEA project, founded by the 7th Framework Programme of the European Union, that creates a common forum for the major new-generation surveys of the Milky Way Galactic Plane from the near-infrared to the radio, both in thermal continuum and molecular lines. Massive volumes of data are produced by space missions and ground-based facilities and the ability to collect and store them is increasing at a higher pace than the ability to analyze them. This gap leads to new challenges in the analysis pipeline to discover information contained in the data. Visual analytics focuses on handling these massive, heterogeneous, and dynamic volumes of information accessing the data previously processed by data mining algorithms and advanced analysis techniques with highly interactive visual interfaces offering scientists the opportunity for in-depth understanding of massive, noisy, and high-dimensional data.

Published
2018

271. The Hi-GAL compact source catalogue – I. The physical properties of the clumps in the inner Galaxy (−71$_.^circ$0 < ℓ < 67$_.^circ$0)

Author

Takahiro Hayakawa, David Eden, Melvin Hoare, Francesco Strafella, F. Piacentini, Kenneth A. Marsh, Sergio Molinari, S. E. Jaffa, Pedro García-Lario, Alessio Traficante, Peter Schilke, Kengo Tachihara, G. Joncas, J.-P. Bernard, M. R. Pestalozzi, S. Martinavarro-Armengol, Amata Mercurio, Alessandro Costa, Friedrich Wyrowski, Eva Sciacca, Robert Butora, B. Maiolo, Joseph C. Mottram, Mark Thompson, D. Polychroni, H. Yamamoto, G. Li Causi, P. Palmeirim, M. Benedettini, D. Russeil, Hidetoshi Sano, Kazi L.J. Rygl, Eugenio Schisano, Stefano Cavuoti, Annie Zavagno, Sarah Ragan, John Bally, M. Veneziani, Carla Buemi, A. P. Whitworth, K. Torii, Massimo Brescia, Péter Kacsuk, Davide Elia, Marco Molinaro, Nicola Schneider, Ugo Becciani, Rene Plume, Göran Pilbratt, A. M. di Giorgio, F. Faustini, P. Mège, Luca Calzoletti, Grazia Umana, Stefano Pezzuto, H. Arab, E. Fiorellino, Derek Ward-Thompson, S. J. Liu, Marilena Bandieramonte, M. T. Beltrán, Paolo Leto, Y. Maruccia, Roberta Paladini, Toby J. T. Moore, Giuseppe Riccio, Fabio Vitello, Luca Olmi, N. Marchili, Frédérique Motte, Corrado Trigilio, Ákos Hajnal, Yasuo Fukui, Nicolas Peretto, Alberto Noriega-Crespo, A. Baldeschi, Riccardo Cesaroni, Leonardo Testi, Lorenzo Piazzo, Manuel Merello, L. Cambrésy, Filomena Bufano, Peter G. Martin, Nicolas Billot, Meng-Lin Huang, Paolo Natoli, Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, Marilena, 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., Palmeirim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltrán, M. T., Billot, N., Cambrésy, L., Cesaroni, R., García-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mège, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Li Causi, G., Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., Yamamoto, H., Elia, Davide, Pezzuto, S., Noriega Crespo, A., Strafella, Francesco, García Lario, P., Maiolo, BERLINDA MARIA TERESA, Maruccia, Ylenia, Ward Thompson, D., and Martinavarro Armengol, S.

Subjects
Astrophysics and Astronomy, Infrared, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, cataloghi astronomici, mezzo interstellare, osservazioni infrarosse, osservazioni submillimetriche, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB, Physics, Spiral galaxy, 010308 nuclear & particles physics, Star formation, Spectral density, Astronomy, Astronomy and Astrophysics, Galactic plane, Galaxy, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, catalogues, ISM clouds, dust, extinction, local interstellar matter, infrared ISM, submillimetre ISM, Longitude
Abstract

Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 μm. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane −71 ∘. 0 < ℓ < 67 ∘. 0. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-μm counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between ‘on-arm’ and ‘interarm’ positions. Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $\mu$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the portion of Galactic plane $-71.0^{\circ}< \ell < 67.0^{\circ}$. The band-merged catalogue contains 100922 sources with a regular SED, 24584 of which show a 70 $\mu$m counterpart and are thus considered proto-stellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterise different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in proto-stellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to proto-stellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between "on-arm" and "inter-arm" positions.

Published
2017

272. An analysis of star formation with Herschel in the Hi-GAL Survey. II. The tips of the Galactic bar

Author

Norikazu Mizuno, B. Maiolo, Sergio Molinari, D. Russeil, F. Piacentini, A. Di Giorgio, Stefano Pezzuto, Y. Maruccia, Francesco Strafella, Davide Elia, Joseph C. Mottram, M. R. Pestalozzi, R. Plume, E. Schisano, Alberto Noriega-Crespo, Toshikazu Onishi, Sean Carey, Yasuo Fukui, Akira Mizuno, Deborah Paradis, Toby J. T. Moore, Roberta Paladini, M. Veneziani, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Veneziani, M., Schisano, E., Elia, D., Noriega Crespo, A., Carey, S., Di Giorgio, A., Fukui, Y., Maiolo, B. M. T., Maruccia, Ylenia, Mizuno, A., Mizuno, N., Molinari, S., Mottram, J. C., Moore, T. J. T., Onishi, T., Paladini, R., Paradis, D., Pestalozzi, M., Pezzuto, S., Piacentini, F., Plume, R., Russeil, D., and Strafella, Francesco

Subjects
Infrared, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, stars formation, Galaxy stellar content, infrared ISM, surveys, Galaxy: stellar content, Infrared: ISM, Stars: formation, Surveys, Astronomy and Astrophysics, Space and Planetary Science, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, infrared: ISM, Spiral galaxy, stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Galactic Center, Galactic plane, Astrophysics - Astrophysics of Galaxies, Stars, Star cluster, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Longitude
Abstract

We present the physical and evolutionary properties of prestellar and protostellar clumps in the Herschel Infrared GALactic plane survey (Hi-GAL) in two large areas centered in the Galactic plane and covering the tips of the long Galactic bar at the intersection with the spiral arms. The areas fall in the longitude ranges 19 < l < 33 and 340 < l < 350, while latitude is -1 < b < 1. Newly formed high mass stars and prestellar objects are identified and their properties derived and compared. A study is also presented on five giant molecular complexes at the further edge of the bar. The star-formation rate was estimated from the quantity of proto-stars expected to form during the collapse of massive turbulent clumps into star clusters. This new method was developed by applying a Monte Carlo procedure to an evolutionary model of turbulent cores and takes into account the wide multiplicity of sources produced during the collapse. The star-formation rate density values at the tips are 1.2 +- 0.3 10-3 Msol/yr/kpc2 and 1.5+-0.3 10-3 Msol/yr/kpc2 in the first and fourth quadrant, respectively. The same values estimated on the entire field of view, that is including the tips of the bar and background and foreground regions, are 0.9+-0.2 10-3 Msol/yr/kpc2 and 0.8+-0.2 10-3 Msol/yr/kpc2. The conversion efficiency is approximately 0.8% in the first quadrant and 0.5% in the fourth quadrant, and does not show a significant difference in proximity of the bar. The star forming regions identified through CO contours at the further edge of the bar show star-formation rate densities larger than the surrounding regions but their conversion efficiencies are comparable. Our results suggest that the star-formation activity at the bar is due to a large amount of dust and molecular material rather than being due to a triggering process., 16 pages, 17 figures, accepted for publication in A&A

Published
2017
Full Text
View/download PDF

273. Milky Way analysis through a Science Gateway: Workflows and Resource Monitoring

Author

Fabio Vitello, Giuseppe Riccio, Stefano Cavuoti, Eva Sciacca, Eugenio Schisano, Ugo Becciani, Péter Kacsuk, Davide Elia, Massimo Brescia, Sergio Molinari, S. J. Liu, Alessandro Costa, Anna Maria Di Giorgio, Ákos Hajnal, Sandra Gesing, Jens Krüger, Sciacca, E., Vitello, F., Becciani, U., Costa, A., Hajnal, A., Kacsuk, P., Molinari, S., di Giorgio, A. M., Schisano, E., Liu, S. J., Elia, D., Cavuoti, S., Riccio, G., and Brescia, M.

Subjects
Engineering, 010504 meteorology & atmospheric sciences, business.industry, QA75 Electronic computers. Computer science / számítástechnika, számítógéptudomány, 010103 numerical & computational mathematics, 02 engineering and technology, Science gateway, 01 natural sciences, Data science, Workflow Systems, Science Gateways, Collaborative Environments, Astrophysics, DCIs, Milky Way Analysis, Infrastructure Tests, Monitoring, World Wide Web, Workflow, Resource (project management), 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, 020201 artificial intelligence & image processing, 0101 mathematics, business, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

This paper presents the latest developments on the VIALACTEA Science Gateway in the context of the FP7 VIALACTEA project. This science gateway operates as a central workbench for the VIALACTEA community in order to allow astronomers to process the new-generation (from Infrared to Radio) surveys of the Galactic Plane to build and deliver a quantitative 3D model of our Milky Way Galaxy. The final model will be used as a template for external galaxies to study star formation across the cosmic time. The adopted AGILE software development process allowed to fulfill the community needs in terms of required workflows and underlying resources monitoring. The scientific requirements arose during the process highlighted the needs for easy parameter setting, fully embarrassingly parallel computations and large-scale input dataset processing. Therefore the science gateway based on the WS-PGRADE/gUSE framework has been able to fulfill the requirements mainly exploiting the parameter sweep paradigm and parallel jobs execution of the workflow management system. Moving from the development to the production environment an efficient resource monitoring system has been implemented to easily analyse and debug sources of failure due to workflows computations. The results of the resource monitoring system are exploitable not only for IT experts administrators and workflow developers but also for the final users of the gateway. The affiliation to the STARnet Gateway Federation ensures the sustainability of the presented products after the end of the project, allowing the usage of VIALACTEA Science Gateway to all the stakeholders and not only to the community members.

Published
2016

274. VIALACTEA knowledge base homogenizing access to Milky Way data

Author

Marilena Bandieramonte, Alessandro Costa, Marco Molinaro, Ugo Becciani, Massimo Brescia, Stefano Cavuoti, S. J. Liu, Davide Elia, Anna Maria Di Giorgio, Fabio Vitello, Ákos Hajnal, Sergio Molinari, Eugenio Schisano, Giuseppe Riccio, Hermann Gabor, Riccardo Smareglia, Péter Kacsuk, Robert Butora, Eva Sciacca, ITA, HUN, Gianluca Chiozzi, Juan C. Guzman, Molinaro, M., Butora, R., Bandieramonte, M., Becciani, U., Brescia, M., Cavuoti, S., Costa, A., Di Giorgio, A. M., Elia, D., Hajnal, A., Gabor, H., Kacsuk, P., Liu, S. J., Molinari, S., Riccio, G., Schisano, E., Sciacca, E., Smareglia, R., and Vitello, F.

Subjects
business.industry, Computer science, Relational database, Data discovery, FOS: Physical sciences, 020206 networking & telecommunications, 02 engineering and technology, Virtual observatory, computer.software_genre, 01 natural sciences, Task (project management), Metadata, World Wide Web, Knowledge base, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Data access, Databases, Milky way, VO, Web service, Astrophysics - Instrumentation and Methods for Astrophysics, business, 010303 astronomy & astrophysics, computer, Instrumentation and Methods for Astrophysics (astro-ph.IM), Data integration
Abstract

The VIALACTEA project has a work package dedicated to Tools and Infrastructure and, inside it, a task for the Database and Virtual Observatory Infrastructure. This task aims at providing an infrastructure to store all the resources needed by the, more purposely, scientific work packages of the project itself. This infrastructure includes a combination of: storage facilities, relational databases and web services on top of them, and has taken, as a whole, the name of VIALACTEA Knowledge Base (VLKB). This contribution illustrates the current status of this VLKB. It details the set of data resources put together; describes the database that allows data discovery through VO inspired metadata maintenance; illustrates the discovery, cutout and access services built on top of the former two for the users to exploit the data content., Comment: 11 pages, 1 figure, SPIE Astronomical Telescopes + Instrumentation 2016, Software and Cyberifrastructure for Astronomy IV, Conference Proceedings

Published
2016

275. Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way

Author

J. A. Rodón, K. Ganga, M. Pomarès, Friedrich Wyrowski, Mika Juvela, F. Piacentini, Melvin Hoare, William T. Reach, Stefano Pezzuto, A. Roy, Jean-Paul Baluteau, Marc-Antoine Miville-Deschenes, Russell H. Taylor, Pierre Royer, Alessio Traficante, Peter Schilke, D. Paradis, Glenn J. White, Cara Battersby, Alberto Noriega-Crespo, Harriet Parsons, M. Veneziani, Dimitrios Stamatellos, Vincent Minier, Lorenzo Piazzo, Guy S. Stringfellow, Michael G. Burton, L. K. Morgan, Frederic Schuller, F. Faustini, P. Saraceno, S. D. Lord, Jason Glenn, E. Sturm, Michael D. Smith, G. Joncas, A. M. di Giorgio, D. Polychroni, L. Montier, D. J. Marshall, N. Billot, José Cernicharo, F. Boulanger, M. T. Beltrán, Paul Martin, Matthew Joseph Griffin, B. Swinyard, Guilaine Lagache, Serena Viti, Mathieu Compiegne, Derek Ward-Thompson, P. de Bernardis, Frédérique Motte, B. Sibthorpe, Sukanya Chakrabarti, Nicolas Flagey, Christopher M. Brunt, Maggie A. Thompson, Qizhou Zhang, J.-P. Bernard, Annie Zavagno, Jean-François Robitaille, L. Spinoglio, Marc Sauvage, D. Russeil, Paolo Natoli, A. Abergel, Babar Ali, Davide Elia, D. Ikhenaode, Gary A. Fuller, C. Joblin, G. de Gasperis, Eugenio Schisano, Pedro García-Lario, Jin-Zeng Li, Isabelle Ristorcelli, Sergio Molinari, Luca Calzoletti, M. R. Pestalozzi, Nicolas Peretto, Thomas P. Robitaille, Mikako Matsuura, Riccardo Cesaroni, Rene Plume, Jan Brand, Paul F. Goldsmith, Leonardo Testi, Joseph C. Mottram, H. W. Yorke, Cristina Popescu, Martin Cohen, M. Benedettini, M. J. Barlow, Antonio Chrysostomou, Paola Caselli, Luca Olmi, Maohai Huang, Massimo Marengo, R. Paladini, Fabrizio Massi, L. A. Wilcock, Grazia Umana, Francesco Strafella, Toby J. T. Moore, Benjamin L. Schulz, R. Vavrek, T. Mueller, John Bally, J. A. D. L. Blommaert, L. D. Anderson, C. Waelkens, T. L. Lim, Richard J. Tuffs, Sean Carey, Yasuo Fukui, J. Neves, Nicola Schneider, Jason M. Kirk, Silvia Masi, Pascal André, Howard A. Smith, Luca Valenziano, Sylvain Bontemps, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), CITA, University of Toronto, European Southern Observatory (ESO), 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), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratory of Comparative Carcinogenesis (LABORATORY OF COMPARATIVE CARCINOGENESIS), National Cancer Institute [Bethesda] (NCI-NIH), National Institutes of Health [Bethesda] (NIH)-National Institutes of Health [Bethesda] (NIH), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-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), FORMATION STELLAIRE 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), 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), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ISO Data Centre (ESA - Espagne), Agence Spatiale Européenne = European Space Agency (ESA), Herschel Science Centre (ESA Espagne), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Universiti Brunei Darussalam, Biology Department, Universitii Brunei Darussalam, Università degli Studi di Roma Tor Vergata [Roma], University of Manchester [Manchester], 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), Tenovus Centre for Cancer Research, Welsh School of Pharmacy, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Inter University Accelerator Centre, Aruna Asaf Ali Marg, LEOSPHERE France, LEOSPHERE, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Atmospheric Sciences Division [Hampton], NASA Langley Research Center [Hampton] (LaRC), School of Physics and Astronomy [Cardiff], Cardiff University, Shanghai Inst Opt & Fine Mech, Key Lab Mat Sci & Technol High Power Lasers, Molinari, S., Swinyard, B., Bally, J., Barlow, M., Bernard, J. P., Martin, P., Moore, T., Noriega Crespo, A., Plume, R., Testi, L., Zavagno, A., Abergel, A., Ali, B., Anderson, L., Andre, P., Baluteau, J. P., Battersby, C., Beltrán, M. T., Benedettini, M., Billot, N., Blommaert, J., Bontemps, S., Boulanger, F., Brand, J., Brunt, C., Burton, M., Calzoletti, L., Carey, S., Caselli, P., Cesaroni, R., Cernicharo, J., Chakrabarti, S., Chrysostomou, A., Cohen, M., Compiegne, M., de Bernardis, P., de Gasperis, G., di Giorgio, A. M., Elia, Davide Quintino, Faustini, F., Flagey, N., Fukui, Y., Fuller, G. A., Ganga, K., Garcia Lario, P., Glenn, J., Goldsmith, P. F., Griffin, M., Hoare, M., Huang, M., Ikhenaode, D., Joblin, C., Joncas, G., Juvela, M., Kirk, J. M., Lagache, G., Li, J. Z., Lim, T. L., Lord, S. D., Marengo, M., Marshall, D. J., Masi, S., Massi, F., Matsuura, M., Minier, V., Miville Deschênes, M. A., Montier, L. A., Morgan, L., Motte, F., Mottram, J. C., Müller, T. G., Natoli, P., Neves, J., Olmi, L., Paladini, R., Paradis, D., Parsons, H., Peretto, N., Pestalozzi, M., Pezzuto, S., Piacentini, F., Piazzo, L., Polychroni, D., Pomarès, M., Popescu, C. C., Reach, W. T., Ristorcelli, I., Robitaille, J. F., Robitaille, T., Rodón, J. A., Roy, A., Royer, P., Russeil, D., Saraceno, P., Sauvage, M., Schilke, P., Schisano, E., Schneider, N., Schuller, F., Schulz, B., Sibthorpe, B., Smith, H. A., Smith, M. D., Spinoglio, L., Stamatellos, D., Strafella, Francesco, Stringfellow, G. S., Sturm, E., Taylor, R., Thompson, M. A., Traficante, A., Tuffs, R. J., Umana, G., Valenziano, L., Vavrek, R., Veneziani, M., Viti, S., Waelkens, C., Ward Thompson, D., White, G., Wilcock, L. A., Wyrowski, F., Yorke, H. W., Zhang, Q., Consiglio Nazionale delle Ricerche (CNR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN), 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), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), European Space Agency (ESA), Dipartimento di Fisica, Universita` di Roma Tor Vergata, 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), Centre National de la Recherche Scientifique (CNRS)-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 normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), ITA, USA, GBR, FRA, DEU, and ESP

Subjects
010504 meteorology & atmospheric sciences, Field (physics), Milky Way, stars: formation, ISM: structure, ISM: clouds, Galaxy: general, FOS: Physical sciences, ism: structure, ism: clouds, galaxy: general, Astrophysics, 01 natural sciences, Protein filament, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Protostar, Infrared dark cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Galactic plane, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Core (optical fiber), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnetohydrodynamics
Abstract

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

Full Text
View/download PDF

276. A Herschel study of YSO evolutionary stages and formation timelines in two fields of the Hi-GAL survey

Author

A. Di Giorgio, Stefano Pezzuto, John Bally, Alessio Traficante, M. R. Pestalozzi, Francesco Strafella, F. Piacentini, Sergio Molinari, L. Calzoletti, Mark Thompson, D. Polychroni, Daniel Anglés-Alcázar, E. Schisano, Thomas P. Robitaille, Davide Elia, Joseph C. Mottram, Milena Benedettini, Roberta Paladini, Guy S. Stringfellow, Paul Martin, Michael D. Smith, Jin-Zeng Li, Leonardo Testi, Luca Olmi, Cara Battersby, M. Veneziani, L. K. Morgan, F. Faustini, Paolo Natoli, Nicolas Billot, Frédérique Motte, Elia, Davide Quintino, Schisano, E., Molinari, S., Robitaille, T., Anglés Alcázar, D., Bally, J., Battersby, C., Benedettini, M., Billot, N., Calzoletti, L., di Giorgio, A. M., Faustini, F., Li, J. Z., Martin, P., Morgan, L., Motte, F., Mottram, J. C., Natoli, P., Olmi, L., Paladini, R., Piacentini, F., Pestalozzi, M., Pezzuto, S., Polychroni, D., Smith, M. D., Strafella, Francesco, Stringfellow, G. S., Testi, L., Thompson, M. A., Traficante, A., and Veneziani, M.

Subjects
Physics, stelle di pre-sequenza principale, Field (physics), Infrared, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, stars: formation / stars: pre-main sequence, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, formazione stellare, Luminosity, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Main sequence, Astrophysics::Galaxy Astrophysics
Abstract

We present a first study of the star-forming compact dust condensations revealed by Herschel in the two 2 \times 2 \degr Galactic Plane fields centered at [l;b] = [30\degr; 0 \degr] and [l;b] = [59\degr; 0 \degr], respectively, and observed during the Science Demonstration Phase for the Herschel infrared Galactic Plane survey (Hi-GAL) Key-Project. Compact source catalogs extracted for the two fields in the five Hi-GAL bands (70, 160, 250, 350 and 500 $\mu$m) were merged based on simple criteria of positional association and spectral energy distribution (SED) consistency into a final catalog which contains only coherent SEDs with counterparts in at least three adjacent Herschel bands. These final source lists contain 528 entries for the l = 30\degr field, and 444 entries for the l = 59\degr field. The SED coverage has been augmented with ancillary data at 24 $\mu$m and 1.1 mm. SED modeling for the subset of 318 and 101 sources (in the two fields, respectively) for which the distance is known was carried out using both a structured star/disk/envelope radiative transfer model and a simple isothermal grey-body. Global parameters like mass, luminosity, temperature and dust properties have been estimated. The Lbol/Menv ratio spans four orders of magnitudes from values compatible with the pre-protostellar phase to embedded massive zero-age main sequence stars. Sources in the l = 59\degr field have on average lower L/M, possibly outlining an overall earlier evolutionary stage with respect to the sources in the l = 30\degr field. Many of these cores are actively forming high-mass stars, although the estimated core surface densities appear to be an order of magnitude below the 1 g cm$^{-2}$ critical threshold for high-mass star formation., Comment: To appear in A&A

277. Atacama Large Aperture Submillimeter Telescope (AtLAST) science: Our Galaxy.

Author

Klaassen P, Traficante A, Beltrán M, Pattle K, Booth M, Lovell J, Marshall J, Hacar A, Gaches B, Bot C, Peretto N, Stanke T, Arzoumanian D, Duarte Cabral A, Duchêne G, Eden D, Hales A, Kauffmann J, Luppe P, Marino S, Redaelli E, Rigby A, Sánchez-Monge Á, Schisano E, Semenov D, Spezzano S, Thompson M, Wyrowski F, Cicone C, Mroczkowski T, Cordiner M, Di Mascolo L, Johnstone D, van Kampen E, Lee M, Liu D, Maccarone T, Saintonge A, Smith M, Thelen A, and Wedemeyer S

Abstract

As we learn more about the multi-scale interstellar medium (ISM) of our Galaxy, we develop a greater understanding for the complex relationships between the large-scale diffuse gas and dust in Giant Molecular Clouds (GMCs), how it moves, how it is affected by the nearby massive stars, and which portions of those GMCs eventually collapse into star forming regions. The complex interactions of those gas, dust and stellar populations form what has come to be known as the ecology of our Galaxy. Because we are deeply embedded in the plane of our Galaxy, it takes up a significant fraction of the sky, with complex dust lanes scattered throughout the optically recognizable bands of the Milky Way. These bands become bright at (sub-)millimetre wavelengths, where we can study dust thermal emission and the chemical and kinematic signatures of the gas. To properly study such large-scale environments, requires deep, large area surveys that are not possible with current facilities. Moreover, where stars form, so too do planetary systems, growing from the dust and gas in circumstellar discs, to planets and planetesimal belts. Understanding the evolution of these belts requires deep imaging capable of studying belts around young stellar objects to Kuiper belt analogues around the nearest stars. Here we present a plan for observing the Galactic Plane and circumstellar environments to quantify the physical structure, the magnetic fields, the dynamics, chemistry, star formation, and planetary system evolution of the galaxy in which we live with AtLAST; a concept for a new, 50m single-dish sub-mm telescope with a large field of view which is the only type of facility that will allow us to observe our Galaxy deeply and widely enough to make a leap forward in our understanding of our local ecology., Competing Interests: No competing interests were disclosed., (Copyright: © 2024 Klaassen P et al.)

Published
2024
Full Text
View/download PDF

278. Exploring the link between star and planet formation with Ariel.

Author

Turrini D, Codella C, Danielski C, Fedele D, Fonte S, Garufi A, Guarcello MG, Helled R, Ikoma M, Kama M, Kimura T, Kruijssen JMD, Maldonado J, Miguel Y, Molinari S, Nikolaou A, Oliva F, Panić O, Pignatari M, Podio L, Rickman H, Schisano E, Shibata S, Vazan A, and Wolkenberg P

Abstract

The goal of the Ariel space mission is to observe a large and diversified population of transiting planets around a range of host star types to collect information on their atmospheric composition. The planetary bulk and atmospheric compositions bear the marks of the way the planets formed: Ariel's observations will therefore provide an unprecedented wealth of data to advance our understanding of planet formation in our Galaxy. A number of environmental and evolutionary factors, however, can affect the final atmospheric composition. Here we provide a concise overview of which factors and effects of the star and planet formation processes can shape the atmospheric compositions that will be observed by Ariel, and highlight how Ariel's characteristics make this mission optimally suited to address this very complex problem., (© The Author(s) 2021.)

Published
2022
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results