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301. Coordinated Optical/X-ray observations of the CTTS V2129 Oph The Chandra View

Author

Flaccomio, E., Costanza ARGIROFFI, Alencar, S. H. P., Bouvier, J., Donati, J. -F, Getman, K., Gregory, S. G., Hussain, G., Ibrahimov, M., Jardine, M. M., Skelly, M., Walter, F., Flaccomio, E, Argiroffi, C, Alencar, SHP, Bouvier, J, Donati, JF, Getman, K, Gregory, SG, Hussain, G, Ibrahimov, M, Jardine, MM, Skelly, M, and Walter, F

Subjects
X-ray, Settore FIS/05 - Astronomia E Astrofisica, accretion, T Tauri
Abstract

Young low-mass accreting stars (classical T Tauri stars; CTTSs) possess strong magnetic fields that are responsible for the regulation of the accretion and outflow processes, and the confinement and heating of coronal plasma. Understanding the physics of CTTS magnetospheres and of their interaction with circumstellar disks can elucidate the history and evolution of our own Sun and Solar System, at the stage when planets were being formed. In June 2009 we have conducted an extensive multi-wavelength observing campaign of V2129 Oph, a K5 CTTS in the ρ Ophiuchi molecular cloud, with the goal of obtaining a synoptic view of its photosphere, magnetic field, coronal plasma, and of its accretion spot(s) and funnel flow(s). We here report on the X-ray emission, as observed by the Chandra High Energy Transmission Grating (HETG). High-density plasma, presumably from the accretion shock, is responsible for the soft X-ray emission, at least during the first half of the observation. The X-ray emission from both the coronal plasma (T˜20MK) and the cooler and denser material from the accretion spot (T˜3MK) is observed to vary between the first and second half of the observation. From the high-resolution X-ray spectra we constrain the emission measure of the two components and the density of the cool plasma. Finally we interpret the time variability of the cool plasma component in terms of stellar rotation and the time-changing viewing angle of the accretion stream, as constrained by simultaneous optical observations.

302. The Gaia-ESO Public Spectroscopic Survey

Author

Gilmore, G., Randich, S., Asplund, M., Binney, J., Bonifacio, P., Drew, J., Feltzing, S., Ferguson, A., Jeffries, R., Micela, G., Negueruela, I., Prusti, T., Rix, H. -W, Vallenari, A., Alfaro, E., Allende-Prieto, C., Babusiaux, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., François, P., Irwin, M., Koposov, S., Korn, A., Lanzafame, A., Pancino, E., Paunzen, E., Recio-Blanco, A., Sacco, G., Smiljanic, R., Eck, S., Walton, N., Aden, D., Aerts, C., Affer, L., Alcala, J. -M, Altavilla, G., Alves, J., Antoja, T., Arenou, F., Costanza ARGIROFFI, Asensio Ramos, A., Bailer-Jones, C., Balaguer-Nunez, L., Bayo, A., Barbuy, B., Barisevicius, G., Barrado Y Navascues, D., Battistini, C., Bellas Velidis, I., Bellazzini, M., Belokurov, V., Bergemann, M., Bertelli, G., Biazzo, K., Bienayme, O., Bland-Hawthorn, J., Boeche, C., Bonito, S., Boudreault, S., Bouvier, J., Brandao, I., Brown, A., Bruijne, J., Burleigh, M., Caballero, J., Caffau, E., Calura, F., Capuzzo-Dolcetta, R., Caramazza, M., Carraro, G., Casagrande, L., Casewell, S., Chapman, S., Chiappini, C., Chorniy, Y., Christlieb, N., Cignoni, M., Cocozza, G., Colless, M., Collet, R., Collins, M., Correnti, M., Covino, E., Crnojevic, D., Cropper, M., Cunha, M., Damiani, F., David, M., Delgado, A., Duffau, S., Edvardsson, B., Eldridge, J., Enke, H., Eriksson, K., Evans, N. W., Eyer, L., Famaey, B., Fellhauer, M., Ferreras, I., Figueras, F., Fiorentino, G., Flynn, C., Folha, D., Franciosini, E., Frasca, A., Freeman, K., Fremat, Y., Friel, E., Gaensicke, B., Gameiro, J., Garzon, F., Geier, S., Geisler, D., Gerhard, O., Gibson, B., Gomboc, A., Gomez, A., Gonzalez-Fernandez, C., Gonzalez Hernandez, J., Gosset, E., Grebel, E., Greimel, R., Groenewegen, M., Grundahl, F., Guarcello, M., Gustafsson, B., Hadrava, P., Hatzidimitriou, D., Hambly, N., Hammersley, P., Hansen, C., Haywood, M., Heber, U., Heiter, U., Held, E., Helmi, A., Hensler, G., Herrero, A., Hill, V., Hodgkin, S., Huelamo, N., Huxor, A., Ibata, R., Jackson, R., Jong, R., Jonker, P., Jordan, S., Jordi, C., Jorissen, A., Katz, D., Kawata, D., Keller, S., Kharchenko, N., Klement, R., Klutsch, A., Knude, J., Koch, A., Kochukhov, O., Kontizas, M., Koubsky, P., Lallement, R., Laverny, P., Leeuwen, F., Lemasle, B., Lewis, G., Lind, K., Lindstrom, H. P. E., Lobel, A., Lopez Santiago, J., Lucas, P., Ludwig, H., Lueftinger, T., Magrini, L., Maiz Apellaniz, J., Maldonado, J., Marconi, G., Marino, A., Martayan, C., Martinez-Valpuesta, I., Matijevic, G., Mcmahon, R., Messina, S., Meyer, M., Miglio, A., Mikolaitis, S., Minchev, I., Minniti, D., Moitinho, A., Momany, Y., Monaco, L., Montalto, M., Monteiro, M. J., Monier, R., Montes, D., Mora, A., Moraux, E., Morel, T., Mowlavi, N., Mucciarelli, A., Munari, U., Napiwotzki, R., Nardetto, N., Naylor, T., Naze, Y., Nelemans, G., Okamoto, S., Ortolani, S., Pace, G., Palla, F., Palous, J., Parker, R., Penarrubia, J., Pillitteri, I., Piotto, G., Posbic, H., Prisinzano, L., Puzeras, E., Quirrenbach, A., Ragaini, S., Read, J., Read, M., Reyle, C., Ridder, J., Robichon, N., Robin, A., Roeser, S., Romano, D., Royer, F., Ruchti, G., Ruzicka, A., Ryan, S., Ryde, N., Santos, N., Sanz Forcada, J., Sarro Baro, L. M., Sbordone, L., Schilbach, E., Schmeja, S., Schnurr, O., Schoenrich, R., Scholz, R. -D, Seabroke, G., Sharma, S., Silva, G., Smith, M., Solano, E., Sordo, R., Soubiran, C., Sousa, S., Spagna, A., Steffen, M., Steinmetz, M., Stelzer, B., Stempels, E., Tabernero, H., Tautvaisiene, G., Thevenin, F., Torra, J., Tosi, M., Tolstoy, E., Turon, C., Walker, M., Wambsganss, J., Worley, C., Venn, K., Vink, J., Wyse, R., Zaggia, S., Zeilinger, W., Zoccali, M., Zorec, J., Zucker, D., Zwitter, T., Gaia-ESO Survey Team, Gilmore, G., Randich, S., Asplund, M., Binney, J., Bonifacio, P., Drew, J., Feltzing, S., Ferguson, A., Jeffries, R., Micela, G., Negueruela, I., Prusti, T., Rix, H.-W., Vallenari, A., Alfaro, E., Allende-Prieto, C., Babusiaux, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., François, P., Irwin, M., Koposov, S., Korn, A., Lanzafame, A., Pancino, E., Paunzen, E., Recio-Blanco, A., Sacco, G., Smiljanic, R., Van Eck, S., Walton, N., Aden, D., Aerts, C., Affer, L., Alcala, J.-M., Altavilla, G., Alves, J., Antoja, T., Arenou, F., Argiroffi, C., Asensio Ramos, A., Bailer-Jones, C., Balaguer-Nunez, L., Bayo, A., Barbuy, B., Barisevicius, G., Barrado y Navascues, D., Battistini, C., Bellas Velidis, I., Bellazzini, M., Belokurov, V., Bergemann, M., Bertelli, G., Biazzo, K., Bienayme, O., Bland-Hawthorn, J., Boeche, C., Bonito, S., Boudreault, S., Bouvier, J., Brandao, I., Brown, A., de Bruijne, J., Burleigh, M., Caballero, J., Caffau, E., Calura, F., Capuzzo-Dolcetta, R., Caramazza, M., Carraro, G., Casagrande, L., Casewell, S., Chapman, S., Chiappini, C., Chorniy, Y., Christlieb, N., Cignoni, M., Cocozza, G., Colless, M., Collet, R., Collins, M., Correnti, M., Covino, E., Crnojevic, D., Cropper, M., Cunha, M., Damiani, F., David, M., Delgado, A., Duffau, S., Edvardsson, B., Eldridge, J., Enke, H., Eriksson, K., Evans, N. W., Eyer, L., Famaey, B., Fellhauer, M., Ferreras, I., Figueras, F., Fiorentino, G., Flynn, C., Folha, D., Franciosini, E., Frasca, A., Freeman, K., Fremat, Y., Friel, E., Gaensicke, B., Gameiro, J., Garzon, F., Geier, S., Geisler, D., Gerhard, O., Gibson, B., Gomboc, A., Gomez, A., Gonzalez-Fernandez, C., Gonzalez Hernandez, J., Gosset, E., Grebel, E., Greimel, R., Groenewegen, M., Grundahl, F., Guarcello, M., Gustafsson, B., Hadrava, P., Hatzidimitriou, D., Hambly, N., Hammersley, P., Hansen, C., Haywood, M., Heber, U., Heiter, U., Held, E., Helmi, A., Hensler, G., Herrero, A., Hill, V., Hodgkin, S., Huelamo, N., Huxor, A., Ibata, R., Jackson, R., de Jong, R., Jonker, P., Jordan, S., Jordi, C., Jorissen, A., Katz, D., Kawata, D., Keller, S., Kharchenko, N., Klement, R., Klutsch, A., Knude, J., Koch, A., Kochukhov, O., Kontizas, M., Koubsky, P., Lallement, R., de Laverny, P., van Leeuwen, F., Lemasle, B., Lewis, G., Lind, K., Lindstrom, H. P. E., Lobel, A., Lopez Santiago, J., Lucas, P., Ludwig, H., Lueftinger, T., Magrini, L., Maiz Apellaniz, J., Maldonado, J., Marconi, G., Marino, A., Martayan, C., Martinez-Valpuesta, I., Matijevic, G., McMahon, R., Messina, S., Meyer, M., Miglio, A., Mikolaitis, S., Minchev, I., Minniti, D., Moitinho, A., Momany, Y., Monaco, L., Montalto, M., Monteiro, M. J., Monier, R., Montes, D., Mora, A., Moraux, E., Morel, T., Mowlavi, N., Mucciarelli, A., Munari, U., Napiwotzki, R., Nardetto, N., Naylor, T., Naze, Y., Nelemans, G., Okamoto, S., Ortolani, S., Pace, G., Palla, F., Palous, J., Parker, R., Penarrubia, J., Pillitteri, I., Piotto, G., Posbic, H., Prisinzano, L., Puzeras, E., Quirrenbach, A., Ragaini, S., Read, J., Read, M., Reyle, C., De Ridder, J., Robichon, N., Robin, A., Roeser, S., Romano, D., Royer, F., Ruchti, G., Ruzicka, A., Ryan, S., Ryde, N., Santos, N., Sanz Forcada, J., Sarro Baro, L. M., Sbordone, L., Schilbach, E., Schmeja, S., Schnurr, O., Schoenrich, R., Scholz, R.-D., Seabroke, G., Sharma, S., De Silva, G., Smith, M., Solano, E., Sordo, R., Soubiran, C., Sousa, S., Spagna, A., Steffen, M., Steinmetz, M., Stelzer, B., Stempels, E., Tabernero, H., Tautvaisiene, G., Thevenin, F., Torra, J., Tosi, M., Tolstoy, E., Turon, C., Walker, M., Wambsganss, J., Worley, C., Venn, K., Vink, J., Wyse, R., Zaggia, S., Zeilinger, W., Zoccali, M., Zorec, J., Zucker, D., and Zwitter, T.

Subjects
spectroscopy, stars, kinematics, abundances, Settore FIS/05 - Astronomia E Astrofisica, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Gaia-ESO Public Spectroscopic Survey has begun and will obtain high quality spectroscopy of some 100000 Milky Way stars, in the field and in open clusters, down to magnitude 19, systematically covering all the major components of the Milky Way. This survey will provide the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy. The motivation, organisation and implementation of the Gaia-ESO Survey are described, emphasising the complementarity with the ESA Gaia mission. Spectra from the very first observing run of the survey are presented.

303. Time-resolved Spectroscopy of DROXO X-ray Sources: Flares and Fe Kα emission

Author

Stelzer, B., Flaccomio, E., Pillitteri, I., Costanza ARGIROFFI, Sciortino, S., Stelzer, B, Flaccomio, E, Pillitteri, I, Argiroffi, C, and Sciortino, S

Subjects
X-ray, young star, Settore FIS/05 - Astronomia E Astrofisica, stellar coronae
Abstract

We present a systematic search for Fe Kα emission from young stellar objects of the ρ Ophiuchi star forming region observed in the Deep Rho Ophiuchi XMM-Newton Observation.

304. The Gaia-ESO Survey: Target selection of open cluster stars.

Author

Bragaglia, A., Alfaro, E. J., Flaccomio, E., Blomme, R., Donati, P., Costado, M., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nunez, L., Bonito, R., Cantat Gaudin, T., Casamiquela, L., Jeffries, R. D., and Jordi, C.

Subjects
*MAIN sequence (Astronomy), *OPEN clusters of stars, *STAR clusters, *STELLAR evolution, *VERY large telescopes, *EARLY stars
Abstract

Context. The Gaia-ESO Survey (GES) is a public, high-resolution spectroscopic survey, conducted with the multi-object spectrograph Fibre Large Array Multi Element Spectrograph (FLAMES) on the Very Large Telescope (European Southern Observatory, ESO, Cerro Paranal, Chile) from December 2011 to January 2018. Gaia-ESO has targeted all the main stellar components of the Milky Way, including thin and thick disc, bulge, and halo. In particular, a large sample of open clusters has been observed, from very young ones, just out of the embedded phase, to very old ones. Aims. The different kinds of clusters and stars targeted in them are useful to reach the main science goals of the open cluster part of GES, which are the study of the open cluster structure and dynamics, the use of open clusters to constrain and improve stellar evolution models, and the definition of Galactic disc properties (e.g., metallicity distribution). Methods. The Gaia-ESO Survey is organised in 19 working groups (WGs), each one being responsible for a task. We describe here the work of three of them, one in charge of the selection of the targets within each cluster or association (WG4), one responsible for defining the most probable candidate member stars (WG1), and another one in charge of the preparation of the observations (WG6). As the entire GES has been conducted before the second Gaia data release, we could not make use of the Gaia astrometry to define cluster member candidates. We made use of public and private photometry to select the stars to be observed with FLAMES, once brought on a common astrometric system (the one defined by 2MASS). Candidate target selection was based on ground-based proper motions, radial velocities, and X-ray properties when appropriate, for example, and it was mostly used to define the position of the clusters' evolutionary sequences in the colour-magnitude diagrams. Targets for GIRAFFE were then selected near the sequences in an unbiased way. We used known information on membership, when available, only for the few stars to be observed with UVES. Results. We collected spectra for 62 confirmed clusters in the main observing campaign (and a few more clusters were taken from the ESO archive). Among them are very young clusters, where the main targets are pre-main sequence stars, clusters with very hot and massive stars currently on the main sequence, intermediate-age and old clusters where evolved stars are the main targets. Our strategy of making the selection of targets as inclusive and unbiased as possible and of observing a significant and representative fraction of all possible targets permitted us to collect the largest, most accurate, and most homogeneous spectroscopic data set on open star clusters ever achieved. [ABSTRACT FROM AUTHOR]

Published
2022
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307. The Gaia-ESO Survey: a quiescent Milky Way with no significant dark/stellar accreted disc

Author

{Ruchti} G.~R., {Read} J.~I., {Feltzing} S., {Serenelli} A.~M., {McMillan} P., {Lind} K., {Bensby} T., {Bergemann} M., {Asplund} M., {Vallenari} A., {Flaccomio} E., {Pancino} E., {Korn} A.~J., {Recio-Blanco} A., {Bayo} A., {Carraro} G., {Costado} M.~T., {Damiani} F., {Heiter} U., {Hourihane} A., {Jofre} P., {Kordopatis} G., {Lardo} C., {de Laverny} P., and {Monaco} L.

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

According to our current cosmological model galaxies like the Milky Way are expected to experience many mergers over their lifetimes. The most massive of the merging galaxies will be dragged towards the disc plane depositing stars and dark matter into an accreted disc structure. In this work we utilize the chemo dynamical template developed in Ruchti et al. to hunt for accreted stars. We apply the template to a sample of 4675 stars in the third internal data release from the Gaia ESO Spectroscopic Survey. We find a significant component of accreted halo stars but find no evidence of an accreted disc component. This suggests that the Milky Way has had a rather quiescent merger history since its disc formed some 8 10 billion years ago and therefore possesses no significant dark matter disc.

308. VizieR Online Data Catalog: Gaia-ESO Survey: Tr 20, NGC4815, NGC6705 (Tautvaisiene+, 2015)

Author

Tautvaisiene, G., Drazdauskas, A., Mikolaitis, S., Barisevicius, G., Puzeras, E., Stonkute, E., Chorniy, Y., Magrini, L., Romano, D., Smiljanic, R., Bragaglia, A., Carraro, G., Friel, E., Morel, T., Pancino, E., Donati, P., Jimenez-Esteban, F., Gilmore, G., Randich, S., Jeffries, R. D., Vallenari, A., Bensby, T., Flaccomio, E., Recio-Blanco, A., Costado, M. T., Hill, V., Jofre, P., Carmela Lardo, Laverny, P., Masseron, T., Moribelli, L., Sousa, S. G., and Zaggia, S.

311. The Gaia-ESO Survey: evidence of atomic diffusion in M67?

Author

Motta, C Bertelli, Pasquali, A, Richer, J, Michaud, G, Salaris, M, Bragaglia, A, Magrini, L, Randich, S, Grebel, EK, Adibekyan, V, Blanco-Cuaresma, S, Drazdauskas, A, Fu, X, Martell, S, Tautvaisiene, G, Gilmore, G, Alfaro, EJ, Bensby, T, Flaccomio, E, Koposov, SE, Korn, AJ, Lanzafame, AC, Smiljanic, R, Bayo, A, Carraro, G, Casey, AR, Costado, MT, Damiani, F, Franciosini, E, Heiter, U, Hourihane, A, Jofre, P, Lardo, C, Lewis, J, Monaco, L, Morbidelli, L, Sacco, GG, Sousa, SG, Worley, CC, and Zaggia, S

Subjects
Galaxy: evolution, stars: abundances, 13. Climate action, Astrophysics::Solar and Stellar Astrophysics, Galaxy: abundances, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, stars: evolution, Astrophysics::Galaxy Astrophysics
Abstract

Investigating the chemical homogeneity of stars born from the same molecular cloud at virtually the same time is very important for our understanding of the chemical enrichment of the interstellar medium and with it the chemical evolution of the Galaxy. One major cause of inhomogeneities in the abundances of open clusters is stellar evolution of the cluster members. In this work, we investigate variations in the surface chemical composition of member stars of the old open cluster M67 as a possible consequence of atomic diffusion effects taking place during the main-sequence phase. The abundances used are obtained from high-resolution UVES/FLAMES spectra within the framework of the Gaia-ESO Survey. We find that the surface abundances of stars on the main sequence decrease with increasing mass reaching a minimum at the turn-off. After deepening of the convective envelope in subgiant branch stars, the initial surface abundances are restored. We found the measured abundances to be consistent with the predictions of stellar evolutionary models for a cluster with the age and metallicity of M67. Our findings indicate that atomic diffusion poses a non-negligible constraint on the achievable precision of chemical tagging methods.

312. CHANDRA Observations of the Open Cluster NGC 2516

Author

Wolk, S. J., Adams, N. R., Drake, J., Evans, N. R., Flaccomio, E., Freeman, P., Harnden, F. R., Kashyap, V., Patten, B. M., Pizzolato, N., Schachter, J., Stauffer, J., Zombeck, M., Damiani, F., Giuseppina Micela, Sciortino, S., Favata, F., and Jeffries, R.

313. VizieR Online Data Catalog: Activity and accretion in γ Vel and Cha I (Frasca+, 2015)

Author

Frasca, A., Biazzo, K., Lanzafame, A. C., Alcala, J. M., Brugaletta, E., Klutsch, A., Stelzer, B., Sacco, G. G., Spina, L., Jeffries, R. D., Montes, D., Alfaro, E. J., Barentsen, G., Bonito, R., Gameiro, J. F., Lopez-Santiago, J., Pace, G., Pasquini, L., Loredana Prisinzano, Sousa, S. G., Gilmore, G., Randich, S., Micela, G., Bragaglia, A., Flaccomio, E., Bayo, A., Costado, M. T., Franciosini, E., Hill, V., Hourihane, A., Jofre, P., Lardo, C., Maiorca, E., Masseron, T., Morbidelli, L., and Worley, C. C.

317. Chandra Observations of Open Cluster NGC 2516. II. Interpretation

Author

Harnden, F. R., Adams, N. R., Drake, J. J., Evans, N. R., Freeman, P., Kashyap, V., Schachter, J. F., Wolk, S. J., Patten, B. M., Stauffer, J., Pizzolato, N., Flaccomio, E., Francesco Damiani, Micela, G., Sciortino, S., Favata, F., Jeffries, R. D., and Chandra OAC - Stellar Team

320. The Gaia-ESO Survey: impact of extra mixing on C and N abundances of giant stars

Author

Lagarde, N, Reyle, C, Robin, AC, Tautvaisiene, G, Drazdauskas, A, Mikolaitis, S, Minkeviciute, R, Stonkute, E, Chorniy, Y, Bagdonas, V, Miglio, A, Nasello, G, Gilmore, G, Randich, S, Bensby, T, Bragaglia, A, Flaccomio, E, Francois, P, Korn, AJ, Pancino, E, Smiljanic, R, Bayo, A, Carraro, G, Costado, MT, Jimenez-Esteban, F, Jofre, P, Martell, SL, Masseron, T, Monaco, L, Morbidelli, L, Sbordone, L, Sousa, SG, and Zaggia, S

Subjects
Galaxy: stellar content, stars: abundances, 13. Climate action, Astrophysics::Solar and Stellar Astrophysics, Galaxy: abundances, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 14. Life underwater, stars: evolution, Astrophysics::Galaxy Astrophysics
Abstract

Context. TheGaia-ESO Public Spectroscopic Survey using FLAMES at the VLT has obtained high-resolution UVES spectra for a large number of giant stars, allowing a determination of the abundances of the key chemical elements carbon and nitrogen at their surface. The surface abundances of these chemical species are known to change in stars during their evolution on the red giant branch (RGB) after the first dredge-up episode, as a result of the extra mixing phenomena.Aims. We investigate the effects of thermohaline mixing on C and N abundances using the first comparison between theGaia-ESO survey [C/N] determinations with simulations of the observed fields using a model of stellar population synthesis.Methods. We explore the effects of thermohaline mixing on the chemical properties of giants through stellar evolutionary models computed with the stellar evolution code STAREVOL. We include these stellar evolution models in the Besançon Galaxy model to simulate the [C/N] distributions determined from the UVES spectra of theGaia-ESO survey and to compare them with the observations.Results. Theoretical predictions including the effect of thermohaline mixing are in good agreement with the observations. However, the field stars in theGaia-ESO survey with C and N abundance measurements have a metallicity close to solar, where the efficiency of thermohaline mixing is not very large. The C and N abundances derived by theGaia-ESO survey in open and globular clusters clearly show the impact of thermohaline mixing at low metallicity, which explains the [C/N] value observed in lower mass and older giant stars. Using independent observations of carbon isotopic ratio in clump field stars and open clusters, we also confirm that thermohaline mixing should be taken into account to explain the behaviour of12C/13C as a function of stellar age.Conclusions. Overall, the current model including thermohaline mixing is able to reproduce very well the C and N abundances over the whole metallicity range investigated by theGaia-ESO survey data.

321. VizieR Online Data Catalog: Classification of stellar spectra 644-681nm (Damiani+, 2014)

Author

Damiani, F., Loredana Prisinzano, Micela, Randich, S., Gilmore, G., Drew, J. E., Jeffries, R. D., Fremat, Y., Alfaro, E. J., Bensby, T., Bragaglia, A., Flaccomio, E., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Sacco, G. G., Smiljanic, R., Jackson, R. J., Laverny, P., Morbidelli, L., Worley, C. C., Hourihane, A., Costado, M. T., Jofre, P., Lind, K., and Maiorca, E.

322. Chandra Observations of the Young Open Cluster NGC 2516

Author

Flaccomio, E., Damiani, F., Giuseppina Micela, Pizzolato, N., Sciortino, S., Adams, N. R., Drake, J. J., Evans, N. R., Freeman, P., Harnden, F. R., Jeffries, R. D., Kashyap, V., Patten, B. M., Schachter, J. F., Stauffer, J. R., Wolk, S. J., and Zombeck, M. V.

323. The Gaia -ESO Survey: radial distribution of abundances in the Galactic disc from open clusters and young-field stars

Author

Magrini, L, Randich, S, Kordopatis, G, Prantzos, N, Romano, D, Chieffi, A, Limongi, M, François, P, Pancino, E, Friel, E, Bragaglia, A, Tautvaišiene, G, Spina, L, Overbeek, J, Cantat-Gaudin, T, Donati, P, Vallenari, A, Sordo, R, Jiménez-Esteban, FM, Tang, B, Drazdauskas, A, Sousa, S, Duffau, S, Jofré, P, Gilmore, G, Feltzing, S, Alfaro, E, Bensby, T, Flaccomio, E, Koposov, S, Lanzafame, A, Smiljanic, R, Bayo, A, Carraro, G, Casey, AR, Costado, MT, Damiani, F, Franciosini, E, Hourihane, A, Lardo, C, Lewis, J, Monaco, L, Morbidelli, L, Sacco, G, Sbordone, L, Worley, CC, and Zaggia, S

Subjects
13. Climate action, Astrophysics::Solar and Stellar Astrophysics, Galaxy: abundances, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 14. Life underwater, open clusters and associations: general, 7. Clean energy, Astrophysics::Galaxy Astrophysics
Abstract

The spatial distribution of elemental abundances in the disc of our Galaxy gives insights both on its assembly process and subsequent evolution, and on the stellar nucleogenesis of the different elements. Gradients can be traced using several types of objects as, for instance, (young and old) stars, open clusters, HII regions, planetary nebulae. We aim at tracing the radial distributions of abundances of elements produced through different nucleosynthetic channels -the alpha-elements O, Mg, Si, Ca and Ti, and the iron-peak elements Fe, Cr, Ni and Sc - by using the Gaia-ESO idr4 results of open clusters and young field stars. From the UVES spectra of member stars, we determine the average composition of clusters with ages >0.1 Gyr. We derive statistical ages and distances of field stars. We trace the abundance gradients using the cluster and field populations and we compare them with a chemo-dynamical Galactic evolutionary model. Results. The adopted chemo-dynamical model, with the new generation of metallicity-dependent stellar yields for massive stars, is able to reproduce the observed spatial distributions of abundance ratios, in particular the abundance ratios of [O/Fe] and [Mg/Fe] in the inner disc (5 kpc, This work was partially supported by the Gaia Research for European Astronomy Training (GREAT-ITN) Marie Curie network, funded through the European Union Seventh Framework Programme [FP7/2007-2013] under grant agreement n. 264895. This work was partly supported support through the European Research Council grant 320360: The Gaia-ESO Milky Way Survey G.T. and A.D. acknowledge support by the Research Council of Lithuania (MIP- 082 / 2015). This research has been partially supported by the National Institute for Astrophysics (INAF) through the grant PRIN-2014 ("Transient Universe, unveiling new types of stellar explosions with PESSTO"). F.J.E. acknowledges financial support from the Spacetec-CM project (S2013/ICE-2822). S.F. and T.B. are supported by the project grant "The New Milky Way" from the Knut and Alice Wallenberg Foundation. Support for SD was provided by the Chile’s Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS.

325. The Gaia-ESO Survey: The inner disc, intermediate-age open cluster Pismis 18

Author

Hatzidimitriou, D, Held, EV, Tognelli, E, Bragaglia, A, Magrini, L, Bravi, L, Gazeas, K, Dapergolas, A, Drazdauskas, A, Delgado-Mena, E, Friel, ED, Minkeviciute, R, Sordo, R, Tautvaisiene, G, Gilmore, G, Randich, S, Feltzing, S, Vallenari, A, Alfaro, EJ, Flaccomio, E, Lanzafame, AC, Pancino, E, Smiljanic, R, Bayo, A, Bergemann, M, Carraro, G, Casey, AR, Costado, MT, Damiani, F, Franciosini, E, Gonneau, A, Jofre, P, Lewis, J, Monaco, L, Morbidelli, L, Worley, CC, and Zaggia, S

Subjects
stars: abundances, Galaxy: abundances, 10. No inequality, open clusters and associations: individual: Pismis 18, Galaxy: formation Galaxy: disk
Abstract

Pismis 18 is a moderately populated, intermediate-age open cluster located within the solar circle at a Galactocentric distance of about 7 kpc. Few open clusters have been studied in detail in the inner disc region before the Gaia-ESO Survey. New data from the Gaia-ESO Survey allowed us to conduct an extended radial velocity membership study as well as spectroscopic metallicity and detailed chemical abundance measurements for this cluster. Gaia-ESO Survey data for 142 potential members, lying on the upper MS and on the red clump, yielded radial velocity measurements, which, together with proper motion measurements from the Gaia DR2, were used to determine the systemic velocity of the cluster and membership of individual stars. Photometry from Gaia DR2 was used to re-determine cluster parameters based on high confidence member stars only. Cluster abundance measurements of six radial-velocity member stars with UVES high-resolution spectroscopy are presented for 23 elements. According to the new estimates, based on high confidence members, Pismis 18 has an age of $700^{+40}_{-50}$ Myr, interstellar reddening of E(B-V) = $0.562^{+0.012}_{-0.026}$ mag and a de-reddened distance modulus of $DM_0 = 11.96^{+0.10}_{-0.24}$ mag. The median metallicity of the cluster (using the six UVES stars) is [Fe/H] = $+0.23 \pm 0.05$ dex, with [$\alpha$/Fe]= $0.07 \pm 0.13$ and a slight enhancement of s- and r- neutron-capture elements. With the present work, we fully characterized the open cluster Pismis 18, confirming its present location in the inner disc. We estimated a younger age than the previous literature values and gave, for the first time, its metallicity and its detailed abundances. Its [$\alpha$/Fe] and [s-process/Fe], both slightly super-solar, are in agreement with other inner-disc open clusters observed by the Gaia-ESO survey. [abridged]

326. COUP census of X-ray stars in BN-KL and OMC-1S

Author

Grosso, N., Feigelson, E. D., Getman, K. V., Townsley, L., Broos, P., Flaccomio, E., Mccaughrean, M. J., Giuseppina Micela, Sciortino, S., Bally, J., Smith, N., Muench, A. A., Palla, F., 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), Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), School of Physics (UNIVERSITY OF EXETER), University of Exeter, Astrophysikalisches Institut Potsdam (AIP), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, INAF - Osservatorio Astrofisico di Arcetri (OAA), F. Casoli, T. Contini, J.M. Hameury et L. Pagani, and The Chandra Orion Ultradeep Project (COUP)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract

We present a study of the X-ray sources detected in the vicinity of the two density peaks of the Orion Molecular Cloud 1 (OMC-1) behind the Orion Nebula Cluster (ONC), as seen in the exceptionally deep (~10 days) exposure of the Chandra Orion Ultradeep Project (COUP).

327. VizieR Online Data Catalog: GES iDR4 Mg-Al anticorrelation in GCs (Pancino+, 2017)

Author

Pancino, E., Romano, D., Tang, B., Tautvaisiene, G., Casey, A. R., Gruyters, P., Geisler, D., San, Roman I., Randich, S., Alfaro, E. J., Bragaglia, A., Flaccomio, E., Andreas Korn, Recio-Blanco, A., Smiljanic, R., Carraro, G., Bayo, A., Costado, M. T., Damiani, F., Jofre, P., Lardo, C., Laverny, P., Monaco, L., Morbidelli, L., Sbordone, L., Sousa, S. G., and Villanova, S.

328. VizieR Online Data Catalog: Gaia-ESO Survey abundances radial distribution (Magrini+, 2017)

Author

Magrini, L., Randich, S., Kordopatis, G., Prantzos, N., Romano, D., Chieffi, A., Limongi, M., Francois, P., Pancino, E., Friel, E., Bragaglia, A., Tautvaisiene, G., Spina, L., Overbeek, J., Cantat-Gaudin, T., Donati, P., Vallenari, A., Sordo, R., Jimenez-Esteban, F. M., Tang, B., Drazdauskas, A., Sousa, S., Duffau, S., Jofre, P., Gilmore, G., Feltzing, S., Alfaro, E., Bensby, T., Flaccomio, E., Koposov, S., Lanzafame, A., Smiljanic, R., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Franciosini, E., Hourihane, A., Carmela Lardo, Lewis, J., Monaco, L., Morbidelli, L., Sacco, G., Sbordone, L., Worley, C. C., and Zaggia, S.

329. VizieR Online Data Catalog: COUP: observations and source lists (Getman+, 2005)

Author

Getman, K. V., Flaccomio, E., Broos, P. S., Grosso, N., Tsujimoto, M., Townsley, L., Garmire, G. P., Kastner, J., Li, J., Harnden, F. R. Jr, Wolk, S., Murray, S. S., Lada, C. J., Muench, A. A., Mccaughrean, M. J., Meeus, G., Damiani, F., Giuseppina Micela, Sciortino, S., Bally, J., Hillenbrand, L. A., Herbst, W., Preibisch, T., and Feigelson, E. D.

330. VizieR Online Data Catalog: Gamma Vel cluster membership and IMF (Prisinzano+, 2016)

Author

Prisinzano, L., Damiani, F., Micela, G., Jeffries, R. D., Franciosini, E., Sacco, G. G., Frasca, A., Klutsch, A., Lanzafame, A., Alfaro, E. J., Biazzo, K., Bonito, R., Bragaglia, A., Caramazza, M., Vallenari, A., Carraro, G., Costado, M. T., Flaccomio, E., Jofre, P., Carmela Lardo, Monaco, L., Morbidelli, L., Mowlavi, N., Pancino, E., Randich, S., and Zaggia, S.

333. COUP sees PMS coronae rotate!

Author

Favata, F., Feigelson, E. D., Flaccomio, E., Harnden Jr, F. R., Herbst, W., Micela, G., Sciortino, S., and Scott Wolk

334. VizieR Online Data Catalog: Gaia-ESO Survey: NGC6705 (Cantat-Gaudin+, 2014)

Author

Cantat-Gaudin, T., Vallenari, A., Zaggia, S., Bragaglia, A., Sordo, R., Drew, J. E., Eisloeffel, J., Farnhill, H. J., Gonzalez-Solares, E., Greimel, R., Irwin, M. J., Kupcu-Yoldas, A., Jordi, C., Blomme, R., Sampedro, L., Costado, M. T., Alfaro, E., Smiljanic, R., Magrini, L., Donati, P., Friel, E. D., Jacobson, H., Abbas, U., Hatzidimitriou, D., Spagna, A., Vecchiato, A., Balaguer-Nunez, L., Lardo, C., Tosi, M., Pancino, E., Klutsch, A., Tautvaisiene, G., Drazdauskas, A., Puzeras, E., Jimenez-Esteban, F., Maiorca, E., Geisler, D., San, I., Villanova, S., Gilmore, G., Randich, S., Bensby, T., Flaccomio, E., Lanzafame, A., Recio-Blanco, A., Damiani, F., Hourihane, A., Jofre, P., Delaverny, P., Masseron, T., Morbidelli, L., Loredana Prisinzano, Sacco, G. G., Sbordone, L., and Worley, C. C.

337. VizieR Online Data Catalog: Abundances from Gaia-ESO Survey (Mikolaitis+, 2014)

Author

Mikolaitis, S., Hill, V., Recio-Blanco, A., Laverny, P., Allende Prieto, C., Kordopatis, G., Tautvaisiene, G., Romano, D., Gilmore, G., Randich, S., Feltzing, S., Micela, G., Vallenari, A., Alfaro, E. J., Bensby, T., Bragaglia, A., Flaccomio, E., Lanzafame, A. C., Pancino, E., Smiljanic, R., Bergemann, M., Carraro, G., Costado, M. T., Damiani, F., Hourihane, A., Jofre, P., Lardo, C., Magrini, L., Maiorca, E., Lorenzo Morbidelli, Sbordone, L., Sousa, S. G., Worley, C. C., and Zaggia, S.

339. Gaia-ESO Survey: INTRIGOSS - A New Library of High-resolution Synthetic Spectra

Author

Franchini, M, Morossi, C, Di Marcantonio, P, Chavez, M, Gilmore, G, Randich, S, Flaccomio, E, Koposov, SE, Korn, AJ, Bayo, A, Carraro, G, Casey, A, Franciosini, E, Hourihane, A, Jofré, P, Lardo, C, Lewis, J, Magrini, L, Morbidelli, L, Sacco, GG, Worley, C, and Zwitter, T

Subjects
13. Climate action, stars: late-type, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, astronomical databases: miscellaneous, 7. Clean energy, Astrophysics::Galaxy Astrophysics
Abstract

We present a high resolution synthetic spectral library, INTRIGOSS, designed for studying FGK stars. The library is based on atmosphere models computed with specified individual element abundances via ATLAS12 code. Normalized SPectra (NSP) and surface Flux SPectra (FSP), in the 4830-5400 A, wavelength range, were computed with the SPECTRUM code. INTRIGOSS uses the solar composition by Grevesse et al. 2007 and four [alpha/Fe] abundance ratios and consists of 15,232 spectra. The synthetic spectra are computed with astrophysical gf-values derived by comparing synthetic predictions with a very high SNR solar spectrum and the UVES-U580 spectra of five cool giants. The validity of the NSPs is assessed by using the UVES-U580 spectra of 2212 stars observed in the framework of the Gaia-ESO Survey and characterized by homogeneous and accurate atmospheric parameter values and by detailed chemical compositions. The greater accuracy of NSPs with respect to spectra from the AMBRE, GES_Grid, PHOENIX, C14, and B17 synthetic spectral libraries is demonstrated by evaluating the consistency of the predictions of the different libraries for the UVES-U580 sample stars. The validity of the FSPs is checked by comparing their prediction with both observed spectral energy distribution and spectral indices. The comparison of FSPs with SEDs derived from ELODIE, INDO--U.S., and MILES libraries indicates that the former reproduce the observed flux distributions within a few percent and without any systematic trend. The good agreement between observational and synthetic Lick/SDSS indices shows that the predicted blanketing of FSPs well reproduces the observed one, thus confirming the reliability of INTRIGOSS FSPs.

343. NGC 2264: A Chandra View.

Author

Corbelli, Edvige, Palla, Francesco, Zinnecker, Hans, Flaccomio, E., Micela, G., Sciortino, S., Harnden, F. R., and Hartmann, L.

Abstract

We present first results from a Chandra ACIS-I observation of the star forming region NGC 2264. Using the X-ray data to select members, we estimate the NGC 2264 stellar Initial Mass Function (IMF). [ABSTRACT FROM AUTHOR]

Published
2005
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345. Chandra Observations of the Open Cluster NGC 2516.

Author

Harnden, Jr., F. R., Adams, N. R., Damiani, F., Drake, J. J., Evans, N. R., Favata, F., Flaccomio, E., Freeman, P., Jeffries, R. D., Kashyap, V., Micela, G., Patten, B. M., Pizzolato, N., Schachter, J. F., Sciortino, S., Stauffer, J., Wolk, S. J., and Zombeck, M. V.

Published
2001
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346. Accretion dynamics and disk evolution in NGC 2264: a study based on CoRoT*photometric observations**

Author

Alencar, S. H. P., Teixeira, P. S., Guimarães, M. M., McGinnis, P. T., Gameiro, J. F., Bouvier, J., Aigrain, S., Flaccomio, E., and Favata, F.

Abstract

Context. The young cluster NGC 2264 was observed with the CoRoT satellite for 23 days uninterruptedly in March 2008 with unprecedented photometric accuracy. We present the first results of our analysis of the accreting population belonging to the cluster as observed by CoRoT. Aims. We search for possible light curve variability of the same nature as that observed in the classical T Tauri star AA Tau, which was attributed to a magnetically controlled inner disk warp. The inner warp dynamics is supposed to be directly associated with the interaction between the stellar magnetic field and the inner disk region. Methods. We analyzed the CoRoT light curves of 83 previously known classical T Tauri stars that belong to NGC 2264 classifying them according to their light-curve morphology. We also studied the CoRoT light-curve morphology as a function of a Spitzer-based classification of the star-disk systems. Results. The classification derived on the basis of the CoRoT light-curve morphology agrees very well with the SpitzerIRAC-based classification of the systems. The percentage of AA Tau-like light curves decreases as the inner disk dissipates, from 40% ±10% in systems with thick inner disks to 36% ±16% in systems with anemic disks and zero in naked photosphere systems. Indeed, 91% ±29% of the CTTS with naked photospheres exhibit pure spot-like variability, while only 18% ±7% of the thick disk systems do so, presumably those seen at low inclination and thus free of variable obscuration. Conclusions. AA Tau-like light curves are found to be fairly common, with a frequency of at least ~30 to 40% in young stars with inner dusty disks. The temporal evolution of the light curves indicates that the structure of the inner disk warp, located close to the corotation radius and responsible for the obscuration episodes, varies over a timescale of a few (~1–3) rotational periods. This probably reflects the highly dynamical nature of the star-disk magnetospheric interaction.

Published
2010

347. Gaia-ESO Survey::INTRIGOSS - A new library of High Resolution Synthetic Spectra

Author

Gerry Gilmore, A. Hourihane, E. Franciosini, Clare Worley, Ettore Flaccomio, L. Morbidelli, Amelia Bayo, G. G. Sacco, James R. Lewis, Andrew R. Casey, Miguel Chavez, Carmela Lardo, Sergey E. Koposov, Paolo Di Marcantonio, Giovanni Carraro, Andreas J. Korn, Sofia Randich, Laura Magrini, Tomaz Zwitter, Paula Jofre, Carlo Morossi, Mariagrazia Franchini, Franchini, M [0000-0001-5611-2333], Flaccomio, E [0000-0002-3638-5788], Koposov, SE [0000-0003-2644-135X], Bayo, A [0000-0001-7868-7031], Carraro, G [0000-0002-0155-9434], Casey, A [0000-0003-0174-0564], Lardo, C [0000-0002-4295-8773], Zwitter, T [0000-0002-2325-8763], Apollo - University of Cambridge Repository, ITA, USA, GBR, AUS, CHL, MEX, SVN, SWE, CHE, Franchini M., Morossi C., Di Marcantonio P., Chavez M., Gilmore G., Randich S., Flaccomio E., Koposov S.E., Korn A.J., Bayo A., Carraro G., Casey A., Franciosini E., Hourihane A., Jofre P., Lardo C., Lewis J., Magrini L., Morbidelli L., Sacco G.G., Worley C., and Zwitter T.

Subjects
astro-ph.SR, FOS: Physical sciences, Flux, Blanketing, Astrophysics::Cosmology and Extragalactic Astrophysics, astronomical databases: miscellaneous, Astrophysics, 7. Clean energy, 01 natural sciences, Spectral line, Atmosphere, Astronomi, astrofysik och kosmologi, Consistency (statistics), 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, stars: late-type, Resolution (electron density), Astronomy and Astrophysics, astronomical databases: miscellaneou, miscellaneous [astronomical databases], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Spectral energy distribution, late-type [stars], Astrophysics::Earth and Planetary Astrophysics
Abstract

We present a high resolution synthetic spectral library, INTRIGOSS, designed for studying FGK stars. The library is based on atmosphere models computed with specified individual element abundances via ATLAS12 code. Normalized SPectra (NSP) and surface Flux SPectra (FSP), in the 4830-5400 A, wavelength range, were computed with the SPECTRUM code. INTRIGOSS uses the solar composition by Grevesse et al. 2007 and four [alpha/Fe] abundance ratios and consists of 15,232 spectra. The synthetic spectra are computed with astrophysical gf-values derived by comparing synthetic predictions with a very high SNR solar spectrum and the UVES-U580 spectra of five cool giants. The validity of the NSPs is assessed by using the UVES-U580 spectra of 2212 stars observed in the framework of the Gaia-ESO Survey and characterized by homogeneous and accurate atmospheric parameter values and by detailed chemical compositions. The greater accuracy of NSPs with respect to spectra from the AMBRE, GES_Grid, PHOENIX, C14, and B17 synthetic spectral libraries is demonstrated by evaluating the consistency of the predictions of the different libraries for the UVES-U580 sample stars. The validity of the FSPs is checked by comparing their prediction with both observed spectral energy distribution and spectral indices. The comparison of FSPs with SEDs derived from ELODIE, INDO--U.S., and MILES libraries indicates that the former reproduce the observed flux distributions within a few percent and without any systematic trend. The good agreement between observational and synthetic Lick/SDSS indices shows that the predicted blanketing of FSPs well reproduces the observed one, thus confirming the reliability of INTRIGOSS FSPs., 32 pages, 12 figures

Published
2018

348. The Gaia-ESO Survey: A new diagnostic for accretion and outflow activity in the young cluster NGC 2264.

Author

Bonito, R., Prisinzano, L., Venuti, L., Damiani, F., Micela, G., Sacco, G., Traven, G., Biazzo, K., Sbordone, L., Masseron, T., Zwitter, T., Gonneau, A., Bayo, A., Roccatagliata, V., Randich, S., Vink, J. S., Jofre, P., Flaccomio, E., Magrini, L., and Carraro, G.

Subjects
*STELLAR winds, *STAR formation, *OPEN clusters of stars, *ACCRETION disks
Abstract

Context. NGC 2264 is a young cluster whose accretion properties can be investigated in detail by taking advantage of the FLAMES data in the context of the Gaia-ESO Survey. In fact, the analysis of the Hα emission line profile can provide us with information about the accretion and ejection activity of young stars. However, a strong nebular emission that contributes to the Hα emission can alter the profiles, with consequences for their physical interpretation. Aims. Our study is aimed at investigating the accretion and ejection properties of NGC 2264 by applying a proper treatment of the sky contribution to the Hα and forbidden emission lines (FELs; [SII] and [NII] doublets). Methods. We developed a tool, the OHαNA-method, to handle the strong nebular contribution and spectra with spurious profiles of the Hα and FELs, namely altered Hα profiles or absorption features artificially created where emission lines (FELs) are expected. We derived the quantitative measurements of relevant parameters to describe the accretion and ejection processes in young members of NGC 2264, focusing on reliable quantities derived from the width of the lines, which is relatively unaffected by the nebular emission, unlike the intensity peak, which can be altered significantly. Results. We derive the quantitative measurements related to the Hα emission line and discuss the comparison between the original and sky-subtracted spectra. We thus reveal possible profile alterations with consequences for their physical interpretation. Furthermore, we show the analysis of the variability for multi-epoch observations, also deriving the velocity of the infalling and outflowing plasma from the wings of the broad Hα emission line (in accreting stars). We also explore the mass accretion rate versus full width at zero intensity of the Hα line, namely Ṁ versus FWZI(Hα), a correlation based on the width of the emission line, which is expected to be more robust with respect to any measurement derived from the peak (e.g., Hα10%) and possibly altered by the nebular contribution. Conclusions. We are able to ascertain that more than 20% of the confirmed accretors, which have already been identified in NGC 2264, are affected by the alteration of their line profiles due to the contribution of the nebular emission. Therefore, this is an important issue to consider when investigating accretion and ejection processes in young stellar clusters. While a small fraction of spectra can be unequivocally classified as either unaffected by nebular emission or dominated by nebular emission, the majority (> 90%) represent intermediate cases whose spectral features have to be investigated in detail to derive reliable measurements of the relevant parameters and their physical implications. [ABSTRACT FROM AUTHOR]

Published
2020
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349. The Gaia-ESO Survey: Exploring the complex nature and origins of the Galactic bulge populations

Author

Mathias Schultheis, Dante Minniti, A. Hourihane, Manuela Zoccali, Amelia Bayo, Francesco Damiani, Giovanni Carraro, C. C. Worley, Elena Pancino, Alejandra Recio-Blanco, Francesca Matteucci, Andrew R. Casey, Paula Jofre, G. G. Sacco, Thomas Bensby, Sergey E. Koposov, S. Mikolaitis, M. T. Costado, Carmela Lardo, L. Morbidelli, Paolo Donati, Vanessa Hill, Michael R. Hayden, Sofia Feltzing, P. de Laverny, Ettore Flaccomio, E. Spitoni, C. Babusiaux, Laura Magrini, Sofia Randich, Karin Lind, Jack Lewis, Gerard Gilmore, Emilio J. Alfaro, E. Franciosini, Oscar A. Gonzalez, Simone Zaggia, Angela Bragaglia, A. Rojas-Arriagada, Millennium Institute of Astrophysics, Instituto de Astrofisica [Santiago], Pontificia Universidad Católica de Chile (UC), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), University of Turin, Groupe d'études pour l'application des méthodes scientifiques à l'architecture et à l'urbanisme (GAMSAU), École nationale supérieure d'architecture de Marseille-Luminy (ENSA-M), Cognition Behaviour Technology (CobTek), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre Hospitalier Universitaire de Nice (CHU Nice)-Institut Claude Pompidou [Nice] (ICP - Nice)-Université Côte d'Azur (UCA), European Commission, European Research Council, Leverhulme Trust, Centre National de la Recherche Scientifique (France), Agence Nationale de la Recherche (France), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Rojas Arriagada, A., Recio Blanco, A., De Laverny, P., Mikolaitis, Š., Matteucci, MARIA FRANCESCA, Spitoni, Emanuele, Schultheis, M., Hayden, M., Hill, V., Zoccali, M., Minniti, D., Gonzalez, O. A., Gilmore, G., Randich, S., Feltzing, S., Alfaro, E. J., Babusiaux, C., Bensby, T., Bragaglia, A., Flaccomio, E., Koposov, S. E., Pancino, E., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Donati, P., Franciosini, E., Hourihane, A., Jofré, P., Lardo, C., Lewis, J., Lind, K., Magrini, L., Morbidelli, L., Sacco, G. G., Worley, C. C., Zaggia, S., Rojas-Arriagada A., Recio-Blanco A., De Laverny P., Mikolaitis S., Matteucci F., Spitoni E., Schultheis M., Hayden M., Hill V., Zoccali M., Minniti D., Gonzalez O.A., Gilmore G., Randich S., Feltzing S., Alfaro E.J., Babusiaux C., Bensby T., Bragaglia A., Flaccomio E., Koposov S.E., Pancino E., Bayo A., Carraro G., Casey A.R., Costado M.T., Damiani F., Donati P., Franciosini E., Hourihane A., Jofre P., Lardo C., Lewis J., Lind K., Magrini L., Morbidelli L., Sacco G.G., Worley C.C., Zaggia S., COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre Hospitalier Universitaire de Nice (CHU Nice)-Institut Claude Pompidou [Nice] (ICP - Nice)

Subjects
stars: abundances, Galaxy: bulge, Galaxy: formation, Galaxy: abundances, Galaxy: stellar content, astro-ph.GA, bulge [Galaxy], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Bulge, 0103 physical sciences, Thick disk, stellar content [Galaxy], Astrophysics::Solar and Stellar Astrophysics, abundance [Galaxy], 010303 astronomy & astrophysics, Red clump, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Plane (geometry), abundances [Galaxy], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Bimodality, Galaxy: abundance, Stars, Thin disk, formation [Galaxy], Space and Planetary Science, abundances [Stars], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Full list of authors: Rojas-Arriagada, A.; Recio-Blanco, A.; de Laverny, P.; Mikolaitis, Š.; Matteucci, F.; Spitoni, E.; Schultheis, M.; Hayden, M.; Hill, V.; Zoccali, M.; Minniti, D.; Gonzalez, O. A.; Gilmore, G.; Randich, S.; Feltzing, S.; Alfaro, E. J.; Babusiaux, C.; Bensby, T.; Bragaglia, A.; Flaccomio, E. Koposov, S. E.; Pancino, E.; Bayo, A.; Carraro, G.; Casey, A. R.; Costado, M. T.; Damiani, F.; Donati, P.; Franciosini, E.; Hourihane, A.; Jofré, P.; Lardo, C.; Lewis, J.; Lind, K.; Magrini, L.; Morbidelli, L.; Sacco, G. G.; Worley, C. C.; Zaggia, S., Context. As observational evidence steadily accumulates, the nature of the Galactic bulge has proven to be rather complex: the structural, kinematic, and chemical analyses often lead to contradictory conclusions. The nature of the metal-rich bulge - and especially of the metal-poor bulge - and their relation with other Galactic components, still need to be firmly defined on the basis of statistically significant high-quality data samples. Aims. We used the fourth internal data release of the Gaia-ESO survey to characterize the bulge metallicity distribution function (MDF), magnesium abundance, spatial distribution, and correlation of these properties with kinematics. Moreover, the homogeneous sampling of the different Galactic populations provided by the Gaia-ESO survey allowed us to perform a comparison between the bulge, thin disk, and thick disk sequences in the [Mg/Fe] vs. [Fe/H] plane in order to constrain the extent of their eventual chemical similarities. Methods. We obtained spectroscopic data for ∼2500 red clump stars in 11 bulge fields, sampling the area -10° ≥ l ≥ +8° and -10° ≥ b ≥ -4° from the fourth internal data release of the Gaia-ESO survey. A sample of ∼6300 disk stars was also selected for comparison. Spectrophotometric distances computed via isochrone fitting allowed us to define a sample of stars likely located in the bulge region. Results. From a Gaussian mixture models (GMM) analysis, the bulge MDF is confirmed to be bimodal across the whole sampled area. The relative ratio between the two modes of the MDF changes as a function of b, with metal-poor stars dominating at high latitudes. The metal-rich stars exhibit bar-like kinematics and display a bimodality in their magnitude distribution, a feature which is tightly associated with the X-shape bulge. They overlap with the metal-rich end of the thin disk sequence in the [Mg/Fe] vs. [Fe/H] plane. On the other hand, metal-poor bulge stars have a more isotropic hot kinematics and do not participate in the X-shape bulge. Their Mg enhancement level and general shape in the [Mg/Fe] vs. [Fe/H] plane is comparable to that of the thick disk sequence. The position at which [Mg/Fe] starts to decrease with [Fe/H], called the "knee", is observed in the metal-poor bulge at [Fe/H] = -0:37 ± 0:09, being 0.06 dex higher than that of the thick disk. Although this difference is inside the error bars, it suggest a higher star formation rate (SFR) for the bulge than for the thick disk. We estimate an upper limit for this difference of Δ[Fe/H] = 0:24 dex. Finally, we present a chemical evolution model that suitably fits the whole bulge sequence by assuming a fast (, This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and the Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR) in the form of the grant "Premiale VLT 2012". The results presented here benefited from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. A. Recio-Blanco, P. de Laverny, and V. Hill acknowledge the Programme National de Cosmologie et Galaxies (PNCG) of CNRS/INSU, France, for financial support. A. Recio-Blanco, P. de Laverny, and V. Hill acknowledge financial support form the ANR 14-CE33-014-01. M. Zoccali gratefully acknowledges support from the Ministry of Economy, Development, and Tourism's Millenium Science Initiative through grant IC120009, awarded to the Millenium Institute of Astrophysics (MAS), by Fondecyt Regular 1150345 and by the BASAL-CATA Center for Astrophysics and Associated Technologies PFB-06.

Published
2017

350. Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines

Author

Rosaria Bonito, Lorenzo Monaco, C. C. Worley, V. M. Kalari, Giovanni Carraro, A. Hourihane, G. G. Sacco, A. C. Lanzafame, Jack Lewis, Sofia Randich, Elena Pancino, Ricardo Dorda, L. Prisinzano, Sergey E. Koposov, Michela Mapelli, Tomaž Zwitter, M. T. Costado, Emilio J. Alfaro, Ettore Flaccomio, J. Maíz Apellániz, A. Klutsch, Carmela Lardo, F. Damiani, L. Morbidelli, Simone Zaggia, Giuseppina Micela, Amelia Bayo, Gerard Gilmore, Laura Magrini, Andrew R. Casey, E. Franciosini, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astrofísica Estelar (AE), Damiani, F., Bonito, R., Magrini, L., Prisinzano, L., Mapelli, M., Micela, G., Kalari, V., Maíz Apellániz, J., Gilmore, G., Randich, S., Alfaro, E., Flaccomio, E., Koposov, S., Klutsch, A., Lanzafame, A., Pancino, E., Sacco, G., Bayo, A., Carraro, G., Casey, A., Costado, M., Franciosini, E., Hourihane, A., Lardo, C., Lewis, J., Monaco, L., Morbidelli, L., Worley, C., Zaggia, S., Zwitter, T., Dorda, R., Damiani F., Bonito R., Magrini L., Prisinzano L., Mapelli M., Micela G., Kalari V., Maiz Apellaniz J., Gilmore G., Randich S., Alfaro E., Flaccomio E., Koposov S., Klutsch A., Lanzafame A.C., Pancino E., Sacco G.G., Bayo A., Carraro G., Casey A.R., Costado M.T., Franciosini E., Hourihane A., Lardo C., Lewis J., Monaco L., Morbidelli L., Worley C., Zaggia S., Zwitter T., Dorda R., European Research Council, Gilmore, Gerard [0000-0003-4632-0213], Koposov, Sergey [0000-0003-2644-135X], Casey, Andrew [0000-0003-0174-0564], Worley, Clare [0000-0001-9310-2898], and Apollo - University of Cambridge Repository

Subjects
HII regions, astro-ph.SR, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, Shell (structure), Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM: individual objects: Carina nebula, ISM: general, Ionization, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, HII region, Emission spectrum, 010303 astronomy & astrophysics, QC, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Astronomía y Astrofísica, Physics, Nebula, general [ISM], 010308 nuclear & particles physics, individual objects: Carina nebula [ISM], Astronomy and Astrophysics, Gas dynamics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Dust lane, Core (optical fiber), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

Aims. We present observations from the Gaia-ESO Survey in the lines of Hα, [N II], [S II], and He I of nebular emission in the central part of the Carina nebula. Methods. We investigate the properties of the two already known kinematic components (approaching and receding), which account for the bulk of emission. Moreover, we investigate the features of the much less known low-intensity high-velocity (absolute RV >50 km s) gas emission. Results. We show that gas giving rise to Hα and He I emission is dynamically well correlated with but not identical to gas seen through forbidden-line emission. Gas temperatures are derived from line-width ratios, and densities from [S II] doublet ratios. The spatial variation of N ionization is also studied, and found to differ between the approaching and receding components. The main result is that the bulk of the emission lines in the central part of Carina arise from several distinct shell-like expanding regions, the most evident found around η Car, the Trumpler 14 core, and the star WR25. These >shells> are non-spherical and show distortions probably caused by collisions with other shells or colder, higher-density gas. Some of them are also partially obscured by foreground dust lanes, while very little dust is found in their interior. Preferential directions, parallel to the dark dust lanes, are found in the shell geometries and physical properties, probably related to strong density gradients in the studied region. We also find evidence that the ionizing flux emerging from η Car and the surrounding Homunculus nebula varies with polar angle. The high-velocity components in the wings of Hα are found to arise from expanding dust reflecting the η Car spectrum. © ESO, 2016., This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541

Published
2016

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