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1. ESA Voyage 2050 white paper -- Faint objects in motion: the new frontier of high precision astrometry

Author

Malbet, F., Abbas, U., Alves, J., Boehm, C., Brown, W., Chemin, L., Correia, A., Courbin, F., Darling, J., Diaferio, A., Fortin, M., Fridlund, M., Gnedin, O., Holl, B., Krone-Martins, A., L��ger, A., Labadie, L., Laskar, J., Mamon, G., McArthur, B., Michalik, D., Moitinho, A., Oertel, M., Ostorero, L., Schneider, J., Scott, P., Shao, M., Sozzetti, A., Tomsick, J., Valluri, M., Wyse, R., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 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), 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the frontier of precision astrometry from evidence of earth-massed habitable worlds around the nearest starts, and also into distant Milky way objects up to the Local Group of galaxies. As we enter the era of the James Webb Space Telescope and the new ground-based, adaptive-optics-enabled giant telescopes, by obtaining these high precision measurements on key objects that Gaia could not reach, a mission that focuses on high precision astrometry science can consolidate our theoretical understanding of the local universe, enable extrapolation of physical processes to remote redshifts, and derive a much more consistent picture of cosmological evolution and the likely fate of our cosmos. Already several missions have been proposed to address the science case of faint objects in motion using high precision astrometry ESA missions: NEAT for M3, micro-NEAT for S1 mission, and Theia for M4 and M5. Additional new mission configurations adapted with technological innovations could be envisioned to pursue accurate measurements of these extremely small motions. The goal of this white paper is to address the fundamental science questions that are at stake when we focus on the motions of faint sky objects and to briefly review quickly instrumentation and mission profiles., White paper for the Voyage 2050 long-term plan in the ESA Science Programme. arXiv admin note: substantial text overlap with arXiv:1707.01348

Published
2019

2. ESA Voyage 2050 white paper -- Faint objects in motion: the new frontier of high precision astrometry

Author

Malbet, Fabien, Abbas, U., Alves, J., Boehm, C., Brown, W., Chemin, L., Correia, A., Courbin, F., Darling, J., Diaferio, A., Fortin, M., Fridlund, M., Gnedin, O., Holl, B., Krone-Martins, A., Léger, A., Labadie, L., Laskar, J., Mamon, G., McArthur, B., Michalik, D., Moitinho, A., Oertel, M., Ostorero, L., Schneider, J., Scott, P., Shao, M., Sozzetti, A., Tomsick, J., Valluri, M., Wyse, R., 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]), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Universität Wien, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), M2A 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Physics, Czech Academy of Sciences [Prague] (CAS), Laboratoire d'Astrophysique [Versoix] (LASTRO), Ecole Polytechnique Fédérale de Lausanne (EPFL), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Heckscher-Klinikum, 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), 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidade de Lisboa = University of Lisbon (ULISBOA), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), State Joint Key Laboratory of Environmental Simulation and Pollution Control, College of Environmental Sciences and Engineering [Peking], Peking University [Beijing]-Peking University [Beijing], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Institut Planetologie Astrophysique de Grenoble, 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), AUTRES, Academy of Sciences of the Czech Republic, Laboratoire d'Astrophysique, European Space Agency (ESA)-European Space Agency (ESA), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universidade de Lisboa (ULISBOA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), University of California [Berkeley], University of California-University of California, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the frontier of precision astrometry from evidence of earth-massed habitable worlds around the nearest starts, and also into distant Milky way objects up to the Local Group of galaxies. As we enter the era of the James Webb Space Telescope and the new ground-based, adaptive-optics-enabled giant telescopes, by obtaining these high precision measurements on key objects that Gaia could not reach, a mission that focuses on high precision astrometry science can consolidate our theoretical understanding of the local universe, enable extrapolation of physical processes to remote redshifts, and derive a much more consistent picture of cosmological evolution and the likely fate of our cosmos. Already several missions have been proposed to address the science case of faint objects in motion using high precision astrometry ESA missions: NEAT for M3, micro-NEAT for S1 mission, and Theia for M4 and M5. Additional new mission configurations adapted with technological innovations could be envisioned to pursue accurate measurements of these extremely small motions. The goal of this white paper is to address the fundamental science questions that are at stake when we focus on the motions of faint sky objects and to briefly review quickly instrumentation and mission profiles.

Published
2019

3. Coma Berenices: first evidence for incomplete vertical phase-mixing in local velocity space with RAVE - confirmed with Gaia DR2

Author

Monari, G., Famaey, B., Minchev, I., Antoja, T., Bienayme, O., Gibson, B. K., Grebel, E. K., Kordopatis, G., McMillan, P., Navarro, J., Parker, Q. A., Quillen, A. C., Reid, W., Seabroke, G., Siebert, A., Steinmetz, M., Wyse, R. F. G., and Zwitter, T.

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

Before the publication of the Gaia DR2 we confirmed with RAVE and TGAS an observation recently made with the GALAH survey by Quillen ey al. concerning the Coma Berenices moving group in the Solar neighbourhood, namely that it is only present at negative Galactic latitudes. This allowed us to show that it is coherent in vertical velocity, providing a first evidence for incomplete vertical phase-mixing. We estimated for the first time from dynamical arguments that the moving group must have formed at most ~ 1.5 Gyr ago, and related this to a pericentric passage of the Sagittarius dwarf satellite galaxy. The present note is a rewritten version of the original arXiv post on this result now also including a confirmation of our finding with Gaia DR2., Comment: AAS Research Notes

Published
2018
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4. Chemodynamics of the Milky Way and disc formation history: insight from the RAVE and Gaia-ESO surveys

Author

Kordopatis, G., Wyse, R. F. G., and Binney, J.

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

Multi-object spectrographs have opened a new window on the analyses of the chemo-dynamical properties of old Milky Way stars. These analyses allow us to trace back the internal mechanisms and the external factors that have influenced the evolution of our Galaxy, and therefore understand fundamental aspects of galaxy evolution in general. Here, we present recent results from the RAdial Velocity Experiment (RAVE) and the Gaia-ESO survey. These surveys explore the Milky Way properties in different ways, in terms of sample size and selection, magnitude range, and spectral resolution. We focus here on (i) the first direct detection of evidence for radial migration within the thin disc, providing insight into the history of spiral structure of the Milky Way, and (ii) the chemo-dynamical characterisation of the metal-weak thick and thin discs, for which chemo-dynamical models still have difficulties in reproducing., 5 pages, to appear in Astronomische Nachrichten, special issue "Reconstruction the Milky Way's History: Spectroscopic surveys, Asteroseismology and Chemo-dynamical models", Guest Editors C. Chiappini, J. Montalban, and M. Steffen, AN 2016 (in press)"

Published
2016

5. DIFFUSE INTERSTELLAR BAND AT 8620 \ufffd IN RAVE: A NEW METHOD FOR DETECTING THE DIFFUSE INTERSTELLAR BAND IN SPECTRA OF COOL STARS

Author

Kos, J., Zwitter, T., Grebel, E. K., Bienayme, O., Binney, J., Bland-Hawthorn, J., Freeman, K. C., Gibson, B. K., Gilmore, G., Kordopatis, G., Navarro, J. F., Parker, Q., Reid, W. A., Seabroke, G., Siebert, A., Siviero, A., Steinmetz, M., Watson, F., and Wyse, R. F. G.

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

Diffuse interstellar bands are usually observed in spectra of hot stars, where interstellar lines are rarely blended with stellar ones. The need for hot stars is a strong limitation in the number of sightlines we can observe and the distribution of sightlines in the Galaxy, as hot stars are rare and concentrated in the Galactic plane. We are introducing a new method, where interstellar lines can be observed in spectra of cool stars in large spectroscopic surveys. The method is completely automated and does not require prior knowledge of the stellar parameters. If known, the stellar parameters only reduce the computational time and are not involved in the extraction of the interstellar spectrum. The main step in extracting interstellar lines is a construction of the stellar spectrum, which is in our method done by finding other observed spectra that lack interstellar features and are otherwise very similar to the spectrum in question. Such spectra are then combined into a single stellar spectrum template, which matches the stellar component in an observed spectrum. We demonstrate the performance of this new method on a sample of 482,430 spectra observed in RAVE survey. However, many spectra have to be combined (48 on average) in order to achieve a S/N ratio high enough to measure the DIB's profile, hence limiting the spatial information about the ISM. Only one strong interstellar line is included in the RAVE spectral range, a diffuse interstellar band at 8620 ��. We compare its equivalent width with extinction maps and with Bayesian reddening, calculated for individual stars, and provide a linear relation between the equivalent width and reddening. Separately from the introduced method, we calculate equivalent widths of the diffuse interstellar band in spectra of hot stars with known extinction and compare all three linear relations with each other and with relations from the literature., 12 pages, 10 figures, submitted to ApJ

Published
2013

6. Chromospherically Active Stars in the RAVE Survey. I. The Catalogue

Author

��erjal, M., Zwitter, T., Matijevi��, G., Strassmeier, K. G., Bienaym��, O., Bland-Hawthorn, J., Boeche, C., Freeman, K. C., Grebel, E. K., Kordopatis, G., Munari, U., Navarro, J. F., Parker, Q. A., Reid, W., Seabroke, G., Siviero, A., Steinmetz, M., and Wyse, R. F. G.

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

RAVE, the unbiased magnitude limited survey of the southern sky stars, contained 456,676 medium-resolution spectra at the time of our analysis. Spectra cover the CaII IRT range which is a known indicator of chromospheric activity. Our previous work (Matijevi\v{c} et al. 2012) classified all spectra using locally linear embedding. It identified 53,347 cases with a suggested emission component in calcium lines. Here we use a spectral subtraction technique to measure the properties of this emission. Synthetic templates are replaced by the observed spectra of non-active stars to bypass the difficult computations of non-LTE profiles of the line cores and stellar parameter dependence. We derive both the equivalent width of the excess emission for each calcium line on a 5\AA\ wide interval and their sum EW_IRT for ~44,000 candidate active dwarf stars with S/N>20 and with no respect to the source of their emission flux. From these ~14,000 show a detectable chromospheric flux with at least 2\sigma\ confidence level. Our set of active stars vastly enlarges previously known samples. Atmospheric parameters and in some cases radial velocities of active stars derived from automatic pipeline suffer from systematic shifts due to their shallower calcium lines. We re-estimate the effective temperature, metallicity and radial velocities for candidate active stars. The overall distribution of activity levels shows a bimodal shape, with the first peak coinciding with non-active stars and the second with the pre main-sequence cases. The catalogue will be publicly available with the next RAVE public data releases., Comment: 13 pages, 9 figures

Published
2013

7. Metallicity and Kinematics of Thick Disc Stars at Intermediate Galactic Latitudes

Author

Kordopatis, G., Recio-Blanco, A., de Laverny, P., Gilmore, G., Hill, V., Wyse, R. F. G., Helmi, A., Bijaoui, A., Zoccali, M., Bienaymé, O., Aoki, W., Ishigaki, M., Suda, T., Tsujimoto, T., Arimoto, N., and Astronomy

Subjects
Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Using the pipeline presented in Kordopatis et al. (2011a), we analysed 700 stellar spectra of targets towards intermediate galactic latitudes, in order to test the formation scenarios of the thick disc of the Milky Way. We found that the properties of the thick disc far from the solar neighbourhood are similar to the ones that have been measured locally by previous studies and that the thick disc is characterised by only one stellar population of constant scalelength and scaleheight, in contradiction with a thick disc mainly formed by radial migration mechanisms.

Published
2012

8. Kinematic groups beyond the Solar neighbourhood with RAVE

Author

Antoja, T., Helmi, A., Bienayme, O., Bland-Hawthorn, J., Famaey, B., Freeman, K., Gibson, B. K., Gilmore, G., Grebel, E. K., Minchev, I., Munari, U., Navarro, J., Parker, Q., Reid, W., Seabroke, G. M., Siebert, A., Siviero, A., Steinmetz, M., Williams, M., Wyse, R., Zwitter, T., Astronomy, and Kapteyn Astronomical Institute

Subjects
Galaxy: evolution, DATA RELEASE, solar neighbourhood, FOS: Physical sciences, DISC, Astrophysics - Astrophysics of Galaxies, BAR, GALACTIC STRUCTURE, HIPPARCOS, Astrophysics of Galaxies (astro-ph.GA), GIANTS, SPACE, STREAMS, Astrophysics::Earth and Planetary Astrophysics, VELOCITY EXPERIMENT RAVE, Galaxy: kinematics and dynamics, Galaxy: structure, NEARBY STARS, Astrophysics::Galaxy Astrophysics
Abstract

We analyse the kinematics of disc stars observed by the RAVE survey in and beyond the Solar neighbourhood.We detect significant overdensities in the velocity distributions using a technique based on the wavelet transform.We find that the main local kinematic groups are large scale features, surviving at least up to ~1 kpc from the Sun in the direction of anti-rotation, and also at ~700 pc below the Galactic plane.We also find that for regions located at different radii than the Sun, the known groups appear shifted in the velocity plane. For example, the Hercules group has a larger azimuthal velocity for regions inside the Solar circle and a lower value outside. We have also discovered a new group at (U, V) = (92,-22) km/s in the Solar neighbourhood and confirmed the significance of other previously found groups. Some of these trends detected for the first time are consistent with dynamical models of the effects of the bar and the spiral arms. More modelling is required to definitively characterise the non-axisymmetric components of our Galaxy using these groups., Minor changes to match the accepted version in MNRAS Letters

Published
2012

9. Probing the thick disc formation scenarios outside the solar neighbourhood

Author

Kordopatis, G., Recio-Blanco, A., de Laverny, P., Gilmore, G., Hill, V., Wyse, R. F. G., Helmi, A., Bijaoui, A., Ordenovic, C., Zoccali, M., Bienaymé, O., Alecian, G., Belkacem, K., Samadi, R., Valls-Gabaud, D., and Astronomy

Subjects
Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy: evolution -- Galaxy: kinematics and dynamics -- stars: abundances -- methods: observational, Astrophysics::Galaxy Astrophysics
Abstract

The origin and evolution of the Milky Way remains one of the key unanswered questions in astrophysics. From a sample of roughly 700 stars selected in order to probe the galactic thick disc outside the solar neighborhood, we investigate the radial scale length and scale height of this structure, based on the spectroscopic measurement of its star members. Estimations of the scale height and scale lengths for different metallicity bins result in consistent values, with HrValue and HzValue, showing no evidence of relics of destroyed massive satellites and challenging the radial migration mechanisms as being the most important processes of creation of the thick disc.

Published
2011

10. VizieR Online Data Catalog: Spectroscopic survey of 479 thick disc stars (Kordopatis+, 2011)

Author

Kordopatis, G., Recio-Blanco, A., de Laverny, P., Gilmore, G., Hill, V., Wyse, R. F. G., Helmi, A., Bijaoui, A., Ordenovic, C., Zoccali, M., Bienayme, O., and Kapteyn Astronomical Institute

Subjects
Photometry, Positional data, Space velocities, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Abundances, Stars: nearby, Effective temperatures
Abstract

These tables contain all the parameters that have been computed, based on the LR8 spectra of targets selected in order to investigate the galactic thick disc outside the solar neighbourhood. The atmospheric parameters and the signal-to-noise ratio (SNR) were computed using the pipeline presented in Kordopatis et al. (2011A&A...535A.106K). The line-of-sight distances were computed by projecting the atmospheric parameters on the Yonsei-Yale isochrones. The velocities and eccentricities were computed using the radial velocities derived by cross-correlation of the spectra with a synthetic mask, and using the proper motions of Ojha et al. (1996A&A...311..456O) No selection has been made on SNR in these tables. A value of -999.99 is meaning that the data for that star is not available (3 data files).

Published
2011

11. Characterization of the thick disc properties up to 8~kpc through a spectroscopic survey

Author

Kordopatis, G., Recio-Blanco, A., de Laverny, P., Gilmore, G., Hill, V., Wyse, R. F. G., Helmi, A., Bijaoui, A., Ordenovic, C., Zoccali, M., Bienaymé, O., Boissier, S., Heydari-Malayeri, M., Samadi, R., Valls-Gabaud, D., and Astronomy

Subjects
stars: abundances, galaxy: evolution, galaxy: kinematics and dynamics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, methods: observational, Astrophysics::Galaxy Astrophysics
Abstract

A spectroscopic survey of nearly 600 stars probing the Galactic Thick Disc far from the Solar neighbourhood is performed. The MATISSE (MATrix Inversion for Spectral SynthEsis) algorithm is developed and trained in order to automatically obtain the atmospheric parameters of the stars. The derived effective temperatures, surface gravities and overall metallicities are then combined to stellar evolution isochrones, radial velocities and proper motions to get the distances, kinematics and orbital parameters of the sample stars, up to 8 kpc. The Galactic components Thin and Thick discs and Halo are then characterized. The velocity ellipsoid for the old Thin Disc is found at (σ_u, σ_v, σ_w)= (39,27,20) km s-1 with a mean [M/H] ˜ -0.12~dex, whereas the Thick Disc has a mean [M/H] ˜ -0.4~dex and a rotational lag of V ˜-76 km s-1

Published
2010

12. Local Stellar Kinematics from RAVE Data: I. Local Standard of Rest

Author

Coskunoglu, B., Ak, S., Bilir, S., Karaali, S., Yaz, E., Gilmore, G., Seabroke, G. M., Bienayme, O., Bland-Hawthorn, J., Campbell, R., Freeman, K. C., Gibson, B., Grebel, E. K., Munari, U., Navarro, J. F., Parker, Q. A., Siebert, A., Siviero, A., Steinmetz, M., Watson, F. G., Wyse, R. F. G., and Zwitter, T.

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

We analyze a sample of 82850 stars from the RAVE survey, with well-determined velocities and stellar parameters, to isolate a sample of 18026 high-probability thin-disc dwarfs within 600 pc of the Sun. We derive space motions for these stars, and deduce the solar space velocity with respect to the Local Standard of Rest. The peculiar solar motion we derive is in excellent agreement in radial $U_{\odot}$ and vertical $W_{\odot}$ peculiar motions with other recent determinations. Our derived tangential peculiar velocity, $V_{\odot}$ agrees with very recent determinations, which favour values near 13 km s$^{-1}$, in disagreement with earlier studies. The derived values are not significantly dependent on the comparison sample chosen, or on the method of analysis. The local galaxy seems very well dynamically relaxed, in a near symmetric potential., Comment: 9 pages, including 9 figures and 3 tables, accepted for publication in MNRAS

Published
2010
Full Text
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13. Dwarf Elliptical Galaxies in the Perseus Cluster

Author

Gallagher, J. S., Conselice, C. J., Wyse, R. F. G., Wisconsin-Madison, U., and U, Johns Hopkins

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

Dwarf ellipticals have the lowest stellar densities of any galaxies, but paradoxically are most common in the densest regions of the universe, and are especially frequent in rich clusters of galaxies. Simple estimates suggest that low luminosity dwarf ellipticals should be subject to substantial tidal heating in rich clusters if most of their mass is in the form of normal stars. We have therefore undertaken a program to image dwarfs in clusters with the 3.5-m high performance WIYN, ARC and smaller, wide field telescopes. Our objectives include testing for evidence of tidal disruption in the form of asymmetries and searching for evidence of recent star formation which might be associated with the production of elliptical dwarfs from in-falling field galaxies., 2 pages, Will appear in proceedings of "Galaxy Dynamics: from the Early Universe to the Present", eds. F. Combes, G.A. Mamon, and V. Charmandaris

Published
1999

14. The Extreme Outer Regions of Disk Galaxies: Star Formation and Metal Abundances

Author

Ferguson, A. M. N., Wyse, R. F. G., and Gallagher, J. S.

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

The extreme outer regions of disk galaxies, lying at or beyond the classical optical radius defined by R25, present an opportunity to study star formation and chemical evolution under unique physical conditions, possibly reminscent of those which existed during the early stages of disk evolution. We present here some of the first results from a large study to measure star formation rates and metallicities in the extreme outer limits of a sample of nearby spiral galaxies. Despite their low gas column densities, massive star formation is often observed in these outer parts, but at an azimuthally--averaged rate much lower than that seen in the inner disk. Gas-phase O/H abundances of roughly 10% solar characterize the gas at 1.5--2 R25. The implications of our results for star formation `laws' and models of disk evolution are discussed., 9 pages, 3 embedded figures, 1 postscript file. To be published in "The Low Surface Brightness Universe", Proc. of IAU Coll. 171, edited by J.I. Davies, C. Impey and S. Phillips

Published
1998

15. 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.

16. VizieR Online Data Catalog: RAVE 3rd data release (Siebert+, 2011)

Author

Siebert, A., Williams, M., Siviero, A., Reid, W., Boeche, C., Steinmetz, M., Fulbright, J., Munari, U., Zwitter, T., Watson, F. G., Wyse, R. F. G., de Jong, R. S., Enke, H., Anguiano, B., Burton, D., Cass, C. J. P., Fiegert, K., Hartley, M., Ritter, A., Russel, K. S., Stupar, M., Bienayme, O., Freeman, K. C., Gilmore, G., Grebel, E. K., Helmi, A., Navarro, J. F., Binney, J., Bland-Hawthorn, J., Campbell, R., Famaey, B., Gerhard, O., Gibson, B. K., Matijevic, G., Parker, Q. A., Seabroke, G. M., Sharma, S., Smith, M. C., Wylie-de Boer, E., and Kapteyn Astronomical Institute

Subjects
Milky Way, Photometry, Radial velocities, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Stars: fundamental, Astrophysics::Galaxy Astrophysics
Abstract

Spectroscopic radial velocities for 83,072 stars in the Milky-Way southern hemisphere using the 6dF instrument at the AAO. Stellar parameters are published for a set of 39,833 stars belonging to the second and third years of observation. (1 data file).

17. RAVE DR2 distance catalogue (Breddels+, 2010)

Author

Breddels, M. A., Smith, M. C., Helmi, A., Bienayme, O., Binney, J., Bland-Hawthorn, J., Boeche, C., Burnett, B. C. M., Campbell, R., Freeman, K. C., Gibson, B., Gilmore, G., Grebel, E. K., Munari, U., Navarro, J. F., Parker, Q. A., Seabroke, G. M., Siebert, A., Siviero, A., Steinmetz, M., Watson, F. G., Williams, M., Wyse, R. F. G., Zwitter, T., and Astronomy

Subjects
Milky Way, Radial velocities, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Surveys, Stars: distances, Astrophysics::Galaxy Astrophysics
Abstract

We used stellar models combined with atmospheric properties from RAVE (effective temperature, surface gravity and metallicity) and (J-Ks) photometry from archival sources to derive absolute magnitudes. In combination with apparent magnitudes, sky coordinates, proper motions from a variety of sources and radial velocities from RAVE, we are able

18. RAVE 3rd data release (Siebert+, 2011)

Author

Siebert, A., Williams, M., Siviero, A., Reid, W., Boeche, C., Steinmetz, M., Fulbright, J., Munari, U., Zwitter, T., Watson, F. G., Wyse, R. F. G., de Jong, R.S., Enke, H., Anguiano, B., Burton, D., Cass, C. J. P., Fiegert, K., Hartley, M., Ritter, A., Russel, K. S., Stupar, M., Bienayme, O., Freeman, K. C., Gilmore, G., Grebel, E. K., Helmi, A., Navarro, J. F., Binney, J., Bland-Hawthorn, J., Campbell, R., Famaey, B., Gerhard, O., Gibson, B. K., Matijevic, G., Parker, Q. A., Seabroke, G. M., Sharma, S., Smith, M. C., Wylie-de Boer, E., and Astronomy

Subjects
Milky Way, Photometry, Radial velocities, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Stars: fundamental, Astrophysics::Galaxy Astrophysics
Abstract

Spectroscopic radial velocities for 83,072 stars in the Milky-Way southern hemisphere using the 6dF instrument at the AAO. Stellar parameters are published for a set of 39,833 stars belonging to the second and third years of observation.

19. SPACE: the spectroscopic all-sky cosmic explorer

Author

A. Cimatti, M. Robberto, C. Baugh, S. V. W. Beckwith, R. Content, E. Daddi, G. De Lucia, B. Garilli, L. Guzzo, G. Kauffmann, M. Lehnert, D. Maccagni, A. Martínez-Sansigre, F. Pasian, I. N. Reid, P. Rosati, R. Salvaterra, M. Stiavelli, Y. Wang, M. Zapatero Osorio, M. Balcells, M. Bersanelli, F. Bertoldi, J. Blaizot, D. Bottini, R. Bower, A. Bulgarelli, A. Burgasser, C. Burigana, R. C. Butler, S. Casertano, B. Ciardi, M. Cirasuolo, M. Clampin, S. Cole, A. Comastri, S. Cristiani, J.-G. Cuby, F. Cuttaia, A. De Rosa, A. Diaz Sanchez, M. Di Capua, J. Dunlop, X. Fan, A. Ferrara, F. Finelli, A. Franceschini, M. Franx, P. Franzetti, C. Frenk, Jonathan P. Gardner, F. Gianotti, R. Grange, C. Gruppioni, A. Gruppuso, F. Hammer, L. Hillenbrand, A. Jacobsen, M. Jarvis, R. Kennicutt, R. Kimble, M. Kriek, J. Kurk, J.-P. Kneib, O. Le Fevre, D. Macchetto, J. MacKenty, P. Madau, M. Magliocchetti, D. Maino, N. Mandolesi, N. Masetti, R. McLure, A. Mennella, M. Meyer, M. Mignoli, B. Mobasher, E. Molinari, G. Morgante, S. Morris, L. Nicastro, E. Oliva, P. Padovani, E. Palazzi, F. Paresce, A. Perez Garrido, E. Pian, L. Popa, M. Postman, L. Pozzetti, J. Rayner, R. Rebolo, A. Renzini, H. Röttgering, E. Schinnerer, M. Scodeggio, M. Saisse, T. Shanks, A. Shapley, R. Sharples, H. Shea, J. Silk, I. Smail, P. Spanó, J. Steinacker, L. Stringhetti, A. Szalay, L. Tresse, M. Trifoglio, M. Urry, L. Valenziano, F. Villa, I. Villo Perez, F. Walter, M. Ward, R. White, S. White, E. Wright, R. Wyse, G. Zamorani, A. Zacchei, W. W. Zeilinger, F. Zerbi, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Space Telescope Science Institute (STScI), Institute for Computational Cosmology, Department of Physics, Durham University, Durham (ICC), Centre for Advanced Instrumentation, Department of Physics, Durham University (CfAI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max-Planck-Institut für Astrophysik (MPA), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Brera, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-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), Max-Planck-Institut für Astronomie (MPIA), INAF-Osservatorio Astronomico di Trieste (INAF-OATs), European Southern Observatory (ESO), Università di Milano, University of Oklahoma, Instituto de Astrofísica de Canarias (IAC), Rheinische Friedrich-Wilhelms-Universität Bonn, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Bologna), Department of Earth Atmospheric and Planetary Sciences, MIT, The Royal Observatory (ROE), Goddard Space Flight Center, NASA, Astrophysics Science Division, INAF-Osservatorio Astronomico di Bologna (OABO), 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), Universidad Politecnica de Cartagena (UPCT), University of Maryland, University of Arizona, Scuola Internazionale Superiore di Studi Avanzati (SISSA), Università degli Studi di Padova = University of Padua (Unipd), University of Leiden, California Institute of Technology, Department of Astronomy (CALTECH), OpSys Project Consulting, University of Hertfordshire [Hatfield] (UH), Institute of Astronomy, University of Cambridge (IoA), Research and Scientific Support Department, ESA-ESTEC (RSSD), University of California, Santa Cruz (UCSC), Steward Observatory, University of Arizona, UC Riverside, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), University of Bucharest, Institute for Astronomy, University of Hawaii, INAF-Osservatorio Astronomico di Padova, Princeton, Ecole Polytechnique Fédérale de Lausanne (EPFL), University of Oxford, Johns Hopkins University (JHU), Yale University, University of California, Los Angeles (UCLA), University of Vienna, Cimatti A., Robberto M., Baugh C., Beckwith S. V. W., Content R., Daddi E., De Lucia G., Garilli B., Guzzo L., Kauffmann G., Lehnert M., Maccagni D., Martínez-Sansigre A., Pasian F., Reid I. N., Rosati P., Salvaterra R., Stiavelli M., Wang Y., Osorio M. Zapatero, Balcells M., Bersanelli M., Bertoldi F., Blaizot J., Bottini D., Bower R., Bulgarelli A., Burgasser A., Burigana C., Butler R. C., Casertano S., Ciardi B., Cirasuolo M., Clampin M., Cole S., Comastri A., Cristiani S., Cuby J.-G., Cuttaia F., de Rosa A., Sanchez A. Diaz, di Capua M., Dunlop J., Fan X., Ferrara A., Finelli F., Franceschini A., Franx M., Franzetti P., Frenk C., Gardner Jonathan P., Gianotti F., Grange R., Gruppioni C., Gruppuso A., Hammer F., Hillenbrand L., Jacobsen A., Jarvis M., Kennicutt R., Kimble R., Kriek M., Kurk J., Kneib J.-P., Le Fevre O., Macchetto D., MacKenty J., Madau P., Magliocchetti M., Maino D., Mandolesi N., Masetti N., McLure R., Mennella A., Meyer M., Mignoli M., Mobasher B., Molinari E., Morgante G., Morris S., Nicastro L., Oliva E., Padovani P., Palazzi E., Paresce F., Garrido A. Perez, Pian E., Popa L., Postman M., Pozzetti L., Rayner J., Rebolo R., Renzini A., Röttgering H., Schinnerer E., Scodeggio M., Saisse M., Shanks T., Shapley A., Sharples R., Shea H., Silk J., Smail I., Spanó P., Steinacker J., Stringhetti L., Szalay A., Tresse L., Trifoglio M., Urry M., Valenziano L., Villa F., Perez I. Villo, Walter F., Ward M., White R., White S., Wright E., Wyse R., Zamorani G., Zacchei A., Zeilinger W., Zerbi F., Cimatti, A., Robberto, M., Baugh, C., Beckwith, S. V. W., Content, R., Daddi, E., De, Lucia, G., Garilli, B., Guzzo, L., Kauffmann, Ferrara, Andrea, and 113, Coauthors

Subjects
Observational cosmology, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space (mathematics), law.invention, Telescope, law, Dark energy, Spectral resolution, media_common, Physics, COSMIC cancer database, Astronomical and space-research instrumentation, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Billion years, Galaxy, Redshift, Space and Planetary Science, Sky, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We describe the scientific motivations, the mission concept and the instrumentation of SPACE, a class-M mission proposed for concept study at the first call of the ESA Cosmic-Vision 2015-2025 planning cycle. SPACE aims to produce the largest three-dimensional evolutionary map of the Universe over the past 10 billion years by taking near-IR spectra and measuring redshifts for more than half a billion galaxies at 0, Comment: 27 pages, Experimental Astronomy, in press. The SPACE team complete list is available at http://urania.bo.astro.it/cimatti/space . The article with full resolution figures is available at http://urania.bo.astro.it/cimatti/space/publications.htm

Published
2008
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20. The Gaia-ESO Survey: the Galactic thick to thin disc transition

Author

Angela Bragaglia, Ulrike Heiter, Georges Kordopatis, R. D. Jeffries, L. Morbidelli, Emilio J. Alfaro, A. Hourihane, R. J. Jackson, Vardan Adibekyan, P. Joffre, Laura Magrini, Maria Bergemann, A. C. Lanzafame, Jack Lewis, L. Prinsinzano, R. F. G. Wyse, C. Allende Prieto, V. Hill, Enrico Maiorca, Martin Asplund, Amina Helmi, Rodolfo Smiljanic, P. de Laverny, G. G. Sacco, Clare Worley, Elena Pancino, Antonella Vallenari, M. T. Costado, Gerard Gilmore, Giuseppina Micela, Sergey E. Koposov, Andreas Korn, Alejandra Recio-Blanco, Thomas Bensby, Carmela Lardo, Ettore Flaccomio, Sofia Feltzing, Sofia Randich, Karin Lind, Recio-Blanco A., De Laverny P., Kordopatis G., Helmi A., Hill V., Gilmore G., Wyse R., Adibekyan V., Randich S., Asplund M., Feltzing S., Jeffries R., Micela G., Vallenari A., Alfaro E., Allende Prieto C., Bensby T., Bragaglia A., Flaccomio E., Koposov S.E., Korn A., Lanzafame A., Pancino E., Smiljanic R., Jackson R., Lewis J., Magrini L., Morbidelli L., Prisinzano L., Sacco G., Worley C.C., Hourihane A., Bergemann M., Costado M.T., Heiter U., Joffre P., Lardo C., Lind K., Maiorca E., and Astronomy

Subjects
stars: abundances, astro-ph.GA, Metallicity, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Galaxy: disk, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Orbital elements, education.field_of_study, Galaxy: stellar content, Number density, 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy: abundance, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy: abundances, Astrophysics::Earth and Planetary Astrophysics
Abstract

(Abridged) We have used the atmospheric parameters, [alpha/Fe] abundances and radial velocities, determined from the Gaia-ESO Survey GIRAFFE spectra of FGK-type stars (iDR1), to provide a chemo-kinematical characterisation of the disc stellar populations. We focuss on a subsample of 1016 stars with high quality parameters, covering the volume |Z, Accepted for publication in Astronomy and Astrophysics

Published
2014
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