Is the sky falling? Searching for stellar streams in the local Milky Way disc in the CORAVEL and RAVE surveys
Identifieur interne : 003731 ( PascalFrancis/Corpus ); précédent : 003730; suivant : 003732Is the sky falling? Searching for stellar streams in the local Milky Way disc in the CORAVEL and RAVE surveys
Auteurs : G. M. Seabroke ; G. Gilmore ; A. Siebert ; O. Bienayme ; J. Binney ; J. Bland-Hawthorn ; R. Campbell ; K. C. Freeman ; B. Gibson ; E. K. Grebel ; A. Helmi ; U. Munari ; J. F. Navarro ; Q. A. Parker ; A. Siviero ; M. Steinmetz ; F. G. Watson ; R. F. G. Wyse ; T. Zwitter ; J. Penarrubia ; M. C. Smith ; M. WilliamsSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008.
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Abstract
We have searched for in-falling stellar streams on to the local Milky Way disc in the COR-relation RAdial VELocities (CORAVEL) and RAdial Velocity Experiment (RAVE) surveys. The CORAVEL survey consists of local dwarf stars (Nordstrom et al. Geneva-Copenhagen survey) and local Famaey et al. giant stars. We select RAVE stars with radial velocities that are sensitive to the Galactic vertical space velocity (Galactic latitude b < -45°). Kuiper statistics have been employed to test the symmetry of the Galactic vertical velocity distribution functions in these samples for evidence of a net vertical flow that could be associated with a (tidal?) stream of stars with vertically coherent kinematics. In contrast to the 'Field of Streams' found in the outer halo, we find that the local volumes of the solar neighbourhood sampled by the CORAVEL dwarfs (complete within ∼3 x 10-4 kpc3), CORAVEL giants (complete within ∼5 x 10-2 kpc3) and RAVE (5-15 per cent complete within ∼8 kpc3) are devoid of any vertically coherent streams containing hundreds of stars. This is sufficiently sensitive to allow our RAVE sample to rule out the passing of the tidal stream of the disrupting Sagittarius (Sgr) dwarf galaxy through the solar neighbourhood. This agrees with the most-recent determinations of its orbit and dissociates it from the Helmi et al. halo stream. Our constraints on the absence of the Sgr stream near the Sun could prove a useful tool for discriminating between Galactic potential models. The lack of a net vertical flow through the solar neighbourhood in the CORAVEL giants and RAVE samples argues against the Virgo overdensity crossing the disc near the Sun. There are no vertical streams in the CORAVEL giants and RAVE samples with stellar densities ≥1.6 x 104 and 1.5 x 103 stars kpc-3, respectively, and therefore no evidence for locally enhanced dark matter.
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| NO : | PASCAL 08-0114708 INIST |
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| ET : | Is the sky falling? Searching for stellar streams in the local Milky Way disc in the CORAVEL and RAVE surveys |
| AU : | SEABROKE (G. M.); GILMORE (G.); SIEBERT (A.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WYSE (R. F. G.); ZWITTER (T.); PENARRUBIA (J.); SMITH (M. C.); WILLIAMS (M.) |
| AF : | Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge CB3 OHA/Royaume-Uni (1 aut., 2 aut., 21 aut.); e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University/Uxbridge UB8 3PH/Royaume-Uni (1 aut.); Astrophysikalisches Institut Potsdam, An der Sterwarte 16/14482 Potsdam/Allemagne (3 aut., 16 aut.); Observatoire de Strasbourg, 11 Rue de L'Université/67000 Strasbourg/France (4 aut.); Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road/Oxford OX1 3NP/Royaume-Uni (5 aut.); Anglo-Australian Observatory, PO Box 296/Epping, NSW 1710/Australie (6 aut., 14 aut., 17 aut.); Macquarie University/Sydney, NSW 2109/Australie (7 aut., 14 aut.); RSAA, Mount Stromlo Observatory, Cotter Road, Weston Creek/Canberra, ACT 72611/Australie (8 aut., 22 aut.); University of Central Lancashire/Preston PR1 2HE/Royaume-Uni (9 aut.); Astronomisches Institut, Universitdt Basel, Venusstrasse 7/Binningen 4102/Suisse (10 aut.); Astronomisches Rechen-Institut, Zentrum für Astronomie der Universitdt Heidelberg, Mönchhofstr. 12-14/69120 Heidelberg/Allemagne (10 aut.); Kapteyn Astronomical Institute, University ofGroningen, PO Box 800/9700 AV Groningen/Pays-Bas (11 aut.); INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8/Asiago 36012/Italie (12 aut., 15 aut.); University of Victoria, PO Box 3055, Station CSC/Victoria, BC V8W3P6/Canada (13 aut., 20 aut.); Johns Hopkins University, 366 Bloomberg Centre, 3400 North Charles Street/Baltimore, MD 21218/Etats-Unis (18 aut.); Department of Physics, University of Ljubljana, Jadranska 19/Ljubljana/Slovénie (19 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2008; Vol. 384; No. 1; Pp. 11-32; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | We have searched for in-falling stellar streams on to the local Milky Way disc in the COR-relation RAdial VELocities (CORAVEL) and RAdial Velocity Experiment (RAVE) surveys. The CORAVEL survey consists of local dwarf stars (Nordstrom et al. Geneva-Copenhagen survey) and local Famaey et al. giant stars. We select RAVE stars with radial velocities that are sensitive to the Galactic vertical space velocity (Galactic latitude b < -45°). Kuiper statistics have been employed to test the symmetry of the Galactic vertical velocity distribution functions in these samples for evidence of a net vertical flow that could be associated with a (tidal?) stream of stars with vertically coherent kinematics. In contrast to the 'Field of Streams' found in the outer halo, we find that the local volumes of the solar neighbourhood sampled by the CORAVEL dwarfs (complete within ∼3 x 10-4 kpc3), CORAVEL giants (complete within ∼5 x 10-2 kpc3) and RAVE (5-15 per cent complete within ∼8 kpc3) are devoid of any vertically coherent streams containing hundreds of stars. This is sufficiently sensitive to allow our RAVE sample to rule out the passing of the tidal stream of the disrupting Sagittarius (Sgr) dwarf galaxy through the solar neighbourhood. This agrees with the most-recent determinations of its orbit and dissociates it from the Helmi et al. halo stream. Our constraints on the absence of the Sgr stream near the Sun could prove a useful tool for discriminating between Galactic potential models. The lack of a net vertical flow through the solar neighbourhood in the CORAVEL giants and RAVE samples argues against the Virgo overdensity crossing the disc near the Sun. There are no vertical streams in the CORAVEL giants and RAVE samples with stellar densities ≥1.6 x 104 and 1.5 x 103 stars kpc-3, respectively, and therefore no evidence for locally enhanced dark matter. |
| CC : | 001E03 |
| FD : | Disque galactique; Vitesse radiale; Etoile naine; Etoile géante; Espace vitesse; Répartition verticale; Fonction distribution vitesse; Cinématique; Voisinage solaire; Galaxies naines; Orbite; Soleil; Modèle; Matière sombre; Galaxies disques; Formation galaxies; Dynamique; Structure galaxies |
| ED : | Galactic disks; Radial velocity; Dwarf stars; Giant stars; Velocity space; Vertical distribution; Velocity distribution function; Kinematics; Solar neighborhood; Dwarf galaxies; Orbits; Sun; Models; Dark matter; Disk galaxies; Galaxy formation; Dynamics; Galaxy structure |
| SD : | Espacio velocidad; Distribución vertical; Función distribución velocidad; Vecindad solar; Modelo; Estructura galaxias |
| LO : | INIST-2067.354000161895330020 |
| ID : | 08-0114708 |
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Pascal:08-0114708Le document en format XML
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Grebel</name><affiliation><inist:fA14 i1="10"><s1>Astronomisches Institut, Universitdt Basel, Venusstrasse 7</s1><s2>Binningen 4102</s2><s3>CHE</s3><sZ>10 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="11"><s1>Astronomisches Rechen-Institut, Zentrum für Astronomie der Universitdt Heidelberg, Mönchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name><affiliation><inist:fA14 i1="12"><s1>Kapteyn Astronomical Institute, University ofGroningen, PO Box 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation><inist:fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>12 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name><affiliation><inist:fA14 i1="14"><s1>University of Victoria, PO Box 3055, Station CSC</s1><s2>Victoria, BC V8W3P6</s2><s3>CAN</s3><sZ>13 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><affiliation><inist:fA14 i1="06"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>14 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="07"><s1>Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><inist:fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>12 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>3 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation><inist:fA14 i1="06"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>14 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wyse, R F G" sort="Wyse, R F G" uniqKey="Wyse R" first="R. F. G." last="Wyse">R. F. G. Wyse</name><affiliation><inist:fA14 i1="15"><s1>Johns Hopkins University, 366 Bloomberg Centre, 3400 North Charles Street</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><inist:fA14 i1="16"><s1>Department of Physics, University of Ljubljana, Jadranska 19</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Penarrubia, J" sort="Penarrubia, J" uniqKey="Penarrubia J" first="J." last="Penarrubia">J. Penarrubia</name><affiliation><inist:fA14 i1="14"><s1>University of Victoria, PO Box 3055, Station CSC</s1><s2>Victoria, BC V8W3P6</s2><s3>CAN</s3><sZ>13 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Smith, M C" sort="Smith, M C" uniqKey="Smith M" first="M. C." last="Smith">M. C. Smith</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation><inist:fA14 i1="08"><s1>RSAA, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">08-0114708</idno><date when="2008">2008</date><idno type="stanalyst">PASCAL 08-0114708 INIST</idno><idno type="RBID">Pascal:08-0114708</idno><idno type="wicri:Area/PascalFrancis/Corpus">003731</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Is the sky falling? Searching for stellar streams in the local Milky Way disc in the CORAVEL and RAVE surveys</title><author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University</s1><s2>Uxbridge UB8 3PH</s2><s3>GBR</s3><sZ>1 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>3 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienayme">O. Bienayme</name><affiliation><inist:fA14 i1="04"><s1>Observatoire de Strasbourg, 11 Rue de L'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation><inist:fA14 i1="05"><s1>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road</s1><s2>Oxford OX1 3NP</s2><s3>GBR</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bland Hawthorn, J" sort="Bland Hawthorn, J" uniqKey="Bland Hawthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><affiliation><inist:fA14 i1="06"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>14 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name><affiliation><inist:fA14 i1="07"><s1>Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name><affiliation><inist:fA14 i1="08"><s1>RSAA, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibson, B" sort="Gibson, B" uniqKey="Gibson B" first="B." last="Gibson">B. Gibson</name><affiliation><inist:fA14 i1="09"><s1>University of Central Lancashire</s1><s2>Preston PR1 2HE</s2><s3>GBR</s3><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Grebel, E K" sort="Grebel, E K" uniqKey="Grebel E" first="E. K." last="Grebel">E. K. Grebel</name><affiliation><inist:fA14 i1="10"><s1>Astronomisches Institut, Universitdt Basel, Venusstrasse 7</s1><s2>Binningen 4102</s2><s3>CHE</s3><sZ>10 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="11"><s1>Astronomisches Rechen-Institut, Zentrum für Astronomie der Universitdt Heidelberg, Mönchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name><affiliation><inist:fA14 i1="12"><s1>Kapteyn Astronomical Institute, University ofGroningen, PO Box 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation><inist:fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>12 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name><affiliation><inist:fA14 i1="14"><s1>University of Victoria, PO Box 3055, Station CSC</s1><s2>Victoria, BC V8W3P6</s2><s3>CAN</s3><sZ>13 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><affiliation><inist:fA14 i1="06"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>14 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="07"><s1>Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><inist:fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>12 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>3 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation><inist:fA14 i1="06"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>14 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wyse, R F G" sort="Wyse, R F G" uniqKey="Wyse R" first="R. F. G." last="Wyse">R. F. G. Wyse</name><affiliation><inist:fA14 i1="15"><s1>Johns Hopkins University, 366 Bloomberg Centre, 3400 North Charles Street</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><inist:fA14 i1="16"><s1>Department of Physics, University of Ljubljana, Jadranska 19</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Penarrubia, J" sort="Penarrubia, J" uniqKey="Penarrubia J" first="J." last="Penarrubia">J. Penarrubia</name><affiliation><inist:fA14 i1="14"><s1>University of Victoria, PO Box 3055, Station CSC</s1><s2>Victoria, BC V8W3P6</s2><s3>CAN</s3><sZ>13 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Smith, M C" sort="Smith, M C" uniqKey="Smith M" first="M. C." last="Smith">M. C. Smith</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation><inist:fA14 i1="08"><s1>RSAA, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2008">2008</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Dark matter</term><term>Disk galaxies</term><term>Dwarf galaxies</term><term>Dwarf stars</term><term>Dynamics</term><term>Galactic disks</term><term>Galaxy formation</term><term>Galaxy structure</term><term>Giant stars</term><term>Kinematics</term><term>Models</term><term>Orbits</term><term>Radial velocity</term><term>Solar neighborhood</term><term>Sun</term><term>Velocity distribution function</term><term>Velocity space</term><term>Vertical distribution</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Disque galactique</term><term>Vitesse radiale</term><term>Etoile naine</term><term>Etoile géante</term><term>Espace vitesse</term><term>Répartition verticale</term><term>Fonction distribution vitesse</term><term>Cinématique</term><term>Voisinage solaire</term><term>Galaxies naines</term><term>Orbite</term><term>Soleil</term><term>Modèle</term><term>Matière sombre</term><term>Galaxies disques</term><term>Formation galaxies</term><term>Dynamique</term><term>Structure galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have searched for in-falling stellar streams on to the local Milky Way disc in the COR-relation RAdial VELocities (CORAVEL) and RAdial Velocity Experiment (RAVE) surveys. The CORAVEL survey consists of local dwarf stars (Nordstrom et al. Geneva-Copenhagen survey) and local Famaey et al. giant stars. We select RAVE stars with radial velocities that are sensitive to the Galactic vertical space velocity (Galactic latitude b < -45°). Kuiper statistics have been employed to test the symmetry of the Galactic vertical velocity distribution functions in these samples for evidence of a net vertical flow that could be associated with a (tidal?) stream of stars with vertically coherent kinematics. In contrast to the 'Field of Streams' found in the outer halo, we find that the local volumes of the solar neighbourhood sampled by the CORAVEL dwarfs (complete within ∼3 x 10<sup>-4</sup> kpc<sup>3</sup>), CORAVEL giants (complete within ∼5 x 10<sup>-2</sup> kpc<sup>3</sup>) and RAVE (5-15 per cent complete within ∼8 kpc<sup>3</sup>) are devoid of any vertically coherent streams containing hundreds of stars. This is sufficiently sensitive to allow our RAVE sample to rule out the passing of the tidal stream of the disrupting Sagittarius (Sgr) dwarf galaxy through the solar neighbourhood. This agrees with the most-recent determinations of its orbit and dissociates it from the Helmi et al. halo stream. Our constraints on the absence of the Sgr stream near the Sun could prove a useful tool for discriminating between Galactic potential models. The lack of a net vertical flow through the solar neighbourhood in the CORAVEL giants and RAVE samples argues against the Virgo overdensity crossing the disc near the Sun. There are no vertical streams in the CORAVEL giants and RAVE samples with stellar densities ≥1.6 x 10<sup>4</sup> and 1.5 x 10<sup>3</sup> stars kpc<sup>-3</sup>, respectively, and therefore no evidence for locally enhanced dark matter.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>384</s2></fA05><fA06><s2>1</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Is the sky falling? Searching for stellar streams in the local Milky Way disc in the CORAVEL and RAVE surveys</s1></fA08><fA11 i1="01" i2="1"><s1>SEABROKE (G. M.)</s1></fA11><fA11 i1="02" i2="1"><s1>GILMORE (G.)</s1></fA11><fA11 i1="03" i2="1"><s1>SIEBERT (A.)</s1></fA11><fA11 i1="04" i2="1"><s1>BIENAYME (O.)</s1></fA11><fA11 i1="05" i2="1"><s1>BINNEY (J.)</s1></fA11><fA11 i1="06" i2="1"><s1>BLAND-HAWTHORN (J.)</s1></fA11><fA11 i1="07" i2="1"><s1>CAMPBELL (R.)</s1></fA11><fA11 i1="08" i2="1"><s1>FREEMAN (K. C.)</s1></fA11><fA11 i1="09" i2="1"><s1>GIBSON (B.)</s1></fA11><fA11 i1="10" i2="1"><s1>GREBEL (E. K.)</s1></fA11><fA11 i1="11" i2="1"><s1>HELMI (A.)</s1></fA11><fA11 i1="12" i2="1"><s1>MUNARI (U.)</s1></fA11><fA11 i1="13" i2="1"><s1>NAVARRO (J. F.)</s1></fA11><fA11 i1="14" i2="1"><s1>PARKER (Q. A.)</s1></fA11><fA11 i1="15" i2="1"><s1>SIVIERO (A.)</s1></fA11><fA11 i1="16" i2="1"><s1>STEINMETZ (M.)</s1></fA11><fA11 i1="17" i2="1"><s1>WATSON (F. G.)</s1></fA11><fA11 i1="18" i2="1"><s1>WYSE (R. F. G.)</s1></fA11><fA11 i1="19" i2="1"><s1>ZWITTER (T.)</s1></fA11><fA11 i1="20" i2="1"><s1>PENARRUBIA (J.)</s1></fA11><fA11 i1="21" i2="1"><s1>SMITH (M. C.)</s1></fA11><fA11 i1="22" i2="1"><s1>WILLIAMS (M.)</s1></fA11><fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>21 aut.</sZ></fA14><fA14 i1="02"><s1>e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University</s1><s2>Uxbridge UB8 3PH</s2><s3>GBR</s3><sZ>1 aut.</sZ></fA14><fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>3 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="04"><s1>Observatoire de Strasbourg, 11 Rue de L'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road</s1><s2>Oxford OX1 3NP</s2><s3>GBR</s3><sZ>5 aut.</sZ></fA14><fA14 i1="06"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>14 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="07"><s1>Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ></fA14><fA14 i1="08"><s1>RSAA, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>22 aut.</sZ></fA14><fA14 i1="09"><s1>University of Central Lancashire</s1><s2>Preston PR1 2HE</s2><s3>GBR</s3><sZ>9 aut.</sZ></fA14><fA14 i1="10"><s1>Astronomisches Institut, Universitdt Basel, Venusstrasse 7</s1><s2>Binningen 4102</s2><s3>CHE</s3><sZ>10 aut.</sZ></fA14><fA14 i1="11"><s1>Astronomisches Rechen-Institut, Zentrum für Astronomie der Universitdt Heidelberg, Mönchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>10 aut.</sZ></fA14><fA14 i1="12"><s1>Kapteyn Astronomical Institute, University ofGroningen, PO Box 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>11 aut.</sZ></fA14><fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>12 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="14"><s1>University of Victoria, PO Box 3055, Station CSC</s1><s2>Victoria, BC V8W3P6</s2><s3>CAN</s3><sZ>13 aut.</sZ><sZ>20 aut.</sZ></fA14><fA14 i1="15"><s1>Johns Hopkins University, 366 Bloomberg Centre, 3400 North Charles Street</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>18 aut.</sZ></fA14><fA14 i1="16"><s1>Department of Physics, University of Ljubljana, Jadranska 19</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>19 aut.</sZ></fA14><fA20><s1>11-32</s1></fA20><fA21><s1>2008</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000161895330020</s5></fA43><fA44><s0>0000</s0><s1>© 2008 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>08-0114708</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We have searched for in-falling stellar streams on to the local Milky Way disc in the COR-relation RAdial VELocities (CORAVEL) and RAdial Velocity Experiment (RAVE) surveys. The CORAVEL survey consists of local dwarf stars (Nordstrom et al. Geneva-Copenhagen survey) and local Famaey et al. giant stars. We select RAVE stars with radial velocities that are sensitive to the Galactic vertical space velocity (Galactic latitude b < -45°). Kuiper statistics have been employed to test the symmetry of the Galactic vertical velocity distribution functions in these samples for evidence of a net vertical flow that could be associated with a (tidal?) stream of stars with vertically coherent kinematics. In contrast to the 'Field of Streams' found in the outer halo, we find that the local volumes of the solar neighbourhood sampled by the CORAVEL dwarfs (complete within ∼3 x 10<sup>-4</sup> kpc<sup>3</sup>), CORAVEL giants (complete within ∼5 x 10<sup>-2</sup> kpc<sup>3</sup>) and RAVE (5-15 per cent complete within ∼8 kpc<sup>3</sup>) are devoid of any vertically coherent streams containing hundreds of stars. This is sufficiently sensitive to allow our RAVE sample to rule out the passing of the tidal stream of the disrupting Sagittarius (Sgr) dwarf galaxy through the solar neighbourhood. This agrees with the most-recent determinations of its orbit and dissociates it from the Helmi et al. halo stream. Our constraints on the absence of the Sgr stream near the Sun could prove a useful tool for discriminating between Galactic potential models. The lack of a net vertical flow through the solar neighbourhood in the CORAVEL giants and RAVE samples argues against the Virgo overdensity crossing the disc near the Sun. There are no vertical streams in the CORAVEL giants and RAVE samples with stellar densities ≥1.6 x 10<sup>4</sup> and 1.5 x 10<sup>3</sup> stars kpc<sup>-3</sup>, respectively, and therefore no evidence for locally enhanced dark matter.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Disque galactique</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Galactic disks</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Vitesse radiale</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Radial velocity</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Etoile naine</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Dwarf stars</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Etoile géante</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Giant stars</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Espace vitesse</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Velocity space</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Espacio velocidad</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Répartition verticale</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Vertical distribution</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Distribución vertical</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Fonction distribution vitesse</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Velocity distribution function</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Función distribución velocidad</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Cinématique</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Kinematics</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Voisinage solaire</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Solar neighborhood</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Vecindad solar</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Galaxies naines</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Dwarf galaxies</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Orbite</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Orbits</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Soleil</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Sun</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Modèle</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Models</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Modelo</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Matière sombre</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Dark matter</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Galaxies disques</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Disk galaxies</s0><s5>40</s5></fC03><fC03 i1="16" i2="3" l="FRE"><s0>Formation galaxies</s0><s5>41</s5></fC03><fC03 i1="16" i2="3" l="ENG"><s0>Galaxy formation</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Dynamique</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>Dynamics</s0><s5>42</s5></fC03><fC03 i1="18" i2="X" l="FRE"><s0>Structure galaxies</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="ENG"><s0>Galaxy structure</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="SPA"><s0>Estructura galaxias</s0><s5>43</s5></fC03><fN21><s1>063</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 08-0114708 INIST</NO><ET>Is the sky falling? Searching for stellar streams in the local Milky Way disc in the CORAVEL and RAVE surveys</ET><AU>SEABROKE (G. M.); GILMORE (G.); SIEBERT (A.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WYSE (R. F. G.); ZWITTER (T.); PENARRUBIA (J.); SMITH (M. C.); WILLIAMS (M.)</AU><AF>Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge CB3 OHA/Royaume-Uni (1 aut., 2 aut., 21 aut.); e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University/Uxbridge UB8 3PH/Royaume-Uni (1 aut.); Astrophysikalisches Institut Potsdam, An der Sterwarte 16/14482 Potsdam/Allemagne (3 aut., 16 aut.); Observatoire de Strasbourg, 11 Rue de L'Université/67000 Strasbourg/France (4 aut.); Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road/Oxford OX1 3NP/Royaume-Uni (5 aut.); Anglo-Australian Observatory, PO Box 296/Epping, NSW 1710/Australie (6 aut., 14 aut., 17 aut.); Macquarie University/Sydney, NSW 2109/Australie (7 aut., 14 aut.); RSAA, Mount Stromlo Observatory, Cotter Road, Weston Creek/Canberra, ACT 72611/Australie (8 aut., 22 aut.); University of Central Lancashire/Preston PR1 2HE/Royaume-Uni (9 aut.); Astronomisches Institut, Universitdt Basel, Venusstrasse 7/Binningen 4102/Suisse (10 aut.); Astronomisches Rechen-Institut, Zentrum für Astronomie der Universitdt Heidelberg, Mönchhofstr. 12-14/69120 Heidelberg/Allemagne (10 aut.); Kapteyn Astronomical Institute, University ofGroningen, PO Box 800/9700 AV Groningen/Pays-Bas (11 aut.); INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8/Asiago 36012/Italie (12 aut., 15 aut.); University of Victoria, PO Box 3055, Station CSC/Victoria, BC V8W3P6/Canada (13 aut., 20 aut.); Johns Hopkins University, 366 Bloomberg Centre, 3400 North Charles Street/Baltimore, MD 21218/Etats-Unis (18 aut.); Department of Physics, University of Ljubljana, Jadranska 19/Ljubljana/Slovénie (19 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2008; Vol. 384; No. 1; Pp. 11-32; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>We have searched for in-falling stellar streams on to the local Milky Way disc in the COR-relation RAdial VELocities (CORAVEL) and RAdial Velocity Experiment (RAVE) surveys. The CORAVEL survey consists of local dwarf stars (Nordstrom et al. Geneva-Copenhagen survey) and local Famaey et al. giant stars. We select RAVE stars with radial velocities that are sensitive to the Galactic vertical space velocity (Galactic latitude b < -45°). Kuiper statistics have been employed to test the symmetry of the Galactic vertical velocity distribution functions in these samples for evidence of a net vertical flow that could be associated with a (tidal?) stream of stars with vertically coherent kinematics. In contrast to the 'Field of Streams' found in the outer halo, we find that the local volumes of the solar neighbourhood sampled by the CORAVEL dwarfs (complete within ∼3 x 10<sup>-4</sup> kpc<sup>3</sup>), CORAVEL giants (complete within ∼5 x 10<sup>-2</sup> kpc<sup>3</sup>) and RAVE (5-15 per cent complete within ∼8 kpc<sup>3</sup>) are devoid of any vertically coherent streams containing hundreds of stars. This is sufficiently sensitive to allow our RAVE sample to rule out the passing of the tidal stream of the disrupting Sagittarius (Sgr) dwarf galaxy through the solar neighbourhood. This agrees with the most-recent determinations of its orbit and dissociates it from the Helmi et al. halo stream. Our constraints on the absence of the Sgr stream near the Sun could prove a useful tool for discriminating between Galactic potential models. The lack of a net vertical flow through the solar neighbourhood in the CORAVEL giants and RAVE samples argues against the Virgo overdensity crossing the disc near the Sun. There are no vertical streams in the CORAVEL giants and RAVE samples with stellar densities ≥1.6 x 10<sup>4</sup> and 1.5 x 10<sup>3</sup> stars kpc<sup>-3</sup>, respectively, and therefore no evidence for locally enhanced dark matter.</EA><CC>001E03</CC><FD>Disque galactique; Vitesse radiale; Etoile naine; Etoile géante; Espace vitesse; Répartition verticale; Fonction distribution vitesse; Cinématique; Voisinage solaire; Galaxies naines; Orbite; Soleil; Modèle; Matière sombre; Galaxies disques; Formation galaxies; Dynamique; Structure galaxies</FD><ED>Galactic disks; Radial velocity; Dwarf stars; Giant stars; Velocity space; Vertical distribution; Velocity distribution function; Kinematics; Solar neighborhood; Dwarf galaxies; Orbits; Sun; Models; Dark matter; Disk galaxies; Galaxy formation; Dynamics; Galaxy structure</ED><SD>Espacio velocidad; Distribución vertical; Función distribución velocidad; Vecindad solar; Modelo; Estructura galaxias</SD><LO>INIST-2067.354000161895330020</LO><ID>08-0114708</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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