Attenzione: i dati modificati non sono ancora stati salvati. Per confermare inserimenti o cancellazioni di voci è necessario confermare con il tasto SALVA/INSERISCI in fondo alla pagina
IRIS
This is a corrigendum to Gaia Collaboration (2018). It corrects errors in Appendix B, which describes the modelling of the Large and Small Magellanic Clouds (LMC and SMC). One of these errors also affects Fig. 18 of the paper, which shows the rotation curve and median radial motion in the LMC. No other results in the paper are affected. There should be no vector products in Appendix B, and everywhere a vector product appears should be a scalar product. This affects Eqs. (B.5), (B.8), (B.10), (B.12), (B.13), and (B.20). Equation (B.10), which defines one component of position within the plane of the galaxy, contains an additional typographical error, and it should have read (Farmula Presented) Equation (B.21) is incorrect. The factor of (ax + by + z) is applied to the wrong part of the equation. It should have read (Farmula Presented) This error affects the derived deprojected motions of stars in the LMC, and means that changes in the observational signature of the bulk motion away from the centre are not properly accounted for. The effect becomes more significant further from the centre. Figure 1 shows the resulting median tangential velocity, vT (the rotation curve), and median radial velocity vR as a function of de-projected radius R for the LMC, which is otherwise produced in the same way as before. The major differences between this and the equivalent figure in Gaia Collaboration (2018) are as follows The rotation curve reaches a greater velocity (~85 km s-1 versus ~75 km s-1) and remains flat beyond 6 kpc, as opposed to starting to fall. The difference in asymmetric drift for the blue and red populations is clearer the blue population, which is typically younger than the redder population, is rotating faster. The apparent outward motion of the stellar populations is much smaller. The blue population has almost no net radial motion, while the red population has one of .8 km s-1 (as opposed to ~20 km s-1). The difference in radial motion between the y < 0 and y > 0 populations is dramatically reduced, as is the difference between the value derived assuming the known line-of-sight bulk motion and the one derived leaving this value free.
Erratum: Gaia Data Release 2: The kinematics of globular clusters and dwarf galaxies around the Milky Way (Astronomy and Astrophysics (2018) 616 (A12) DOI: 10.1051/0004-6361/201832698)
Helmi A.;Van Leeuwen F.;McMillan P. J.;Massari D.;Antoja T.;Robin A. C.;Lindegren L.;Bastian U.;Arenou F.;Babusiaux C.;Biermann M.;Breddels M. A.;Hobbs D.;Jordi C.;Pancino E.;Reyle C.;Veljanoski J.;Brown A. G. A.;Vallenari A.;Prusti T.;De Bruijne J. H. J.;Bailer-Jones C. A. L.;Evans D. W.;Eyer L.;Jansen F.;Klioner S. A.;Lammers U.;Luri X.;Mignard F.;Panem C.;Pourbaix D.;Randich S.;Sartoretti P.;Siddiqui H. I.;Soubiran C.;Walton N. A.;Cropper M.;Drimmel R.;Katz D.;Lattanzi M. G.;Bakker J.;Cacciari C.;Castaneda J.;Chaoul L.;Cheek N.;De Angeli F.;Fabricius C.;Guerra R.;Holl B.;Masana E.;Messineo R.;Mowlavi N.;Nienartowicz K.;Panuzzo P.;Portell J.;Riello M.;Seabroke G. M.;Tanga P.;Thevenin F.;Gracia-Abril G.;Comoretto G.;Garcia-Reinaldos M.;Teyssier D.;Altmann M.;Andrae R.;Audard M.;Bellas-Velidis I.;Benson K.;Berthier J.;Blomme R.;Burgess P.;Busso G.;Carry B.;Cellino A.;Clementini G.;Clotet M.;Creevey O.;Davidson M.;De Ridder J.;Delchambre L.;Dell'Oro A.;Ducourant C.;Fernandez-Hernandez J.;Fouesneau M.;Fremat Y.;Galluccio L.;Garcia-Torres M.;Gonzalez-Nunez J.;Gonzalez-Vidal J. J.;Gosset E.;Guy L. P.;Halbwachs J. -L.;Hambly N. C.;Harrison D. L.;Hernandez J.;Hestroffer D.;Hodgkin S. T.;Hutton A.;Jasniewicz G.;Jean-Antoine-Piccolo A.;Jordan S.;Korn A. J.;Krone-Martins A.;Lanzafame A. C.;Lebzelter T.;Loffler W.;Manteiga M.;Marrese P. M.;Martin-Fleitas J. M.;Moitinho A.;Mora A.;Muinonen K.;Osinde J.;Pauwels T.;Petit J. -M.;Recio-Blanco A.;Richards P. J.;Rimoldini L.;Sarro L. M.;Siopis C.;Smith M.;Sozzetti A.;Suveges M.;Torra J.;Van Reeven W.;Abbas U.;Abreu Aramburu A.;Accart S.;Aerts C.;Altavilla G.;Alvarez M. A.;Alvarez R.;Alves J.;Anderson R. I.;Andrei A. H.;Anglada Varela E.;Antiche E.;Arcay B.;Astraatmadja T. L.;Bach N.;Baker S. G.;Balaguer-Nunez L.;Balm P.;Barache C.;Barata C.;Barbato D.;Barblan F.;Barklem P. S.;Barrado D.;Barros M.;Barstow M. A.;Bartholome Munoz S.;Bassilana J. -L.;Becciani U.;Bellazzini M.;Berihuete A.;Bertone S.;Bianchi L.;Bienayme O.;Blanco-Cuaresma S.;Boch T.;Boeche C.;Bombrun A.;Borrachero R.;Bossini D.;Bouquillon S.;Bourda G.;Bragaglia A.;Bramante L.;Bressan A.;Brouillet N.;Brusemeister T.;Brugaletta E.;Bucciarelli B.;Burlacu A.;Busonero D.;Butkevich A. G.;Buzzi R.;Caffau E.;Cancelliere R.;Cannizzaro G.;Cantat-Gaudin T.;Carballo R.;Carlucci T.;Carrasco J. M.;Casamiquela L.;Castellani M.;Castro-Ginard A.;Charlot P.;Chemin L.;Chiavassa A.;Cocozza G.;Costigan G.;Cowell S.;Crifo F.;Crosta M.;Crowley C.;Cuypers J.;Dafonte C.;Damerdji Y.;Dapergolas A.;David P.;David M.;De Laverny P.;De Luise F.;De March R.;De Martino D.;De Souza R.;De Torres A.;Debosscher J.;Del Pozo E.;Delbo M.;Delgado A.;Delgado H. E.;Di Matteo P.;Diakite S.;Diener C.;Distefano E.;Dolding C.;Drazinos P.;Duran J.;Edvardsson B.;Enke H.;Eriksson K.;Esquej P.;Eynard Bontemps G.;Fabre C.;Fabrizio M.;Faigler S.;Falcao A. J.;Farras Casas M.;Federici L.;Fedorets G.;Fernique P.;Figueras F.;Filippi F.;Findeisen K.;Fonti A.;Fraile E.;Fraser M.;Frezouls B.;Gai M.;Galleti S.;Garabato D.;Garcia-Sedano F.;Garofalo A.;Garralda N.;Gavel A.;Gavras P.;Gerssen J.;Geyer R.;Giacobbe P.;Gilmore G.;Girona S.;Giuffrida G.;Glass F.;Gomes M.;Granvik M.;Gueguen A.;Guerrier A.;Guiraud J.;Gutierrez-Sanchez R.;Haigron R.;Hatzidimitriou D.;Hauser M.;Haywood M.;Heiter U.;Heu J.;Hilger T.;Hofmann W.;Holland G.;Huckle H. E.;Hypki A.;Icardi V.;Janssen K.;Jevardat De Fombelle G.;Jonker P. G.;Juhasz A. L.;Julbe F.;Karampelas A.;Kewley A.;Klar J.;Kochoska A.;Kohley R.;Kolenberg K.;Kontizas M.;Kontizas E.;Koposov S. E.;Kordopatis G.;Kostrzewa-Rutkowska Z.;Koubsky P.;Lambert S.;Lanza A. F.;Lasne Y.;Lavigne J. -B.;Le Fustec Y.;Le Poncin-Lafitte C.;Lebreton Y.;Leccia S.;Leclerc N.;Lecoeur-Taibi I.;Lenhardt H.;Leroux F.;Liao S.;Licata E.;Lindstrom H. E. P.;Lister T. A.;Livanou E.;Lobel A.;Lopez M.;Managau S.;Mann R. G.;Mantelet G.;Marchal O.;Marchant J. M.;Marconi M.;Marinoni S.;Marschalko G.;Marshall D. J.;Martino M.;Marton G.;Mary N.;Matijevic G.;Mazeh T.;Messina S.;Michalik D.;Millar N. R.;Molina D.;Molinaro R.;Molnar L.;Montegriffo P.;Mor R.;Morbidelli R.;Morel T.;Morris D.;Mulone A. F.;Muraveva T.;Musella I.;Nelemans G.;Nicastro L.;Noval L.;O'Mullane W.;Ordenovic C.;Ordonez-Blanco D.;Osborne P.;Pagani C.;Pagano I.;Pailler F.;Palacin H.;Palaversa L.;Panahi A.;Pawlak M.;Piersimoni A. M.;Pineau F. -X.;Plachy E.;Plum G.;Poggio E.;Poujoulet E.;Prsa A.;Pulone L.;Racero E.;Ragaini S.;Rambaux N.;Ramos-Lerate M.;Regibo S.;Riclet F.;Ripepi V.;Riva A.;Rivard A.;Rixon G.;Roegiers T.;Roelens M.;Romero-Gomez M.;Rowell N.;Royer F.;Ruiz-Dern L.;Sadowski G.;Sagrista Selles T.;Sahlmann J.;Salgado J.;Salguero E.;Sanna N.;Santana-Ros T.;Sarasso M.;Savietto H.;Schultheis M.;Sciacca E.;Segol M.;Segovia J. C.;Segransan D.;Shih I. -C.;Siltala L.;Silva A. F.;Smart R. L.;Smith K. W.;Solano E.;Solitro F.;Sordo R.;Soria Nieto S.;Souchay J.;Spagna A.;Spoto F.;Stampa U.;Steele I. A.;Steidelmuller H.;Stephenson C. A.;Stoev H.;Suess F. F.;Surdej J.;Szabados L.;Szegedi-Elek E.;Tapiador D.;Taris F.;Tauran G.;Taylor M. B.;Teixeira R.;Terrett D.;Teyssandier P.;Thuillot W.;Titarenko A.;Torra Clotet F.;Turon C.;Ulla A.;Utrilla E.;Uzzi S.;Vaillant M.;Valentini G.;Valette V.;Van Elteren A.;Van Hemelryck E.;Van Leeuwen M.;Vaschetto M.;Vecchiato A.;Viala Y.;Vicente D.;Vogt S.;Von Essen C.;Voss H.;Votruba V.;Voutsinas S.;Walmsley G.;Weiler M.;Wertz O.;Wevers T.;Wyrzykowski L.;Yoldas A.;Zerjal M.;Ziaeepour H.;Zorec J.;Zschocke S.;Zucker S.;Zurbach C.;Zwitter T.
2020-01-01
Abstract
This is a corrigendum to Gaia Collaboration (2018). It corrects errors in Appendix B, which describes the modelling of the Large and Small Magellanic Clouds (LMC and SMC). One of these errors also affects Fig. 18 of the paper, which shows the rotation curve and median radial motion in the LMC. No other results in the paper are affected. There should be no vector products in Appendix B, and everywhere a vector product appears should be a scalar product. This affects Eqs. (B.5), (B.8), (B.10), (B.12), (B.13), and (B.20). Equation (B.10), which defines one component of position within the plane of the galaxy, contains an additional typographical error, and it should have read (Farmula Presented) Equation (B.21) is incorrect. The factor of (ax + by + z) is applied to the wrong part of the equation. It should have read (Farmula Presented) This error affects the derived deprojected motions of stars in the LMC, and means that changes in the observational signature of the bulk motion away from the centre are not properly accounted for. The effect becomes more significant further from the centre. Figure 1 shows the resulting median tangential velocity, vT (the rotation curve), and median radial velocity vR as a function of de-projected radius R for the LMC, which is otherwise produced in the same way as before. The major differences between this and the equivalent figure in Gaia Collaboration (2018) are as follows The rotation curve reaches a greater velocity (~85 km s-1 versus ~75 km s-1) and remains flat beyond 6 kpc, as opposed to starting to fall. The difference in asymmetric drift for the blue and red populations is clearer the blue population, which is typically younger than the redder population, is rotating faster. The apparent outward motion of the stellar populations is much smaller. The blue population has almost no net radial motion, while the red population has one of .8 km s-1 (as opposed to ~20 km s-1). The difference in radial motion between the y < 0 and y > 0 populations is dramatically reduced, as is the difference between the value derived assuming the known line-of-sight bulk motion and the one derived leaving this value free.
I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11769/523717
Citazioni
ND
3
4
social impact
Conferma cancellazione
Sei sicuro che questo prodotto debba essere cancellato?
simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.
