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La Vierge 1 La Vierge (Vir = Virgo) Nom distance magnitude type remarques (al) spectral ααα ou Spica ou l’épi ou Azimech 270 0,98 à 1,3 B2III Ts= 20 000K, var. à éclipse La Vierge 2 βββ ou Alaraph ou Zavijava 31 3,8 F8IV γγγ ou Arich ou Porrima 38 2,74 et 3 F0IV et Binaire à 4,6" (diminue) F0 δδδ ou Minelauva ou Auva 200 3,39 M0II εεε ou Vindémiatrix 100 2,85 K0III ζζζ ou Heze 72 3,38 A2IV ηηη ou Zaniah 204 4 A0V ιιι ou Syrma 76 4,2 F5III µµµ ou Rijl al Auwa 72 3,9 F5III ννν 233 4,2 M0III τττ 136 4,3 A2IV θθθ 125 4,4 et 4,8 A2 Binaire à 7,2 ‘’ 70 72 5,0 G2V possède 1 planète extrasolaire b: m=7,44MJup. p=117j.d=0,48ua HD106252 122 7,36 G0 possède 1 planète extrasolaire b :m=6,8MJup. p=1500j.d=2,61ua HD114783 72 7,57 K0 possède 1 planète extrasolaire b: m=0,99MJup. p=501j.d=1,2ua HD 130322 99 8,05 K0V possède 1 planète extrasolaire b: m=1,1MJup. p=11j. d=0;088ua HD 102195 93 8,05 K0V possède 1 planète extrasolaire b: m=0,48MJup. p=4j. d=0;049ua Objet Distance (al) magnitude remarques M49(NGC4472) 48,2 millions 9,3 galaxie E4 (3' X2'), découverte par: Messier en 1771, diamètre réel: 50 000al, masse : 5 fois la Galaxie M58 (NGC4579) 66,8 millions 10,6 galaxie SBb (5'X4'), découverte par: Messier en 1779, diamètre réel: 50000al, 160 milliards de masses solaires M59 (NGC4621) 60 millions 10,8 galaxie E3 (2'7X2'8) , découverte par: J.G.Koehler en 1779, vitesse d'éloignement: 350km/s, diamètre réel: 24 000al,masse : 250 milliards de masses solaires. M60 (NGC4649) 60 millions 9,8 galaxie E1 (2'X2') ,découverte par: J.G.Koehler en 1779,vitesse d'éloignement: 350km/s, diamètre réel: 25 000al, masse : 5 X la Galaxie. M61(NGC4303) 60 millions 10,2 galaxie Sc (5'6X5'3), découverte par: Abbé Oriani en 1779, diamètre réel: 60 000al, M84 (NGC4374) 51,2 millions 10,3 galaxie S0(2'X2'),diamètre réel: 25 000al, découverte en 1781 par Charles Messier. Début de la "chaîne de Markarian" (voir la carte) M86(NGC4406) 60 millions 10,1 galaxie Eed (1,5'X1,2'), découverte par: J.G.Koehler en 1779, vitesse de rapprochement: 450km/s, diamètre réel: 25 000al. M87(NGC4486) 60 millions 9,6 galaxie EOp (2'X2'), découverte par: Messier en mars 1781, diamètre réel: 24 000al propriétés: puissante source radio (3C274) provenant d'un immense jet de matière. Elle renfermerait un trou noir massif. La Vierge 3 M89 (NGC4552) 60 millions 10,6 galaxieSO (1'3X1'3), découverte par: Messier en 1781, masse : 250 milliards de masses solaires. M90 (NGC4569) 71,4 millions 10,2 galaxie Sb (7'5X2'2)découverte par : Messier en 1781, masse : 80milliards de masses solaires M104 (NGC4594) 45 millions 9,3 galaxie "Sombrero"Sa/Sb (6'X2'5), découverte par: Méchain en mai 1781, vitesse d'éloignement: 1150km/s, diamètre réel: 130 000al, masse : 250milliards de m. sol. NGC4608 11 galaxie SB0(3,3’ X2,9’) NGC4216 70 millions 11,0 galaxie SBb (8,3’ X2,2’) NGC4365 63,6 millions 10,5 galaxie E3 (6,2' X 4,6') NGC4435 60 millions 11,8 galaxie E4/SB0 (3’X2’) NGC4438 63,6 millions 10,9 galaxie S0/Sa (9,3'X4') NGC4461 59 millions 12 ou 11,2 galaxie SB0/Sa (3,7’X1,5’) NGC4478 63,6 millions 12,1 galaxie E2(2,4'X2,1') NGC4526 71,4 millions 10,6 galaxie E7/So (7,2' X2,3') NGC4564 11,1 galaxie E6 (3,2' X1,8') NGC4567 52milions 10,8 les jumelles : galaxie SA(3,1’X2,2’) et NGC4568 52milions 11,3 galaxie SA(3,1’X2,2’) NGC4596 10,4 galaxie SBa (4’X3,4’) NGC4636 50 millions 9,5 galaxieE (5,9'x4,6') un trou noir central. NGC4643 10,8 galaxie SB (3,1'X2,5') elle ressemble à Saturne NGC4638 11,3 galaxie E-S0 (2,8'X2,8') NGC4660 60 millions 11,9 galaxie E5 (3'X2') NGC4665 =NGC4624 10,5 galaxie (3,5'X3,5') NGC4697 9,2 galaxieE (6,2'X4,5') NGC4699 39,1 millions 10,5 galaxie Sb (3'X2') NGC4753 9,9 galaxie (8,6'X2') NGC4754 55millions 11,3 galaxie SB(r)0 ( 4.5 x 2.4') NGC4762 55millions 10,3 galaxie SO (5,1'X2,6') NGC5363 17 millions 11,2 galaxieSa (2'X1') NGC5566 49,2 millions 11,4 galaxie Sba (6'X1') NGC5634 4900 11 amas globulaire (d=1,4') NGC5746 95 millions 10,3 galaxie Sb (6,9'X1,2') NGC5846 10 galaxie E (4,0'X3,7') NGC5838 10,9 galaxie E-S0 (3,7'X1,6') 3C273, Cambridge en 3milliards 13 Quasar (d=1"), vitesse d'éloignement: 50 millions de 1959, km/s, présence d'un jet de matière. La Vierge 4 A partir de Vindémiatrix ( εεε), au T406mm Dans le même champ : au 24mm (78X), NGC 4762 une galaxie bien vue par la tranche sous un arc de 3 étoiles; et NGC 4754 bien vue de face alignée avec 2 étoiles. Non loin de là, dans le même champ 3 galaxies M 60 la galaxie plus brillante et ronde NGC 4638 au-dessus, assez faible, M 59 plus à gauche, un peu plus loin, NGC 4660 au dessus difficile très petite. Elle se trouve placée au milieu entre 2 groupes d'étoiles. Il faut la vision décalée pour bien l'apercevoir. M 58 plus brillante et ronde proche d'une étoile Près de 4 étoiles en forme de petit bélier NGC 4567 et NGC4568 ronde et faible (je n'ai pas séparé les 2 jumelles) NGC 4564 faible et vue par la tranche M89 et M90: ces 2 galaxies ne sont pas dans le même champ du chercheur Au T200mm, dans le champ du 26mm (77X), on voit un alignement d'étoiles et M87 se trouve dans cet alignement. NGC4478 se trouve à gauche de M87 Un bel alignement de galaxies : M84, M86, NGC4435 et NGC4438 : la Chaîne de Markarian On voit très nettement 3 galaxies pratiquement alignées, la 3ème étant double. M84 puis M86 puis côte à côte NGC4435 et NGC4438 NGC4461 en suivant encore l'alignement ,on la voit assez brillante Il y a encore NGC4473 puis NGC4477 qui sont dans la Chevelure de Bérénice. Plus loin à gauche, NGC4216. Elle montre sa tranche illuminée par un noyau brillant. Repartir de Vindemiatrix et se diriger vers rho ( ρ) Vierge Tout près : NGC 4608 et dans le même champ un peu plus loin , NGC 4596 , il faut bien regarder pour les voir au T200 plus visible au T406 La Vierge 5 Repartir de Vindemiatrix et se diriger vers une petite couronne d'étoiles NGC4526 . Facile à trouver, elle est coincée entre 2 étoiles qui appartiennent à une couronne d'étoiles brillantes près d' ε-Vierge. Belle image au 26mm. M49 est toute proche. M49 . Il faut la rechercher entre 2 étoiles, visibles dans le chercheur. La galaxie est bien visible au 26 mmVoir la description au-dessus. NGC4365 est assez difficile à voir au T200 car c'est une galaxie vue par dessus. Il faut être sûr d'être au bon endroit pour l'apercevoir. Située non loin de NGC4526, il faut partir de l'étoile brillante à gauche de cette galaxie puis au 26mm trouver 2 couples d'étoiles doubles et poursuivre de la même distance. Elle est sous une étoile. A partir de 109 Vierge NGC 5746 faible, sortir 109 du champ NGC 5846 bien visible et ronde NGC 5838, vue près d'une étoile brillante A partir de mu (µ) NGC5634 Elle se voit très bien, près d’une étoile. La Vierge 6 A partir de zèta ( ζζζ) NGC5363 est proche d'une étoile assez brillante. NGC5566 , dans les environs de τ -Vierge, proche d'un étoile double. Il faut la sortir du champ pour bien voir la galaxie en vision décalée au T200 A partir de l'Epi ( ααα) M104 : L a galaxie Sombrero. Magnifique, sa forme caractéristique est bien reconnaissable. NGC4699 Repérée facilement, elle semble d'abord un point brillant mais avec plus d'attention on voit bien que c'est une galaxie. La Vierge 7 A partir de Porrima ( γγγ) NGC4636 bien observée. NGC4665 bien évidente en vision décalée près d'une étoile NGC4643 petite mais brillante au 26mm. NGC4753 bien vue NGC4697 bien vue. M61 Elle aussi est située entre 2 étoiles. La recherche est facile. La galaxie est bien visible. .
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  • A New Neptune-Mass Planet Orbiting HD 219828

    A New Neptune-Mass Planet Orbiting HD 219828

    A&A 467, 721–727 (2007) Astronomy DOI: 10.1051/0004-6361:20066845 & c ESO 2007 Astrophysics A new Neptune-mass planet orbiting HD 219828 C. Melo1,N.C.Santos2,3,4,W.Gieren5, G. Pietrzynski5,M.T.Ruiz6,S.G.Sousa2,7,8, F. Bouchy9,C.Lovis3, M. Mayor3,F.Pepe3,D.Queloz3, R. da Silva3,andS.Udry3 1 European Southern Observatory, Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal 3 Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 4 Centro de Geofisica de Évora, Rua Romão Ramalho 59, 7002-554 Évora, Portugal 5 Universidad de Concepcion, Departamento de Fisica, Casilla 160-C, Concepcion, Chile 6 Departamento de Astronomia, Universidad de Chile, Casilla Postal 36D, Santiago, Chile 7 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 8 Departamento de Matemática Aplicada, Faculdade de Ciências da Universidade do Porto, Portugal 9 Institut d’Astrophysique de Paris, 98bis Bd. Arago, 75014 Paris, France Received 30 November 2006 / Accepted 28 January 2007 ABSTRACT Two years ago a new benchmark for the planetary survey was set with the discoveries of three extrasolar planets with masses be- low 20 M⊕. In particular, the serendipitous discovery of the 14 M⊕ planet around µ Ara found with HARPS with a semi-amplitude of only 4 m s−1 put in evidence the tremendous potential of HARPS for the search of this class of very low-mass planets.