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The potential of the VLTI for studying novae

Olivier CHESNEAU Observatoire de la Côte d’Azur, Département Gemini N. Nardetto (OCA), F. Millour (LUAN), C. Hummel (ESO), M. Vannier (ESO), F Rantakyro (ESO) F. Malbet (LAOG), A. Spang (OCA), D. Bonneau (OCA), A. Domiciano,(LUAN) ,D. Mourard (OCA),

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The potential of the VLTI for studying novae

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  1. Olivier CHESNEAU Observatoire de la Côte d’Azur, Département Gemini N. Nardetto (OCA), F. Millour (LUAN), C. Hummel (ESO), M. Vannier (ESO), F Rantakyro (ESO) F. Malbet (LAOG), A. Spang (OCA), D. Bonneau (OCA), A. Domiciano,(LUAN) ,D. Mourard (OCA), R. Petrov (LUAN), Ph. Stee (OCA), F. Vakili (LUAN) M.F. Bode (Liveropoll), T. O’Brien (Jodrell Bank), G. Skinner (CESR) The potential of the VLTIfor studying novae

  2. What is the distance of the source? Is the ejection spherical? How a jet can form? How dust can form? Is the nova wind spherical? The potential of the VLTI for the observations of Novae

  3. Observations AMBER de la nova récurrente RS Oph 5 jours après sa découverte • Un triplet de base, • Résolution spectrale R=1500 (200 km/s), • Deux observations: • a) Une observation grand S/B centrée sur Brg et son proche continuum, • b) Une observations à faible S/B couvrant la 1.95 à 2.22mm (moitié de la bande K) • Pour chaque observation, le set de donnée: • 3 visibilités dispersées, • 3 phase différentielles, • 1 clôture de phase Chesneau, Nardetto, Millour et al. A&A 2007special issue Ilustrate the potential of the VLTI for the study of novae et autres variables cataclysmiques The potential of the VLTI for the observations of Novae

  4. Continu K: 2.6 x 4.4 mas Brg 2.17 mm: 7.6 x 5.1 mas HeI 2.06 mm: 10.6 x 7.1 The potential of the VLTI for the observations of Novae

  5. Image VLBA: O’Brien, Bode, Porcas et al., 2006, Nature • Rsol • 2.5 mas Attention! Astrométrie arbitraire! D~1600pc jorb=0.97 Rrg~50 Rsol (M3III) NB+disque~10 Rsol Kcont:2.2 mas (0.4mas/jour, 430km/s) Brg:3.8 mas (0.69mas/jour,720km/s) HeI: 5.3mas (0.96mas/jour,1000km/s) The potential of the VLTI for the observations of Novae

  6. The phase information: kinematics of the ejecta (I) Typical S-shape signal Two lobes ejection Phase jump: visibility null crossing Closure phase close to zero Centro-symetrical source The potential of the VLTI for the observations of Novae

  7. Orbital plane The phase information: kinematics of the ejecta (II) The potential of the VLTI for the observations of Novae

  8. First observations, K=3.3 Second observations, K=4.5 H=2.9, near-IR C lines End of PTI obs. (14), K~6.5 H=3.7 DDT submitted Rapid end of outburst 10 days Strong dust formation event One year Again a new nova: V1280 Sco How organizing these observations? RS Oph was a reccurrent nova: this implies many earlier studies! Complex light curves in visual and different in K band… The potential of the VLTI for the observations of Novae

  9. Needs in terms of spectral resolution? Early days, wind phase: YES!, medium resolution No dust, coronal phase: YES!, probably high resolution Dust: probably NO, the dust continuum overwhelm the lines information The potential of the VLTI for the observations of Novae

  10. Toward a systematic approach DDT versus ToO? Faster reaction, on-going research: but need of a well-prepared group! How to react on events based that are unknown in advance? Novae have many different behaviors in term of light curves, lines, dust production… Dust not expected in the DDT proposal  Some AMBER time to be converted into MIDI time Optimizing configuration and VLTI flexibility: this is ATs job and not for UTs So proposal limited to bright nova event only Need of an intense time coverage (more than uv coverage? Depends on the scientific goals, See PTI paper) The potential of the VLTI for the observations of Novae

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