Optical interferometry and adaptive optics of bright transients

1. Myworkplace  Monaco Mediterraneansee Esterel Antibes Cannes Optical interferometry and adaptive optics of brighttransients Nice airport Nice F. Millour O. Chesneau, D. P. K. Banerjee, E. Lagadec, C. Lykou, A. Meilland, N. Nardetto, M. Otulaskova, A. Spang

2. A word on optical long-baselineinterferometry F. Millour, HTWUIII, Santa Fe

3. A word on (optical) high-angularresolution Binary D UD + point UD Gaussian F. Millour, HTWUIII, Santa Fe

4. A word on optical long-baselineinterferometry Binary B1 UD + point UD Gaussian F. Millour, HTWUIII, Santa Fe

5. A word on optical long-baselineinterferometry Binary B2 UD + point UD Gaussian F. Millour, HTWUIII, Santa Fe

6. A word on optical long-baselineinterferometry Binary B3 UD + point UD Gaussian F. Millour, HTWUIII, Santa Fe

7. A word on optical long-baselineinterferometry Binary HD87643 Binary 34 mas UD + point VLTI array VLT (NACO) UD Gaussian F. Millour, HTWUIII, Santa Fe

8. NPOI array CHARA array

9. An illustration:the 2007 V1280 Sco nova • One of the historically slowest nova observed • Reached V~3.8, • Monitored during 5 months by the VLTI and Mt Abu (1-2 and 8-13 micron observations) • Sparseuvcoverage (1-3 bases at a time): slow process, assuming spherical symmetry • use of the DUSTY code for the interpretation. JHK light curve Chesneau, et al. 2008, Das, et al. 2008 Chesneau et al. 2012 F. Millour, HTWUIII, Santa Fe

10. An illustration:the 2007 V1280 Sco nova • Follow-up nova expansion from 23 days up to 5 months after outburst, • Modelsuggests an accumulation of 10-6Mʘof dust • Expansion of 0.35 mas per day. • Indications that the source is not spherical F. Millour, HTWUIII, Santa Fe

11. An illustration:the 2007 V1280 Sco nova • High inclination bipolar nebula • No equatorial structures in IR, • VLTI expansion measurements in line with major axis expansion, • D>1kpc(Sadakane et al. 2009,Naito et al. 2012) A slow nova can ALSO create a striking bipolar nebula: common envelop effect? Perfect (bright) ALMA target Should now be a 1”x0.6” nebula But need continuous monitoring! 2009-2011, VISIR 2009, 2010, NACO F. Millour, HTWUIII, Santa Fe

12. TPyx (2011) • Discoveredby H. Leavitt in 1913, • ‘Recurrent’ nova, ouburstsin • 1890 • 1902 • 1920 • 1944 • 1966 • … ? • … 2011! • Nebuladeeplystudied by the HST(Shara et al. 1997), • ‘Slow motions’ measured(v~600km/s, Schaefer et al. 2010) • Binaryspectrocopic signal resolved, q=0.2, i~10(Utas et al. 2010) F. Millour, HTWUIII, Santa Fe

13. TPyx (2011) • 2011 T Pyxoutburst • combinedCHARA and VLTI observations • Results • Slow expansion (v<700 km/s)assumingD=3.5kpc(but Shore et al. 2011 D>3.5 kpc) • The source appearscircular (r=1+/-0.07), • Extended complex phase signal in the Brg line, Chesneau, Meilland, Banerjeeet al. 2011 thanksto: A. Meilland, G. Schaefer, S. Ridgway, T. tenBrummelaar, A. Merand, J. B. Le Bouquin, M. Wittkowski… F. Millour, HTWUIII, Santa Fe

14. Are these ejecta spherically distributed? No, probably concentrated near the equatorial plane facing us. This should be checked with a careful polarization study of the clumps (see the recent controversy on RS Pup, Kervella et al.; Bond et al.) t=35d • Face-on bipolar nebula! • PA angle 110° well constrained • Inclination not well constrained

15. RS Oph (2006) HST Visible 240 mas 380 AU t = 150 days Radio 40 mas 65 AU t = 22 days VLTI IR 9 mas 15 AU t = 5 days Time O’Brien et al. 2006, Chesneau et al. 2007, Bode et al. 2008… F. Millour, HTWUIII, Santa Fe

16. Novae:fastcreation of bipolarnebulae t=35d t=150 d RS Oph: O’Brien et al. 2006, Chesneau et al. 2007, Bode et al. 2008… t=5d TPyx:a face-on bipolarnebula Chesneau et al., 2011 t=900 d V1280 Sco: Chesneau et al. 2008, Chesneau et al. 2012 V445 Pup: Woudt et al. 2009 F. Millour, HTWUIII, Santa Fe

17. Why bipolarity? Binary systems! And then??? • Channeling of the outburst by dense circumbinary material? • Perhaps for V445 Pup, • Circumbinary density enough in the case of RS Oph? • Probably not applicable for V1280 Sco, and not for T Pyx, • We need to evaluate carefully the mass around manyrecurrent/classical novae • Common envelop interaction? • Favors slow nova, since time scale is short, and effects might be limited • Difficult to observe the effect of the companion during this phase • Transient jets? • Would explain velocities observed and collimation, • Intrinsically massive ejection? • Spun-up WD, rotating a P<1min  what effect on detonation/explosion? • Channeling through strong magnetic field, that should be detectable

18. The born-again Sakurai’s object 10 years after the outburst (1996) a disk is found in the core of the old PN (Chesneau et al. 2007) The PA. of the equatorial overdensities coincides with the old PN symmetrical axis 13 micron • The born-againphenomenon in the frame of the evolution (Lai, De Marco et al. 2010) : • a VLTP? But the 2D aspect must betakenintoaccount! 1D models to date… • a merger? The O16/O18 ratio is normal contrary to R CrBs (Clayton et al. 2010)… 10 micron 8 micron Chesneau, Clayton, Lykou et al. 2009

19. The outburst of V838 Mon The prototype of ILOT • The near-IR and mid-IR flux of V838 Mon remainshighenough for VLTI observations. • Twohypothesesthatcanbetested in the near/mid-IR (AMBER/MIDI) • The mid-IR flux isdominated by a late M supergiant, • The mid-IR isdominated by an expandingdustywind, • The mid-IR source isdominated by a formingdisk, whosecharacteristicssuch as the inclination, maybemeasured • In the near-IR, wemaybe able to follow and measure the angular size of the supergiant. • Do weexpect an emergingfastrotating source when the source mayeventuallygetsmaller and hotter? • Other question: • - Is there an expandingbipolarnebulaaround? MIDI/VLTI observations (2011-2012)

20. Thanks! TPyx A. Merand F. Millour, HTWUIII, Santa Fe