f. millour o. chesneau, d. p. k. banerjee, e. lagadec, c. lykou, a. meilland, n. nardetto, m....

OPTICAL INTERFEROMETRY AND ADAPTIVE OPTICS OF BRIGHT TRANSIENTS

F. MillourO. Chesneau, D. P. K. Banerjee, E. Lagadec, C. Lykou, A. Meilland, N. Nardetto, M. Otulaskova, A. Spang

Cannes Esterel Monaco

My workplace

NiceNice airport

AntibesMediterranean see

A WORD ON OPTICAL LONG-BASELINE INTERFEROMETRY

15/11/2013 F. Millour, HTWUIII, Santa Fe 2

F. Millour, HTWUIII, Santa Fe 315/11/2013

A WORD ON (OPTICAL) HIGH-ANGULAR RESOLUTION

Binary

UD + point

UD

Gaussian

D



Binary

UD + point

UD

Gaussian

B1



Binary

UD + point

UD

Gaussian

B2



Binary

UD + point

UD

Gaussian

B3



Binary

UD + point

UD

GaussianVLTI array VLT (NACO)

34 mas

Binary HD87643

NPOI array

CHARA array

8

AN ILLUSTRATION:THE 2007 V1280 SCO NOVA

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Chesneau, et al. 2008,Das, et al. 2008Chesneau et al. 2012

• 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)

• Sparse uv coverage (1-3 bases at a time): slow process, assuming spherical symmetry

• use of the DUSTY code for the interpretation.

JHK light curve

15/11/2013 F. Millour, HTWUIII, Santa Fe


• Follow-up nova expansion from 23 days up to 5 months after outburst,• Model suggests an accumulation of 10-6 Mʘ of dust• Expansion of 0.35 mas per day.• Indications that the source is not spherical


2009, 2010, NACO2009-2011, VISIR

• 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 targetShould now be a 1”x0.6” nebulaBut need continuous monitoring!



• Discovered by H. Leavitt in 1913,• ‘Recurrent’ nova, oubursts in

• 1890• 1902• 1920• 1944• 1966• … ?• … 2011!

• Nebula deeply studied by the HST(Shara et al. 1997),

• ‘Slow motions’ measured(v~600km/s, Schaefer et al. 2010)

• Binary spectrocopic signal resolved, q=0.2, i~10(Utas et al. 2010)

T PYX (2011)


Chesneau, Meilland, Banerjee et al. 2011

2011 T Pyx outburst• combined CHARA and VLTI

observations• Results

• Slow expansion (v<700 km/s)assuming D=3.5kpc(but Shore et al. 2011 D>3.5 kpc)

• The source appears circular (r=1+/-0.07),• Extended complex phase signal in the

Brg line,

thanks to: A. Meilland, G. Schaefer, S. Ridgway, T. ten Brummelaar, A. Merand, J. B. Le Bouquin, M. Wittkowski…

T PYX (2011)


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

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RS OPH (2006)


Radio40 mas65 AU

t = 22 days

HST Visible240 mas380 AU

t = 150 days

Time

VLTI IR9 mas15 AU

t = 5 days

O’Brien et al. 2006,Chesneau et al. 2007,Bode et al. 2008…

V1280 Sco: Chesneau et al. 2008,Chesneau et al. 2012

T Pyx:a face-on bipolar nebulaChesneau et al., 2011

t=150 dRS Oph: O’Brien et al. 2006, Chesneau et al. 2007,Bode et al. 2008…

t=5d

t=35d

V445 Pup: Woudt et al. 2009

NOVAE:FAST CREATION OF BIPOLAR NEBULAE

t=900 d


Why bipolarity?

1. 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 many

recurrent/classical novae2. 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

3. Transient jets?• Would explain velocities observed and collimation,

4. Intrinsically massive ejection?• Spun-up WD, rotating a P<1min what effect on detonation/explosion?• Channeling through strong magnetic field, that should be detectable

And then???

Binary systems!

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Chesneau, Clayton, Lykou et al. 2009

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

8 micron10 micron13 micron

The born-again phenomenon in the frame of the evolution (Lai, De Marco et al. 2010) : - a VLTP? But the 2D aspect must be taken into account! 1D models to date…- a merger? The O16/O18 ratio is normal contrary to R CrBs (Clayton et al. 2010)…

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The outburst of V838 MonThe prototype of ILOT

The near-IR and mid-IR flux of V838 Mon remains high enough for VLTI observations.

Two hypotheses that can be tested in the near/mid-IR (AMBER/MIDI)

- The mid-IR flux is dominated by a late M supergiant,- The mid-IR is dominated by an expanding dusty wind,- The mid-IR source is dominated by a forming disk,

whose characteristics such as the inclination, may be measured

In the near-IR, we may be able to follow and measure the angular size of the supergiant.

Do we expect an emerging fast rotating source when the source may eventually get smaller and hotter?

Other question:- Is there an expanding bipolar nebula around?

MIDI/VLTI observations (2011-2012)

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THANKS!

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T Pyx

A. Merand

15/11/2013 F. Millour, HTWUIII, Santa Fe

f. millour o. chesneau, d. p. k. banerjee, e. lagadec, c. lykou, a. meilland, n. nardetto, m....

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