VLTI monitoring of the dust formation event  of the Nova V1280 Scorpii

Chesneau, O.; Banerjee, D. P. K.; Millour, F.; Nardetto, N.; Sacuto, Stéphane; Spang, A.; Wittkowski, M.; Ashok, N. M.; Das, Ramkrishna; Hummel, C. A.; Kraus, Stefan; Lagadec, E.; Morel, S.; Petr-Gotzens, M. G.; Rantakyrö, F.; Schöller, M.

doi:10.1051/0004-6361:200809485

Cited by 44 publications

(63 citation statements)

References 36 publications

(45 reference statements)

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“…Some recent examples suggest that bipolarity in the ejecta of classical/recurrent novae may be relatively frequent: RS Oph (Ribeiro et al 2009;Bode et al 2007;Chesneau et al 2007), V445 Pup (Woudt et al 2009), V1280 Sco (Chesneau et al 2008;Chesneau et al, in prep. ) or HR Del (Harman & O'Brien 2003).…”

Section: A Face-on Bipolar Eventmentioning

confidence: 99%

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

Chesneau¹,

Meilland²,

Banerjee³

et al. 2011

A&A

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Aims. T Pyx is the first recurrent nova ever historically studied. It was seen in outburst six times between 1890 and 1966 and then not for 45 years. We report on near-IR interferometric observations of the recent outburst of 2011. Methods. We obtained near-IR observations of T Pyx at dates ranging from t = 2.37 d to t = 48.2 d after the outburst, with the CLASSIC recombiner located at the CHARA array and with the PIONIER and AMBER recombiners located at the VLTI array. These data are supplemented with near-IR photometry and spectra obtained at Mount Abu, India. We compare expansion of the H and K band continua and the Brγ emission line, and infer information on the kinematics and morphology of the early ejecta. Results. Slow expansion velocities were measured (≤300 km s −1 ) before t = 20 d. From t = 28 d on, the AMBER and PIONIER continuum visibilities (K and H band, respectively) are best simulated with a two-component model consisting of an unresolved source plus an extended source whose expansion velocity onto the sky plane is lower than ∼700 km s −1 . The expansion of the Brγ lineforming region, as inferred at t = 28 d and t = 35 d, is slightly larger, implying velocities in the range 500−800 km s −1 , which is still strikingly lower than the velocities of 1300−1600 km s −1 inferred from the Doppler width of the line. Moreover, a remarkable pattern was observed in the Brγ differential phases. A semi-quantitative model using a bipolar flow with a contrast of 2 between the pole and equator velocities, an inclination of i = 15• , and a position angle PA = 110• provides a good match to the AMBER observables. At t = 48 d, a PIONIER dataset confirms the two-component nature of the H band emission, consisting of an unresolved stellar source and an extended region whose appearance is circular and symmetric within error bars. Conclusions. These observations are most simply interpreted within the frame of a bipolar model, oriented nearly face-on. This finding has profound implications for interpreting past, current, and future observations of the expanding nebula.

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Section: A Face-on Bipolar Eventmentioning

confidence: 99%

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

Chesneau¹,

Meilland²,

Banerjee³

et al. 2011

A&A

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“…P-Cygni lines were systematically observed even four years after the outburst, which is indicative of a sustained and significant mass loss (Schwarz et al 2011). The typical P-Cygni type velocities reached 500 km s −1 , from which Chesneau et al (2008) inferred a distance of 1.6 ± 0.4 kpc. However, Hounsell et al (2010) recently derived a distance of 630 ± 100 pc from space-based visual light curves that span the first 20 days after discovery.…”

Section: Introductionmentioning

confidence: 95%

“…Owing to the sparse uv coverage, an interpretation involving a spherical dusty shell was developed, providing estimates of the dust formation rate. Based on an estimate of the total dust mass formed during the 250 days after outburst, Chesneau et al (2008) suggested that a mass as large as 10 −4 M was ejected. Naito et al (2012) provided an independent estimate from neutral oxygen lines that confirmed the high mass ejected, an additional argument for a low-mass WD progenitor, known to statistically eject more mass that fast, massive ones.…”

Section: Introductionmentioning

confidence: 99%

The expanding dusty bipolar nebula around the nova V1280 Scorpi

Chesneau

Lagadec

Otulakowska-Hypka

et al. 2012

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Context. The fast temporal evolution of the ejecta morphology of novae can be considered as an important test bench for studying the shaping of many kinds of nebulae. V1280 Sco is one of the slowest dust-forming nova ever historically observed that has experienced a particularly long common-envelope phase. Aims. We performed multi-epoch high-spatial resolution observations of the circumstellar dusty environment of V1280 Sco to investigate the level of asymmetry of the ejecta. Methods. We observed V1280 Sco in 2009, 2010 and 2011 (from t = 877 days after discovery until t = 1664 d) using unprecedented high angular resolution techniques. We used the NACO/VLT adaptive optics system in the J, H and K bands, together with contemporaneous VISIR/VLT mid-IR imaging that resolved the dust envelope of V1280 Sco, and SINFONI/VLT observations secured in 2011. Results. We report the discovery of a dusty hourglass-shaped bipolar nebula. The apparent size of the nebula increased from 0.30 × 0.17 in July 2009 to 0.64 × 0.42 in July 2011. The aspect ratio suggests that the source is seen at high inclination. The central source shines efficiently in the K band and represents more than 56 ± 5% of the total flux in 2009, and 87 ± 6% in 2011. A mean expansion rate of 0.39 ± 0.03 milliarcsec per day is inferred from the VISIR observations in the direction of the major axis, which represents a projected upper limit. Assuming that the dust shell expands in that direction as fast as the low-excitation slow ejecta detected in spectroscopy, this yields a lower limit distance to V1280 Sco of ∼1 kpc; however, the systematic errors remain large due to the complex shape and velocity field of the dusty ejecta. The dust seems to reside essentially in the polar caps and no infrared flux is detected in the equatorial regions in the latest dataset. This may imply that the mass-loss was dominantly polar. Conclusions. V1280 Sco is an excellent test case for studying the temporal evolution of dusty bipolar ejecta. As the nebula expands, observations will be easier and we advocate a yearly monitoring of the source using high angular resolution techniques.

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“…Dust has formed in novae where there has been no CO formation. An example is the bright nova V1280 Sco, which formed copious dust (Das et al 2008;Chesneau et al 2008;Chesneau et al 2012), but where no CO emission was detected. NIR spectroscopic observations of V1280 Sco up till the dust forming stage, were taken at high and sufficiently regular cadence to detect CO had it formed notwithstanding its transient nature (Das et al 2008).…”

Section: Early Phase Spectramentioning

confidence: 99%

Near-infrared and optical studies of the highly obscured nova V1831 Aquilae (Nova Aquilae 2015)

Banerjee

Srivastava

Ashok

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Near Infrared (NIR) and optical photometry and spectroscopy are presented for the nova V1831 Aquilae, covering the early decline and dust forming phases during the first ∼90 days after its discovery. The nova is highly reddened due to interstellar extinction. Based solely on the nature of NIR spectrum we are able to classify the nova to be of the Fe II class. The distance and extinction to the nova are estimated to be 6.1 ± 0.5 kpc and A v ∼ 9.02 respectively. Lower limits of the electron density, emission measure and ionized ejecta mass are made from a Case B analysis of the NIR Brackett lines while the neutral gas mass is estimated from the optical [OI] lines. We discuss the cause for a rapid strengthening of the He I 1.0830 µm line during the early stages. V1831 Aql formed a modest amount of dust fairly early (∼ 19.2 days after discovery); the dust shell is not seen to be optically thick. Estimates are made of the dust temperature, dust mass and grain size. Dust formation commences around day 19.2 at a condensation temperature of 1461 ± 15 K, suggestive of a carbon composition, following which the temperature is seen to gradually decrease to 950K. The dust mass shows a rapid initial increase which we interpret as being due to an increase in the number of grains, followed by a period of constancy suggesting the absence of grain destruction processes during this latter time. A discussion is made of the evolution of these parameters, including certain peculiarities seen in the grain radius evolution.

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VLTI monitoring of the dust formation event of the Nova V1280 Scorpii

Cited by 44 publications

References 36 publications

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

The expanding dusty bipolar nebula around the nova V1280 Scorpi

Near-infrared and optical studies of the highly obscured nova V1831 Aquilae (Nova Aquilae 2015)

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