The expanding fireball of Nova Delphini 2013 (original) (raw)

References

  1. Bode, M. F. & Evans, A. Classical Novae (Cambridge Univ. Press, 2008)
    Book Google Scholar
  2. Gehrz, R. D. The infrared temporal development of classical novae. Annu. Rev. Astron. Astrophys. 26, 377–412 (1988)
    Article CAS ADS Google Scholar
  3. Slavin, A. J., O'Brien, T. J. & Dunlop, J. S. A deep optical imaging study of the nebular remnants of classical novae. Mon. Not. R. Astron. Soc. 276, 353–371 (1995)
    Article ADS Google Scholar
  4. Woudt, P. A. et al. The expanding bipolar shell of the helium nova V445 Puppis. Astrophys. J. 706, 738–746 (2009)
    Article CAS ADS Google Scholar
  5. Chesneau, O. et al. The expanding dusty bipolar nebula around the nova V1280 Scorpi. Astron. Astrophys. 545, A63 (2012)
    Article Google Scholar
  6. Livio, M., Shankar, A., Burkert, A. & Truran, J. W. The common envelope phase in the outbursts of classical novae. Astrophys. J. 356, 250–254 (1990)
    Article ADS Google Scholar
  7. Lloyd, H. M., O'Brien, T. J. & Bode, M. F. Shaping of nova remnants by binary motion. Mon. Not. R. Astron. Soc. 284, 137–147 (1997)
    Article ADS Google Scholar
  8. Orio, M. & Shaviv, G. Local thermonuclear runaways among classical novae. Astrophys. Space Sci. 202, 273–288 (1993)
    Article ADS Google Scholar
  9. Porter, J. M., O'Brien, T. J. & Bode, M. F. On the asphericity of nova remnants caused by rotating white dwarf envelopes. Mon. Not. R. Astron. Soc. 296, 943–948 (1998)
    Article ADS Google Scholar
  10. Scott, A. D. Nova outbursts on rotating oblate white dwarfs. Mon. Not. R. Astron. Soc. 313, 775–782 (2000)
    Article CAS ADS Google Scholar
  11. Chesneau, O. & Banerjee, D. P. K. Interferometric studies of novae in the infrared. Bull. Astron. Soc. India 40, 267–292 (2012)
    ADS Google Scholar
  12. Nakano, S. et al. Nova Delphini 2013 = Pnv J20233073+2046041. Central Bureau Electron. Telegr. 3628, 1 (2013)
    ADS Google Scholar
  13. ten Brummelaar, T. A. et al. First results from the CHARA array. II. A description of the instrument. Astrophys. J. 628, 453–465 (2005)
    Article ADS Google Scholar
  14. Wren, J., Vestrand, W. T., Wozniak, P. & Davis, H. Pre-discovery detections of the Nova Delphini outburst. Astron. Telegr. 5316, 1 (2013)
    ADS Google Scholar
  15. Munari, U., Henden, A., Dallaporta, S. & Cherini, G. Photometric evolution of Nova Del 2013 (V339 Del) during the optically thick phase. Inform. Bull. Variable Stars 6080, 1 (2013)
    ADS Google Scholar
  16. Deacon, N. R. et al. Pre-outburst observations of Nova Del 2013 from Pan-STARRS 1. Astron. Astrophys. 563, A129 (2014)
    Article Google Scholar
  17. Shore, S. N. et al. Continuing spectroscopic observations (3500–8800A) of Nova Del 2013 with the Ondrejov Observatory and the ARAS group. Astron. Telegr. 5312, 1 (2013)
    ADS Google Scholar
  18. Gill, C. D. & O'Brien, T. J. Emission-line profiles from model nova shells. Mon. Not. R. Astron. Soc. 307, 677–684 (1999)
    Article CAS ADS Google Scholar
  19. Shore, S. N. et al. The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. II. The optically thin phase and the structure of the ejecta in recurrent novae. Astron. Astrophys. 549, A140 (2013)
    Article Google Scholar
  20. Shore, S. N. A unified model for the spectrophotometric development of classical and recurrent novae. The role of asphericity of the ejecta. Astron. Astrophys. 559, L7 (2013)
    Article ADS Google Scholar
  21. Taranova, O. G., Tatarnikov, A. M., Shenavrin, V. I. & Tatarnikova, A. A. Infrared photometry of Nova Delphini 2013 ( = V339 Del) in the first sixty days after its outburst. Astron. Lett. 40, 120–124 (2014)
    Article ADS Google Scholar
  22. Shore, S. N., Augusteijn, T., Ederoclite, A. & Uthas, H. The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. I. The optically thick phase and the origin of moving lines in novae. Astron. Astrophys. 533, L8 (2011)
    Article ADS Google Scholar
  23. Ireland, M. J., Monnier, J. D. & Thureau, N. Monte-Carlo imaging for optical interferometry. Proc. SPIE 6268, 62681T (2006)
    Article ADS Google Scholar
  24. Ford, H. C. & Ciardullo, R. in The Extragalactic Distance Scale (eds van den Bergh, S. & Pritchet, C. J. ) ASP Conf. Ser. 4, 128–144 (1988)
    Google Scholar
  25. Wade, R. A., Harlow, J. J. B. & Ciardullo, R. Biases in expansion distances of novae arising from the prolate geometry of nova shells. Publ. Astron. Soc. Pacif. 112, 614–624 (2000)
    Article ADS Google Scholar
  26. Downes, R. A. & Duerbeck, H. W. Optical imaging of nova shells and the maximum magnitude-rate of decline relationship. Astron. J. 120, 2007–2037 (2000)
    Article CAS ADS Google Scholar
  27. Shore, S. N. et al. First high resolution ultraviolet (HST/STIS) and supporting optical spectroscopy of V339 Del = Nova Del 2013. Astron. Telegr. 5409 1 (2013) ; correction 5410, 1 (2013)
    ADS Google Scholar
  28. Lane, B. F. et al. Interferometric observations of V1663 Aquilae (Nova Aql 2005). Astrophys. J. 669, 1150–1155 (2007)
    Article CAS ADS Google Scholar
  29. Chesneau, O. et al. AMBER/VLTI interferometric observations of the recurrent Nova RS Ophiuchii 5.5 days after outburst. Astron. Astrophys. 464, 119–126 (2007)
    Article CAS ADS Google Scholar
  30. Chesneau, O. et al. The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection. Astron. Astrophys. 534, L11 (2011)
    Article ADS Google Scholar
  31. ten Brummelaar, T. A. et al. The CLASSIC/CLIMB Beam Combiner at the CHARA Array. J. Astron. Instrum. 2, 1340004 (2013)
    Article Google Scholar
  32. Monnier, J. D. et al. Michigan Infrared Combiner (MIRC): commissioning results at the CHARA Array. Proc. SPIE 6268, 62681P (2006)
    Article Google Scholar
  33. Bonneau, D. et al. SearchCal: a virtual observatory tool for searching calibrators in optical long baseline interferometry. I. The bright object case. Astron. Astrophys. 456, 789 (2006)
    Article ADS Google Scholar
  34. Boyajian, T. S. et al. Stellar diameters and temperatures. III. Main-sequence A, F, G, and K stars: additional high-precision measurements and empirical relations. Astrophys. J. 771, 40 (2013)
    Article ADS Google Scholar
  35. Crepp, J. R. et al. The dynamical mass and three-dimensional orbit of HR7672B: a benchmark brown dwarf with high eccentricity. Astrophys. J. 751, 97 (2012)
    Article ADS Google Scholar
  36. Skrutskie, M. F. et al. The Two Micron All Sky Survey (2MASS). Astron. J. 131, 1163–1183 (2006)
    Article ADS Google Scholar
  37. Henden, A. A. The AAVSO International Database. http://www.aavso.org (2013)
  38. Tuthill, P. et al. Double-Fourier spatio-spectral decoding. In Advances in Stellar Interferometry, SPIE Conf. Ser. 6268 62680X (2006) http://dx.doi.org/10.1117/12.672277
    Google Scholar
  39. Markwardt, C. B. in Astronomical Data Analysis Software and Systems XVIII, Astron. Soc. Pacif. Conf. Ser. 411, 251–254 (2009)
    ADS Google Scholar
  40. Press, W. H., Teukolsky, S. A., Vetterling, W. T. & Flannery, B. P. Numerical Recipes in C (Cambridge Univ. Press, 1992)
    MATH Google Scholar
  41. Wilson, J. C. et al. in Ground-based Instrumentation for Astronomy, SPIE Conf. Ser. 5492, 1295–1305 (2004); http://dx.doi.org/10.1117/12.550925
  42. Herter, T. L. et al. in Ground-based and Airborne Instrumentation for Astronomy II, SPIE Conf. Ser. 7014, 70140X (2008); http://dx.doi.org/10.1117/12.789660
  43. Cushing, M. C., Vacca, W. D. & Rayner, J. T. Spextool: a spectral extraction package for SpeX, a 0.8-5.5 micron cross-dispersed spectrograph. Proc. Astron. Soc. Pacif. 116, 362–376 (2004)
    Article ADS Google Scholar
  44. Muirhead, P. S. et al. Precise stellar radial velocities of an M dwarf with a Michelson interferometer and a medium-resolution near-infrared spectrograph. Publ. Astron. Soc. Pacif. 123, 709–724 (2011)
    Article ADS Google Scholar
  45. Vacca, W. D., Cushing, M. C. & Rayner, J. T. A method of correcting near-infrared spectra for telluric absorption. Publ. Astron. Soc. Pacif. 115, 389–409 (2003)
    Article ADS Google Scholar
  46. Banerjee, D. P. K. Ashok, N. M., Joshi, V. & Evans, A. Ongoing near-infrared observations of V339 Del (Nova Del 2013). Astron. Telegr. 5404, 1 (2013)
    ADS Google Scholar
  47. Das, R. K., Banerjee, D. P. K., Ashok, N. M. & Chesneau, O. Near-infrared studies of V1280 Sco (Nova Scorpii 2007). Mon. Not. R. Astron. Soc. 391, 1874–1886 (2008)
    Article CAS ADS Google Scholar
  48. Hjellming, R. M., Wade, C. M., Vandenberg, N. R. & Newell, R. T. Radio emission from nova shells. Astron. J. 84, 1619–1631 (1979)
    Article ADS Google Scholar

Download references

Acknowledgements

We acknowledge the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. We thank O. Garde and other members of the Astronomical Ring for Access to Spectroscopy for use of their archive of Nova Del 2013 spectra. We thank G. J. Schwarz, S. N. Shore, and F. M. Walter for discussions that helped us to interpret the nova observations. This material is based upon work supported by the National Science Foundation under grant number AST-1009080. The CHARA Array is funded by the National Science Foundation through NSF grants AST 0908253 and AST 1211129, and by Georgia State University through the College of Arts and Sciences. This publication made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.

Author information

Authors and Affiliations

  1. The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, 91023, California, USA
    G. H. Schaefer, T. ten Brummelaar, C. D. Farrington, N. Scott, J. Sturmann, N. Vargas, L. Sturmann & N. H. Turner
  2. Center for High Angular Resolution Astronomy and Department of Physics and Astronomy, Georgia State University, PO Box 5060, Atlanta, Georgia 30302, USA,
    D. R. Gies, B. Kloppenborg, H. A. McAlister, F. Baron & J. Jones
  3. Laboratoire Lagrange, UMR 7293, Université de Sophia-Antipolis (UNS)–Centre National de la Recherche Scientifique (CNRS)–Observatoire de la Côte d’Azur (OCA), Boulevard de l’Observatoire, CS 34229, F-06304 Nice, Cedex 4, France,
    O. Chesneau, D. Mourard, A. Meilland, N. Nardetto & P. Stee
  4. Department of Astronomy, University of Michigan, 941 Dennison Building, Ann Arbor, Michigan 48109, USA,
    J. D. Monnier, X. Che, R. M. Roettenbacher & J. Becker
  5. National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, 85719, Arizona, USA
    S. T. Ridgway
  6. Université de Lyon; Université Lyon 1, Observatoire de Lyon, 9 avenue Charles André, 69230 Saint Genis Laval; CNRS UMR 5574, Centre de Recherche Astrophysique de Lyon; École Normale Supérieure, 69007 Lyon, France,
    I. Tallon-Bosc
  7. Université Lyon 1, Observatoire de Lyon, 9 avenue Charles André, 69230 Saint Genis Laval,
    I. Tallon-Bosc
  8. Department of Astronomy, Yale University, New Haven, 06511, Connecticut, USA
    T. Boyajian
  9. Sydney Institute for Astronomy, School of Physics, University of Sydney, New South Wales 2006, Sydney, Australia,
    V. Maestro & P. Tuthill
  10. Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australian Capital Territory 2611, Australia,
    M. Ireland
  11. Remote Sensing Division, Naval Research Laboratory, 4555 Overlook Avenue Southwest, Washington, DC 20375, USA,
    E. K. Baines
  12. Département de Physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, CP 6128, Succursale Centre-Ville, Montréal, Québec H3C 3J7, Canada,
    N. D. Richardson
  13. Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, 86001, Arizona, USA
    G. van Belle
  14. Max Planck Institute for Astronomy (MPIA), Konigstuhl 17, 69117 Heidelberg, Germany,
    K. von Braun
  15. United States Naval Observatory, Flagstaff Station, 10391 West Naval Observatory Road, Flagstaff, Arizona 86001, USA,
    R. T. Zavala
  16. Astronomy and Astrophysics Division, Physical Research Laboratory, Navrangpura, Ahmedabad, Gujarat 380009, India,
    D. P. K. Banerjee, N. M. Ashok & V. Joshi
  17. Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, 91106, California, USA
    J. Becker
  18. Department of Astronomy, Boston University, Boston, 02215, Massachusetts, USA
    P. S. Muirhead

Authors

  1. G. H. Schaefer
  2. T. ten Brummelaar
  3. D. R. Gies
  4. C. D. Farrington
  5. B. Kloppenborg
  6. O. Chesneau
  7. J. D. Monnier
  8. S. T. Ridgway
  9. N. Scott
  10. I. Tallon-Bosc
  11. H. A. McAlister
  12. T. Boyajian
  13. V. Maestro
  14. D. Mourard
  15. A. Meilland
  16. N. Nardetto
  17. P. Stee
  18. J. Sturmann
  19. N. Vargas
  20. F. Baron
  21. M. Ireland
  22. E. K. Baines
  23. X. Che
  24. J. Jones
  25. N. D. Richardson
  26. R. M. Roettenbacher
  27. L. Sturmann
  28. N. H. Turner
  29. P. Tuthill
  30. G. van Belle
  31. K. von Braun
  32. R. T. Zavala
  33. D. P. K. Banerjee
  34. N. M. Ashok
  35. V. Joshi
  36. J. Becker
  37. P. S. Muirhead

Contributions

Observations with the CHARA Array were originally proposed by B.K. and D.R.G. Modelling and interpreting the angular expansion curve and asymmetries were done by G.H.S., D.R.G., B.K., T.t.B., O.C., I.T.-B. and S.T.R. The CHARA data were reduced by T.t.B., J.D.M., O.C., I.T.-B., D.M., V.M., C.D.F., N.S. and G.H.S. The observations were planned and conducted by C.D.F., N.S., N.V., B.K., D.R.G., T.B., G.H.S., D.M., A.M., N.N., P.S., M.I., V.M., P.T., J.J., N.D.R., R.M.R., G.v.B., K.v.B. and R.T.Z. Observational setup and technical support were provided by J.S., L.S., N.H.T. and X.C. Administrative oversight and access to CHARA were provided by H.A.M. and T.t.B. Reconstructing and interpreting the nova images were done by G.H.S., F.B., J.D.M. and B.K. Infrared magnitudes derived from CHARA data were computed by N.S. and G.H.S. Infrared spectra were taken and reduced by D.P.K.B., N.M.A., V.J., P.S.M., J.B. and analysed by D.R.G. All authors discussed the results and commented on the manuscript.

Corresponding author

Correspondence toG. H. Schaefer.

Ethics declarations

Competing interests

The authors declare no competing financial interests.

Extended data figures and tables

Extended Data Figure 1 Integrated emission line to continuum flux ratios measured from infrared spectroscopy.

The squares represent the H-band ratios while the diamonds represent the K′-band ratios. The rise in the emission line flux is consistent with an increasing contribution from optically thin emission. The down turn in the curve during the last measurement is probably caused by a rising contribution of the continuum owing to the formation of dust.

Source data

Extended Data Figure 2 Closure phases measured with MIRC on ut 2013 August 21.

The measurements are plotted against the length of the maximum baseline (B) for the group of three telescopes that were used to form the closure phase. The non-zero closure phases indicate an asymmetry in the light distribution that is not point symmetric. The colours of the symbols are used to differentiate the measurements from each grouping of three telescopes in the array. The closure phases are measured in eight wavelength channels. Error bars represent 1_σ_ measurement uncertainties.

Extended Data Figure 3 Example of MIRC observations obtained on ut 2013 August 21.

The light is dispersed over eight wavelength channels in the H-band. a, Coverage of the interferometric baselines projected on the plane of the sky in right ascension (RA) and declination (Dec.) in units of spatial frequencies (u = B x /λ, v = B y /λ). b, Squared, normalized visibility amplitude measurements, colour-coded to match the baselines on the left. The solid line shows the best-fitting uniform disk model. The small black dots show the best-fitting uniform ellipse model. Error bars represent 1_σ_ measurement uncertainties.

Extended Data Figure 4 Interferometric visibilities of Nova Del 2013 measured with the CHARA Array.

The red line shows the best-fitting model for a uniformly bright, circular disk. The time since the explosion (in days) is indicated in the upper right corner of each panel. The measurements were obtained with the CLASSIC, CLIMB, and MIRC beam combiners (see Extended Table 1). Error bars represent 1_σ_ measurement uncertainties.

Extended Data Figure 5 Time evolution of the two-component model of Nova Del 2013.

The model consists of a circular core surrounded by a halo ring. The expansion rate and size ratio were determined by minimizing _χ_2 across all of the nights while allowing the flux ratio to vary night by night. In plotting the images, we used the flux ratio measured directly for the first three nights, the linear fit plotted in Fig. 3 of the main paper for t = 4–27 days, and our measurement that the ring contributes an average of 68% of the light on the last five nights (dust emission in the outer layers). Each panel is 12 mas on a side. We scaled the model flux by the infrared magnitude measured on each night to show how the surface brightness changes. The time since the explosion (in days) is indicated in each panel. Intensity refers to the flux per unit area.

Extended Data Table 1 Journal of observations and angular diameters measurements of Nova Del 2013

Full size table

Extended Data Table 2 Uniform ellipse models of Nova Del 2013

Full size table

Extended Data Table 3 Infrared magnitudes of Nova Del 2013

Full size table

Extended Data Table 4 Effective bandwidth of the CLASSIC/CLIMB observations

Full size table

PowerPoint slides

Source data

Rights and permissions

About this article

Cite this article

Schaefer, G., Brummelaar, T., Gies, D. et al. The expanding fireball of Nova Delphini 2013.Nature 515, 234–236 (2014). https://doi.org/10.1038/nature13834

Download citation