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The dusty aftermath of a rapid nova: V5579 Sgr

Published online by Cambridge University Press:  20 September 2024

Ashish Raj Open the ORCID record for Ashish Raj [Opens in a new window] ,
Mohit Singh Bisht ,
F.M. Walter ,
R. Pandey ,
C.E. Woodward ,
D.E. Harker ,
Devendra Bisht ,
H.P. Singh ,
A. Agarwal  and
Jeewan Pandey
...Show all authors
Ashish Raj*
Affiliation:
Indian Centre for Space Physics, Kolkata, West Bengal, India
Mohit Singh Bisht
Affiliation:
Indian Centre for Space Physics, Kolkata, West Bengal, India
F.M. Walter
Affiliation:
Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY, USA
R. Pandey
Affiliation:
Physical Research Laboratory, Navrangpura, Ahmedabad, Gujarat, India
C.E. Woodward
Affiliation:
Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, MN, USA
D.E. Harker
Affiliation:
Department of Astronomy and Astrophysics, University of California, San Diego, La Jolla, CA, USA
Devendra Bisht
Affiliation:
Indian Centre for Space Physics, Kolkata, West Bengal, India
H.P. Singh
Affiliation:
Department of Physics and Astrophysics, University of Delhi, Delhi, India
A. Agarwal
Affiliation:
Center for Cosmology and Science Popularization(CCSP), SGT University, Budhera, Delhi, NCR, India
Jeewan Pandey
Affiliation:
Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital, India
Arti Joshi
Affiliation:
Institute of Astrophysics, Pontificia Universidad Católica de Chile, Santiago, Chile
K. Belwal
Affiliation:
Indian Centre for Space Physics, Kolkata, West Bengal, India
Christian Buil
Affiliation:
Castanet Tolosan Observatory, Castanet Tolosan, France
*
Corresponding author: Ashish Raj; Email: ashishpink@gmail.com
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Abstract

V5579 Sgr was a fast nova discovered in 2008 April 18.784 UT. We present the optical spectroscopic observations of the nova observed from the Castanet Tolosan, SMARTS, and CTIO observatories spanning over 2008 April 23 to 2015 May 11. The spectra are dominated by hydrogen Balmer, Fe II, and O I lines with P-Cygni profiles in the early phase, typical of an Fe II class nova. The spectra show He I and He II lines along with forbidden lines from N, Ar, S, and O in the nebular phase. The nova showed a pronounced dust formation episode that began about 20 days after the outburst. The dust temperature and mass were estimated using the WISE data from spectral energy distribution (SED) fits. The PAH-like features are also seen in the nova ejecta in the mid-infrared Gemini spectra taken 522 d after the discovery. Analysis of the light curve indicates values of $t_2$ and $t_3$ about 9 and 13 days, respectively, placing the nova in the category of fast nova. The best-fit cloudy model of the early decline phase JHK spectra obtained on 2008 May 3 and the nebular optical spectrum obtained on 2011 June 2 shows a hot white dwarf source with $T_{BB}$ $\sim$ 2.6 $\times$ 10$^5$ K having a luminosity of 9.8 $\times$ 10$^{36}$ ergs s$^{-1}$. Our abundance analysis shows that the ejecta is significantly enhanced relative to solar, O/H = 32.2, C/H = 15.5, and N/H = 40.0 in the early decline phase and O/H = 5.8, He/H = 1.5, and N/H = 22.0 in the nebular phase.

Keywords

Stars: novaecataclysmic variablesstars: individual (V5579 Sgr)techniques: spectroscopicline: identification
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 41 , 2024 , e051
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of Astronomical Society of Australia

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References

Allamandola, L. J., Tielens, A. G. G. M., & Barker, J. R. 1989, ApJS, 71, 733 (ISSN 0067-0049). Research supported by NASA, DOE, and NSF.Google Scholar
Banerjee, D. P. K., Srivastava, M. K., Ashok, N. M., Munari, U., Hambsch, F.-J., Righetti, G. L., & Maitan, A. 2018, MNRAS, 473, 1895.Google Scholar
Blanco, A., Falcicchia, G., & Merico, F. 1983, Ap&SS, 89, 163.Google Scholar
Bode, M. F., & Evans, A. 2008, Classical Novae, Vol. 43. https://doi.org/10.1017/CBO9780511536168.Google Scholar
Chatzikos, M., et al. 2023, RMxAA, 59, 327. https://doi.org/10.22201/ia.01851101p.2023.59.02.12.Google Scholar
De Buizer, J. M., & Scott Fisher, R. 2005, in High Resolution Infrared Spectroscopy in Astronomy (Berlin, Heidelberg: Springer Berlin Heidelberg), 84. ISBN: 978-3-540-31606-0.Google Scholar
Downes, R. A., & Duerbeck, H. W. 2000, AJ, 120, 2007.Google Scholar
Draine, B. T., & Li, A. 2007, ApJ, 657, 810.Google Scholar
Dvorak, S., Guido, E., & Sostero, G. 2008, Central Bureau Electronic Telegrams, Vol. 1342, 2.Google Scholar
Ederoclite, A., et al. 2006, A&A, 459, 875.Google Scholar
Evans, A., et al. 2017, MNRAS, 466, 4221.Google Scholar
Evans, A., Tyne, V. H., Smith, O., Geballe, T. R., Rawlings, J. M. C., & Eyres, S. P. S. 2005, MNRAS, 360, 1483.Google Scholar
Eyres, S. P. S., Evans, A., Geballe, T. R., Davies, J. K., & Rawlings, J. M. C. 1997, ASS, 251, 303. https://doi.org/10.1023/A:1000787528827.Google Scholar
Ferland, G. J., et al. 2013, RMxAA, 49, 137.Google Scholar
Ferland, G. J., & Shields, G. A. 1978, ApJ, 226, 172.Google Scholar
Gehrz, R. D., et al. 2018, ApJ, 858, 78.Google Scholar
Gehrz, R. D., Truran, J. W., Williams, R. E., & Starrfield, S. 1998, PASP, 110, 3.Google Scholar
Gehrz, R. D. 1988, ARA&A, 26, 377. https://doi.org/10.1146/annurev.aa.26.090188.002113.Google Scholar
Gehrz, R. D. 2008, in Classical Novae, Cambridge Astrophysics, ed. Bode, M. F., & Evans, A., 167 (Cambridge University Press).Google Scholar
Grevesse, N., Asplund, M., Sauval, A. J., & Scott, P. 2010, ASS, 328, 179. https://doi.org/10.1007/s10509-010-0288-z.Google Scholar
Habtie, G. R., Das, R., Pandey, R., Ashok, N. M., & Dubovsky, P. A. 2024, MNRAS, 527, 1405.Google Scholar
Hachisu, I., & Kato, M. 2007, ApJ, 662, 552.Google Scholar
Hachisu, I., & Kato, M. 2019, ApJS, 242, 18.Google Scholar
Hachisu, I., & Kato, M. 2021, ApJS, 253, 27.Google Scholar
Harker, D. E., Woodward, C. E., Kelley, M. S. P., & Wooden, D. H. 2018, AJ, 155, 199.Google Scholar
Hauschildt, P. H., Starrfield, S., Shore, S. N., Gonzalez-Riestra, R., Sonneborn, G., & Allard, F. 1994, AJ, 108, 1008.Google Scholar
Helton, L. A., et al. 2010, AJ, 140, 1347.Google Scholar
Helton, L. A., Evans, A., Woodward, C. E., & Gehrz, R. D. 2011, in Eas Publications Series, Vol. 46, ed. Joblin, C., & Tielens, A. G. G. M. (EAS Publications Series), 407. https://doi.org/10.1051/eas/1146042.Google Scholar
Henden, A., & Munari, U. 2008, IBVS, 5834, 1.Google Scholar
Iijima, T., & Naito, H. 2011, A&A, 526, A73.Google Scholar
José, J., Shore, S. N., & Casanova, J. 2020, A&A, 634, A5. https://doi.org/10.1051/0004-6361/201936893.Google Scholar
Jurdana-Sepic, R., & Munari, U. 2008, IBVS, 5839, 1.Google Scholar
Kafka, S, 2021. Observations from the AAVSO International Database.Google Scholar
Kamath, U., Anupama, G. C., Ashok, N., & Chandrasekhar, T. 1997, AJ, 114, 2671. https://doi.org/10.1086/118677.Google Scholar
Kiss, L. L., & Thomson, J. R. 2000, A&A, 355, L9.Google Scholar
Kruegel, E. 2003, The Physics of Interstellar Dust.Google Scholar
Livio, M. 1992, ApJ, 393, 522 (ISSN 0004-637X). Research supported by Space Telescope Science Institute.Google Scholar
Munari, U., Siviero, A., Moretti, S., Tomaselli, S., Maitan, A., Castellani, F., Dallaporta, S., & Ochner, P. 2008, Central Bureau Electronic Telegrams, 1352, 1.Google Scholar
Munari, U., et al. 2008, A&A, 492, 145.Google Scholar
Nakano, S., et al. 2008, International Astronomical Union Circular, 8937, 1.Google Scholar
Osterbrock, D. E., & Ferland, G. J. 2006, Astrophysics of Gaseous Nebulae and Active Galactic Nuclei (Sausalito, CA: University Science Books).Google Scholar
Pandey, R., Das, R., Shaw, G., & Mondal, S. 2022a, ApJ, 925, 187.Google Scholar
Pandey, R., Habtie, G. R., Bandyopadhyay, R., Das, R., Teyssier, F., & Fló, J. G. 2022, MNRAS, 515, 4655.Google Scholar
Pavana, M., Raj, A., Bohlsen, T., Anupama, G. C., Gupta, R., & Selvakumar, G. 2020, MNRAS, 495, 2075.Google Scholar
Raj, A., Ashok, N. M., & Banerjee, D. P. K. 2011, MNRAS, 415, 3455.Google Scholar
Raj, A., Das, R. K., & Walter, F. M. 2017, ApJ, 835, 274.Google Scholar
Raj, A., Pavana, M., Kamath, U. S., Anupama, G. C., & Walter, F. M. 2018, AcA, 68, 79. ISSN: 00015237. https://doi.org/10.32023/0001-5237/68.1.4.Google Scholar
Rudy, R. J., Lynch, D. K., Russell, R. W., Crawford, K., Kaneshiro, B., Woodward, C. E., Sitko, M., & Skinner, M. 2008, International Astronomical Union Circular, 8952, 2.Google Scholar
Russell, R. W., Rudy, R. J., Lynch, D. K., Woodward, C. E., Marion, H., & Griep, D. 2008, V5579 Sagittarii, 8948, 1.Google Scholar
Sakon, I., et al. 2016, ApJ, 817, 145.Google Scholar
Schwarz, G. J., et al. 2011, ApJS, 197, 31.Google Scholar
Schwarz, G. J., Shore, S. N., Starrfield, S., Hauschildt, P. H., Della Valle, M., & Baron, E. 2001, MNRAS, 320, 103.Google Scholar
Shore, S. N., Paul Kuin, N., Mason, E., & De Gennaro Aquino, I. 2018, A&A, 619, A104.Google Scholar
Shore, S. N., et al. 2003. AJ, 125, 1507.Google Scholar
Shore, S. N. 2008, in Classical Novae, ed. Bode, M. F., & Evans, A., Astrophysics, Cambridge (Cambridge University Press), 194.Google Scholar
Starrfield, S., Bose, M., Iliadis, C., Raphael Hix, W., Woodward, C. E., & MarkWagner, R. 2020, ApJ, 895, 70. https://doi.org/10.3847/1538-4357/ab8d23.Google Scholar
Starrfield, S., Iliadis, Ch., & WRHix 2016, PASP, 128, 051001.Google Scholar
Strope, R. J., Schaefer, B. E., & Henden, A. A. 2010, AJ, 140, 34.Google Scholar
Wallace, P. T. 1994, Astronomical Data Analysis Software and Systems III, 61, 481.Google Scholar
Walter, F. M., Battisti, A., Towers, S. E., Bond, H. E., & Stringfellow, G. S. 2012, PASP, 124, 1057.Google Scholar
Warner, B. 1995, Cataclysmic Variable Stars, Vol. 28.Google Scholar
Warner, B. 2008, Cambridge Astrophysics Series, Vol. 43, 16.Google Scholar
Waters, L. B. F. M. 2004, in Astrophysics of Dust, ed. Witt, A. N., Clayton, G. C., & Draine, B. T., Society, Astronomical of the Pacific Conference Series, 309, 229.Google Scholar
Williams, R. E. 1994, ApJ, 426, 279 (ISSN 0004-637X).Google Scholar
Williams, R. E., Hamuy, M., Phillips, M. M., Heathcote, S. R., LisaWells, & Navarrete, M. 1991, ApJ, 376, 721 (ISSN 0004-637X).Google Scholar
Woodward, C. E., Shaw, G., Starrfield, S., Evans, A., & Page, K. L. 2024, ApJ, 968, 31. https://doi.org/10.3847/1538-4357/ad4097.Google Scholar
Wright, E. L., et al. 2010, AJ, 140, 1868.Google Scholar
Yamaoka, H., Haseda, K., & Fujii, M. 2008, Central Bureau Electronic Telegrams, Vol. 1344, 1.Google Scholar