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Observations of galactic and extragalactic novae

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Abstract

The recent GAIA DR2 measurements of distances to galactic novae have allowed to re-analyse some properties of nova populations in the Milky Way and in external galaxies on new and more solid empirical bases. In some cases, we have been able to confirm results previously obtained, such as the concept of nova populations into two classes of objects, that is disk and bulge novae and their link with the Tololo spectroscopic classification in Fe II and He/N novae. The recent and robust estimates of nova rates in the Magellanic Clouds galaxies provided by the OGLE team have confirmed the dependence of the normalized nova rate (i.e., the nova rate per unit of luminosity of the host galaxy) with the colors and/or class of luminosity of the parent galaxies. The nova rates in the Milky Way and in external galaxies have been collected from literature and critically discussed. They are the necessary ingredient to asses the contribution of novae to the nucleosynthesis of the respective host galaxies, particularly to explain the origin of the overabundance of lithium observed in young stellar populations. A direct comparison between distances obtained via GAIA DR2 and maximum magnitude vs. rate of decline (MMRD) relationship points out that the MMRD can provide distances with an uncertainty better than 30%. Multiwavelength observations of novae along the whole electromagnetic spectrum, from radio to gamma rays, have revealed that novae undergo a complex evolution characterized by several emission phases and a non-spherical geometry for the nova ejecta.

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Notes

  1. Out of 37 that constitute his entire work

  2. We derived the GAIA DR2 distance of V1500 Cyg using the parallax provided in the GAIA DR2 database and using the formula given in Bailer-Jones et al. (2018), see also Muraveva et al. (2018). The GAIA DR2 archive is available at https://gea.esac.esa.int/archive/

  3. http://leda.univ-lyon1.fr/

  4. The GAIA DR2 distance of V1500 Cyg used in this paper, \(d = 1.29 \pm 0.31\), can be derived using the parallex measurement as provided in the GAIA DR2 data archive: https://gea.esac.esa.int/archive/.

  5. see Hyperleda archive: http://leda.univ-lyon1.fr

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Acknowledgements

The authors thank the referees for their constructive criticisms that have significantly improved the presentation and discussion of the data. We are also very grateful to Bob Williams for giving us valuable comments on the manuscript and to Roberto Gilmozzi and Tatiana Muraveva for helpful discussions about nova parallaxes. We also thank Martín Guerrero, Patrick Schmeer and Ken Croswell for further insights. MDV is deeply grateful to Prof. Leonida Rosino for having introduced him to the realm of nova physics and to Hilmar Duerbeck for the many nights shared at the La Silla telescopes. MDV thanks ESO-Garching, where this manuscript was drafted for the creative and friendly atmosphere. LI was supported by grants from VILLUM FONDEN (project number 16599 and 25501). LI also acknowledges support from funding associated with Juan de la Cierva Incorporación fellowship IJCI-2016-30940.

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Authors and Affiliations

  1. INAF-Capodimonte, Naples, Italy

    Massimo Della Valle

  2. ESO, Garching, Germany

    Massimo Della Valle

  3. DARK/NBI, Copenhagen, Denmark

    Luca Izzo

  4. IAA/CSIC, Granada, Spain

    Luca Izzo

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  1. Massimo Della Valle
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  2. Luca Izzo
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Correspondence to Massimo Della Valle.

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Appendix: Tables

Appendix: Tables

Table 9 The list of novae (Col. 1), their distance as measured from GAIA DR2 (Col. 2), the V magnitude at maximum (Col. 3) and at minimum (Col. 4), the corresponding \(t_2\) and \(t_3\) values (Cols. 5 and 6) and the Galactic longitude l and latitude b (Cols. 7 and 8)
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Table 10 The list of absortions \(A_\mathrm{V}\) used in this work
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Table 11 The average expansion velocity and spectroscopic type for each nova shown in Fig. 28
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Table 12 Distance measured from the nebular parallax method (Col. 2) by Downes and Duerbeck (2000) compared with the recent GAIA DR2 measurements (Col. 3) as given in S18 and SG19
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Table 13 List of M31 novae used in this work. Data from Arp (1956), Rosino (1964), Rosino (1973) and Rosino et al. (1989)
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Table 14 List of LMC novae used in this work. Data from Capaccioli et al. (1990) and Shafter (2013)
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Table 15 List of M31 novae taken from Kasliwal et al. (2011) and Cao et al. (2012)
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Table 16 List of M31 novae taken from Hubble (1929)
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Table 17 List of Virgo novae used in this work
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Della Valle, M., Izzo, L. Observations of galactic and extragalactic novae. Astron Astrophys Rev 28, 3 (2020). https://doi.org/10.1007/s00159-020-0124-6

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