Euclid: Searching for pair-instability supernovae with the Deep Survey
Abstract
Pair-instability supernovae are theorized supernovae that have not yet been observationally confirmed. They are predicted to exist in low-metallicity environments. Because overall metallicity becomes lower at higher redshifts, deep near-infrared transient surveys probing high-redshift supernovae are suitable to discover pair-instability supernovae. The Euclid satellite, which is planned to be launched in 2023, has a near-infrared wide-field instrument that is suitable for a high-redshift supernova survey. The Euclid Deep Survey is planned to make regular observations of three Euclid Deep Fields (40 deg2 in total) spanning the Euclid's 6 year primary mission period. While the observations of the Euclid Deep Fields are not frequent, we show that the predicted long duration of pair-instability supernovae would allow us to search for high-redshift pair-instability supernovae with the Euclid Deep Survey. Based on the current observational plan of the Euclid mission, we conduct survey simulations in order to estimate the expected numbers of pair-instability supernova discoveries. We find that up to several hundred pair-instability supernovae at z < ~ 3.5 can be discovered within the Euclid Deep Survey. We also show that pair-instability supernova candidates can be efficiently identified by their duration and color that can be determined with the current Euclid Deep Survey plan. We conclude that the Euclid mission can lead to the first confirmation of pair-instability supernovae if their event rates are as high as those predicted by recent theoretical studies. We also update the expected numbers of superluminous supernova discoveries in the Euclid Deep Survey based on the latest observational plan.
Keywords
Cite
@article{arxiv.2204.08727,
title = {Euclid: Searching for pair-instability supernovae with the Deep Survey},
author = {T. J. Moriya and C. Inserra and M. Tanaka and E. Cappellaro and M. Della Valle and I. Hook and R. Kotak and G. Longo and F. Mannucci and S. Mattila and C. Tao and B. Altieri and A. Amara and N. Auricchio and D. Bonino and E. Branchini and M. Brescia and J. Brinchmann and S. Camera and V. Capobianco and C. Carbone and J. Carretero and M. Castellano and S. Cavuoti and A. Cimatti and R. Cledassou and G. Congedo and C. J. Conselice and L. Conversi and Y. Copin and L. Corcione and F. Courbin and M. Cropper and A. Da Silva and H. Degaudenzi and M. Douspis and F. Dubath and C. A. J. Duncan and X. Dupac and S. Dusini and A. Ealet and S. Farrens and S. Ferriol and M. Frailis and E. Franceschi and M. Fumana and B. Garilli and W. Gillard and B. Gillis and C. Giocoli and A. Grazian and F. Grupp and S. V. H. Haugan and W. Holmes and F. Hormuth and A. Hornstrup and K. Jahnke and S. Kermiche and A. Kiessling and M. Kilbinger and T. Kitching and H. Kurki-Suonio and S. Ligori and P. B. Lilje and I. Lloro and E. Maiorano and O. Mansutti and O. Marggraf and K. Markovic and F. Marulli and R. Massey and H. J. McCracken and M. Melchior and M. Meneghetti and G. Meylan and M. Moresco and L. Moscardini and E. Munari and S. M. Niemi and C. Padilla and S. Paltani and F. Pasian and K. Pedersen and V. Pettorino and M. Poncet and L. Popa and F. Raison and J. Rhodes and G. Riccio and E. Rossetti and R. Saglia and B. Sartoris and P. Schneider and A. Secroun and G. Seidel and C. Sirignano and G. Sirri and L. Stanco and P. Tallada-Crespí and A. N. Taylor and I. Tereno and R. Toledo-Moreo and F. Torradeflot and Y. Wang and G. Zamorani and J. Zoubian and S. Andreon and V. Scottez and P. W. Morris},
journal= {arXiv preprint arXiv:2204.08727},
year = {2023}
}
Comments
12 pages, 13 figures, 2 tables, accepted by Astronomy & Astrophysics