Hostname: page-component-cd9895bd7-dk4vv Total loading time: 0 Render date: 2024-12-25T05:03:49.026Z Has data issue: false hasContentIssue false
  • English
  • Français

Bar pattern speed at z∼1–2 to explore challenges of the Standard Cosmology

Published online by Cambridge University Press:  13 February 2024

Virginia Cuomo Open the ORCID record for Virginia Cuomo [Opens in a new window] ,
Mahmood Roshan ,
J. Alfonso L. Aguerri  and
Lorenzo Morelli
Virginia Cuomo*
Affiliation:
Instituto de Astronoma y Ciencias Planetarias, Universidad de Atacama, Avenida Copayapu 485, Copiapó, Atacama 1530000, Chile
Mahmood Roshan
Affiliation:
Department of Physics, Faculty of Science, Ferdowsi University of Mashhad, P.O. Box 1436, Mashhad, Iran
J. Alfonso L. Aguerri
Affiliation:
Instituto de Astrofsica de Canarias, calle Va Láctea s/n, 38205 La Laguna, Tenerife, Spain Departamento de Astrofsica, Universidad de La Laguna, Avenida Astrofsico Francisco Sánchez s/n, 38206 La Laguna, Tenerife, Spain
Lorenzo Morelli
Affiliation:
Instituto de Astronoma y Ciencias Planetarias, Universidad de Atacama, Avenida Copayapu 485, Copiapó, Atacama 1530000, Chile
*
email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Stellar bars drive the galaxy secular evolution. While rotating around the galaxy centre with a given angular frequency, the bar pattern speed, they sweep material and modify the galaxy structure. In the LCDM model, bars are expected to slow down by exchanging angular momentum with the other omponents and/or through dynamical friction exerted by the dark matter halo. The only direct method to derive the bar pattern speed, the Tremaine-Weinberg method, revealed that real bars rotate fast, stressing a tension between the observations, conducted to date in the local universe, and the LCDM model. Measuring the bar pattern speed to bars up to z∼1-2 will reveal if the expected bar evolutionary path is actually taking place and/or to confirm if the dark matter is able to exert friction. Using high resolution N-body simulations we tested the applicability of the Tremaine-Weinberg method to deep spectroscopy of the NIRSpec@JWST for a sample of bars at z∼1-2. Our analysis can be used to prepare an observational proposal to get dedicated data.

Keywords

galaxies: evolutiongalaxies: generalgalaxies: structuredark matter
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S377: Early Disk-Galaxy Formation from JWST to the Milky Way , December 2022 , pp. 48 - 52
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Athanassoula 1992, MNRAS, 259, 345 CrossRefGoogle Scholar
Athanassoula, Machado, Rodionov 2013, MNRAS, 429, 1949CrossRefGoogle Scholar
Buttitta et al. 2022, A&A, 664, L10 CrossRefGoogle Scholar
Contopoulos 1981, A&A, 102, 265 CrossRefGoogle Scholar
Cuomo et al. 2020, A&A, 641, A111 Google Scholar
Debattista & Sellwood 2000, ApJ, 543, 704 Google Scholar
Erwin 2018, MNRAS, 474, 5372 Google Scholar
Guo et al. 2022, arXiv e-prints, arXiv:2210.08658Google Scholar
James & Percival 2016, MNRAS, 457, 917 Google Scholar
Kroupa 2012, PASA, 29, 395 CrossRefGoogle Scholar
Roshan et al. 2021, MNRAS, 508, 926 Google Scholar
Tremaine & Weinberg 1984, ApJ, 282, L5 CrossRefGoogle Scholar