Hostname: page-component-54dcc4c588-rz4zl Total loading time: 0 Render date: 2025-10-07T00:33:06.756Z Has data issue: false hasContentIssue false
  • English
  • Français

The structure of emission lines in planetary nebulae at very high spectral resolution

Published online by Cambridge University Press:  06 October 2025

Michael G. Richer Open the ORCID record for Michael G. Richer [Opens in a new window] ,
José Alberto López ,
Anabel Arrieta Open the ORCID record for Anabel Arrieta [Opens in a new window] ,
Lorena Arias Open the ORCID record for Lorena Arias [Opens in a new window]  and
Silvia Torres-Peimbert Open the ORCID record for Silvia Torres-Peimbert [Opens in a new window]
Michael G. Richer
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónomo de México, Apartado Postal 106, CP 22800 Ensenada, Baja California, México
José Alberto López
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónomo de México, Apartado Postal 106, CP 22800 Ensenada, Baja California, México
Anabel Arrieta
Affiliation:
Departamento de Física y Matemáticas, Universidad Iberoamericana, Prolongación Paseo de la Reforma 880, Lomas de Santa Fe, CP 01210, Ciudad de México, México
Lorena Arias
Affiliation:
Departamento de Física y Matemáticas, Universidad Iberoamericana, Prolongación Paseo de la Reforma 880, Lomas de Santa Fe, CP 01210, Ciudad de México, México
Silvia Torres-Peimbert
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónomo de México, Apartado Postal 70-264, CP 04510 Ciudad de México, México
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.

We present spectroscopy of NGC 3242, NGC 6153, and NGC 7009 at very high spectral resolution (λ / δλ = 75, 000 – 100, 000) obtained with the Manchester Echelle Spectrograph at the 2.1m telescope of the Observatorio Astronómico Nacional on the Sierra San Pedro Mártir. We study the kinematics of the plasma within the nebular shells, decomposing the observed line profiles considering the microscopic, macroscopic, and observational processes that broaden them. The residual kinematic structure, defined as the sum of velocity gradients, kinematic structure, and seeing dominates the broadening of the lines of heavy elements. We estimate the effect of velocity gradients, finding that it can account only for a minority of this residual kinematic structure. Whatever the origin of this residual kinematic structure, it is an important component of the kinematics of the ionized plasma within the nebular shell and implies an important energy source that is not contemplated in photoionization models of planetary nebulae.

Keywords

planetary nebulaespectroscopykinematicsturbulence

Information

Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S384: Planetary Nebulae: A Universal Toolbox in the Era of Precision Astrophysics , December 2023 , pp. 136 - 142
Check for updates
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2025. Published by Cambridge University Press on behalf of International Astronomical Union

References

Clegg, R. E. S., Miller, S., Storey, P. J., & Kisielius, R. 1999, A&AS, 135, 359 CrossRefGoogle Scholar
Dekker, H., D’Odorico, S., Kaufer, A., Delabre, B., & Kotzlowski, H. 2000, Proc. SPIE, 4008, 534 Google Scholar
García-DGarcía-Díaz, Ma. T., Henney, W. J., López, J. A., & Doi, T. 2008, RMxAA, 44, 181 Google Scholar
Lang, K. R. 1980, Astrophysical Formulae (Berlin: Springer)CrossRefGoogle Scholar
Massey, P., Valdes, F., & Barnes, J. 1992, IRAF User Guide 2B, A User’s Guide to Reducing Slit Spectra with IRAF (Tucson, AZ: National Optical Astronomy Observatory)Google Scholar
Meaburn, J., López, J. A., Gutiérrez, L., et al. 2003, RMxAA, 39, 185 Google Scholar
Perinotto, M., Schönberner, D., Steffen, M., & Calonaci, C. 2004, A&A, 414, 993 CrossRefGoogle Scholar
Pradhan, A. K., & Nahar, S. N. 2011, Atomic Astrophysics and Spectroscopy (Cambridge University Press)CrossRefGoogle Scholar
Richer, M. G., Arrieta, A., Arias, L., et al. 2022, AJ, 164, 243 CrossRefGoogle Scholar
Richer, M. G., Suárez, G., López, J. A., & García-Díaz, Ma. T 2017, AJ, 153, 140 CrossRefGoogle Scholar
Sabbadin, F., Turatto, M., Benedetti, S., Ragazzoni, R., & Cappellaro, E. 2008, A&A, 488, 225 CrossRefGoogle Scholar
Su, K. Y., Chu, Y.-H., Rieke, G. H., et al. 2007, ApJL, 657, 41 CrossRefGoogle Scholar
Villaver, E., Garca-Segura, G., & Manchado, A. 2002, ApJ, 581, 1204 CrossRefGoogle Scholar
Wesson, R., Matsuura, M., Zijlstra, A. A., et al. 2023, arXiv:2308.09027 Google Scholar
Wilson, O. C. 1950, ApJ, 111, 279 CrossRefGoogle Scholar