WHaD diagram: Classifying the ionizing source with one single emission line

¹ Instituto de Astronomía, Universidad Nacional Autonóma de México, A.P. 106, Ensenada, 22800 BC, Mexico
e-mail: sfsanchez@astro.unam.mx
² Instituto de Astronomía, Universidad Nacional Autonóma de México, A.P. 70-264, 04510 CDMX, Mexico
³ Instituto de Astrofísica de Canarias, La Laguna, Tenerife 38200, Spain
⁴ Instituto de Radioastronomía and Astrofísica (IRyA-UNAM), 3-72 (Xangari), 8701 Morelia, Mexico
⁵ Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Spain
⁶ Department of Astronomy, Indiana University, Bloomington, IN 47405, USA

Received: 11 August 2023
Accepted: 17 November 2023

Abstract

Context. The usual approach to classify the ionizing source using optical spectroscopy is based on the use of diagnostic diagrams that compare the relative strength of pairs of collisitional metallic lines (e.g., [O III] and [N II]) to recombination hydrogen lines (e.g., Hβ and Hα). Despite it having been accepted as the standard procedure, it presents known problems, including confusion regimes and/or limitations related to the required signal-to-noise (S/N) of the emission lines involved. These problems not only affect our intrinsic understanding of the interstellar medium and its properties, but also the fundamental galaxy properties, such as the star formation rate and the oxygen abundance. This raises key questions related to the fraction of active galactic nuclei and other essential parameters.

Aims. We attempt to minimize the problems introduced by the use of these diagrams, in particular, their implementation when the available information is limited due to either the fact that not all lines are available or they do not have the required S/N value.

Methods. We explored the existing alternatives in the literature to minimize the confusion among different ionizing sources. We have proposed a new, simple diagram that uses the equivalent width and the velocity dispersion from one single emission line, Hα, to classify the ionizing sources.

Results. We used aperture-limited and spatially resolved spectroscopic data from the nearby Universe (z ∼ 0.01) to demonstrate that the new diagram, which we have named WHaD, segregates the different ionizing sources in a more efficient way than earlier procedures. A new set of regions have been defined in this diagram to select among different ionizing sources.

Conclusions. The new proposed diagram is well positioned to assist in determining the ionizing source when only Hα is available or when the S/N of the emission lines is too low to obtain reliable fluxes for the weakest emission lines in classical diagnostic diagrams (e.g., Hβ).