Mapping Hα excess candidate point sources in the southern hemisphere using S-PLUS data

¹ Instituto de Astrofísica de La Plata (CCT La Plata – CONICET – UNLP), B1900FWA, La Plata, Argentina
² Departamento de Astronomia, Instituto de Astronomia, Geofísica e Ciências Atmosféricas da USP, Cidade Universitária, 05508-900 São Paulo, SP, Brazil
³ Departamento de Física, Universidade Federal de Sergipe, Av. Marechal Rondon S/N, 49100-000 São Cristóvão, SE, Brazil
⁴ Observatório Nacional, Rua Gal. José Cristino 77, 20921-400 Rio de Janeiro, RJ, Brazil
⁵ Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, GR 15236 Penteli, Greece
⁶ Universidade Federal do Rio de Janeiro, Observatório do Valongo, Ladeira do Pedro Antônio, 43, Saúde CEP 20080-090 Rio de Janeiro, RJ, Brazil
⁷ Instituto de Astrofísica de Andalucía, CSIC, Apt 3004, 18080 Granada, Spain
⁸ Instituto de Física Aplicada a las Ciencias y las Tecnologías, Universidad de Alicante, San Vicent del Raspeig, 03080 Alicante, Spain
⁹ Instituto de Astronomía y Ciencias Planetarias, Universidad de Atacama, Copayapu 485, Copiapó, Chile
¹⁰ Millennium Institute of Astrophysics, Nuncio Monseñor Sotero Sanz 100, Of. 104, Providencia, Santiago, Chile
¹¹ Departmento de Astronomía, Universidad de La Serena, Avenida Raúl Bitrán 1305, La Serena, Chile
¹² International Gemini Observatory/NSF NOIRLab, Casilla 603, La Serena, Chile
¹³ Departamento de Física, Universidade Federal de Santa Catarina, Florianópolis, SC 88040-900, Brazil
¹⁴ Rubin Observatory Project Office, 950 N. Cherry Ave., Tucson, AZ 85719, USA
¹⁵ The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St, Pasadena, CA 91101, USA

^★ Corresponding author; gsotoangel@fcaglp.unlp.edu.ar

Received: 26 November 2024
Accepted: 26 January 2025

Abstract

Context. We use the Southern Photometric Local Universe Survey (S-PLUS) Fourth Data Release (DR4) to identify and classify Hα excess point source candidates in the southern sky. This approach combines photometric data from 12 S-PLUS filters with machine learning techniques to improve source classification and advance our understanding of Hα-related phenomena.

Aims. Our goal is to enhance the classification of Hα excess point sources by distinguishing between Galactic and extragalactic objects, particularly those with redshifted emission lines, and to identify sources where the Hα excess is associated with variability phenomena, such as short-period RR Lyrae stars.

Methods. We selected Hα excess candidates using the (r − J0660) versus (r − i) colour–colour diagram from the S-PLUS main survey (MS) and Galactic Disk Survey (GDS). For the MS sample, dimensionality reduction was achieved using UMAP, followed by HDBSCAN clustering. We refined this by incorporating infrared data, which improved the separation of source types. A random forest model was then trained on the clustering results to identify key colour features for the classification of Hα excess sources. New effective colour–colour diagrams were constructed by combining data from S-PLUS MS and infrared data. These diagrams, alongside tentative colour criteria, offer a preliminary classification of Hα excess sources without the need for complex algorithms.

Results. Combining multi-wavelength photometric data with machine learning techniques significantly improved the classification of Hα excess sources. We identified 6956 sources with an excess in the J0660 filter, and cross-matching with SIMBAD allowed us to explore the types of objects present in our catalogue, including emission-line stars, young stellar objects, nebulae, stellar binaries, cataclysmic variables, variable stars, and extragalactic sources such as Quasi-Stellar Objects (QSOs), Active Galactic Nuclei (AGN), and galaxies. The cross-match also revealed X-ray sources, transients, and other peculiar objects. Using S-PLUS colours and machine learning, we successfully separated RR Lyrae stars from other Galactic stars and from extragalactic objects. Additionally, we achieved a clear separation between Galactic and extragalactic sources. However, distinguishing cataclysmic variables from QSOs at specific redshifts remained challenging. Incorporating infrared data refined the classification, enabling us to separate Galactic from extragalactic sources and to distinguish cataclysmic variables from QSOs. The Random Forest model, trained on HDBSCAN results, highlighted key colour features that distinguish the different classes of Hα excess sources, providing a robust framework for future studies, such as follow-up spectroscopy.