J-PLUS: Turning Off the Bright Stars
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arXiv
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2025
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| author | Eskandarlou, Sepideh Akhlaghi, Mohammad Knapen, Johan H. López-Sanjuan, Carlos Infante-Sainz, Raúl Sánchez, Helena Domínguez Sharbaf, Zahra Ramió, Héctor Vázquez Ontiveros, Juan Antonio Fernández García, César Iñiguez Lorenzo, Tamara Civera Gallardo, David José Muniesa Coelho, Paula R. T. Ederoclite, Alessandro Varela, Jesus Jiménez-Esteban, Fran Cenarro, A. Javier Marín-Franch, Antonio Dupke, Renato A. Moles, Mariano Hernández-Monteagudo, Carlos T., Rahna P. Cristóbal-Hornillos, David Alcaniz, Jailson Sodré Jr., Laerte Angulo, Raul E. |
| author_facet | Eskandarlou, Sepideh Akhlaghi, Mohammad Knapen, Johan H. López-Sanjuan, Carlos Infante-Sainz, Raúl Sánchez, Helena Domínguez Sharbaf, Zahra Ramió, Héctor Vázquez Ontiveros, Juan Antonio Fernández García, César Iñiguez Lorenzo, Tamara Civera Gallardo, David José Muniesa Coelho, Paula R. T. Ederoclite, Alessandro Varela, Jesus Jiménez-Esteban, Fran Cenarro, A. Javier Marín-Franch, Antonio Dupke, Renato A. Moles, Mariano Hernández-Monteagudo, Carlos T., Rahna P. Cristóbal-Hornillos, David Alcaniz, Jailson Sodré Jr., Laerte Angulo, Raul E. |
| contents | Photometric surveys require precise point spread function (PSF) characterization, as it varies across filters and is crucial for accurate photometry and low surface brightness (LSB) studies. However, the small PSF size provided by default pipelines suits only barely resolved objects, making it difficult to analyze regions near bright stars (rendering those regions unusable). These components are then combined to generate a final PSF for each exposure and filter, spanning 15 mag arcsec-2 in surface brightness and 4 arcmin in radius in the broad bands. In narrow-band filters, the J-PLUS PSF exhibits two rings, whereas in broad-band filters, only one ring is observed. Additionally, the position of the ring shifts with filter wavelength: as the filters become redder, the ring radius increases. We find that there is no significant variation in the extended PSF observed as a function of time (within 2.5h) or position in the field of view. The radial profile of NGC 4212 (which is close to a star) is also studied before/after PSF-subtraction. We developed a novel method to determine the central coordinates of saturated stars, and classify stars without using Gaia magnitudes. Additionally, mirror reflections are automatically detected and masked. Furthermore, in combining different stars and various components of the PSF, we avoided the use of a fixed radius by introducing a new method that does not depend on radial measurements. Accurate characterization of the extended PSF and its subtraction improves sky subtraction, increases the effective area of the survey by about 10%, and enables the study of extended large LSB features in wide area surveys like J-PLUS. Our pipeline is published as free software (GNU GPLv3) an can be customized to other surveys such as J-PAS, where its impact will be even greater due to its depth. This paper is fully reproducible and produced from Commit 4860c70. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_12940 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | J-PLUS: Turning Off the Bright Stars Eskandarlou, Sepideh Akhlaghi, Mohammad Knapen, Johan H. López-Sanjuan, Carlos Infante-Sainz, Raúl Sánchez, Helena Domínguez Sharbaf, Zahra Ramió, Héctor Vázquez Ontiveros, Juan Antonio Fernández García, César Iñiguez Lorenzo, Tamara Civera Gallardo, David José Muniesa Coelho, Paula R. T. Ederoclite, Alessandro Varela, Jesus Jiménez-Esteban, Fran Cenarro, A. Javier Marín-Franch, Antonio Dupke, Renato A. Moles, Mariano Hernández-Monteagudo, Carlos T., Rahna P. Cristóbal-Hornillos, David Alcaniz, Jailson Sodré Jr., Laerte Angulo, Raul E. Instrumentation and Methods for Astrophysics Astrophysics of Galaxies Photometric surveys require precise point spread function (PSF) characterization, as it varies across filters and is crucial for accurate photometry and low surface brightness (LSB) studies. However, the small PSF size provided by default pipelines suits only barely resolved objects, making it difficult to analyze regions near bright stars (rendering those regions unusable). These components are then combined to generate a final PSF for each exposure and filter, spanning 15 mag arcsec-2 in surface brightness and 4 arcmin in radius in the broad bands. In narrow-band filters, the J-PLUS PSF exhibits two rings, whereas in broad-band filters, only one ring is observed. Additionally, the position of the ring shifts with filter wavelength: as the filters become redder, the ring radius increases. We find that there is no significant variation in the extended PSF observed as a function of time (within 2.5h) or position in the field of view. The radial profile of NGC 4212 (which is close to a star) is also studied before/after PSF-subtraction. We developed a novel method to determine the central coordinates of saturated stars, and classify stars without using Gaia magnitudes. Additionally, mirror reflections are automatically detected and masked. Furthermore, in combining different stars and various components of the PSF, we avoided the use of a fixed radius by introducing a new method that does not depend on radial measurements. Accurate characterization of the extended PSF and its subtraction improves sky subtraction, increases the effective area of the survey by about 10%, and enables the study of extended large LSB features in wide area surveys like J-PLUS. Our pipeline is published as free software (GNU GPLv3) an can be customized to other surveys such as J-PAS, where its impact will be even greater due to its depth. This paper is fully reproducible and produced from Commit 4860c70. |
| title | J-PLUS: Turning Off the Bright Stars |
| topic | Instrumentation and Methods for Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2510.12940 |