The PAU survey: classifying low-z SEDs using Machine Learning clustering
Author
González-Morán, A. L.; Haro, P. Arrabal; Muñoz-Tuñón, C.; Rodríguez-Espinosa, J. M.; Sánchez-Almeida, J.; Calhau, J.; Gaztañaga, E.; Castander, F. J.; Renard, P.; Cabayol, L.; Fernandez, E.; Padilla, C.; García-Bellido Capdevila, Juan; Miquel, R.; De Vicente, J.; Sanchez, E.; Sevilla-Noarbe, I.; Navarro-Girones, D.Entity
UAM. Departamento de Física TeóricaPublisher
Oxford University PressDate
2023-07-17Citation
10.1093/mnras/stad2123
Monthly Notices of the Royal Astronomical Society 524.3 (2023): 3569-3581
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stad2123Funded by
This work has been supported by the Ministry of Science and Innovation of Spain, project PID2019-107408GB-C43 (ESTALLIDOS), and the Government of the Canary Islands through EU FEDER funding, projects PID2020010050 and PID2021010077. This article is based on observations made in the Observatorios de Canarias of the Instituto de Astrofísica de Canarias (IAC) with the WHT operated on the island of La Palma by the Isaac Newton Group of Telescopes (ING) in the Observatorio del Roque de los Muchachos. The PAU Survey is partially supported by MINECO under grants CSD2007-00060, AYA2015-71825, ESP2017-89838, PGC2018-094773, PGC2018-102021, PID2019-111317GB, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509 and Juan de la Cierva fellowship and LACEGAL and EWC Marie Sklodowska-Curie grant No 734374 and no.776247 with ERDF funds from the EU Horizon 2020 Programme, some of which include ERDF funds from the European Union. IEEC and IFAE are partially funded by the CERCA and Beatriu de Pinos program of the Generalitat de Catalunya. Funding for PAUS has also been provided by Durham Univer sity (via the ERC StG DEGAS-259586), ETH Zurich, Leiden University (via ERC StG ADULT-279396 and Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512), University College London and from the European Union’s Horizon 2020 research and innovation programme under the grant agreement No 776247 EWC. The PAU data center is hosted by the Port d’Información Científica (PIC), maintained through a collaboration of CIEMAT and IFAE, with additional support from Universitat Autónoma de Barcelona and ERDF. We acknowledge the PIC services department team for their support and fruitful discussionsProject
Gobierno de España. PID2019-107408GB-C43; Gobierno de España. PID2020-010050; Gobierno de España. PID2021-010077; Gobierno de España. CSD2007-00060; Gobierno de España. AYA2015-71825; Gobierno de España. ESP2017-89838; Gobierno de España. PGC2018-094773-B-C32; Gobierno de España. PGC2018-102021-B-I00; Gobierno de España. PID2019-111317GB-C31; Gobierno de España. SEV-2016-0588; Gobierno de España. SEV-2016-0597; Gobierno de España. MDM-2015-0509; info:eu-repo/grantAgreement/EC/H2020/734374/EU//LACEGAL; info:eu-repo/grantAgreement/EC/H2020/776247/EU//EWCEditor's Version
https://doi.org/10.1093/mnras/stad2123Subjects
Fundamental Parameters; Galaxies: Star Formation; Photometry; Starburst; Stellar Content; Star Formation; Galactic Evolution; Galaxies; FísicaNote
This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society 524.3 (2023): 3569-3581 is available online at: https://academic.oup.com/mnras/article-abstract/524/3/3569/7225529?redirectedFrom=fulltextRights
© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical SocietyAbstract
We present an application of unsupervised Machine Learning clustering to the PAU survey of galaxy spectral energy distribution (SED) within the COSMOS field. The clustering algorithm is implemented and optimized to get the relevant groups in the data SEDs. We find 12 groups from a total number of 5234 targets in the survey at 0.01 < z < 0.28. Among the groups, 3545 galaxies (68 per cent) show emission lines in the SEDs. These groups also include 1689 old galaxies with no active star formation. We have fitted the SED to every single galaxy in each group with CIGALE. The mass, age, and specific star formation rates (sSFR) of the galaxies range from 0.15 < age/Gyr <11; 6 < log (M/M⊙) <11.26, and -14.67 < log (sSFR/yr-1) <-8. The groups are well-defined in their properties with galaxies having clear emission lines also having lower mass, are younger and have higher sSFR than those with elliptical like patterns. The characteristic values of galaxies showing clear emission lines are in agreement with the literature for starburst galaxies in COSMOS and GOODS-N fields at low redshift. The star-forming main sequence, sSFR versus stellar mass and UVJ diagram show clearly that different groups fall into different regions with some overlap among groups. Our main result is that the joint of low- resolution (R ∼50) photometric spectra provided by the PAU survey together with the unsupervised classification provides an excellent way to classify galaxies. Moreover, it helps to find and extend the analysis of extreme ELGs to lower masses and lower SFRs in the local Universe
Files in this item
Google Scholar:González-Morán, A. L.
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Haro, P. Arrabal
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Muñoz-Tuñón, C.
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Rodríguez-Espinosa, J. M.
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Sánchez-Almeida, J.
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Calhau, J.
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Gaztañaga, E.
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Castander, F. J.
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Renard, P.
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Cabayol, L.
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Fernandez, E.
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Padilla, C.
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García-Bellido Capdevila, Juan
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Miquel, R.
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De Vicente, J.
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Sanchez, E.
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Sevilla-Noarbe, I.
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Navarro-Girones, D.
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