{"work":{"id":"de98c48d-2146-4d71-8546-fe4725d1ca87","openalex_id":"https://openalex.org/W2519918655","doi":"10.1093/mnras/stw2231","arxiv_id":"1612.01187","raw_key":null,"title":"UV-extended E-MILES stellar population models: young components in massive early-type galaxies","authors":[{"given":"A.","family":"Vazdekis","sequence":"first","affiliation":[]},{"given":"M.","family":"Koleva","sequence":"additional","affiliation":[]},{"given":"E.","family":"Ricciardelli","sequence":"additional","affiliation":[]},{"given":"B.","family":"Röck","sequence":"additional","affiliation":[]},{"given":"J.","family":"Falcón-Barroso","sequence":"additional","affiliation":[]}],"authors_text":"Vazdekis, A","year":2016,"venue":"astro-ph.GA","abstract":"We present UV-extended E-MILES stellar population synthesis models covering the spectral range 1680-50000A at moderately high resolution. We employ the NGSL space-based stellar library to compute spectra of single-age, single-metallicity stellar populations in the wavelength range from 1680 to 3540A. These models represent a significant improvement in resolution and age/metallicity coverage over previous studies based on earlier space-based libraries. These model spectra were joined with those we computed in the visible using MILES, and other empirical libraries for redder wavelengths. The models span the metallicity range -1.79<[M/H]<+0.26 and ages above 30 Myr, for a suite of IMF types with varying slopes. We focus on the behaviour of colours, spectra and line-strength indices in the UV range as a function of relevant stellar population parameters. Whereas some indices strengthen with increasing age and metallicity, as most metallicity indicators in the visible, other indices peak around 3 Gyr for metal-rich stellar populations, such as Mg at 2800A. Our models provide reasonably good fits to the integrated colours and most line-strengths of the stellar clusters of the Milky-Way and LMC. Our full-spectrum fits in the UV range for a representative set of ETGs of varying mass yield age and metallicity estimates in very good agreement with those obtained in the optical range. The comparison of UV colours and line-strengths of massive ETGs with our models reveals the presence of young stellar components, with ages in the range 0.1-0.5 Gyr and mass fractions 0.1-0.5%, on the top of an old stellar population.","external_url":"https://arxiv.org/abs/1612.01187","cited_by_count":453,"metadata_source":"pith","metadata_fetched_at":"2026-07-02T18:17:16.567934+00:00","pith_arxiv_id":"1612.01187","created_at":"2026-05-08T16:48:28.005932+00:00","updated_at":"2026-07-02T18:17:16.567934+00:00","title_quality_ok":true,"display_title":"2016, MNRAS, 463, 3409, doi: 10.1093/mnras/stw2231","render_title":"2016, MNRAS, 463, 3409, doi: 10.1093/mnras/stw2231"},"hub":{"state":{"work_id":"de98c48d-2146-4d71-8546-fe4725d1ca87","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":18,"external_cited_by_count":453,"distinct_field_count":4,"first_pith_cited_at":"2025-08-14T18:00:06+00:00","last_pith_cited_at":"2026-07-01T13:24:29+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-07-04T22:07:08.808735+00:00","tier_text":"hub"},"tier":"hub","role_counts":[],"polarity_counts":[],"runs":{},"summary":{},"graph":{},"authors":[]}}