> Details

Ramón-Pérez, Marina; Bongiovanni, Ángel; Pérez García, Ana María; Cepa, Jordi; Lara-López, Maritza A.; de Diego, José A.; Alfaro, Emilio; Castañeda, Héctor O.; Cerviño, Miguel; Fernández-Lorenzo, Mirian; Gallego, Jesús; González, J. Jesús; González-Serrano, J. Ignacio; Nadolny, Jakub; Oteo Gómez, Iván; Pérez Martínez, Ricardo; Pintos-Castro, Irene; Pović, Mirjana; Sánchez-Portal, Miguel

The OTELO survey : II. The faint-end of the Hα luminosity function at z ∼ 0.40 : II. The faint-end of the H<i>α</i> luminosity function at <i>z</i> ∼ 0.40

Reference
management

Bookmarks

Remove from
bookmarks

Share this on Whatsapp

Close

Bookmarks



You can manage bookmarks using lists, please log in to your user account for this.
  • Media type: E-Article
  • Title: The OTELO survey : II. The faint-end of the Hα luminosity function at z ∼ 0.40 : II. The faint-end of the H<i>α</i> luminosity function at <i>z</i> ∼ 0.40
  • Contributor: Ramón-Pérez, Marina; Bongiovanni, Ángel; Pérez García, Ana María; Cepa, Jordi; Lara-López, Maritza A.; de Diego, José A.; Alfaro, Emilio; Castañeda, Héctor O.; Cerviño, Miguel; Fernández-Lorenzo, Mirian; Gallego, Jesús; González, J. Jesús; González-Serrano, J. Ignacio; Nadolny, Jakub; Oteo Gómez, Iván; Pérez Martínez, Ricardo; Pintos-Castro, Irene; Pović, Mirjana; Sánchez-Portal, Miguel
  • imprint: EDP Sciences, 2019
  • Published in: Astronomy & Astrophysics
  • Language: Not determined
  • DOI: 10.1051/0004-6361/201833295
  • ISSN: 0004-6361; 1432-0746
  • Keywords: Space and Planetary Science ; Astronomy and Astrophysics
  • Origination:
  • Footnote:
  • Description: <jats:p><jats:italic>Aims</jats:italic>. We take advantage of the capability of the OTELO survey to obtain the H<jats:italic>α</jats:italic> luminosity function (LF) at z ∼ 0.40. Because of the deepest coverage of OTELO, we are able to determine the faint end of the LF, and thus better constrain the star formation rate and the number of galaxies at low luminosities. The AGN contribution to this LF is estimated as well.</jats:p> <jats:p><jats:italic>Methods</jats:italic>. We make use of the multiwavelength catalogue of objects in the field compiled by the OTELO survey, which is unique in terms of minimum flux and equivalent width. We also take advantage of the pseudo-spectra built for each source, which allow the identification of emission lines and the discrimination of different types of objects.</jats:p> <jats:p><jats:italic>Results</jats:italic>. The H<jats:italic>α</jats:italic> luminosity function at <jats:italic>z</jats:italic> ∼ 0.40 is obtained, which extends the current faint end by almost 1 dex, reaching minimal luminosities of log<jats:sub>10</jats:sub><jats:italic>L</jats:italic><jats:sub>lim</jats:sub> = 38.5 erg s<jats:sup>−1</jats:sup> (or ∼0.002 <jats:italic>M</jats:italic><jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup>). The AGN contribution to the total H<jats:italic>α</jats:italic> luminosity is estimated. We find that no AGN should be expected below a luminosity of log<jats:sub>10</jats:sub><jats:italic>L</jats:italic> = 38.6 erg s<jats:sup>−1</jats:sup>. From the sample of non-AGN (presumably, pure SFG) at <jats:italic>z</jats:italic> ∼ 0.40 we estimated a star formation rate density of <jats:italic>ρ</jats:italic><jats:sub>SFR</jats:sub> = 0.012 ± 0.005 <jats:italic>M</jats:italic><jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup> Mpc<jats:sup>−3</jats:sup>.</jats:p>
  • Access State: Open Access