The OTELO survey: II. The faint-end of the Hα luminosity function at z ∼ 0.40

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

doi:10.1051/0004-6361/201833295

The OTELO survey: II. The faint-end of the Hα luminosity function at z ∼ 0.40

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

Escuela Superior de Física y Matemáticas (ESFM)

Research output: Contribution to journal › Article › peer-review

1 Scopus citations

Abstract

Aims. We take advantage of the capability of the OTELO survey to obtain the Hα 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. Methods. 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. Results. The Hα luminosity function at z ∼ 0:40 is obtained, which extends the current faint end by almost 1 dex, reaching minimal luminosities of log10 Llim = 38:5 erg s-1 (or ∼0:002 M yr-1). The AGN contribution to the total Hα luminosity is estimated. We find that no AGN should be expected below a luminosity of log10 L = 38:6 erg s-1. From the sample of non-AGN (presumably, pure SFG) at z ∼ 0:40 we estimated a star formation rate density of πSFR = 0:012 ± 0:005 M yr-1 Mpc-3.c ESO 2019.

Original language	English
Article number	A10
Journal	Astronomy and Astrophysics
Volume	631
DOIs	https://doi.org/10.1051/0004-6361/201833295
State	Published - 1 Nov 2019

Keywords

Active - galaxies
Luminosity function, mass function
Star formation - galaxies
Surveys - galaxies

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10.1051/0004-6361/201833295

Cite this

Ramón-Pérez, M., Bongiovanni, Á., García, A. M. P., Cepa, J., Lara-López, M. A., De Diego, J. A., Alfaro, E., Castañeda, H. O., Cerviño, M., Fernández-Lorenzo, M., Gallego, J., Jesús González, J., Ignacio González-Serrano, J., Nadolny, J., Gómez, I. O., Martínez, R. P., Pintos-Castro, I., Pović, M., & Sánchez-Portal, M. (2019). The OTELO survey: II. The faint-end of the Hα luminosity function at z ∼ 0.40. Astronomy and Astrophysics, 631, Article A10. https://doi.org/10.1051/0004-6361/201833295

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title = "The OTELO survey: II. The faint-end of the Hα luminosity function at z ∼ 0.40",

abstract = "Aims. We take advantage of the capability of the OTELO survey to obtain the Hα 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. Methods. 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. Results. The Hα luminosity function at z ∼ 0:40 is obtained, which extends the current faint end by almost 1 dex, reaching minimal luminosities of log10 Llim = 38:5 erg s-1 (or ∼0:002 M yr-1). The AGN contribution to the total Hα luminosity is estimated. We find that no AGN should be expected below a luminosity of log10 L = 38:6 erg s-1. From the sample of non-AGN (presumably, pure SFG) at z ∼ 0:40 we estimated a star formation rate density of πSFR = 0:012 ± 0:005 M yr-1 Mpc-3.c ESO 2019.",

keywords = "Active - galaxies, Luminosity function, mass function, Star formation - galaxies, Surveys - galaxies",

author = "Marina Ram{\'o}n-P{\'e}rez and {\'A}ngel Bongiovanni and Garc{\'i}a, {Ana Mar{\'i}a P{\'e}rez} and Jordi Cepa and Lara-L{\'o}pez, {Maritza A.} and {De Diego}, {Jos{\'e} A.} and Emilio Alfaro and Casta{\~n}eda, {H{\'e}ctor O.} and Miguel Cervi{\~n}o and Mirian Fern{\'a}ndez-Lorenzo and Jes{\'u}s Gallego and {Jes{\'u}s Gonz{\'a}lez}, J. and {Ignacio Gonz{\'a}lez-Serrano}, J. and Jakub Nadolny and G{\'o}mez, {Iv{\'a}n Oteo} and Mart{\'i}nez, {Ricardo P{\'e}rez} and Irene Pintos-Castro and Mirjana Povi{\'c} and Miguel S{\'a}nchez-Portal",

year = "2019",

month = nov,

day = "1",

doi = "10.1051/0004-6361/201833295",

language = "Ingl{\'e}s",

volume = "631",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

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Ramón-Pérez, M, Bongiovanni, Á, García, AMP, Cepa, J, Lara-López, MA, De Diego, JA, Alfaro, E, Castañeda, HO, Cerviño, M, Fernández-Lorenzo, M, Gallego, J, Jesús González, J, Ignacio González-Serrano, J, Nadolny, J, Gómez, IO, Martínez, RP, Pintos-Castro, I, Pović, M & Sánchez-Portal, M 2019, 'The OTELO survey: II. The faint-end of the Hα luminosity function at z ∼ 0.40', Astronomy and Astrophysics, vol. 631, A10. https://doi.org/10.1051/0004-6361/201833295

TY - JOUR

T1 - The OTELO survey

T2 - II. The faint-end of the Hα luminosity function at z ∼ 0.40

AU - Ramón-Pérez, Marina

AU - Bongiovanni, Ángel

AU - García, Ana María Pérez

AU - Cepa, Jordi

AU - Lara-López, Maritza A.

AU - De Diego, José A.

AU - Alfaro, Emilio

AU - Castañeda, Héctor O.

AU - Cerviño, Miguel

AU - Fernández-Lorenzo, Mirian

AU - Gallego, Jesús

AU - Jesús González, J.

AU - Ignacio González-Serrano, J.

AU - Nadolny, Jakub

AU - Gómez, Iván Oteo

AU - Martínez, Ricardo Pérez

AU - Pintos-Castro, Irene

AU - Pović, Mirjana

AU - Sánchez-Portal, Miguel

PY - 2019/11/1

Y1 - 2019/11/1

N2 - Aims. We take advantage of the capability of the OTELO survey to obtain the Hα 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. Methods. 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. Results. The Hα luminosity function at z ∼ 0:40 is obtained, which extends the current faint end by almost 1 dex, reaching minimal luminosities of log10 Llim = 38:5 erg s-1 (or ∼0:002 M yr-1). The AGN contribution to the total Hα luminosity is estimated. We find that no AGN should be expected below a luminosity of log10 L = 38:6 erg s-1. From the sample of non-AGN (presumably, pure SFG) at z ∼ 0:40 we estimated a star formation rate density of πSFR = 0:012 ± 0:005 M yr-1 Mpc-3.c ESO 2019.

AB - Aims. We take advantage of the capability of the OTELO survey to obtain the Hα 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. Methods. 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. Results. The Hα luminosity function at z ∼ 0:40 is obtained, which extends the current faint end by almost 1 dex, reaching minimal luminosities of log10 Llim = 38:5 erg s-1 (or ∼0:002 M yr-1). The AGN contribution to the total Hα luminosity is estimated. We find that no AGN should be expected below a luminosity of log10 L = 38:6 erg s-1. From the sample of non-AGN (presumably, pure SFG) at z ∼ 0:40 we estimated a star formation rate density of πSFR = 0:012 ± 0:005 M yr-1 Mpc-3.c ESO 2019.

KW - Active - galaxies

KW - Luminosity function, mass function

KW - Star formation - galaxies

KW - Surveys - galaxies

UR - http://www.scopus.com/inward/record.url?scp=85082647245&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201833295

DO - 10.1051/0004-6361/201833295

M3 - Artículo

SN - 0004-6361

VL - 631

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A10

ER -

The OTELO survey: II. The faint-end of the Hα luminosity function at z ∼ 0.40

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Keywords

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