Muestra métricas de impacto externas asociadas a la publicación. Para mayor detalle:
Departamento Gestión de Conocimiento, Monitoreo y Prospección
Consultas o comentarios: productividad@anid.cl
Consultas o comentarios: productividad@anid.cl
Determining the fraction of reddened quasars in COSMOS with multiple selection techniques from X-ray to radio wavelengths
| Indexado |
|
||||
| DOI | 10.1051/0004-6361/201628836 | ||||
| Año | 2016 | ||||
| Tipo | artículo de investigación |
Citas Totales
Autores Afiliación Chile
Instituciones Chile
% Participación
Internacional
Autores
Afiliación Extranjera
Instituciones
Extranjeras
Abstract
The sub-population of quasars reddened by intrinsic or intervening clouds of dust are known to be underrepresented in optical quasar surveys. By defining a complete parent sample of the brightest and spatially unresolved quasars in the COSMOS field, we quantify to which extent this sub-population is fundamental to our understanding of the true population of quasars. By using the available multiwavelength data of various surveys in the COSMOS field, we built a parent sample of 33 quasars brighter than J = 20 mag, identified by reliable X-ray to radio wavelength selection techniques. Spectroscopic follow-up with the NOT/ALFOSC was carried out for four candidate quasars that had not been targeted previously to obtain a 100% redshift completeness of the sample. The population of high AV quasars (HAQs), a specific sub-population of quasars selected from optical/near-infrared photometry, some of which were shown to be missed in large optical surveys such as SDSS, is found to contribute 21%(+9)(-5) of the parent sample. The full population of bright spatially unresolved quasars represented by our parent sample consists of 39%(+9)(-8) reddened quasars defined by having A(V) > 0.1, and 21%(+9)(-5) of the sample having E(B-V) > 0.1 assuming the extinction curve of the Small Magellanic Cloud. We show that the HAQ selection works well for selecting reddened quasars, but some are missed because their optical spectra are too blue to pass the g - r color cut in the HAQ selection. This is either due to a low degree of dust reddening or anomalous spectra. We find that the fraction of quasars with contributing light from the host galaxy, causing observed extended spatial morphology, is most dominant at z less than or similar to 1. At higher redshifts the population of spatially unresolved quasars selected by our parent sample is found to be representative of the full population of bright active galactic nuclei at J < 20 mag. This work quantifies the bias against reddened quasars in studies that are based solely on optical surveys.
| Ord. | Autor | Género | Institución - País |
|---|---|---|---|
| 1 | Heintz, K. E. | Hombre |
Univ Copenhagen - Dinamarca
Niels Bohr Institute - Dinamarca Niels Bohr Institutet - Dinamarca |
| 2 | Fynbo, J. P. U. | Hombre |
Univ Copenhagen - Dinamarca
Niels Bohr Institute - Dinamarca Niels Bohr Institutet - Dinamarca |
| 3 | Moller, P. | Hombre |
ESO - Alemania
|
| 4 | Milvang-Jensen, B. | - |
Univ Copenhagen - Dinamarca
Niels Bohr Institute - Dinamarca Niels Bohr Institutet - Dinamarca |
| 5 | Zabl, J. | Hombre |
Niels Bohr Institute - Dinamarca
Niels Bohr Institutet - Dinamarca |
| 6 | Maddox, N. | Mujer |
Netherlands Inst Radio Astron - Países Bajos
Netherlands Foundation for Research in Astronomy - Países Bajos |
| 7 | Krogager, J. K. | Hombre |
Univ Copenhagen - Dinamarca
CNRS UPMC - Francia Niels Bohr Institute - Dinamarca Institut d 'Astrophysique de Paris - Francia Niels Bohr Institutet - Dinamarca Institut d’Astrophysique de Paris - Francia |
| 8 | Geier, S. | Hombre |
Gran Telescopio Canarias GRANTECAN - España
Inst Astrofis Canarias - España Gran Telescopio Canarias (GRANTECAN) - España Instituto Astrofisico de Canarias - España |
| 9 | Vestergaard, M. | Mujer |
Univ Copenhagen - Dinamarca
UNIV ARIZONA - Estados Unidos Niels Bohr Institute - Dinamarca The University of Arizona - Estados Unidos Niels Bohr Institutet - Dinamarca |
| 10 | Noterdaeme, Pasquier | - |
CNRS UPMC - Francia
Institut d 'Astrophysique de Paris - Francia Institut d’Astrophysique de Paris - Francia |
| 11 | Ledoux, Cedric | Hombre |
ESO - Chile
European Southern Observatory Santiago - Chile |
| Fuente |
|---|
| National Science Foundation |
| European Union |
| European Research Council |
| Ohio State University |
| Vanderbilt University |
| University of Tokyo |
| Yale University |
| FP7/2007 |
| Seventh Framework Programme |
| Alfred P. Sloan Foundation |
| University of Arizona |
| Brazilian Participation Group |
| Brookhaven National Laboratory |
| Carnegie Mellon University |
| University of Florida |
| French Participation Group |
| German Participation Group |
| Harvard University |
| Instituto de Astrofisica de Canarias |
| Michigan State/Notre Dame/JINA Participation Group |
| Johns Hopkins University |
| Lawrence Berkeley National Laboratory |
| Max Planck Institute for Astrophysics |
| Max Planck Institute for Extraterrestrial Physics |
| New Mexico State University |
| New York University |
| Pennsylvania State University |
| University of Portsmouth |
| Princeton University |
| Spanish Participation Group |
| University of Utah |
| University of Virginia |
| University of Washington |
| ESO programme |
| US Department of Energy Office of Science |
| Carnegie Mellon University, University of Florida |
| Danish Council for Independent Research |
| Københavns Universitet |
| Københavns Universitet |
| Natur og Univers, Det Frie Forskningsråd |
| Instituto de Astrofisica de Andalucia |
| Danmarks Frie Forskningsfond |
| European Union's Seventh Framework program |
| European Research Council under the European Union's Seventh Framework Program (FP7)/ERC Grant |
| US Department of Energy Oce of Science |
| NOTSA |
| State University, New York University |
| Max-Planck-Institut fur Astrophysik |
| Agradecimiento |
|---|
| We would like to thank the anonymous referee for a constructive and insightful report that gave valuable suggestions to present the results of this paper in the best possible way. Furthermore, we would like to thank D. Malesani and C. Grillo for carrying out the observations of the candidate quasars at the NOT. Otherwise we would not have succeeded in obtaining a 100% redshift completeness of our parent sample. We also wish to thank I. Paris for her help with the SDSS-III/BOSS DR12Q sample and the general SDSS/BOSS selection functions. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013)/ERC Grant agreement No. EGGS-278202. J.K.K. acknowledges support from the European Union's Seventh Framework Programme for research and innovation under the Marie-Curie grant agreement No. 600207 with reference DFF-MOBILEX-5051-00115. M.V. gratefully acknowledges support from the Danish Council for Independent Research via grant No. DFF 4002-00275. The data presented here were obtained with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. |
| We would like to thank the anonymous referee for a constructive and insightful report that gave valuable suggestions to present the results of this paper in the best possible way. Furthermore, we would like to thank D. Malesani and C. Grillo for carrying out the observations of the candidate quasars at the NOT. Otherwise we would not have succeeded in obtaining a 100% redshift completeness of our parent sample.We also wish to thank I. Pâris for her help with the SDSS-III/BOSS DR12Q sample and the general SDSS/BOSS selection functions. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013)/ERC Grant agreement No. EGGS-278202. J.K.K. acknowledges support from the European Union's Seventh Framework Programme for research and innovation under the Marie-Curie grant agreement No. 600207 with reference DFF-MOBILEX-5051-00115. M.V. gratefully acknowledges support from the Danish Council for Independent Research via grant No. DFF 4002-00275. The data presented here were obtained with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Oce of Science. The SDSS-III web site is http: //www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. |
