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November 24, 2024
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The PAU Survey: The quasar Lyα and UV luminosity functions at 2.7 < z < 5.3

Publicated to: ASTRONOMY & ASTROPHYSICS. 690 A388- - 2024-10-24 690(), DOI: 10.1051/0004-6361/202451675

Authors:

Torralba-Torregrosa, A; Renard, P; Spinoso, D; Arnalte-Mur, P; Gurung-López, S; Fernández-Soto, A; Gaztañaga, E; Navarro-Gironés, D; Cai, Z; Carretero, J; Castander, FJ; Eriksen, M; Garcia-Bellido, J; Hildebrandt, H; Hoekstra, H; Miquel, R; Sanchez, E; Tallada-Crespi, P; De Vicente, J; Fernandez, E
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Affiliations

Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, Bellaterra 08193, Barcelona, Spain - Author
CSIC UC, Inst Fis Cantabria, Avda Los Castros S N, Santander 39005, Spain - Author
CSIC, ICE, Inst Space Sci, E-08193 Barcelona, Spain - Author
Ctr Invest Energet Medioambientales & Tecnol CIEMA, Ave Complutense 40, E-28040 Madrid, Spain - Author
Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain - Author
Inst Estudis Espacials Catalunya IEEC, Edifici RDIT,Campus UPC, Castelldefels 08860, Barcelona, Spain - Author
Leiden Univ, Leiden Observ, Einsteinweg 55, NL-2333 CC Leiden, Netherlands - Author
Port Informacio Cient PIC, Campus UAB,C Albareda S N, Bellaterra 08193, Barcelona, Spain - Author
Ruhr Univ Bochum, Astron Inst AIRUB, Fac Phys & Astron, German Ctr Cosmol Lensing, D-44780 Bochum, Germany - Author
Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China - Author
UAM CSIC, Inst Fis Teor, Nicolas Cabrera 13, E-28049 Madrid, Spain - Author
Univ Politecn Valencia, CSIC, IFCA, Unidad Asociada Grp Astrofis Extragalact & Cosmol, Valencia, Spain - Author
Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth, England - Author
Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain - Author
Univ Valencia, Observ Astron, Ed Inst Invest,Parc Cient,C Catedrat Jose Beltran,, E-46980 Paterna, Valencia, Spain - Author
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Abstract

We present the Lyman-alpha (Ly alpha) and ultraviolet (UV) luminosity function (LF) in bins of redshift for quasars selected in the Physics of the Accelerating Universe Survey (PAUS). A sample of 915 objects was selected at 2.7 < z < 5.3 within an effective area of similar to 36 deg(2) observed in 40 narrow-band (NB) filters (FWHM similar to 120 & Aring;). We cover the intermediate-bright luminosity regime of the LF (; -29 < M-UV < -24). The continuous wavelength coverage of the PAUS NB set allows very efficient target identification and precise redshift measurements. We show that our method is able to retrieve a relatively complete (C similar to 85%) and pure (P similar to 90%) sample of Ly alpha-emitting quasars for L-Ly alpha > 10(44) erg s(-1). In order to obtain corrections for the LF estimation, and assess the accuracy of our selection method, we produced mock catalogs of 0 < z < 4.3 quasars and galaxies that mimic our target population and their main contaminants. Our results show a clear evolution of the Ly alpha and UV LFs, with a declining tendency in the number density of quasars toward increasing redshifts. In addition, the faint-end power-law slope of the Ly alpha LF becomes steeper with redshift, suggesting that the number density of Ly alpha-bright quasars declines faster than that of fainter emitters. By integrating the Ly alpha LF, we find that the total Ly alpha emitted by bright quasars per unit volume rapidly declines with increasing redshift, being subdominant to that of star-forming galaxies by several orders of magnitude by z similar to 4. Finally, we stack the NB pseudo-spectra of a visually selected "golden sample" of 591 quasars to obtain photometric composite SEDs in bins of redshift, enabling us to measure the mean intergalactic medium absorption using the Lyman-alpha forest as a function of redshift, yielding results consistent with previous spectroscopic determinations.
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Keywords

Active galactic nucleiData releaseFaint-endGalaxies: high-redshiftGalaxies: luminosity functionHubble deep fieldLess-than 5Line: identificationMass functionMean transmitted fluxMethods: observationalOscillation spectroscopic surveyPhotometric redshiftQuasars: emission lineSimilar-to 2Star-forming galaxies

Quality index

Bibliometric impact. Analysis of the contribution and dissemination channel

The work has been published in the journal ASTRONOMY & ASTROPHYSICS due to its progression and the good impact it has achieved in recent years, according to the agency WoS (JCR), it has become a reference in its field. In the year of publication of the work, 2024 there are still no calculated indicators, but in 2023, it was in position 15/84, thus managing to position itself as a Q1 (Primer Cuartil), in the category Astronomy & Astrophysics.

Independientemente del impacto esperado determinado por el canal de difusión, es importante destacar el impacto real observado de la propia aportación.

Según las diferentes agencias de indexación, el número de citas acumuladas por esta publicación hasta la fecha 2026-04-03:

  • WoS: 3
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Impact and social visibility

From the perspective of influence or social adoption, and based on metrics associated with mentions and interactions provided by agencies specializing in calculating the so-called "Alternative or Social Metrics," we can highlight as of 2026-04-03:

  • The use, from an academic perspective evidenced by the Altmetric agency indicator referring to aggregations made by the personal bibliographic manager Mendeley, gives us a total of: 10.
  • The use of this contribution in bookmarks, code forks, additions to favorite lists for recurrent reading, as well as general views, indicates that someone is using the publication as a basis for their current work. This may be a notable indicator of future more formal and academic citations. This claim is supported by the result of the "Capture" indicator, which yields a total of: 10 (PlumX).

With a more dissemination-oriented intent and targeting more general audiences, we can observe other more global scores such as:

  • The Total Score from Altmetric: 1.
  • The number of mentions on the social network X (formerly Twitter): 2 (Altmetric).

It is essential to present evidence supporting full alignment with institutional principles and guidelines on Open Science and the Conservation and Dissemination of Intellectual Heritage. A clear example of this is:

  • The work has been submitted to a journal whose editorial policy allows open Open Access publication.
  • Additionally, the work has been submitted to a journal classified as Diamond in relation to this type of editorial policy.
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Leadership analysis of institutional authors

This work has been carried out with international collaboration, specifically with researchers from: China; Germany; Netherlands; United Kingdom.

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Awards linked to the item

The authors acknowledge the insightful feedback from the scientific referee, which has significantly contributed to enhancing the quality of this paper. This work has been funded by project PID2019-109592GBI00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovacion (MCIN)-Agencia Estatal de Investigacion, by the Project of Excellence Prometeo/2020/085 from the Conselleria d'Innovacio Universitats, Ciencia i Societat Digital de la Generalitat Valenciana. The authors acknowledge the financial support from the MCIN with funding from the European Union NextGenerationEU and Generalitat Valenciana in the call Programa de Planes Complementarios de I+D+i (PRTR 2022). Project (VAL-JPAS), reference ASFAE/2022/025. PR and DS acknowledge the support by the Tsinghua Shui Mu Scholarship. PR, DS and ZC acknowledge the funding of the National Key R&D Program of China (grant no. 2023YFA1605600), the science research grants from the China Manned Space Project with No. CMS-CSST2021-A05, and the Tsinghua University Initiative Scientific Research Program (No. 20223080023). PR acknowledges additional funding from the National Science Foundation of China (grant no. 12350410365). EG acknowledges grants from Spain Plan Nacional (PGC2018-102021-B-100) and Maria de Maeztu (CEX2020-001058-M). 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 University (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'Informacio Cientifica (PIC), maintained through a collaboration of CIEMAT and IFAE, with additional support from Universitat Autonoma de Barcelona and ERDF. We acknowledge the PIC services department team for their support and fruitful discussions. EG acknowledges grants from Spain Plan Nacional (PGC2018-102021-B-100) and Maria de Maeztu (CEX2020-001058-M). JC acknowledges support from the grant PID2021-123012NA-C44 funded by MCIN/AEI/10.13039/501100011033 and by "ERDF A way of making Europe". FJC is supported by grants PID2022-141079NB and CEX2020-001058-M funded by MCIN/AEI/10.13039/501100011033. ME acknowledges funding by MCIN with funding from European Union NextGenerationEU (PRTR-C17.I1) and by Generalitat de Catalunya. IFT participation is supported by the grant PID2021-123012NB-C43P funded by MCIN/AEI/10.13039/501100011033. H. Hildebrandt is supported by a DFG Heisenberg grant (Hi 1495/5-1), the DFG Collaborative Research Center SFB1491, as well as an ERC Consolidator Grant (No. 770935). IFAE participation is supported by grant PID2021-123012NB funded by MCIN/AEI/10.13039/501100011033. CIEMAT participation is supported by the grant PID2021-123012NB-C42P funded by MCIN/AEI/10.13039/501100011033.
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