Euclid preparation
The statistical distribution and evolution of key properties of active galactic nuclei (AGN), such as their accretion rate, mass, and spin, remains a subject of open debate in astrophysics. The ESA Euclid space mission, launched on July 1 2023, promises a breakthrough in this field. We create detail...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2024-05, Vol.685 |
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| creator | Lusso, E Scodeggio, M Gabarra, L Palazzi, E Moresco, M Zamorani, G Cresci, G Landt, H Marconi, A Pozzetti, L Spinoglio, L Stern, D Aghanim, N Amara, A Auphan, T Bardelli, S Bonino, D Brescia, M Brinchmann, J Capobianco, V Carretero, J Cavuoti, S Conselice, C J Conversi, L Corcione, L Courtois, H M Duncan, C A J Ferriol, S Fourmanoit, N Frailis, M Franzetti, P Fumana, M Grazian, A Holmes, W Hook, I Hornstrup, A Kümmel, M Kunz, M Lilje, P B Lindholm, V Mansutti, O Marulli, F Medinaceli, E Merlin, E Meylan, G Moscardini, L Pasian, F Pettorino, V Poncet, M Raison, F Roncarelli, M Sapone, D Sartoris, B Schneider, P Serrano, S Surace, C Tallada-Crespí, P Taylor, A N Teplitz, H I Veropalumbo, A Vibert, D Wang, Y Weller, J Zoubian, J Bolzonella, M Scottez, V Viel, M Akrami, Y Anselmi, S Bruton, S Cabanac, R Cappi, A Castignani, G Castro, T Chambers, K C Cooray, A R Coupon, J Cucciati, O Ganga, K García-Bellido, J Giacomini, F Gozaliasl, G Hall, A Kansal, V Legrand, L Macias-Perez, J C. J. A. P. Martins Maturi, M Popa, V Porciani, C P.-F. Rocci Sánchez, A G Schneider, A Sereno, M Shulevski, A Stadel, J Stanford, S A Troja, A Tucci, M Valieri, C |
| description | The statistical distribution and evolution of key properties of active galactic nuclei (AGN), such as their accretion rate, mass, and spin, remains a subject of open debate in astrophysics. The ESA Euclid space mission, launched on July 1 2023, promises a breakthrough in this field. We create detailed mock catalogues of AGN spectra from the rest-frame near-infrared down to the ultraviolet – including emission lines – to simulate what Euclid will observe for both obscured (type 2) and unobscured (type 1) AGN. We concentrate on the red grisms of the NISP instrument, which will be used for the wide-field survey, opening a new window for spectroscopic AGN studies in the near-infrared. We quantify the efficiency in the redshift determination as well as in retrieving the emission line flux of the Hα+[N II] complex, as Euclid is mainly focused on this emission line, given that it is expected to be the brightest one in the probed redshift range. Spectroscopic redshifts are measured for 83% of the simulated AGN in the interval where the Hα is visible (i.e. 0.89 < z < 1.83 at a line flux of > 2 × 10−16 erg s−1 cm−2, encompassing the peak of AGN activity at z ≃ 1 − 1.5) within the spectral coverage of the red grism. Outside this redshift range, the measurement efficiency decreases significantly. Overall, a spectroscopic redshift iscorrectly determined for about 90% of type 2 AGN down to an emission line flux of roughly 3 × 10−16 erg s−1 cm−2, and for type 1 AGN down to 8.5 × 10−16 erg s−1 cm−2. Recovered values for black hole mass show a small offset with respect to the input values by about 10%, but the agreement is good overall. With such a high spectroscopic coverage at z < 2, we will be able to measure AGN demography, scaling relations, and clustering from the epoch of the peak of AGN activity down to the present-day Universe for hundreds of thousands of AGN with homogeneous spectroscopic information. |
| doi_str_mv | 10.1051/0004-6361/202348326 |
| format | Article |
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J. A. P. Martins ; Maturi, M ; Popa, V ; Porciani, C ; P.-F. Rocci ; Sánchez, A G ; Schneider, A ; Sereno, M ; Shulevski, A ; Stadel, J ; Stanford, S A ; Troja, A ; Tucci, M ; Valieri, C</creator><creatorcontrib>Lusso, E ; Scodeggio, M ; Gabarra, L ; Palazzi, E ; Moresco, M ; Zamorani, G ; Cresci, G ; Landt, H ; Marconi, A ; Pozzetti, L ; Spinoglio, L ; Stern, D ; Aghanim, N ; Amara, A ; Auphan, T ; Bardelli, S ; Bonino, D ; Brescia, M ; Brinchmann, J ; Capobianco, V ; Carretero, J ; Cavuoti, S ; Conselice, C J ; Conversi, L ; Corcione, L ; Courtois, H M ; Duncan, C A J ; Ferriol, S ; Fourmanoit, N ; Frailis, M ; Franzetti, P ; Fumana, M ; Grazian, A ; Holmes, W ; Hook, I ; Hornstrup, A ; Kümmel, M ; Kunz, M ; Lilje, P B ; Lindholm, V ; Mansutti, O ; Marulli, F ; Medinaceli, E ; Merlin, E ; Meylan, G ; Moscardini, L ; Pasian, F ; Pettorino, V ; Poncet, M ; Raison, F ; Roncarelli, M ; Sapone, D ; Sartoris, B ; Schneider, P ; Serrano, S ; Surace, C ; Tallada-Crespí, P ; Taylor, A N ; Teplitz, H I ; Veropalumbo, A ; Vibert, D ; Wang, Y ; Weller, J ; Zoubian, J ; Bolzonella, M ; Scottez, V ; Viel, M ; Akrami, Y ; Anselmi, S ; Bruton, S ; Cabanac, R ; Cappi, A ; Castignani, G ; Castro, T ; Chambers, K C ; Cooray, A R ; Coupon, J ; Cucciati, O ; Ganga, K ; García-Bellido, J ; Giacomini, F ; Gozaliasl, G ; Hall, A ; Kansal, V ; Legrand, L ; Macias-Perez, J ; C. J. A. P. Martins ; Maturi, M ; Popa, V ; Porciani, C ; P.-F. Rocci ; Sánchez, A G ; Schneider, A ; Sereno, M ; Shulevski, A ; Stadel, J ; Stanford, S A ; Troja, A ; Tucci, M ; Valieri, C</creatorcontrib><description>The statistical distribution and evolution of key properties of active galactic nuclei (AGN), such as their accretion rate, mass, and spin, remains a subject of open debate in astrophysics. The ESA Euclid space mission, launched on July 1 2023, promises a breakthrough in this field. We create detailed mock catalogues of AGN spectra from the rest-frame near-infrared down to the ultraviolet – including emission lines – to simulate what Euclid will observe for both obscured (type 2) and unobscured (type 1) AGN. We concentrate on the red grisms of the NISP instrument, which will be used for the wide-field survey, opening a new window for spectroscopic AGN studies in the near-infrared. We quantify the efficiency in the redshift determination as well as in retrieving the emission line flux of the Hα+[N II] complex, as Euclid is mainly focused on this emission line, given that it is expected to be the brightest one in the probed redshift range. Spectroscopic redshifts are measured for 83% of the simulated AGN in the interval where the Hα is visible (i.e. 0.89 < z < 1.83 at a line flux of > 2 × 10−16 erg s−1 cm−2, encompassing the peak of AGN activity at z ≃ 1 − 1.5) within the spectral coverage of the red grism. Outside this redshift range, the measurement efficiency decreases significantly. Overall, a spectroscopic redshift iscorrectly determined for about 90% of type 2 AGN down to an emission line flux of roughly 3 × 10−16 erg s−1 cm−2, and for type 1 AGN down to 8.5 × 10−16 erg s−1 cm−2. Recovered values for black hole mass show a small offset with respect to the input values by about 10%, but the agreement is good overall. With such a high spectroscopic coverage at z < 2, we will be able to measure AGN demography, scaling relations, and clustering from the epoch of the peak of AGN activity down to the present-day Universe for hundreds of thousands of AGN with homogeneous spectroscopic information.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/202348326</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Active galactic nuclei ; Black holes ; Clustering ; Demography ; Emission ; Red shift ; Space missions</subject><ispartof>Astronomy and astrophysics (Berlin), 2024-05, Vol.685</ispartof><rights>2024. This work is licensed under https://creativecommons.org/licenses/by/4.0 (the “License”). 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J. A. P. Martins</creatorcontrib><creatorcontrib>Maturi, M</creatorcontrib><creatorcontrib>Popa, V</creatorcontrib><creatorcontrib>Porciani, C</creatorcontrib><creatorcontrib>P.-F. Rocci</creatorcontrib><creatorcontrib>Sánchez, A G</creatorcontrib><creatorcontrib>Schneider, A</creatorcontrib><creatorcontrib>Sereno, M</creatorcontrib><creatorcontrib>Shulevski, A</creatorcontrib><creatorcontrib>Stadel, J</creatorcontrib><creatorcontrib>Stanford, S A</creatorcontrib><creatorcontrib>Troja, A</creatorcontrib><creatorcontrib>Tucci, M</creatorcontrib><creatorcontrib>Valieri, C</creatorcontrib><title>Euclid preparation</title><title>Astronomy and astrophysics (Berlin)</title><description>The statistical distribution and evolution of key properties of active galactic nuclei (AGN), such as their accretion rate, mass, and spin, remains a subject of open debate in astrophysics. The ESA Euclid space mission, launched on July 1 2023, promises a breakthrough in this field. We create detailed mock catalogues of AGN spectra from the rest-frame near-infrared down to the ultraviolet – including emission lines – to simulate what Euclid will observe for both obscured (type 2) and unobscured (type 1) AGN. We concentrate on the red grisms of the NISP instrument, which will be used for the wide-field survey, opening a new window for spectroscopic AGN studies in the near-infrared. We quantify the efficiency in the redshift determination as well as in retrieving the emission line flux of the Hα+[N II] complex, as Euclid is mainly focused on this emission line, given that it is expected to be the brightest one in the probed redshift range. Spectroscopic redshifts are measured for 83% of the simulated AGN in the interval where the Hα is visible (i.e. 0.89 < z < 1.83 at a line flux of > 2 × 10−16 erg s−1 cm−2, encompassing the peak of AGN activity at z ≃ 1 − 1.5) within the spectral coverage of the red grism. 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Rocci</creator><creator>Sánchez, A G</creator><creator>Schneider, A</creator><creator>Sereno, M</creator><creator>Shulevski, A</creator><creator>Stadel, J</creator><creator>Stanford, S A</creator><creator>Troja, A</creator><creator>Tucci, M</creator><creator>Valieri, C</creator><general>EDP Sciences</general><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20240501</creationdate><title>Euclid preparation</title><author>Lusso, E ; Scodeggio, M ; Gabarra, L ; Palazzi, E ; Moresco, M ; Zamorani, G ; Cresci, G ; Landt, H ; Marconi, A ; Pozzetti, L ; Spinoglio, L ; Stern, D ; Aghanim, N ; Amara, A ; Auphan, T ; Bardelli, S ; Bonino, D ; Brescia, M ; Brinchmann, J ; Capobianco, V ; Carretero, J ; Cavuoti, S ; Conselice, C J ; Conversi, L ; Corcione, L ; Courtois, H M ; Duncan, C A J ; Ferriol, S ; Fourmanoit, N ; Frailis, M ; Franzetti, P ; Fumana, M ; Grazian, A ; Holmes, W ; Hook, I ; Hornstrup, A ; Kümmel, M ; Kunz, M ; Lilje, P B ; Lindholm, V ; Mansutti, O ; Marulli, F ; Medinaceli, E ; Merlin, E ; Meylan, G ; Moscardini, L ; Pasian, F ; Pettorino, V ; Poncet, M ; Raison, F ; Roncarelli, M ; Sapone, D ; Sartoris, B ; Schneider, P ; Serrano, S ; Surace, C ; Tallada-Crespí, P ; Taylor, A N ; Teplitz, H I ; Veropalumbo, A ; Vibert, D ; Wang, Y ; Weller, J ; Zoubian, J ; Bolzonella, M ; Scottez, V ; Viel, M ; Akrami, Y ; Anselmi, S ; Bruton, S ; Cabanac, R ; Cappi, A ; Castignani, G ; Castro, T ; Chambers, K C ; Cooray, A R ; Coupon, J ; Cucciati, O ; Ganga, K ; García-Bellido, J ; Giacomini, F ; Gozaliasl, G ; Hall, A ; Kansal, V ; Legrand, L ; Macias-Perez, J ; C. J. A. P. Martins ; Maturi, M ; Popa, V ; Porciani, C ; P.-F. Rocci ; Sánchez, A G ; Schneider, A ; Sereno, M ; Shulevski, A ; Stadel, J ; Stanford, S A ; Troja, A ; Tucci, M ; Valieri, C</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-p736-c98848bc82bf8524d18bdced751f00b5773bc3afcd7646a96d761b5b27162e3f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Active galactic nuclei</topic><topic>Black holes</topic><topic>Clustering</topic><topic>Demography</topic><topic>Emission</topic><topic>Red shift</topic><topic>Space missions</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Lusso, E</creatorcontrib><creatorcontrib>Scodeggio, M</creatorcontrib><creatorcontrib>Gabarra, L</creatorcontrib><creatorcontrib>Palazzi, E</creatorcontrib><creatorcontrib>Moresco, M</creatorcontrib><creatorcontrib>Zamorani, G</creatorcontrib><creatorcontrib>Cresci, G</creatorcontrib><creatorcontrib>Landt, H</creatorcontrib><creatorcontrib>Marconi, A</creatorcontrib><creatorcontrib>Pozzetti, L</creatorcontrib><creatorcontrib>Spinoglio, L</creatorcontrib><creatorcontrib>Stern, D</creatorcontrib><creatorcontrib>Aghanim, N</creatorcontrib><creatorcontrib>Amara, A</creatorcontrib><creatorcontrib>Auphan, T</creatorcontrib><creatorcontrib>Bardelli, S</creatorcontrib><creatorcontrib>Bonino, D</creatorcontrib><creatorcontrib>Brescia, M</creatorcontrib><creatorcontrib>Brinchmann, J</creatorcontrib><creatorcontrib>Capobianco, V</creatorcontrib><creatorcontrib>Carretero, J</creatorcontrib><creatorcontrib>Cavuoti, S</creatorcontrib><creatorcontrib>Conselice, C J</creatorcontrib><creatorcontrib>Conversi, L</creatorcontrib><creatorcontrib>Corcione, L</creatorcontrib><creatorcontrib>Courtois, H M</creatorcontrib><creatorcontrib>Duncan, C A J</creatorcontrib><creatorcontrib>Ferriol, S</creatorcontrib><creatorcontrib>Fourmanoit, N</creatorcontrib><creatorcontrib>Frailis, M</creatorcontrib><creatorcontrib>Franzetti, P</creatorcontrib><creatorcontrib>Fumana, M</creatorcontrib><creatorcontrib>Grazian, A</creatorcontrib><creatorcontrib>Holmes, W</creatorcontrib><creatorcontrib>Hook, I</creatorcontrib><creatorcontrib>Hornstrup, A</creatorcontrib><creatorcontrib>Kümmel, M</creatorcontrib><creatorcontrib>Kunz, M</creatorcontrib><creatorcontrib>Lilje, P B</creatorcontrib><creatorcontrib>Lindholm, V</creatorcontrib><creatorcontrib>Mansutti, O</creatorcontrib><creatorcontrib>Marulli, F</creatorcontrib><creatorcontrib>Medinaceli, E</creatorcontrib><creatorcontrib>Merlin, E</creatorcontrib><creatorcontrib>Meylan, G</creatorcontrib><creatorcontrib>Moscardini, L</creatorcontrib><creatorcontrib>Pasian, F</creatorcontrib><creatorcontrib>Pettorino, V</creatorcontrib><creatorcontrib>Poncet, M</creatorcontrib><creatorcontrib>Raison, F</creatorcontrib><creatorcontrib>Roncarelli, M</creatorcontrib><creatorcontrib>Sapone, D</creatorcontrib><creatorcontrib>Sartoris, B</creatorcontrib><creatorcontrib>Schneider, P</creatorcontrib><creatorcontrib>Serrano, S</creatorcontrib><creatorcontrib>Surace, C</creatorcontrib><creatorcontrib>Tallada-Crespí, P</creatorcontrib><creatorcontrib>Taylor, A N</creatorcontrib><creatorcontrib>Teplitz, H I</creatorcontrib><creatorcontrib>Veropalumbo, A</creatorcontrib><creatorcontrib>Vibert, D</creatorcontrib><creatorcontrib>Wang, Y</creatorcontrib><creatorcontrib>Weller, J</creatorcontrib><creatorcontrib>Zoubian, J</creatorcontrib><creatorcontrib>Bolzonella, M</creatorcontrib><creatorcontrib>Scottez, V</creatorcontrib><creatorcontrib>Viel, M</creatorcontrib><creatorcontrib>Akrami, Y</creatorcontrib><creatorcontrib>Anselmi, S</creatorcontrib><creatorcontrib>Bruton, S</creatorcontrib><creatorcontrib>Cabanac, R</creatorcontrib><creatorcontrib>Cappi, A</creatorcontrib><creatorcontrib>Castignani, G</creatorcontrib><creatorcontrib>Castro, T</creatorcontrib><creatorcontrib>Chambers, K C</creatorcontrib><creatorcontrib>Cooray, A R</creatorcontrib><creatorcontrib>Coupon, J</creatorcontrib><creatorcontrib>Cucciati, O</creatorcontrib><creatorcontrib>Ganga, K</creatorcontrib><creatorcontrib>García-Bellido, J</creatorcontrib><creatorcontrib>Giacomini, F</creatorcontrib><creatorcontrib>Gozaliasl, G</creatorcontrib><creatorcontrib>Hall, A</creatorcontrib><creatorcontrib>Kansal, V</creatorcontrib><creatorcontrib>Legrand, L</creatorcontrib><creatorcontrib>Macias-Perez, J</creatorcontrib><creatorcontrib>C. J. A. P. Martins</creatorcontrib><creatorcontrib>Maturi, M</creatorcontrib><creatorcontrib>Popa, V</creatorcontrib><creatorcontrib>Porciani, C</creatorcontrib><creatorcontrib>P.-F. Rocci</creatorcontrib><creatorcontrib>Sánchez, A G</creatorcontrib><creatorcontrib>Schneider, A</creatorcontrib><creatorcontrib>Sereno, M</creatorcontrib><creatorcontrib>Shulevski, A</creatorcontrib><creatorcontrib>Stadel, J</creatorcontrib><creatorcontrib>Stanford, S A</creatorcontrib><creatorcontrib>Troja, A</creatorcontrib><creatorcontrib>Tucci, M</creatorcontrib><creatorcontrib>Valieri, C</creatorcontrib><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Lusso, E</au><au>Scodeggio, M</au><au>Gabarra, L</au><au>Palazzi, E</au><au>Moresco, M</au><au>Zamorani, G</au><au>Cresci, G</au><au>Landt, H</au><au>Marconi, A</au><au>Pozzetti, L</au><au>Spinoglio, L</au><au>Stern, D</au><au>Aghanim, N</au><au>Amara, A</au><au>Auphan, T</au><au>Bardelli, S</au><au>Bonino, D</au><au>Brescia, M</au><au>Brinchmann, J</au><au>Capobianco, V</au><au>Carretero, J</au><au>Cavuoti, S</au><au>Conselice, C J</au><au>Conversi, L</au><au>Corcione, L</au><au>Courtois, H M</au><au>Duncan, C A J</au><au>Ferriol, S</au><au>Fourmanoit, N</au><au>Frailis, M</au><au>Franzetti, P</au><au>Fumana, M</au><au>Grazian, A</au><au>Holmes, W</au><au>Hook, I</au><au>Hornstrup, A</au><au>Kümmel, M</au><au>Kunz, M</au><au>Lilje, P B</au><au>Lindholm, V</au><au>Mansutti, O</au><au>Marulli, F</au><au>Medinaceli, E</au><au>Merlin, E</au><au>Meylan, G</au><au>Moscardini, L</au><au>Pasian, F</au><au>Pettorino, V</au><au>Poncet, M</au><au>Raison, F</au><au>Roncarelli, M</au><au>Sapone, D</au><au>Sartoris, B</au><au>Schneider, P</au><au>Serrano, S</au><au>Surace, C</au><au>Tallada-Crespí, P</au><au>Taylor, A N</au><au>Teplitz, H I</au><au>Veropalumbo, A</au><au>Vibert, D</au><au>Wang, Y</au><au>Weller, J</au><au>Zoubian, J</au><au>Bolzonella, M</au><au>Scottez, V</au><au>Viel, M</au><au>Akrami, Y</au><au>Anselmi, S</au><au>Bruton, S</au><au>Cabanac, R</au><au>Cappi, A</au><au>Castignani, G</au><au>Castro, T</au><au>Chambers, K C</au><au>Cooray, A R</au><au>Coupon, J</au><au>Cucciati, O</au><au>Ganga, K</au><au>García-Bellido, J</au><au>Giacomini, F</au><au>Gozaliasl, G</au><au>Hall, A</au><au>Kansal, V</au><au>Legrand, L</au><au>Macias-Perez, J</au><au>C. J. A. P. Martins</au><au>Maturi, M</au><au>Popa, V</au><au>Porciani, C</au><au>P.-F. Rocci</au><au>Sánchez, A G</au><au>Schneider, A</au><au>Sereno, M</au><au>Shulevski, A</au><au>Stadel, J</au><au>Stanford, S A</au><au>Troja, A</au><au>Tucci, M</au><au>Valieri, C</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Euclid preparation</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2024-05-01</date><risdate>2024</risdate><volume>685</volume><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>The statistical distribution and evolution of key properties of active galactic nuclei (AGN), such as their accretion rate, mass, and spin, remains a subject of open debate in astrophysics. The ESA Euclid space mission, launched on July 1 2023, promises a breakthrough in this field. We create detailed mock catalogues of AGN spectra from the rest-frame near-infrared down to the ultraviolet – including emission lines – to simulate what Euclid will observe for both obscured (type 2) and unobscured (type 1) AGN. We concentrate on the red grisms of the NISP instrument, which will be used for the wide-field survey, opening a new window for spectroscopic AGN studies in the near-infrared. We quantify the efficiency in the redshift determination as well as in retrieving the emission line flux of the Hα+[N II] complex, as Euclid is mainly focused on this emission line, given that it is expected to be the brightest one in the probed redshift range. Spectroscopic redshifts are measured for 83% of the simulated AGN in the interval where the Hα is visible (i.e. 0.89 < z < 1.83 at a line flux of > 2 × 10−16 erg s−1 cm−2, encompassing the peak of AGN activity at z ≃ 1 − 1.5) within the spectral coverage of the red grism. Outside this redshift range, the measurement efficiency decreases significantly. Overall, a spectroscopic redshift iscorrectly determined for about 90% of type 2 AGN down to an emission line flux of roughly 3 × 10−16 erg s−1 cm−2, and for type 1 AGN down to 8.5 × 10−16 erg s−1 cm−2. Recovered values for black hole mass show a small offset with respect to the input values by about 10%, but the agreement is good overall. With such a high spectroscopic coverage at z < 2, we will be able to measure AGN demography, scaling relations, and clustering from the epoch of the peak of AGN activity down to the present-day Universe for hundreds of thousands of AGN with homogeneous spectroscopic information.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/202348326</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6361 |
| ispartof | Astronomy and astrophysics (Berlin), 2024-05, Vol.685 |
| issn | 0004-6361 1432-0746 |
| language | eng |
| recordid | cdi_proquest_journals_3057071204 |
| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; EZB-FREE-00999 freely available EZB journals |
| subjects | Active galactic nuclei Black holes Clustering Demography Emission Red shift Space missions |
| title | Euclid preparation |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-31T00%3A03%3A51IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Euclid%20preparation&rft.jtitle=Astronomy%20and%20astrophysics%20(Berlin)&rft.au=Lusso,%20E&rft.date=2024-05-01&rft.volume=685&rft.issn=0004-6361&rft.eissn=1432-0746&rft_id=info:doi/10.1051/0004-6361/202348326&rft_dat=%3Cproquest%3E3057071204%3C/proquest%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=3057071204&rft_id=info:pmid/&rfr_iscdi=true |