Euclid preparation
We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, updating the calculation presented in the Euclid Red Book in several ways. We account for revisions to the Euclid near-infrared filter wavelengths; we adopt steeper rates of decline of the quasar luminosity...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2019-11, Vol.631 |
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| creator | Barnett, R. Warren, S. J. Mortlock, D. J. Conselice, C. Hewett, P. C. Willott, C. J. Auricchio, N. Baldi, M. Bender, R. Bonino, D. Branchini, E. Brinchmann, J. Burigana, C. Camera, S. Capobianco, V. Carbone, C. Carvalho, C. S. Castander, F. J. Cimatti, A. Clédassou, R. Congedo, G. Conversi, L. Copin, Y. Corcione, L. Coupon, J. Cropper, M. Da Silva, A. Duncan, C. A. J. Dusini, S. Ealet, A. Farrens, S. Fosalba, P. Fotopoulou, S. Frailis, M. Galeotta, S. Garilli, B. Gillard, W. Gillis, B. R. Grupp, F. Israel, H. Jahnke, K. Kermiche, S. Kilbinger, M. Kirkpatrick, C. C. Kitching, T. Kohley, R. Kubik, B. Kunz, M. Kurki-Suonio, H. Laureijs, R. Ligori, S. Lilje, P. B. Lloro, I. Maiorano, E. Mansutti, O. Marggraf, O. Martinet, N. Marulli, F. Massey, R. Mauri, N. Medinaceli, E. Mei, S. Mellier, Y. Metge, J. J. Meylan, G. Moscardini, L. Munari, E. Niemi, S. M. Nutma, T. Padilla, C. Paltani, S. Pasian, F. Percival, W. J. Pettorino, V. Poncet, M. Pozzetti, L. Raison, F. Renzi, A. Rhodes, J. Rix, H.-W. Roncarelli, M. Rossetti, E. Saglia, R. Sapone, D. Scaramella, R. Schneider, P. Scottez, V. Secroun, A. Sirri, G. Stanco, L. Sureau, F. Tavagnacco, D. Tenti, M. Tereno, I. Toledo-Moreo, R. Valenziano, L. Vassallo, T. Zacchei, A. Zoubian, J. Zucca, E. |
| description | We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, updating the calculation presented in the Euclid Red Book in several ways. We account for revisions to the Euclid near-infrared filter wavelengths; we adopt steeper rates of decline of the quasar luminosity function (QLF; Φ) with redshift, Φ ∝ 10k(z − 6), k = −0.72, and a further steeper rate of decline, k = −0.92; we use better models of the contaminating populations (MLT dwarfs and compact early-type galaxies); and we make use of an improved Bayesian selection method, compared to the colour cuts used for the Red Book calculation, allowing the identification of fainter quasars, down to JAB ∼ 23. Quasars at z > 8 may be selected from Euclid OYJH photometry alone, but selection over the redshift interval 7 < z < 8 is greatly improved by the addition of z-band data from, e.g., Pan-STARRS and LSST. We calculate predicted quasar yields for the assumed values of the rate of decline of the QLF beyond z = 6. If the decline of the QLF accelerates beyond z = 6, with k = −0.92, Euclid should nevertheless find over 100 quasars with 7.0 < z < 7.5, and ∼25 quasars beyond the current record of z = 7.5, including ∼8 beyond z = 8.0. The first Euclid quasars at z > 7.5 should be found in the DR1 data release, expected in 2024. It will be possible to determine the bright-end slope of the QLF, 7 < z < 8, M1450 < −25, using 8 m class telescopes to confirm candidates, but follow-up with JWST or E-ELT will be required to measure the faint-end slope. Contamination of the candidate lists is predicted to be modest even at JAB ∼ 23. The precision with which k can be determined over 7 < z < 8 depends on the value of k, but assuming k = −0.72 it can be measured to a 1σ uncertainty of 0.07. |
| doi_str_mv | 10.1051/0004-6361/201936427 |
| format | Article |
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J. ; Mortlock, D. J. ; Conselice, C. ; Hewett, P. C. ; Willott, C. J. ; Auricchio, N. ; Baldi, M. ; Bender, R. ; Bonino, D. ; Branchini, E. ; Brinchmann, J. ; Burigana, C. ; Camera, S. ; Capobianco, V. ; Carbone, C. ; Carvalho, C. S. ; Castander, F. J. ; Cimatti, A. ; Clédassou, R. ; Congedo, G. ; Conversi, L. ; Copin, Y. ; Corcione, L. ; Coupon, J. ; Cropper, M. ; Da Silva, A. ; Duncan, C. A. J. ; Dusini, S. ; Ealet, A. ; Farrens, S. ; Fosalba, P. ; Fotopoulou, S. ; Frailis, M. ; Galeotta, S. ; Garilli, B. ; Gillard, W. ; Gillis, B. R. ; Grupp, F. ; Israel, H. ; Jahnke, K. ; Kermiche, S. ; Kilbinger, M. ; Kirkpatrick, C. C. ; Kitching, T. ; Kohley, R. ; Kubik, B. ; Kunz, M. ; Kurki-Suonio, H. ; Laureijs, R. ; Ligori, S. ; Lilje, P. B. ; Lloro, I. ; Maiorano, E. ; Mansutti, O. ; Marggraf, O. ; Martinet, N. ; Marulli, F. ; Massey, R. ; Mauri, N. ; Medinaceli, E. ; Mei, S. ; Mellier, Y. ; Metge, J. J. ; Meylan, G. ; Moscardini, L. ; Munari, E. ; Niemi, S. M. ; Nutma, T. ; Padilla, C. ; Paltani, S. ; Pasian, F. ; Percival, W. J. ; Pettorino, V. ; Poncet, M. ; Pozzetti, L. ; Raison, F. ; Renzi, A. ; Rhodes, J. ; Rix, H.-W. ; Roncarelli, M. ; Rossetti, E. ; Saglia, R. ; Sapone, D. ; Scaramella, R. ; Schneider, P. ; Scottez, V. ; Secroun, A. ; Sirri, G. ; Stanco, L. ; Sureau, F. ; Tavagnacco, D. ; Tenti, M. ; Tereno, I. ; Toledo-Moreo, R. ; Valenziano, L. ; Vassallo, T. ; Zacchei, A. ; Zoubian, J. ; Zucca, E.</creator><creatorcontrib>Barnett, R. ; Warren, S. J. ; Mortlock, D. J. ; Conselice, C. ; Hewett, P. C. ; Willott, C. J. ; Auricchio, N. ; Baldi, M. ; Bender, R. ; Bonino, D. ; Branchini, E. ; Brinchmann, J. ; Burigana, C. ; Camera, S. ; Capobianco, V. ; Carbone, C. ; Carvalho, C. S. ; Castander, F. J. ; Cimatti, A. ; Clédassou, R. ; Congedo, G. ; Conversi, L. ; Copin, Y. ; Corcione, L. ; Coupon, J. ; Cropper, M. ; Da Silva, A. ; Duncan, C. A. J. ; Dusini, S. ; Ealet, A. ; Farrens, S. ; Fosalba, P. ; Fotopoulou, S. ; Frailis, M. ; Galeotta, S. ; Garilli, B. ; Gillard, W. ; Gillis, B. R. ; Grupp, F. ; Israel, H. ; Jahnke, K. ; Kermiche, S. ; Kilbinger, M. ; Kirkpatrick, C. C. ; Kitching, T. ; Kohley, R. ; Kubik, B. ; Kunz, M. ; Kurki-Suonio, H. ; Laureijs, R. ; Ligori, S. ; Lilje, P. B. ; Lloro, I. ; Maiorano, E. ; Mansutti, O. ; Marggraf, O. ; Martinet, N. ; Marulli, F. ; Massey, R. ; Mauri, N. ; Medinaceli, E. ; Mei, S. ; Mellier, Y. ; Metge, J. J. ; Meylan, G. ; Moscardini, L. ; Munari, E. ; Niemi, S. M. ; Nutma, T. ; Padilla, C. ; Paltani, S. ; Pasian, F. ; Percival, W. J. ; Pettorino, V. ; Poncet, M. ; Pozzetti, L. ; Raison, F. ; Renzi, A. ; Rhodes, J. ; Rix, H.-W. ; Roncarelli, M. ; Rossetti, E. ; Saglia, R. ; Sapone, D. ; Scaramella, R. ; Schneider, P. ; Scottez, V. ; Secroun, A. ; Sirri, G. ; Stanco, L. ; Sureau, F. ; Tavagnacco, D. ; Tenti, M. ; Tereno, I. ; Toledo-Moreo, R. ; Valenziano, L. ; Vassallo, T. ; Zacchei, A. ; Zoubian, J. ; Zucca, E.</creatorcontrib><description><![CDATA[We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, updating the calculation presented in the Euclid Red Book in several ways. We account for revisions to the Euclid near-infrared filter wavelengths; we adopt steeper rates of decline of the quasar luminosity function (QLF; Φ) with redshift, Φ ∝ 10k(z − 6), k = −0.72, and a further steeper rate of decline, k = −0.92; we use better models of the contaminating populations (MLT dwarfs and compact early-type galaxies); and we make use of an improved Bayesian selection method, compared to the colour cuts used for the Red Book calculation, allowing the identification of fainter quasars, down to JAB ∼ 23. Quasars at z > 8 may be selected from Euclid OYJH photometry alone, but selection over the redshift interval 7 < z < 8 is greatly improved by the addition of z-band data from, e.g., Pan-STARRS and LSST. We calculate predicted quasar yields for the assumed values of the rate of decline of the QLF beyond z = 6. If the decline of the QLF accelerates beyond z = 6, with k = −0.92, Euclid should nevertheless find over 100 quasars with 7.0 < z < 7.5, and ∼25 quasars beyond the current record of z = 7.5, including ∼8 beyond z = 8.0. The first Euclid quasars at z > 7.5 should be found in the DR1 data release, expected in 2024. It will be possible to determine the bright-end slope of the QLF, 7 < z < 8, M1450 < −25, using 8 m class telescopes to confirm candidates, but follow-up with JWST or E-ELT will be required to measure the faint-end slope. Contamination of the candidate lists is predicted to be modest even at JAB ∼ 23. The precision with which k can be determined over 7 < z < 8 depends on the value of k, but assuming k = −0.72 it can be measured to a 1σ uncertainty of 0.07.]]></description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201936427</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Astronomical models ; Compact galaxies ; Contamination ; Infrared filters ; Luminosity ; methods: statistical ; Quasars ; quasars: general ; Red shift ; surveys ; Telescopes</subject><ispartof>Astronomy and astrophysics (Berlin), 2019-11, Vol.631</ispartof><rights>Copyright EDP Sciences Nov 2019</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c1167-2a29d37094fa8b560e32fce12717bb72da857550d6fbd6a4cad8a4392441b3b83</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,27901,27902</link.rule.ids></links><search><creatorcontrib>Barnett, R.</creatorcontrib><creatorcontrib>Warren, S. 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J.</creatorcontrib><creatorcontrib>Pettorino, V.</creatorcontrib><creatorcontrib>Poncet, M.</creatorcontrib><creatorcontrib>Pozzetti, L.</creatorcontrib><creatorcontrib>Raison, F.</creatorcontrib><creatorcontrib>Renzi, A.</creatorcontrib><creatorcontrib>Rhodes, J.</creatorcontrib><creatorcontrib>Rix, H.-W.</creatorcontrib><creatorcontrib>Roncarelli, M.</creatorcontrib><creatorcontrib>Rossetti, E.</creatorcontrib><creatorcontrib>Saglia, R.</creatorcontrib><creatorcontrib>Sapone, D.</creatorcontrib><creatorcontrib>Scaramella, R.</creatorcontrib><creatorcontrib>Schneider, P.</creatorcontrib><creatorcontrib>Scottez, V.</creatorcontrib><creatorcontrib>Secroun, A.</creatorcontrib><creatorcontrib>Sirri, G.</creatorcontrib><creatorcontrib>Stanco, L.</creatorcontrib><creatorcontrib>Sureau, F.</creatorcontrib><creatorcontrib>Tavagnacco, D.</creatorcontrib><creatorcontrib>Tenti, M.</creatorcontrib><creatorcontrib>Tereno, I.</creatorcontrib><creatorcontrib>Toledo-Moreo, R.</creatorcontrib><creatorcontrib>Valenziano, L.</creatorcontrib><creatorcontrib>Vassallo, T.</creatorcontrib><creatorcontrib>Zacchei, A.</creatorcontrib><creatorcontrib>Zoubian, J.</creatorcontrib><creatorcontrib>Zucca, E.</creatorcontrib><title>Euclid preparation</title><title>Astronomy and astrophysics (Berlin)</title><description><![CDATA[We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, updating the calculation presented in the Euclid Red Book in several ways. We account for revisions to the Euclid near-infrared filter wavelengths; we adopt steeper rates of decline of the quasar luminosity function (QLF; Φ) with redshift, Φ ∝ 10k(z − 6), k = −0.72, and a further steeper rate of decline, k = −0.92; we use better models of the contaminating populations (MLT dwarfs and compact early-type galaxies); and we make use of an improved Bayesian selection method, compared to the colour cuts used for the Red Book calculation, allowing the identification of fainter quasars, down to JAB ∼ 23. Quasars at z > 8 may be selected from Euclid OYJH photometry alone, but selection over the redshift interval 7 < z < 8 is greatly improved by the addition of z-band data from, e.g., Pan-STARRS and LSST. We calculate predicted quasar yields for the assumed values of the rate of decline of the QLF beyond z = 6. If the decline of the QLF accelerates beyond z = 6, with k = −0.92, Euclid should nevertheless find over 100 quasars with 7.0 < z < 7.5, and ∼25 quasars beyond the current record of z = 7.5, including ∼8 beyond z = 8.0. The first Euclid quasars at z > 7.5 should be found in the DR1 data release, expected in 2024. It will be possible to determine the bright-end slope of the QLF, 7 < z < 8, M1450 < −25, using 8 m class telescopes to confirm candidates, but follow-up with JWST or E-ELT will be required to measure the faint-end slope. Contamination of the candidate lists is predicted to be modest even at JAB ∼ 23. The precision with which k can be determined over 7 < z < 8 depends on the value of k, but assuming k = −0.72 it can be measured to a 1σ uncertainty of 0.07.]]></description><subject>Astronomical models</subject><subject>Compact galaxies</subject><subject>Contamination</subject><subject>Infrared filters</subject><subject>Luminosity</subject><subject>methods: statistical</subject><subject>Quasars</subject><subject>quasars: general</subject><subject>Red shift</subject><subject>surveys</subject><subject>Telescopes</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNo9zUtLw0AUBeBBFIzVjVs3guvYe-d1J0upbRQKIvjCzTCTmUBqbeIkAf33BiquDgc-zmHsAuEaQeEcAGSuhcY5ByyElpwOWIZS8BxI6kOW_YtjdtL3m6lyNCJj58ux2jbhskuxc8kNTbs7ZUe12_bx7C9n7Hm1fFrc5euH8n5xs84rRE05d7wIgqCQtTNeaYiC11VETkjeEw_OKFIKgq590E5WLhgnRcGlRC-8ETN2td_tUvs1xn6wm3ZMu-nScmm00hIMTSrfq6Yf4rftUvPp0o916cNqEqSsgVf7SOXbbfnybkH8AgnvSSA</recordid><startdate>20191101</startdate><enddate>20191101</enddate><creator>Barnett, R.</creator><creator>Warren, S. 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B.</creator><creator>Lloro, I.</creator><creator>Maiorano, E.</creator><creator>Mansutti, O.</creator><creator>Marggraf, O.</creator><creator>Martinet, N.</creator><creator>Marulli, F.</creator><creator>Massey, R.</creator><creator>Mauri, N.</creator><creator>Medinaceli, E.</creator><creator>Mei, S.</creator><creator>Mellier, Y.</creator><creator>Metge, J. J.</creator><creator>Meylan, G.</creator><creator>Moscardini, L.</creator><creator>Munari, E.</creator><creator>Niemi, S. M.</creator><creator>Nutma, T.</creator><creator>Padilla, C.</creator><creator>Paltani, S.</creator><creator>Pasian, F.</creator><creator>Percival, W. J.</creator><creator>Pettorino, V.</creator><creator>Poncet, M.</creator><creator>Pozzetti, L.</creator><creator>Raison, F.</creator><creator>Renzi, A.</creator><creator>Rhodes, J.</creator><creator>Rix, H.-W.</creator><creator>Roncarelli, M.</creator><creator>Rossetti, E.</creator><creator>Saglia, R.</creator><creator>Sapone, D.</creator><creator>Scaramella, R.</creator><creator>Schneider, P.</creator><creator>Scottez, V.</creator><creator>Secroun, A.</creator><creator>Sirri, G.</creator><creator>Stanco, L.</creator><creator>Sureau, F.</creator><creator>Tavagnacco, D.</creator><creator>Tenti, M.</creator><creator>Tereno, I.</creator><creator>Toledo-Moreo, R.</creator><creator>Valenziano, L.</creator><creator>Vassallo, T.</creator><creator>Zacchei, A.</creator><creator>Zoubian, J.</creator><creator>Zucca, E.</creator><general>EDP Sciences</general><scope>BSCLL</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20191101</creationdate><title>Euclid preparation</title><author>Barnett, R. ; Warren, S. J. ; Mortlock, D. J. ; Conselice, C. ; Hewett, P. C. ; Willott, C. J. ; Auricchio, N. ; Baldi, M. ; Bender, R. ; Bonino, D. ; Branchini, E. ; Brinchmann, J. ; Burigana, C. ; Camera, S. ; Capobianco, V. ; Carbone, C. ; Carvalho, C. S. ; Castander, F. J. ; Cimatti, A. ; Clédassou, R. ; Congedo, G. ; Conversi, L. ; Copin, Y. ; Corcione, L. ; Coupon, J. ; Cropper, M. ; Da Silva, A. ; Duncan, C. A. J. ; Dusini, S. ; Ealet, A. ; Farrens, S. ; Fosalba, P. ; Fotopoulou, S. ; Frailis, M. ; Galeotta, S. ; Garilli, B. ; Gillard, W. ; Gillis, B. R. ; Grupp, F. ; Israel, H. ; Jahnke, K. ; Kermiche, S. ; Kilbinger, M. ; Kirkpatrick, C. C. ; Kitching, T. ; Kohley, R. ; Kubik, B. ; Kunz, M. ; Kurki-Suonio, H. ; Laureijs, R. ; Ligori, S. ; Lilje, P. B. ; Lloro, I. ; Maiorano, E. ; Mansutti, O. ; Marggraf, O. ; Martinet, N. ; Marulli, F. ; Massey, R. ; Mauri, N. ; Medinaceli, E. ; Mei, S. ; Mellier, Y. ; Metge, J. J. ; Meylan, G. ; Moscardini, L. ; Munari, E. ; Niemi, S. M. ; Nutma, T. ; Padilla, C. ; Paltani, S. ; Pasian, F. ; Percival, W. J. ; Pettorino, V. ; Poncet, M. ; Pozzetti, L. ; Raison, F. ; Renzi, A. ; Rhodes, J. ; Rix, H.-W. ; Roncarelli, M. ; Rossetti, E. ; Saglia, R. ; Sapone, D. ; Scaramella, R. ; Schneider, P. ; Scottez, V. ; Secroun, A. ; Sirri, G. ; Stanco, L. ; Sureau, F. ; Tavagnacco, D. ; Tenti, M. ; Tereno, I. ; Toledo-Moreo, R. ; Valenziano, L. ; Vassallo, T. ; Zacchei, A. ; Zoubian, J. ; Zucca, E.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c1167-2a29d37094fa8b560e32fce12717bb72da857550d6fbd6a4cad8a4392441b3b83</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Astronomical models</topic><topic>Compact galaxies</topic><topic>Contamination</topic><topic>Infrared filters</topic><topic>Luminosity</topic><topic>methods: statistical</topic><topic>Quasars</topic><topic>quasars: general</topic><topic>Red shift</topic><topic>surveys</topic><topic>Telescopes</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Barnett, R.</creatorcontrib><creatorcontrib>Warren, S. J.</creatorcontrib><creatorcontrib>Mortlock, D. J.</creatorcontrib><creatorcontrib>Conselice, C.</creatorcontrib><creatorcontrib>Hewett, P. C.</creatorcontrib><creatorcontrib>Willott, C. J.</creatorcontrib><creatorcontrib>Auricchio, N.</creatorcontrib><creatorcontrib>Baldi, M.</creatorcontrib><creatorcontrib>Bender, R.</creatorcontrib><creatorcontrib>Bonino, D.</creatorcontrib><creatorcontrib>Branchini, E.</creatorcontrib><creatorcontrib>Brinchmann, J.</creatorcontrib><creatorcontrib>Burigana, C.</creatorcontrib><creatorcontrib>Camera, S.</creatorcontrib><creatorcontrib>Capobianco, V.</creatorcontrib><creatorcontrib>Carbone, C.</creatorcontrib><creatorcontrib>Carvalho, C. S.</creatorcontrib><creatorcontrib>Castander, F. J.</creatorcontrib><creatorcontrib>Cimatti, A.</creatorcontrib><creatorcontrib>Clédassou, R.</creatorcontrib><creatorcontrib>Congedo, G.</creatorcontrib><creatorcontrib>Conversi, L.</creatorcontrib><creatorcontrib>Copin, Y.</creatorcontrib><creatorcontrib>Corcione, L.</creatorcontrib><creatorcontrib>Coupon, J.</creatorcontrib><creatorcontrib>Cropper, M.</creatorcontrib><creatorcontrib>Da Silva, A.</creatorcontrib><creatorcontrib>Duncan, C. A. J.</creatorcontrib><creatorcontrib>Dusini, S.</creatorcontrib><creatorcontrib>Ealet, A.</creatorcontrib><creatorcontrib>Farrens, S.</creatorcontrib><creatorcontrib>Fosalba, P.</creatorcontrib><creatorcontrib>Fotopoulou, S.</creatorcontrib><creatorcontrib>Frailis, M.</creatorcontrib><creatorcontrib>Galeotta, S.</creatorcontrib><creatorcontrib>Garilli, B.</creatorcontrib><creatorcontrib>Gillard, W.</creatorcontrib><creatorcontrib>Gillis, B. R.</creatorcontrib><creatorcontrib>Grupp, F.</creatorcontrib><creatorcontrib>Israel, H.</creatorcontrib><creatorcontrib>Jahnke, K.</creatorcontrib><creatorcontrib>Kermiche, S.</creatorcontrib><creatorcontrib>Kilbinger, M.</creatorcontrib><creatorcontrib>Kirkpatrick, C. C.</creatorcontrib><creatorcontrib>Kitching, T.</creatorcontrib><creatorcontrib>Kohley, R.</creatorcontrib><creatorcontrib>Kubik, B.</creatorcontrib><creatorcontrib>Kunz, M.</creatorcontrib><creatorcontrib>Kurki-Suonio, H.</creatorcontrib><creatorcontrib>Laureijs, R.</creatorcontrib><creatorcontrib>Ligori, S.</creatorcontrib><creatorcontrib>Lilje, P. B.</creatorcontrib><creatorcontrib>Lloro, I.</creatorcontrib><creatorcontrib>Maiorano, E.</creatorcontrib><creatorcontrib>Mansutti, O.</creatorcontrib><creatorcontrib>Marggraf, O.</creatorcontrib><creatorcontrib>Martinet, N.</creatorcontrib><creatorcontrib>Marulli, F.</creatorcontrib><creatorcontrib>Massey, R.</creatorcontrib><creatorcontrib>Mauri, N.</creatorcontrib><creatorcontrib>Medinaceli, E.</creatorcontrib><creatorcontrib>Mei, S.</creatorcontrib><creatorcontrib>Mellier, Y.</creatorcontrib><creatorcontrib>Metge, J. J.</creatorcontrib><creatorcontrib>Meylan, G.</creatorcontrib><creatorcontrib>Moscardini, L.</creatorcontrib><creatorcontrib>Munari, E.</creatorcontrib><creatorcontrib>Niemi, S. M.</creatorcontrib><creatorcontrib>Nutma, T.</creatorcontrib><creatorcontrib>Padilla, C.</creatorcontrib><creatorcontrib>Paltani, S.</creatorcontrib><creatorcontrib>Pasian, F.</creatorcontrib><creatorcontrib>Percival, W. J.</creatorcontrib><creatorcontrib>Pettorino, V.</creatorcontrib><creatorcontrib>Poncet, M.</creatorcontrib><creatorcontrib>Pozzetti, L.</creatorcontrib><creatorcontrib>Raison, F.</creatorcontrib><creatorcontrib>Renzi, A.</creatorcontrib><creatorcontrib>Rhodes, J.</creatorcontrib><creatorcontrib>Rix, H.-W.</creatorcontrib><creatorcontrib>Roncarelli, M.</creatorcontrib><creatorcontrib>Rossetti, E.</creatorcontrib><creatorcontrib>Saglia, R.</creatorcontrib><creatorcontrib>Sapone, D.</creatorcontrib><creatorcontrib>Scaramella, R.</creatorcontrib><creatorcontrib>Schneider, P.</creatorcontrib><creatorcontrib>Scottez, V.</creatorcontrib><creatorcontrib>Secroun, A.</creatorcontrib><creatorcontrib>Sirri, G.</creatorcontrib><creatorcontrib>Stanco, L.</creatorcontrib><creatorcontrib>Sureau, F.</creatorcontrib><creatorcontrib>Tavagnacco, D.</creatorcontrib><creatorcontrib>Tenti, M.</creatorcontrib><creatorcontrib>Tereno, I.</creatorcontrib><creatorcontrib>Toledo-Moreo, R.</creatorcontrib><creatorcontrib>Valenziano, L.</creatorcontrib><creatorcontrib>Vassallo, T.</creatorcontrib><creatorcontrib>Zacchei, A.</creatorcontrib><creatorcontrib>Zoubian, J.</creatorcontrib><creatorcontrib>Zucca, E.</creatorcontrib><collection>Istex</collection><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>Barnett, R.</au><au>Warren, S. J.</au><au>Mortlock, D. J.</au><au>Conselice, C.</au><au>Hewett, P. C.</au><au>Willott, C. J.</au><au>Auricchio, N.</au><au>Baldi, M.</au><au>Bender, R.</au><au>Bonino, D.</au><au>Branchini, E.</au><au>Brinchmann, J.</au><au>Burigana, C.</au><au>Camera, S.</au><au>Capobianco, V.</au><au>Carbone, C.</au><au>Carvalho, C. S.</au><au>Castander, F. J.</au><au>Cimatti, A.</au><au>Clédassou, R.</au><au>Congedo, G.</au><au>Conversi, L.</au><au>Copin, Y.</au><au>Corcione, L.</au><au>Coupon, J.</au><au>Cropper, M.</au><au>Da Silva, A.</au><au>Duncan, C. A. J.</au><au>Dusini, S.</au><au>Ealet, A.</au><au>Farrens, S.</au><au>Fosalba, P.</au><au>Fotopoulou, S.</au><au>Frailis, M.</au><au>Galeotta, S.</au><au>Garilli, B.</au><au>Gillard, W.</au><au>Gillis, B. R.</au><au>Grupp, F.</au><au>Israel, H.</au><au>Jahnke, K.</au><au>Kermiche, S.</au><au>Kilbinger, M.</au><au>Kirkpatrick, C. C.</au><au>Kitching, T.</au><au>Kohley, R.</au><au>Kubik, B.</au><au>Kunz, M.</au><au>Kurki-Suonio, H.</au><au>Laureijs, R.</au><au>Ligori, S.</au><au>Lilje, P. B.</au><au>Lloro, I.</au><au>Maiorano, E.</au><au>Mansutti, O.</au><au>Marggraf, O.</au><au>Martinet, N.</au><au>Marulli, F.</au><au>Massey, R.</au><au>Mauri, N.</au><au>Medinaceli, E.</au><au>Mei, S.</au><au>Mellier, Y.</au><au>Metge, J. J.</au><au>Meylan, G.</au><au>Moscardini, L.</au><au>Munari, E.</au><au>Niemi, S. M.</au><au>Nutma, T.</au><au>Padilla, C.</au><au>Paltani, S.</au><au>Pasian, F.</au><au>Percival, W. J.</au><au>Pettorino, V.</au><au>Poncet, M.</au><au>Pozzetti, L.</au><au>Raison, F.</au><au>Renzi, A.</au><au>Rhodes, J.</au><au>Rix, H.-W.</au><au>Roncarelli, M.</au><au>Rossetti, E.</au><au>Saglia, R.</au><au>Sapone, D.</au><au>Scaramella, R.</au><au>Schneider, P.</au><au>Scottez, V.</au><au>Secroun, A.</au><au>Sirri, G.</au><au>Stanco, L.</au><au>Sureau, F.</au><au>Tavagnacco, D.</au><au>Tenti, M.</au><au>Tereno, I.</au><au>Toledo-Moreo, R.</au><au>Valenziano, L.</au><au>Vassallo, T.</au><au>Zacchei, A.</au><au>Zoubian, J.</au><au>Zucca, E.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Euclid preparation</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2019-11-01</date><risdate>2019</risdate><volume>631</volume><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract><![CDATA[We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, updating the calculation presented in the Euclid Red Book in several ways. We account for revisions to the Euclid near-infrared filter wavelengths; we adopt steeper rates of decline of the quasar luminosity function (QLF; Φ) with redshift, Φ ∝ 10k(z − 6), k = −0.72, and a further steeper rate of decline, k = −0.92; we use better models of the contaminating populations (MLT dwarfs and compact early-type galaxies); and we make use of an improved Bayesian selection method, compared to the colour cuts used for the Red Book calculation, allowing the identification of fainter quasars, down to JAB ∼ 23. Quasars at z > 8 may be selected from Euclid OYJH photometry alone, but selection over the redshift interval 7 < z < 8 is greatly improved by the addition of z-band data from, e.g., Pan-STARRS and LSST. We calculate predicted quasar yields for the assumed values of the rate of decline of the QLF beyond z = 6. If the decline of the QLF accelerates beyond z = 6, with k = −0.92, Euclid should nevertheless find over 100 quasars with 7.0 < z < 7.5, and ∼25 quasars beyond the current record of z = 7.5, including ∼8 beyond z = 8.0. The first Euclid quasars at z > 7.5 should be found in the DR1 data release, expected in 2024. It will be possible to determine the bright-end slope of the QLF, 7 < z < 8, M1450 < −25, using 8 m class telescopes to confirm candidates, but follow-up with JWST or E-ELT will be required to measure the faint-end slope. Contamination of the candidate lists is predicted to be modest even at JAB ∼ 23. The precision with which k can be determined over 7 < z < 8 depends on the value of k, but assuming k = −0.72 it can be measured to a 1σ uncertainty of 0.07.]]></abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201936427</doi></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6361 |
| ispartof | Astronomy and astrophysics (Berlin), 2019-11, Vol.631 |
| issn | 0004-6361 1432-0746 |
| language | eng |
| recordid | cdi_proquest_journals_2486564087 |
| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals |
| subjects | Astronomical models Compact galaxies Contamination Infrared filters Luminosity methods: statistical Quasars quasars: general Red shift surveys Telescopes |
| title | Euclid preparation |
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