'$ to 0.86 '$, these dual and lensed systems are among the most compact systems discovered to date at $z \u003E0.5$. This is the largest sample of distant dual AGN with sub-arcsecond separations ever presented in a single paper.","authors":[{"id":"65f7e284aba54d76180c33a4","name":"M. Scialpi","org":"Univ Trento, Via Sommar 14, I-38123 Trento, Italy","orgid":"5f71b3021c455f439fe3fcf6"},{"id":"53f43964dabfaee1c0ab9b3e","name":"F. Mannucci","org":"INAF Osservat Astrofis Arcetri, Via Largo E Fermi 5, I-50125 Florence, Italy"},{"id":"6525690555b3f8ac4679061f","name":"C. Marconcini","org":"Univ Firenze, Dipartimento Fis & Astron, via G Sansone 1, I-50019 Florence, Italy","orgid":"5f71b2a81c455f439fe3d512"},{"id":"64cc9b9870d44317c2e33535","name":"G. Venturi","org":"INAF Osservat Astrofis Arcetri, Via Largo E Fermi 5, I-50125 Florence, Italy"},{"id":"65f7e284aba54d76180c33af","name":"E. 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Volonteri","org":"Inst Astrophys Paris, 98bis Bd Arago, F-75014 Paris, France","orgid":"61e69ca2689627346573fa07"}],"create_time":"2024-08-05T01:38:07.787Z","doi":"10.1051\u002F0004-6361\u002F202347242","id":"646aecaad68f896efa05a813","issn":"0004-6361","keywords":["galaxies: active","quasars: general"],"lang":"en","num_citation":1,"pdf":"https:\u002F\u002Fcz5waila03cyo0tux1owpyofgoryroob.aminer.cn\u002F96\u002FEA\u002FA7\u002F96EAA705EC0B805095544014294F41D0.pdf","title":"MUSE Adaptive-Optics Spectroscopy Confirms Dual Active Galactic Nuclei and Strongly Lensed Systems at Sub-Arcsec Separation","update_times":{"u_a_t":"2024-12-25T17:47:12Z","u_v_t":"2024-12-25T17:47:12Z"},"urls":["http:\u002F\u002Farxiv.org\u002Fabs\u002F2305.11850"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"volume":"690"},"venue_hhb_id":"5ea6227dedb6e7d53c043ca8","versions":[{"id":"646aecaad68f896efa05a813","sid":"2305.11850","src":"arxiv","vsid":"ASTRONOMY & ASTROPHYSICS","year":2024},{"id":"66a05f9c01d2a3fbfcafe789","sid":"10.1051\u002F0004-6361\u002F202347242","src":"crossref","year":2024},{"id":"672dc02c01d2a3fbfc9274ba","sid":"W4400917127","src":"openalex","vsid":"S205231332","year":2024},{"id":"673f0fb7ae8580e7ff3cbb2e","sid":"WOS:001322237700034","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2024}],"year":2024},{"authors":[{"id":"56289ee445cedb33987ced91","name":"Anna Brucalassi"},{"id":"53f7a456dabfae90ec10fa83","name":"Andrea Tozzi"},{"id":"64cc9de370d44317c2e3804c","name":"Ernesto Oliva"},{"id":"561960a245ce1e5964348b8e","name":"José A. 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It is a fiber-fed high-resolution, high-stability spectrograph. Its design follows the guidelines of successful predecessors such as HARPS and ESPRESSO. In this paper we present the status of the spectrograph at the preliminary design stage. The spectrograph will be a warm, vacuum-operated, thermally controlled and fiber-fed echelle spectrograph. Following the phase A design, the huge etendue of the telescope will be reformed in the instrument with a long slit made of smaller fibers. We discuss the system design of the spectrographs system.","authors":[{"id":"53f43ab6dabfaedd74dc9f74","name":"Bruno Chazelas"},{"name":"Yevgeniy Ivanisenko"},{"id":"66987c63cc679af4819de4d3","name":"Audrey Lanotte"},{"name":"Pablo Santos Diaz"},{"id":"63796788f789b382be99f2c3","name":"Ludovic Genolet"},{"id":"65310e6c933f74a274e371fc","name":"Michael Sordet"},{"id":"6379f9b6f789b382be9e120f","name":"Ian Hughes"},{"id":"53f78669dabfae92b40c2d0d","name":"Christophe Lovis"},{"id":"64ccaa73d6fcf4e73504419b","name":"Tobias M. Schmidt"},{"id":"637aaf95f789b382bea301c1","name":"Manuel Amate"},{"id":"65e073f08a47b621f78beeba","name":"José Peñate Castro"},{"id":"662312722173360a69120155","name":"Afrodisio Vega Moreno"},{"id":"637b0a64f789b382bea55847","name":"Fabio Tenegi"},{"id":"66987c58f53397aa74b8e6c4","name":"Roberto Simoes"},{"id":"668b619f6a21953c983a7863","name":"Jonay I. 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The ESA space mission, launched on July $ 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 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 H alpha N ii complex, as 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 H alpha is visible (i.e. $0.892 $\\,erg $ cm$^ $, encompassing the peak of AGN activity at $z within the spectral coverage of the red grism. Outside this redshift range, the measurement efficiency decreases significantly. Overall, a spectroscopic redshift is correctly determined for about 90 of type 2 AGN down to an emission line flux of roughly $3 $\\,erg $ cm$^ $, and for type 1 AGN down to $8.5 $\\,erg $ cm$^ $. 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 $z\u003C2$, 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.","authors":[{"id":"53f42af6dabfaeb22f3e0614","name":"E. Lusso","org":"INAF, Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy"},{"id":"53f3965fdabfae4b34a74c08","name":"S. 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Mignoli","org":"INAF, Osservatorio Astrofis & Sci Spazio Bologna, Via Piero Gobetti 93-3, I-40129 Bologna, Italy"},{"id":"53f3735cdabfae4b349c8e2b","name":"M. Scodeggio","org":"INAF, IASF Milano, Via Alfonso Corti 12, I-20133 Milan, Italy"},{"id":"53f3735cdabfae4b349c8e2b","name":"L. Bisigello","org":"Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy","orgid":"5f71b29f1c455f439fe3d265"},{"id":"5613ede745cedb3397a0c375","name":"A. Feltre","org":"INAF, Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy"},{"id":"561dbdfe45ce1e59648811f5","name":"F. Ricci","org":"Roma Tre Univ, Dept Math & Phys, Via Vasca Navale 84, I-00146 Rome, Italy","orgid":"5f71b3091c455f439fe3fff7"},{"id":"561dbdfe45ce1e59648811f5","name":"F. La Franca","org":"Roma Tre Univ, Dept Math & Phys, Via Vasca Navale 84, I-00146 Rome, Italy","orgid":"5f71b3091c455f439fe3fff7"},{"id":"560b809045cedb339733797e","name":"D. 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Zamorani","org":"INAF, Osservatorio Astrofis & Sci Spazio Bologna, Via Piero Gobetti 93-3, I-40129 Bologna, Italy"},{"id":"53f44d53dabfaefedbb2ed70","name":"G. Cresci","org":"INAF, Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy"},{"id":"53f449a7dabfaeb22f4cd4fb","name":"K. Jahnke","org":"Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany"},{"id":"53f436d4dabfaee43ec33cdd","name":"A. Humphrey","org":"Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal","orgid":"5f71b5bc1c455f439fe52f31"},{"id":"53f436d4dabfaee43ec33cdd","name":"H. Landt","org":"Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England","orgid":"5f71b50b1c455f439fe4e5f8"},{"id":"53f43964dabfaee1c0ab9b3e","name":"F. Mannucci","org":"INAF, Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy"},{"id":"53f42eaddabfaee0d9b0da50","name":"A. 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Zinchenko"}],"create_time":"2023-11-22T02:31:15.886Z","doi":"10.1051\u002F0004-6361\u002F202348326","id":"655d63dc939a5f4082db925d","issn":"0004-6361","keywords":["galaxies: active","quasars: general","quasars: supermassive black holes"],"lang":"en","num_citation":0,"pdf":"https:\u002F\u002Fcz5waila03cyo0tux1owpyofgoryroob.aminer.cn\u002FF0\u002FE9\u002FD1\u002FF0E9D14714FA56CB62A16B9DEE17B548.pdf","title":"Euclid Preparation XXXVIII. Spectroscopy of Active Galactic Nuclei with NISP","update_times":{"u_a_t":"2024-12-25T03:31:31Z","u_v_t":"2024-12-25T03:31:31Z"},"urls":["http:\u002F\u002Farxiv.org\u002Fabs\u002F2311.12096"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"volume":"685"},"versions":[{"id":"655d63dc939a5f4082db925d","sid":"2311.12096","src":"arxiv","vsid":"ASTRONOMY & ASTROPHYSICS","year":2024},{"id":"6612d82213fb2c6cf6716d53","sid":"W4391741303","src":"openalex","vsid":"S205231332","year":2024},{"id":"66651c4101d2a3fbfc246d50","sid":"10.1051\u002F0004-6361\u002F202348326","src":"crossref","year":2024},{"id":"673f2796ae8580e7ffc667c5","sid":"WOS:001271220100004","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2024}],"year":2024},{"abstract":"PDS 456 is the most luminous (L-bol similar to 10(47) erg s(-1)) radio-quiet quasar at z \u003C 0.3 and can be regarded as a local counterpart of the powerful quasars shining at Cosmic Noon. It hosts a strong nuclear X-ray ultra-fast (similar to 0.3c) outflow, and a massive and clumpy CO (3-2) molecular outflow extending up to similar to 5 kpc from the nucleus. We analyzed the first MUSE Wide Field Mode (WFM) and Adaptive-Optics Narrow Field Mode (AO-NFM) optical integral field spectroscopic observations of PDS456. The AO-NFM observations provide an unprecedented spatial resolution, reaching up to similar to 280 pc. Our findings reveal a complex circumgalactic medium around PDS 456, extending to a maximum projected size of approximate to 46 kpc. This includes a reservoir of gas with a mass of similar to 10(7) - 10(8) M-circle dot, along with eight companion galaxies and a multi-phase outflow. WFM and NFM MUSE data reveal an outflow on a large scale (approximate to 12 kpc from the quasar) in [O III], and on smaller scales (within 3 kpc) with higher resolution (about 280 pc) in H alpha, respectively. The [O III] outflow mass rate is 2.3 +\u002F- 0.2 M-circle dot yr(-1) which is significantly lower than those typically found in other luminous quasars. Remarkably, the H alpha outflow shows a similar scale, morphology, and kinematics to the CO (3-2) molecular outflow, with the latter dominating in terms of kinetic energy and mass outflow rate by two and one orders of magnitude, respectively. Our results therefore indicate that mergers, powerful active galactic nucleus (AGN) activity, and feedback through AGN-driven winds collectively contribute to shaping the host galaxy evolution of PDS 456, and likely that of similar objects at the brightest end of the AGN luminosity function across all redshifts. Moreover, the finding that the momentum boost of the total outflow deviates from the expected energy-conserving expansion for large-scale outflows highlights the need of novel AGN-driven outflow models to comprehensively interpret these phenomena.","authors":[{"email":"andrea.travascio@unimib.it","id":"64e12ae5e64457845b8914d9","name":"A. Travascio","org":"Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy","orgid":"5f71b5181c455f439fe4ec03"},{"id":"53f43ce7dabfaeb22f4a6d68","name":"E. Piconcelli","org":"INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Rome, Italy"},{"id":"655712b6145e064b7afcbd72","name":"M. Bischetti","org":"INAF, Osservatorio Astron Trieste, Via G B Tiepolo 11, I-34143 Trieste, Italy"},{"id":"53f44d53dabfaefedbb2ed70","name":"G. Cresci","org":"INAF, Osservatorio Astrofisco Arcetri, Largo E Fermi 5, I-50127 Florence, Italy","orgid":"5f71b3fe1c455f439fe46ce5"},{"id":"53f43e9ddabfaeb22f4aab33","name":"C. Feruglio","org":"INAF, Osservatorio Astron Trieste, Via G B Tiepolo 11, I-34143 Trieste, Italy"},{"id":"64cc9ca270d44317c2e35911","name":"M. Perna","org":"CSIC, Ctr Astrobiol CAB, INTA, Cra Ajalvir Km 4, Torrejon De Ardoz 28850, Madrid, Spain"},{"id":"62e494ddd9f204418d6b561c","name":"G. Vietri","org":"INAF, Ist Astrofis Spaziale & Fis cosm Milano, Via Alfonso Corti 12, I-20133 Milan, Italy","orgid":"5f71b3fe1c455f439fe46ce5"},{"id":"62e48be4d9f204418d6a4302","name":"S. Carniani","org":"Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy"},{"id":"662e9bd778ac4d5586208376","name":"S. Cantalupo","org":"Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy","orgid":"5f71b5181c455f439fe4ec03"},{"id":"62e48aa1d9f204418d6a1c9e","name":"C. Cicone","org":"Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway","orgid":"5f71b2841c455f439fe3c6ae"},{"id":"62e4b8a6d9f204418d6fb357","name":"M. Ginolfi","org":"Univ Studi Firenze, Dipartimento Astron & Sci Spazio, Largo E Fermi 2, I-50125 Florence, Italy"},{"id":"64cc9b9870d44317c2e33535","name":"G. Venturi","org":"INAF, Osservatorio Astrofisco Arcetri, Largo E Fermi 5, I-50127 Florence, Italy","orgid":"5f71b3fe1c455f439fe46ce5"},{"name":"K. Zubovas","org":"Ctr Phys Sci & Technol, Sauletekio al 3, LT-10257 Vilnius, Lithuania"},{"id":"560be1e945cedb339740f6ac","name":"A. Bongiorno","org":"INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Rome, Italy"},{"id":"541079cadabfae44f08b1cce","name":"M. Brusa","org":"Univ Bologna, Dipartimento Fis & Astron Augusto Righi, Via P Gobetti, 93-2, I-40129 Bologna, Italy"},{"id":"62e4bb14d9f204418d7072e1","name":"A. Luminari","org":"INAF, Ist Astrofis & Planetol Spaziali, Via Fosso Caveliere 100, I-00133 Rome, Italy"},{"id":"6695d72e3e4f48d5c85b1072","name":"V. Mainieri","org":"European Southern Observ, Karl Schwarzschild Str 2, Garching, Germany","orgid":"61e69b5d689627346573cd3a"},{"id":"53f42eaddabfaee0d9b0da50","name":"A. Marconi","org":"Univ Studi Firenze, Dipartimento Astron & Sci Spazio, Largo E Fermi 2, I-50125 Florence, Italy"},{"id":"66828bb271bd11f631c0963b","name":"N. Menci","org":"INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Rome, Italy"},{"id":"561e7ec745ce1e596493576f","name":"E. Nardini","org":"INAF, Osservatorio Astrofisco Arcetri, Largo E Fermi 5, I-50127 Florence, Italy","orgid":"5f71b3fe1c455f439fe46ce5"},{"id":"62e4bf12d9f204418d71e798","name":"A. Pensabene","org":"Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy","orgid":"5f71b5181c455f439fe4ec03"},{"id":"65570e31145e064b7afc713a","name":"C. Ramos Almeida","org":"Inst Astrofis Canarias, Calle Via Lactea,S-N, San Cristobal la Laguna 38205, Tenerife, Spain"},{"id":"65d52acdc136ef13319d2c4c","name":"F. Tombesi","org":"INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Rome, Italy"},{"id":"62aab0c4d9f2040d085cac23","name":"C. Vignali","org":"Univ Bologna, Dipartimento Fis & Astron Augusto Righi, Via P Gobetti, 93-2, I-40129 Bologna, Italy"},{"id":"53f434eddabfaedce5521c4e","name":"L. Zappacosta","org":"INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Rome, Italy"},{"id":"53f32ad1dabfae9a8448c3fe","name":"F. Fiore","org":"INAF, Osservatorio Astron Trieste, Via G B Tiepolo 11, I-34143 Trieste, Italy"}],"create_time":"2024-03-29T18:14:36.935Z","doi":"10.1051\u002F0004-6361\u002F202449201","id":"6604cf0513fb2c6cf6b6cc17","issn":"0004-6361","keywords":["galaxies: active","intergalactic medium","galaxies: nuclei","quasars: emission lines","quasars: supermassive black holes","quasars: individual: PDS 456"],"lang":"en","num_citation":0,"pdf":"https:\u002F\u002Fcz5waila03cyo0tux1owpyofgoryroob.aminer.cn\u002F1C\u002F72\u002F4A\u002F1C724A63035C23746A06DCE7AF26C7C8.pdf","title":"MUSE View of PDS 456: Kiloparsec-scale Wind, Extended Ionized Gas, and Close Environment","update_times":{"u_a_t":"2024-12-25T20:25:05Z","u_v_t":"2024-12-25T20:25:05Z"},"urls":["http:\u002F\u002Farxiv.org\u002Fabs\u002F2403.18043"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"volume":"686"},"venue_hhb_id":"5ea6227dedb6e7d53c043ca8","versions":[{"id":"6604cf0513fb2c6cf6b6cc17","sid":"2403.18043","src":"arxiv","vsid":"ASTRONOMY & ASTROPHYSICS","year":2024},{"id":"661dd7f613fb2c6cf6b1f8f2","sid":"10.1051\u002F0004-6361\u002F202449201","src":"crossref","year":2024},{"id":"6652a32f01d2a3fbfc034fb6","sid":"W4393299907","src":"openalex","vsid":"S4306400194","year":2024},{"id":"66589cfe01d2a3fbfca4bad4","sid":"W4394822549","src":"openalex","vsid":"S205231332","year":2024},{"id":"66b4746b01d2a3fbfcb25e0a","sid":"WOS:001250131100009","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2024}],"year":2024}],"profilePubsTotal":438,"profilePatentsPage":0,"profilePatents":null,"profilePatentsTotal":null,"profilePatentsEnd":false,"profileProjectsPage":0,"profileProjects":null,"profileProjectsTotal":null,"newInfo":null,"checkDelPubs":[]}};