Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISP

E. Lusso; S. Fotopoulou; M. Selwood; V. Allevato; G. Calderone; C. Mancini; M. Mignoli; M. Scodeggio; L. Bisigello; A. Feltre; F. Ricci; F. La Franca; D. Vergani; L. Gabarra; V. Le Brun; E. Maiorano; E. Palazzi; M. Moresco; G. Zamorani; G. Cresci; K. Jahnke; A. Humphrey; H. Landt; F. Mannucci; A. Marconi; L. Pozzetti; P. Salucci; M. Salvato; F. Shankar; L. Spinoglio; D. Stern; S. Serjeant; N. Aghanim; B. Altieri; A. Amara; S. Andreon; T. Auphan; N. Auricchio; M. Baldi; S. Bardelli; R. Bender; D. Bonino; E. Branchini; M. Brescia; S. M. Niemi; P. Schneider; Y. Wang; G. Gozaliasl; A. Hall; A. G. Sánchez; Euclid Collaboration

doi:10.1051/0004-6361/202348326

Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISP

E. Lusso^*, S. Fotopoulou, M. Selwood, V. Allevato, G. Calderone, C. Mancini, M. Mignoli, M. Scodeggio, L. Bisigello, A. Feltre, F. Ricci, F. La Franca, D. Vergani, L. Gabarra, V. Le Brun, E. Maiorano, E. Palazzi, M. Moresco, G. Zamorani, G. CresciK. Jahnke, A. Humphrey, H. Landt, F. Mannucci, A. Marconi, L. Pozzetti, P. Salucci, M. Salvato, F. Shankar, L. Spinoglio, D. Stern, S. Serjeant, N. Aghanim, B. Altieri, A. Amara, S. Andreon, T. Auphan, N. Auricchio, M. Baldi, S. Bardelli, R. Bender, D. Bonino, E. Branchini, M. Brescia, S. M. Niemi, P. Schneider, Y. Wang, G. Gozaliasl, A. Hall, A. G. Sánchez, Euclid Collaboration

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Tutkimustuotos: Lehtiartikkeli › Article › Scientific › vertaisarvioitu

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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.

Alkuperäiskieli	Englanti
Artikkeli	A108
Sivut	1-30
Sivumäärä	30
Julkaisu	Astronomy and Astrophysics
Vuosikerta	685
DOI - pysyväislinkit	https://doi.org/10.1051/0004-6361/202348326
Tila	Julkaistu - 1 toukok. 2024
OKM-julkaisutyyppi	A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä

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10.1051/0004-6361/202348326

Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISPFinal published version, 8,64 MBLisenssi: CC BY

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Lusso, E., Fotopoulou, S., Selwood, M., Allevato, V., Calderone, G., Mancini, C., Mignoli, M., Scodeggio, M., Bisigello, L., Feltre, A., Ricci, F., La Franca, F., Vergani, D., Gabarra, L., Le Brun, V., Maiorano, E., Palazzi, E., Moresco, M., Zamorani, G., ... Euclid Collaboration (2024). Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISP. Astronomy and Astrophysics, 685, 1-30. Artikkeli A108. https://doi.org/10.1051/0004-6361/202348326

@article{47252f9665d94291ba3cbcd021c80dc9,

title = "Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISP",

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.",

keywords = "Galaxies: active, Quasars: general, Quasars: supermassive black holes",

author = "E. Lusso and S. Fotopoulou and M. Selwood and V. Allevato and G. Calderone and C. Mancini and M. Mignoli and M. Scodeggio and L. Bisigello and A. Feltre and F. Ricci and {La Franca}, F. and D. Vergani and L. Gabarra and {Le Brun}, V. and E. Maiorano and E. Palazzi and M. Moresco and G. Zamorani and G. Cresci and K. Jahnke and A. Humphrey and H. Landt and F. Mannucci and A. Marconi and L. Pozzetti and P. Salucci and M. Salvato and F. Shankar and L. Spinoglio and D. Stern and S. Serjeant and N. Aghanim and B. Altieri and A. Amara and S. Andreon and T. Auphan and N. Auricchio and M. Baldi and S. Bardelli and R. Bender and D. Bonino and E. Branchini and M. Brescia and Niemi, {S. M.} and P. Schneider and Y. Wang and G. Gozaliasl and A. Hall and S{\'a}nchez, {A. G.} and {Euclid Collaboration}",

year = "2024",

month = may,

day = "1",

doi = "10.1051/0004-6361/202348326",

language = "English",

volume = "685",

pages = "1--30",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Lusso, E, Fotopoulou, S, Selwood, M, Allevato, V, Calderone, G, Mancini, C, Mignoli, M, Scodeggio, M, Bisigello, L, Feltre, A, Ricci, F, La Franca, F, Vergani, D, Gabarra, L, Le Brun, V, Maiorano, E, Palazzi, E, Moresco, M, Zamorani, G, Cresci, G, Jahnke, K, Humphrey, A, Landt, H, Mannucci, F, Marconi, A, Pozzetti, L, Salucci, P, Salvato, M, Shankar, F, Spinoglio, L, Stern, D, Serjeant, S, Aghanim, N, Altieri, B, Amara, A, Andreon, S, Auphan, T, Auricchio, N, Baldi, M, Bardelli, S, Bender, R, Bonino, D, Branchini, E, Brescia, M, Niemi, SM, Schneider, P, Wang, Y, Gozaliasl, G, Hall, A, Sánchez, AG & Euclid Collaboration 2024, 'Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISP', Astronomy and Astrophysics, Vuosikerta 685, A108, Sivut 1-30. https://doi.org/10.1051/0004-6361/202348326

TY - JOUR

T1 - Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISP

AU - Lusso, E.

AU - Fotopoulou, S.

AU - Selwood, M.

AU - Allevato, V.

AU - Calderone, G.

AU - Mancini, C.

AU - Mignoli, M.

AU - Scodeggio, M.

AU - Bisigello, L.

AU - Feltre, A.

AU - Ricci, F.

AU - La Franca, F.

AU - Vergani, D.

AU - Gabarra, L.

AU - Le Brun, V.

AU - Maiorano, E.

AU - Palazzi, E.

AU - Moresco, M.

AU - Zamorani, G.

AU - Cresci, G.

AU - Jahnke, K.

AU - Humphrey, A.

AU - Landt, H.

AU - Mannucci, F.

AU - Marconi, A.

AU - Pozzetti, L.

AU - Salucci, P.

AU - Salvato, M.

AU - Shankar, F.

AU - Spinoglio, L.

AU - Stern, D.

AU - Serjeant, S.

AU - Aghanim, N.

AU - Altieri, B.

AU - Amara, A.

AU - Andreon, S.

AU - Auphan, T.

AU - Auricchio, N.

AU - Baldi, M.

AU - Bardelli, S.

AU - Bender, R.

AU - Bonino, D.

AU - Branchini, E.

AU - Brescia, M.

AU - Niemi, S. M.

AU - Schneider, P.

AU - Wang, Y.

AU - Gozaliasl, G.

AU - Hall, A.

AU - Sánchez, A. G.

AU - Euclid Collaboration

PY - 2024/5/1

Y1 - 2024/5/1

N2 - 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.

AB - 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.

KW - Galaxies: active

KW - Quasars: general

KW - Quasars: supermassive black holes

UR - http://www.scopus.com/inward/record.url?scp=85193450196&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202348326

DO - 10.1051/0004-6361/202348326

M3 - Article

AN - SCOPUS:85193450196

SN - 0004-6361

VL - 685

SP - 1

EP - 30

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A108

ER -

Euclid preparation. XXXVIII. Spectroscopy of active galactic nuclei with NISP

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