JADES NIRSpec Spectroscopy of GN-z11: Lyman- α emission and possible enhanced nitrogen abundance in a z = 10.60 luminous galaxy

被引：118

作者：

Bunker A.J. ^{[1
]}

Saxena A. ^{[1
,2
]}

Cameron A.J. ^{[1
]}

Willott C.J. ^{[3
]}

Curtis-Lake E. ^{[4
]}

Jakobsen P. ^{[5
,6
]}

Carniani S. ^{[7
]}

Smit R. ^{[8
]}

Maiolino R. ^{[2
,9
,10
]}

Witstok J. ^{[9
,10
]}

Curti M. ^{[9
,10
,11
]}

D'eugenio F. ^{[9
,10
]}

Jones G.C. ^{[1
]}

Ferruit P. ^{[12
]}

Arribas S. ^{[13
]}

Charlot S. ^{[14
]}

Chevallard J. ^{[1
]}

Giardino G. ^{[15
]}

De Graaff A. ^{[16
]}

Looser T.J. ^{[9
,10
]}

Lützgendorf N. ^{[17
]}

Maseda M.V. ^{[18
]}

Rawle T. ^{[17
]}

Rix H.-W. ^{[16
]}

Del Pino B.R. ^{[13
]}

Alberts S. ^{[19
]}

Egami E. ^{[19
]}

Eisenstein D.J. ^{[20
]}

Endsley R. ^{[21
]}

Hainline K. ^{[19
]}

Hausen R. ^{[22
]}

Johnson B.D. ^{[20
]}

Rieke G. ^{[19
]}

Rieke M. ^{[19
]}

Robertson B.E. ^{[23
]}

Shivaei I. ^{[19
]}

Stark D.P. ^{[19
]}

Sun F. ^{[19
]}

Tacchella S. ^{[9
,10
]}

Tang M. ^{[19
]}

Williams C.C. ^{[19
,24
]}

Willmer C.N.A. ^{[19
]}

Baker W.M. ^{[9
,10
]}

Baum S. ^{[25
]}

Bhatawdekar R. ^{[12
,26
]}

Bowler R. ^{[27
]}

Boyett K. ^{[28
,29
]}

Chen Z. ^{[19
]}

Circosta C. ^{[12
]}

Helton J.M. ^{[19
]}

机构：

[1] Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford

[2] Department of Physics and Astronomy, University College London, Gower Street, London

[3] NRC Herzberg, 5071 West Saanich Rd, Victoria, V9E 2E7, BC

[4] Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield

[5] Cosmic Dawn Center (DAWN), Copenhagen

[6] Niels Bohr Institute, University of Copenhagen, Jagtvej 128, Copenhagen

[7] Scuola Normale Superiore, Piazza dei Cavalieri 7, Pisa

[8] Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool

[9] Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge

[10] Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge

[11] European Southern Observatory, Karl-Schwarzschild-Strasse 2, Garching bei Muenchen

[12] European Space Agency (ESA), European Space Astronomy Centre (ESAC), Camino Bajo del Castillo s/n, Villanueva de la Cañada, Madrid

[13] Centro de Astrobiología (CAB), CSIC-INTA, Cra. de Ajalvir Km. 4, Torrej'on de Ardoz, Madrid

[14] Sorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, Paris

[15] ATG Europe for the European Space Agency, ESTEC, Noordwijk

[16] Max-Planck-Institut für Astronomie, Königstuhl 17, Heidelberg

[17] European Space Agency, Space Telescope Science Institute, Baltimore, MD

[18] Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St, Madison, 53706, WI

[19] Steward Observatory, University of Arizona, 933 N. Cherry Ave, Tucson, 85721, AZ

[20] Center for Astrophysics - Harvard & Smithsonian, 60 Garden St., Cambridge, 02138, MA

[21] Department of Astronomy, University of Texas, Austin, 78712, TX

[22] Department of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, 21218, MD

[23] Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, 95064, CA

[24] NSF's National Optical-Infrared Astronomy Research Laboratory, 950 North Cherry Avenue, Tucson, 85719, AZ

[25] Department of Physics and Astronomy, University of Manitoba, Winnipeg, R3T 2N2, MB

[26] European Space Agency, ESA/ESTEC, Keplerlaan 1, Noordwijk

[27] Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, School of Natural Sciences, The University of Manchester, Manchester

[28] School of Physics, University of Melbourne, Parkville, 3010, VIC

[29] AURA for European Space Agency, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, 21210, MD

[30] Department for Astrophysical and Planetary Science, University of Colorado, Boulder, 80309, CO

[31] Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics, Stanford University, Stanford, 94305, CA

来源：

Astronomy and Astrophysics | 2023年 / 677卷

基金：

英国科研创新办公室; 欧盟地平线“2020”; 澳大利亚研究理事会; 美国国家科学基金会; 英国科学技术设施理事会; 欧洲研究理事会;

关键词：

Galaxies: Abundances; Galaxies: Evolution; Galaxies: Groups: Individual: GN-z11; Galaxies: High-redshift;

D O I：

10.1051/0004-6361/202346159

中图分类号：

学科分类号：

摘要：

We present JADES JWST/NIRSpec spectroscopy of GN-z11, the most luminous candidate z>10 Lyman break galaxy in the GOODS-North field with MUV =-21.5. We derive a redshift of z = 10.603 (lower than previous determinations) based on multiple emission lines in our low and medium resolution spectra over 0.7- 5.3 μm. We significantly detect the continuum and measure a blue rest-UV spectral slope of β =-2.4. Remarkably, we see spatially extended Lyman-α in emission (despite the highly neutral intergalactic medium expected at this early epoch), offset 555 km s-1 redwards of the systemic redshift. From our measurements of collisionally excited lines of both low and high ionisation (including [O II] λ3727, [Ne III] λ3869, and C III] λ1909), we infer a high ionisation parameter (log U ∼-2). We detect the rarely seen N IV] λ1486 and N III] λ1748 lines in both our low and medium resolution spectra, with other high ionisation lines seen in the low resolution spectrum, such as He II (blended with O III]) and C IV (with a possible P-Cygni profile). Based on the observed rest-UV line ratios, we cannot conclusively rule out photoionisation from an active galactic nucleus (AGN), although the high C III]/He II and N III]/He II ratios are compatible with a star formation explanation. If the observed emission lines are powered by star formation, then the strong N III] λ1748 observed may imply an unusually high N/O abundance. Balmer emission lines (Hγ, Hδ) are also detected, and if powered by star formation rather than an AGN, we infer a star formation rate of ∼20-30 M⊙ yr-1 (depending on the initial mass function) and low dust attenuation. Our NIRSpec spectroscopy confirms that GN-z11 is a remarkable galaxy with extreme properties seen 430 Myr after the Big Bang. © The Authors 2023.

引用

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