In-orbit Performance of the Near-infrared Spectrograph NIRSpec on the James Webb Space Telescope

Beck, Tracy; Birkmann, Stephan M.; Giardino, G.; Keyes, C. D.; Kumari, Nimisha; Muzerolle, James; Rawle, Tim; Zeidler, Peter; Abul-Huda, Yasin; Oliveira, Catarina Alves de; Arribas, S.; Bechtold, Katie; Bhatawdekar, Rachana; Bonaventura, Nina; Bunker, A. J.; Cameron, Alex; Carniani, Stefano; Charlot, S.; Curti, Mirko; Espinoza, N.; Ferruit, Pierre; Franx, Marijn; Jakobsen, P.; Karakla, Diane; López‐Caniego, M.; Lützgendorf, Nora; Maiolino, R.; Manjavacas, Elena; Marston, A. P.; Moseley, S. H.; Ogle, Patrick; Perna, M.; Peña-Guerrero, María; Pirzkal, Norbert; Plesha, Rachel; Proffitt, Charles; Rauscher, Bernard J.; Rix, Hans─Walter; Pino, Bruno Rodríguez Del; Rustamkulov, Zafar; Sabbi, E.; Sing, David K.; Sirianni, M.; Plate, Maurice te; Úbeda, Leonardo; Wahlgren, G. M.; Wislowski, Emily; Wu, Rai

doi:10.1088/1538-3873/acb846

Cited by 91 publications

(35 citation statements)

References 29 publications

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“…The complete details of the CEERS program will be presented in Finkelstein et al (2023, in preparation), and the program data can be found at doi:10.17909/z7p0-8481 and at https:// archive.stsci.edu/hlsp/ceers. This source is one of the first to be observed and published with four JWST (Gardner et al 2023) observing modes: NIRSpec (Böker et al 2023), NIRCam (Rieke et al 2023), MIRI (Wright et al 2023), and NIRCam/ Wide-Field Slitless Spectrograph, or WFSS (Greene et al 2017). We describe these observations below and provide a summary of information about this source in Table 1.…”

Section: Datamentioning

confidence: 99%

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

Larson,

Finkelstein,

Kocevski

et al. 2023

ApJL

146

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We report the discovery of an accreting supermassive black hole at z = 8.679. This galaxy, denoted here as CEERS_1019, was previously discovered as a Lyα-break galaxy by Hubble with a Lyα redshift from Keck. As part of the Cosmic Evolution Early Release Science (CEERS) survey, we have observed this source with JWST/NIRSpec, MIRI, NIRCam, and NIRCam/WFSS and uncovered a plethora of emission lines. The Hβ line is best fit by a narrow plus a broad component, where the latter is measured at 2.5σ with an FWHM ∼1200 km s−1. We conclude this originates in the broadline region of an active galactic nucleus (AGN). This is supported by the presence of weak high-ionization lines (N V, N IV], and C III]), as well as a spatial point-source component. The implied mass of the black hole (BH) is log (M BH/M ⊙) = 6.95 ± 0.37, and we estimate that it is accreting at 1.2 ± 0.5 times the Eddington limit. The 1–8 μm photometric spectral energy distribution shows a continuum dominated by starlight and constrains the host galaxy to be massive (log M/M⊙ ∼9.5) and highly star-forming (star formation rate, or SFR ∼ 30 M⊙ yr−1; log sSFR ∼ − 7.9 yr−1). The line ratios show that the gas is metal-poor (Z/Z ⊙ ∼ 0.1), dense (n e ∼ 103 cm−3), and highly ionized (log U ∼ − 2.1). We use this present highest-redshift AGN discovery to place constraints on BH seeding models and find that a combination of either super-Eddington accretion from stellar seeds or Eddington accretion from very massive BH seeds is required to form this object.

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Section: Datamentioning

confidence: 99%

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

Larson,

Finkelstein,

Kocevski

et al. 2023

ApJL

146

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“…For the data reduction, we began by retrieving the uncal files from the Mikulksi Archive for Space Telescopes (MAST; doi:10.17909/jzze-5611). We performed ramps-to-slopes processing on those files using the NIRSpec Instrument Pipeline Software, 11 which features a correction for "snowballs" (Böker et al 2023) and a correction for residual correlated noise in IFU data. The resulting count rate maps (rate files) were used as inputs to the JWST calwebb_spec2 pipeline with the default processing steps, including assignment of the world coordinate system, flat-fielding, and aperture correction.…”

Section: Data Reductionmentioning

confidence: 99%

JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B*

Luhman

Tremblin

Birkmann

et al. 2023

ApJL

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We present 1–5 μm spectroscopy of the young planetary mass companion TWA 27B (2M1207B) performed with NIRSpec on board the James Webb Space Telescope. In these data, the fundamental band of CH4 is absent, and the fundamental band of CO is weak. The nondetection of CH4 reinforces a previously observed trend of weaker CH4 with younger ages among L dwarfs, which has been attributed to enhanced nonequilibrium chemistry among young objects. The weakness of CO may reflect an additional atmospheric property that varies with age, such as the temperature gradient or cloud thickness. We are able to reproduce the broad shape of the spectrum with an ATMO cloudless model that has T eff = 1300 K, nonequilibrium chemistry, and a temperature gradient reduction caused by fingering convection. However, the fundamental bands of CH4 and CO are somewhat stronger in the model. In addition, the model temperature of 1300 K is higher than expected from evolutionary models given the luminosity and age of TWA 27B (T eff = 1200 K). Previous models of young L-type objects suggest that the inclusion of clouds could potentially resolve these issues; it remains to be seen whether cloudy models can provide a good fit to the 1–5 μm data from NIRSpec. TWA 27B exhibits emission in Paschen transitions and the He I triplet at 1.083 μm, which are signatures of accretion that provide the first evidence of a circumstellar disk. We have used the NIRSpec data to estimate the bolometric luminosity of TWA 27B (log L/L ⊙ = −4.466 ± 0.014), which implies a mass of 5–6 M Jup according to evolutionary models.

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“…31 We note that the GLASS-JWST program also obtained Near-Infrared Imager and Slitless Spectrograph (NIRISS; Doyon et al 2012, R. Doyon et al 2023, in preparation) spectroscopy of the cluster core covering wavelengths λ ∼ 1.1-2.2 μm. The UNCOVER program also includes spectroscopic follow-up observations with JWST's Near Infrared Spectrograph (NIRSpec; Ferruit et al 2022;Jakobsen et al 2022;Böker et al 2023), which are scheduled for 2023 July and would allow deeper spectroscopic measurements and to longer wavelengths. A2744 will also be observed with NIRCam as part of the JWST guaranteed time observation (GTO) program Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS; Program ID: GTO 1176; PI: R. Windhorst;Windhorst et al 2023).…”

Section: Datamentioning

confidence: 99%

JWST UNCOVER: Extremely Red and Compact Object at z _phot ≃ 7.6 Triply Imaged by A2744

Furtak¹,

Zitrin²,

Plat³

et al. 2023

ApJ

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Recent JWST/NIRCam imaging taken for the ultra-deep UNCOVER program reveals a very red dropout object at z phot ≃ 7.6, triply imaged by the galaxy cluster A2744 (z d = 0.308). All three images are very compact, i.e., unresolved, with a delensed size upper limit of r e ≲ 35 pc. The images have apparent magnitudes of m F444W ∼ 25−26 AB, and the magnification-corrected absolute UV magnitude of the source is M UV,1450 = −16.81 ± 0.09. From the sum of observed fluxes and from a spectral energy distribution (SED) analysis, we obtain estimates of the bolometric luminosities of the source of L bol ≳ 1043 erg s−1 and L bol ∼ 1044–1046 erg s−1, respectively. Based on its compact, point-like appearance, its position in color–color space, and the SED analysis, we tentatively conclude that this object is a UV-faint dust-obscured quasar-like object, i.e., an active galactic nucleus at high redshift. We also discuss other alternative origins for the object’s emission features, including a massive star cluster, Population III, supermassive, or dark stars, or a direct-collapse black hole. Although populations of red galaxies at similar photometric redshifts have been detected with JWST, this object is unique in that its high-redshift nature is corroborated geometrically by lensing, that it is unresolved despite being magnified—and thus intrinsically even more compact—and that it occupies notably distinct regions in both size–luminosity and color–color space. Planned UNCOVER JWST/NIRSpec observations, scheduled in Cycle 1, will enable a more detailed analysis of this object.

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In-orbit Performance of the Near-infrared Spectrograph NIRSpec on the James Webb Space Telescope

Cited by 91 publications

References 29 publications

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B*

JWST UNCOVER: Extremely Red and Compact Object at z _phot ≃ 7.6 Triply Imaged by A2744

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In-orbit Performance of the Near-infrared Spectrograph NIRSpec on the James Webb Space Telescope

Cited by 91 publications

References 29 publications

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars

JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B*

JWST UNCOVER: Extremely Red and Compact Object at z phot ≃ 7.6 Triply Imaged by A2744

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JWST UNCOVER: Extremely Red and Compact Object at z _phot ≃ 7.6 Triply Imaged by A2744