CANDELS EGS F160W J141956.5+525527.4 , the SIMBAD biblio

CANDELS EGS F160W J141956.5+525527.4 , the SIMBAD biblio (8 results) C.D.S. - SIMBAD4 rel 1.8 - 2026.10.19CEST02:12:25


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Title First 3 Authors
2014ApJS..214...24S viz 15       D               1 97940 733 3D-HST WFC3-selected photometric catalogs in the five CANDELS/3D-HST fields: photometry, photometric redshifts, and stellar masses. SKELTON R.E., WHITAKER K.E., MOMCHEVA I.G., et al.
2015ApJ...803...34B viz 16       D               1 10313 1045 UV luminosity functions at redshifts z ∼ 4 to z ∼ 10: 10,000 galaxies from HST legacy fields. BOUWENS R.J., ILLINGWORTH G.D., OESCH P.A., et al.
2017ApJS..229...32S viz 16       D               1 37883 113 CANDELS multi-wavelength catalogs: source identification and photometry in the CANDELS Extended Groth Strip. STEFANON M., YAN H., MOBASHER B., et al.
2023ApJ...949L..18P 17       D               1 28 19 CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear-Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging. PAPOVICH C., COLE J.W., YANG G., et al.
2023ApJ...956..139I 17       D               1 16 ~ Redshift Evolution of Electron Density in the Interstellar Medium at z ∼ 0-9 Uncovered with JWST/NIRSpec Spectra and Line-spread Function Determinations. ISOBE Y., OUCHI M., NAKAJIMA K., et al.
2023ApJS..269...33N viz 17       D               1 187 ~ JWST Census for the Mass-Metallicity Star Formation Relations at z = 4-10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators. NAKAJIMA K., OUCHI M., ISOBE Y., et al.
2023ApJ...959..100I 17       D               1 67 ~ JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6-10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation. ISOBE Y., OUCHI M., TOMINAGA N., et al.
2025A&A...700A..12M 19       D               1 57 ~ Narrow-line AGN selection in CEERS: Spectroscopic selection, physical properties, and X-ray and radio analysis. MAZZOLARI G., SCHOLTZ J., MAIOLINO R., et al.

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