Outshining in the spatially resolved analysis of a strongly lensed galaxy at z = 6.072 with JWST NIRCam
Artikel i vetenskaplig tidskrift, 2024

We present JWST/NIRCam observations of a strongly lensed, sub-L∗, multiply imaged galaxy at z=6.072, with magnification factors μ³20 across the galaxy. The galaxy has rich HST, MUSE, and ALMA ancillary observations across a broad wavelength range. Aiming to quantify the reliability of stellar mass estimates of high redshift galaxies, we performed a spatially resolved analysis of the physical properties at scales of ~200 pc, inferred from spectral energy distribution (SED) modelling of five JWST/NIRCam imaging bands covering 0.16 μm < λrest < 0.63 μm on a pixel-by-pixel basis. We find young stars surrounded by extended older stellar populations. By comparing Hα+[Nâ¯II] and [Oâ¯III]+Hβ maps inferred from the image analysis with our additional NIRSpec integral field unit (IFU) data, we find that the spatial distribution and strength of the line maps are in agreement with the IFU measurements. We explore different parametric star formation history (SFH) forms with BAGPIPES on the spatially integrated photometry, finding that a double power-law (DPL) star formation history retrieves the closest value to the spatially resolved stellar mass estimate, and other SFH forms suffer from the dominant outshining emission from the youngest stars, thus underestimating the stellar mass - up to ~0.5 dex. On the other hand, the DPL cannot match the IFU-measured emission lines. Additionally, the ionising photon production efficiency may be overestimated in a spatially integrated approach by ~0.15 dex, when compared to a spatially resolved analysis. The agreement with the IFU measurements implies that our pixel-by-pixel results derived from the broadband images are robust, and that the mass discrepancies we find with spatially integrated estimates are not just an effect of SED-fitting degeneracies or the lack of NIRCam coverage. Additionally, this agreement points towards the pixel-by-pixel approach as a way to mitigate the general degeneracy between the flux excess from emission lines and underlying continuum, especially when lacking photometric medium-band coverage and/or IFU observations. This study stresses the importance of studying galaxies as the complex systems that they are, resolving their stellar populations when possible, or using more flexible SFH parameterisations. This can aid our understanding of the early stages of galaxy evolution by addressing the challenge of inferring robust stellar masses and ionising photon production efficiencies of high redshift galaxies.

Galaxies: structure

Galaxies: photometry

Galaxies: high-redshift

Galaxies: star formation

Författare

C. Giménez-Arteaga

Niels Bohr Institute

Cosmic Dawn Center (DAWN)

S. Fujimoto

The University of Texas at Austin

F. Valentino

Cosmic Dawn Center (DAWN)

European Southern Observatory (ESO)

G. Brammer

Niels Bohr Institute

Cosmic Dawn Center (DAWN)

C. A. Mason

Niels Bohr Institute

Cosmic Dawn Center (DAWN)

F. Rizzo

Niels Bohr Institute

Cosmic Dawn Center (DAWN)

V. Rusakov

Cosmic Dawn Center (DAWN)

Niels Bohr Institute

L. Colina

Centro de Astrobiologia (CAB)

G. Prieto-Lyon

Niels Bohr Institute

Cosmic Dawn Center (DAWN)

Pascal A. Oesch

Cosmic Dawn Center (DAWN)

Université de Genève

Niels Bohr Institute

D. Espada

Universidad de Granada

K. E. Heintz

Niels Bohr Institute

Cosmic Dawn Center (DAWN)

Kirsten Knudsen

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik

M. Dessauges-Zavadsky

Université de Genève

N. Laporte

Laboratoire d'Astrophysique de Marseille

M. M. Lee

Danmarks Tekniske Universitet (DTU)

Cosmic Dawn Center (DAWN)

Georgios E. Magdis

Cosmic Dawn Center (DAWN)

Danmarks Tekniske Universitet (DTU)

Niels Bohr Institute

Y. Ono

University of Tokyo

Y. Ao

University of Science and Technology of China

Chinese Academy of Sciences

Masami Ouchi

National Astronomical Observatory of Japan

The Graduate University for Advanced Studies (SOKENDAI)

University of Tokyo

K. Kohno

Research Center for the Early Universe

University of Tokyo

Anton M. Koekemoer

Space Telescope Science Institute (STScI)

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 686 A63

Ämneskategorier

Astronomi, astrofysik och kosmologi

DOI

10.1051/0004-6361/202349135

Mer information

Senast uppdaterat

2024-07-03