The ALPINE-CRISTAL-JWST survey: spatially resolved star formation relations at $z\sim5$

Fuente: arXiv

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Hauptverfasser:	Accard, C., Béthermin, M., Boquien, M., Buat, V., Vallini, L., Renaud, F., Kraljic, K., Aravena, M., Cassata, P., da Cunha, E., Dam, P., de Looze, I., Dessauges-Zavadsky, M., Dubois, Y., Faisst, A., Fudamoto, Y., Ginolfi, M., Gruppioni, C., Han, S., Herrera-Camus, R., Inami, H., Koekemoer, A. M., Lemaux, B. C., Li, J., Li, Y., Mobasher, B., Molina, J., Nanni, A., Palla, M., Pozzi, F., Relaño, M., Romano, M., Sawant, P., Spilker, J., Tsujita, A., Veraldi, E., Villanueva, V., Wang, W., Yi, S. K., Zamorani, G.
Format:	Preprint
Veröffentlicht:	2025
Schlagworte:	Astrophysics of Galaxies
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author	Accard, C. Béthermin, M. Boquien, M. Buat, V. Vallini, L. Renaud, F. Kraljic, K. Aravena, M. Cassata, P. da Cunha, E. Dam, P. de Looze, I. Dessauges-Zavadsky, M. Dubois, Y. Faisst, A. Fudamoto, Y. Ginolfi, M. Gruppioni, C. Han, S. Herrera-Camus, R. Inami, H. Koekemoer, A. M. Lemaux, B. C. Li, J. Li, Y. Mobasher, B. Molina, J. Nanni, A. Palla, M. Pozzi, F. Relaño, M. Romano, M. Sawant, P. Spilker, J. Tsujita, A. Veraldi, E. Villanueva, V. Wang, W. Yi, S. K. Zamorani, G.
author_facet	Accard, C. Béthermin, M. Boquien, M. Buat, V. Vallini, L. Renaud, F. Kraljic, K. Aravena, M. Cassata, P. da Cunha, E. Dam, P. de Looze, I. Dessauges-Zavadsky, M. Dubois, Y. Faisst, A. Fudamoto, Y. Ginolfi, M. Gruppioni, C. Han, S. Herrera-Camus, R. Inami, H. Koekemoer, A. M. Lemaux, B. C. Li, J. Li, Y. Mobasher, B. Molina, J. Nanni, A. Palla, M. Pozzi, F. Relaño, M. Romano, M. Sawant, P. Spilker, J. Tsujita, A. Veraldi, E. Villanueva, V. Wang, W. Yi, S. K. Zamorani, G.
contents	Star formation governs galaxy evolution, shaping stellar mass assembly and gas consumption across cosmic time. The Kennicutt-Schmidt (KS) relation, linking star formation rate (SFR) and gas surface densities, is fundamental to understand star formation regulation, yet remains poorly constrained at $z > 2$ due to observational limitations and uncertainties in locally calibrated gas tracers. The [CII] $158 {\rm μm}$ line has recently emerged as a key probe of the cold ISM and star formation in the early Universe. We investigate whether the resolved [CII]-SFR and KS relations established at low redshift remain valid at $4 < z < 6$ by analysing 13 main-sequence galaxies from the ALPINE and CRISTAL surveys, using multi-wavelength data (HST, JWST, ALMA) at $\sim2$ kpc resolution. We perform pixel-by-pixel spectral energy distribution (SED) modelling with CIGALE on resolution-homogenised images. We develop a statistical framework to fit the [CII]-SFR relation that accounts for pixel covariance and compare our results to classical fitting methods. We test two [CII]-to-gas conversion prescriptions to assess their impact on inferred gas surface densities and depletion times. We find a resolved [CII]-SFR relation with a slope of $0.87 \pm 0.15$ and intrinsic scatter of $0.19 \pm 0.03$ dex, which is shallower and tighter than previous studies at $z\sim5$. The resolved KS relation is highly sensitive to the [CII]-to-gas conversion factor: using a fixed global $α_{\rm [CII]}$ yields depletion times of $0.5$-$1$ Gyr, while a surface brightness-dependent $W_{\rm [CII]}$, places some galaxies with high gas density in the starburst regime ($<0.1$ Gyr). Future inputs from both simulations and observations are required to better understand how the [CII]-to-gas conversion factor depends on local ISM properties. We need to break this fundamental limit to properly study the KS relation at $z\gtrsim4$.
format	Preprint
id	arxiv_https___arxiv_org_abs_2508_13136
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	The ALPINE-CRISTAL-JWST survey: spatially resolved star formation relations at $z\sim5$ Accard, C. Béthermin, M. Boquien, M. Buat, V. Vallini, L. Renaud, F. Kraljic, K. Aravena, M. Cassata, P. da Cunha, E. Dam, P. de Looze, I. Dessauges-Zavadsky, M. Dubois, Y. Faisst, A. Fudamoto, Y. Ginolfi, M. Gruppioni, C. Han, S. Herrera-Camus, R. Inami, H. Koekemoer, A. M. Lemaux, B. C. Li, J. Li, Y. Mobasher, B. Molina, J. Nanni, A. Palla, M. Pozzi, F. Relaño, M. Romano, M. Sawant, P. Spilker, J. Tsujita, A. Veraldi, E. Villanueva, V. Wang, W. Yi, S. K. Zamorani, G. Astrophysics of Galaxies Star formation governs galaxy evolution, shaping stellar mass assembly and gas consumption across cosmic time. The Kennicutt-Schmidt (KS) relation, linking star formation rate (SFR) and gas surface densities, is fundamental to understand star formation regulation, yet remains poorly constrained at $z > 2$ due to observational limitations and uncertainties in locally calibrated gas tracers. The [CII] $158 {\rm μm}$ line has recently emerged as a key probe of the cold ISM and star formation in the early Universe. We investigate whether the resolved [CII]-SFR and KS relations established at low redshift remain valid at $4 < z < 6$ by analysing 13 main-sequence galaxies from the ALPINE and CRISTAL surveys, using multi-wavelength data (HST, JWST, ALMA) at $\sim2$ kpc resolution. We perform pixel-by-pixel spectral energy distribution (SED) modelling with CIGALE on resolution-homogenised images. We develop a statistical framework to fit the [CII]-SFR relation that accounts for pixel covariance and compare our results to classical fitting methods. We test two [CII]-to-gas conversion prescriptions to assess their impact on inferred gas surface densities and depletion times. We find a resolved [CII]-SFR relation with a slope of $0.87 \pm 0.15$ and intrinsic scatter of $0.19 \pm 0.03$ dex, which is shallower and tighter than previous studies at $z\sim5$. The resolved KS relation is highly sensitive to the [CII]-to-gas conversion factor: using a fixed global $α_{\rm [CII]}$ yields depletion times of $0.5$-$1$ Gyr, while a surface brightness-dependent $W_{\rm [CII]}$, places some galaxies with high gas density in the starburst regime ($<0.1$ Gyr). Future inputs from both simulations and observations are required to better understand how the [CII]-to-gas conversion factor depends on local ISM properties. We need to break this fundamental limit to properly study the KS relation at $z\gtrsim4$.
title	The ALPINE-CRISTAL-JWST survey: spatially resolved star formation relations at $z\sim5$
topic	Astrophysics of Galaxies
url	https://arxiv.org/abs/2508.13136