The ALMA-CRISTAL survey: Dust temperature and physical conditions of the interstellar medium in a typical galaxy at <i>z</i> = 5.66

We present new λ rest = 77 μm dust continuum observations from the Atacama Large Millimeter/submillimeter Array of HZ10 (CRISTAL-22). This dusty main sequence galaxy at z = 5.66 was observed as part of the [CII] Resolved Ism in STar-forming Alma Large program (CRISTAL). The high angular resolution of the ALMA Band 7 and new Band 9 data (∼0′′​​.4) reveals the complex structure of HZ10, which comprises two main components (HZ10-C and HZ10-W), along with a bridge-like dusty emission between them (i.e., “the bridge”). Using a modified blackbody function to model the dust spectral energy distribution (SED), we constrained the physical conditions of the interstellar medium (ISM) and its variations among the different components identified in HZ10. We find that HZ10-W (the more UV-obscured component) has an SED dust temperature of T SED ∼ 51.2 ± 13.1 K; this was found to be ∼5 K higher (which is statistically insignificant; i.e., less than 1 σ ) than that of the central component and previous global estimations for HZ10. Our new ALMA data allow us to reduce the uncertainties of global T SED measurements by a factor of ∼2.3, compared to previous studies. The HZ10 components have [CII]-to-far-infrared (FIR) luminosity ratios and FIR surface densities values that are consistent with local starburst galaxies. However, HZ10-W shows a lower [CII]/FIR ratio compared to the other two components (albeit still within the uncertainties), which may suggest a harder radiation field destroying polycyclic aromatic hydrocarbon associated with [CII] emission (e.g., active galactic nuclei or young stellar populations). While HZ10-C appears to follow the tight IRX- β UV relation seen in local UV-selected starburst galaxies and high- z star-forming galaxies, we find that both HZ10-W and the bridge depart from this relation and are well described by dust-screen models with holes in front of a hard UV radiation field. This suggests that the UV emission, which is likely coming from young stellar populations, is strongly attenuated in the “dustier” components of the HZ10 system.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2024-09-30
DOI
https://doi.org/10.1051/0004-6361/202451490
Citations
11
Primary Topic
Astronomy and Astrophysical Research
Type
article
Field-Weighted Citation Impact
5.57

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article

The ALMA-CRISTAL survey: Dust temperature and physical conditions of the interstellar medium in a typical galaxy at z = 5.66

M. Relano, I. De Looze, S. Bovino, Thorsten Naab et al.
11 citations
Astronomy and Astrophysics
Astronomy and Astrophysical Research
5.57
article

The ALMA-CRISTAL survey: Dust temperature and physical conditions of the interstellar medium in a typical galaxy at z = 5.66

M. Relano, I. De Looze, S. Bovino, Thorsten Naab, R.A. Bowler, A. Posses, Roberto J. Assef, Ken-ichi Tadaki, Marco Palla, M. Solimano, Vicente Villanueva, Hiddo S. B. Algera, Rodrigo Herrera-Camus, Ikki Mitsuhashi, K. Telikova, J. Gonzalez-Lopez, A. Ferrara, Hannah Übler, Justin Spilker, Meghana Killi, Ryota Ikeda, Elisabete da Cunha, Manuel Aravena, Sedona H. Price, T. Díaz-Santos, N. M. Förster Schreiber, M. Baeza-Garay, Loreto Barcos-Muñoz
article en
11 citations

Abstract

We present new λ rest = 77 μm dust continuum observations from the Atacama Large Millimeter/submillimeter Array of HZ10 (CRISTAL-22). This dusty main sequence galaxy at z = 5.66 was observed as part of the [CII] Resolved Ism in STar-forming Alma Large program (CRISTAL). The high angular resolution of the ALMA Band 7 and new Band 9 data (∼0′′​​.4) reveals the complex structure of HZ10, which comprises two main components (HZ10-C and HZ10-W), along with a bridge-like dusty emission between them (i.e., “the bridge”). Using a modified blackbody function to model the dust spectral energy distribution (SED), we constrained the physical conditions of the interstellar medium (ISM) and its variations among the different components identified in HZ10. We find that HZ10-W (the more UV-obscured component) has an SED dust temperature of T SED ∼ 51.2 ± 13.1 K; this was found to be ∼5 K higher (which is statistically insignificant; i.e., less than 1 σ ) than that of the central component and previous global estimations for HZ10. Our new ALMA data allow us to reduce the uncertainties of global T SED measurements by a factor of ∼2.3, compared to previous studies. The HZ10 components have [CII]-to-far-infrared (FIR) luminosity ratios and FIR surface densities values that are consistent with local starburst galaxies. However, HZ10-W shows a lower [CII]/FIR ratio compared to the other two components (albeit still within the uncertainties), which may suggest a harder radiation field destroying polycyclic aromatic hydrocarbon associated with [CII] emission (e.g., active galactic nuclei or young stellar populations). While HZ10-C appears to follow the tight IRX- β UV relation seen in local UV-selected starburst galaxies and high- z star-forming galaxies, we find that both HZ10-W and the bridge depart from this relation and are well described by dust-screen models with holes in front of a hard UV radiation field. This suggests that the UV emission, which is likely coming from young stellar populations, is strongly attenuated in the “dustier” components of the HZ10 system.

Astronomy and AstrophysicsVol. 691
Hiroshima University (JP), Bunkyo University (JP), Scuola Normale Superiore (IT), Pontificia Universidad Católica de Chile (CL), University of Pittsburgh (US), University of Concepción (CL), Universidad de Granada (ES), Carnegie Institution for Science (US), The Graduate University for Advanced Studies, SOKENDAI (JP), European University Cyprus (CY), University of Cambridge (GB), National Radio Astronomy Observatory (US), Mitchell Institute (US), University of Manchester (GB), Ghent University (BE), Max Planck Institute for Extraterrestrial Physics (DE), Max Planck Institute for Astrophysics (DE), Istituto di Radioastronomia di Bologna (IT), Carnegie Observatories (US), Las Campanas Observatory (CL), National Astronomical Observatory of Japan (JP), International Centre for Radio Astronomy Research (AU), Osservatorio di Astrofisica e Scienza dello Spazio, University College London (GB), The University of Tokyo (JP), Sapienza University of Rome (IT), Foundation for Research and Technology Hellas (GR), Universidad Diego Portales (CL), Hokkai Gakuen University (JP), University of Bologna (IT)
National Science Foundation, National Aeronautics and Space Administration, Space Telescope Science Institute, European Commission, Max-Planck-Gesellschaft, Universidad de Concepción, Agencia Nacional de Investigación y Desarrollo, HORIZON EUROPE Framework Programme, Science and Technology Facilities Council, Japan Society for the Promotion of Science, Agencia Estatal de Investigación
Openalex Percentile: Top 4%
Astronomy and Astrophysical Research
5.57
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