Prospects for Observing Galaxy Spectral Energy Distribution from the Radio to the far-Infrared in the Era of Next-Generation Radio Telescopes

Prospects for Observing Galaxy Spectral Energy Distribution from the Radio to the far-Infrared in the Era of Next-Generation Radio Telescopes
Ilsang Yoon, Jonathan Letai, Hansung B. Gim, Eric F. Jim’enez-Andrade, Intae Jung, Caitlin Casey, Eric J. Murphy, Min S. Yun
arXiv:2605.01000v1 Announce Type: new
Abstract: The superb sensitivity and angular resolution of the next-generation radio telescopes with combined frequency coverage of approximately over three orders of magnitude (100 MHz–100 GHz) will sample the radio and far-infrared (FIR) spectral energy distribution (SED) of galaxies and revolutionize the galaxy formation study at the epoch of re-ionization and beyond. We present a prospect of observing the radio–FIR continuum SEDs of galaxies in the redshift of up to $zapprox 20$ based on an ensemble of the simulated `energy balanced’ panchromatic SED (from UV to FIR) extended to the radio. For `realistic’ populations of UV star-forming galaxies and dusty star-forming galaxies, we simulate their SEDs by accounting for the CMB effect and the radio–IR correlation. The flux density evolution of the UV-bright star-forming galaxies and the dusty star-forming galaxies at the selected observing frequencies covered by the current (ALMA) and next generation (SKA and ngVLA) radio-millimeter telescopes, suggest that massive galaxies (M$_* gtrsim 10^{10}$M$_{odot}$) are detectable at any redshift ($090$GHz). In particular, when operating, the ngVLA high-frequency ($approx 100$ GHz) band is capable of detecting galaxies with M$_* gtrsim 10^{9}$M$_{odot}$ almost independently from redshift and the SKA low-frequency observing window ($lesssim1$ GHz) has sufficient sensitivity to detect M$_* gtrsim 10^{10}$M$_{odot}$ dusty star-forming galaxies up to the epoch of reionization ($z=5sim7$). We also show that the brightness of anomalous microwave emission (AME) in the galaxy SED is insignificant if the galaxies are beyond the local Universe (e.g., $zgtrsim 0.1$).arXiv:2605.01000v1 Announce Type: new
Abstract: The superb sensitivity and angular resolution of the next-generation radio telescopes with combined frequency coverage of approximately over three orders of magnitude (100 MHz–100 GHz) will sample the radio and far-infrared (FIR) spectral energy distribution (SED) of galaxies and revolutionize the galaxy formation study at the epoch of re-ionization and beyond. We present a prospect of observing the radio–FIR continuum SEDs of galaxies in the redshift of up to $zapprox 20$ based on an ensemble of the simulated `energy balanced’ panchromatic SED (from UV to FIR) extended to the radio. For `realistic’ populations of UV star-forming galaxies and dusty star-forming galaxies, we simulate their SEDs by accounting for the CMB effect and the radio–IR correlation. The flux density evolution of the UV-bright star-forming galaxies and the dusty star-forming galaxies at the selected observing frequencies covered by the current (ALMA) and next generation (SKA and ngVLA) radio-millimeter telescopes, suggest that massive galaxies (M$_* gtrsim 10^{10}$M$_{odot}$) are detectable at any redshift ($090$GHz). In particular, when operating, the ngVLA high-frequency ($approx 100$ GHz) band is capable of detecting galaxies with M$_* gtrsim 10^{9}$M$_{odot}$ almost independently from redshift and the SKA low-frequency observing window ($lesssim1$ GHz) has sufficient sensitivity to detect M$_* gtrsim 10^{10}$M$_{odot}$ dusty star-forming galaxies up to the epoch of reionization ($z=5sim7$). We also show that the brightness of anomalous microwave emission (AME) in the galaxy SED is insignificant if the galaxies are beyond the local Universe (e.g., $zgtrsim 0.1$).