The astrophysical agenda of the 21st century requires a very sharp view of celestial objects. High angular resolution studies are essential for fundamental studies of a broad variety of astrophysical phenomena ranging from relativistic physics of black holes, their gravitational and electromagnetic imprints, violent transient processes, including those producing detectable gravitational waves, birth and evolution of planetary systems. Over the past decades, radio astronomy made huge leap in achieving ground-breaking angular resolution measured in tens of microarcseconds (one tenth of nanoradian and better). Recently a global Event Horizon Telescope (EHT) collaboration obtained first direct images of the shadow of a super-massive black hole in the nucleus of the active galaxy M87. These observations were conducted at 230 GHz. The two first generation Space Very Long Baseline Interferometry (VLBI) missions, VSOP/HALCA led by the Japan Aerospace Exploration Agency (JAXA) and RadioAstron led by the Russia Roscosmos State Corporation and Russia Academy of Sciences, achieved the highest angular resolution at frequencies from 0.3 to 22 GHz in observations conducted in the period 1997 - 2019. The next step in advancing high angular resolution radio astronomy is in combining high frequency (millimeter and sub-millimeter wavelengths) and interferometric baselines exceeding the Earth diameter. The present THEZA White Paper describes a combination which would unify technology developments in giga-/tera-hertz instrumentation and space-borne radio astronomy. The current preprint version of the THEZA White Paper is slightly re-formatted and edited comparing to the official submitted version.

/pdf/terahertz-exploration-and-zooming-in-for-astrophysics-theza-4ovtul0d84.pdf

TeraHertz Exploration and Zooming-in for Astrophysics (THEZA): ESA Voyage 2050 White Paper

Line intensity mapping (LIM) is rapidly emerging as a powerful technique to study galaxy formation and cosmology in the high-redshift Universe. We present LIM estimates of select spectral lines originating from the interstellar medium (ISM) of galaxies and 21 cm emission from neutral hydrogen gas in the Universe using the large volume, high resolution THESAN reionization simulations. A combination of sub-resolution photo-ionization modelling for HII regions and Monte Carlo radiative transfer calculations is employed to estimate the dust-attenuated spectral energy distributions (SEDs) of high-redshift galaxies ($z\gtrsim5.5$). We show that the derived photometric properties such as the ultraviolet (UV) luminosity function and the UV continuum slopes match observationally inferred values, demonstrating the accuracy of the SED modelling. We provide fits to the luminosity--star formation rate relation (L-SFR) for the brightest emission lines and find that important differences exist between the derived scaling relations and the widely used low-$z$ ones because the interstellar medium of reionization era galaxies is generally less metal-enriched than in their low redshift counterparts. We use these relations to construct line intensity maps of nebular emission lines and cross correlate with the 21 cm emission. Interestingly, the wavenumber at which the correlation switches sign ($k_\mathrm{transition}$) depends heavily on the reionization model and to a lesser extent on the targeted emission line, which is consistent with the picture that $k_\mathrm{transition}$ probes the typical sizes of ionized regions. The derived scaling relations and intensity maps represent a timely state-of-the-art framework for forecasting and interpreting results from current and upcoming LIM experiments.

The THESAN project: predictions for multi-tracer line intensity mapping in the Epoch of Reionization

ABSTRACT Line intensity mapping (LIM) is rapidly emerging as a powerful technique to study galaxy formation and cosmology in the high-redshift Universe. We present LIM estimates of select spectral lines originating from the interstellar medium (ISM) of galaxies and 21 cm emission from neutral hydrogen gas in the Universe using the large volume, high resolution thesan reionization simulations. A combination of subresolution photoionization modelling for H ii regions and Monte Carlo radiative transfer calculations is employed to estimate the dust-attenuated spectral energy distributions (SEDs) of high-redshift galaxies (z ≳ 5.5). We show that the derived photometric properties such as the ultraviolet (UV) luminosity function and the UV continuum slopes match observationally inferred values, demonstrating the accuracy of the SED modelling. We provide fits to the luminosity–star formation rate relation (L–SFR) for the brightest emission lines and find that important differences exist between the derived scaling relations and the widely used low-z ones because the ISM of reionization era galaxies is generally less metal enriched than in their low-redshift counterparts. We use these relations to construct line intensity maps of nebular emission lines and cross-correlate with the 21 cm emission. Interestingly, the wavenumber at which the correlation switches sign (ktransition) depends heavily on the reionization model and to a lesser extent on the targeted emission line, which is consistent with the picture that ktransition probes the typical sizes of ionized regions. The derived scaling relations and intensity maps represent a timely state-of-the-art framework for forecasting and interpreting results from current and upcoming LIM experiments. 

https://authors.library.caltech.edu/116009/1/stac1557.pdf

The <scp>thesan</scp> project: predictions for multitracer line intensity mapping in the epoch of reionization

The Origins Space Telescope (Origins) is one of four science and technology definition studies selected by National Aeronautics and Space Administration (NASA) in preparation of the 2020 Astronomy and Astrophysics Decadal survey in the US. Origins will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. It is designed to answer three major science questions: How do galaxies form stars, make metals, and grow their central supermassive black holes from reionization? How do the conditions for habitability develop during the process of planet formation? Do planets orbiting M-dwarf stars support life? Origins operates at mid- to far-infrared wavelengths from ~2.8 to 588 {\mu}m, is more than 1000 times more sensitive than prior far-IR missions due to its cold (~4.5 K) aperture and state-of-the-art instruments.

Origins Space Telescope: From First Light to Life -- ESA Voyage 2050 White Paper

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Origins Space Telescope: From First Light to Life -- ESA Voyage 2050 White Paper