Manuel Aravena

Several wide-scale surveys are being planned and ongoing with various telescopes from the optical to centimeter bands. These include the Rubin Observatory, The Roman Space Telescope, Euclid, ASKAP, SKA, etc. Among these, the Fred Young Submillimeter Telescope (formerly CCAT-p), with its Prime-Cam instrument, will enable wide-field and very deep mapping from 100 to 900 GHz (3 to 0.3 mm wavelength). This spectral regime has been explored through a variety of surveys, including those using ground-based telescopes (e.g. CSO, JCMT, APEX, SPT and ACT) and space telescopes (e.g. Planck and Herschel) with many striking discoveries. FYST and its associated instrumentation will move beyond these surveys in terms of confusion limited depth, areal coverage, and/or frequency coverage, enabling new science. The main surveys conducted with FYST will enable us to tackle several areas, including (a) Epoch of Reionization, (b) Galaxy evolution through cosmic time, (c) Measurements of CMB backgrounds, (d) Galaxy cluster evolution, etc. A major challenge is coordinating efforts in the submm and other wavelengths, finding optical counterparts (LSST) to the submm-detected DSFGs (350um) sources. This will enable the characterization of these objects and searches for distant objects (z>5) and IR bright protocluster fields.

I have been involved in the FYST project (currently as "co-lead" of the galaxy evolution efforts) and expect the planned surveys will open a large variety of scientific projects to identify and characterize the large number of star-forming galaxies detected with FYST.

For more info, check:

https://ui.adsabs.harvard.edu/abs/2021arXiv210710364C/abstract

https://ui.adsabs.harvard.edu/abs/2018SPIE10700E..1MS/abstract

https://www.ccatobservatory.org/

ASPECS represents one of the first systematic efforts to conduct a 3-dimensional mapping of the best studied cosmological deep field: the Hubble Ultra Deep Field (HUDF). ASPECS constitutes a molecular deep field obtained by scanning the full ALMA bands 3 and 6 (3-mm and 1-mm bands, respectively) over a significant area of this field. Thereby, blind searches for molecular line (CO/CII) and dust continuum emission can be done. We performed a pilot project by imaging a 1 arcmin^2 region, resulting in 7 high-impact peer-reviewed publications. We were awarded an ALMA large program (the 1st extragalactic large program) to expand our pilot project to an area 5x larger, effectively covering what has been called the "eXtremely Deep Field" (XDF). ASPECS has had a critical legacy value given upcoming efforts with JWST, etc. We are working on similar efforts in other deep fields like the COLDz project. M. Aravena has co-lead the ASPECS project together with F. Walter (MPIA), C. Carilli (NRAO) and R. Decarli (INAF/Bologna).

For more info and visuals, go to: http://www.aspecs.info

As a follow-up to this large program, we are pursuing deep observations at 870-microns with ALMA in this field (40-hrs campaign), which will be critical for studies of the faint sources and complementarity to JWST GTO programs.

CRISTAL is a recently approved Cycle 8 ALMA Large Program that will spatially resolve the [CII] 158 μm line and dust continuum emission in 19 mass-selected star-forming galaxies at z ∼ 4–5. All targets have HST rest-frame UV data, and more than half of them will have Cycle 1 JWST rest-frame optical observations. With the combination of ALMA, HST, and JWST, CRISTAL will produce the first systematic census of gas, dust, and stars on ∼1–2 kpc scales in typical star-forming galaxies when the Universe was only ∼1 Gyr old. This will allow us to connect the properties of the interstellar medium (ISM), circumgalactic medium (CGM), star formation, and feedback in the form of outflows. The CRISTAL program will be led from Chile by R. Herrera-Camus (PI, UdeC), M. Aravena (co-PI, UDP), J. González-López (co-PI, Las Campanas Observatory), together with a team of ~40 scientists from around the world, including co-PIs N. Forster-Schreiber (MPE, Germany), I. De Looze (Ghent U., Belgium), J. Spilker (U. Texas A&M, USA), and K. Tadaki (SOKENDAI, Japan).

For more information, go to: www.alma-cristal.info

At UDP, and in direct collaboration with Dr. J. González-López, we are conducting studies of individual galaxies with the [CII] line at high-resolution (Posses et al. 2022; Lambert et al. 2022, submitted) as pilot studies for CRISTAL, and are pursuing studies of the connection between the ISM and CGM through observations of the Lyman-a 1216A line using MUSE and other IFU optical instruments. Additionally, we are pursuing low-J CO observations with the VLA to measure the total molecular gas content.