ATLAS probe: Breakthrough science of galaxy evolution, cosmology, Milky Way, and the Solar System

Abstract

Astrophysics Telescope for Large Area Spectroscopy Probe is a concept for a National Aeronautics and Space Administration probe-class space mission that will achieve ground-breaking science in the fields of galaxy evolution, cosmology, Milky Way, and the Solar System. It is the follow-up space mission to Wide Field Infrared Survey Telescope (WFIRST), boosting its scientific return by obtaining deep 1–4 μm slit spectroscopy for ∼70% of all galaxies imaged by the ∼2 000 deg2WFIRST High Latitude Survey atz> 0.5. Astrophysics Telescope for Large Area Spectroscopy will measure accurate and precise redshifts for ∼200 M galaxies out toz< 7, and deliver spectra that enable a wide range of diagnostic studies of the physical properties of galaxies over most of cosmic history. Astrophysics Telescope for Large Area Spectroscopy Probe and WFIRST together will produce a 3D map of the Universe over 2 000 deg2, the definitive data sets for studying galaxy evolution, probing dark matter, dark energy and modifications of General Relativity, and quantifying the 3D structure and stellar content of the Milky Way. Astrophysics Telescope for Large Area Spectroscopy Probe science spans four broad categories: (1) Revolutionising galaxy evolution studies by tracing the relation between galaxies and dark matter from galaxy groups to cosmic voids and filaments, from the epoch of reionisation through the peak era of galaxy assembly; (2) Opening a new window into the dark Universe by weighing the dark matter filaments using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of General Relativity using galaxy clustering; (3) Probing the Milky Way’s dust-enshrouded regions, reaching the far side of our Galaxy; and (4) Exploring the formation history of the outer Solar System by characterising Kuiper Belt Objects. Astrophysics Telescope for Large Area Spectroscopy Probe is a 1.5 m telescope with a field of view of 0.4 deg2, and uses digital micro-mirror devices as slit selectors. It has a spectroscopic resolution ofR= 1 000, and a wavelength range of 1–4 μm. The lack of slit spectroscopy from space over a wide field of view is the obvious gap in current and planned future space missions; Astrophysics Telescope for Large Area Spectroscopy fills this big gap with an unprecedented spectroscopic capability based on digital micro-mirror devices (with an estimated spectroscopic multiplex factor greater than 5 000). Astrophysics Telescope for Large Area Spectroscopy is designed to fit within the National Aeronautics and Space Administration probe-class space mission cost envelope; it has a single instrument, a telescope aperture that allows for a lighter launch vehicle, and mature technology (we have identified a path for digital micro-mirror devices to reach Technology Readiness Level 6 within 2 yr). Astrophysics Telescope for Large Area Spectroscopy Probe will lead to transformative science over the entire range of astrophysics: from galaxy evolution to the dark Universe, from Solar System objects to the dusty regions of the Milky Way.

How dark are filaments in the cosmic web?

“…At face value, the observed mass of the filament appears to decrease with the increasing of redshift, although the difference is not statistically significant. Theoretically, the scaling of the filament mass with redshift can be predicted from evolution of the three-point correlation function which depends on the bispectrum whose evolution should scale like square of the linear growth factor (Clampitt et al 2016;Epps & Hudson 2017;Wang et al 2019). The redshift scaling is shown in Figure 2, after fixing the normalization to agree with the mean filament mass at the mean filament redshift.…”

“…The advent of other surveys could do help to provide more accurate and precise measurements. such as Euclid (Laureijs et al 2011) and WFIRST (Spergel et al 2015) will improve the weak lensing measurements by orders of magnitude while proposed spectroscopic missions such as ATLAS probe (Wang et al 2019) could map the cosmic web at high resolution. With the increase in the accuracy and completeness of different surveys, we hope to provide more reliable and complete measurements of the cosmic web.…”

Artificial Intelligence-Aided Massively Parallel Spectroscopy of Freely Diffusing Nanoscale Entities

“…A similar optical setting is quite common in astronomy when the spectra of stars are studied . The use of a prism as a dispersing element was proven more effective than using a diffraction grating. , In contrast to light dispersion, the mask of optical filters, such as red-green-blue pixels, can also provide rudimental spectra information. However, the mask reduces the attainable signal by absorbing the photons and cannot be easily replaced for the wavelengths of interest.…”

“…For the first time, we introduce massively parallel spectroscopy (MPS) with a significantly larger detection volume to circumvent the limitations of cross-correlation spectroscopy. MPS, also known as slitless spectroscopy, is commonly used in astronomy for the spectroscopy of stars and other cosmic objects. , In its simplest setting, a dispersive element such as a prism or a diffraction grating is placed in front of the camera. Then, numerous spectra of stars are projected onto the camera sensor.…”

Cosmologia no cone de luz: o espectro angular no espaço de redshift, o espectro de potencia no espaço de Fourier e mocks do cone de luz

“…Figura 8: Comparativo entre as estimativas espectrográficas e fotométricas: a figura faz parte de uma simulac ¸ão semi-analítica para a distribuic ¸ão de galáxias emissoras de Lyman-alpha, denominada GALFORM [32], realizada nesta região especialmente para mostrar o poder de mapeamento de um próximo levantamento denominado ATLAS [33]. O erro esperado para a determinac ¸ão do redshift espectrográfico é σ z = 10 −4 (1 + z), enquanto que o erro associado às medidas fotométricas é, num cenário otimista, σ z = 10 −2 (1 + z).…”