CASTOR: the Cosmological Advanced Survey Telescope for Optical and Ultraviolet Research

Côté, Patrick; Scott, Alan; Balogh, Michael L.; Buckingham, Ron; Aldridge, David; Carlberg, R. G.; Chen, Weiguo; Dupuis, J.; Evans, Clinton; Drissen, Laurent; Fraser, Wes; Grandmont, Frédéric; Harrison, P. A.; Hutchings, J. B.; Kavelaars, J. J.; Landry, John-Thomas; Lange, Christian; Laurin, Denis; Patel, Tarun; Pillay, Venka; Piche, Louis; Rader, Andres; Robert, Carmelle; Sawicki, Marchin; Sorba, Robert; Thériault, Guillaume; Waerbeke, Ludovic Van

doi:10.1117/12.926198

Cited by 16 publications

(5 citation statements)

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“…Additionally, a notable fraction is expected to lie around M31 in the sky. These are strong predictions that might be possible to verify with upcoming wide-field deep imaging surveys, such as that planned by the LSST, if existing methods for detecting dwarfs using ground-based imaging can be improved enough to target such objects, or if planned widefield imaging surveys from space (such as that envisioned by the CASTOR mission 11 , Côte et al 2012) come to fruition.…”

Section: Mw Sats M31 Satsmentioning

confidence: 94%

The missing dwarf galaxies of the Local Group

Fattahi

Navarro

Frenk

2020

Monthly Notices of the Royal Astronomical Society

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We study the Local Group (LG) dwarf galaxy population using cosmological simulations of volumes selected to resemble the surroundings of the Milky Way (MW) and Andromeda (M31) galaxies. The simulations, from the APOSTLE project, indicate that the total mass within 3 Mpc of the pair's midpoint (M 3Mpc ) typically exceeds ∼ 3 times the sum of the virial masses of the two primaries and that the dwarf galaxy formation efficiency per unit mass is uniform throughout the volume. This suggests that MW and M31 satellites should make up fewer than one third of all LG dwarfs within 3 Mpc. This is consistent with the fraction (28 per cent) of galaxies with stellar mass M * > 10 7 M that are satellites. In addition, the total number of such galaxies (42) suggests, for the APOSTLE galaxy mass-halo mass relation, a total LG mass of M 3Mpc ∼ 10 13 M . At lower galaxy masses, however, the satellite fraction is substantially higher (42 per cent for M * > 10 5 M , or 42 out of 99). If this is due to incompleteness in the field sample, then ∼ 50 dwarf galaxies at least as massive as the Draco dwarf spheroidal are missing from our current LG field dwarf inventory. The incompleteness interpretation is supported by the pronounced flattening of the LG luminosity function below M * ∼ 10 7 M , and by the scarcity of low-surface brightness LG field galaxies: whereas ∼ 40 per cent of all M * > 10 5 M MW/M31 satellites have effective surface brightness below Σ eff = 26.5 m V /arcsec 2 , only 1 out of all field dwarfs does. The simulations indicate that most missing dwarfs should lie near the virial boundaries of the two LG primaries, and predict a trove of nearby dwarfs that await discovery by upcoming wide-field imaging surveys.

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Section: Mw Sats M31 Satsmentioning

confidence: 94%

The missing dwarf galaxies of the Local Group

Fattahi

Navarro

Frenk

2020

Monthly Notices of the Royal Astronomical Society

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“…SPace Infrared telescope for Cosmology and Astrophysics, https://spica-mission.org/ 14 https://asd.gsfc.nasa.gov/firs/ 15 CASTOR is the Cosmological Advanced Survey Telescope for Optical and ultraviolet Research proposed by the Canadian Space Agency(Côte et al 2012). This satellite could launch as early as 2027, surveying the UV with a ×30 better resolution than GALEX and a ×100 larger field of view than HST.MNRAS 000, 1-22(2019)…”

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confidence: 99%

horizon-AGN virtual observatory – 2. Template-free estimates of galaxy properties from colours

Davidzon

Laigle

Capak

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using the Horizon-AGN hydrodynamical simulation and self-organising maps (SOMs), we show how to compress the complex, high-dimensional data structure of a simulation into a 2-d grid, which greatly facilitates the analysis of how galaxy observables are connected to intrinsic properties. We first verify the tight correlation between the observed 0.3−5µm broad-band colours of Horizon-AGN galaxies and their high-resolution spectra. The correlation is found to extend to physical properties such as redshift, stellar mass, and star formation rate (SFR). This direct mapping from colour to physical parameter space is shown to work also after including photometric uncertainties that mimic the COSMOS survey. We then label the SOM grid with a simulated calibration sample, and estimate redshift and SFR for COSMOS-like galaxies up to z ∼ 3. In comparison to state-of-the-art techniques based on synthetic templates, our method is comparable in performance but less biased at estimating redshifts, and significantly better at predicting SFRs. In particular our "data-driven" approach, in contrast to model libraries, intrinsically allows for the complexity of galaxy formation and can handle sample biases. We advocate that obtaining the calibration for this method should be one of the goals of next-generation galaxy surveys.

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“…This technology is seen as a key enabler of both future large aperture space telescopes such as LUVOIR, 2 and moderate aperture survey missions such as CETUS 3 and CASTOR. 4,5 The desired performance requirements are: high quantum efficiency (>70%), large-format (>2k × 2k) detector arrays for operation at 90 to 350 nm wavelength or broader and ideally with red leak (longer wavelength) suppression. 1 Large-area silicon charge-coupled device (CCD) and complementary metal-oxidesemiconductor (CMOS) detectors for near-UV and visible wavelengths are a mature technology.…”

Section: Introductionmentioning

confidence: 99%

Quantum yield estimation for an electron-multiplying charge-coupled device from photon counting test data

Gleisinger

Rowlands

Scott

et al. 2020

J. Astron. Telesc. Instrum. Syst.

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Electron-multiplying charge-coupled devices (EMCCDs) allow for subelectron effective read noise and thus for imaging at extremely low flux levels. In the ultraviolet, quantum yield creates an additional source of stochastic gain variation, which can be difficult to quantify using existing techniques. We propose a method for measuring the quantum yield gain of these devices, independent of existing methods, using images that are part of the existing test regimen for new EMCCDs. With this method, we were able to recover the quantum yield used to create simulated images within an accuracy of ∼5% and the method provided consistent results with test images after only minor modifications. However, the measured quantum yield remains anomalously low, consistent with other measurements on Teledyne-e2v devices. We hypothesize that this discrepancy is due to lateral transfer of secondary electrons between pixels at the surface explained by the band structure and crystal geometry of typical silicon wafers used in array detector manufacture. © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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CASTOR: the Cosmological Advanced Survey Telescope for Optical and Ultraviolet Research

Cited by 16 publications

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The missing dwarf galaxies of the Local Group

The missing dwarf galaxies of the Local Group

horizon-AGN virtual observatory – 2. Template-free estimates of galaxy properties from colours

Quantum yield estimation for an electron-multiplying charge-coupled device from photon counting test data

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