The TAOS II Survey: Real-time Detection and Characterization of Occultation Events

Huang, Chung Kai; Lehner, M. J.; Contreras, Agueda Paula Granados; Castro-Chacón, J. H.; Chen, Wen-Ping; Alcock, Charles; Álvarez-Santana, F. I.; Cook, K. H.; Geary, John C.; Peña, Carlos Alberto Guerrero; Hernández-Águila, J. B.; Hernández-Valencia, B.; Karr, J.; Kavelaars, J. J.; Norton, Timothy; Núñez, Juan; Ochoa, Diego A.; Reyes-Ruiz, M.; Sánchez, E.; Silva, José Sergio; Szentgyorgyi, Andrew; Wang, Shiang‐Yu; Yen, Wei-Ling; Zhang, Zhi Wei

doi:10.1088/1538-3873/abd4bc

Cited by 8 publications

(8 citation statements)

References 52 publications

(53 reference statements)

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“…One of the best next steps is to send orbiters to the Uranus (Cartwright et al 2021;Leonard et al 2021) and Neptune systems 6 to complete crater measurements to much smaller diameters and deepen understanding of the satellites' geologies. It is also important to perform occultation surveys of KBOs, including bodies with diameters <1 km (Huang et al 2021), as escaped KBOs are the expected main source of the heliocentric population of satellite impactors. However, even this may not completely resolve what has impacted outer solar system satellites, as this will only provide a snapshot of the current (0 to ∼3 Ga) heliocentric impactor population and not show what this or the other possible populations may have looked like in the very early solar system (see Morbidelli & Nesvorný 2020, for a review of dynamical and collisional evolution of the Kuiper Belt).…”

Section: Implications For Outer Solar System Impactormentioning

confidence: 99%

Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment

Kirchoff¹,

Dones²,

Singer³

et al. 2022

Planet. Sci. J.

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Outer solar system impact bombardment is largely unconstrained. Although recent data from the Jupiter, Saturn, and Pluto systems have produced new constraints, analysis is incomplete without inclusion of the Uranus system. We reanalyze Uranus system crater populations with recent improvements in processing of Voyager 2 imaging. No consensus in crater populations on mid-sized Uranian satellites, Miranda, Ariel, Umbriel, Titania, and Oberon, was resolved during the Voyager era. For satellites with available data, we find variability in crater size–frequency distributions (SFDs) for diameters (D) < 10 km. Most terrains on Miranda show a shallower slope (ratio of smaller to larger craters is smaller), while Inverness Corona on Miranda and Ariel's terrains show a steeper slope (ratio increases). For D > 10 km, satellites with available data show a steeper slope. Shallower-sloped SFDs for D < 10 km and steeper slopes for D > 10 km agree with Pluto system data—a proxy for the heliocentric impactor population originating from the Kuiper Belt—implying these SFDs represent heliocentric bombardment in the Uranus system. The shallow-sloped population for smaller diameters is also observed on Jovian satellites, but not on mid-sized, heavily cratered Saturnian satellites or Triton (Neptune), which have steeper slopes. This implies the heliocentric impactor population originating from the Kuiper Belt reaches throughout the outer solar system, but that the Saturnian, Neptunian, and maybe Uranian systems also might have their own planet-specific impactors. Finally, we find Ariel appears overall younger than the other Uranian satellites, supporting relatively recent geologic activity.

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Section: Implications For Outer Solar System Impactormentioning

confidence: 99%

Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment

Kirchoff¹,

Dones²,

Singer³

et al. 2022

Planet. Sci. J.

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show abstract

“…Nevertheless, the last decade has seen increased availability of QE-boosting technologies such as backside illumination (BSI) in CIS, improvements in the performance and arrangement of column-parallel ADCs allowing larger area and threesided buttable sensors. Specific applications are already making use of the advantages of CIS, such as the ability to address subsets of individual pixels as in the TAOS-II project (Huang et al 2021), which uses the Teledyne CIS113 (Wang et al 2020) with deported ADCs. Another useful characteristic of CIS is the achievement of high frame rates coupled with low readout noise ( 1 e − ) thanks to highly parallel readout.…”

Section: Introductionmentioning

confidence: 99%

StarDICE

Betoule

Antier

Bertin³

et al. 2023

A&A

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Context. The Hubble diagram of type-Ia supernovae (SNe-Ia) provides cosmological constraints on the nature of dark energy with an accuracy limited by the flux calibration of currently available spectrophotometric standards. This motivates new developments to improve the link between existing astrophysical flux standards and laboratory standards. Aims. The StarDICE experiment aims to establish a five-stage metrology chain from NIST photodiodes to stars, with a targeted accuracy of 1 mmag in griz colors. We present the first two stages, resulting in the calibration transfer from NIST photodiodes to a demonstration 150 Mpixel CMOS sensor (Sony IMX411ALR as implemented in the QHY411M camera by QHYCCD). As a sideproduct, we provide full characterization of this camera, which we believe to be of potential interest in astronomical imaging and photometry and specifically discuss its use in the context of gravitational wave optical follow-up. Methods. A fully automated spectrophotometric bench was built to perform the calibration transfer. The sensor readout electronics was studied using thousands of flat-field images from which we derived stability, high-resolution photon transfer curves, and estimates of the individual pixel gain. The sensor quantum efficiency was then measured relatively to a NIST-calibrated photodiode, in a welldefined monochromatic light beam from 375 to 1078 nm. Last, flat-field scans at 16 different wavelengths were used to build maps of the sensor response, fully characterizing the sensor for absolute photometric measurements. Results. We demonstrated statistical uncertainty on quantum efficiency below 0.001 e − /γ between 387 nm and 950 nm, the range being limited by the sensitivity decline of the tested sensor in the infrared. Systematic uncertainties in the bench optics are controlled at the level of 1 × 10 −3 e − /γ. Linearity issues are detected at the level of 5 × 10 −3 e − /γ for the tested camera and require further developments to fully correct. Uncertainty in the overall normalization of the quantum efficiency curve (without relevance for the cosmology, but relevant to evaluate the performance of the camera itself) is 1%. Regarding the camera we demonstrate stability in steady state conditions at the level of 32.5 ppm. Homogeneity in the response is below 1 % RMS across the entire sensor area. Quantum efficiency stays above 50 % in most of the visible range, peaking well above 80 % between 440 nm and 570 nm. Differential nonlinearities at the level of 1 % are detected. A simple two-parameter model is proposed to mitigate the effect and found to adequately correct the shape of the PTC on half the numerical scale. No significant deviations from integral linearity were detected in our limited test. Static and dynamical correlations between pixels are low, making the device likely suitable for galaxy shape measurements.

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“…Nevertheless, the last decade has seen increased availability of QE-boosting technologies such as backside illumination (BSI) in CIS, improvements in the performance and arrangement of column-parallel ADCs allowing larger area and 3-side buttable sensors. Specific applications are already making use of the advantages of CIS such as the ability to address subsets of individual pixels as in the TAOS-II project (Huang et al 2021), which uses the Teledyne CIS113 (Wang et al 2020) with deported ADCs. Another useful characteristic of CIS is the achievement of high frame rates coupled with low readout noise ( 1 e − ), thanks to highly parallel readout.…”

Section: Introductionmentioning

confidence: 99%

StarDICE I: sensor calibration bench and absolute photometric calibration of a Sony IMX411 sensor

Betoule¹,

Antier²,

Bertin³

et al. 2022

Preprint

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Context. The Hubble diagram of type-Ia supernovae (SNe-Ia) provides cosmological constraints on the nature of dark energy with an accuracy limited by the flux calibration of currently available spectrophotometric standards. This motivates new developments to improve the link between existing astrophysical flux standards and laboratory standards. Aims. The StarDICE experiment aims at establishing a 5-stage metrology chain from NIST photodiodes to stars, with a targeted accuracy of 1 mmag in griz colors. We present the first two stages, resulting in the calibration transfer from NIST photodiodes to a demonstration 150 Mpixel CMOS sensor (Sony IMX411ALR as implemented in the QHY411M camera by QHYCCD). As a sideproduct, we provide full characterization of this camera which we believe of potential interest in astronomical imaging and photometry and specifically discuss its use in the context of gravitational wave optical follow-up. Methods. A fully automated spectrophotometric bench is built to perform the calibration transfer. The sensor readout electronics is studied using thousands of flat-field images from which we derive stability, high resolution photon transfer curves and estimates of the individual pixel gain. The sensor quantum efficiency is then measured relative to a NIST-calibrated photodiode, in a well defined monochromatic light-beam from 375 to 1078 nm. Last, flat-field scans at 16 different wavelengths are used to build maps of the sensor response, fully characterizing the sensor for absolute photometric measurements. Results. We demonstrate statistical uncertainty on quantum efficiency below 0.001 e − /γ between 387 nm and 950 nm, the range being limited by the sensitivity decline of the tested sensor in the infrared. Systematic uncertainties in the bench optics are controlled at the level of 1 × 10 −3 e − /γ. Linearity issues are detected at the level of 5 × 10 −3 e − /γ for the tested camera and require further developments to fully correct. Uncertainty in the overall normalization of the QE curve (without relevance for the cosmology, but relevant to evaluate the performance of the camera itself) is 1%. Regarding the camera we demonstrate stability in steady state conditions at the level of 32.5 ppm. Homogeneity in the response is below 1 % RMS across the entire sensor area. Quantum efficiency stays above 50 % in most of the visible range, peaking well above 80 % between 440 nm and 570 nm. Differential non-linearities at the level of 1 % are detected. A simple 2-parameter model is proposed to mitigate the effect and found to adequately correct the shape of the PTC on half the numerical scale. No significant deviations from integral linearity were detected in our limited test. Static and dynamical correlations between pixels are low, making the device likely suitable for galaxy shape measurements.

show abstract

The TAOS II Survey: Real-time Detection and Characterization of Occultation Events

Cited by 8 publications

References 52 publications

Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment

Crater Distributions of Uranus's Mid-sized Satellites and Implications for Outer Solar System Bombardment

StarDICE

StarDICE I: sensor calibration bench and absolute photometric calibration of a Sony IMX411 sensor

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