Probability Distributions.- Linear Models for Regression.- Linear Models for Classification.- Neural Networks.- Kernel Methods.- Sparse Kernel Machines.- Graphical Models.- Mixture Models and EM.- Approximate Inference.- Sampling Methods.- Continuous Latent Variables.- Sequential Data.- Combining Models.

Pattern Recognition and Machine Learning

Context. We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. Aims: A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey. Recommendations are made on the responsible use of Gaia DR2 results. Methods: The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products. Results: Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the GBP (330-680 nm) and GRP (630-1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14 000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent. Conclusions: Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy.

/pdf/gaia-data-release-2-summary-of-the-contents-and-survey-539viwt72y.pdf

Gaia Data Release 2. Summary of the contents and survey properties

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ at a luminosity distance of $40^{+8}_{-8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Msun. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim$40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over $\sim$10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim$9 and $\sim$16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. (Abridged)

Multi-messenger Observations of a Binary Neutron Star Merger

This paper describes the ATLAS experiment as installed in i ts experimental cavern at point 1 at CERN. It also presents a brief overview of the expec ted performance of the detector.

http://absimage.aps.org/image/SES08/MWS_SES08-2008-020010.pdf

The ATLAS Experiment at the CERN Large Hadron Collider

基礎講座 電気泳動(Electrophoresis)

A reconfigurable Single-Photon Avalanche Diode integration mode receiver in 130nm CMOS is presented for optical links with an array readout bandwidth of 100MHz. The all-digital 32×32 SPAD array achieves a minimum dead time of 5.9ns, and a median dark count rate of 2.5kHz per SPAD. Pulse shortening increases the dynamic range by preventing pulse overlap. An in-pixel feedback loop allows synchronous or self-clocked asynchronous time division multiplexing. The internal gain of SPADs and spatio-temporal summation removes the need for analogue amplification. A maximum count rate of 58GHz is observed, with SNR of 79dB, a sensitivity of −31.7dBm at 100MHz and a BER of 10−9. The sensor core draws 89mW at maximum count rate.

A reconfigurable 14-bit 60GPhoton/s Single-Photon receiver for visible light communications

A solid state image sensor has an array of pixels in which each column has a reset voltage line and a read line. The sensor is reset and read a row at a time, with reset-related values held in a frame buffer for subsequent subtraction from read values. Reset-related values are derived in each column by sampling the voltage during reset on one capacitor and the voltage on release of reset on a second capacitor, and differencing these values to provide an output for the frame buffer. This provides a reduction in the size of frame buffer which would otherwise be required.

Image sensor reading during reset and reading on release from reset

The fabrication of gallium-nitride (GaN)-based light-emitting diode (LED) arrays by a direct writing technique, itself using micron-sized LEDs (micro-LEDs), is reported. CMOS-driven ultraviolet GaN-based micro-LED arrays are used to pattern photoresist layers with feature sizes as small as 500 nm. Checkerboard-type square LED array devices are then fabricated using such photoresist patterns based on either single pixel or multipixel direct writing, and implemented as part of a completely mask-less process flow. These exemplar arrays are composed of either 450-nm-emitting 199 $\,\times\,$ 199 $\mu{\rm m}^{2}$ pixels on a 200- $\mu{\rm m}$ pitch or 520-nm-emitting 21 $\,\times\,$ 18 $\mu{\rm m}^{2}$ pixels on a 23- $\mu{\rm m}$ pitch. Fill factors of 99% and 71.5% are achieved with optical output power densities per pixel of 5 and 20 ${\rm W}/{\rm cm}^{2}$ at 90- and 6-mA dc-injected currents, respectively.

/pdf/sub-micron-lithography-using-ingan-micro-leds-mask-free-4vrmx5dxdk.pdf

Sub-Micron Lithography Using InGaN Micro-LEDs: Mask-Free Fabrication of LED Arrays

A 192×128 pixel single photon avalanche diode (SPAD) time-resolved single photon counting (TCPSC) image sensor is implemented in STMicroelectronics 40nm CMOS technology. The 13 % fill-factor, 18.4×9.2 µm pixel contains a 33 ps resolution, 135 ns full-scale, 12-bit time to digital converter (TDC) with 0.9 LSB differential and 5.64 LSB integral nonlinearity (DNL/INL). The sensor achieves a mean 219 ps full-width half maximum (FWHM) impulse response function (IRF) and is operable at up to 18.6 kfps. Cylindrical microlenses with a concentration factor of 3.25 increase the fill-factor to 42 %. The median dark count rate (DCR) is 25 Hz at 1.5 V excess bias. Fluorescence lifetime imaging (FLIM) results are presented.

/pdf/a-192-128-time-correlated-single-photon-counting-imager-in-2yvy0s4o7t.pdf

A 192×128 Time Correlated Single Photon Counting Imager in 40nm CMOS Technology

A CMOS image sensor that employs a vertically integrated double-junction photodiode structure is presented. This allows color imaging with only two filters. The sensor uses a 184*154 (near-QCIF) 6-transistor pixel array at a 9.6-/spl mu/m pitch implemented in 0.35-/spl mu/m technology. Results of the device characterization are presented. The imaging performance of an integrated two-filter color sensor is also projected, using measurements and software processing of subsampled images from the monochrome sensor with two color filters.

Robert Henderson

Papers

A reconfigurable 14-bit 60GPhoton/s Single-Photon receiver for visible light communications

Image sensor reading during reset and reading on release from reset

Sub-Micron Lithography Using InGaN Micro-LEDs: Mask-Free Fabrication of LED Arrays

A 192×128 Time Correlated Single Photon Counting Imager in 40nm CMOS Technology

A CMOS image sensor with a double-junction active pixel