Field-of-view control of segmented NIR VCSEL arrays for next-generation flash LiDARs

2020 ◽  
Author(s):  
Babu Dayal Padullaparthi ◽  
Takemasa Tamanuki ◽  
Dieter H. Bimberg
Keyword(s):  
Field Of View ◽  
Next Generation ◽  
Vcsel Arrays

scholarly journals LSST and the Epoch of Reionization Experiments

2017 ◽  
Vol 12 (S333) ◽  
pp. 222-227
Author(s):  
Željko Ivezić
Keyword(s):  
Dark Matter ◽  
Dark Energy ◽  
Time Domain ◽  
Point Sources ◽  
Field Of View ◽  
Next Generation ◽  
Imaging Data ◽  
Primary Mirror ◽  
Scientific Investigations ◽  
Near Earth Asteroids

AbstractThe Large Synoptic Survey Telescope (LSST), a next generation astronomical survey, sited on Cerro Pachon in Chile, will provide an unprecedented amount of imaging data for studies of the faint optical sky. The LSST system includes an 8.4m (6.7m effective) primary mirror and a 3.2 Gigapixel camera with a 9.6 sq. deg. field of view. This system will enable about 10,000 sq. deg. of sky to be covered twice per night, every three to four nights on average, with typical 5-sigma depth for point sources ofr= 24.5 (AB). With over 800 observations in theugrizybands over a 10-year period, these data will enable coadded images reachingr= 27.5 (about 5 magnitudes deeper than SDSS) as well as studies of faint time-domain astronomy. The measured properties of newly discovered and known astrometric and photometric transients will be publicly reported within 60 sec after closing the shutter. The resulting hundreds of petabytes of imaging data for about 40 billion objects will be used for scientific investigations ranging from the properties of near-Earth asteroids to characterizations of dark matter and dark energy. For example, simulations estimate that LSST will discover about 1,000 quasars at redshifts exceeding 7; this sample will place tight constraints on the cosmic environment at the end of the reionization epoch. In addition to a brief introduction to LSST, I review the value of LSST data in support of epoch of reionization experiments and discuss how international participants can join LSST.

scholarly journals Everything we’d like to do with LSST data, but we don’t know (yet) how

2016 ◽  
Vol 12 (S325) ◽  
pp. 93-102 ◽  
Author(s):  
Željko Ivezić ◽  
Andrew J. Connolly ◽  
Mario Jurić
Keyword(s):  
Optical Imaging ◽  
Time Domain ◽  
Point Sources ◽  
Field Of View ◽  
Next Generation ◽  
Maximum Information ◽  
Primary Mirror

AbstractThe Large Synoptic Survey Telescope (LSST), the next-generation optical imaging survey sited at Cerro Pachon in Chile, will provide an unprecedented database of astronomical measurements. The LSST design, with an 8.4m (6.7m effective) primary mirror, a 9.6 sq. deg. field of view, and a 3.2 Gigapixel camera, will allow about 10,000 sq. deg. of sky to be covered twice per night, every three to four nights on average, with typical 5-sigma depth for point sources of r=24.5 (AB). With over 800 observations in ugrizy bands over a 10-year period, these data will enable a deep stack reaching r=27.5 (about 5 magnitudes deeper than SDSS) and faint time-domain astronomy. The measured properties of newly discovered and known astrometric and photometric transients will be publicly reported within 60 sec after observation. The vast database of about 30 trillion observations of 40 billion objects will be mined for the unexpected and used for precision experiments in astrophysics. In addition to a brief introduction to LSST, we discuss a number of astro-statistical challenges that need to be overcome to extract maximum information and science results from LSST dataset.

scholarly journals LSST survey: millions and millions of quasars

2016 ◽  
Vol 12 (S324) ◽  
pp. 330-337 ◽  
Author(s):  
Željko Ivezić
Keyword(s):  
Optical Imaging ◽  
Time Domain ◽  
Point Sources ◽  
Field Of View ◽  
Next Generation ◽  
Primary Mirror

AbstractThe Large Synoptic Survey Telescope (LSST), the next-generation optical imaging survey sited at Cerro Pachon in Chile, will provide hundreds of detections for a sample of more than ten million quasars with redshifts up to about seven. The LSST design, with an 8.4m (6.7m effective) primary mirror, a 9.6 sq. deg. field of view, and a 3.2 Gigapixel camera, will allow about 10,000 sq. deg. of sky to be covered twice per night, every three to four nights on average, with typical 5-sigma depth for point sources of r=24.5 (AB). With about 1000 observations in ugrizy bands over a 10-year period, these data will enable a deep stack reaching r=27.5 (about 5 magnitudes deeper than SDSS) and faint time-domain astronomy. The measured properties of newly discovered and known astrometric and photometric transients will be publicly reported within 60 sec after closing the shutter. In addition to a brief introduction to LSST, I review optical quasar selection techniques, with emphasis on methods based on colors, variability properties, and astrometric behavior.

Incorporating Dynamic Field of View Information to Design the Next-Generation Black Hawk Helicopter Cockpit

1989 ◽  
Vol 33 (16) ◽  
pp. 1124-1128
Author(s):  
Robert Simon ◽  
Dennis Dunn
Keyword(s):  
Night Vision ◽  
Field Of View ◽  
Next Generation ◽  
Independent Contractor ◽  
Technical Data ◽  
Critical Areas ◽  
Study Team ◽  
Accident Data ◽  
Static Conditions ◽  
Cockpit Design

Changing flight tactics and increased use of Night Vision Goggles (NVGs) has focused attention on the limited Field of View (FOV) of the Army UH-60A Black Hawk Helicopter. To improve the FOV in the next generation Black Hawk, the U.S. Army tasked an independent contractor to investigate the problem and propose alternatives. The study involved a comprehensive review of Army requirement documents, existing FOV studies, and accident data. Close attention was given to dynamic flight characteristics that affect FOV. Also, the study team collected technical data related to military rotary wing design, administered a survey to pilots; and interviewed users and other technical experts. The study revealed the current UH-60A design meets the requirements of MIL-STD-850B under static conditions. The only exception is the obstructed view that the door and windshield vertical structures create. However, under dynamic conditions the UH-60A cockpit design and normal flight characteristics substantially reduce the FOV in critical areas. The study produced eleven options that can improve and/or enhance the next generation Black Hawk's FOV if incorporated into the new design. Each option is presented and discussed.

Very High Resolution Analysis of the Dynamics of a Coronal Plasmoid

1994 ◽  
Vol 144 ◽  
pp. 593-596
Author(s):  
O. Bouchard ◽  
S. Koutchmy ◽  
L. November ◽  
J.-C. Vial ◽  
J. B. Zirker
Keyword(s):  
High Resolution ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Field Of View ◽  
Small Field ◽  
High Resolution Analysis ◽  
Ccd Observations ◽  
Resolution Analysis ◽  
Very High ◽  
Small Field Of View

AbstractWe present the results of the analysis of a movie taken over a small field of view in the intermediate corona at a spatial resolution of 0.5“, a temporal resolution of 1 s and a spectral passband of 7 nm. These CCD observations were made at the prime focus of the 3.6 m aperture CFHT telescope during the 1991 total solar eclipse.

Dynamic Scanning Electron Microscopy of Small Particles

1975 ◽  
Vol 33 ◽  
pp. 280-281
Author(s):  
W. Krakow ◽  
W. C. Nixon
Keyword(s):  
Electron Microscopy ◽  
Low Noise ◽  
Time Sequence ◽  
Field Of View ◽  
Video Tape ◽  
Small Particles ◽  
Polystyrene Spheres ◽  
Field Distributions ◽  
Dynamic Scanning ◽  
Scanning Electron

The scanning electron microscope (SEM) can be run at television scanning rates and used with a video tape recorder to observe dynamic specimen changes. With a conventional tungsten source, a low noise TV image is obtained with a field of view sufficient to cover the area of the specimen to be recorded. Contrast and resolution considerations have been elucidated and many changing specimens have been studied at TV rates.To extend the work on measuring the magnitude of charge and field distributions of small particles in the SEM, we have investigated their motion and electrostatic interaction at TV rates. Fig. 1 shows a time sequence of polystyrene spheres on a conducting grating surface inclined to the microscope axis. In (la) there are four particles present in the field of view, while in (lb) a fifth particle has moved into view.

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