The paper describes a large format 4 Megapixel (2352x1728) sensor with on-chip parallel 10 bit ADCs. The chip size is 20 x 20 mm with 7 μm pixel pitch. It achieves a high frame rate of 240 frames/s delivering 9.75 Gbit of data per second. The sensor also features an additional fixed pattern noise cancellation circuitry. The sensor operation voltage is 3.3 V with power dissipation of ~1 W at master clock rate of 66 MHz. Principal architecture of the sensor is discussed along with the results of its characterization. Introduction CMOS sensors are rapidly advancing in high-speed imaging. Compared to high-speed CCDs, with a degree of parallelism represented by the number of panels, CMOS sensors utilize the natural advantage of a column-parallel readout from the pixels. Row processing time can be readily reduced to one microsecond and lower, and the highspeed design focuses on such challenges as the column-multiplexing, ADC, and the reduction of system noise. Another advantage of a CMOS sensor to CCD is practically no smear nor blooming. Two years ago, a 1Mpixel digital image sensor with rolling shutter running at 500 Frames per second was presented [1]. It was an order improvement in data rate compared to the state-of the art high-speed CMOS sensors. Since that time, the progress was steady, but gave only about a factor of 2 increase in data throughput over 2 years. Mostly, the efforts were centered on the development of the pixels with full-frame shutter, featuring competitive performance. We believe that the stateof-the-art by the end of 2001 would be a 1K x 1K x 1K sensor (1000 Fps) with a shutter pixel. It is very likely that the progress in high speed CMOS imaging for many years in a row will still be defined by column-parallel architectures. However, a new generation of digital sensors [2] utilizing a higher, pixel-level degree of parallelism and using the benefits of the scaling along with the mainstream digital CMOS technology may be an additional path to high speed image capture. This article presents a chip, which is a result of the direct evolution of the baseline high-speed digital sensor design [1]. The architecture did not change much, but the following improvements were made: resolution was increased 4 times, from 1024x1024 to 2352x1728, column-parallel ADC evolved from 8 to 10 bit, temporal and fixed-pattern noise was reduced, sensitivity was improved. The overall throughput increased from 4 Gbit/s to almost 10 Gbit/s. Sensor building blocks The sensor block diagram is presented in Fig.1. In addition to the pixel array based on the conventional 3T APS pixel, the sensor contains columnparallel ADCs and memory, column and row decoders, row drivers, and two controllers to run concurrently row operations including A/D conversion and read-write memory operations. Circuit solutions for these blocks did not change much since the previous design, so we refer the reader to [1] for details. One thing that changed about the ADC is that in order to achieve 10 bit operation without using too large capacitors, we generated a reference voltage equal of 1⁄4 of the ADC reference and used larger capacitors for 3 of the less significant bits. Sensor resolution, 2352x1728 was defined by a customer and, although it did not represent any up-to-date industry standard, it has a very useful aspect ratio of 4:3. Also, the sensor can support a Super XGA (2048x1536) format just emerging on the computer market. And, the chip can be used as a high speed HDTV imager with subresolution of 1920x1080 (Fig.2.). The sensor was designed so that the row operations are completed in 128 clocks. This corresponds to reading out of 2048 columns. Thus, the speed in subresolution modes can be further increased by skipping the rest of unread columns. Of course, this is in addition to the reduction of the frame time with less number of rows in the frame. Direct external addressing to the rows gives the user a flexibility of selecting the window of interest within the center of the pixel array, achieving maximum photoresponse uniformity. The earlier 1Mpixel sensor had an offset-calibration circuit for each ADC. However, the resolution of the internal compensation DAC was only 5 bits. In the reported sensor, the DAC resolution was increased to 7 bits. In addition, a read/write access to the calibration DACs is provided through a serial interface. This yields stability of calibration vectors during the sensor operation. Also, if for some reasons, the internal calibration does not fully remove column-wise fixed pattern noise, the values can be calculated externally and downloaded into the chip. Layout and CMOS process The floorplan of the chip layout is outlined in Fig.3. ADCs and memory are split between the top and the bottom for symmetry, performance, and routing considerations. Digital pads are on the left, and at the top/bottom. Analog pads are to the right. The pixel array area slightly exceeds 1’’ format. The chip with the size of 20mm x 20mm fits into one reticule. Wafers were fabricated in a 0.35um CMOS sensor process with double poly used for capacitors and triple metal for routing. Characterization results The sensor was characterized using a custom board with a frame grabber and a PC interface. The board provided 9 upper bits image recording. So the lsb in the following pictures represents the second bit. By the time of writing the paper, only limited characterization using only green light has been done. All the measurements were performed for the sensor running at 130 frames/s and for 1V ADC reference voltage. The results of the characterization are summarized in Table.1.
This paper describes a large-format 4-Mpixel (2352/spl times/1728) sensor with on-chip parallel 10-b analog-to-digital converters (ADCs). The chip size is 20/spl times/20 mm with a 7-/spl mu/m pixel pitch. At a 66-MHz master clock rate and 3.3-V operating voltage, it achieves a high frame rate of 240 frames/s delivering 9.75 Gb/s of data with power dissipation of less than 700 mW. The principal architectural features of the sensor are discussed along with the results of sensor characterization.
The paper presents a high-speed (500 f/s) large-format 1 K/spl times/1 K 8 bit 3.3 V CMOS active pixel sensor (APS) with 1024 ADCs integrated on chip. The sensor achieves an extremely high output data rate of over 500 Mbytes per second and a low power dissipation of 350 mW at the 66 MHz master clock rate. Principal architecture and circuit solutions allowing such a high throughput are discussed along with preliminary results of the chip characterization.
Passive electrical circuits whose voltage and current equations are exactly equivalent to the small-signal rate equations of a semiconductor laser are derived to model an electrically modulated laser (verified to be the same as that given in the literature), an optically modulated laser (i.e., a laser used as an optical amplifier), and a multimode laser. These circuits offer a fast and efficient simulation tool with little computational complexity in which the small-signal assumption (i.e., small modulation range) is neither violated nor insufficient for the simulation.
The heterogeneous integration of optoelectronic, electronic, and micro-mechanical components from different origins and substrates makes possible many advanced systems in diverse applications. Besides the monolithic integration approach, which is the basis for the success of today's silicon industry, various hybrid integration technologies have been explored. These include flip-chip bonding, micro-robotic placement, epitaxial lift-off and direct bonding, substrate removal and bonding, and several self-assembly methods. In this paper, we describe the results of our monolithic integration effort involving a 2 by 2 optoelectronic switching circuit and an 8 by 8 active-pixel sensor array on GaAs substrates, and a 16 by 16 spatial light modulator array produced by flip-chip bonding of III-V multi-quantum-well (MQW) modulators and silicon driver circuits. We also present our preliminary experimental results on the self-assembly of small inorganic devices coated with DNA polymers with self- recognition properties.
Optical interconnections have been proposed to replace electrical wires for global data communications in computing systems to alleviate communication bottlenecks on the electronic processing planes. The potential for high speed, high connection density, and low energy has been analyzed.['] Compared to an all-electronic system, an additional subsystem is needed in an optical interconnection system. This subsystem, referred to as the photonics layer, provides elecytrical-optical signal conversions and proper signal routing. It contains optical transmitters and drivers, detectors and amplifiers, and optical routing elements, and is considered to begin at the transmitter driver input and end at the detector amplifier output. We attempt to evaluate the performance of the photonics layers for free-space optical interconnections when using lead-lanthanum-zirconate-titanate (PLZT) modulators, III-V semiconductor multiple-quantumwell (MQW) modulators, or vertical-cavity surface emitting lasers (VCSELs) transmitter technologies. The areal data throughputs and the energy requirements are discussed for implementations of various network architectures.
view Abstract Citations (2) References (7) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A simple estimate of the effect of a thick circumstellar dust shell on photospheric line profiles. van Blerkom, D. ; Castor, J. I. Abstract A star embedded in an optically thick dust shell may have a line spectrum that closely resembles the spectrum of some unobscured star - e.g., VY CMa (shrouded) and alpha Her (unshrouded). This implies that the surface temperatures of the two stars are nearly equal, but since one is subject to a back-warming effect, the distributions of temperature with depth in the respective atmospheres are dissimilar. We find that effective temperatures and absorption line strengths are reduced in shrouded stars below the values that obtain in their unshrouded counterparts. For models of VY CMa that yield grain temperatures at the inner boundary of the dust shell consistent with observation, the reduction in strength of a visible line is small (not more than 15%). Thus the spectral distribution of alpha Her may be used as an approximation to that of VY CMa before it is scattered by the dust, without the necessity of first correcting for back warming. Publication: The Astrophysical Journal Pub Date: January 1979 DOI: 10.1086/156763 Bibcode: 1979ApJ...227..543V Keywords: Cosmic Dust; Line Spectra; Photosphere; Stellar Envelopes; Stellar Spectra; Absorption Spectra; Optical Thickness; Stellar Atmospheres; Stellar Models; Stellar Temperature; Astrophysics; Circumstellar Shells; Circumstellar Shells:Line Profiles; Circumstellar Shells:Radiative Transfer; Circumstellar Shells:Supergiants; Stellar Photospheres full text sources ADS |
view Abstract Citations (27) References (12) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS The effect of an expanding dust cloud on radial velocity measurements. van Blerkom, J. ; van Blerkom, D. Abstract Radial velocities of 'supergiant' maser sources, such as VY CMa, do not always agree with what would be expected if the maser emission originates in an expanding spherical shell. It has been proposed that the photospheric absorption lines are shifted to the red by scattering off dust grains in the shell. A Monte Carlo computation of this process is performed. The results strongly support the scattering hypothesis, although the question of how the redshift can disappear in only a few years is bothersome. In particular, it is shown that if the spectrum of Alpha Her is passed through an expanding dust shell, the emergent spectrum is remarkably close to that of VY CMa. Publication: The Astrophysical Journal Pub Date: October 1978 DOI: 10.1086/156508 Bibcode: 1978ApJ...225..482V Keywords: Cosmic Dust; Interstellar Masers; Radial Velocity; Stellar Envelopes; Supergiant Stars; Velocity Measurement; Absorption Spectra; Electromagnetic Scattering; Hydroxyl Emission; Monte Carlo Method; Photosphere; Stellar Spectra; Astrophysics; Circumstellar Shells:Supergiants; Masers:Radial Velocities; Masers:Supergiants full text sources ADS |
view Abstract Citations (8) References (5) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS HD 45166: a dwarf in Wolf-Rayet clothing. van Blerkom, D. Abstract A coarse analysis of the hydrogen and helium lines of HD 45166 is performed which supports the interpretation that the object is a binary composed of a late B star and a star of approximately one solar radius with a continuous energy distribution very much like that of Zeta Pup. It is surrounded by an envelope expanding at 150 km/s formed by mass ejection at a rate of only 5 hundred-millionths of a solar mass per yr. The small size and low ejection velocity give densities of He II in the envelope of about 100 billion per cu cm. The envelope environment is thus much like that of a normal Wolf-Rayet star, which it mimics with remarkable consistency. Publication: The Astrophysical Journal Pub Date: October 1978 DOI: 10.1086/156478 Bibcode: 1978ApJ...225..175V Keywords: Binary Stars; Dwarf Stars; Hot Stars; Stellar Spectra; Wolf-Rayet Stars; B Stars; Balmer Series; Emission Spectra; H Lines; Helium; Stellar Envelopes; Stellar Winds; Astronomy; Binaries:Emission-Line Stars; Envelopes:Wolf-Rayet Stars full text sources ADS | data products SIMBAD (1)
view Abstract Citations (19) References (9) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Indications of circumstellar ring systems from SiO and H2O maser lines. van Blerkom, D. Abstract Not infrequently, profiles of maser emission lines show a symmetrical structure in which satellite components are spaced evenly about a central peak. This structure has been observed in the SiO and H2O spectra from cool supergiants. One possible geometry for matter in the vicinity of a luminous star is that of a circumstellar ring system. In this paper, the maser emission from such a geometry is computed, and shown to have the observed characteristics. The interpretation is not, however, unique: VLBI maps of H2O emission from VY CMa show a haphazard geometry, but the line profile is identical to that derived for a ring system. One feature which may distinguish the circumstellar rings from other geometries is the stability in time of the pattern of emission components. Subject headings: interstellar: molecules - masers - stars: circumstellar shells Publication: The Astrophysical Journal Pub Date: August 1978 DOI: 10.1086/156316 Bibcode: 1978ApJ...223..835V Keywords: Fine Structure; Interstellar Gas; Silicon Oxides; Stellar Envelopes; Supergiant Stars; Water Masers; Line Spectra; Maser Outputs; Ring Structures; Spherical Shells; Stellar Luminosity; Very Long Base Interferometry; Astrophysics; Circumstellar Shells:Emission Lines; Circumstellar Shells:M Supergiants full text sources ADS |
view Abstract Citations (22) References (6) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Mass loss from P Cygni. II. An equivalent two-level-atom approach. Kunasz, P. ; van Blerkom, D. Abstract The formation of the Balmer-line spectrum of P Cygni is investigated by using an equivalent two-level-atom formalism. This approach eliminates the artificial distinction between a continuum-emitting core and line-emitting envelope, and also does not employ a supersonic approximation in the line-transfer problem. The results support the conclusion that a velocity distribution similar to the linear law, v(r) is proportional to r, exists in the envelope and can account for the observed Balmer lines. A more complicated velocity law derived from infrared continuum measurements does not give a good representation of the Balmer lines. Publication: The Astrophysical Journal Pub Date: August 1978 DOI: 10.1086/156365 Bibcode: 1978ApJ...224..193K Keywords: Astronomical Spectroscopy; Balmer Series; Stellar Envelopes; Stellar Mass Ejection; Cygnus Constellation; Emission Spectra; H Lines; Spectral Line Width; Stellar Models; Astrophysics; Balmer Lines:Emission-Line Stars; Line Formation:P Cygni Stars; Mass Loss:P Cygni Stars full text sources ADS |
A simple approximation for line transfer problems is presented which is useful when photons scatter only a few times before being destroyed. Comparison is made to solutions of high accuracy.
view Abstract Citations (9) References (7) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A Non-Lte Theory of Overlapping Lines Near the Series Limit van Blerkom, D. ; Hummer, D. G. Abstract The effects of overlapping on the formation of spectral lines near the series limit are investigated through the introduction of a band model Numerical solutions are obtained which show that the source function can be increased by a factor of 2 for e = 0 1 and by much larger amounts for smaller A cri- terion is presented to check when overlapping is likely to be important Publication: The Astrophysical Journal Pub Date: November 1968 DOI: 10.1086/149793 Bibcode: 1968ApJ...154..741V full text sources ADS |