Engineering topics
Publications and source records attributed to Hereld, Mark.
Advances in robotic automation, high-performance computing, and artificial intelligence encourage us to propose large, general-purpose science factories with the scale needed to tackle large discovery problems and to support thousands of scientists.
Self-driving labs (SDLs) leverage combinations of artificial intelligence, automation, and advanced computing to accelerate scientific discovery.
A system to generate image representations includes a first objective that receives a first light beam emitted from a sample and a second objective that receives a second light beam emitted from the sample, where the first light beam and the second light beam have conjugate phase. The system also includes a first diffractive element to receive the first light beam and separate it into a first plurality of diffractive light beams that are spatially distinct, and a second diffractive element to receive the second light beam and separate it into a second plurality of diffractive light beams that are spatially distinct. The system further includes a detector that receives the first and second plurality of diffractive light beams. The first plurality of diffractive light beams and the second plurality of diffractive light beams are simultaneously directed and focused onto different portions of an image plane of the detector.
We present optical and near-infrared photometry and spectroscopic redshifts of a well defined sample of 171 field galaxies selected from three high galactic latitude fields. This data set forms the basis for subsequent studies to characterize the trends, dispersion, and evolution of rest-frame colors and image structure. A subset of 143 galaxies constitutes a magnitude-limited sample to B approx. 19.9-20.75 (depending on field), with a median redshift of 0.14, and a maximum redshift of 0.54. This subset is statistically representative in its sampling of the apparent color distribution of galaxies. Thirty six galaxies were selected to have the reddest red-optical colors in two redshift intervals between 0.2 less than z less than 0.3. Photometric passbands are similar to U, B, V, I, and K, and sample galaxy spectral energy distributions between 0.37 and 2.2 micrometers in the observed frame, or down to 0.26 micrometers in the rest frame for the most distant galaxies. B and K images of the entire sample are assembled to form the first optical and near-infrared atlas of a statistically-representative sample of field galaxies. We discuss techniques for faint field-galaxy photometry, including a working definition of a total magnitude, and a method for matching magnitudes in different passbands and different seeing conditions to ensure reliable, integrated colors. Photographic saturation, which substantially affects the brightest 12% of our sample in the optical bands, is corrected with a model employing measured plate-density distributions for each galaxy, calibrated via similar measurements for stars as a function of known saturation level. Both the relative and absolute calibration of our photometry are demonstrated.
Long-slit optical spectroscopy, astrometry, and H-alpha forbidden S II and broad-band 2 micron images of HH 5 and of the HH 6 complex have been obtained. The excitations and radial velocities of the individual HH knots are described. The morphology of the optical and the 2 micron images (the latter dominated by H2 emission and/or the continuum of any embedded exciting stars) is compared; and the new astrometry is discussed. Finally, the likely sources of excitation of these HH nebulae are commented on.