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Virtual Symmetry Axes for the Layout of Analog IC's
Malavasi, Enrico,Charbon, Edoardo,Jusuf, Gani,Totaro, Roberto,Vincentelli, Alberto Sangiovanni 대한전자공학회 1991 ICVC : International Conference on VLSI and CAD Vol.2 No.1
A new approach to the layout of integrated circuits with multiple symmetry axes is presented in this paper. When more than one symmetry is present, the usual approach to placement grad compaction makes extensive ruse of hierarchy, which requires firmed positions for symmetry ayes. As a result, wiring and area optimizations rare poor. The position of a virtual symmetry axis is variable, and dynamically defined by the center of a group of symmetric modules and wires called cluster. Virtual symmetry axes have been implemented in a placement tool using the Simulated Annealing algorithm and in a compaction tool based on the constraint-graph longest-path algorithm. Results are shown proving the suitability of this approach.
Malavasi, N.,Arnouts, S.,Vibert, D.,de la Torre, S.,Moutard, T.,Pichon, C.,Davidzon, I.,Kraljic, K.,Bolzonella, M.,Guzzo, L.,Garilli, B.,Scodeggio, M.,Granett, B. R.,Abbas, U.,Adami, C.,Bottini, D.,Ca Oxford University Press 2017 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.465 No.4
<P>We present the first quantitative detection of large-scale filamentary structure at z similar or equal to 0.7 in the large cosmological volume probed by the VIMOS Public Extragalactic Redshift Survey (VIPERS). We use simulations to show the capability of VIPERS to recover robust topological features in the galaxy distribution, in particular the filamentary network. We then investigate how galaxies with different stellar masses and stellar activities are distributed around the filaments, and find a significant segregation, with the most massive or quiescent galaxies being closer to the filament axis than less massive or active galaxies. The signal persists even after downweighting the contribution of peak regions. Our results suggest that massive and quiescent galaxies assemble their stellar mass through successive mergers during their migration along filaments towards the nodes of the cosmic web. On the other hand, low-mass star-forming galaxies prefer the outer edge of filaments, a vorticity-rich region dominated by smooth accretion, as predicted by the recent spin alignment theory. This emphasizes the role of large-scale cosmic flows in shaping galaxy properties.</P>
CMOS Layout Module Generation with Matching Constraints
Pandini, Davide,Malavasi, Enrico 대한전자공학회 1993 ICVC : International Conference on VLSI and CAD Vol.3 No.1
In this contribution a general and effective methodology for module generation in a full-stacked layout paradigm for CMOS analog integrated circuits is presented. Analog constraints an symmetry and marching reduce the computational complexity of robust graph algorithms. Matching constraints arc carefully taken into account and an algorithm is proposed to satisfy precise matching requirements in analog stacked layouts. Along with sensitivity analysis and automatic constraint generation, this algorithm provides a suitable performance-driven approach to CMOS layout module generation.
COSMOS2015 photometric redshifts probe the impact of filaments on galaxy properties
Laigle, C,Pichon, C,Arnouts, S,McCracken, H J,Dubois, Y,Devriendt, J,Slyz, A,Le Borgne, D,Benoit-Lé,vy, A,Hwang, Ho Seong,Ilbert, O,Kraljic, K,Malavasi, N,Park, Changbom,Vibert, D Oxford University Press 2018 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.474 No.4
<P>The variation of galaxy stellar masses and colour types with the distance to projected cosmic filaments are quantified using the precise photometric redshifts of the COSMOS2015 catalogue extracted from Cosmological Evolution Survey (COSMOS) field (2 deg(2)). Realistic mock catalogues are also extracted from the lightcone of the cosmological hydrodynamical simulation HORIZON-AGN. They show that the photometric redshift accuracy of the observed catalogue (sigma(z) < 0.015 at M-* > 10(10)M(circle dot) and z < 0.9) is sufficient to provide two-dimensional (2D) filaments that closely match their projected three-dimensional (3D) counterparts. Transverse stellar mass gradients are measured in projected slices of thickness 75 Mpc between 0.5 < z < 0.9, showing that the most massive galaxies are statistically closer to their neighbouring filament. At fixed stellar mass, passive galaxies are also found closer to their filament, while active star-forming galaxies statistically lie further away. The contributions of nodes and local density are removed from these gradients to highlight the specific role played by the geometry of the filaments. We find that the measured signal does persist after this removal, clearly demonstrating that proximity to a filament is not equivalent to proximity to an overdensity. These findings are in agreement with gradients measured in both 2D and 3D in the HORIZON-AGN simulation and those observed in the spectroscopic surveys VIPERS and GAMA (which both rely on the identification of 3D filaments). They are consistent with a picture in which the influence of the geometry of the large-scale environment drives anisotropic tides that impact the assembly history of galaxies, and hence their observed properties.</P>
Galaxy evolution in the metric of the cosmic web
Kraljic, K.,Arnouts, S.,Pichon, C.,Laigle, C.,de la Torre, S.,Vibert, D.,Cadiou, C.,Dubois, Y.,Treyer, M.,Schimd, C.,Codis, S.,de Lapparent, V.,Devriendt, J.,Hwang, H. S.,Le Borgne, D.,Malavasi, N.,Mi Oxford University Press 2018 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.474 No.1
Discovery of a Very Large (≈20 kpc) Galaxy at <i>z</i> = 3.72
Lee, Kyoung-Soo,Dey, Arjun,Matheson, Thomas,Shi, Ke,Hung, Chao-Ling,Xue, Rui,Inami, Hanae,Huang, Yun,Lee, Khee-Gan,Ashby, Matthew L. N.,Jannuzi, Buell,Reddy, Naveen,Hong, Sungryong,Mo, Wenli,Malavasi, American Astronomical Society 2018 The Astrophysical journal Vol.862 No.1
<P>We report the discovery and spectroscopic confirmation of a very large star-forming galaxy, G6025, at z(spec) = 3.721 +/- 0.003. In the rest frame approximate to 2100 angstrom, G6025 subtends approximate to 24 kpc in physical extent when measured from the 1.5 sigma isophote, in agreement with the parametric size measurements that yield a half-light radius of 4.9 +/- 0.5 kpc and a semimajor axis of 12.5 +/- 0.1 kpc. It is also very UV-luminous (approximate to 5L(UV,z similar to 4)*) and young (approximate to 140 +/- 60 Myr). Despite its unusual size and luminosity, the stellar population parameters and dust reddening (M-star similar to M-z similar to 4*( )and E(B - V) similar to 0.18 +/- 0.05) estimated from the integrated light are similar to those of smaller galaxies at comparable redshifts. The ground-based morphology and spectroscopy show two dominant components, both located off-center, embedded in more diffuse emission. We speculate that G6025 may be a scaled-up version of chain galaxies seen in deep HST imaging or, alternatively, a nearly equal-mass merger involving two super-L* galaxies in its early stage. It lies close to but not within a known massive protocluster at z = 3.78. We find four companions within 6 Mpc from G6025, two of which lie within 1.6 Mpc. While the limited sensitivity of the existing spectroscopy does not allow us to robustly characterize the local environment of G6025, it likely resides in a locally overdense environment. The luminosity, size, and youth of G6025 make it uniquely suited to study the early formation of massive galaxies in the universe.</P>