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The Bay of Bengal exhibits a diverse and complex topography on its seafloor, characterized by deep trenches, abyssal plains, submarine canyons, seamounts, and volcanic ridges. The topography is influenced by tectonic processes, sediment accumulation from the Himalayas, and river transport. The sediment distribution patterns in the Bay of Bengal are influenced by various factors, including river inputs, ocean currents, and seafloor topography.

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PESTS OF SUGARCANE - BORERS BORERS 1. Early shoot borer, Chilo infuscatellus, Crambidae, Lepidoptera Symptom of damage: Deadheart in 1-3 month old crop, which can be easily pulled out, rotten portion of the straw coloured dead-heart emits an offensive odour. A number of bore holes at the base of the shoot just above the ground level. Nature of damage: Caterpillar bores into the central shoot and feeds on the internal tissue. This cause interference in the translocation of plant sap and damage the sugar storing tissues. Egg: Flat-scale like eggs are laid in 3-5 rows on the lower surface of leaves in masses of 4-100. The masses are slightly overlapping like tiles. Larva: Larva is dirty white with five dark violet longitudinal stripes and dark brown head. Pupa: Pupation takes place within the tunnel. Caterpillar before pupating makes a large exit hole in the stem and blocks the opening with silken discs. Adult: Pale greyish brown moth with black dots near the costal margin of the forewings and with white hindwings. 2. Internode borer, Chilo sacchariphagus indicus, Crambidae, Lepidoptera Symptom of damage: Internodes constricted and shortened, with a number of boreholes and fresh excreta in the nodal region. Affected tissues reddened. Nature of damage: Caterpillars attack sugarcane plants after 3 months of planting. They bore into the canes near the nodes; entry holes are plugged with excreta. Entry is generally confined to the first five internodes. Egg: Scale-like white eggs are laid by female moths in batches of 9-11, near the midribs, on leaf sheaths or on stem. Larva: White larva with four violet longitudinal stripes and light brown head. Pupa: Pupation takes place in semi-dried leaf sheath. Adult: Pale brown with white hind wings. 3. Top borer, Scirpophaga excerptalis, Pyralidae, Lepidoptera Symptom of damage: Deadheart in grownup canes, which cannot be easily pulled; deadheart reddish brown in colour; parallel row of shot holes in the emerging leaves and red tunnels in the midribs of leaves; bunchy tip due to the growth of side shoots. Nature of damage: Caterpillars are mainly found in the apical portion of the canes, boring through the growing point and down the upper joints until it reaches the sappy portion of the stem, there it feeds on the tissues and destroys the cane. They also bore into the unfolded leaves preferably into the midrib, mining its way to the base. Egg: Eggs are laid on the lower surface of top leaves in clusters particularly near midribs. The clusters are covered with buff coloured hairs. Larva :Smooth, white or cream coloured with a red coloured mid-dorsal line and yellow head. Pupa: Pupation takes place within the larval tunnel in a chamber with an exit hole constructed by the caterpillar. Adult: White coloured moth (with a buff coloured anal tuft in the abdominal tip of female).

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Below are the important points I note from the 2020 paper by Martin Grohe: - 1-WL distinguishes almost all graphs, in a probabilistic sense - Classical WL is two dimensional Weisfeiler-Leman - DeepWL is an unlimited version of WL graph that runs in polynomial time. - Knowledge graphs are essentially graphs with vertex/edge attributes ABSTRACT: Vector representations of graphs and relational structures, whether handcrafted feature vectors or learned representations, enable us to apply standard data analysis and machine learning techniques to the structures. A wide range of methods for generating such embeddings have been studied in the machine learning and knowledge representation literature. However, vector embeddings have received relatively little attention from a theoretical point of view. Starting with a survey of embedding techniques that have been used in practice, in this paper we propose two theoretical approaches that we see as central for understanding the foundations of vector embeddings. We draw connections between the various approaches and suggest directions for future research.

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We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and 30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1 . Our search finds no candidates at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to infer the properties of the evolving luminosity function without binning in redshift or luminosity that marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results, and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5 from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical models for evolution of the dark matter halo mass function.

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We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors 42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory, as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of 12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.

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