(Kpi summer school 2015) theano tutorial part2

•

4 likes•1,618 views

Serhii Havrylov

https://github.com/sergii-gavrylov/theano-tutorial-AACIMP2015

Theano tutorial
part 2
AACIMP 2015
Sergii Gavrylov

Overview
● Brief recap
● Multivariate logistic regression
● Multilayer perceptron
● Convolution
● Convolutional neural network
● scan
● Recurrent neural network

Brief recap
● Symbolic variables
● Functions
● Shared variables / updates
● Gradients
● Substitution

Computational graph
X
+
Z
Y
● Code generation
● Symbolic differentiation

Multivariate logistic
regression
0
1
2
3
softmax(x * W)

Multilayer perceptron
0
1
2
3
relu(x * W) softmax(x * W)

1D Convolution

1D Convolution

1D Convolution

1D Convolution

2D Convolution
filter =

Max pooling
cs231n.github.io/convolutional-networks

ConvPoolLayer

Convolutional NN
cs231n.github.io/convolutional-networks
deeplearning.net/tutorial/lenet.html

Convolutional NN
deeplearning.net/tutorial/lenet.html

scan
(Symbolic loop in theano)

Recurrent neural network
www.iro.umontreal.ca/~bengioy/dlbook/rnn.html

“Vanilla” RNN
www.iro.umontreal.ca/~bengioy/dlbook/rnn.html

Conclusion
● Theano has a lot of useful building blocks (convolution, scan).
● Theano supports both cpu and gpu backends.

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GBSN - Microbiology (Unit 1)

GBSN - Microbiology (Unit 1)

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Context. WASP-76 b has been a recurrent subject of study since the detection of a signature in high-resolution transit spectroscopy data indicating an asymmetry between the two limbs of the planet. The existence of this asymmetric signature has been confirmed by multiple studies, but its physical origin is still under debate. In addition, it contrasts with the absence of asymmetry reported in the infrared (IR) phase curve. Aims. We provide a more comprehensive dataset of WASP-76 b with the goal of drawing a complete view of the physical processes at work in this atmosphere. In particular, we attempt to reconcile visible high-resolution transit spectroscopy data and IR broadband phase curves. Methods. We gathered 3 phase curves, 20 occultations, and 6 transits for WASP-76 b in the visible with the CHEOPS space telescope. We also report the analysis of three unpublished sectors observed by the TESS space telescope (also in the visible), which represents 34 phase curves. Results. WASP-76 b displays an occultation of 260±11 and 152±10 ppm in TESS and CHEOPS bandpasses respectively. Depending on the composition assumed for the atmosphere and the data reduction used for the IR data, we derived geometric albedo estimates that range from 0.05 ± 0.023 to 0.146 ± 0.013 and from <0.13 to 0.189 ± 0.017 in the CHEOPS and TESS bandpasses, respectively. As expected from the IR phase curves, a low-order model of the phase curves does not yield any detectable asymmetry in the visible either. However, an empirical model allowing for sharper phase curve variations offers a hint of a flux excess before the occultation, with an amplitude of ∼40 ppm, an orbital offset of ∼−30◦ , and a width of ∼20◦ . We also constrained the orbital eccentricity of WASP-76 b to a value lower than 0.0067, with a 99.7% confidence level. This result contradicts earlier proposed scenarios aimed at explaining the asymmetry observed in high-resolution transit spectroscopy. Conclusions. In light of these findings, we hypothesise that WASP-76 b could have night-side clouds that extend predominantly towards its eastern limb. At this limb, the clouds would be associated with spherical droplets or spherically shaped aerosols of an unknown species, which would be responsible for a glory effect in the visible phase curves.

Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

A botany file is similar to a chemistry practical file but specifically focuses on experiments and observations related to plants. It typically includes detailed descriptions of plant-related experiments, such as germination studies, growth experiments, tissue culture techniques, plant anatomy investigations, and ecological surveys. The file may contain records of plant specimens collected, their classification, characteristics, and ecological significance. Additionally, it may include diagrams, photographs, drawings, tables, and data analysis related to plant research. Like a chemistry practical file, a botany file serves as a documentation of practical work conducted in the field of botany and is often used for assessment and educational purposes.

Botany 4th semester file By Sumit Kumar yadav.pdf

Botany 4th semester file By Sumit Kumar yadav.pdf

Botany 4th semester file By Sumit Kumar yadav.pdf

Sumit Kumar yadav

HotJupiters are amongthebest-studied exoplanets, but it is still poorly understood how their chemical composition and cloud properties vary with longitude. Theoretical models predict that clouds may condense on the nightside and that molecular abundances can be driven out of equilibrium by zonal winds. Here we report a phase-resolved emission spectrum of the hot Jupiter WASP-43b measured from 5–12µ 5–12µ 5–12µm with JWST’s Mid-Infrared Instrument (MIRI). 1524 ±35 1524 ±35 and 863±23 The spectra reveal a large day–night temperature contrast (with average brightness temperatures of 1524 ± 35 863 ±23 863 ±23Kelvin, respectively) and evidence for water absorption at all orbital phases. Comparisons with three-dimensional atmospheric models show that both the phase curve shape and emission spectra strongly suggest the presence of nightside clouds which become optically thick to thermal emission at pressures greater than ∼100mbar. The dayside is consistent with a cloudless atmosphere above the mid-infrared photosphere. Con3trary to expectations from equilibrium chemistry but consistent with disequilibrium kinetics models, methane is not detected on the nightside (2σ upper limit of 1–6 parts per million, depending on model assumptions).

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b

Conjugation, transduction and transformation

Conjugation, transduction and transformation

Conjugation, transduction and transformation

Theoretical predictions and observational data indicate a class of sub-Neptune exoplanets may have water-rich interiors covered by hydrogen-dominated atmospheres. Provided suitable climate conditions, such planets could host surface liquid oceans. Motivated by recent JWST observations of K2-18 b, we self-consistently model the photochemistry and potential detectability of biogenic sulfur gases in the atmospheres of temperate sub-Neptune waterworlds for the first time. On Earth today, organic sulfur compounds produced by marine biota are rapidly destroyed by photochemical processes before they can accumulate to significant levels. Domagal-Goldman et al. suggest that detectable biogenic sulfur signatures could emerge in Archean-like atmospheres with higher biological production or low UV flux. In this study, we explore biogenic sulfur across a wide range of biological fluxes and stellar UV environments. Critically, the main photochemical sinks are absent on the nightside of tidally locked planets. To address this, we further perform experiments with a 3D general circulation model and a 2D photochemical model (VULCAN 2D) to simulate the global distribution of biogenic gases to investigate their terminator concentrations as seen via transmission spectroscopy. Our models indicate that biogenic sulfur gases can rise to potentially detectable levels on hydrogen-rich water worlds, but only for enhanced global biosulfur flux (20 times modern Earth’s flux). We find that it is challenging to identify DMS at 3.4 μm where it strongly overlaps with CH4, whereas it is more plausible to detect DMS and companion byproducts, ethylene (C2H4) and ethane (C2H6), in the mid-infrared between 9 and 13 μm. Unified Astronomy Thesaurus concepts: Exoplanet atmospheres (487); Exoplanet

Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

Wepresent Atacama Large Millimeter/submillimeter Array 12-m, 7-m, and Total Power Array observations of the FUOrionis outbursting system, covering spatial scales ranging from 160 to 25,000 au. The high-resolution interferometric data reveal an elongated 12CO(2–1) feature previously observed at lower resolution in 12CO(3–2). Kinematic modeling indicates that this feature can be interpreted as an accretion streamer feeding the binary system. The mass infall rate provided by the streamer is significantly lower than the typical stellar accretion rates (even in quiescent states), suggesting that this streamer alone is not massive enough to sustain the enhanced accretion rates characteristic of the outbursting class prototype. The observed streamer may not be directly linked to the current outburst, but rather a remnant of a previous, more massive streamer that may have contributed enough to the disk mass to render it unstable and trigger the FU Orionis outburst. The new data detect, for the first time, a vast, slow-moving carbon monoxide molecular outflow emerging from this object. To accurately assess the outflow properties (mass, momentum, and kinetic energy), we employ 13CO(2–1) data to correct for optical depth effects. The analysis indicates that the outflow corresponds to swept-up material not associated with the current outburst, similar to the slow molecular outflows observed around other FUor and Class I protostellar objects.

Discovery of an Accretion Streamer and a Slow Wide-angle Outflow around FUOri...

Discovery of an Accretion Streamer and a Slow Wide-angle Outflow around FUOri...

Discovery of an Accretion Streamer and a Slow Wide-angle Outflow around FUOri...

Chemistry is the scientific study of matter, its properties, composition, structure, and the changes it undergoes. It's often divided into various sub-disciplines such as organic chemistry, inorganic chemistry, physical chemistry, analytical chemistry, and biochemistry. Chemistry plays a crucial role in understanding the world around us and has applications in various fields such as medicine, materials science, environmental science, and industry.

Chemistry 4th semester series (krishna).pdf

Chemistry 4th semester series (krishna).pdf

Chemistry 4th semester series (krishna).pdf

Sumit Kumar yadav

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Site Acceptance Test .

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Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

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Botany 4th semester file By Sumit Kumar yadav.pdf

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Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

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(Kpi summer school 2015) theano tutorial part2

1. Theano tutorial part 2 AACIMP 2015 Sergii Gavrylov

2. Overview ● Brief recap ● Multivariate logistic regression ● Multilayer perceptron ● Convolution ● Convolutional neural network ● scan ● Recurrent neural network

3. Brief recap ● Symbolic variables ● Functions ● Shared variables / updates ● Gradients ● Substitution

4. Computational graph X + Z Y ● Code generation ● Symbolic differentiation

5. Multivariate logistic regression 0 1 2 3 softmax(x * W)

6. Multilayer perceptron 0 1 2 3 relu(x * W) softmax(x * W)

7. 1D Convolution

8. 1D Convolution

9. 1D Convolution

10. 1D Convolution

11. 2D Convolution filter =

12. Max pooling cs231n.github.io/convolutional-networks

13. ConvPoolLayer

14. Convolutional NN cs231n.github.io/convolutional-networks deeplearning.net/tutorial/lenet.html

15. Convolutional NN deeplearning.net/tutorial/lenet.html

16. scan (Symbolic loop in theano)

17. Recurrent neural network www.iro.umontreal.ca/~bengioy/dlbook/rnn.html

18. “Vanilla” RNN www.iro.umontreal.ca/~bengioy/dlbook/rnn.html

19. Conclusion ● Theano has a lot of useful building blocks (convolution, scan). ● Theano supports both cpu and gpu backends.