The document summarizes our current understanding of the structure and composition of the Milky Way Galaxy. It describes how observations across the electromagnetic spectrum have revealed that the Milky Way is a spiral galaxy with a disk, bulge, and halo structure, and that it contains around 100 billion stars and 1 trillion solar masses of total mass, most of which is dark matter. Precision measurements have also shown that the center of the Milky Way contains a supermassive black hole around 3 million times the mass of our Sun.
Types of galaxies
You can edit this powerpoint for your own presentation but don't re-upload.
I used hyperlink(especially on images) and alot of animation.
Types of galaxies
You can edit this powerpoint for your own presentation but don't re-upload.
I used hyperlink(especially on images) and alot of animation.
This presentation investigates different asteroid deflection (orbital change) methods and assesses its useability for asteroid mining purposes. Presented at the International Space University, Space Engineering Department, Space Studies Program 2013
Kind of funny - with all the news about Planetary Resources Inc and asteroid mining, here's some notes I made back in 2006 on the topic to talk with some of my colleagues on the subject.
introduction to galaxies in space.
chapter 9 earth and space class.
about the scientist edwin hubble.
and his theories. The study of asstronomy. space study of planets and galaxies.
Astronomy - State of the Art - GalaxiesChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the properties of galaxies are discussed, including supermassive black holes and dark matter.
JMeter webinar - integration with InfluxDB and GrafanaRTTS
Watch this recorded webinar about real-time monitoring of application performance. See how to integrate Apache JMeter, the open-source leader in performance testing, with InfluxDB, the open-source time-series database, and Grafana, the open-source analytics and visualization application.
In this webinar, we will review the benefits of leveraging InfluxDB and Grafana when executing load tests and demonstrate how these tools are used to visualize performance metrics.
Length: 30 minutes
Session Overview
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During this webinar, we will cover the following topics while demonstrating the integrations of JMeter, InfluxDB and Grafana:
- What out-of-the-box solutions are available for real-time monitoring JMeter tests?
- What are the benefits of integrating InfluxDB and Grafana into the load testing stack?
- Which features are provided by Grafana?
- Demonstration of InfluxDB and Grafana using a practice web application
To view the webinar recording, go to:
https://www.rttsweb.com/jmeter-integration-webinar
Neuro-symbolic is not enough, we need neuro-*semantic*Frank van Harmelen
Neuro-symbolic (NeSy) AI is on the rise. However, simply machine learning on just any symbolic structure is not sufficient to really harvest the gains of NeSy. These will only be gained when the symbolic structures have an actual semantics. I give an operational definition of semantics as “predictable inference”.
All of this illustrated with link prediction over knowledge graphs, but the argument is general.
Dev Dives: Train smarter, not harder – active learning and UiPath LLMs for do...UiPathCommunity
💥 Speed, accuracy, and scaling – discover the superpowers of GenAI in action with UiPath Document Understanding and Communications Mining™:
See how to accelerate model training and optimize model performance with active learning
Learn about the latest enhancements to out-of-the-box document processing – with little to no training required
Get an exclusive demo of the new family of UiPath LLMs – GenAI models specialized for processing different types of documents and messages
This is a hands-on session specifically designed for automation developers and AI enthusiasts seeking to enhance their knowledge in leveraging the latest intelligent document processing capabilities offered by UiPath.
Speakers:
👨🏫 Andras Palfi, Senior Product Manager, UiPath
👩🏫 Lenka Dulovicova, Product Program Manager, UiPath
Smart TV Buyer Insights Survey 2024 by 91mobiles.pdf91mobiles
91mobiles recently conducted a Smart TV Buyer Insights Survey in which we asked over 3,000 respondents about the TV they own, aspects they look at on a new TV, and their TV buying preferences.
GraphRAG is All You need? LLM & Knowledge GraphGuy Korland
Guy Korland, CEO and Co-founder of FalkorDB, will review two articles on the integration of language models with knowledge graphs.
1. Unifying Large Language Models and Knowledge Graphs: A Roadmap.
https://arxiv.org/abs/2306.08302
2. Microsoft Research's GraphRAG paper and a review paper on various uses of knowledge graphs:
https://www.microsoft.com/en-us/research/blog/graphrag-unlocking-llm-discovery-on-narrative-private-data/
UiPath Test Automation using UiPath Test Suite series, part 4DianaGray10
Welcome to UiPath Test Automation using UiPath Test Suite series part 4. In this session, we will cover Test Manager overview along with SAP heatmap.
The UiPath Test Manager overview with SAP heatmap webinar offers a concise yet comprehensive exploration of the role of a Test Manager within SAP environments, coupled with the utilization of heatmaps for effective testing strategies.
Participants will gain insights into the responsibilities, challenges, and best practices associated with test management in SAP projects. Additionally, the webinar delves into the significance of heatmaps as a visual aid for identifying testing priorities, areas of risk, and resource allocation within SAP landscapes. Through this session, attendees can expect to enhance their understanding of test management principles while learning practical approaches to optimize testing processes in SAP environments using heatmap visualization techniques
What will you get from this session?
1. Insights into SAP testing best practices
2. Heatmap utilization for testing
3. Optimization of testing processes
4. Demo
Topics covered:
Execution from the test manager
Orchestrator execution result
Defect reporting
SAP heatmap example with demo
Speaker:
Deepak Rai, Automation Practice Lead, Boundaryless Group and UiPath MVP
The Art of the Pitch: WordPress Relationships and SalesLaura Byrne
Clients don’t know what they don’t know. What web solutions are right for them? How does WordPress come into the picture? How do you make sure you understand scope and timeline? What do you do if sometime changes?
All these questions and more will be explored as we talk about matching clients’ needs with what your agency offers without pulling teeth or pulling your hair out. Practical tips, and strategies for successful relationship building that leads to closing the deal.
Essentials of Automations: Optimizing FME Workflows with ParametersSafe Software
Are you looking to streamline your workflows and boost your projects’ efficiency? Do you find yourself searching for ways to add flexibility and control over your FME workflows? If so, you’re in the right place.
Join us for an insightful dive into the world of FME parameters, a critical element in optimizing workflow efficiency. This webinar marks the beginning of our three-part “Essentials of Automation” series. This first webinar is designed to equip you with the knowledge and skills to utilize parameters effectively: enhancing the flexibility, maintainability, and user control of your FME projects.
Here’s what you’ll gain:
- Essentials of FME Parameters: Understand the pivotal role of parameters, including Reader/Writer, Transformer, User, and FME Flow categories. Discover how they are the key to unlocking automation and optimization within your workflows.
- Practical Applications in FME Form: Delve into key user parameter types including choice, connections, and file URLs. Allow users to control how a workflow runs, making your workflows more reusable. Learn to import values and deliver the best user experience for your workflows while enhancing accuracy.
- Optimization Strategies in FME Flow: Explore the creation and strategic deployment of parameters in FME Flow, including the use of deployment and geometry parameters, to maximize workflow efficiency.
- Pro Tips for Success: Gain insights on parameterizing connections and leveraging new features like Conditional Visibility for clarity and simplicity.
We’ll wrap up with a glimpse into future webinars, followed by a Q&A session to address your specific questions surrounding this topic.
Don’t miss this opportunity to elevate your FME expertise and drive your projects to new heights of efficiency.
Builder.ai Founder Sachin Dev Duggal's Strategic Approach to Create an Innova...Ramesh Iyer
In today's fast-changing business world, Companies that adapt and embrace new ideas often need help to keep up with the competition. However, fostering a culture of innovation takes much work. It takes vision, leadership and willingness to take risks in the right proportion. Sachin Dev Duggal, co-founder of Builder.ai, has perfected the art of this balance, creating a company culture where creativity and growth are nurtured at each stage.
Slack (or Teams) Automation for Bonterra Impact Management (fka Social Soluti...Jeffrey Haguewood
Sidekick Solutions uses Bonterra Impact Management (fka Social Solutions Apricot) and automation solutions to integrate data for business workflows.
We believe integration and automation are essential to user experience and the promise of efficient work through technology. Automation is the critical ingredient to realizing that full vision. We develop integration products and services for Bonterra Case Management software to support the deployment of automations for a variety of use cases.
This video focuses on the notifications, alerts, and approval requests using Slack for Bonterra Impact Management. The solutions covered in this webinar can also be deployed for Microsoft Teams.
Interested in deploying notification automations for Bonterra Impact Management? Contact us at sales@sidekicksolutionsllc.com to discuss next steps.
2. The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our Milky Way might look very much like our cosmic neighbor, the Andromeda galaxy
3. The Structure of the Milky Way (1) Disk Nuclear Bulge Halo Sun Globular Clusters
4. The Structure of the Milky Way (2) Galactic Plane Galactic Center The structure is hard to determine because: 1) We are inside 2) Distance measurements are difficult 3) Our view towards the center is obscured by gas and dust
5. First Studies of the Galaxy First attempt to unveil the structure of our Galaxy by William Herschel (1785), based on optical observations The shape of the Milky Way was believed to resemble a grindstone, with the sun close to the center
6. Strategies to Explore the Structure of Our Milky Way I. Select bright objects that you can see throughout the Milky Way and trace their directions and distances II. Observe objects at wavelengths other than visible (to circumvent the problem of optical obscuration), and catalogue their directions and distances III. Trace the orbital velocities of objects in different directions relative to our position
7. Exploring the Galaxy Using Clusters of Stars Two types of star clusters: 1) Open clusters : young clusters of recently formed stars; within the disk of the Galaxy Open clusters h and Persei 2) Globular clusters : old, centrally concentrated clusters of stars; mostly in a halo around the Galaxy Globular Cluster M 19
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9. Locating the Center of the Milky Way Distribution of globular clusters is not centered on the sun… … but on a location which is heavily obscured from direct (visual) observation
10. Infrared View of the Milky Way Interstellar dust (absorbing optical light) emits mostly infrared Near infrared image Infrared emission is not strongly absorbed and provides a clear view throughout the Milky Way Nuclear bulge Galactic Plane
11. A View of Galaxies Similar to Our Milky Way Sombrero Galaxy NGC 2997 We also see gas and dust absorbing light in other galaxies… … and as dark clouds in the spiral arms when we see a galaxy face-on … as dark dust lanes when we see a galaxy edge-on
12. Exploring the Milky Way with Massive Stars and Open Clusters O and B stars are the most massive, most luminous stars (unfortunately, also the shortest-lived ones) => Look for very young clusters or associations containing O and B stars: O/B Associations!
13. Massive Stars and Open Clusters Problem : Many stars in the field of the O/B association do not belong to the association (foreground and background stars) Members of the association have been formed together and move in the same direction Identify members through their similar motion on the sky.
14. Orbital Motion in the Milky Way (1) Disk stars: Nearly circular orbits in the disk of the Galaxy Halo stars: Highly elliptical orbits; randomly oriented
15.
16. Finding Mass from Orbital Velocity M = 11 billion M sun M = 25 billion M sun M = 100 billion M sun M = 400 billion M sun The more mass there is inside the orbit, the faster the sun has to orbit around the Galactic center Combined mass: M = 4 billion M sun
17. The Mass of the Milky Way If all mass were concentrated in the center, the rotation curve would follow a modified version of Kepler’s 3rd law rotation curve = orbital velocity as function of radius
18. The Mass of the Milky Way (2) Total mass in the disk of the Milky Way: Approx. 100 billion solar masses Additional mass in an extended halo: Total: Approx. 1 trillion solar masses Most of the mass is not emitting any radiation: Dark Matter!
19. Metals in Stars Absorption lines almost exclusively from hydrogen: Population II Many absorption lines also from heavier elements (metals): Population I At the time of formation, the gases forming the Milky Way consisted exclusively of hydrogen and helium. Heavier elements (“metals”) were later only produced in stars. => Young stars contain more metals than older stars
20. Stellar Populations Population I: Young stars: metal rich; located in spiral arms and disk Population II: Old stars: metal poor; located in the halo (globular clusters) and nuclear bulge
21. The Abundance of Elements in the Universe Logarithmic Scale All elements heavier than He are very rare. Linear Scale
22.
23. History of the Milky Way The traditional theory: Quasi-spherical gas cloud fragments into smaller pieces, forming the first, metal-poor stars (pop. II); Rotating cloud collapses into a disk-like structure Later populations of stars (pop. I) are restricted to the disk of the Galaxy
24. Changes to the Traditional Theory Ages of stellar populations may pose a problem to the traditional theory of the history of the Milky Way Possible solution: Later accumulation of gas, possibly due to mergers with smaller galaxies Recently discovered ring of stars around the Milky Way may be the remnant of such a merger
25. O and B Associations O and B Associations Distances to O and B associations determined using cepheid variables O and B Associations trace out 3 spiral arms near the Sun Sagittarius arm Orion-Cygnus arm Perseus arm Sun
26. Radio View of the Milky Way Radio map at a wavelength of 21 cm, tracing neutral hydrogen Interstellar dust does not absorb radio waves We can observe any direction throughout the Milky Way at radio waves
27. Radio Observations (2) 21-cm radio observations reveal the distribution of neutral hydrogen throughout the galaxy Distances to hydrogen clouds determined through radial-velocity measurements (Doppler effect!) Galactic Center Sun Neutral hydrogen concentrated in spiral arms
28. Tracing Molecular Clouds Radio emission of the CO molecule can be used to trace the distribution of molecular clouds In some directions, many molecular clouds overlap Clouds can be disentangled using velocity information Molecular Clouds are concentrated along spiral arms
29. Structure of the Milky Way Revealed Distribution of dust Sun Ring Bar Distribution of stars and neutral hydrogen
30. Star Formation in Spiral Arms Shock waves from supernovae, ionization fronts initiated by O and B stars, and shock fronts forming spiral arms help trigger star formation (Spiral arms are quasi-stationary shock waves)
31. Star Formation in Spiral Arms (2) Spiral arms are basically stationary shock waves Stars and gas clouds orbit around the Galactic center and cross spiral arms Dense gas and shocks induce star formation Star formation self-regulating through O and B ionization fronts and supernova shock waves
32. The Nature of Spiral Arms Chance coincidence of small spiral galaxy in front of a large background galaxy Spiral arms appear bright (newly formed, massive stars!) against the dark sky background… but dark (gas and dust in dense, star-forming clouds) against the bright background of the large galaxy
33. Grand-Design Spiral Galaxies Grand-Design Spirals have two dominant spiral arms M 100 Flocculent (woolly) galaxies also have spiral patterns, but no dominant pair of spiral arms NGC 300
34. Self-Sustained Star Formation in Spiral Arms Star forming regions get elongated due to differential rotation Star formation is self-sustaining due to ionization fronts and supernova shocks
35. The Whirlpool Galaxy Grand-design galaxy M 51 (Whirlpool Galaxy) Self-sustaining star forming regions along spiral arm patterns are clearly visible
36. The Galactic Center (1) Wide-angle optical view of the GC region Galactic center Our view (in visible light) towards the galactic center (GC) is heavily obscured by gas and dust Extinction by 30 magnitudes Only 1 out of 10 12 optical photons makes its way from the GC towards Earth!
37. Radio View of the Galactic Center Many supernova remnants; shells and filaments Sgr A Arc Sgr A*: The center of our galaxy The galactic center contains a supermassive black hole of approx. 3 million solar masses Sgr A
38. A Black Hole at the Center of Our Galaxy By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to ~ 3 million solar masses
39. X-ray View of the Galactic Center Chandra X-ray image of Sgr A* Supermassive black hole in the galactic center is unusually faint in X-rays, compared to those in other galaxies Galactic center region contains many black-hole and neutron-star X-ray binaries