Measurement Tutorial. Open the opaque filter image it s called (Dark-B FITS) in MicroObservatory Image.
|
|
|
- Buddy Doyle
- 5 years ago
- Views:
Transcription
1 Measurement Tutorial Now that you ve mastered finding stars in the pattern matching game, here s a new challenge. How accurate are you at measuring the brightness of a star? Test your ability against members of the Center for Astrophysics. Good luck. Using the attached image of HATP-10, you ll measure the brightness of the target star, two comparison stars and two dark areas of the sky to get the most accurate reading. Step 1. Subtracting out excess light Open the opaque filter image it s called (Dark-B FITS) in MicroObservatory Image. Open the FITS image of HATP-10 in MicroObservatory Image. Under Process in the drop down menu select Image Calculator. Subtract the opaque image from HATP-10 and hit ok. A third untitled image will be created. This is the image you will use for your measurements.
2 Why am I doing this? Light pixels that are simply noise associated with the telescope hardware have been subtracted from the image. Step 2. Adjust the image Under the Process menu, select Adjust Image. In the small window that opens, select Auto.
3 Why am I doing this? Adjusting the image will make the stars in your image easier to see.
4 Step 3 Locate HATP-10 and two comparison stars on this image using the star chart. Step 3 Measuring the brightness of a star Click on the magnifying glass icon at the top left of the image. Move the cursor so it is centered between HATP-10 and the two reference stars noted on the star chart. Click several times to enlarge the image. HATP-10 and its two reference stars should remain in the field of view.
5 Click on the circle icon at the top of the image. Move the cursor so it is near HATP-10 and drag it to make a circle that is 4.5in in radius. This radius should be used for all measurements! Adjust the location of the circle so it completely encircles the pixels of light associated with HATP-10. You can move the circle by dragging it or by using the i, j, k, and l keys (i=up, j=left, k=down, l=right).
6 Hold down the command/apple m on Macs and control m on PCs. A table is created at the top of the image with the brightness measurement. Step 4 Measuring the brightness of comparison stars
7 Drag the circle to the first companion star, moving in a clockwise direction. Position the circle and take another image. Repeat for the second comparison star.
8 Why am I doing this? Lots of things in nature can cause a star s brightness to appear to dim (for example clouds drifting across the telescope view). These natural occurrences should have the same effect on all of the stars in our field of view. If we assume that the comparison stars don t normally change in brightness due to transiting planets, we can compare the brightness of HATP-10 to the comparison stars. Step 5 Measuring the brightness of background sky Repeat step 4 for two background locations. Select locations that are not on top of any stars. Why am I doing this? The sky between the stars is not completely black. When you measure a star s brightness, you re actually measuring the brightness of the star plus the background sky. These background sky measurements will be subtracted. All of the images taken in step 4 and 5 will be added to your table. What does all of the information in the table mean?
9 Area = the total number of pixels in your circle Mean= the average value for each of the pixels in your circle Total= the total brightness of the star (or background) Min= Max= Step 6 - Calculating the actual brightness of a star (the numbers you ll use to are the brightness measurements from column 4 Total) a. Find the average background sky. First, find the average brightness of the background sky (add the two background measurements and divide by two. ( )/2 = 1753 b. Find the corrected brightness for each star. Subtract this average background measurement from each of the three brightness measurements (HATP-10 and the two comparison stars) = = = 3458 c. Calculate the average correct brightness of the two comparison stars. Add the two corrected brightnesses and divide by 2. ( )/2 = 3600 Compare the brightness of HATP-10 with the average of the comparison stars by taking the ratio of the corrected HATP-10 brightness/average corrected comparison star brightness What s your final measurement? Compare your number to classmates and to the staff at CfA. Now try this image of COROT2 and compare your results with ours! Our results: CoRoT FITS Set Set Set Set Set How did you do?
10
Relative Photometry with data from the Peter van de Kamp Observatory D. Cohen and E. Jensen (v.1.0 October 19, 2014)
Relative Photometry with data from the Peter van de Kamp Observatory D. Cohen and E. Jensen (v.1.0 October 19, 2014) Context This document assumes familiarity with Image reduction and analysis at the Peter
Assignment #0 Using Stellarium
Name: Class: Date: Assignment #0 Using Stellarium The purpose of this exercise is to familiarize yourself with the Stellarium program and its many capabilities and features. Stellarium is a visually beautiful
DATA LAB. Data Lab Page 1
NOTE: This DataLab Activity Guide will be updated soon to reflect April 2015 changes DATA LAB PURPOSE. In this lab, students analyze and interpret quantitative features of their brightness graph to determine
LAB: Photometry of the Pleiades Cluster
LAB: Photometry of the Pleiades Cluster ASTR 203 - Instructors Olszewski & Rigby Due IN CLASS on Oct. 30 You may work with 1 partner. If you do, only turn in 1 assignment with both your names on it! You
This is the third of 3 parts detailing my experience of auto guiding for astrophotography.
AstronomyShed Tutorials Autoguiding - Part 3 - Using you autoguiding setup This is the third of 3 parts detailing my experience of auto guiding for astrophotography. Prerequisites In writing this article
Can we communicate with an alien star system?
EXPLORATION 5: TO THE STARS! Can we communicate with an alien star system? The challenge R ecently, astronomers have discovered more than 100 stars, in addition to our own Sun, that are orbited by planets!
Photometry with Iris Photometry with Iris
Author: Daniel Duggan & Sarah Roberts - Faulkes Telescope Project Introduction Photometry is the measurement of the intensity or brightness of an astronomical object, such as a star or galaxy by adding
AstroBITS: Open Cluster Project
AstroBITS: Open Cluster Project I. Introduction The observational data that astronomers have gathered over many years indicate that all stars form in clusters. In a cloud of hydrogen gas, laced with helium
Lecture 8. October 25, 2017 Lab 5
Lecture 8 October 25, 2017 Lab 5 News Lab 2 & 3 Handed back next week (I hope). Lab 4 Due today Lab 5 (Transiting Exoplanets) Handed out and observing will start Friday. Due November 8 (or later) Stellar
Photoelectric Photometry of the Pleiades Student Manual
Name: Lab Partner: Photoelectric Photometry of the Pleiades Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Edited by Lucy Kulbago, John Carroll University 11/24/2008
CLEA/VIREO PHOTOMETRY OF THE PLEIADES
CLEA/VIREO PHOTOMETRY OF THE PLEIADES Starting up the program The computer program you will use is a realistic simulation of a UBV photometer attached to a small (diameter=0.4 meters) research telescope.
Photometry of Supernovae with Makali i
Photometry of Supernovae with Makali i How to perform photometry specifically on supernovae targets using the free image processing software, Makali i This worksheet describes how to use photometry to
RETROGRADE MOTION AND PLANETARY ORBITS Computer Simulations
RETROGRADE MOTION AND PLANETARY ORBITS Computer Simulations OBJECTIVE: To see planetary orbits simulated on a computer and to see how this suncentered model explains retrograde motion. Initial Procedure:
Open Cluster Research Project
Open Cluster Research Project I. Introduction The observational data indicate that all stars form in clusters. In a cloud of hydrogen gas, laced with helium and a trace of other elements, something triggers
Polar alignment in 5 steps based on the Sánchez Valente method
1 Polar alignment in 5 steps based on the Sánchez Valente method Compared to the drift alignment method, this one, allows you to easily achieve a perfect polar alignment in just one step. By "perfect polar
Students will explore Stellarium, an open-source planetarium and astronomical visualization software.
page 22 STELLARIUM* OBJECTIVE: Students will explore, an open-source planetarium and astronomical visualization software. BACKGROUND & ACKNOWLEDGEMENTS This lab was generously provided by the Red Rocks
Tutorial 8 Raster Data Analysis
Objectives Tutorial 8 Raster Data Analysis This tutorial is designed to introduce you to a basic set of raster-based analyses including: 1. Displaying Digital Elevation Model (DEM) 2. Slope calculations
Star Cluster Photometry and the H-R Diagram
Star Cluster Photometry and the H-R Diagram Contents Introduction Star Cluster Photometry... 1 Downloads... 1 Part 1: Measuring Star Magnitudes... 2 Part 2: Plotting the Stars on a Colour-Magnitude (H-R)
Photoelectric Photometry of the Pleiades Student Manual
Photoelectric Photometry of the Pleiades Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Document SM 2: Version 1.1.1 lab Department of Physics Gettysburg College
Life Cycle of Stars. Photometry of star clusters with SalsaJ. Authors: Daniel Duggan & Sarah Roberts
Photometry of star clusters with SalsaJ Authors: Daniel Duggan & Sarah Roberts Photometry of star clusters with SalsaJ Introduction Photometry is the measurement of the intensity or brightness of an astronomical
CHARTING THE HEAVENS USING A VIRTUAL PLANETARIUM
Name Partner(s) Section Date CHARTING THE HEAVENS USING A VIRTUAL PLANETARIUM You have had the opportunity to look at two different tools to display the night sky, the celestial sphere and the star chart.
Planet Club. Version AUG-2005
Planet Club Raleigh Astronomy Club Version 1.2 05-AUG-2005 Introduction Welcome to the RAC Planet Club! This is one of the entry-level observing clubs, but still has some challenges for more advanced observers.
Okay now go back to your pyraf window
PHYS 391 Astronomical Image Data: Measuring the Distance and Age of a Stellar Cluster Goals This lab is designed to demonstrate basic astronomy data analysis and how extracting stellar population information
HOMEWORK 4: H-R DIAGRAM
NAME(S) SECTION DAY/TIME ASTRONOMY25 (LLOYD) SPRING 2012 Purpose HOMEWORK 4: H-R DIAGRAM To plot the H-R diagram of a star cluster and estimate its age and distance. Background Magnitude is a measure of
Astronomy 101 Lab: Stellarium Tutorial
Name: Astronomy 101 Lab: Stellarium Tutorial Please install the Stellarium software on your computer using the instructions in the procedure. If you own a laptop, please bring it to class. You will submit
Extrasolar planets. Lecture 23, 4/22/14
Extrasolar planets Lecture 23, 4/22/14 Extrasolar planets Extrasolar planets: planets around other stars Also called exoplanets 1783 exoplanets discovered as of 4/21/14 Orbitting 1105 different stars Number
PHYS133 Lab 7 The HR Diagram
PHYS133 Lab 7 Goals: Measure brightness of various stars in the Pleiades star cluster in two different wavelength bands. Create an HR diagram based on the data taken. Use the distance modulus to determine
Objectives: (a) To understand how to display a spectral image both as an image and graphically.
Texas Tech University Department of Physics & Astronomy Astronomy 2401 Observational Astronomy Lab 8:- CCD Image Analysis:- Spectroscopy Objectives: There are two principle objectives for this laboratory
Zeeman Effect Physics 481
Zeeman Effect Introduction You are familiar with Atomic Spectra, especially the H- atom energy spectrum. Atoms emit or absorb energies in packets, or quanta which are photons. The orbital motion of electrons
Starry Night Version 5.7 Features What s new and how to use them!
Starry Night Version 5.7 Features What s new and how to use them! New Features Overview 1. Space Missions (Probe Paths) 2. 3-D Object Models 3. Advanced Telescope Control panel 4. Google Maps Integration
Observing Asteroids. Finding Asteroids using the Asteroid Portal NEA Planner. Author: Daniel Duggan
Finding Asteroids using the Asteroid Portal NEA Planner Author: Daniel Duggan - Faulkes Telescope Project Finding Asteroids using the Asteroid Portal NEA Planner Finding Asteroids Asteroids are awkward;
Is there life outside of Earth? Activity 2: Moving Stars and Their Planets
Is there life outside of Earth? Activity 2: Moving Stars and Their Planets Overview In this activity, students are introduced to the wobble-method (officially known as the radial velocity method) of detecting
Hubble's Law and the Age of the Universe
Hubble's Law and the Age of the Universe Procedure: Name: 1. Login into the network using your user ID and your password. 2. Double click on the Astronomy shortcuts folder on the desktop. 3. Double click
2: SIMPLE HARMONIC MOTION
2: SIMPLE HARMONIC MOTION Motion of a Mass Hanging from a Spring If you hang a mass from a spring, stretch it slightly, and let go, the mass will go up and down over and over again. That is, you will get
Interacting Galaxies
Interacting Galaxies Contents Introduction... 1 Downloads... 1 Selecting Interacting Galaxies to Observe... 2 Measuring the sizes of the Galaxies... 5 Making a Colour Image in IRIS... 8 External Resources...
Instruction Manual. Model #: (Reflector) Lit #: / 06-07
Instruction Manual Model #: 49114500 (Reflector) Model #: 49060700 () Model #: 49070800 () Lit #: 93-0468 / 06-07 PARTS DIAGRAM C E D B A F G H I J NOTE: Actual product may have improvements that are not
Astron 104 Laboratory #4 Orbital Motion of a Planet
Name: Date: Section: Astron 104 Laboratory #4 Orbital Motion of a Planet Introduction The nature of the Solar System was first derived from careful measurements of the positions of the planets in the night
Create Satellite Image, Draw Maps
Create Satellite Image, Draw Maps 1. The goal Using Google Earth, we want to create and import a background file into our Adviser program. From there, we will be creating paddock boundaries. The accuracy
PROJECT GLOBULAR CLUSTERS
PROJECT 5 GLOBULAR CLUSTERS Objective: The objective of this exercise is the calculation of the core and tidal radius of a globular cluster in the Milky Way. Measure the tidal radius of a globular cluster
Color-Magnitude Diagram Lab Manual
Color-Magnitude Diagram Lab Manual Due Oct. 21, 2011 1 Pre-Lab 1.1 Photometry and the Magnitude Scale The brightness of stars is represented by its value on the magnitude scale. The ancient Greek astronomer
Astron 104 Laboratory #5 The Size of the Solar System
Name: Date: Section: Astron 104 Laboratory #5 The Size of the Solar System Section 1.3 In this exercise, we will use actual images of the planet Venus passing in front of the Sun (known as a transit of
Gravity: How fast do objects fall? Teacher Advanced Version (Grade Level: 8 12)
Gravity: How fast do objects fall? Teacher Advanced Version (Grade Level: 8 12) *** Experiment with Audacity and Excel to be sure you know how to do what s needed for the lab*** Kinematics is the study
Introduction: Objectives: (a) To understand how to compile a list of objects for imaging with a CCD.
Texas Tech University Department of Physics Astronomy 2401 Observational Astronomy Lab 2:- Planning Observations Introduction: Observing time at the telescope is generally very limited. Therefore, in order
Operating the Celestron 14 Telescope
Operating the Celestron 14 Telescope 1. The Telescope and Its Controls The Celestron 14-inch telescope is located in the east bay of the observatory (Fig. 1). It is a Schmidt-Cassegrain type instrument;
2: SIMPLE HARMONIC MOTION
2: SIMPLE HARMONIC MOTION Motion of a mass hanging from a spring If you hang a mass from a spring, stretch it slightly, and let go, the mass will go up and down over and over again. That is, you will get
Exercises for Windows
Exercises for Windows CAChe User Interface for Windows Select tool Application window Document window (workspace) Style bar Tool palette Select entire molecule Select Similar Group Select Atom tool Rotate
Photoelectric Photometry of the Pleiades
Photoelectric Photometry of the Pleiades Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Document SM 2: Version 1 Department of Physics Gettysburg College Gettysburg,
UNIVERSITY COLLEGE LONDON. Measuring a Stellar Spectrum
University Of London Observatory 1 Introduction UNIVERSITY COLLEGE LONDON Measuring a Stellar Spectrum 1B30 Practical Astronomy 1B13 Frontiers of Astronomy The primary way astronomers find out about physical
Astron 104 Laboratory #9 Cepheid Variable Stars
Name: ate: Section: stron 104 Laboratory #9 Variable Stars Section 14.2 To determine the distances to most stars, we often use the relationship among the following three quantities: The apparent of the
Photoelectric Photometry of the Pleiades
Photoelectric Photometry of the Pleiades Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Document SM 2: Version 0.96lab Department of Physics Gettysburg College
Large Scale Structure of the Universe Lab
Large Scale Structure of the Universe Lab Introduction: Since the mid-1980 s astronomers have gathered data allowing, for the first time, a view of the structure of the Universe in three-dimensions. You
Making an H-R diagram Earth & Sky
Making an H-R diagram Earth & Sky Name: Introduction Astronomers have discovered relationships between the surface temperatures and luminosities (brightnesses) of stars. These relationships are often presented
Experiment 1: The Same or Not The Same?
Experiment 1: The Same or Not The Same? Learning Goals After you finish this lab, you will be able to: 1. Use Logger Pro to collect data and calculate statistics (mean and standard deviation). 2. Explain
SkyGlobe Planetarium
SkyGlobe Planetarium Introduction: This exercise will simulate the night sky and demonstrate a number of principles of the celestial sphere and the motions of the Earth and planets. Getting Started: 1.
The Revolution of the Moons of Jupiter
The Revolution of the Moons of Jupiter Overview: During this lab session you will make use of a CLEA (Contemporary Laboratory Experiences in Astronomy) computer program generously developed and supplied
PHYS133 Lab 4 The Revolution of the Moons of Jupiter
PHYS133 Lab 4 Goals: Use a simulated remotely controlled telescope to observe iter and the position of its four largest moons. Plot their positions relative to the planet vs. time and fit a curve to them
IN REPORT: Plate Scale and FOV of CCD for Each Telescope using Albireo Stars
USE ASTROIMAGEJ NOT AIP4WIN To download ALL the public data from Canvas, go to Files, then click the 3 dots next to the Public Data Folder and click Download. It will download all the files at once. 6.1
Lecture 9. November 1, 2018 Lab 5 Analysis
Lecture 9 November 1, 2018 Lab 5 Analysis News Lab 2 Handed back with solution; mean: 92.1, std dev: 5.5 Lab 3 Handed back next week (I hope). Lab 4 Due November 1 (today) News Lab 5 (Transiting Exoplanets)
Experiment 10. Zeeman Effect. Introduction. Zeeman Effect Physics 244
Experiment 10 Zeeman Effect Introduction You are familiar with Atomic Spectra, especially the H-atom energy spectrum. Atoms emit or absorb energies in packets, or quanta which are photons. The orbital
Comparing Ultraviolet and Infrared Star Formation Tracers
Comparing Ultraviolet and Infrared Star Formation Tracers George J. Bendo and Rebecca Freestone Jodrell Bank Centre for Astrophysics, The University of Manchester 15 February 2018 Overview The DS9 image
Observing Night 1 DON T FORGET TO KEEP NOTES ON YOUR PROCEDURE AND KEEP AN OBSERVING LOG FOR THE NIGHT!!!!!
Observing Night 1 Objects : Name RA (2000) Dec V B-V V-R R-I MK source HD 5015 00 53 04 +61 07 26 5.34 0.54 0.48 0.30 F9V Ducati 2002 HD 30197 4 46 17 +18 44.1 6.01 1.21 0.620 0.533 K4III J66/T86 HD 7615
The Hertzsprung-Russell Diagram
Introduction + Aims Installing the Software Theory of Hertzsprung-Russell Diagrams Method: Part 1 - Distance to the Star Cluster Part 2 - Age of the Star Cluster Part 3 - Comparison of Star Clusters Extension
Photometry of Messier 34
Photometry of Messier 34 J. Kielkopf November 12, 2012 1 Messier 34 The open cluster Messier 34 (M34) is in the solar neighborhood, lying roughly in the plane of the Milky Way galaxy in the direction of
The Sun s center is much hotter than the surface. The Sun looks large and bright in the sky. Other stars look much smaller.
The Sun A star is a huge ball of hot, glowing gases. The Sun is a star. The width of the Sun is equal to the width of 100 Earths placed side by side. The Sun is extremely hot. The surface of the Sun has
Measuring the Milky Way
Printed: Mar/01/2013 Milky Way Lab Page MW- 13 NAME Name Group NAME Name Date Measuring the Milky Way References B Carroll and D. Ostlie, An Introduction to Modern Astrophysics (Addison-Wesley, 1996),
The Hubble Redshift Distance Relation
The Hubble Redshift Distance Relation Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Document SM 3: Version 1 Department of Physics Gettysburg College Gettysburg,
PoleMaster User Manual (Northern Hemisphere)
PoleMaster User Manual (Northern Hemisphere) 1. Hardware Installation 1.1 Attach the PoleMaster camera unit to the quick install plate using the three bolts supplied. In the case of the AZ EQ5-GT and Mesu
Algebra Review. Finding Zeros (Roots) of Quadratics, Cubics, and Quartics. Kasten, Algebra 2. Algebra Review
Kasten, Algebra 2 Finding Zeros (Roots) of Quadratics, Cubics, and Quartics A zero of a polynomial equation is the value of the independent variable (typically x) that, when plugged-in to the equation,
EXPERIMENT : Work and Energy. Topics of investigation: The relation between force and acceleration
EXPERIMENT 2000031: Work and Energy Topics of investigation: The relation between force and acceleration Read about this topic in: Serway, Ch 7, 8; C&J Ch 6 Toolkit: Computer Laboratory interface & software
EQUATION OF A CIRCLE (CENTRE A, B)
EQUATION OF A CIRCLE (CENTRE A, B) A circle can have different centres as well as different radii. Let s now consider a more general equation for a circle with centre (a, b) and radius r Exercise 1 Consider
The Revolution of the Moons of Jupiter Student Manual
The Revolution of the Moons of Jupiter Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Document SM 1: Circ.Version 1.1.1 Department of Physics Gettysburg College
Math 1241, Spring 2014 Section 3.3. Rates of Change Average vs. Instantaneous Rates
Math 1241, Spring 2014 Section 3.3 Rates of Change Average vs. Instantaneous Rates Average Speed The concept of speed (distance traveled divided by time traveled) is a familiar instance of a rate of change.
SAMPLE PROBLEMS HIGH SCHOOL PRAXIS II. 1. Find the volume of a pyramid having slant height 5 and a base that is a square with side 8.
SAMPLE PROBLEMS HIGH SCHOOL PRAXIS II 1. Find the volume of a pyramid having slant height 5 and a base that is a square with side 8. A. 64 B. 106.67 C. 320 D. 576 2. Approximate the value of (log 3 4)
GRAVITATION. F = GmM R 2
GRAVITATION Name: Partner: Section: Date: PURPOSE: To explore the gravitational force and Kepler s Laws of Planetary motion. INTRODUCTION: Newton s law of Universal Gravitation tells us that the gravitational
PHY 111L Activity 2 Introduction to Kinematics
PHY 111L Activity 2 Introduction to Kinematics Name: Section: ID #: Date: Lab Partners: TA initials: Objectives 1. Introduce the relationship between position, velocity, and acceleration 2. Investigate
Introduction to Astronomy Laboratory Exercise #1. Intro to the Sky
Introduction to Astronomy Laboratory Exercise #1 Partners Intro to the Sky Date Section Purpose: To develop familiarity with the daytime and nighttime sky through the use of Stellarium. Equipment: Computer
Asteroid Investigation
Asteroid Investigation Contents Introduction... 1 Downloads... 1 Selecting an Asteroid to Observe... 2 Finding the Asteroid... 5 Obtaining an Accurate Position... 6 Stacking Images to show the path of
How to use your astronomical telescope for the first time.
How to use your astronomical telescope for the first time. A quick guide to setting up and using your telescope for the first time. There are 10 pages in this section which cover a variety of topics to
Student Exploration: H-R Diagram
Name: Date: Student Exploration: H-R Diagram Vocabulary: giant, H-R diagram, luminosity, main sequence, star, supergiant, white dwarf Prior Knowledge Questions (Do these BEFORE using the Gizmo.) 1. The
NMR Assignments using NMRView II: Sequential Assignments
NMR Assignments using NMRView II: Sequential Assignments DO THE FOLLOWING, IF YOU HAVE NOT ALREADY DONE SO: For Mac OS X, you should have a subdirectory nmrview. At UGA this is /Users/bcmb8190/nmrview.
Overview Objectives Materials Background Activity Procedure
Overview In this activity, students will explore how to determine how to assemble information about plant distributions, and relate those distributional to the environment by assembling information on
Using Microsoft Excel
Using Microsoft Excel Objective: Students will gain familiarity with using Excel to record data, display data properly, use built-in formulae to do calculations, and plot and fit data with linear functions.
Astro 3 Lab Exercise
Astro 3 Lab Exercise Lab #4: Measuring Redshifts of Galaxies Dates: August 5 6 Lab Report due: 5 pm Friday August 15 Summer 2014 1 Introduction This project involves measuring the redshifts of distant
An eclipse is when light from a moon or sun gets blocked. People can see two kinds of eclipses from Earth.
What is an eclipse? By NASA, adapted by Newsela staff on 07.17.17 Word Count 584 Level 570L This image of the moon crossing in front of the sun was captured on January 30, 2014, by NASA's Solar Dynamics
BUILDING BASICS WITH HYPERCHEM LITE
BUILDING BASICS WITH HYPERCHEM LITE LAB MOD1.COMP From Gannon University SIM INTRODUCTION A chemical bond is a link between atoms resulting from the mutual attraction of their nuclei for electrons. There
Tutorial 12 Excess Pore Pressure (B-bar method) Undrained loading (B-bar method) Initial pore pressure Excess pore pressure
Tutorial 12 Excess Pore Pressure (B-bar method) Undrained loading (B-bar method) Initial pore pressure Excess pore pressure Introduction This tutorial will demonstrate the Excess Pore Pressure (Undrained
BOND LENGTH WITH HYPERCHEM LITE
BOND LENGTH WITH HYPERCHEM LITE LAB MOD2.COMP From Gannon University SIM INTRODUCTION The electron cloud surrounding the nucleus of the atom determines the size of the atom. Since this distance is somewhat
EE Power Gain and Amplifier Design 10/31/2017
EE 40458 Power Gain and Amplifier Design 10/31/017 Motivation Brief recap: We ve studied matching networks (several types, how to design them, bandwidth, how they work, etc ) Studied network analysis techniques
THE HAVERFORD UNIVERSITY S STRAWBRIDGE OBSERVATORY S OF THE 16 MEADE. A quick guide to using the 16 Meade Schmidt-Cassegrain Telescope
THE S OF THE 16 MEADE HAVERFORD UNIVERSITY S STRAWBRIDGE OBSERVATORY A quick guide to using the 16 Meade Schmidt-Cassegrain Telescope First draft: Scott Engle, Fall 2010; Update: Steve Boughn, Fall 2012
CONFIRMATION OF A SUPERNOVA IN THE GALAXY NGC6946
CONFIRMATION OF A SUPERNOVA IN THE GALAXY NGC6946 G. Iafrate and M. Ramella INAF - Astronomical Observatory of Trieste 1 Introduction Suddenly a star runs out its nuclear fuel. Its life as a normal star
Lab 2 Astronomical Coordinates, Time, Focal Length, Messier List and Open Clusters
Lab 2 Astronomical Coordinates, Time, Focal Length, Messier List and Open Clusters Name: Partner(s): Boxes contain questions that you are expected to answer (in the box). You will also be asked to put
Polynomial Models Studio Excel 2007 for Windows Instructions
Polynomial Models Studio Excel 2007 for Windows Instructions A. Download the data spreadsheet, open it, and select the tab labeled Murder. This has the FBI Uniform Crime Statistics reports of Murder and
1 GSW Sets of Systems
1 Often, we have to solve a whole series of sets of simultaneous equations of the form y Ax, all of which have the same matrix A, but each of which has a different known vector y, and a different unknown
Name: Lab Partner: Department of Physics Gettysburg College Gettysburg, PA 17325
Name: Lab Partner: The Revolution of the Moons of Jupiter Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Edited by Lucy Kulbago, John Carroll University 11/24/2008
MIS 0855 Data Science (Section 005) Fall 2016 In-Class Exercise (Week 4) Visualizing with Maps
MIS 0855 Data Science (Section 005) Fall 2016 In-Class Exercise (Week 4) Visualizing with Maps Objective: Learn how to use Tableau s powerful mapping tools Learning Outcomes: Learn at what levels (e.g.
Magnetic Fields. Experiment 1. Magnetic Field of a Straight Current-Carrying Conductor
General Physics Lab Department of PHYSICS YONSEI University Lab Manual (Lite) Magnetic Fields Ver.20181029 NOTICE This LITE version of manual includes only experimental procedures for easier reading on
Stellarium Walk-through for First Time Users
Stellarium Walk-through for First Time Users Stellarium is the computer program often demonstrated during our planetarium shows at The MOST, Syracuse s science museum. It is our hope that visitors to our
HR Diagram of Globular Cluster Messier 80 Using Hubble Space Telescope Data
Jason Kendall, William Paterson University, Department of Physics HR Diagram of Globular Cluster Messier 80 Using Hubble Space Telescope Data Background Purpose: HR Diagrams are central to understanding
Solar System Test - Grade 5
Solar System Test - Grade 5 Multiple Choice Directions: Identify the choice that best completes the statement or answers the question. Write this answer on your answer document. 1. The tilt of Earth s
Imaging with the 70AT and the Meade electronic eyepiece CCD imager By Ted Wilbur 2/4/02
Imaging with the 70AT and the Meade electronic eyepiece CCD imager By Ted Wilbur 2/4/02 Background: Follow-up 3/10/02: Process improvements and comments in red - TW I took up the hobby of astronomy in