Photometric Analysis with TAOS Zipper Mode Data Wang, Tanya T.-Y. Supervisor : King, Sun-Kun.

Slides:

Advertisements

Similar presentations

Video cameras and photometry Dave Herald. Background Occultations are usually step events When video introduced, it overcame issues of Personal Equation,

Advertisements

Enabling Outreach with Virtual Observatories Mark Voit – NVO Outreach Coordinator.

Volumes – The Disk Method Lesson 7.2. Revolving a Function Consider a function f(x) on the interval [a, b] Now consider revolving that segment of curve.

Taiwan America Occultation Survey TAOS 2002/8/28 TAOS photometry using IRAF Shao-Er Chuang Department of Earth sciences, National Taiwan Normal University,

Analysis of chip with 100 events, July 2001 Variation in pixel to pixel average ADC values (fixed pattern noise) Pixel ADC value event to event repeatability.

Forward-Backward Correlation for Template-Based Tracking Xiao Wang ECE Dept. Clemson University.

Different Tracking Techniques  1.Gaussian Mixture Model:  1.Construct the model of the Background.  2.Given sequence of background images find the.

Rectangular Coordinate System

Tracking Features with Large Motion. Abstract Problem: When frame-to-frame motion is too large, KLT feature tracker does not work. Solution: Estimate.

Objective of Computer Vision

Multimedia Data Introduction to Image Data Dr Mike Spann Electronic, Electrical and Computer Engineering.

Copyright 2002, Pearson Education Canada1 How to Read and Understand Graphs Appendix to Chapter 1.

Control & Robotics Lab  Presented By: Yishai Eilat & Arnon Sattinger  Instructor: Shie Mannor Project Presentation.

PSF Reconstruction: Part I The PSF “Core” Primary Goal: Derive PSFs for point source detection and PSF fitting photometry. Secondary Goal: Derive PSFs.

Astro-DISC: Astronomy and cosmology applications of distributed super computing.

The Coordinate Plane coordinate plane In coordinate Geometry, grid paper is used to locate points. The plane of the grid is called the coordinate plane.

Can people meet from 2:40 to 3:30 on Tuesday, September 5?

EE392J Final Project, March 20, Multiple Camera Object Tracking Helmy Eltoukhy and Khaled Salama.

Objective The student will be able to: graph ordered pairs on a coordinate plane.

Introduction to Graphing Foundations of Algebra. In the beginning of the year, I created a seating chart for your class. I created 5 rows of desks with.

Do Now: #10 on p.391 Cross section width: Cross section area: Volume:

Warm-Up Graph the point (2, -3) If

Naoyuki Tamura (University of Durham) Expected Performance of FMOS ~ Estimation with Spectrum Simulator ~ Introduction of simulators  Examples of calculations.

Geometry 1-6 Midpoint and Distance. Vocabulary Coordinate Plane- a plane divided into four regions by a horizontal line (x-axis) and a vertical line (y-axis).

Sullivan PreCalculus Section 3.2 Polynomial Functions

Motion in 1 Dimension Physics: Chapter 2-1 Pages

Graphing Equations of Lines Using x- and y-Intercepts.

Reflections Section 9.3.

Month Rent Revenue 0 $400.00$ $410.00$ $420.00$

Sec 1.5 Scatter Plots and Least Squares Lines Come in & plot your height (x-axis) and shoe size (y-axis) on the graph. Add your coordinate point to the.

Padova-Asiago Supernova Group (

Conventional Graphing Techniques 2. Use a pencil. 1. Use graph paper. 3. Use a straightedge.

Graphing With Coordinates

Graphing. 2. Coordinate Plane 3. Grid 4. Lattice Points 1. Number Line.

An x-intercept of a graph is the x- coordinate of a point where the graph crosses the x-axis. An y-intercept of a graph is the y- coordinate of a point.

Measuring Sky Brightness with a Digital Camera Paris 2004.

Multimedia Data Introduction to Image Data Dr Sandra I. Woolley Electronic, Electrical and Computer.

The Taiwanese-American Occultation Survey (TAOS) Matthew Lehner ASIAA.

MOS Data Reduction Michael Balogh University of Durham.

What can we see in the sky?. IN THE SKY WE CAN SEE MUCH MORE!

Hybrid Dual Energy (HDE) Fluoroscopy for Real-Time Tracking of Lung Tumors JC Roeske PhD, R Patel PhD, M Campana BS, J Panfil BS, M Surucu PhD, AM Block.

The good students will take copious notes.

MMT Observation Database for Light Curve Analysis Vladimir Agapov Presentation for the WG1 session 33rd IADC meeting, Houston.

4.2 Polynomial Functions and Models. A polynomial function is a function of the form.

Chapter 3.3 – 3.5 Linear Equations and slope Alg. 2 Notes Name:__________________ Date:________________.

Spotting the life of stars „Pi of the Sky” Project Katarzyna Kwiecińska UKSW-SNŚ on behalf of the Pi of the Sky collaboration.

The Coordinate Plane 101 ALGEBRA 11/16/15. The coordinate plane is a set of axis on which ordered pairs of input and output values can be plotted.

Quit Introduction Reflection in a Line Two Axial Symmetries Reflection in a Point.

Volume: The Disk Method. Some examples of solids of revolution:

Observations with AMBER  General overview  P2VM  OB preparation with P2PP P2PP / OB / templates Available templates for observation procedure Typical.

The Coordinate Plane SWBAT identify the four quadrants; identify and graph points in all four quadrants.

STROUD Worked examples and exercises are in the text Programme 20: Integration applications 2 INTEGRATION APPLICATIONS 2 PROGRAMME 20.

Volume Find the area of a random cross section, then integrate it.

Redshifts and optical identification of a sample of scintillating flat spectrum radio sources.

Algebra Review Objective: Students will be able to demonstrate their ability to plot points on the Cartesian coordinate system.

In conclusion the intensity level of the CCD is linear up to the saturation limit, but there is a spilling of charges well before the saturation if.

GSPC -II Program GOAL: extend GSPC-I photometry to B = V ˜ 20 add R band to calibrate red second-epoch surveys HOW: take B,V,R CCD exposures centered at.

Welcome back eager young artists! Ms. Edelman Tuesday, June 21, 2016 DO NOW:  Download and open eraser.ppt from the lessons folder in Dropbox.  Take.

4.1 NOTES. x-Axis – The horizontal line on the coordinate plane where y=0. y-Axis – The vertical line on the coordinate plane where x=0.

The First Release of AST3 point source catalog from Dome A, Antarctica in 2012 MA Bin, WEI Peng, SHANG Zhaohui, LIU Qiang, HU Yi (NAOC) 973 课题二

Ordered Pairs Objective:Find how to graph ordered pairs.

M11.E Draw, find and/or write an equation for a line of best fit for a scatter plot.

Find the equation of the tangent line to the curve y = 1 / x that is parallel to the secant line which runs through the points on the curve with x - coordinates.

A Forest of Sensors: Tracking

Basics of Photometry.

Announcements HR Diagram lab will be extended for one week. I’ll talk about it today. Homework: Chapter 9 # 1, 2 & 3 Next week is a Dark Sky Night. If.

Karen Meech Institute for Astronomy TOPS 2003

Non-numeric Data Representation

Modern Observational/Instrumentation Techniques Astronomy 500

The Image The pixels in the image The mask The resulting image 255 X

Presentation transcript:

Photometric Analysis with TAOS Zipper Mode Data Wang, Tanya T.-Y. Supervisor : King, Sun-Kun

TAOS Part 1 － Zipper-Mode image row block 2048*32pixel Our real image 2048*2048 Time interval : 0.3 sec Steady state 2048*7200 pixel

Part 2 － Dealing with the Data ( IDL ) Setup the file of each star which includes the information of it’s coordinates and magnitude in our interesting region of sky. Whole zipper-mode image row blocks. Use Source Extractor to determine the magnitudes of stars in all row blocks. Use sky-list to collate the coordinates of stars in each row block and put the same coordinates of stars into a file. TAOS

Find special data point in our star files Standard deviation. curve(ΔX, ΔY, magnitude) ： x-axis is the time sequence which means the same star in different time and y-axis is the value of Δx (x-mx), Δy (y-my), magnitude. TAOS MAGNITUDEMAGNITUDE MAGNITUDEMAGNITUDE

TAOS Zipper-mode imageRow blocks Using Source Extractor Get a file including x, y and magnitudes of all stars in a row block. x y mag Star_1 Star_2 Star_3 Star_n row x y mag n File of star_5 Curve of x, y, mag

Part 3 － example _zipperc_a020.fit Starc20_52 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a020.fit Starc20_60 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a020.fit Starc20_155 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a020.fit Starc20_186 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a020.fit Starc20_231 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a020.fit Starc20_239 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a025.fit Starc25_30 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a025.fit Starc25_190 TAOS ΔX ΔY M A G N I T U D E

010719_zipperc_a030.fit Starc30_36 TAOS ΔX ΔY M A G N I T U D E

Four zipper-mode images TAOS Total star Possible Data point _zipperc_a020192* _zipperc_a021178* _zipperc_a025190* _zipperc_a030192*951

Part 4 － Future Use another tool to determine the magnitude. Eliminate background from our image – black frame. Calibration Improve the ability of tracking. 2-D cross correlation An photometric analysis program in real-time. TAOS