Testing and fine tuning hands automated photometric pipeline
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Testing and Fine-Tuning HANDS’ Automated Photometric Pipeline. Austin Barnes Oceanit Mentor: Russell Knox Advisors: Rita Cognion and Curt Leonard Home Institution: Harvard University. 2009. Overview. Problem: Space Situational Awareness Solution: Introduction to HANDS

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Testing and Fine-Tuning HANDS’ Automated Photometric Pipeline

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Testing and fine tuning hands automated photometric pipeline

Testing and Fine-Tuning HANDS’ Automated Photometric Pipeline

Austin Barnes

Oceanit

Mentor: Russell Knox

Advisors: Rita Cognion and Curt Leonard

Home Institution: Harvard University

2009


Overview

Overview

  • Problem: Space Situational Awareness

  • Solution: Introduction to HANDS

  • Automated Photometric Pipeline

    • Calibration Star Correlator

  • Recommendations

  • Goal of Photometric Pipeline


Problem space situational awareness

Problem: Space Situational Awareness

  • >19,000 objects larger than 10 cm known to orbit the planet at ~17,000 mph

  • >300,000 objects between 1 and 10 cm

  • February 2009 satellite collision

Nasa Orbital Debris Program Office: www.orbitaldebris.jsc.nasa.gov


Solution hands

Solution: HANDS

High

Accuracy Network Determination System

  • Network of deployable robotic telescopes

  • Capable of:

    • Astrometry

    • Photometry


Automated photometric pipeline

Automated Photometric Pipeline

Aperture

Photometry

Satellite

Image

Reduced Satellite Image

Calibration Images

Calibration Star Correlator

Star Field

Image

Reduced Star Field Image


Calibration star correlator

Calibration Star Correlator

  • 276 stars found

  • 35 matched by position to stars in Landolt catalogue with known magnitudes

Image Credit: Kawailehua Kuluhiwa


Determining tolerance

Determining Tolerance

Average Magnitude Offset

Magnitude Offset:

Landolt – Observed

Angular Separation (arcsec): Landolt – Observed


Automated photometric pipeline1

Automated Photometric Pipeline

Aperture

Photometry

Satellite

Image

Reduced Satellite Image

Calibration Images

Calibration Star Correlator

Star Field

Image

Reduced Star Field Image

Calculate Extinction Coefficients


Calculating extinction coefficients

Calculating Extinction Coefficients

Slope = Extinction Coefficient

Y-Intercept = Instrumental Magnitude Offset

Magnitude Offset:

Landolt – Observed

Airmass


Recommendations

Recommendations

  • Reject outliers based on deviation of ~0.8 mag from average

  • Allow ≥3 arcseconds of angular separation (up to 5)

Average Magnitude Offset

Magnitude Offset:

Landolt – Observed

Angular Separation (arcsec): Landolt – Observed


Calculating extinction coefficients1

Calculating Extinction Coefficients

Slope = Extinction Coefficient

Y-Intercept = Instrumental Magnitude Offset

Magnitude Offset:

Landolt – Observed

Airmass


Calculating extinction coefficients2

Calculating Extinction Coefficients

Slope = Extinction Coefficient

Y-Intercept = Instrumental Magnitude Offset

Magnitude Offset:

Landolt – Observed

Same Plot

Using

Outlier Rejection

Airmass


Automated photometric pipeline2

Automated Photometric Pipeline

Aperture

Photometry

Satellite

Image

Reduced Satellite Image

Standardized

Light Curves

and Measurements

of Tracked Objects

Calibration Images

Calibration Star Correlator

Star Field

Image

Reduced Star Field Image

Calculate Extinction Coefficients


Goal of pipeline

Goal of Pipeline

  • Catalogue standardized magnitudes of detected objects

  • Identify and differentiate each object

  • Identify when particular objects change

Time 


Acknowledgments

Acknowledgments

  • Thank you to:

    • Rita Cognion, Curt Leonard, Russell Knox, James Frith, Kawailehua Kuluhiwa, Brooke Gibson, and the rest of the Oceanit Ohana

    • Dave Harrington, Mike Foley, Mark Pitts

    • Lisa Hunter, Nina Arnberg, Mike Nassir, Mark Hoffman

    • Aunty Lani LeBron, Akamai Workforce Initiative, and the rest of the Maui 2009 Interns

The 2009 Maui Akamai Internship Program is funded by the University of Hawaii, the Department of Business, Economic Development, and Tourism, the National Science Foundation Center for Adaptive Optics (NSF #AST - 9876783).


Questions

Questions?

Nasa Orbital Debris Program Office: www.orbitaldebris.jsc.nasa.gov


Using extinction coefficients

Using Extinction Coefficients

  • Equation for Standardized Satellite Magnitude:

    Ms = Mi – k*X + C

    Ms = Standardized Satellite Magnitude

    Mi = Instrumental Magnitude

    k = Extinction coefficient (slope of fitted line)

    X = Airmass (1 directly overhead, increases towards horizon)

    C = Instrumental Offset (Y-intercept of fitted line)


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