Reconstructing HST Images of Asteroids A. Storrs, S. Bank, H. Gerhardt (Towson Univ.), K. Makhoul (MIT) Acknowledgements: Support for this work provided.

Slides:

Advertisements

Similar presentations

A Crash Course in Radio Astronomy and Interferometry: 4

Advertisements

Speaker: Laird Close University of Arizona ADAPTIVE OPTICS IN ASTRONOMY THE PROBLEM: Since Newton’s time it was realized that the mixing of hot and cold.

Multi-color adaptive optics imaging of asteroid 1 Ceres Christophe Dumas, JPL - USA ESO Bill Merline, SwRI - USA Thierry Fusco, ONERA - France.

Lightcurve Signatures of Multiple Object Systems in Mutual Orbits Eileen V. Ryan and William H. Ryan New Mexico Institute of Mining and Technology Magdalena.

Composite colliding winds (CWo - orbiting; CWc - concentric; CWb - binary) and Seaquist, Taylor and Button (STB) model of HM Sge (open circle - hot component;

New Moons Around Pluto Jau-Shian Liang Department of Physics, NTHU 2005/11/24.

TOPS 2003 Remote Obs 1 Karen Meech Institute for Astronomy TOPS 2003 Image copyright, R. Wainscoat, IfA Image courtesy K. Meech.

Searching for Extrasolar Planets at the VLT and MMT with Simultaneous Differential Imaging Searching for Extrasolar Planets at the VLT and MMT with Simultaneous.

Center to Limb Variation of Hard X-Ray Spectra from RHESSI J.McTiernan (SSL/UCB) ABSTRACT: We use the RHESSI flare database to measure the center to limb.

Center to Limb Variation of Hard X-Ray Spectra from RHESSI J. McTiernan SSL/UCB.

The First Adaptive Optics High Resolution Mid – IR Imaging of Evolved Stars: Case Studies of RV Boo and AC Her B.A. Biller, L.M.Close, D. Potter, J. Bieging,

Image Enhancement.

Potentially Hazardous Asteroid 2004 XP14: Constraining Albedo, Diameter, & Taxonomy Target of Opportunity, NASA IRTF V. Reddy, M.J. Gaffey, P.S. Hardersen,

Ch 25 1 Chapter 25 Optical Instruments © 2006, B.J. Lieb Some figures electronically reproduced by permission of Pearson Education, Inc., Upper Saddle.

NICMOS IntraPixel Sensitivity Chun Xu and Bahram Mobasher Space Telescope Science Institute Abstract We present here the new measurements of the NICMOS.

HST Archival Studies of HH 30 WFPC2 Data Retrieval and Reduction Liu, Jimmy Chun-Fan Supervisor: Dr. Shang, Hsien August 23, 2002 Summer Student Program.

NASA’s Dawn Mission Journey to the Asteroid Frontier

Radiation & Telescopes ____________ radiation: Transmission of energy through space without physical connection through varying electric and magnetic fields.

Small Bodies of the Solar System Pluto, Comets, Asteroids, Meteors and Zodiacal Light.

ASTR-1010 Planetary Astronomy Day Announcements Smartworks Chapters 4: Due Monday, March 1. Smartworks Chapter 5 is also posted Exam 2 will cover.

PHYSICAL CHARACTERIZATION OF ASTEROIDS NEON Group 5: Koraljka Mužić Nikola Vitas Grzegorz Nowak Mario Mars Simone Marchi (tutor) 5 th NEON SCHOOL, OHP,

Printed by ACS 2 Gyro Mode Data Analysis Cheryl Pavlovsky, Marco Sirianni, Ken Sembach, ACS Instrument Team and the 2 Gyro Mode Team.

The B-V colors and photometric variability of Nix and Hydra, Pluto’s two small satellites Max Mutchler (STScI) S. Alan Stern (SwRI) Hal Weaver (JHU/APL)

Imaging Asteroidal Companions with the Hubble Space Telescope (HST) A. Storrs, K. Makhoul (Towson Univ.), E. Wells (CSC/STScI), M. Gaffey (Univ. of N.

Sent August 23, 2005 Here in the department of geological sciences at Arizona State University we are using a MAT 253 (instrument serial number 8632) for.

Tools for Studying Space. © 2011 Pearson Education, Inc. Telescopes.

SPIE Astronomical Telescopes and Instrumentation, San Diego, CA, 27 th June – 2 nd July 2010 Characterization of the mid-IR image quality at Gemini South.

Welcome to the Party! Why are we here? Celebrate the beginning of Dawn's year-long exploration of new worlds! Share in the excitement as we see something.

Asteroid Mining Jake Pan. What are Asteroids? Asteroids are chunks of rock floating in space: Left over from the formation of our solar system Created.

Digital Image Processing GSP 216. Digital Image Processing Pre-Processing – Correcting for radiometric and geometric errors in data Image Rectification.

2004 January 27Mathematical Challenges of Using Point Spread Function Analysis Algorithms in Astronomical ImagingMighell 1 Mathematical Challenges of Using.

Dawn NASA’s Dawn Mission Journey to the Asteroid Frontier Lucy McFadden, Co-Investigator University of Maryland College Park, MD July 18, 2007 Night Sky.

Near-infrared photometry of Venus Richard W. Schmude, Jr. Gordon State College.

Non-Optical Telescopes

Telescopes Key Words Optical Telescopes: make use of electromagnetic radiation in the range of visible light Refraction Telescopes: use lenses Reflecting.

D. E. McKenzie (Montana State University), S. Gburek (Space Research Centre, Polish Academy of Sciences), L. W. Acton, P. C. Martens (Montana State University)

Stars, Suns, and Moons. A spherical object in space made up of Hydrogen, Helium (or other gases), and that gives off its own light is called a A: moon.

Image Processing: Critical to Hubble Discoveries

The B-V colors and photometric variability of Nix and Hydra, Pluto’s two small satellites Max Mutchler (STScI) S. Alan Stern (SwRI) Hal Weaver (JHU/APL)

Image enhancement. Image from a ground based telescope The next slide shows an image of the same source.

The Hubble Space Telescope explores the limits of “roundness”: Ceres and Vesta Max Mutchler (Space Telescope Science Institute), Lucy McFadden, Jian-Yang.

Hubble Space Telescope imaging of Ceres and Vesta L. McFadden and J.Y. Li (University of Maryland, College Park), J. Parker and E. Young (Southwest Research.

Modeling and Correcting the Time- Dependent ACS PSF for Weak Lensing Jason Rhodes, JPL With: Justin Albert (Caltech) Richard Massey (Caltech) HST Calibration.

Adaptive Optics for Astronomy Kathy Cooksey. AO Basics Photons –Travel in straight lines Wavefront –Line perpendicular to all photons’ paths Atmospheric.

Asteroids are balls of rock a few feet to several miles in diameter. The are not large enough to be considered planets.. The total mass of all asteroids.

Asteroids Irregular (sometimes spherical) lumps of rock and metal that had never formed into planets during the formation of the solar system Several hundred.

HLA WFPC2 Source List Photometric Quality Checks Version: August 25, 2008 Brad Whitmore 1.Introduction 2.Comparison with Ground-based Stetson Photometry.

Small Bodies of the Solar System Pluto, Comets, Asteroids, Meteors and Zodiacal Light.

On the Evaluation of Optical Performace of Observing Instruments Y. Suematsu (National Astronomical Observatory of Japan) ABSTRACT: It is useful to represent.

The Critical Importance of Data Reduction Calibrations In the Interpretability of S-type Asteroid Spectra Michael J. Gaffey Space Studies Department University.

 Distance is the most important & most difficult quantity to measure in Astronomy  Method of Trigonometric Parallaxes  Direct geometric method of finding.

The Hubble Space Telescope Nikki Martin Physics 11A Mr. Jennings Dec. 9, 2005.

A PowerPoint by; Destin, Carley, and Eden. What Does Pluto look like The planet Pluto is a dwarf planet, meaning it’s really small compared to other planets,

Spatial Image Enhancement

NASA’s Dawn Mission will be the first to orbit a main belt asteroid, doing a detailed and extensive study of the two largest asteroids Ceres and Vesta.

Figure 2: Definition of the potential

Table 1. Details of the HST WFPC2 imaging and WHT ISIS spectroscopy presented in this paper. The F656N filter has central wavelength λ6560 Å and a FWHM.

Chandra HETG Spectra of SN 1987A at 20 Years

What kinds of objects are in the solar system?

Asteroids: between the planets

A “Field Guide” to WFPC2 HLA Image Anomalies

Multi-Wavelength Imaging Using Multi-Observatory Data

Asteroids Not just for kids anymore..

Ryugu's surface seen from Hayabusa2's remote-sensing observations

Diameters, Volumes and bulk densities of 40 asteroids

Chapter 9: The Family of Stars

T. J. Okamoto (NAOJ/Kyoto Univ.)

Comets & Asteroids in the PTF survey

UVIS Calibration Update

2/19/18 - POD FIRST, submit PODs in the black trays. Then, start a new page for PODS. POD #1 - Asteroids are made up of similar components that make.

Presentation transcript:

Reconstructing HST Images of Asteroids A. Storrs, S. Bank, H. Gerhardt (Towson Univ.), K. Makhoul (MIT) Acknowledgements: Support for this work provided by NASA through grant GO from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS Abstract: We present reconstructions of images of 22 large main belt asteroids that were observed by Hubble Space Telescope with the Wide-Field/Planetary cameras. All images were restored with the MISTRAL program (Mugnier, Fusco, and Conan 2003) at enhanced spatial resolution. This is possible thanks to the well-studied and stable point spread function (PSF) on HST. We present some modeling of this process and determine that the Strehl ratio for WF/PC (aberrated) images can be improved to 130%, while WFPC-2 images can achieve a Strehl ratio over 80% after reconstruction. We report sizes, shapes, and albedos for these objects, as well as any surface features. Images taken with the WFPC-2 instrument were made in a variety of filters so that it should be possible to investigate changes in mineralogy across the surface of the larger asteroids in a manner similar to that done on 4 Vesta by Binzel et al. (1997). Of particular interest are a possible water of hydration feature on 1 Ceres (see figure), and the non- observation of a constriction or gap between the components of 216 Kleopatra. References: Mugnier, L.M., T. Fusco, and J.-M. Conan, JOSA A (submitted) Binzel, R.P., Gaffey, M.J., Thomas, P.C., Zellner, B.H., Storrs, A.D., and Wells, E.N Icarus 128 pp Krist, J The Tiny Tim User’s Manual, Space Telescope Science Institute Image Restoration: Normal astronomical deconvolution processes do not work well on extended objects with sharp brightness variations, such as asteroids. These deconvolution processes will tend to over-enhance the edges of such sources, and so here we have used the MISTRAL routine (Mugnier et al. 2003) to avoid this problem. WFPC-2 images of the asteroids were restored with a theoretical (TinyTim, Krist 1993) PSF. The resultant images have a four times resolution improvement over the unrestored images. The above images demonstrate the technique. The top row contains the unrestored images, and the second row the results of optimal MISTRAL restoration. Both log stretched and oblique surface plots of each image are shown. The left group is an image of a standard star taken with the WF/PC (aberrated) camera, and the right group is taken with the WFPC-2 camera (F439W filter). The Strehl ratio for the WF/PC images is 50% before correction, and 180% after. For WFPC-2, the reconstruction process does not improve the Strehl ratio (about 85% in this image) but does sharpen the image and lower the background level. Note companion star in WFPC-2 image. 11 Parthenope RawRestored S – type Distance from Earth: 1.39 AU Diameter: 162 km Shape: spherical Albedo: Vibilia Raw Restored C – type Dist. from Earth: 1.20 AU Diameter: 146 km Shape: irregular Albedo: Julia RawRestored S – type Distance from Earth: 1.34 AU Diameter: 159 km Shape: irregular Albedo: Flora Restored S – type Distance from Earth: 0.90 AU Diameter: 141 km Shape: irregular Albedo: 0.22 Raw Crocus RawRestored Unknown Distance from Earth: 2.05 AU Diameter: unknown Shape: irregular Albedo: unknown 10 - Hygiea RawRestored C – type Distance from Earth: 2.54 AU Diameter: 429 km Shape: spherical Albedo: Amphitrite RawRestored S – type Distance from Earth: 4.44 AU Diameter: 219 km Shape: irregular Albedo: Alexandra RawRestored C – type Distance from Earth: 1.27 AU Diameter: 171 km Shape: spherical Albedo: Ceres C – type Distance from Earth: 1.94 AU Projected size 880 x 890 km Shape: spherical Albedo: 0.10 RawRestored Ratio 2:5 Ratio 1:2 Ratio 1:2 – F439W/F673N filter- Blue Continuum Slope Ratio 2:5 – F673N /F791W filter- Water of Hydration Map WFPC-2 Images: 5 - Astraea Visit #1 RawRestored Visit #2 S – type Dist. from Earth: 2.07 AU Diameter: 125 km Shape: spherical Albedo: Hestia RawRestored P – type Dist. from Earth: 1.63 AU Diameter: 131 km Shape: spherical Albedo: Minerva RawRestored C – type Dist. from Earth: 1.99 AU Diameter: 146 km Shape: spherical Albedo: Melpomene RawRestored S – type Dist. from Earth: 1.87 AU Diameter: 148 km Shape: spherical Albedo: Pales RawRestored C – type Dist. from Earth: 2.58 AU Diameter: 154 km Shape: spherical Albedo: RawRestored Hermione C – type Dist. from Earth: 2.31 AU Diameter: 217 km Shape: spherical Albedo: Leda RawRestored C – type Dist. from Earth: 1.38 AU Diameter: 120 km Shape: spherical Albedo: Ursula RawRestored C – type Dist. from Earth: 2.49 AU Diameter: Unknown Shape: spherical Albedo: Nemausa RawRestored G – type Dist. from Earth: 1.53 AU Diameter: 153 km Shape: spherical Albedo: WF/PC Images: The figure to the right shows the results of running MISTRAL on an extended image. The test image is on the left, convolved with WF/PC (aberrated) PSF in the center, and after restoration with MISTRAL on the right. 9-Metis 18-Melpomene 19-Fortuna 216-Kleopatra 624-Hektor S-type R=2.32 AU,  =1.49 AU Projected size 222x182 km Albedo S-type R=2.22 AU,  =1.26 AU Projected size 155x170 km Albedo G-type R=2.30 AU,  =1.53 AU Projected size 225x205 km Albedo M-type R=3.24 AU,  =2.38 AU Projected size 238x121 km Albedo D-type R=5.24 AU,  =4.33 AU Projected size 363x207 km Albedo Apparent rotation of 216 Kleopatra during observations. Apparent rotation of 624 Hektor during observations.