Tests of AST3-2 at Xinglong: Image Analysis Ma Bin NAOC 2013.05.20.

Slides:



Advertisements
Similar presentations
Enrico Giro – INAF – OAPD - ASTRI general meeting #9– Bologna, 24 Feb Towards the upgrade of the ASTRI structure following the consolidation of.
Advertisements

Using a DSLR to Study Variable Stars. Canon 450D - linear over a magnitude using RAW images with a specific setting.
Thomas Stalcup June 15, 2006 Laser Guidestar System Status.
Small Refractor CCD Imaging David Haworth
Optical Astronomy Imaging Chain: Telescopes & CCDs.
David Haworth Copyright 2001 Imaging the Sky 2001.
Active Control of Aberrations for the Large Synoptic Survey Telescope (LSST) Brice Cannon Lawrence Livermore National Laboratory Research Supervisor: Scot.
Towards Creation of a JWST Astrometric Reference Field: Calibration of HST/ACS Absolute Scale and Rotation Roeland van der Marel Jay Anderson, Colin Cox,
Announcements No lab tonight due to Dark Sky Observing Night last night Homework: Chapter 6 # 1, 2, 3, 4, 5 & 6 First Quarter Observing Night next Wednesday.
Current astrometric error is as low as 0.25 mas. Galactic Center observed with NIRC2 on Keck astrometric accuracy is a function of atmospheric conditions.
Darcy Bibb Oceanit Mentor: Tony Bartnicki Advisor: Curt Leonard Home Institution: Maui Community College Integration of a Small Telescope System for Space.
How to Get Equator Coordinates of Objects from Observation Zhenghong TANG Yale Astrometry Summer Workshop July, 2005.
LBC-Blue pre-commissioning LBC-Blue LBC-Blue –E Giallongo (PI) Rome: diPaola, Pedichini, Speziali, Testa, Gallozzi Rome: diPaola, Pedichini, Speziali,
Adding TDI mode to PRISM Li Zeng Advisor: Brian Taylor Jan.25, 2008.
1 Time-Delayed Integration/ Drift scanning William van Altena Yale University Basic Astrometric Methods Yale University July 18-22, 2005.
VISTA pipelines summit pipeline: real time DQC verified raw product to Garching standard pipeline: instrumental signature removal, catalogue production,
HI 1A - Raw Image. HI 1A – Shutterless/Flatfield Corrected Image (secchi_prep)
Front Yard CCD Astrophotography
The University of Alabama Observatory - New Visions April 2005.
NEO Research Project in Korea Wonyong Han 1, Yong-Ik Byun 2, Hong-Suh Yim 1, Young-Jun Choi 1, Hong-Kyu Moon 1 & NESS Team 1 Korea Astronomy and Space.
AST3 detector properties
July 13, 2006, Starsplitters of Wyalusing 1 TPoint What the is Bisque doing now?
Test and Operation of AST3 (Survey Control and Data System) Zhaohui Shang Tianjin Normal University National Astronomical Observatories, CAS On behalf.
Analysis of a Suspected Variable Star. What is a Variable Star? Variable stars are stars that change brightness. The changes in brightness of these stars.
The Chinese SONG proposal: scientific concerns Jianning Fu (Beijing Normal University) and Chinese SONG team Beijing ─ March 29, 2010 The third workshop.
The Observations of LAMOST Jianrong Shi NAOC 1/
CCD Detectors CCD=“charge coupled device” Readout method:
1 DES Photometric Calibration Strategy Douglas L. Tucker (FNAL) Filter and Calibrations Strategy Workshop 4 April 2008.
MARS Design Review PP-1 Requirements Definition Performance: –Tip/Tilt error < 0.06″ rms mirror coordinates 0.12″ rms image coodinates 0.28″ fwhm image.
ACS Drizzling Overview J. Mack; DA Training 10/5/07 Distortion Dither Strategies MultiDrizzle ‘Fine-tuning’ Data Quality Photometry.
Telescopes come in three basic styles. Refracting telescopes use lenses Refractors are either achromatic (some color distortion) or apochromatic (very.
Introduction of SONG telescope design Guomin Wang, Bozhong Gu, Xiangyan Yuan Zhiyong Zhang, Xiang Jiang, Shihai Yang The Third Workshop of SONG Beijing.
AST3-1 photometry from Dome A Bin Ma, Peng Wei, Yi Hu, Zhaohui Shang NAOC AST3
4-PARAMETER TRANSFORMATION OF DIGITIZED ASTRONOMICAL IMAGES Yavor Chapanov 1 1 – National Institute of Geophysics, Geodesy and Geography, Bulgarian Academy.
Henry Heetderks Space Sciences Laboratory, UCB
Introduction4 Data acquisition and analysis8 Results17 Conclusion24 ASTEROID PHOTOMETRY GROUP, VSA
April 2001 OPTICON workshop in Nice 1 The PSF homogenization problem in large imaging surveys Emmanuel BERTIN (TERAPIX)
Na Laser Guide Stars for CELT CfAO Workshop on Laser Guide Stars 99/12/07 Rich Dekany.
C2PU TELESCOPES © C2PU, Observatoire de la Cote d’Azur, Université de Nice Sophia-Antipolis Jean-Pierre Rivet CNRS, OCA, Dept. Lagrange
Weak Lensing - PSF Calibrations Steve Kent Apr 1, 2005 ● Motivation for studies: – 1. Develop concise metrics for requirements for weak lensing calibrations.
MMT Observation Database for Light Curve Analysis Vladimir Agapov Presentation for the WG1 session 33rd IADC meeting, Houston.
Telescope pointing models Gregor project meeting AIP, 14 th /15 th Oct, 2010 T. Granzer.
Telescopes 3 Functions 1. Gather light Size does matter The bigger, the better 2. Resolve detail 3. Magnification Only important for solar system objects.
Chapter 2: The Lens. Focal Length is the distance between the center of a lens and the film plane when focused at infinity.
National Aeronautics and Space Administration Pluto Astrometry From Table Mountain Observatory William M. Owen, Jr. Jet Propulsion Laboratory California.
CCD Image Processing: Issues & Solutions. CCDs: noise sources dark current –signal from unexposed CCD read noise –uncertainty in counting electrons in.
Identification of X-ray Point Sources and Study on the Nature of 62 X-ray Globular Cluster Candidates in M31 Zhou Fan, Jun Ma, Xu Zhou, Jiansheng Chen,
Camera Operations Pentax K1000. #2 & 3: Shutter Speed Dial/Index controls exposure time Slow shutter speed = longer exposure time = more blur and.
Remote observatory ISON-NM Survey of Minor Solar System bodies L. Elenin¹, I. Molotov¹, V. Savanevich², A. Kozhukhov³, A. Bryukhovetskiy³, V. Vlasenko³,
Gaia SSWG Workshop May Focal Plane Detection D. Hestroffer (IMCCE) & F. Arenou (GEPI) Paris Observatory On-board detection procedure but not localisation.
Auto Focus System based on RTS2 and EPICS Jiajing Liu, Guangyu Zhang, Jian Wang Modern Physics Department, University of Science and.
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.
Telescope pointing models Telescope & Instrumentation Robotisation on Dome C Puerto Santiago, Tenerife T. Granzer.
WFC3 SMOV UVIS and IR Geometric Distortion Calibration and Multidrizzle Vera Kozhurina-Platais and WFC3 team.
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
AST3 Experience Zhaohui Shang NAOC/Tianjin Normal University Chinese Center for Antarctic Astronomy
April / 2010 UFOAnalyzerV2 1 UFOAnalyzerV2 (UA2) the key of accuracy UA2 inputs video clip files and outputs meteor trajectories. UA2 does following steps.
Telescopes come in three basic styles
UFOAnalyzerV2 (UA2) the key of accuracy
Presented by: Kevin Beaulieu & Dustin Crabtree
WFPC2 1-Gyro Test Results
Astronomy 920 Commissioning of the Prime Focus Imaging Spectrograph
Intro to CCD Imaging Joe Roberts
The pointing calibration of the WFCTA tracking system
Source Environment Analysis 101
UCAC U.S. Naval Observatory CCD Astrograph Catalog T.J. Rafferty
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
FMOS astrometry plan Masayuki Akiyama.
Telescopes come in three basic styles
Presentation transcript:

Tests of AST3-2 at Xinglong: Image Analysis Ma Bin NAOC

Tests of AST3-2 at Xinglong Date: late Feb – early April Tests: focusing pointing, tracking operation & data system auto-survey real-time pipeline & database remote control

High Dark Level CCD TEC did NOT work well t_CCD ~ t_air ( ~ 0 ℃ ) dark: 100ADU/s (sky: 10ADU/s) Pixel-to-pixel variance Limiting depth!

Field Rotation Alt-Az mount

Field Rotation 30 sec

Field Rotation Speed Limiting Exptime !

Focusing Steps: Frames at diff. f FWHM measurement Fitting Influences: Seeing Unsteady due to movement

Focal Plane

Pointing Correction Tpoint: telescope axes.vs. alt-az

Pointing Time Neighbor field: 1.5 degree Firstly criterion RMS<2“, 40sec sec, but elongated 0409 RMS<1.5”, <15sec, unelongated

Astrometric Accuracy 0324 M35 1ses Scamp Ref cat: PPMX RMS ~ 0.15”

Limiting Mag 0306 open cluster M44 10sec

Trail of Bright Star Frame transfer 0.43sec 2640 lines bright star -> trail high speed sampling

Trail of Bright Star Movement of the center when both tracking and untracking Cause: Seeing ? Shake of the telescope ?

Thank you !