BRITE-Constellation Meeting Warzaw Feb 2010 BRITE - Constellation BRIght Target Explorer BRITE-AUTBRITE-CAN BRITE-POL.

Slides:

Advertisements

Similar presentations

EUCLID : From Dark Energy to Earth mass planets and beyond Jean-Philippe Beaulieu Institut dAstrophysique de Paris Dave Bennett University of Notre Dame.

Advertisements

Advanced CCD Workshop Arne A. Henden

000509EISPDR_SciInvGIs.1 EIS Performance and Operations Louise Harra Mullard Space Science Laboratory University College London.

A Search for Earth-size Planets Borucki – Page 1 KEPLER; Data Validation and Follow Up Observations CoRoT Symposium W.J. Borucki & the Kepler Team 5 February.

A NEW CTE PHOTOMETRIC CORRECTION FORMULA FOR ACS Marco Chiaberge TIPS meeting 05/16/2012.

PHOTOMETRIC AND SPECTROSCOPIC MONITORING OF DSCT, GDOR AND BCEP VARIABLES Recent and future observations Ennio Poretti INAF – Osservatorio Astronomico.

Less is More S. R.Kulkarni Director, Caltech Optical Observatories Chairman, SIM-Lite Science Team.

1 M. Auvergne. Natal October 2004 Instrument performances. Signal perturbations: Radiations. Scattered light. ACS. Temperature. Readout electronic. Calibrations.

Low Energy, Low Cost Swift A design experiment June 2010.

Stellar Continua How do we measure stellar continua? How precisely can we measure them? What are the units? What can we learn from the continuum? –Temperature.

Using DELPHI for Weak Lensing Measurements: Science Return and Mirror Size Jes Ford, JPL, UNR SURF /21/07 Mentor: Jason Rhodes Co-mentor: David Johnston.

Photometric follow-up of transiting planet candidates Marton Hidas UNSW.

HST WFC3 IR channel: 1k x 1k HgCdTe detector, QE 80% 18 micron pixels (0.13”/pix), ~2’x2’ FOV Detector sensitivity engineered to cut off above 1.7 micron,

BRITE-Constellation Overview and Status Feb 2010 BRITE - Constellation BRIght Target Explorer BRITE - ATBRITE - CABRITE – PL UniBRITE BRITE-AUSTRIA BRITE-PL1.

BRITE-Constellation Nov BRITE Satellites Cubic form factor (20cm/side) with mass < 8kg Cubic form factor (20cm/side) with mass < 8kg Pre-deployed.

The Search for Earth-sized Planets Around Other Stars The Kepler Mission (2009)

The Transient Universe: AY 250 Spring 2007 Extra Solar Planets Geoff Bower.

Extrasolar Planets.I. 1.What do we know and how do we know it. 2.Basic planetary atmospheres 3.Successful observations and future plans.

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

Asteroseismology: Looking inside stars Jørgen Christensen-Dalsgaard & Hans Kjeldsen Aarhus Universitet Rømer.

SDW20051 Vincent Lapeyrère LESIA – Observatoire de Paris Calibration of flight model CCDs for CoRoT mission.

Constellation Orion Visible Light Constellation Orion Infrared Light.

LIM: Near IR from a mini-satellite Dani Maoz. HST WFC3 IR channel: 1k x 1k HgCdTe detector, QE 80% 18 micron pixels (0.13”/pix), ~2’x2’ FOV Detector.

WIRE SATELLITE PHOTOMETRY OF ECLIPSING BINARY STARS John Southworth H Bruntt D L Buzasi.

SDW2005, juin, Taormina The Corot Space instrument.

Stargazing on Mars Stargazing on Mars Cover Page Environment Constellations Polar Axis Observing Moons Observing Mars Moon to Moon Solar Eclipses Earth.

X-ray Timing and Polarization mission & instrumentation DONG Yongwei Center for Particle Astrophysics Institute of High Energy Physics, Chinese Academy.

BRITE-Constellation consists of six nano-satellites: UniBRITE and BRITE-AUSTRIA (TUGSAT-1) are funded by Austria, two more by.

The Gaia mission Data reduction activities in the UK Floor van Leeuwen, IoA.

A SEMINAR ON HUBBLE SPACE TELESCOPE PRESENTED BY: HARI OM ELECTRONICS & COMMUNICATION REG NO SECTION-C ROLL NO.– 123.

BRITE-Constellation currently consists of two satellites, UniBRITE and BRITE-AUSTRIA (TUGSAT-1) and two satellites to be funded by the Canadian Space Agency.

The Hard X-ray Modulation Telescope Mission

The Chinese SONG proposal: scientific concerns Jianning Fu (Beijing Normal University) and Chinese SONG team Beijing ─ March 29, 2010 The third workshop.

SRG 1 X-RAY Astronomy 2009, Bologna, 11 September, 2009 Spectrum-Roentgen-Gamma astrophysical project, current status Mikhail Pavlinsky (IKI, Moscow) on.

10/9/ Studying Hybrid gamma Doradus/ delta Scuti Variable Stars with Kepler Joyce A. Guzik (for the Kepler Asteroseismic Science Consortium) Los.

Astronomy & Astrophysics Advisory Committee (AAAC) May 11, 2006 Vladimir Papitashvili Antarctic Sciences Section Office of Polar Programs National Science.

18-April-2006XRT Team1 Initial Science Observations Solar-B XRT Ed DeLuca for the XRT Team.

Stellar variability monitoring in open clusters with mini-SONG X.B. Zhang National Astronomical Observatories, Chinese Academy of Sciences.

A Search for Earth-size Planets Borucki – Page 1 Roger Hunter (Ames Research Center) & Kepler Team March 26, 2010.

G. Ricker (MIT) George Ricker MIT Kavli Institute Transiting Exoplanet Survey Satellite David Latham SAO 30 May 2008.

CDE CDR, September 14, 2004 Your Position, Your Name 1 GATS AIM Science Team Meeting January 23-24, 2007 CIPS Calibration Review, Aimee Merkel, Bill McClintock.

1 WB/lct CCD OVERVIEW Kepler will have 42 CCDs 2,200 column x 1,024 row full frame CCDs Field of View (FOV) > 100 square degrees (113 w/ vignetting)

AST3-1 photometry from Dome A Bin Ma, Peng Wei, Yi Hu, Zhaohui Shang NAOC AST3

The experience of BEST Heike Rauer and the BEST Team Institut für Planetenforschung Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR) and Zentrum für.

1 Optical observations of asteroids – and the same for space debris… Dr. D. Koschny European Space Agency Chair of Astronautics, TU Munich Stardust school.

SNAP Calibration Program Steps to Spectrophotometric Calibration The SNAP (Supernova / Acceleration Probe) mission’s primary science.

A Search for Earth-size Planets Borucki – Page 1 W.J. Borucki & Kepler Team (NASA Ames Research Center) NASA Academy 14 July 2010.

1 AAS Meeting, San Diego – January 13, 2005 Swift-UVOT Post-Launch Status Pete Roming S. D. Hunsberger, C. Gronwall, J. A. Nousek, A. A. Breeveld, K. O.

Science Lessons Learned from TESIS and their Relevance to SWAP V. Slemzin, LPI PROBA 2 SWT, La Roche, 14 June 2010.

Expectations and Limitations of Kepler Ground-Based Follow-Up Observations Joanna Molenda-Żakowicz Uniwersytet Wrocławski, Instytut Astronomiczny ul. Kopernika.

Use this loopy starter to highlight areas you need to focus on during this revision lesson. Stop the presentation after Slide 11 - Q 10. Replay at the.

1 Transiting Exoplanet Survey Satellite Daryl Swade Archive Team Meeting June 16, 2014.

Astronomical Projects BEYOND NIGHT SKY. General requirements Weekly Night sky observation. Good knowledge of telescope controlling Imaging. Inviting few.

EXPLORE/OC: Photometry Results for the Open Cluster NGC 2660 K. von Braun (Carnegie/DTM), B. L. Lee (Toronto), S. Seager (Carnegie/DTM), H. K. C. Yee (Toronto),

Update on results of Molniya-type HEO surveys performed by ISON in 2014 Vladimir Agapov (KIAM RAS) Roscosmos delegation Presentation for the WG1 session.

ISUAL Design Concept S. Mende. SDR 7 Jun NCKU UCB Tohoku ISUAL Design Concept S. Mende Sprite Example Sprite Image obtained by Berkeley/NCKU 1999.

The work has been supported by the FP-7 eHEROES Project № of the European Commission 10th European Space Weather Week, November 18-22, 2013, Antwerp,

Transient Identification and Classification with WISE Doug Hoffman R. Cutri & T. Jarrett The Eventful Universe, 2010.

1 Near-Earth objects – a threat for Earth? Or: NEOs for engineers and physicists Lecture 2 – From observations to measurements Dr. D. Koschny (ESA) Prof.

for Lomonosov-GRB collaboration

The Kepler Mission S. R. Kulkarni.

The first light of the Corot telescope.

Ultra-Violet Imaging Telescope for ASTROSAT

Onboard Instruments of ASTROSAT

Single Object & Time Series Spectroscopy with JWST NIRCam

First Assessments of EUVI Performance on STEREO SECCHI

N0--> N1 Chain Includes corrections of all the known instrumental perturbators - electronics: offset, EMI, gain - Time integration - Sky background -

MOST Guide Star Photometry

Observational Prospect of NIREBL

CHEOPS - CHaracterizing ExOPlanet Satellite

Presentation transcript:

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE - Constellation BRIght Target Explorer BRITE-AUTBRITE-CAN BRITE-POL

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Mission Goals high precision photometry (~mmag) high precision photometry (~mmag) selected very bright stars (<4 mag) selected very bright stars (<4 mag) 15 stars per field minimum (24deg FOV) 15 stars per field minimum (24deg FOV) obtained during at least 15min per orbit (100min) obtained during at least 15min per orbit (100min) in (at least) two wavelength regions (blue-red) in (at least) two wavelength regions (blue-red) long time base observations (180 d/y/field) long time base observations (180 d/y/field) all sky access including polar regions all sky access including polar regions 3 years lifetime per satellite (minimum 2) 3 years lifetime per satellite (minimum 2) 1MByte/day science data (compressed) 1MByte/day science data (compressed)

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Photometry 101 min BLUE - RED

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Sky BRITE: BRI ght T arget E xplorer

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Target Stars Selection  42 proposals have been submitted  13 PI‘s and their teams Austria (15), Australia (1), Belgium (2), Bulgaria (1), Canada (4), Croatia (1), Germany (6), Iran (1), Poland (2), Spain (1), Switzerland (1), U.K. (3) and USA (3) O, B and Be stars, beta Cephei stars, hot Supergiants, delta Scuti variables, gamma Doradus pulsators, roAp / CP stars, red Giants, eclipsing binaries and more BRITE CANDIDATE TARGET STAR CATALOG BRITE-sky: a target fields evaluations tool

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE - Constellation  nano-satellites  20cm cube spacecrafts <8kg  3 axis pointing control  LEO sunsynchronous (polar) orbit  small aperture (3cm) telescopes  wide (24deg) field of view  one instrument is RED sensitive one BLUE

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Orbit and Observing Strategy Low Earth Orbit (LEO) Sun-Synch (Dawn-Dusk) 820 km, LTDN 6AM (BRITE_AUT) Orbit Period ~ 101min 15-40min/per orbit per field 1-3 fields per orbit days per year 300 days per year (near pole) Sun

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE-AUT Launch Madras SFL is contracted to launch BRITE-AUT Q1-2011

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Instrument - Telescope 5 lens system plus filter & baffle for a 24 deg cicular FOV, telecentric low distortion, mimimal vignetting RED design BLUE design

BRITE-Constellation Meeting Warzaw Feb 2010 good performance at high (+20C) temperatures low power consumption and reasonable price ReadNoise ~15e rms KODAK KA11002 BRITE Detectors

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE - Filters

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE - Filters

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE – Point Spread Function ZEMAX Model PSF - 5 deg offsets BRITE Blue intra focalextra focal best focusdesign red: rms scatter in mmag black: CCD distance in [mm]

BRITE-Constellation Meeting Warzaw Feb 2010 ZEMAX Model PSF - 7 deg offsets BRITE Red design red: rms scatter in mmag black: CCD distance in [mm] BRITE – Point Spread Function

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Point Spread Function BRITE Blue PSF 5 deg offsets 8 pixels diameter – 80 pixels carry signal ~30“/pixel

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE – Field Of View 2670 pixel 4000 pixel 30“/pixel

BRITE-Constellation Meeting Warzaw Feb 2010

up to 15 (32x32pixel) ROI/Raster Region of Interest ROI/Raster

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Onboard Data Processing processed data: sections: R nnn B backgrounds R nnn A apertures for each background median and sigma are calculated + the sum of signals values encompassed in the two apertures a total of 10 values H pix V pix R nnn B4 R nnn B2 R nnn B3 R nnn B1 BW pix ROI R nnn R nn A1 R nnn A2 X1 Y1 Y2 X2 BW... width of background [pixels]

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Photometric Performance mag(V) = 0-> 1.3 sec / 14 exp per min mag(V) = 2-> 8.0 sec / 5 exp per min mag(V) = 4-> 50.0 sec / 1 exp per min mag(V) scatter

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Operational Software Science Data Generation Code

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE Ground Station(s)  Primary Ground Station: IKS – TU Graz  Additional Locations: UTIAS – Toronto Canada TU Wien IfA Uni Wien

BRITE-Constellation Meeting Warzaw Feb 2010 BRITE-AUT Project Timeline  development of the hardware and software hardware and software  completion of two satellites June 2010 satellites June 2010  launch targeted for January 2011 January 2011

BRITE-Constellation Meeting Warzaw Feb