PSF in-flight calibration for MOS 1 and MOS 2 cameras
|
|
|
- Emerald Ellis
- 5 years ago
- Views:
Transcription
1 PSF in-flight calibration - MOS 1 - MOS 2 PSF in-flight calibration for MOS 1 and MOS 2 cameras Simona Ghizzardi Silvano Molendi
2 PSF in-flight calibration - MOS 1 - MOS 2 OVERVIEW The data set The analysis procedure Building the radial profile A model for the PSF Fitting the radial profile Results
3 PSF in-flight calibration - MOS 1 - MOS 2 THE DATA SET ENERGY RANGES: 0.3 kev [ ] ev 0.6 kev [ ] ev 1.0 kev [ ] ev 1.8 kev [ ] ev 3.7 kev [ ] ev 6.5 kev [ ] ev 10.0 kev [ ] ev SOURCES: ON-AXIS CAPELLA EXO C273 GX13+1 HR1099 PKS0558 LMC X-3 PKS0312 PSR0540 OFF-AXIS (> ~ 2 arcmin) HR (arcmin) CAPELLA 9.00; 4.48 (Capella) 9.48 GX ; 9.00;9.18;1.92 (GX13+1) 11.89; 2.74; C ;1.55 PSR (HCG016) (LMC) 11.9; 5.63 OMC2/ > 10.44
4 PSF in-flight calibration - MOS 1 - MOS 2 Building the radial profile FOR EACH MOS we merged the observations having the same source target the same pointing position different filters and/or operative mode ---> ---> different pile-up levels The centroid is determined accounting for the mask of the detector For each curve a good fitting range must be defined (points suffering for pile-up must be excluded).
5 PSF in-flight calibration - MOS 1 - MOS 2 Algorithm for the averaged radial profile Energy selection and pattern (0-12) selection BASIC METHOD We bin the image (with larger bins at larger radii) RADIAL PROFILE: dn/da (the area is not 2prdr because of the mask) each (squared) pixel is assigned to the (round) bin to which its CENTER belongs for these pixels it works fairly these pixels belong to two different bins in comparable fractions the effect is less important at larger radii ADDITIONAL RECIPE ADDED TO THE BASIC PROCEDURE We enclose each pixel in a circle. If the circle is fully enclosed in the bin then the pixel is too. If the circle is partly enclosed in another bin, the pixel may belong to two bins: we divide such pixels in NSUBPIXELS
6 PSF in-flight calibration - MOS 1 - MOS 2 A Model for the PSF we want an analytical function to describe the PSF according to the ground calibration results (FM1) PSF = KING + GAUSS In orbit PSF PSF = KING + GAUSS + BKG BKG in the data is high and Gauss component becomes negligible. Fitting is Gauss parameters-insensitive Data often suffer of pile-up. The King slope is well sampled but a large set of data is not useful for the core radius.
7 PSF in-flight calibration - MOS 1 - MOS 2 King profile core slope α King = 1 + A r 2 α Two shape parameters: core radius and slope. IT CAN BE INTEGRATED ANALYTICALLY IN rdr!!!
8 Fitting the radial profiles In order to enhance the statistics, we fit simultaneously the different curves with different pile- up levels PSF = King + BKG a e are the same for the different curves BKG and the normalization are different for each curve for each energy and off- axis angle we derive a and.
9 FOR FIXED OFF- AXIS = (E, J ) a = a (E, J ) CORE RADIUS: tends to decrease when energy increases ( LINEAR). SLOPE: the slope is roughly constant with energy OFF- AXIS = 0.15 (arcmin) (( slightly decreasing -- LINEAR). At higher off- axis angles few data are available.
10 FOR FIXED OFF- AXIS = (E, J ) a = a (E, J ) CORE RADIUS: tends to decrease when energy increases ( LINEAR). SLOPE: the slope is roughly constant with energy OFF- AXIS = 5.66 (arcmin) (( slightly decreasing -- LINEAR). At higher off- axis angles few data are available.
11 FOR FIXED OFF- AXIS = (E, J ) a = a (E, J ) CORE RADIUS: tends to decrease when energy increases ( LINEAR). SLOPE: the slope is roughly constant with energy OFF- AXIS = (arcmin) (( slightly decreasing -- LINEAR). At higher off- axis angles few data are available.
12 FOR FIXED OFF- AXIS = (E, J ) a = a (E, J ) CORE RADIUS: : tends to decrease when energy increases (( LINEAR). SLOPE: the slope is roughly constant with energy OFF- AXIS = 0.25 (arcmin) ( slightly decreasing - LINEAR). At higher off- axis angles few data are available.
13 FOR FIXED OFF- AXIS = (E, J ) a = a (E, J ) CORE RADIUS: : tends to decrease when energy increases (( LINEAR). SLOPE: the slope is roughly constant with energy OFF- AXIS = 1.72 (arcmin) ( slightly decreasing - LINEAR). At higher off- axis angles few data are available.
14 FOR FIXED OFF- AXIS = (E, J ) a = a (E, J ) CORE RADIUS: : tends to decrease when energy increases (( LINEAR). SLOPE: the slope is roughly constant with energy OFF- AXIS = (arcmin) ( slightly decreasing - LINEAR). At higher off- axis angles few data are available.
15 FOR FIXED ENERGY = (E, J ) a = a (E, J ) CORE RADIUS: is roughly constant with off- axis angle ( LINEAR). SLOPE: is roughly constant ENERGY = 1.0 kev with off-- axis angle (( LINEAR). At higher off- axis angles few data are available. At higher energies few data are available.
16 FOR FIXED ENERGY = (E, J ) a = a (E, J ) CORE RADIUS: is roughly constant with off- axis angle ( LINEAR). SLOPE: is roughly constant ENERGY = 3.7 kev with off-- axis angle (( LINEAR). At higher off- axis angles few data are available. At higher energies few data are available.
17 FOR FIXED ENERGY = (E, J ) a = a (E, J ) CORE RADIUS: is roughly constant with off- axis angle ( LINEAR). SLOPE: is roughly constant ENERGY = 6.5 kev with off-- axis angle (( LINEAR). At higher off- axis angles few data are available. At higher energies few data are available.
18 FOR FIXED ENERGY = (E, J ) a = a (E, J ) CORE RADIUS: : is roughly constant with off-- axis angle (( LINEAR). SLOPE: is roughly constant ENERGY = 1.0 kev with off- axis angle ( LINEAR). At higher off- axis angles few data are available. At higher energies few data are available.
19 FOR FIXED ENERGY = (E, J ) a = a (E, J ) CORE RADIUS: : is roughly constant with off-- axis angle (( LINEAR). SLOPE: is roughly constant ENERGY = 3.7 kev with off- axis angle ( LINEAR). At higher off- axis angles few data are available. At higher energies few data are available.
20 FOR FIXED ENERGY = (E, J ) a = a (E, J ) CORE RADIUS: : is roughly constant with off-- axis angle (( LINEAR). SLOPE: is roughly constant ENERGY = 6.5 kev with off- axis angle ( LINEAR). At higher off- axis angles few data are available. At higher energies few data are available.
21 FOR FIXED ENERGY = (E, J ) a = a (E, J ) CORE RADIUS: : is roughly constant with off-- axis angle (( LINEAR). SLOPE: is roughly constant ENERGY = 6.5 kev with off-axis angle ( LINEAR). At higher off-axis angles few data are available. At higher energies few data are available. No data for high ENERGIES AND OFF-AXIS ANGLES. No calibration is possible for these values.
22 2 DIMENSIONAL FIT = a + b E + c J + d E J a = x + y E + z J + w E J
23 King Core Radius for MOS 1
24 King Slope for MOS 1
25 2 DIMENSIONAL FIT = a + b E + c J + d E J a = x + y E + z J + w E J
26 and α are fixed to the best fit parameters. The normalization and the background are free parameters.
27 and α are fixed to the best fit parameters. The normalization and the background are free parameters.
28 Range of Application Calibration here is well sampled and the modelization provides a good description of the PSF. Few scattered data with large errors are available here. The modeled PSF must be used with caution. No data are available here. No calibration is possible in this region. DON T USE THE MODEL FOR THESE VALUES.
29 ENCIRCLED ENERGY FRACTION EEF IS ANALYTICAL Radii enclosing 50% and 80% of the energy at 1.5 kev, 8 kev, 9 kev for the on- axis PSF. EEF also for piled- up sources.
30 SUMMARY An analytical model for the PSF and the EEF has been provided Using a wide set of data, the best fit parameters are provided as functions of the energy and of the off-axis angle. A range of application of the model is defined: At high energies and off-axis angles no calibration is possible. The model must be used with caution at intermediate energies/ off-axis angles Full detailed report available at ~ simona/psf_inorbitmos. ps NEXT PN!
Evaluation of the capabilities of the XMM-Newton SciSim from the EPIC calibration point-of-view. André Burzlaff, FH Aachen
Evaluation of the capabilities of the XMM-Newton SciSim from the EPIC calibration point-of-view André Burzlaff, FH Aachen Menu XMM-Newton and EPIC SciSim Test Results Conclusion Outlook XMM Newton Launched
EPIC Straylight. telescopes/sieves/rga revisited. David Lumb, Athena Study Scientist
EPIC Straylight telescopes/sieves/rga revisited David Lumb, Athena Study Scientist Leicester BOC 7 Mar 2012 Topics Covered 1. The X-ray sieves 2. Initial in flight calibration (Crab ~Rev 54-56) 3. Sco
Status of the EPIC calibration
Status of the calibration 16 October 2003 Marcus G. F. Kirsch Marcus G. F. Kirsch with the input of the whole consortium Page 1 progress in calibration general absolute timing problem seems to be solved
A Parameterization of the Chandra Point Spread Function
Christopher L. Allen, Diab Jerius, and Terry Gaetz SAO 27 Oct 2003 Overview The off-axis Chandra PSF is a complex function of source position and energy: It is roughly elliptical, more so as off-axis angle
Analysis of extended sources with the EPIC cameras
Analysis of extended sources with the EPIC cameras 7 th ESAC SAS Workshop June 19 22, 2007 Science Operations Centre 1 Status Analysis of extended sources is complex, challenging and time-consuming There
Status and Calibration of the erosita X ray Telescope
Status and Calibration of the erosita X ray Telescope Vadim Burwitz Max Planck Institut für extraterrestrische Physik on behalf of the erosita Team IACHEC, Lake Arrowhead, USA, 29 Mar 2017 Spektr Rentgen
Calibration of ACS Prism Slitless Spectroscopy Modes
The 2005 HST Calibration Workshop Space Telescope Science Institute, 2005 A. M. Koekemoer, P. Goudfrooij, and L. L. Dressel, eds. Calibration of ACS Prism Slitless Spectroscopy Modes S. S. Larsen, M. Kümmel
arxiv: v1 [astro-ph.he] 11 May 2017
![arxiv: v1 [astro-ph.he] 11 May 2017](/thumbs/92/111039649.jpg "arxiv: v1 [astro-ph.he] 11 May 2017")
Noname manuscript No. (will be inserted by the editor) A Systematic Analysis of the XMM-Newton Background: I. Dataset and Extraction Procedures arxiv:1705.04171v1 [astro-ph.he] 11 May 2017 Martino Marelli
Lab 4: Differential Photometry of an Extrasolar Planetary Transit
Lab 4: Differential Photometry of an Extrasolar Planetary Transit Neil Lender 1, Dipesh Bhattarai 2, Sean Lockwood 3 December 3, 2007 Abstract An upward change in brightness of 3.97 ± 0.29 millimags in
XMM-Newton Calibration
XMM-Newton Calibration Michael Smith, on behalf of XMM-SOC and Instrument Teams 18 th XMM-Newton Users Group Meeting, ESAC, 11 May 2017 ESA UNCLASSIFIED - For Official Use Outline 1. Status of calibration
e e-03. which is distributed with standard chandra processing. visual inspection are included.
1 SUMMARY 1 SNR 0505-67.9 1 Summary Common Name: DEM L71 Distance: 50 kpc (distance to LMC, Westerlund(1990) ) Center of X-ray emission (J2000): ( 05 05 42.0, -67 52 39.8 ) X-ray size: 86 x 74 Description:
XMM-Newton Chandra Blazar Flux Comparison. M.J.S. Smith (ESAC) & H. Marshall (MIT) 7 th IACHEC, Napa, March 2012
XMM-Newton Chandra Blazar Flux Comparison M.J.S. Smith (ESAC) & H. Marshall (MIT) 7 th IACHEC, Napa, March 2012 Blazar Sample Objective: Comparison of XMM-Newton Chandra fluxes in various bands. Using
XMM-Newton SOC Technical Note
XMM-Newton SOC Technical Note XMM-SOC-CAL-TN-0082 Accuracy of energy reconstruction in EPIC-MOS Timing Mode M. Guainazzi April 6, 2009 History Version Date Editor Note 1.0 April 6, 2009 M.Guainazzi SASv8.0
X-ray burst science with Astrosat
X-ray burst science with Astrosat A R Rao Tata Institute of Fundamental Research, India (arrao@tifr.res.in) 40 years of X-ray bursts: Extreme explosions in dense environments 19 June 2015 17-19 June 2015
Practice Problems for Final Exam
Math 1280 Spring 2016 Practice Problems for Final Exam Part 2 (Sections 6.6, 6.7, 6.8, and chapter 7) S o l u t i o n s 1. Show that the given system has a nonlinear center at the origin. ẋ = 9y 5y 5,
Lessons learned from Bright Pixels and the Internal Background of the EPIC pn-ccd Camera
Lessons learned from Bright Pixels and the Internal Background of the EPIC pn-ccd Camera Elmar Pfeffermann, Norbert Meidinger, Lothar Strüder, Heinrich Bräuninger, Gisela Hartner Max-Planck-Institut für
A M BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY. WALSH et al Akiyama Group M1 Genki Suzuki
A 5 10 9 M BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY WALSH et al. 2015 Akiyama Group M1 Genki Suzuki Introduction NGC 1277 is thought to harbor one of the most massive black holes in the
Expected precision on planet radii with
Expected precision on planet radii with Adrien Deline 1, Didier Queloz 1,2 1 University of Geneva 2 University of Cambridge 24 th 26 th July 2017 CHEOPS Science Workshop 5 Schloss Seggau, Austria Field
Characterization of low energy ionization signals from Compton scattering in a CCD Dark Matter detector
Characterization of low energy ionization signals from Compton scattering in a CCD Dark Matter detector Karthik Ramanathan University of Chicago arxiv:1706.06053 (Accepted PRD) TeVPA 2017/08/07 1 Motivation
arxiv:astro-ph/ v1 6 Oct 2002
Astronomy & Astrophysics manuscript no. hkatayama January 18, 218 (DOI: will be inserted by hand later) Properties of the background of EPIC-pn onboard XMM-Newton H. Katayama 1, I. Takahashi 2, Y. Ikebe
XMM-Newton. Routine Calibration Plan. Version Edited by: M. J. S. Smith. September 6, Revision history
XMM-Newton Routine Calibration Plan Version 2.26 Edited by: M. J. S. Smith September 6, 2017 Revision history Revision number Date Revision author Comments Version 2.26 06/09/2017 M. J. S. Smith 3C 273
Annapurni Subramaniam IIA UVIT-PMB Meeting 08 June 2012
UVIT IN ORBIT CALIBRATIONS Annapurni Subramaniam IIA UVIT-PMB Meeting 08 June 2012 UVIT Telescope various components Calibrations are of two types: 1. Ground calibrations 2. In orbit calibrations In general,
NICMOS Status and Plans
1997 HST Calibration Workshop Space Telescope Science Institute, 1997 S. Casertano, et al., eds. NICMOS Status and Plans Rodger I. Thompson Steward Observatory, University of Arizona, Tucson, AZ 85721
Rotation of the Hot Gas around the Milky Way. Edmund Hodges-Kluck Matthew Miller and Joel Bregman University of Michigan
Rotation of the Hot Gas around the Milky Way Edmund Hodges-Kluck Matthew Miller and Joel Bregman University of Michigan Agenda Galaxy Halos OVII Absorption Lines in the RGS Archive Halo Model Halo Rotation?
WFC3 TV2 Testing: IR Channel Read Noise
Instrument Science Report WFC3 2008-04 WFC3 TV2 Testing: IR Channel Read B. Hilbert 12 Feb 2008 ABSTRACT Using data taken during WFC3's Thermal Vacuum 2 (TV2) testing campaign, we have characterized the
A space probe to Jupiter
Problem 3 Page 1 Problem 3 A space probe to Jupiter We consider in this problem a method frequently used to accelerate space probes in the desired direction. The space probe flies by a planet, and can
WFC3 IR Blobs, IR Sky Flats and the measured IR background levels
The 2010 STScI Calibration Workshop Space Telescope Science Institute, 2010 Susana Deustua and Cristina Oliveira, eds. WFC3 IR Blobs, IR Sky Flats and the measured IR background levels N. Pirzkal 1 Space
The Impact of x-cte in the WFC3/UVIS detector on Astrometry
Instrument Science Report WFC3 2014-02 The Impact of x-cte in the WFC3/UVIS detector on Astrometry Jay Anderson April 4, 2014 ABSTRACT Recent observations of the center of globular cluster Omega Centauri
PACS Spectrometer Wavelength Calibration
PACS Spectrometer Wavelength Calibration H. Feuchtgruber Max-Planck-Institut für extraterrestrische Physik, Garching PACS WaveCal 1 Description of the Calibration Problem - Blue array: 400 pixels - Red
Galaxy Clusters with XEUS. Silvano Molendi Stefano Borgani Stefano Ettori
Galaxy Clusters with XEUS Silvano Molendi Stefano Borgani Stefano Ettori Cosmic Vision Under the Cosmic Vision theme "The Universe taking shape" Investigation of galaxy clusters is declared to be amongst
UVIT IN ORBIT CALIBRATIONS AND CALIBRATION TOOLS. Annapurni Subramaniam IIA (On behalf of the UVIT team)
UVIT IN ORBIT CALIBRATIONS AND CALIBRATION TOOLS Annapurni Subramaniam IIA (On behalf of the UVIT team) Calibrations: : Calibrations are of two types: 1. Ground calibrations 2. In orbit calibrations In
Calibration Activities the MOS perspective
Calibration Activities the perspective Changing the Quantum Efficiency Calibration: Motivation and Justification. Flux comparison using a sample (17) of AGN observations: as presented at MPE (May 2006)
Exoplanet Search Techniques: Overview. PHY 688, Lecture 28 April 3, 2009
Exoplanet Search Techniques: Overview PHY 688, Lecture 28 April 3, 2009 Course administration final presentations Outline see me for paper recommendations 2 3 weeks before talk see me with draft of presentation
Figure 1: Left: Apparent radial velocities of Capella measured with the Chandra/HETGS. The dotted line shows the calculated apparent radial motion of
Figure 1: Left: Apparent radial velocities of Capella measured with the Chandra/HETGS. The dotted line shows the calculated apparent radial motion of Capella Aa viewed from Earth (including the barycentric,
n_tof EAR-1 Simulations Neutron fluence Spatial profile Time-to-energy
n_tof EAR-1 Simulations Neutron fluence Spatial profile Time-to-energy A. Tsinganis (CERN/NTUA), V. Vlachoudis (CERN), C. Guerrero (CERN) and others n_tof Annual Collaboration Meeting Lisbon, December
Basics of Photometry
Basics of Photometry Photometry: Basic Questions How do you identify objects in your image? How do you measure the flux from an object? What are the potential challenges? Does it matter what type of object
Measurement of Long-Scale-Length Plasma Density Profiles for Two-Plasmon Decay Studies
Measurement of Long-Scale-Length Plasma Density Profiles for Two-Plasmon Decay Studies Plasma density scale length at 10 21 cm 3 (nm) 350 300 250 200 150 100 0 Flat foil 2 4 6 8 10 100 Target diameter
Expected Performance From WIYN Tip-Tilt Imaging
Expected Performance From WIYN Tip-Tilt Imaging C. F. Claver 3 September 1997 Overview Image motion studies done at WIYN show that a significant improvement to delivered image quality can be obtained from
Galaxies in Pennsylvania. Bernstein, Jarvis, Nakajima, & Rusin: Implementation of the BJ02 methods
Galaxies in Pennsylvania Bernstein, Jarvis, Nakajima, & Rusin: Implementation of the BJ02 methods Bases of our methods: Shapes with geometric meaning: No empirical polarizabilities; simple optimizations
Pile-up Modeling. John E. Davis. CXC 6th Chandra/CIAO Workshop, October 2008
1 Pile-up Modeling Outline Event Detection Grade Migration The Standard Model The Pile-up Model Data Preparation Using the model in sherpa and isis Examples 2 3 When a photon is absorbed
arxiv:astro-ph/ v1 27 Sep 2004
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) XMM-Newton observation of the most X-ray-luminous galaxy cluster RX J1347.5 1145 arxiv:astro-ph/0409627v1 27 Sep 2004 Myriam Gitti
Study of the evolution of the ACS/WFC sensitivity loss
Instrument Science Report ACS 2013 01 Study of the evolution of the ACS/WFC sensitivity loss Leonardo Úbeda and Jay Anderson Space Telescope Science Institute January 28, 2013 ABSTRACT We present a study
Chapters 31 Atomic Physics
Chapters 31 Atomic Physics 1 Overview of Chapter 31 Early Models of the Atom The Spectrum of Atomic Hydrogen Bohr s Model of the Hydrogen Atom de Broglie Waves and the Bohr Model The Quantum Mechanical
Discovery of TeV Gamma-ray Emission Towards Supernova Remnant SNR G Last Updated Tuesday, 30 July :01
Background-subtracted gamma-ray count map of SNR G78.2+2.1 showing the VERITAS detection (VER2019+407). For details, see Figure 1 below. Reference: E. Aliu et al. (The VERITAS Collaboration), Astrophysical
Zeeman Effect. Alex Povilus Physics 441- Fall 2003 December 20, 2003
Zeeman Effect Alex Povilus Physics 441- Fall 2003 December 20, 2003 Abstract The Zeeman Effect is observed by application of a strong magnetic field to a mercury vapor cell and exciting transitions by
Time Dependence of ACS WFC CTE Corrections for Photometry and Future Predictions
Time Dependence of ACS WFC CTE Corrections for Photometry and Future Predictions Adam Riess, Jennifer Mack May 5, 2004 ABSTRACT We present measurements of photometric losses due to imperfect parallel and
Notes on the point spread function and resolution for projection lens/corf. 22 April 2009 Dr. Raymond Browning
Notes on the point spread function and resolution for projection lens/corf Abstract April 009 Dr. Raymond Browning R. Browning Consultants, 4 John Street, Shoreham, NY 786 Tel: (63) 8 348 This is a calculation
Math 1120 Calculus, sections 3 and 10 Test 1
October 3, 206 Name The problems count as marked The total number of points available is 7 Throughout this test, show your work This is an amalgamation of the tests from sections 3 and 0 (0 points) Find
Supernovae SN1987A OPERA Constraints on neutrino parameters. Supernova neutrinos. Ly Duong. January 25, 2012
January 25, 2012 Overview Supernovae Supernovae Supernova types Core collapse model Neutrino properties Detection of neutrinos Data and analysis Experiment results Comparison with results Possible neutrino
Photometric Products. Robert Lupton, Princeton University LSST Pipeline/Calibration Scientist PST/SAC PST/SAC,
Photometric Products Robert Lupton, Princeton University LSST Pipeline/Calibration Scientist PST/SAC 2018-02-27 PST/SAC, 2018-02-27 LSST2017 Tucson, AZ August 14-18, 2017 1 Outline Photometry Point Sources
The Behaviour of the XMM-Newton Background: From the beginning of the mission until May XMM-SOC-GEN-TN-0014 issue 3.10
The Behaviour of the XMM-Newton Background: From the beginning of the mission until May 2017 XMM-SOC-GEN-TN-0014 issue 3.10 R. González-Riestra and P.M. Rodríguez-Pascual XMM-SOC User Support Group June
Legacy IACHEC Working Group: the first steps
Legacy IACHEC Working Group: the first steps Matteo Guainazzi 1 & Andy Pollock 2 1 Astro-H & MM-Newton ESA-SOC, ESAC, Spain 2 GAIA and multi-mission Archive Scientist, ESA-SOC, ESA, Spain Scope Provide
Calibration of the AGILE Gamma Ray Imaging Detector
Calibration of the AGILE Gamma Ray Imaging Detector Andrew Chen on behalf of the AGILE Team April 11, 2011 AGILE Astrorivelatore Gamma ad Immagini LEggero Italian Space Agency (ASI) small mission Participation
Coronagraphic Imaging of Exoplanets with NIRCam
Coronagraphic Imaging of Exoplanets with NIRCam C. Beichman NASA Exoplanet Science Institute, Jet Propulsion Laboratory, California Institute of Technology For the NIRCam Team September 27, 2016 Copyright
1. Nuclear Size. A typical atom radius is a few!10 "10 m (Angstroms). The nuclear radius is a few!10 "15 m (Fermi).
1. Nuclear Size We have known since Rutherford s! " scattering work at Manchester in 1907, that almost all the mass of the atom is contained in a very small volume with high electric charge. Nucleus with
Tracking properties of the ATLAS Transition Radiation Tracker (TRT)
2 racking properties of the ALAS ransition Radiation racker (R) 3 4 5 6 D V Krasnopevtsev on behalf of ALAS R collaboration National Research Nuclear University MEPhI (Moscow Engineering Physics Institute),
Mapping the non thermal emission in Coma cluster of galaxies using the FeXXV/FeXXVI line ratio
Mapping the non thermal emission in Coma cluster of galaxies using the FeXXV/FeXXVI line ratio J. Nevalainen 1 & D. Eckert 2 1 Helsinki University Observatory, Finland 2 ISDC, Geneva, Switzerland Evidence
Model Selection for Galaxy Shapes
Model Selection for Galaxy Shapes Chunzhe Zhang Advisor: Thomas C.M. Lee Collaborators: Vinay Kashyap, Andreas Zezas May 24, 2016 Chunzhe Zhang (UCDavis) Model Selection May 24, 2016 1 / 20 Overview 1
INTEGRAL. Science Operations Centre. Announcement of Opportunity for Observing Proposals (AO-11) JEM-X Observer s Manual
Science Operations Centre Announcement of Opportunity for Observing Proposals (AO-11) INT/OAG/13-0381/Dc Issue 1.0 4 March 2013 Prepared by E. Kuulkers Page: ii Based on inputs from the JEM-X team, National
Response of DIMM turbulence sensor
Response of DIMM turbulence sensor A. Tokovinin Version 1. December 20, 2006 [tdimm/doc/dimmsensor.tex] 1 Introduction Differential Image Motion Monitor (DIMM) is an instrument destined to measure optical
1 Introduction to POPPY and WebbPSF
WFIRST Technical Report Doc #: WFIRST-STScI-TR1703 Rev: A Date: October 4, 2017 WebbPSF for WFIRST Joseph Long, Marshall Perrin Space Telescope Science Institute, Baltimore, Maryland Abstract: WebbPSF
The WFIRST Coronagraphic Instrument (CGI)
The WFIRST Coronagraphic Instrument (CGI) N. Jeremy Kasdin Princeton University CGI Adjutant Scientist WFIRST Pasadena Conference February 29, 2016 The Coronagraph Instrument Optical Bench Triangular Support
Ivan Valtchanov Herschel Science Centre European Space Astronomy Centre (ESAC) ESA. ESAC,20-21 Sep 2007 Ivan Valtchanov, Herschel Science Centre
SPIRE Observing Strategies Ivan Valtchanov Herschel Science Centre European Space Astronomy Centre (ESAC) ESA Outline SPIRE quick overview Observing with SPIRE Astronomical Observation Templates (AOT)
The cosmic distance scale
The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,
E. not enough information given to decide
Q22.1 A spherical Gaussian surface (#1) encloses and is centered on a point charge +q. A second spherical Gaussian surface (#2) of the same size also encloses the charge but is not centered on it. Compared
Discovery of a New Gamma-Ray Binary: 1FGL J
Discovery of a New Gamma-Ray Binary: 1FGL J1018.6-5856 Robin Corbet (UMBC/NASA GSFC) on behalf of the Fermi-LAT collaboration, & M.J. Coe, P.G. Edwards, M.D. Filipovic, J.L. Payne, J. Stevens, M.A.P. Torres
Spectral Analysis of the Double Pulsar PSR J with XMM-Newton
Spectral Analysis of the Double Pulsar PSR J0737-3039 with XMM-Newton * E. Egron, A. Pellizzoni, M.N. Iacolina, A. Pollock, et al. INAF - Osservatorio Astronomico di Cagliari, Italy * ESAC, Madrid, Spain
High accuracy imaging polarimetry with NICMOS
Rochester Institute of Technology RIT Scholar Works Articles 11-6-28 High accuracy imaging polarimetry with NICMOS Daniel Batcheldor G. Schneider D.C. Hines Follow this and additional works at: http://scholarworks.rit.edu/article
X-ray diffraction geometry
X-ray diffraction geometry Setting controls sample orientation in the diffraction plane. most important for single-crystal diffraction For any poly- (or nano-) crystalline specimen, we usually set: 1 X-ray
The shapes of faint galaxies: A window unto mass in the universe
Lecture 15 The shapes of faint galaxies: A window unto mass in the universe Intensity weighted second moments Optimal filtering Weak gravitational lensing Shear components Shear detection Inverse problem:
SUPPLEMENTARY INFORMATION
doi:10.1038/nature11686 Database: In the present study we used a photometric database collected over the last 20 years for 21 Galactic globular clusters (GCs). In each cluster the central regions have
Recent results and prospects of exotic hadrons at B-factory
Recent results and prospects of exotic hadrons at B-factory XiaoLong Wang Virginia Tech & Belle Collaboration XVI International Conference on Hadron Spectroscopy Jefferson Lab, Newport News, Virginia 9/13
pseudo- evolution of halo mass and observable-mass relations Andrey Kravtsov The University of Chicago
pseudo- evolution of halo mass and observable-mass relations Andrey Kravtsov The University of Chicago Baseline model for cluster scaling relations Kaiser 1986, 1991 If mass is defined within a spherical
SOTANCP4. Is the Hoyle state condensed? Probing nuclear structure via 3-body decays. University of Birmingham, United Kingdom SOTANCP4.
Is the condensed? Probing nuclear structure via 3-body decays University of Birmingham, United Kingdom 1/29 Overview 1 2 3 4 1/29 Trinity of? 12 C 2/29 Cluster description of the 12 C as an equilateral
Weak lensing calibrated scaling relations for galaxy groups and clusters in the COSMOS and CFHTLS fields
Weak lensing calibrated scaling relations for galaxy groups and clusters in the COSMOS and CFHTLS fields Kimmo Kettula COSMOS, CFHTLenS and XMM-CFHTLS collaborations 06/19/2014 1 Introduction Mass calibration
Solar wind Magnetosphere Ionosphere Link Explorer: SoH X-ray Imager (SMILE-SXI)
Solar wind Magnetosphere Ionosphere Link Explorer: SoH X-ray Imager (SMILE-SXI) Steve Sembay SMILE-SXI PI Department of Physics and Astronomy University of Leicester, UK On behalf of the SMILE-SXI collaborabon
CMS Note Mailing address: CMS CERN, CH-1211 GENEVA 23, Switzerland
Available on CMS information server CMS NOTE 21/17 The Compact Muon Solenoid Experiment CMS Note Mailing address: CMS CERN, CH-1211 GENEVA 23, Switzerland 2 March 21 Study of a Level-3 Tau Trigger with
Fundamentals of Plasma Physics
Fundamentals of Plasma Physics Definition of Plasma: A gas with an ionized fraction (n i + + e ). Depending on density, E and B fields, there can be many regimes. Collisions and the Mean Free Path (mfp)
Hughes et al., 1998 ApJ, 505, 732 : ASCA. Westerlund, 1990 A&ARv, 2, 29 : Distance to LMC 1 ) ) (ergs s F X L X. 2 s 1. ) (ergs cm
1 SUMMARY 1 SNR 0525-66.1 1 Summary Common Name: N 49 Distance: 50 kpc (distance to LMC, Westerlund(1990) ) Position of Central Source (J2000): ( 05 25 59.9, -66 04 50.8 ) X-ray size: 85 x 65 Description:??
A New Analysis in the Field of the Open Cluster Collinder 223
Chin. J. Astron. Astrophys. Vol. 4 (2004), No. 1, 67 74 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics A New Analysis in the Field of the Open Cluster
WFC3/IR Persistence as Measured in Cycle 17 using Tungsten Lamp Exposures
WFC3/IR Persistence as Measured in Cycle 17 using Tungsten Lamp Exposures Knox S. Long, Sylvia Baggett, Susana Deustua & Adam Riess November 17, 2010 ABSTRACT Like most IR arrays, the IR detector incorporated
Homework 4 PHYS 212 Dr. Amir
Homework 4 PHYS Dr. Amir. (I) A uniform electric field of magnitude 5.8 passes through a circle of radius 3 cm. What is the electric flux through the circle when its face is (a) perpendicular to the field
Calibration of the IXPE Instrument
Calibration of the IXPE Instrument Fabio Muleri (INAF-IAPS) On behalf of the IXPE Italian Team 13th IACHEC Meeting 2018 Avigliano Umbro (Italy), 9-12 April 2018 IXPE MISSION IXPE will (re-)open the polarimetric
Absolute Flux Calibration for STIS First-Order, Low-Resolution Modes
Instrument Science Report STIS 97-14 Absolute Flux Calibration for STIS First-Order, Low-Resolution Modes Ralph Bohlin, Space Telescope Science Institute Nicholas Collins, Hughes STX/LASP/GSFC Anne Gonnella,
Physics 202: Spring 1999 Solution to Homework Assignment #3
Physics 202: Spring 1999 Solution to Homework Assignment #3 Questions: Q3. (a) The net electric flux through each surface shown is zero, since every electric field line entering from one end exits through
Status / Progress of the erosita X ray Observatory:
Status / Progress of the erosita X ray Observatory: Vadim Burwitz, Max Planck Institut für extraterrestrische Physik On behalf of the erosita Team IACHEC #9, May 13, 2014, Airlie Center, Warrenton, Virginia,
A Beam Size Monitor Based on Appearance Intensities for Multiple Gas Ionization INTRODUCTION
A Beam Size Monitor Based on Appearance Intensities for Multiple Gas Ionization T. Katsouleas and J. Yoshii Department of Electrical Engineering-Electrophysics, University of Southern California Los Angeles,
FLAT FIELDS FROM THE MOONLIT EARTH
Instrument Science Report WFPC2 2008-01 FLAT FIELDS FROM THE MOONLIT EARTH R. C. Bohlin, J. Mack, and J. Biretta 2008 February 4 ABSTRACT The Earth illuminated by light from the full Moon was observed
4. An electron moving in the positive x direction experiences a magnetic force in the positive z direction. If B x
Magnetic Fields 3. A particle (q = 4.0 µc, m = 5.0 mg) moves in a uniform magnetic field with a velocity having a magnitude of 2.0 km/s and a direction that is 50 away from that of the magnetic field.
Laura Barragán. Universidad Complutense de Madrid
. Universidad Complutense de Madrid Tutors: Erik Kuulkers & Peter Kretschmar INTEGRAL: International Gamma-Ray Astrophysics Laboratory The payload The mission The project IBIS (Imager on-board the Integral
ACIS ( , ) Total e e e e-10 4.
1 SUMMARY 1 G21.5-0.9 1 Summary Distance: 5 kpc ( Safi-Harb et al., 2001 ) Position of Central Source (J2000): ( 18 33 34.0, -10 34 15.3 ) X-ray size: 4.7 x4.6 Description: 1.1 Summary of Chandra Observations
The temperature and distribution of gas in CL measured
Mon. Not. R. Astron. Soc. 340, 161 168 (003) The temperature and distribution of gas in CL 0016+16 measured with XMM Newton D. M. Worrall and M. Birkinshaw Department of Physics, University of Bristol,
Encircled energy factor in impulse response functions of optical systems with first-order parabolic filters
Available online at www.elagiaresearchlibrary.com Advances in Alied Science Research,, 3 (6):3935-3943 ISSN: 976-86 CODEN (USA): AASRFC Encircled energy factor in imulse resonse functions of otical systems
Large Area Imaging Survey of Near-Infrared Sky with Korean Compact Space Telescopes
Large Area Imaging Survey of Near-Infrared Sky with Korean Compact Space Telescopes Science & Technology Satellite Series (KARI) (2000 ~ 2013. 02) 1 st Satellite: FIMS (Far-ultraviolet IMaging Spectrograph)
The energy-dependent temporal variation of the ROSAT PSPC gain
ASTRONOMY & ASTROPHYSICS NOVEMBER II 1996, PAGE 187 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 120, 187-193 (1996) The energy-dependent temporal variation of the ROSAT PSPC gain M.A. Prieto 1,G.Hasinger
Herschel Photodetector Array Camera & Spectrometer
Herschel Photodetector Array Camera & Spectrometer Albrecht Poglitsch, MPE Garching Christoffel Waelkens, Katholieke Universiteit Leuven Otto H. Bauer, Max-Planck-Institut für extraterrestrische Physik
MERIS US Workshop. Instrument Characterization Overview. Steven Delwart
MERIS US Workshop Instrument Characterization Overview Steven Delwart Presentation Overview On-Ground Characterisation 1. Diffuser characterisation 2. Polarization sensitivity 3. Optical Transmission 4.
The Extragalactic Distance Database: Hawaii Photometry Catalog
The Extragalactic Distance Database: Hawaii Photometry Catalog Hélène M. Courtois Université Lyon, CNRS/IN2P3/INSU, Institut de Physique Nucléaire, Lyon, France and Institute for Astronomy, University
Detection of Artificial Satellites in Images Acquired in Track Rate Mode.
Detection of Artificial Satellites in Images Acquired in Track Rate Mode. Martin P. Lévesque Defence R&D Canada- Valcartier, 2459 Boul. Pie-XI North, Québec, QC, G3J 1X5 Canada, martin.levesque@drdc-rddc.gc.ca
Measuring MNS, RNS, MNS/RNS or R
Measuring MNS, RNS, MNS/RNS or R Sebastien Guillot Advisor: Robert Rutledge Galileo Galilei Institute, Firenze March 2014 Some Reviews Lattimer and Prakash, 2007 Miller C., 2013 Heinke et al., 2013 Reminder