CIBER estimates of the Absolute ZL Foreground Intensity through Fraunhofer Absorption Line Spectroscopy
|
|
- Ashlyn King
- 5 years ago
- Views:
Transcription
1 CIBER estimates of the Absolute ZL Foreground Intensity through Fraunhofer Absorption Line Spectroscopy Phil Korngut Caltech NIR Background II, Munich Jun 1st, 2015
2 CIBER estimates of the Absolute ZL Foreground Intensity through Fraunhofer Absorption Line Spectroscopy Cosmologically pertinent results are currenty awaiting publication. Details of the technique will be discussed as implemented by CIBER.
3 Relative Brightness of Zodi and EBL Outdated EBL plot, (sorry if your measurements are not shown) Assume the brightest EBL reported and faintest ZL reported.
4 Relative Brightness of Zodi and EBL Outdated EBL plot, (sorry if your measurements are not shown) Zodi at NEP Assume the brightest EBL reported and faintest ZL reported.
5 Relative Brightness of Zodi and EBL Outdated EBL plot, (sorry if your measurements are not shown) Zodi at ecliptic lat = 10deg Zodi at NEP Assume the brightest EBL reported and faintest ZL reported.
6 DIRBE Annual Modulation 25um Animation from Ned Wright Pyo et al 2012 using Akari Kelsall and Wright DIRBE models are geometric and time/position dependent Difference in Absolute Photometry measurements is predominantly Foreground Model
7 Alternate Method of absolute ZL Estimation independent of Geometry Joseph von Fraunhofer (6 March June 1826) CaII 8542A line Line depth Short of ~2microns, the ZL is reflected Solar Spectrum with well characterized Absorption features.
8 Alternate Method of absolute ZL Estimation independent of Geometry Joseph von Fraunhofer (6 March June 1826) CaII 8542A line Isotropic EBL Line depth Short of ~2microns, the ZL is reflected Solar Spectrum with well characterized Absorption features.
9 Alternate Method of absolute ZL Estimation independent of Geometry Joseph von Fraunhofer (6 March June 1826) CaII 8542A line Isotropic EBL Line depth Line depth Sum Short of ~2microns, the ZL is reflected Solar Spectrum with well characterized Absorption features.
10 Previous Application of Fraunhofer Line Measurements to EBL Bernstein et al 2002 Measurements From the Ground Airglow Lines Credit: NASA/ Atmospheric Extinction Atmospheric scattering Many systematics can be avoided by doing this measurement from Space!
11 Previous Application of Fraunhofer Line Measurements to EBL Bernstein et al 2002 Measurements From the Ground Airglow Lines Credit: NASA/ Atmospheric Extinction Atmospheric scattering Many systematics can be avoided by doing this measurement from Space!
12 The CIBER Collaboration John Battle Jamie Bock Viktor Hristov Alicia Lanz Phil Korngut Peter Mason Michael Zemcov Asantha Cooray Joseph Smidt Yan Gong Chang Feng Toshiaki Arai Shuji Matsuura Kohji Tsumura Takehiko Wada Yosuke Onishi Mai Shirahata Toshio Matsumoto Dae Hee Lee Uk Won Nam Min Gyu Kim Keith Lykke Steve Brown Allan Smith
13 Design Requirements for a Space-based Fraunhofer line Spectrometer, $$$ Large apertures or lots of time in space is expensive Make very large pixels ZL Brightness and Line width R ~ 1000 sufficient for 854.2nm CaII line Use a sounding rocket
14 The Narrow Band Spectrometer 256x256 HgCdTe PICNIC array made by Teledyne.
15 The Narrow Band Spectrometer λ δθ = 8.5deg Instantaneous FOV =72.25 deg^2 Pixel size = 2 256x256 HgCdTe PICNIC array made by Teledyne.
16 The Narrow Band Spectrometer λ δθ = 8.5deg Instantaneous FOV =72.25 deg^2 Pixel size = 2 256x256 HgCdTe PICNIC array made by Teledyne.
17 CIBER s approach to the NIR EBL R Wide = 20 field Spectrometer (2.5x2.5deg) from Dual 800nm band to imager 2000nm (1.1um and 1.6um to (Measure measure spatial the Absolute R = fluctuations 1200 Intensity Spectrometer in the Spectrum background) to Measure of the the Zodiacal EBL) foreground via the 854.2nm CaII Fraunhofer line
18 Co-mounted in a LN2 Cryostat
19 Absolute NBS Calibration with the NIST SIRCUS Laser
20 Absolute NBS Calibration with the NIST SIRCUS Laser
21 CIBER Flight History -Flown 3 times from 2010 to 2012 on a BBIX 2 stage rocket. -Flight 4 on a four stage BBXII rocket.
22
23 Field Selection to Sample Parameter Space 9 Fields over 3 flights (6 independent) Bootes Elat-30 Elat-10 SWIRE NEP
24 Narrow Band Spectrometer Data Reduction Raw Single field NBS Image Ideal ZL CaII image Subtract Dark Current Template and mask outlier regions.
25 Narrow Band Spectrometer Data Reduction Single field NBS Image Dark Current, Flat field, Bad pixels masked Ideal ZL CaII image
26 Narrow Band Spectrometer Data Reduction Single field NBS Image Dark Current, Flat field, Bad pixels masked Ideal ZL CaII image Smoothed for Ease of Viewing only Register Astrometry & Create synthetic image based on 2mass stars
27 Narrow Band Spectrometer Data Reduction Single field NBS Image Dark Current, Flat field, Bad pixels masked Ideal ZL CaII image Binned By Wavelength Results as of Austin Meeting
28 Modelling all of the components required for Accurate ZL Estimates What we measure What we want Zodiacal Light Diffuse Galactic Light amplitude Stellar Light EBL, Airglow resid, Dark Current Resid etc. Spatial Distribution Effective CaII absorption profile of the component
29 Modelling all of the components required for Accurate ZL Estimates
30 Modelling all of the components required for Accurate ZL Estimates For CaII depth in ISL to first order use Lehtinen and Mattila 2013 ISL model Δλ = 1nm Approximately Solar and stable at our Glats at Δλ = 1nm
31 Modelling all of the components required for Accurate ZL Estimates Rely on Ancillary all-sky catalog (DSS-i2 (880nm)) et astrometry and perform a Sub-pixel stack to measure PSF enerate Model Star Template Including CaII NBS Measured Star Field (NEP)
32 Modelling all of the components required for Accurate ZL Estimates Rely on Ancillary all-sky catalog (DSS-i2 (880nm)) et astrometry and perform a Sub-pixel stack to measure PSF enerate Model Star Template Including CaII Mask Model Remnant Contribution Generate a mask removing pixels brighter than t from stars brighter than M in a catalog based model map
33 Modelling all of the components required for Accurate ZL Estimates Average correlation slope is for whole model
34 Modelling all of the components required for Accurate ZL Estimates
35 Modelling all of the components required for Accurate ZL Estimates With an 8.5 degree FOV the ZL is not uniform and gradient is important Shape of Free parameter in Fit
36 Fit For the ZL amplitude Low Ecliptic Lat DGL ISL DGL+ISL DGL+ISL+ ZL(free) Data 1D Spectra Data ISL+DGL Total Fit
37 Fit For the ZL amplitude Large Relative Contamination DGL ISL DGL+ISL DGL+ISL+ ZL(free) Data 1D Spectra Data ISL+DGL Total Fit
38 Best Fit Spectra For the Whole Sample Mean subtracted shown on same scale
39 Conclusions -Look for NBS paper soon with ZL model tests! -Going to space for this measurement avoids atmospheric systematics. -Large pixel size and FOV allows for detection in short exposures, but allows for other systematics. - Absolutely calibrated satellite mission could make excellent measurements.
Near-IR Background Fluctuation Results from the Cosmic Infrared Background Experiment
Near-IR Background Fluctuation Results from the Cosmic Infrared Background Experiment Michael Zemcov The Near- IR Background II: From Reionization to the Present Epoch Max- Planck- Gesellschaft, June 2,
More informationCIBER Measurements of the Mean Intensity of the NIR background
CIBER Measurements of the Mean Intensity of the NIR background Shuji Matsuura (ISAS, JAXA) for the CIBER CollaboraDon Near Infrared Background and the Epoch of Reioniza6on AusDn, Texas May 14, 2012 ObservaDonal
More informationNear Infrared Background Spectrum Obtained by AKARI
Near Infrared Background Spectrum Obtained by AKARI Tsumura et al. 2013, PASJ 65, 119: Zodiacal Light, Data Reduction PASJ 65, 120: Diffuse Galactic Light PASJ 65, 121: Extragalactic Background Light Tsumura
More informationEscaping the Zodi Light! Harvey Moseley! NASA/GSFC! The View from 5 AU! March 26, 2010!
Escaping the Zodi Light! Harvey Moseley! NASA/GSFC! The View from 5 AU! March 26, 2010! The Galaxy and the Zodi Light are the dominant sources of diffuse light in the night sky! Both are much brighter
More informationLarge 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)
More informationMEASUREMENTS OF THE MEAN DIFFUSE GALACTIC LIGHT SPECTRUM IN THE 0.95 µm TO 1.65µm BAND FROM CIBER arxiv: v2 [astro-ph.
MEASUREMENTS OF THE MEAN DIFFUSE GALACTIC LIGHT SPECTRUM IN THE.95 µm TO 1.65µm BAND FROM CIBER arxiv:153.4926v2 [astro-ph.ga] 19 Mar 215 T. Arai 1, S. Matsuura 1, J. Bock 2,3, A. Cooray 4, M. G. Kim 5,
More informationLarge Area Surveys of the Near-Infrared Sky with MIRIS
Large Area Surveys of the Near-Infrared Sky with MIRIS Jeonghyun Pyo 1 MIRIS Team 1 Korean Astronomy and Space Science Institute (KASI), KOREA The 2nd Survey Science Group Workshop 2013 Feb. 13 16 @ High1
More informationSPHEREx. Olivier Doré JPL/Caltech. for the SPHEREx team.
SPHEREx Olivier Doré JPL/Caltech for the SPHEREx team http://spherex.caltech.edu Olivier Doré Aspen - Cosmological Signals from Cosmic Dawn to Present - January 2018 1 SPHEREX HAS THREE CORE SCIENCE THEMES
More informationarxiv: v1 [astro-ph.im] 20 Jun 2012
Submitted to ApJS February 13 2012; accepted June 20 2012 as part of CIBER Instrument Special Issue. Preprint typeset using L A TEX style emulateapj v. 5/2/11 THE COSMIC INFRARED BACKGROUND EXPERIMENT
More informationThe cosmic infrared background experiment-2 (CIBER-2) for studying the near-infrared extragalactic background light
The cosmic infrared background experiment-2 (CIBER-2) for studying the near-infrared extragalactic background light Mai Shirahata a, Toshiaki Arai a,b, John Battle c, James Bock c,d, Asantha Cooray e,
More informationMeasuring Light from the Epoch of Reionization with CIBER, the Cosmic Infrared Background Experiment
Measuring Light from the Epoch of Reionization with CIBER, the Cosmic Infrared Background Experiment California Institute of Technology/Jet Propulsion Laboratory E-mail: zemcov@caltech.edu T. Arai a, J.
More informationGALAXIES 626 Spring Introduction: What do we want to learn?
GALAXIES 626 Spring 2007 Introduction: What do we want to learn? The light of the universe is in discrete chunks: Why? How did we get from the tiny density fluctuations at recombination to the beautifully
More informationCurrent Status of MIRIS
Current Status of MIRIS Jeonghyun Pyo, MIRIS Team (KASI) Survey Science Group Workshop High 1 Resort 2015 January 26 Members of MIRIS Team Development Team 한원용 (PI), 이대희 (PM), 가능현, 김일중, 남욱원, 문봉곤, 박성준,
More informationCosmic Optical Background: The View from Pioneer 10/11. Cosmic Optical Background the View from Pioneer 10/11
Cosmic Optical Background: The View from Pioneer 10/11 Cosmic Optical Background the View from Pioneer 10/11 Matsuoka et al. 2011, ApJ, 736, 119 Yoshiki Matsuoka (Nagoya University) Nobuyuki Ienaka, Kimiaki
More informationExtragalactic Background Light Rebecca A Bernstein. Encyclopedia of Astronomy & Astrophysics P. Murdin
eaa.iop.org DOI: 10.1888/0333750888/2639 Extragalactic Background Light Rebecca A Bernstein From Encyclopedia of Astronomy & Astrophysics P. Murdin IOP Publishing Ltd 2006 ISBN: 0333750888 Institute of
More informationMIRIS. Korean Compact Infrared Space Telescope, MIRIS
Korean Compact Infrared Space Telescope, D.-H. Lee 1, W.-S. Jeong 1, Y. Park 1, C.H. Ree 1, U.-W. Nam 1, B. Moon 1, S.-J. Park 1, S.-M. Cha 1, J. Pyo 1, J.-H. Park 1, K. Seon 1, D. Lee 1,2, S.-W. Rhee
More informationProgress Towards an Absolute Calibration of Lunar Irradiance at Reflected Solar Wavelengths
Progress Towards an Absolute Calibration of Lunar Irradiance at Reflected Solar Wavelengths Claire Cramer, Steve Brown, Keith Lykke, John Woodward (NIST) Tom Stone (USGS) Motivation for using the Moon
More informationarxiv: v1 [astro-ph.im] 26 Oct 2015
Submitted to PASP July 16, 2015. Spatial and Temporal Stability of Airglow Measured in the Meinel Band Window at 1191.3 nm arxiv:1510.07567v1 [astro-ph.im] 26 Oct 2015 Hien T. Nguyen 1,2, Michael Zemcov
More informationSky Background Calculations for the Optical Monitor (Version 6)
Sky Background Calculations for the Optical Monitor (Version 6) T. S. Poole August 3, 2005 Abstract Instructions on how to calculate the sky background flux for the Optical Monitor on XMM-Newton, by considering
More informationIntroduction of near-infrared (NIR) spectroscopy. Ken-ichi Tadaki (NAOJ)
Introduction of near-infrared (NIR) spectroscopy Ken-ichi Tadaki (NAOJ) Near-infrared in astronomy absorption by terrestrial atmosphere - wavelength range of 1-5 um - observable windows are limited (J,
More informationOccupy Dark Matter: Accessing the 99% of dusty galaxies that lie beneath the confusion noise floor. Marco Viero - Caltech
Occupy Dark Matter: Accessing the 99% of dusty galaxies that lie beneath the confusion noise floor Marco Viero - Caltech hermes.sussex.ac.uk The Team Marco Viero, Plus engineers, instrument builders, software
More informationNear-infrared brightness of the Galilean satellites eclipsed in Jovian shadow TSUMURA Kohji (FRIS, Tohoku Univ.)
Near-infrared brightness of the Galilean satellites eclipsed in Jovian shadow TSUMURA Kohji (FRIS, Tohoku Univ.) Collaborators: Shirahata M., Minowa Y., Hayano Y.(NAOJ), Arimatsu K.(Univ.of Tokyo), Takahashi
More informationPoint source calibration of the AKARI/FIS all-sky survey maps for stacking analysis
Publ. Astron. Soc. Jpn (2014) 66 (2), 47 (1 9) doi: 10.1093/pasj/psu010 Advance Access Publication Date: 2014 April 16 47-1 Point source calibration of the AKARI/FIS all-sky survey maps for stacking analysis
More informationThe Two Micron All-Sky Survey: Removing the Infrared Foreground
University of Massachusetts Amherst ScholarWorks@UMass Amherst Astronomy Department Faculty Publication Series Astronomy 2000 The Two Micron All-Sky Survey: Removing the Infrared Foreground John E. Gizis
More informationSignal Model vs. Observed γ-ray Sky
Signal Model vs. Observed γ-ray Sky Springel+, Nature (2008) Two main dark matter signal components: 1. galactocentric diffuse 2. small structures Observed sky modeled with bremsstrahlung π 0 decay up-scattered
More informationarxiv: v1 [astro-ph.im] 22 Mar 2015
PASJ: Publ. Astron. Soc. Japan, 1??, c 2018. Astronomical Society of Japan. Calibration of the AKARI Far-infrared All Sky Survey Maps. arxiv:1503.06422v1 [astro-ph.im] 22 Mar 2015 Satoshi Takita, 1 Yasuo
More informationThe SPICA Coronagraph
The SPICA Coronagraph 2007, Jun 7 th, UC BERKELEY K. Enya 1, L. Abe 2, S. Tanaka 1, T. Nakagawa 1, M. Tamura 2, H. Kataza 1, O. Guyon 3, SPICA Working Group ( 1: ISAS/JAXA, 2: NAOJ, 3: NAOJ/SUBARU observatory)
More informationarxiv: v1 [astro-ph.im] 11 Mar 2014
Point source calibration of the AKARI/FIS all-sky survey maps for staking analysis arxiv:1403.2772v1 [astro-ph.im] 11 Mar 2014 Ko Arimatsu 1,2 Yasuo Doi 3 Takehiko Wada 1 Satoshi Takita 1 Mitsunobu Kawada
More informationarxiv: v2 [astro-ph.ep] 22 Jul 2010
Accepted by the Astrophysical Journal Preprint typeset using L A TEX style emulateapj v. 11/10/09 OBSERVATIONS OF THE NEAR-INFRARED SPECTRUM OF THE ZODIACAL LIGHT WITH CIBER K. Tsumura 1, J. Battle 2,
More informationStudies of diffuse UV radiation
Bull. Astr. Soc. India (2007) 35, 295 300 Studies of diffuse UV radiation N. V. Sujatha and Jayant Murthy Indian Institute of Astrophysics, Bangalore 560 034, India Abstract. The upcoming TAUVEX mission
More informationTransiting Exoplanet in the Near Infra-red for the XO-3 System
Transiting Exoplanet in the Near Infra-red for the XO-3 System Nathaniel Rodriguez August 26, 2009 Abstract Our research this summer focused on determining if sufficient precision could be gained from
More informationView from 5 AU. Final Discussion. Michael Hauser, STScI Michael Werner, JPL
View from 5 AU Final Discussion Michael Hauser, STScI Michael Werner, JPL Questions for Final Discussion What is the desired long term objective we are working towards? How can we build support and interest
More informationSearching for dark matter. with gamma-ray anisotropies
Image Credit: NASA/DOE/International LAT Team Searching for dark matter with gamma-ray anisotropies Jennifer Siegal-Gaskins CCAPP, Ohio State University with Brandon Hensley (Caltech!Princeton) Eiichiro
More informationThe 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:
More informationMESSIER Unveiling galaxy formation
MESSIER Unveiling galaxy formation David Valls-Gabaud on behalf of the MESSIER consortium Challenges in UV astronomy ESO - 2013 Oct 09 Two driving science cases for critical tests of the ΛCDM paradigm
More informationA Random Walk Through Astrometry
A Random Walk Through Astrometry Astrometry: The Second Oldest Profession George H. Kaplan Astronomical Applications Department Astrometry Department U.S. Naval Observatory Random Topics to be Covered
More informationAnalyzing Spiral Galaxies Observed in Near-Infrared
Analyzing Spiral Galaxies Observed in Near-Infrared Preben Grosbøl European Southern Observatory Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany Abstract A sample of 54 spiral galaxies was observed
More informationNICMOS 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
More informationLaboratory Emulation of Observations from Space
Science with a Wide-field Infrared Telescopes in Space, Pasadena, Feb 13, 2012 of Observations from Space Roger Smith -- Caltech Jason Rhodes, Suresh Seshadri -- JPL Previous culture, friendly collaboration
More informationKepler photometric accuracy with degraded attitude control
Kepler photometric accuracy with degraded attitude control Hans Kjeldsen, Torben Arentoft and Jørgen Christensen-Dalsgaard KASOC, Stellar Astrophysics Centre, Aarhus University, Denmark - 25 July 2013
More informationDiffuse Galactic Light in a high Galactic latitude cloud
Diffuse Galactic Light in a high Galactic latitude cloud Nobuyuki Ienaka Department of Astronomy, Guraduate School of Science, The University of Tokyo February, 2013 ii Abstract Diffuse Galactic Light
More informationIntracluster light in individual moderate redshift (0.02 < z < 0.31) clusters
Intracluster light in individual moderate redshift (0.02 < z < 0.31) clusters John Feldmeier (YSU) A1914 (Feldmeier et al. 2004) A 1651 (Gonzalez et al. 2000) A 4010 (Krick et al. 2008) Collaborators:
More informationMODELING OF THE INTERPLANETARY DUST CLOUD
MODELING OF THE INTERPLANETARY DUST CLOUD S. S. HONG Seoul National University, KOREA My long time collaborators with Zodiac Matters: Jerry L. Weinberg S.M. Kwon, J. Pyo, Y.M. Seo Hero Tanabe, M. Ueno,
More informationMultiphysics Simulation of Polymer-Based Filters for Sub-Millimetre Space Optics
Multiphysics Simulation of Polymer-Based Filters for Sub-Millimetre Space Optics N. Baccichet 1, G. Savini 1 1 Department of Physics and Astronomy, University College London, London, UK Sponsored by: EU
More informationarxiv: v1 [astro-ph.co] 30 May 2017
Mon. Not. R. Astron. Soc. 000, 1?? (2002) Printed 29 October 2017 (MN LATEX style file v2.2) arxiv:1705.10681v1 [astro-ph.co] 30 May 2017 Extragalactic Background Light: a measurement at 400 nm using dark
More informationBINGO simulations and updates on the performance of. the instrument
BINGO simulations and updates on the performance of BINGO telescope the instrument M.-A. Bigot-Sazy BINGO collaboration Paris 21cm Intensity Mapping Workshop June 2014 21cm signal Observed sky Credit:
More informationThe View from 5 AU Beckman Center, UC Irvine, March 2010
The View from 5 AU Beckman Center, UC Irvine, 25-26 March 2010 Introduc)on & Objec)ves Jamie Bock Jet Propulsion Laboratory California Ins)tute of Technology Memorial for Andrew Lange May 7 afernoon: Public
More informationComet Measurement Techniques. Karen Meech Institute for Astronomy Session 27 1/18/05
Comet Measurement Techniques Karen Meech Institute for Astronomy Session 27 1/18/05 Image copyright, R. Wainscoat, IfA Image courtesy K. Meech Techniques Summary Imaging & Detectors Photometry Deep Imaging
More informationSMTN-002: Calculating LSST limiting magnitudes and SNR
SMTN-002: Calculating LSST limiting magnitudes and SNR Release Lynne Jones 2017-12-05 Contents 1 Source Counts 3 2 Instrumental Zeropoints 5 3 Sky Counts 7 4 Instrumental Noise 9 5 Source footprint (n
More informationThe Plato Input Catalog (PIC)
The Plato Input Catalog (PIC) Giampaolo Piotto and the WP130000 group Dipartimento di Fisica e Astronomia Universita di Padova Because of the huge size of PLATO field (~2124 sq deg) and the consequent
More informationAstronomical image reduction using the Tractor
the Tractor DECaLS Fin Astronomical image reduction using the Tractor Dustin Lang McWilliams Postdoc Fellow Carnegie Mellon University visiting University of Waterloo UW / 2015-03-31 1 Astronomical image
More informationAstronomical calibrations of the AKARI Far-Infrared Surveyor
Astronomical calibrations of the AKARI Far-Infrared Surveyor Issei Yamamura, Sunao Hasegawa, Shuji Matsuura, Mai Shirahata, Sin itirou Makiuti (ISAS/JAXA) Martin Cohen (UCB), Thomas Müller (MPE) on behalf
More informationSpatial Stray Light Correction for Imaging Instruments Using Matrix Method Yuqin Zong
CORM 2007 Annual Conference, Gaithersburg, Maryland, May 8-11, 2007 Spatial Stray Light Correction for Imaging Instruments Using Matrix Method Yuqin Zong Outline 1) Introduction 2) Principle of spatial
More informationEBL Studies with the Fermi Gamma-ray Space Telescope
EBL Studies with the Fermi Gamma-ray Space Telescope Luis C. Reyes KICP The Extragalactic Background Light (EBL) What is it? Accumulation of all energy releases in the form of electromagnetic radiation.
More informationAstronomical Techniques I
Astronomical Techniques I Lecture 8 Yogesh Wadadekar Jan-Feb 2015 IUCAA-NCRA Grad School 1 / 28 Assignment 1 will be posted on the website by tonight or tomorrow morning. Kaustubh Vaghmare (kaustubh@iucaa.ernet.in)
More informationarxiv: v1 [astro-ph.ga] 14 May 2015
Publications of the Korean Astronomical Society pissn: 1225-1534 / eissn: 2287-6936 00: 1 99, 2014 March http://dx.doi.org/10.5303/pkas.2014.00.0.1 c 2014. The Korean Astronomical Society. All rights reserved.
More informationAstronomical Techniques
Astronomical Techniques Spectrographs & Spectroscopy Spectroscopy What is spectroscopy? A little history. What can we learn from spectroscopy? Play with simple spectrographs. Basic optics of a spectrograph.
More informationScience with large imaging surveys
Science with large imaging surveys Hiranya V. Peiris University College London Science from LSS surveys: A case study of SDSS quasars Boris Leistedt (UCL) with Daniel Mortlock (Imperial) Aurelien Benoit-Levy
More informationGALEX GR1 Instrument Performance and Calibration Review
GALEX GR1 Instrument Performance and Calibration Review Patrick Morrissey Caltech Operations Overview GALEX is operating quite smoothly in 2004. Active space weather has mostly dissipated. FUV is shut
More informationTHE SPITZER SPACE TELESCOPE EXTRAGALACTIC FIRST LOOK SURVEY: 24 m DATA REDUCTION, CATALOG, AND SOURCE IDENTIFICATION
The Astronomical Journal, 131:2859 2876, 2006 June # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. A THE SPITZER SPACE TELESCOPE EXTRAGALACTIC FIRST LOOK SURVEY: 24 m
More informationFuture X-rayX Spectroscopy Missions. Jan-Willem den Herder
Future X-rayX Spectroscopy Missions Jan-Willem den Herder contents Plasma diagnostics in the 0.1 to 10 kev band with resolution > 100 X-ray spectrometers: instrumental promises Future missions (a dream)
More informationSurvey of dusty AGNs based on the mid-infrared all-sky survey catalog. Shinki Oyabu (Nagoya University) & MSAGN team
Survey of dusty AGNs based on the mid-infrared all-sky survey catalog Shinki Oyabu (Nagoya University) & MSAGN team Search for Active Galactic Nuclei Purpose 1 The MIR selection can minimize wavelength-dependent
More informationA New Method for Characterizing Unresolved Point Sources: applications to Fermi Gamma-Ray Data
A New Method for Characterizing Unresolved Point Sources: applications to Fermi Gamma-Ray Data Ben Safdi Massachusetts Institute of Technology 2015 B.S., S. Lee, M. Lisanti, and B.S., S. Lee, M. Lisanti,
More informationImaging with Micado at the E-ELT. WORKSHOP: Imaging at the E-ELT
Imaging with Micado at the E-ELT Renato Falomo INAF Observatory of Padova, Italy WORKSHOP: Imaging at the E-ELT 29 May 2009, Garching Resolved stellar population in Virgo (high SB) Detailed View of high
More informationDeriving stellar masses from SDSS
Deriving stellar masses from SDSS Reference: Bruzual and Charlot 2003MNRAS.344.1000B Kauffmann et al. 2003MNRAS.341.33 Salim et al. 2007ApJS..173..267S Bell et al. 2003ApJS..149..289B Outline! Basic idea!
More informationROSAT Roentgen Satellite. Chandra X-ray Observatory
ROSAT Roentgen Satellite Joint facility: US, Germany, UK Operated 1990 1999 All-sky survey + pointed observations Chandra X-ray Observatory US Mission Operating 1999 present Pointed observations How do
More informationThe Evolution of Massive Galaxies at 3 < z < 7 (The Hawaii 20 deg 2 Survey H2O)
D. Sanders, I. Szapudi, J. Barnes, K. Chambers, C. McPartland, A. Repp (Hawaii) P. Capak, I. Davidson (Caltech), S. Toft (Copenhagen), B. Mobasher (UCRiverside) The Evolution of Massive Galaxies at 3
More informationSolar System Science with JWST!
Solar System Science with JWST! Dean C. Hines Space Telescope Science Institute JWST Imaging Modes! Mode Imaging Aperture Mask Interferometry Coronography Instrument Wavelength (microns) Pixel Scale (arcsec)
More informationMass Astronomical Data at Dome A and VO
Mass Astronomical Data at Dome A and VO Qiang LIU (NAOC/CCAA) Outline Kunlun Station CSTAR AST3 Database and VO Why Dome A? Kunlun Station at Dome A Position: 80.25 S, 77.06 E Temperature: Mean: -50 C
More informationAstroBITS: Open Cluster Project
AstroBITS: Open Cluster Project I. Introduction The observational data that astronomers have gathered over many years indicate that all stars form in clusters. In a cloud of hydrogen gas, laced with helium
More informationObserving with the Infrared Spectrograph
Observing with the Infrared Spectrograph C. Grillmair, L. Armus GO Workshop 21-22 November 2002 Outline 1) Meet the IRS IST 2) Basic IRS capabilities 3) Observing and readout modes 4) Data products and
More informationThe DoE/NASA Joint Dark Energy Mission. November 2005 Kim Griest
The DoE/NASA Joint Dark Energy Mission November 2005 Kim Griest JDEM Science Definition Team (SDT): Cochairs: Chuck Bennett and Kim Griest Members: Albrecht, Baltay, Barish, Bernstein, Blandford, Caldwell,
More informationMURCHISON WIDEFIELD ARRAY
MURCHISON WIDEFIELD ARRAY STEPS TOWARDS OBSERVING THE EPOCH OF RE-IONIZATION Ravi Subrahmanyan Raman Research Institute INDIA View from Earth: cosmic radio background from cosmological evolution in gas
More informationIntroduction to SDSS -instruments, survey strategy, etc
Introduction to SDSS -instruments, survey strategy, etc (materials from http://www.sdss.org/) Shan Huang 17 February 2010 Survey type Status Imaging and Spectroscopy Basic Facts SDSS-II completed, SDSS-III
More information(Present and) Future Surveys for Metal-Poor Stars
(Present and) Future Surveys for Metal-Poor Stars Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics SDSS 1 Why the Fascination
More informationExoplanetary Atmospheres: Atmospheric Dynamics of Irradiated Planets. PHY 688, Lecture 24 Mar 23, 2009
Exoplanetary Atmospheres: Atmospheric Dynamics of Irradiated Planets PHY 688, Lecture 24 Mar 23, 2009 Outline Review of previous lecture: atmospheric temperature structure of irradiated planets isothermal
More informationStudy of Physical Characteristics of High Apogee Space Debris
Study of Physical Characteristics of High Apogee Space Debris Yongna Mao, Jianfeng Wang, Xiaomeng Lu, Liang Ge, Xiaojun Jiang (National Astronomical Observatories, Beijing, 100012, China) Abstract Date
More informationarxiv: v1 [astro-ph.im] 16 Dec 2015
Publ. Astron. Soc. Japan (204) 00(0), 6 doi:.93/pasj/xxx000 arxiv:52.05046v [astro-ph.im] 6 Dec 205 Revised calibration for near- and mid-infrared images from 4000 pointed observations with AKARI/IRC Fumi
More informationGaia Photometric Data Analysis Overview
Gaia Photometric Data Analysis Overview Gaia photometric system Paola Marrese Sterrewacht Leiden marrese@strw.leidenuniv.nl Role of photometry in overall Gaia data analysis Photometric data analysis goals
More informationBOWSER Balloon Observatory for Wavelength and Spectral Emission Readings
COSGC Space Research Symposium 2009 BOWSER Balloon Observatory for Wavelength and Spectral Emission Readings BOWSER 1 Mission Premise 4.3 km above sea level 402.3km above sea level BOWSER 2 Information
More informationGDR1 photometry. CU5/DPCI team
GDR1 photometry CU5/DPCI team What is, or isn't included GDR1 only provides G mean flux and error Derived mean magnitude, all entries Zero point used is in Vega system Zero point for AB system also available
More informationAstonomy 62 Lecture #10. Last Time. Applications of Stefan-Boltzmann Law Color Magnitudes Color Index
Last Time Applications of Stefan-Boltzmann Law Color Magnitudes Color Index Standard Visual Band Filters U B V R I Flux through filter X: F x = 0 F S x d F x F x W x Apparent Color Magnitude: m x,1 m x,2
More informationKeck/Subaru Exchange Program Subaru Users Meeting January 20, 2011
Keck/Subaru Exchange Program Subaru Users Meeting January 20, 2011 Taft Armandroff, Director W. M. Keck Observatory With science results from: Drew Newman and Richard Ellis, Caltech A. Romanowsky, J. Strader,
More informationData Processing in DES
Data Processing in DES Brian Yanny Oct 28, 2016 http://data.darkenergysurvey.org/fnalmisc/talk/detrend.p Basic Signal-to-Noise calculation in astronomy: Assuming a perfect atmosphere (fixed PSF of p arcsec
More informationAmateur Astronomer Participation in the TESS Exoplanet Mission
Amateur Astronomer Participation in the TESS Exoplanet Mission Dennis M. Conti Chair, AAVSO Exoplanet Section Member, TESS Follow-up Observing Program Copyright Dennis M. Conti 2018 1 Copyright Dennis
More informationData Reduction - Optical / NIR Imaging. Chian-Chou Chen Ph319
Data Reduction - Optical / NIR Imaging Chian-Chou Chen (T.C.) @ Ph319 Images at different wavelengths... Images at different wavelengths... However, the raw data are always not as pretty Why? The total
More informationSTRUCTURE OF GALAXIES
STRUCTURE OF GALAXIES 2., classification, surface photometry Piet van der Kruit Kapteyn Astronomical Institute University of Groningen the Netherlands February 2010, classification, surface photometry
More informationMeasuring the Redshift of M104 The Sombrero Galaxy
Measuring the Redshift of M104 The Sombrero Galaxy Robert R. MacGregor 1 Rice University Written for Astronomy Laboratory 230 Department of Physics and Astronomy, Rice University May 3, 2004 2 Abstract
More informationLab 4 Radial Velocity Determination of Membership in Open Clusters
Lab 4 Radial Velocity Determination of Membership in Open Clusters Sean Lockwood 1, Dipesh Bhattarai 2, Neil Lender 3 December 2, 2007 Abstract We used the Doppler velocity of 29 stars in the open clusters
More informationCalibration of MERIS on ENVISAT Status at End of 2002
Calibration of MERIS on ENVISAT Status at End of 2002 Bourg L. a, Delwart S. b, Huot J-P. b a ACRI-ST, 260 route du Pin Montard, BP 234, 06904 Sophia-Antipolis Cedex, France b ESA/ESTEC, P.O. Box 299,
More informationComets observed with XMM-Newton
A major step in cometary X-ray research Konrad Dennerl Max-Planck-Institut für extraterrestrische Physik Comets the most surprising X-ray objects in space 1996: Comet Hyakutake (C/1996 B2) EPIC Consortium
More informationEarth Flats. 1. Introduction. Instrument Science Report ACS R. C. Bohlin, J. Mack, G. Hartig, & M. Sirianni October 25, 2005
Instrument Science Report ACS 2005-12 Earth Flats R. C. Bohlin, J. Mack, G. Hartig, & M. Sirianni October 25, 2005 ABSTRACT Since the last ISR 2003-02 on the use of Earth observations for a source of flat
More informationThe Infrared Properties of Sources in the H-ATLAS and WISE Surveys
The Infrared Properties of Sources in the H-ATLAS and WISE Surveys Nicholas Bond (NASA Goddard) Collaborators: Jonathan Gardner, Dominic Benford (Goddard), Andrew Blain (Leicester), Loretta Dunne (Nottingham),
More informationFLAT 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
More informationFirst Results from BOKS: Searching for extra-solar planets in the Kepler Field
First Results from BOKS: Searching for extra-solar planets in the Kepler Field John Feldmeier Youngstown State University The BOKS TEAM PIs: John Feldmeier (YSU), Steve Howell (NOAO/WIYN) Co-Is: Mandy
More informationWater Ice on the Satellite of Kuiper Belt Object 2003 EL61
Water Ice on the Satellite of Kuiper Belt Object 2003 EL61 K.M Barkume, M.E. Brown, and E.L. Schaller Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125
More informationarxiv: v2 [astro-ph.ep] 2 Nov 2017
Palomar Optical Spectrum of Hyperbolic Near-Earth Object A/2017 U1 Joseph R. Masiero 1 ABSTRACT arxiv:1710.09977v2 [astro-ph.ep] 2 Nov 2017 We present optical spectroscopy of the recently discovered hyperbolic
More informationJINA Observations, Now and in the Near Future
JINA Observations, Now and in the Near Future Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics Examples SDSS-I, II, and III
More informationHICO Science Mission Overview
HICO Science Mission Overview Michael R. Corson* and Curtiss O. Davis** * Naval Research Laboratory Washington, DC corson@nrl.navy.mil ** College of Oceanic and Atmospheric Sciences Oregon State University
More informationConstraining Galactic dark matter in the Fermi-LAT sky with photon counts statistics
Constraining Galactic dark matter in the Fermi-LAT sky with photon counts statistics Moriond Cosmology 2018 Silvia Manconi (University of Turin & INFN) March 20, 2018 In collaboration with: Hannes Zechlin,
More information