Transcript HMI_spd.aas_May_2010.ppt

The
HMI – AIA Joint Science Operations (JSOC-SDP)
Science Data Processing for the Solar Dynamics Observatory
Helioseismic & Magnetic Imager on the Solar Dynamics Observatory
The HMI Team – Stanford University, LMSAL, HAO, ++
HMI Recent Progress & Current HMI Activities
HMI Major Science Objectives
The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to
study the origin of solar variability and to characterize and understand the Sun’s interior
and the various components of magnetic activity. The HMI investigation is based on
measurements obtained with the HMI instrument as part of the Solar Dynamics
Observatory (SDO) mission. HMI makes measurements of the motion of the solar
photosphere to study solar oscillations and measurements of the polarization in a spectral
line to study all three components of the photospheric magnetic field. HMI produces data
to determine the interior sources and mechanisms of solar variability and how the
physical processes inside the Sun are related to surface magnetic field and activity. It also
produces data to enable estimates of the coronal magnetic field for studies of variability in
the extended solar atmosphere. HMI observations will enable establishing the
relationships between the internal dynamics and magnetic activity in order to understand
solar variability and its effects, leading to reliable predictive capability, one of the key
elements of the Living With a Star (LWS) program.
The broad goals described above will be addressed in a coordinated investigation in a
number of parallel studies. These segments of the HMI investigation are to observe and
understand these interlinked processes:
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The JSOC-SDP Team – Stanford University
Convection-zone dynamics and the solar dynamo;
Origin and evolution of sunspots, active regions and complexes of activity;
Sources and drivers of solar activity and disturbances;
Links between the internal processes and dynamics of the corona & heliosphere;
Precursors of solar disturbances for space-weather forecasts.
These goals address long-standing problems that can be studied by a number of
immediate tasks. The approaches to study these processes reflect our current level of
understanding and will obviously evolve in the course of the investigation.
(as of May 2010)
•SDO with HMI was launched on Feb 11, 2010.
HMI Data Processing
•The HMI aperture door was opened on March 24.
HMI Data
•The SDO commissioning was complete on April 30.
Michelson Interferometer
ISS Beam-splitter
Assembly
Alignment Mechanism
Limb Sensor Assembly
Filter Oven Assembly
ISS Pre-Amp Electronics
Box
Lyot Filter Assembly
Oven Controller E-Box
Camera Electronics Box
Focus Mechanism
Telescope Assembly
ISS Mirror Assembly
Hollow Core Motors
Secondary Lens Assembly
Front Door Assembly
Structure
Z
Optical Characteristics:
Effective Focal Length: 495 cm
Telescope Clear Aperture: 14 cm
Mechanical Characteristics:
Box: 0.84 × 0.55 × 0.16 m
Over All: 1.19 × 0.83 × 0.30 m
Mass: 44.0 kg
First Mode: 73 Hz
X
Y
Level-1
•We expect stable data products to be regularly available starting mid
June 2010.
•HMI “level-1” science data will be available within a day or so after
observation.
•Regular processing of higher level products will begin during the
next few months.
•Access to HMI data is available via the HMI/AIA JSOC (see right half
of this poster) and VSO.
HMI Implementation
The HMI instrument design and observing strategy are based on the highly
successful MDI instrument, with several important improvements. HMI observes
the full solar disk in the Fe I absorption line at 6173Å with a resolution of 1 arcsecond. HMI consists of a refracting telescope, a polarization selector, an image
stabilization system, a narrow band tunable filter and two 4096² pixel CCD
cameras with mechanical shutters and control electronics. The continuous data rate
is 55Mbits/s.
The polarization selector, a set of rotating waveplates, enables measurement of
Stokes I, Q, U and V with high polarimetric efficiency. The tunable filter, a Lyot
filter with one tunable element and two tunable Michelson interferometers, has a
tuning range of 600 mÅ and a FWHM filter profile of 76 mÅ.
Images are made in a sequence of tuning and polarizations at a 4-second cadence
for each camera. One camera is dedicated to a 45s Doppler and line-of-sight field
sequence while the other to a 90s vector field sequence. All of the images are
downlinked for processing at the HMI/AIA Joint Science Operations Center at
Stanford University.
All HMI data is available. Science level data products are being placed on an open web
server with a lag of a day or so of time of observation.
Lower level and intermediate products are available on request.
The data volume is large, more than a terabyte per day. Thus we encourage users to export
only the data they actually need for immediate analysis. We are committed to provide tools
to allow subsetting of the data and of providing multiple access tools appropriate for
different data volumes for different users.
JSOC SeriesName
hmi_test.V_45s
Hmi_test.M_45s
Hmi_test.Ic_45s
Hmi_test.Ld_45s
HMI_test.Lw_45s
Hmi_test.S_720s
Product
Dopplergrams, Line-of-Sight
magnetograms, Continuum
Proxy Intensity, 6173A line
width, line depth
respectively, observed at
45-second cadence.
Notes
“Final” products available
after mid June will not have
the “_test” suffix to the
project name. Units are
m/s, gauss, DN/s, mA, and
DN/s resp.
Stokes I,Q,U,V at 12 minute 24 quantities are saved for
cadence.
each time step. IQUV for
each of 6 filter tuning
positions.
The solid lines show the HMI filter transmission profiles at 76 mÅ spacing. The
black dashed line is the profile used for the continuum filtergram. The dotted line
shows the Fe I line profile.
Contributors to the HMI development up through launch include:
HMI Team
HEPL, Stanford
University
**Phil Scherrer
*John. Beck
*Richard. Bogart
*Rock Bush
*Tom Duvall, Jr.
*J.Todd Hoeksema
*Alexander
Kosovichev
*Yang Liu
*Jesper Schou
*XuePu. Zhao
Jim Aloise
Art Amezcua
Kelly Beck
Sudeepto
Chakraborty
Millie Chethik
Keh-Cheng Chu
Carl Cimilluca
Sebastien Couvidat
Nancy Christensen
Romeo Durscher
Thomas Hartlep
Keiji Hayashi
Tim Huynh
Stathis Ilonidis
Kevin Kempter
Irina Kitiashvili
Rasmus Larsen
Tim Larson
Leyan Lo
Rakesh Nigam
Konstantin
Parchevsky
Bala Poduval
Brian Roberts
Kim Ross
Deborah Scherrer
Jeneen Sommers
Jennifer Spencer
Margie Stehle
Xudong Sun
Hao Thai
Karen Tian
Jeff Wade
Richard Wachter
Junwei Zhao
HEPL Staff
LMSAL
*Alan. Title
*Tom Berger
*Karel Schrijver
*TedTarbell
Dave Akin
Brett Allard
Ron Baraze
M. Baziuk
E. Bogle
Bob Caravalho
Brock Carpenter
C Cheung
Roger Chevalier
K. Chulick
Tom Cruz
Jerry Drake
Dexter Duncan
Jay Dusenbury
Janet Embrich
Chris Edwards
Cliff Evans
Peter Feher
Barbara Fischer
Chuck Fischer
Sam Freeland
Frank Friedlander
Glen Gradwohl
Hank Hacook
Gary Heyman
Bob Honeycutt
Elizabeth Hui
Bruce Imai
Jerry Janecka
Romona Jimenez
Dwana Kacensky
Pete Kacensky
Claude Kam
Noah Katz
Karen Kao
Dave Kirkpatrick
Gary Kushner
Michael Levay
Russ Lindgren
Gary Linford
Andrea Lynch
Dnyanesh Mathur
Ed McFeaters
John Miles
Keith Mitchell
Sarah Mitchell
Ruth Mix
Margaret Morgan
Rose Navarro
Tom Nichols
Tracey Niles
Jackie Pokorny
Roger Rehse
Rick Rairden
J-P Riley
Lomita Rubio
David Schiff
Isella Scott
Ralph Sequin
Cherl Seeley
Lawrence Shing
Araya Silpikul
Larry Springer
Dick Shine
Bob Stern
R. Timmons
Louie Tavarez
Edgar Thomas
Darrell Torgerson
Angel Vargas
Shan Varaitch
Dale Wolf
Jake Wolfson
Carl Yanari
Ross Yamamoto
Kent Zickuhr
HAO
*Steve Tomczyk
Bruce Lites
Jonathan Graham
Anthony Darnell
Gregory L. Card
Aimee Norton
Juan Borrero
Santiago
Rebecca C. Elliott
David Elmore
Bruce Lites
Hector SocasNavarro
Arturo Lopez Ariste
Matthias Rempel
JPL
Michael Turman
JILA
*Juri Toomre
Deborah Haber
Bradley Hindman
Nicholas Fetherstone
Regner Trampedach
Swati Routh
Benjamin Brown
Gwen Dickenson0
NASA Ames
*Nagi Mansour
*Alan Wray
NJIT, BBSO
*Phil Goode
Vasyl Yurchyshyn
NWRA/CoRA
*Doug.C. Braun
*Charlie.A. Lindsey
Graham Barnes
Aaron Birch
Ashley Crouch
KD Leka
*†Tom Metcalf
Orion Poplawski
Martin Woodard
NSO
*Frank Hill
*Rachel Howe
Igor Suarez-Sola
Walter Allen
Olga Burtseva
Irene GonzalezHernandez
Rudi Komm
Sushanta Tripathy
Kiran Jain
Shakur Kholikov
Predictive Science
Inc.
*Jon. Linker
Zoran Mickic
Pete Riley
Janvier Wijaya
Michael Choy
Timofey Titov
MPS, DE
*Sami Solanki,
Laurent Gizon
Raymond Burston
Yacine Saidi
SAO
*Sylvain Korzennik
Alisdair Davey
MSSL, UK
*Len Culhane
Elizabeth Auden
UCLA
*Roger Ulrich
NAOJ, JP
*Takashi Sekii
Kaori Nagashima
U. of Hawaii
*Jeff. R. Kuhn
Marcelo Emilio
Isabelle Scholl
UMCP
*Judit Pap
USC
*Ed J. Rhodes, Jr.
Anthony Spinella
Shawn Irish
Johann Reiter
Yale University
*Sarbani Basu
Charles Baldner
RAL, UK
*Richard Harrison
Sheffield Univ. UK
*Mike Thompson
Univ. Tokyo, JP
*Hiromoto Shibahashi
Industrial
e2v - CCDs
Gary Auker
Rob Wilson
RAL - Cameras
Nick Waltham
International
Aarhus University,
DK
*Joergen
ChristensenDalsgaard
Cambridge, UK
*Douglas Gough
ESA
*Bernhard Fleck
IIAP, IN
S. Paul Rajaguru
Dipankar Banerjee
Siraj Hasan
LightMachinery
- Michelson
interferometers
Ian Miller
John Hunter
Andover
Corporation &
Zygo Corporation
- Filters
John Cotton
H. Magnetics
- motors
Ralph Horber
Spherical
Harmonic
Time series
To l=1000
Mode frequencies
And splitting
Ring diagrams
Local wave
frequency shifts
Time-distance
Cross-covariance
function
Wave travel times
Egression and
Ingression maps
Wave phase
shift maps
Data Product
Internal rotation Ω(r,Θ)
(0<r<R)
Internal sound speed,
cs(r,Θ) (0<r<R)
Full-disk velocity, v(r,Θ,Φ),
And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
High-resolution v and cs
maps (0-30Mm)
Stokes
I,Q,U,V
Full-disk 10-min
Averaged maps
Vector Magnetograms
Fast algorithm
Tracked Tiles
Vector Magnetograms
Inversion algorithm
Coronal magnetic
Field Extrapolations
Solar limb parameters
Coronal and
Solar wind models
Brightness feature
maps
Brightness Images
Tracked full-disk
1-hour averaged
Continuum maps
(Joint Science & Operations Center)
•Data Capture from SDO ground system
•Archive of telemetry and processed data
•Distribution to team and exports to all
users
•HMI and AIA processing to “level-1”
•HMI higher level science data products
Far-side activity index
Line-of-sight
Magnetograms
Continuum
Brightness
HMI/AIA JSOC
Deep-focus v and cs
maps (0-200Mm)
Stokes
I,V
HMI Data Analysis Pipeline
•There will be about 5 months of overlap with SOHO/MDI for
cross-calibrations.
HMI Data Products and Access
HMI Data Products as of May 22, 2010
Higher level products will begin to be processed on a regular basis over the coming
weeks.
Level-0
•Calibration and “observable” analysis code development
activities are continuing.
Primary Lens Assembly
Front Window Assembly
Doppler
Velocity
Tracked Tiles
Of Dopplergrams
Fold Mirror Assembly
Focal Plane Assembly
Heliographic
Doppler velocity
maps
Filtergrams
•Regular observations with preliminary calibrations are available since
May 4 for data from door opening to the current day – 1.
HMI Principal Optics Package Components
BDS Beam-splitter Assembly
The JSOC consists of three components: The IOC (Instrument Operations Center) at LMSAL performs instrument operations for both HMI and AIA; The SDP
(Science Data Processing) facility at Stanford handles data for both HMI and AIA by receiving it from the SDO ground system, short term and long term archive,
processing to “level-1” products for both instruments, higher level processing for HMI and data access and export for both instruments; The AVC (AIA Visualization
Center) provides tools for interactive inspection and analysis of AIA images and HMI magnetic data.
Line-of-Sight
Magnetic Field Maps
Vector Magnetic
Field Maps
Products from Level-1 and above are served through the open server at
the JSOC web site. The higher level products are in development and
are expected to become available over the coming months.
•Expect to archive ~ 1000TB/yr
•Metadata stored in PostgreSQL database
•Image data is stored online and on tape (LTO-4)
•“Pipeline” processing system to generate standard
products
•Special products computed automatically “on demand”
http://jsoc.stanford.edu
The JSOC web site includes a “wiki” for JSOC documentation, online code documents are maintained by the Doxygen system, the base infrastructrue
code is maintained in the CVS system with online access. Basic tools (AJAX style) are available for inspection of image metadata and access to
individual data files. Data is maintained in compressed FITS files with minimal headers. The data metadata is maintained in a PostGreSQL database.
Metadata may be bound to data files on export. The metadata system and supporting software API is called the “Data Record Management System”
(DRMS). The basic unit of storage is called a “Storage Unit” and maintained by SUMS (Storage Unit Management System). The DRMS/SUMS system
has heritage in the SOHO/MDI data system. DRMS/SUMS make each of the expected many hundreds of millions of files individually available.
SOHO/MDI data has been ingested into the JSOC DRMS/SUMS system as its Resident Archive and had been the source of most exported MDI data for
several years.
SDO (HMI and AIA) is available through multiple channels:
•Direct access via programming interface in “c” for pipeline processing and local analysis.
•Basic access and export directly from the JSOC data servers,
•High volume users are served by the netDRMS distributed data system.
•Most Level-1 and selected higher level products via the Virtual Solar Observatory (VSO),
•3rd party servers such as jhelioviewer.org will provide streaming access to images.
•JSOC-AVC will provide daily images to science museums and planetariums.
•The AVC will provide a “Sun Today” web service.
•NASA SDO will provide high volume access for selected event image sequences.