Near Infrared Spectro-Polarimeter Use Case
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1 Project Documentation RPT-0036 Revision A Near Infrared Spectro-Polarimeter Use Case S. Gibson, L. Fletcher, R. Hubbard, S. Keil, J. Kuhn, H. Lin, M. Penn Science Working Group May 2008 Approved for use: Project Scientist Date Project Manager Date Systems Engineer Date Original on file Advanced Technology Solar Telescope 950 N. Cherry Avenue Tucson, AZ Phone atst@nso.edu Fax
2 ATST Science Use Case Title: The Magnetic Field of Prominence Cavities Prepared by: S. Gibson, L. Fletcher, R. Hubbard, S. Keil, J. Kuhn, H. Lin, M. Penn Section 1: Observing Proposal Near Infrared Spectro-Polarimeter Use Case Abstract: We will measure the three-dimensional magnetic field in a coronal cavity and prominence. Two complementary routes will be taken: direct spectropolarimetric magnetic field measurements and an indirect measurement inferring magnetic field strength from magnetoacoustic wave propagation. Scientific Justification: The storage and release of magnetic energy is the fundamental driver of coronal dynamics. Coronal prominence cavities represent coronal MHD quasi-equilibrium states, which have been shown to bodily erupt in coronal mass ejections (CMEs). In order to understand the origins of CMEs, we must understand the nature of the magnetic fields of the equilibrium that is lost. At the moment there are some observations of cavity densities, but these are insufficient to constrain models. Magnetic field measurements strength and direction - are required to pin down the preeruption coronal field configuration. Observation Description: Goal 1: Determine overall magnetic configuration of cavity and surrounding helmet streamer, to test global models of equilibrium. This includes: 1) radial profiles of longitudinal magnetic field strength and density, as measured at cavity center; 2) radial profiles of longitudinal magnetic field strength and density in surrounding (poleward) helmet streamer rim; 3) Measurement of density and (longitudinal) magnetic field strength gradient across cavity/streamer interface; and 4) Plane-of-sky magnetic field direction. Note that this Use Case could be run in conjunction with a complementary study of the prominence within the cavity; however, the details provided below are for the cavity observations only. Core observation 1: Map of longitudinal and azimuthal magnetic field over a 5 arcmin field of view with 3 pixels, within 5 of limb. Field measurement is required (i) in center of cavity and (ii) centered on poleward helmet cavity interface. The wavelength to be used is Fe XIII Å. Requires sensitivity of 1 G. Core observation 2: density obtained from line ratios of the Fe XIII lines at Å and Å. Requires photometric precision of a few percent. Complementary observations 1.1: Prominence observations TBD (at a minimum, one or two context images in Å to establish where the prominence lies in the field of view). Goal 2: Search for magnetoacoustic wave signatures, to be used in conjunction with density measurements, as an independent magnetic field diagnostic. Core observations 2: Doppler shift measurements at a sensitivity of 5 m/s. Requires a cadence of 30s. 3 pixels, within 5 of limb. Core observations 3: High cadence azimuthal field maps RPT-0036, Revision A Page 2 of 12
3 Complementary observations 3.1: N/A RPT-0036, Revision A Page 3 of 12
4 Instruments: Section 2: Observation Details Instrument Status Wavelength Range Spectral Lines/Features Image Size and Scale Cameras NIRSP required to 1083 nm Fe XIII 3 /pixel 0.1 K x 0.1 K 1 cameras 1 frame/sec AO Open loop Sequences: Instrument Stepping Number of Steps Sampling Definition Desired Cadence NIRSP spatial 2 Repointing 1000 sec Repeats/ Duration 8 repeats Data Rates: Instrument Data Volume/Sequence Data Rate NIRSP 2 TB 128 MB/sec Data Processing: Repeats/ Duration 1 repeats 4 hours Calibration Data Volume Total Data Volume 10 GB 2.01 TB Instrument Processing Types Reduction Cadence Purpose Output NIRSP Real time Gain corrected Dark removed Demodulated Processing Level Definition: Level 0 raw data Level 1 instrumental signatures removes Level 1.5 instrumental polarization corrected Level 2 seeing corrected Level 3 physical parameter maps 1s Required for quicklook Level 1 RPT-0036, Revision A Page 4 of 12
5 Calibrations: Instrument Dark/Bias Frame Sky Flat Field Target/Grid Polarimetric Calibration Scattered light Photometric calibration Wavelength calibration Spectral Flat F NIRSP 1% 1% Yes Yes No 1% Absolute velocities within 10m/s 1% Calibration needs are expressed in terms of the required accuracy of the measurement for each calibration type (as required). The actual calibration sequences will then be defined in the preplanning or observation definition phase. RPT-0036, Revision A Page 5 of 12
6 Telescope Setup: Telescope Tracking Fixed Position 1 Tracking Solar Rotation Tracking Feature 4 Mosaicing X Off-Limb Tracking 5 Carrington Rotation Rate Differential Rotation 2 Custom Rate 3 Comments: or fixed tracking plus post-processing co-registration 1 Fixed position may be used for limb or fixed disk center observations. 2 Will there be a single standard model rotation curve, or multiple curves for different features? 3 User specified tracking curve (tracking motion only in heliographic longitude? or also latitude?) 4 Using AO-offload to coordinate telescope motion with observed feature drift 5 Same as fixed position? Image Rotation X Fixed Heliographic Orientation 1 Fixed Geographic Orientation Parallactic Angle 2 Stepped Parallactic Alignment 3 Comments: 1 Fixed orientation with respect to Sun e.g. solar north aligned with detector axis 2 Fixed orientation with with respect to Earth's horizon i.e. slit aligned with direction of dispersion 3 Orientation is kept sufficiently close to the parallactic angle, but between adjustments image is rotated to keep a fixed orientation in heliographic coordinates. Scattered Light Control 1 X Mirror Cleaning X Telescope Scattered Light Level 2 Comments: 25 millionths required 1 Primarily for coronal observations (or other observations such as sunspot umbrae) 2 Requirement on level of scattered light introduced by telescope (i.e. depending on cleanliness of other optical surfaces?) RPT-0036, Revision A Page 6 of 12
7 AO Telemetry 1 Triggered 2 Covariances 3 Engineering Seeing Monitor 4 Light-Level Monitor 5 Comments: N/A 1 Information from the AO system that can be recorded during data acquisition for use in data analysis 2 Is recording of AO data triggered synchronously with images or sequences acquired by an instrument? 3 Basic information needed to compute long-exposure PSF 4 Real-time monitoring of r 0 or other atmospheric parameters as determined by the AO. 5 Measurement of (integrated) illumination. May be determined from AO or other system. Atmospheric Conditions: resolution wavelength nm Desired Resolution nm Minimum Resolution 2 derived median r 0 Coronal sky Sky Condition Constraints 3 < 15 millionths Sky Light Level 4 Comments: 1 What is the desired spatial resolution for these observations? 2 What is the minimum acceptable spatial resolution for these observations? 3 Are there any particular sky condition that may (or may not) be needed for these observations? For example, are cirrus or fog acceptable? 4 Primarily for coronal observations. RPT-0036, Revision A Page 7 of 12
8 Target Selection: Required Solar Conditions 1 Y N N/A Active Regions Flares Quiet Sun X Filaments/Prominences Coronal Hole Other: Comments: requires small, long-lived cavity 1 What particular solar features are needed (or must not be present) for this observing program? Auxiliary Target Selection Data 1 Y N N/A X Full-Disk Magnetogram 2 X High-Resolution Magnetogram X Hα Full-Disk Image 2 X EUV Image 3 Hα High-Resolution Image X X-Ray Image 3 X Other: coronal WL URL: X Time Series 4 Grid Overlay 5 Comments: magnetograms from previous / following days; high res magnetogram desired not required. Coronagraph observations over course of a month. 1 What other types of solar data should be used to select the observing target? Data should be displayed with a fixed orientation (e.g. solar north up) for all images. 2 Will these be available from a local telescope? 3 Can these be obtained from a single, fixed source? 4 Will time series of any of these data be necessary to choose the target (e.g. to find location of flares or emerging flux) 5 Data should be displayed with a grid overlay in a choice of coordinate systems. Will all auxiliary data have WCS metadata? Target Definition Fixed Coordinates 1 Disk Center RPT-0036, Revision A Page 8 of 12
9 X Feature Defined 2 Interactive Definition Coordinate System 4 X Limb (N/S/E/W) ATST Staff X Investigators 3 X Heliographic X Heliocentric X Carrington Comments: coronal cavity features will be targeted 1 Target can be defined by a fixed position is some coordinate system. 2 Target coordinates are derived from feature position, possibly based on external feature lists (e.g. pointing based on active region position from NOAA lists). 3 Final pointing can only be defined based on investigator input (as opposed to ATST staff choosing appropriate target for observing program). 4 Coordinate system in which target pointing will be given (if applicable). Data Display: Data Display Purposes 1 X Target Selection X Quality Assurance 2 Activity Monitoring 3 Instrument Monitoring 4 Data Selection 5 X Examination of Processed Data Instrument Setup 6 Comments: 1 For what reasons will the investigator or ATST staff need to display or examine the data obtained as part of the execution of the observing program. 2 To confirm acquired data is being correctly obtained and suffices for the observational program. 3 To monitor changes of solar conditions 4 To monitor proper operation of instruments 5 To identify or flag data that does or does not meet certain quality standards 6 To confirm instrument operation during instrument setup and calibration. Quick Look Display 1 Raw Data Corrected Data (i.e. flat/dark corrected) X Instrument Specific Reduction RPT-0036, Revision A Page 9 of 12
10 Scan 2 Profiles 3 Fixed Interval Display (frame number, time step) Frame Selection 4 X Stokes Parameters Additional Algorithms 5 Description: Source: 6 Comments: image descrambling required from fiber array 1 The Quick-Look System (QLS) will allow for real-time examination of the data obtained by any instrument or camera. The system can extract data at any point in the processing stream and optionally apply certain algorithms or plugins to the data before display. None of the displayed data will be recorded, though it may be possible to make notes (i.e. entries into a log or the header database) via the QLS. The nature of the data displayed may be fixed (e.g. show every 10 th image) or may involve user interaction with the display itself (e.g. zoom and pan controls, blinking two images, cursor-defined profile display, or scrolling through a sequence of images) through a predefined set of implemented display tools. The user may choose to hold the currently displayed image for closer examination and then release and allow the display to be updated with the latest data. The system should always indicate the currency of the displayed data (e.g. real-time, one minute old). 2 Display of multiple images from a single set of images obtained with a single instrument as part of a observing sequence. Due to data rates, only a subset of the scans obtained during the observations might be shown. This may be a fixed or an interactive display. 3 Interactive display of one or two axes through a 3-D data cube (one axis is typically wavelength). 4 Choose a single image within a fixed interval based on some predefined criteria (e.g. contrast). 5 Additional plugins may be applied to data prior to display, but these will require prior testing and approval. 6 Who will provide the plugin? Investigator? Instrument Scientist? Other ATST staff? Interactive Examination 1 X IDL X Other Software Package X User-Provided Computer 4 Standard Packages 2 Instrument Software 3 User-Provided Routines Interactive Workflow Definition 5 Comments: 1 What types of tools does the investigator expect to need for immediate examination of the data? 2 For example, SolarSoft 3 Standard instrument-specific data reduction pipelines 4 Allow access to data store from external computers (i.e. investigators laptop) while on-site. May be yes yes RPT-0036, Revision A Page 10 of 12
11 provided subject to bandwidth limitations or with read-only access. Only selected sequences or scans will be provided to the user with this mechanism (in FITS format and perhaps in processed form). An interface may be needed to allow user to select which data to be exported or made available. 5 User-defined data analysis processing pipelines Remote Data Display 1 X Target Selection X Real-Time Images for: X Quality Assurance X Activity Monitoring X Post-Observation Examination X Telescope and Environmental Data : sky brightness, dust levels, mirror conditions Engineering Data Comments: 1 What information and images may need to be displayed away from the telescope for remote investigators and off-site ATST staff? Data Delivery: Data Delivery Mechanisms X Take Data from Telescope Off-Site Data Delivery X Network Retrieval Preferred Medium X Comments: Tape Disks / RAID Pack Network Optical Media RPT-0036, Revision A Page 11 of 12
12 Observation Definition for Core Observation 1: Über-Instrument Configuration File: Set Tracking: Image Rotation: Image Orientation: Coordinate System: AO Telemetry: Seeing Monitor: Pointing: Warnings: Calibration: Pixel Resolution: Binning: Area: Wavelength Sequence 1: Pointing Sequence 1: ; Science Observations Start Observation 1: Pointing Sequence 1: Loop 1: Loop 2: Repeat: Loop 3: Repeat: Loop 4: Repeat: End Observation 1: ; Flat Field Observations Start Observation 2: Loop 1: Repeat: Loop 2: Repeat: Loop 3: Repeat: End Observation 2: Section 3: Observation Definition Near Infrared Spectro-Polarimeter Use Case RPT-0036, Revision A Page 12 of 12
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