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Request GST Observing Time
Please do not use special characters as they will be ignored.
Proposal Title (20 char minimum)
PI Name
PI Affiliation
PI email address:
Co-Is:
Target
Active Region
Quiet Sun
Solar Limb
Polar Regions
Specific Solar Activity
Proposal Information
Related to an NSF Grant
Related to an NASA Grant
Related to a PhD Thesis
Coordination with Ground Based Facility
Coordination with Space Based Facility
Short Summary of the Request (250 char minimum)
Why, What, and How
Scientific Rationale (250 char minimum)
Describe science behind the request
Prefereed Observing Dates
When operating in the "Service Mode" we will do our best satisfy the data request in the case of coordinated observations
Broad Band Filter Imager (BFI)
Tio
G-Band
Cadence
Second(s)
BFI provides continuum data using a highspeed 2048x2048 CCD camera. The bands currently used are G-band (430.5 nm, 0.5 nm bandpass) with a field of view of 55" and 0.027"/pixel image scale, and TiO (705.7 nm, 1 nm bandpass) with a field of view of 70" at 0.034"/pixel image scale. Filtergrams are typically taken in short bursts of 100 frames every 15 s, and processed via speckle reconstruction. Minimal cadence 10s; We only provide speckle reconstructed BFI data.
VIS and FISS can't be used simultaneously. Choose Instrument
VIS
FISS
Visible Imaging Spectrometer (VIS): Select Desired Spectral Positions along the H-alpha Line
Do not use this option if you chose FISS
Ha-1.2A
Ha-1.0A
Ha-0.8A
Ha-0.6A
Ha-0.4A
Ha-0.2A
Ha
Ha+0.2A
Ha+0.4A
Ha+0.6A
Ha+0.8A
Ha+1.0A
Ha+1.2A
Time Delay Between Line Scans. Note that the acquisition time at one position is about 2 sec
Second(s)
VIS uses a single Fabry-Pérot etalon to produce a narrow 0.07-Å bandpass over a 70" circular field of view, centered at the H-alpha line. The image scale is 0.029"/pixel, and typically 11 line positions are sampled in 15 s. Bursts of typically 25 frames are used for speckle reconstruction at each line position. We only provide speckle reconstructed VIS data.
Fast Imaging Solar Spectrograph (FISS)
Do not use this option if you chose VIS
Select the Desired Pair of Spectral Lines
Fe I 5354 Å and D3 5876 Å
Hα 6563 Å and Ca II 8542 Å
Time Cadence
(a 40" wide raster is scanned in about 60 sec)
Second(s)
FISS a scanning Echelle-type spectrograph that typically uses the Ca II H and K lines near 854 nm and the H-alpha line. Both spectral regions can be observed simultaneously using a dual-camera system. The spectrograph slit is 40" long, and a field of view of 40"x60" is typically scanned in 60 s. The H-alpha camera is a 512 x 512 CCD, while the Ca II camera is a 1004x1000 CCD. The slit width is 32 µm, which corresponds to a spatial sampling of 0.16". The spectral sampling at H-alpha is typically 0.0019 nm and at Ca II it is 0.0025 nm, and the resolving power (λ/∆λ = 1.4x105) gives a spectral resolution of 0.005 nm and 0.006 nm, respectively.
Near InfraRed Imaging Polarimeter (NIRIS)
Polarimetry Fe I 1.56 micron
Spectroscopy He I 10830 Å
Spectroscopy: Select Desired Spectral Positions along the He I 10830 Å Line
Do not use this option if you chose Polarimetry at Fe I 1.56 micron
He-1.2A
He-1.0A
He-0.8A
He-0.6A
He-0.4A
He-0.2A
He
He+0.2A
He+0.4A
He+0.6A
He+0.8A
He+1.0A
He+1.2A
Time Delay between Line Scans
Second(s)
NIRIS uses dual Fabry-Pérot etalons that provide an 85" round field of view on a 2024 x 2048 HgCdTe Teledyne closed-cycle He cooled IR array. The primary lines used by NIRIS are the Fe I 1565 nm doublet (polarimetry), and the He I 1083 nm multiplet (spectrometry). The Fe I bandpass is 0.01 nm, while the He I bandpass is 0.005 nm. The polarimetry is done via a rotating waveplate that samples 16 phase angles at each line position, and more than 100 line positions at a cadence of 10 s per full spectroscopic measurement (full-Stokes I, Q, U and V). Full NIRIS polarimetric scan is done in about 40s; We only provide Stokes profiles; In sprectroscopy mode one line position is measured in about 2s.
Cryogenic Infrared Spectrograph (CYRA). CYRA operates only in a standalone mode, no other instruments are available at that time.
Spectroscopy 2.2 micron Ti Line
Spectroscopy 4.6 micron CO BandA
Time Delay between Line Scans
Second(s)
Cyra is a fully cryogenic, folded Czerny-Turner spectrograph based on a 2048 x 2048 HgCdTe array sensitive through the 1-5 µm region. Photospheric lines offered are Ti I 2231 nm and Fe I 4064 nm. One CYRA scan lasts between 60 and 100s.
Strategy of Observations
Details of the desired observing run
Targets, Conditions, etc
Desired target(s), seeing conditions, etc