- JWST Cycle 1 Proposal Opportunities
- James Webb Space Telescope Call for Proposals for Cycle 1
- •JWST Cycle 1 Proposal Checklist and Resources
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- •JWST DD ERS Special Observational Policies
- •JWST DD ERS Special Submission Requirements
- •JWST DD ERS Proposal Process
- •JWST DD ERS Proposal Preparation
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- •JWST DD ERS Proposal Science Categories and Keywords
- JWST Cycle 1 Guaranteed Time Observations Call for Proposals
- •JWST Cycle 1 GTO Proposal Submission Policies
- •JWST Cycle 1 GTO Proposal Submission Process
- •JWST Cycle 2 and 3 GTO Proposal Process
- JWST GTO Observation Specifications
- James Webb Space Telescope Call for Proposals for Cycle 1
- JWST General Science Policies
- • JWST Observing Overheads and Time Accounting Policy
- • JWST Duplicate Observations Policy
- • JWST Science Parallel Observation Policies and Guidelines
- • JWST Observing Program Modification Policy
- • Policies for the Telescope Time Review Board
- • JWST Target of Opportunity Program Activation
- NASA-SMD Policies and Guidelines for the Operations of JWST at STScI
- •Policy 2 - Data Rights and Data Dissemination
- •Policy 3 - Data Requests and Facilities
- •Policy 4 - Post-Launch Commissioning of JWST
- •Policy 5 - Clarification of Extensions of Exclusive Access Data to Public Affairs Activities
- •Policy 7 - NASA Needs for Support for Other Missions
- •Policy 8 - Definition of Observing Time
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- •Policy 12 - Education and Public Outreach
- Methods and Roadmaps
- JWST Imaging
- • JWST Slit Spectroscopy
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- •Contrast Considerations for JWST High-Contrast Imaging
- •JWST Coronagraphic Observation Planning
- •JWST Coronagraphic Sequences
- •JWST Coronagraphy in ETC
- •JWST High-Contrast Imaging in APT
- •JWST High-Contrast Imaging Inner Working Angle
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- •JWST Small Grid Dither Technique
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- •Overview of Time-Series Observation (TSO) Modes
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- •Preparing Time-Series Observations with JWST
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- •Field of Regard Considerations for Moving Targets
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- •JWST Moving Target Policies
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- • JWST Dithering Overview
- JWST Duplication Checking
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- •JWST Observing Overheads Summary
- •JWST Slew Times and Overheads
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- Observing Overheads for NIRCam Imaging
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- Astronomers Proposal Tool
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- • APT Proposal Information
- APT Targets
- • APT Observations
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- Other Tools
- Mid Infrared Instrument
- • MIRI Overview
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- •MIRI MRS Simultaneous Imaging
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- MIRI Predicted Performance
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- MIRI Example Programs
- •MIRI Coronagraphy of GJ 758 b
- MIRI and NIRSpec Observations of SN1987A
- •MIRI and NIRCam Coronagraphy of the Debris Disk Archetype around Beta Pictoris
- •MIRI IFU and NIRSpec Observations of Cas A
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- Near Infrared Spectrograph
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- NIRSpec Example Programs
- NIRSpec and MIRI Observations of SN1987A
- •NIRSpec and MIRI IFU Observations of Cas A
- NIRSpec Bright Object Time Series Observations of GJ 1214b
- NIRSpec MOS Deep Extragalactic Survey
- •NIRSpec MOS Observations of NGC 346
- Understanding Data Files
- Obtaining Data
- Data Processing and Calibration Files
- JWST Data Reduction Pipeline
- • Primer and Tutorials
- • Pipeline User's Guide
- • Software Reference Documentation
- Algorithm Documentation
- • Obtaining and Installing Software
The JWST Exposure Time Calculator (ETC) allows observers to simulate sky scenes and perform signal to noise calculation for a given telescope/instrument configuration. We show the step-by-step instructions to perform ETC calculations for observations following a real science case, namely IR imaging and spectroscopy IFU observations of Supernova 1987A.
Exposure Time Calculator (ETC) instructions
These instructions are based on the ETC workbook demonstration presented at the 2017 Proposal Planning Workshop. The instructions show in detail the steps needed to create the sources, setup the instrument and run a simulation
The main goals of the ETC calculations are :
- To create an extended source using composite extended shapes and simple spectra and specify the flux and normalization parameters.
- To present example signal to noise ratio (SNR) calculations for:
Defining the sources
SN1987A consists of a bright ring, enclosing the dust ejecta material. The outer region of the dust ejecta includes several knots of shocked emission. The geometry of the dust source could be defined as:
- A dust ring with a diameter of ~1.1" and a thickness of ~0.2" for MIRI calculations.
- The central dust continuum ejecta that occupy ~4 MIRI MRS pixels.
- Discrete knots of shocked emission, for NIRSpec calculations to investigate molecular hydrogen emission at 2.12 μm.
Using the ETC web interface, it is possible to define sources within a scene. The ring part of the supernova is defined as an extended source with a flat-flux distribution and using a circular shape with a radius of 0.63".
The Source Editor panel (right side of Figure 1) includes a set of tabs that allow the user to define the characteristics of the sources in the scene. Figure 1 shows the first step in defining a new source in the scene. We start by assigning it a source identification ID, in this case the ID "ring".
The Continuum tab allows us to select an SED for the source. In this case we model the source with a Blackbody Spectrum of 400 K as shown in Figure 2.
In the normalization (Reform) tab, we can normalize the spectrum to have a flux density of 80 mJy at 10 μm as shown in Figure 3.
The shape of the source is defined in the Shape tab. In this case we select an extended source with a flat flux distribution and we give it the shape of a disk with a 0.63" radius. See Figure 4.
The ETC web interface creates a simple sketch of the scene and displays it at the bottom of the GUI. The spectrum of the source is also plotted when selected as shown in Figure 5.
Following the same procedure, it is possible to define another source in the scene, in this case the "ejecta", which we can assume is a point source with a Blackbody SED of 100 K, and with its flux density normalized to 0.1 mJy at 10 μm. Figure 6 shows the ETC workbook with both sources selected.
A third source in the scene is defined with a name "shock knot1. This will be a source of pure line emission at 2.12 μm to simulate shocked molecular hydrogen in an extended knot. This source is added in a similar manner to the instructions described above. The detailed steps for this are:
- Add a "new" source in the 'select a source' region of the ETC.
- In the ID area for the source, name the new source "shock knot1"
- Choose 'no continuum' in the "Continuum" tab for the source definition.
- In the "Renorm" tab, select 'Do not renormalize'.
- In the "Lines" tab, fill out the appropriate parameters for molecular hydrogen H2 emission: 2.12 μm wavelength, line width of 50km/s (a possible value for shocked H2 lines), and a line flux of 1.0e-16 ergs/cm2/s. The intrinsic flux of the expected emission may not be well known. The ETC can be used to estimate S/N on a range of source fluxes by changing this line emission flux, or by adding additional sources of varying flux levels.
- Click "Add" to add the line to the source. Additional lines can be added to build up a more complex emission line spectrum, but here we describe only the 2.12 μm H2 feature.
- In the "Shape" tab, keep the default point source for a compact H2 knot of emission.
- In order to offset this simulated H2 line to the outer region of the dust source, the 'shock knot1' source must be added to the scene. Highlight 'shock knot1' in the "Select a Source" region, and add it to the SN1987A using the "Add a Source" (blue) button in the "Select a Scene" area.
- Now, offset the source in the scene to the outer region of the dust emission. Do this in the "Offset" tab, by adding and saving x, y offset values of 0.4, -0.4.
Figure 7 shows the ETC workbook with all sources selected.
Overview of NIRSpec calculations
Once the sources are defined, it is possible to perform many signal to noise calculations on the scene using the different JWST instruments. This is carried out under the Calculations tab in the ETC view. For each calculation, few additional parameters need to be set under the following tabs: Backgrounds, Instrument Setup, Detector Setup, and Strategy.
For this example we used the Medium background configuration as shown in Figure 8.
Instrument Setup tab:
Based on the science goals, the selection for Grating/Filter pair should be G235M/F170LP as shown in Figure 9. Note that the ETC automatically shows the Total System Throughout for this configuration in its corresponding wavelength range.
Detector Setup tab:
In order to achieve the desired exposure time, the number of Groups is set to 10, and the number of Integrations is set to 2. Multiple integrations are used in this case to ensure that uncertain source fluxes will not saturate in the allocated exposure time. The Readout pattern used for this example is NRS IRS2, see Figure 10. The exposure time is automatically calculated and displayed. For this example the total exposure time is ~25 minutes.
In the Strategy tab it is possible to select the type of nodding with the options "In Scene" and "Off scene". We select "Off scene" so that this extended source has no residual subtraction effects. We select the wavelength 2.12 μm to correspond to run the calculation on the molecular hydrogen emission line. Note that this value has to be in the range determined by the grating/filter combination, in this case 1.66–3.17 in units of μm. We define the calculation to have offsets in x and y that correspond to the location of the extended knot of H2 emission modeled in the 'shock knot1' source. The top section of Figure 11 shows the Strategy tab and the IFU Nod selection.
Once all parameters are in place, simply click on the Calculate button to perform the calculation. This might take some time because the NIRSpec IFU ETC calculates information on the full IFU data cube (which can be saved to disk in the 'downloads' section of the ETC). Figure 11 shows the results of the calculation, a signal-to-noise of 21 is achieved on the H2 emission line. A detailed description of the ETC outputs are described in the article JWST ETC Outputs Overview.
Overview of MIRI calculations
Following a similar approach, we can perform a couple of calculations for the JWST instrument MIRI. We begin with a signal to noise calculation on the mid-infrared dust morphology using the MIRI Imaging mode.
We create a new calculation by selecting MIRI→ Imaging. This sets default values in the calculation space that need to be customized to our specific needs for this project. The few additional parameters that need to be set are under the following tabs: Backgrounds, Instrument Setup, Detector Setup, and Strategy.
In the Backgrounds tab we set the value to 'Low'. In the Instrument Setup tab we select the MIRI filter F560W. Under the Detector Setup, there are a few options for subarray. We select BRIGHTSKY for this project. From the Readout pattern we select FAST. The number of groups is set to 16 to avoid saturation and eight is the number of integrations. Leave number of exposures equal to one.
Under the Strategy tab, there is only one option which is Imaging Aperture Photometry. We center on the "ring" and modify the radii for the aperture and sky annulus as follows: aperture radius 0.6", inner sky radius 0.7", and outer sky radius 0.9". Once these parameters are set, we can perform the calculation. Figure 12 shows a screen grab of the ETC GUI with the MIRI imaging mode highlighted. The plot in the bottom left shows a recreation of what the scene looks like at the detector level. the signal to noise for this calculation yields a value of 4936.5 in a total exposure time of 355.20 s.
The warning on this calculation can be viewed in the 'Warning' tab in the Reports area. In this case, the warning simply states that the background region used for the subtraction is smaller than the science aperture area. This can lower the signal to noise in this calculation on an extended source area. In actual data processing, a larger spatial region can be defined that will improve noise results in background subtraction.
Next we show an example of MIRI spectroscopy to investigate dust composition in SN 1987A using the Medium Resolution Spectroscopy mode (MRS).
We create a new calculation by selecting MIRI→ MRS. This sets default values in the calculation space that need to be customized to our specific needs for this project. The few additional parameters that need to be set are under the following tabs: Backgrounds, Instrument Setup, Detector Setup, and Strategy.
In the Backgrounds tab we set the value to 'Low'. In the Instrument Setup tab we are presented with four channels. The science line of interest is the 12.8 μm neon line, so we select Channel 3 that spans the wavelength range 11.53-13.48 in units of μm. We leave the Disperser as the default value of 'Short'. Under the Detector Setup, there is only the FULL subarray option. From the Readout pattern we select SLOW. The number of groups is set to 7 to avoid saturation and three is the number of integrations. Leave number of exposures equal to one.
Under the Strategy tab, there are two methods: 'Nod In Scene', or 'Nod Off Scene'. We choose to 'Nod Off Scene' and use and aperture radius of 0.1". We center the calculation on the "ring" source. Once these parameters are set, we can perform the calculation. Figure 13 shows a screen grab of the ETC GUI with the MIRI MRS mode highlighted in yellow. The plot in the bottom left shows a recreation of what the scene looks like at the detector level. The signal to noise for this calculation yields a value of 110.88 in a total exposure time of 501.69 s.
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