Science Data for Webb’s First Images Now Available

 

The process to make the data for Webb’s First Images public has started at the Mikulski Archive for Space Telescopes (MAST). Visit the Webb First Image Observations webpage for a description of the programs, including additional details about the observations, and download links.

 

While it will take several hours for the data associated with these observations to transition from exclusive access to anonymous access, the data can be downloaded immediately by running the provided bulk download scripts that retrieve data from the Amazon Web Services cloud or by logging in to the MASTportal. The downloads from AWS are free and do not require an account. For large data downloads, MAST highly recommends using the AWS bulk download scripts provided to leverage the cloud to serve large data volumes efficiently to the community.

 

The JWST pipeline has not yet completed the third stage for Webb’s First Deep Field (Program ID 2736). As the products become available, they will appear in the MAST portal and download scripts will be made. Processing is expected to complete around 12 pm EDT on July 14, 2022.

 

The transfer of data to AWS has not completed for Stephan’s Quintet (Program ID 2732) and Webb’s First Deep Field (Program ID 2736). Once the copy is complete, AWS bulk download scripts will be provided on the Webb First Image Observations webpage.

 

While low-level products provided by the MAST are the same used to produce Webb’s First Images, the higher-level products available in the MAST are from the standard JWST data pipeline. The high-level products used to produce the public images are from a custom analysis of the data.

 

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MIRISim, the MIRI Simulator

Simulator

Simulators are frequently used in astronomy to model the behaviour of a telescope and instrument, and to simulate its data products. MIRI is no exception. MIRISim is the official MIRI simulator, able to model Imager, MRS and LRS simulations. Special needs not covered by MIRISim can be answered by our centre of expertise, as several members are active developpers of the simulator.

Simulators are frequently used in astronomy to model the behaviour of a telescope and instrument, and to simulate its data products. MIRI is no exception. MIRISim is the official MIRI simulator, able to model Imager, MRS and LRS simulations. Special needs not covered by MIRISim can be answered by our centre of expertise, as several members are active developpers of the simulator.

 

In parallel, MICE, the French Centre of Expertise for MIRI, has developped an IDL simulator for the coronagraphs. This simulator can be used upon request and scientists who would make use of it should contact directly MICE.

It was thus decided to develop a general MIRI simulator, MIRISim, as a communicating suite of packages. This MIRI simulator is being developed in Python by the European Consortium. It will include all functionalities of the instrument, taking into account all of the detectors effects and will be distributed worldwide.

 

MIRISim takes as input either a user defined ‘scene’ or a FITS file, and simulates an observation based on user defined Imager filters or MRS channels, and exposure parameters (number of groups, integrations, etc). The results are JWST ‘level 1B’ data which are suitable for processing with the JWST pipeline. The data produced by MIRISim is consistent with the MIRI sensitivity model, but should not be used as a replacement for the JWST Exposure Time Calculator (ETC).

MICE has been working in simulations for the Imager and LRS in Python, with some support from outside (Stephen Beard from STFC, Örs Detre from MPIA, and Steffen Rost from the University of Cologne) for integration in the general MIRISim simulator.
A stable public version has been released August 17th 2017 for general users. However, there is a “private” version « MIRICLE » for the MIRI team and collaborators, on which MICE has been working actively. 

MIRISimReleases
  • MICE’s work on MIRIMSim includes:
  •  
  • – A user manual with some exemples.
  • – A description of MIRISim.
  • – Extensive test of the public release.
  • – Investigation of the noise which has been then after corrected in SCASim.
  • – Up-dating and corrections of the part which handles the imager, which is at present (2018) evolving and maintained in the course of changing versions.
To be kept up to date with MIRISim developments, including announcements of new releases, please sign up to the announcement list.
Here

MIRISim is available on an as-is, best-effort basis, and information about MIRISim and example use cases can be found.

Here

Other attachment

Public MIRISim page
The official installation page for MIRISim

The MIRI Simulator software package, MIRISim has been released for public use on April 9, 2018.

The current version is Python 2.7 based, with a planned update to Python 3 coming soon.

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    High Level Data Analysis Tools

    Another task of MICE is to develop high level data analysis tools to be plugged at the end of the imager branch of the general STScI pipeline. Those tools need to be built from a combination of the instrument design plus the results of test data analysis. They will, therefore, only mature once test data had been fully analysed. Not only MICE will watch over this test data analysis and their results, but the MICE team will also keep track of the developments of the various software pieces and understand their functionality and interconnection.

    Specific work packages, for example the derivation of parameters for ghosts in the imager data,  the analysis and modeling of the flat field structure in the imager and in the low resolution spectrometer, the study of the background subtraction, and the issues related to the astrometry, will be specifically studied by various Working Groups (Imager, MRS, Pipeline/Calibration, RTS, etc..) ; the results will be compared and discussed within the MIRI European Consortium (EC) first and then within the US/NASA community. . 

     

     

    Although the work has been  distributed it needs to be coordinated to avoid both duplication and missing items. MICE members are not only included in the MIRI Test and Science Teams but also in all working groups working on the JWST mission. As such they are playing an active role in all discussions not only inside the MIRI European Consortium but also with the Space Telescope Science Institute (STScI) at Baltimore, the Goddard Space Flight Center (GSFC) at Greenbelt, and the Jet Propulsion Laboratory (JPL) at Pasadena, for contributing taking relevant decisions. High level imager data handling tools (e.g. for instance images deconvolution, background filtering, mapping, etc.. for the imager) are also under the responsibility of MICE.

    MICE members are also responsible for various Commissioning Activity Requests (CARs) and Commissioning Analysis Projects (CAPs).

     

    High level coronagraphs data handling tools are being built by, and under the responsibility of, the Coronagraph Working Group (CWG) at STScI: several MICE members belong to this working group and as such must be sure to not only discuss and propose solutions but also to get well acquainted with these tools in order to help the community.

     

    Many projects are underway or already accomplished. For instance :

    Exoplanets transits: data analysis.

    SN 1987A observed with MIRI.

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    Simulations

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    ARCHIVING

    Data rate

    As stated in Johns et al. (2008), JWST is the first L2 mission to be defined as a high data rate mission. JWST is also the first mission that pushes the spectrum allocation group to design a new spectra band in the 26 GHz Ka-band to meet data rates of more than 8 Mbps. JWST pushes for enhancements to the DSN capabilities that previously were limited to 5 Mbps. JWST requirements are to downlink 270 Gb science and engineering data every day. One of the main challenges for missions beyond the moon (300,000 km+) is in the spacecraft to earth communications.

    The scheme of the communications between the space-craft and the NASA ground stations is illustrated here 

    Communications

    Geostationary satellites have straight forward satellite to earth communications since they are stationary over the same spot of the earth, Low Earth Orbiting (LEO) satellites have many alternatives with ground stations and the for NASA missions the Tracking and Data Relay Satellite System (TDRSS), but the challenges for the JWST mission are that:

    Due to the earth rotation each viewing period of from a given ground station is between 8 – 14 hours a day. Communication coverage can vary greatly, based on the satellite’s ground track and latitude of ground stations.

    Ranging is required for JWST, using alternate ground stations in the southern and northern hemisphere. For LEO and L2 missions the accuracy of the ranging is dependent on the tracking of the spacecraft across the sky. For the JWSTs L2 orbit, 21 days of tracking equals about 15 minutes of tracking for a LEO spacecraft.

    The JWST original concept was to have a daily 8-hour contact using X-band with an 8 Mbps downlink rate. 8 Mbps required an allocation of a 20 MHz X-band frequency. The NASA Spectrum office objected to provide more than the 10 MHz band in X-band range and suggested using Ka-band. JWST project decided to move to K-band and have one (1) 4-hour contact per day for communication and ranging. Furthermore, data will be transmitted to Earth in an uncompressed format.

     

    It is foreseen that MIRI will observe 14% of the time during the first 650 days, which means 91 days of observations (8640000 sec.). In fast reading mode (slow mode will be used only in very special cases), the frame time is 2.7 sec for 4Mb per frame, which yield to 13 Tb. Considering side product data (including housekeeping) we estimate that 26 Tb of MIRI data will arrive to Earth during the first two years of the mission. MICE envisage therefore acquiring a 100 Tb disk for data archiving.

     

    The main reason for archiving the MIRI data in MICE is for being able to reprocess them as the pipe line developed at STScI evolves. MICE envisages therefore using a hardware similar to that used by STScI. That is 32 to 54 Gb of RAM for running the pipeline, and a Linux Based Big multinode server array (quite a powerful machine but not a “super-computer”!).

     

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    DATA PROCESSIONG TOOLS FOR MIRI

    Pipeline

    Data processing tools for MIRI data reduction are being developed by STScI on the basis of algorithms provided by the Performance Tests and Calibration Team (PTCT) and by individual institutions belonging to the European Consortium (EC). Inside the EC MICE members were heavily involved in the imager pipeline working group (IPWG),  which task was to define the overall architecture and to produce those algorithms to be coded in Python and included in the general pipeline built at STScI.

    Indeed, MICE leads the Imager and Coronagraphs Working Groups : MICE is in particular responsible for the calibration, the mosaicking, the source detection and the photometry.

     

    • The pipeline delivered by STScI has been tested in the course of changing versions (currently 7.3 – October 2019).
    • Programmes for the throw on one or several files in an automated way have been written.
    • The dependence in memory and processor according to the size of the files of entry has been studied.
    •  

    The proposed architecture shown below is in particular based on so-called “self-calibrations”. Not all of them will be applied in the general pipeline developed at STScI. A copy of this software will be kept updated at MICE’s premises. It will be the task of MICE’s management to decide when and which modifications should be made to this pipeline.

    MIRI CALIMAGE 3

    Self-calibration is commonly referred to as taking advantage of the fact that a set of dithered images will have different pixels sampling the same position in the sky. Comparing the measured signal in these pixels can be used to study the performance of the detector and to make a correction of the image, if necessary. Calibration steps in the pipe line can then be thought of as an active rather than a passive correction.

    Three primary calibration steps have been identified:

    •  – Baseline/background removal
    •  – Delta cosmic ray rejection
    •  – Solving for delta-flat and delta-dark (note that the suffix delta is used here to not confuse with calibration steps earlier on in the pipeline i.e. in cosmic ray rejection).

    Calibration images are made as close to the epoch of the observation as possible. But these calibrations may not be sensitive enough due to the change in the sky background and flat field in time. Self-calibration has the advantage that one is using the data taken at the same epoch to calculate the background and flat field.

    • For MIRI the thermal signature of the telescope and other components (<15μm) is expected to change in time and therefore require self-calibration for correction. MIRI has been designed to take dithered images that are specifically optimized for self-calibration: 12-point Reuleaux pattern and 311-point cycling pattern. 
    •  
    • Note that it may not be necessary to use self-calibration if the thermal backgrounds are more stable than predicted in the worst-case scenarios. It has to be said also that historically, Spitzer processing had a self-calibration option.  
    •  
    • However, a strategy of spatial redundancy and masking worked well in most cases. Notably for Spitzer it was used for some programs such as for observations of exoplanet transits, using a dedicated pipeline: it is part of MICE’s tasks to develop such dedicated pipe lines. 

    •  It is worth noting also that :

      •  
      • – Parallelization is foreseen for the future; it will be necessary for running Astro-Drizzle.
      •  
      • – The distribution of the data by the STScI to the users is not yet well defined: it will most probably be of the ESO/Archiving kind, although with the sending of a CD containing data and an executable version of the pipe line. It remains to be decided how MICE will proceed in that respect when data will be re-processed. 
      •  
      • – MICE will use a VO compatible archiving system for data products coming from our pipeline (and its specific extra steps), as the STScI will do (MAST: Mikulski Archive for Space Telescopes).

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    Detectors

    The 5 to 28 micron imager and spectrometer that is slated to fly aboard the JWST in 2018, MIRI (Mid-Infrared Instrument), is equipped with three  flight detector arrays, each 1024 × 1024 pixels, Si:As impurity band conductors, developed by Raytheon Vision Systems.

    JPL

    • La salle de contrôle à JPL

    JPL, in conjunction with the MIRI science team, has selected the three flight arrays along with their spares.

    In parallel, and in addition, to the tests performed at the Goddard Space Flight Center (GSFC, see report in the same page), several members of MICE supported the continued characterization at the Jet Propulsion Lab de la NASA (JPL, Pasadena en Californie), of the state-of-the-art Si:As detectors and its associated focal plane electronics (FPE), in view of understanding better the detectors behaviour and specific related issues. The goals of these tests are to: characterize the performance of readout modes; establish subarray operations; characterize changes to performance when switching between subarrays and/or readout modes; fine tune detector settings to mitigate residual artifacts; optimize anneal effectiveness; and characterize persistence. These tests are part of a continuing effort to support the MIRI pipeline development. 

    They are being followed by an extensive analysis. Thus, MIRI team members not only staffed shifts during the testing but are are also collaborating in analyzing the data taken. The 8th campaign at JPL took place during the first 2 weeks of March, 2018.
    • The room at JPL where the detectors stand

    A tutorial on how these detectors work (from M. Ressler, JPL) is available at: Detector Handout

    Rieke et al., 2015.
    Detector Handout
    For a thorough review of the detectors characteristics and performances, see this documents.
    Ressler et al., 2015.

    List

    The list below includes reports based on tests made at GSFC during which MIRI was inside ISIM (CV1, CV2, CV3), and on the 9 tests performed at JPL. The following reports are NOT intended for the general public, but rather for the professionals. Some of them my be consulted upon request (see Contact).

    • – MIRI-TR-00003-CEA: Study of the Signal to Noise Ratio, Drifts and other odd behaviours (Aug. 2012)
    • – MIRI-TR-00004-CEA: A Further Analysis of MIRI High Signal to Noise Data (Aug. 2012)
    • – MIRI-TR-00005-CEA: Impact on a Fluctuating Focal Plane Temperature on the Integration Ramps (Oct. 2012)
    • – MIRI-TR-00006-CEA: Signal drifts (July. 2013)
    • – MIRI-TR-00007-CEA: Scattered Light (July 2013)
    • – MIRI-TR-00008-CEA: Latents in darks (Aug. 2014)
    • – MIRI-TR-00009-CEA:Latents decay timescales (March 2015)
    • – MIRI-TR-00010-CEA: Slow Drifts (July 2015)
    • – MIRI-TR-00011-CEA: Fast Latents (Sept. 2015)
    • – MIRI-TR-00012-CEA: Slow Latents (Sept. 2015)
    • – MIRI-TR-00013-CEA: Sensitivity Baseline (in colaboration with M. Garcia-Marin (ESA) and Ori Fox (STScI)) (March 2016)
    • – MIRI-TR-00014-CEA: Electronic Anneal (April 2016)
    • – MIRI-TR-00015-CEA: Long Timescale Latents (March 2018)
    • – MIRI-TR-00016-CEA: Trap Mechanisms (Nov. 2016)
    • – MIRI-TR-00017-CEA: Dark Persistence (Feb. 2014)
    • – MIRI-TR-00018-CEA: Fast vs. Slow Mode (Jan. 2018, Draft)
    • – MIRI-TR-00019-CEA: Dwell Time (Jan. 2018, Draft)
    • – MIRI-TR-00020-CEA: Imprints (Jan 2018, Draft)
    •  
    • From Macarena Garcia-Marin (ESA) on BIAS Levels (July 2015)
    • From Gordon et al., MIRI Reset Switch Charge Decay: frameresets study, JWST-STScI-007340 (STScI, Baltimore, February 2020)

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    BY OR RELEVANT TO JWST & MIRI

    Documents

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    BY OR RELEVANT TO JWST & MIRI

    Documents

    These are the MICE related documents

    MICE_Management_Plan_vs8

    MICE_Management_Plan_vs8

    MICE_Requirements

    All technical details and performances of MIRI

    are described in 10 articles published in the Publications of the Astronomical Society of Pacific

    Volume 127, Issue 953, in July 2015

    Introduction

    Design_and_Build

    MIRIM

    LRS

    Coronagraphs

    MRS

    FPS

    Detectors

    Sensitivity

    Operations

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    PROPOSAL TOOLS

    Tools

    STIPS

    • Pseudocolor image of the central region of a globular cluster viewed in the Z087, J129, and F184 filters of the WFIRST Wide Field Imager, as simulated using STIPS.

    The Space Telescope Image and Spectroscopy Simulator

    It is used to simulate JWST observations of large astronomical fields.

     

    The STIPS (Space Telescope Image Product Simulator) software produces simulated imaging data for complex wide-area astronomical scenes, based on user inputs, instrument models and library catalogues for a range of stellar and/or galactic populations. It was originally developed for the JWST mission, but now has been extended to include WFIRST functionality as well. The current JWST version produces images covering the MIRI detector, either one or both NIRCam Long detectors, and either one, four, or all eight NIRCam Short detectors. STIPS includes the most current information about the telescope sensitivity, spectral elements, and detector properties; it uses the PSF model generated by WebbPSF for JWST, and it calls the appropriate Pandeia/JWST ETC modules to compute instrumental throughput and count rates. 

     

    STIPS is based on a Python module and a web interface that provides a straightforward way of creating observation simulations. In its current implementation, it runs server-side and allows users to submit simulations and view/retrieve the results .

    More on STIPS

    WebbPSF

    The PSF Simulation Tool 

    it is used to simulate detailed point spread functions for all the JWST instruments.

    The WebbPSF computes PSFs from a supplied library of optical path difference (OPD) files consistent with the JWST optical error budget, including wavefront errors in the Optical Telescope Element (OTE) and in each instrument. 10 independent statistical realizations are provided for each. Using these, WebbPSF computes observed PSFs assuming Fraunhofer (far-field) propagation. WebbPSF provides:

    – PSF simulations for direct imaging and coronagraphic modes, and for non-redundant aperture masking on NIRISS.

    – A greatly improved graphical user interface.

    – Arbitrary oversampling of output PSFs

    – Built-in functions for PSF evaluation such as producing radial profile plots, measuring encircled energy curves, FWHMs, etc.– 

    – Improved instrument properties such as normalized filter throughputs for NIRCam, NIRspec, and NIRISS, and detector pixel scales and orientations for all instruments.

    – Quick calculations using optimized matrix Fourier transforms, the fast semi-analytic coronagraphy algorithm, and the FFTW3 library (optional).

    – An easy-to-use scripting interface for integration with other tools.

    Limitations

    • The spectroscopy modes of NIRSpec and MIRI are not yet supported. Detector imperfections are likewise not included. The current OPD models do not support field-dependent wavefront error across the instrument FOVs. Future versions of WebbPSF and related software packages will address these issues.

    Simulated observations

    • have been created for each of the instruments listed below as a way to familiarize investigators with JWST data products. These high fidelity simulations were developed by JWST instrument team members, including instrument scientists at STScI and ESA. Simulation data for MIRI and NIRSpec remains available through an FTP hosted by ESA. Data files that were used to generate the simulated observations, such as catalogs of sources, SEDs, background, etc., are also provided where available. Most data are organized and formatted in substantially the same way as they would from a genuine observing program for various observing modes. 
    •  
    • Data files may be retrieved individually or, in some cases, in bulk from the linked pages listed below:
    MIRI data simulations
    • (At ESA) include an Integral Field observation with the Medium Resolution Spectrograph (MRS), a Low Resolution Spectrograph (LRS) observation, and an imaging observation (voir MIRISim) 
    NIRISS data simulations
    • include the following science modes: Imaging, Wide-Field Slitless Spectroscopy (WFSS), Single Object Slitless Spectroscopy (SOSS) and Aperture-Masking Interferometry (AMI).
    NIRISS data simulations
    • (at ESA) include observations using the Multi-Object Spectroscopy (MOS) mode and Integral Field Spectroscopy (IFU) mode.
    MIRISim
    • A simulator for the Mid-Infrared Instrument on JWST
    • Note: The format and organization of most of the data and metadata in the FITS files offered here is the same as that expected for Level-1b products.

    APT

    The Astronomer’s Proposal Tool

    APT is an integrated toolset consisting of editors for filling out proposal information, an Orbit Planner for determining feasibility of the observations, a Visit Planner for determining schedulability, diagnostic and reporting tools, a Bright Object Tool for performing bright object checks, and eventually an integrated tool which will be based on Aladin for viewing exposure specifications overlaid on FITS images.

     

    An important tool when elaborating a proposal is the Field of Regard of the JWST: the Figure illustrates the great coverage of the telescope (more on the Coordinate System and Field of Regard).

    The JWST project provides two quick-look target visibility tools to help in pre-planning observations, and for determining their feasibility, prior to entering them in APT: the General Target Visibility Tool (GTVT) predicts visibility windows and position angles for all instruments (GTV), and the Coronagraphic Visibility Tool (CVT) provides target visibility information for the NIRCam and MIRI coronagraphic modes (CVT). The JWST APT Visit Planner (VP) includes other aspects of schedulability beyond just visibility, including the availability of guide stars at relevant position angles, and any special requirements levied on the observations in APT. 

    APT is the final arbiter of schedulability.

    The APT version  2020.4 

    • has been formally released on September 8, 2020 by the Space Telescope Science Institut (STScI).  The upgrade to this new version is required for people working on JWST Cycle 1 Proposals.

    Download
    • APT 2020.4 contains the following changes for JWST:

      • Update to default Visit Planner dates: The default Visit Planner processing date range has been slipped by seven months for consistency with the change in JWST launch date. (92240)
      • Support for Background Observations for MIRI Coronagraphic Imaging: Associated background observations for MIRI Coronagraphic Imaging are now supported. These observations are associated with particular primary targets, but do not require target acquisition. Detailed guidance is provided in JDox. (92144)
      • More Acq Readout Patterns for MIRI LRS: Target Acquisition for a MIRI LRS SLITLESSPRISM observations will now allow the Acq Readout Patterns: FASTGROUPAVG8, FASTGROUPAVG16, FASTGROUPAVG32 and FASTGROUPAVG64. (91859)
      • Overhead correction for MSA proposals that use 5 shutter slit with gaps: The MPT had been creating 5 exposures when the « 5 shutter slitlet with gaps » was chosen. This has been corrected and now only 3 exposures are created which takes less time. (92084)
      • Pure Parallels are non-propriety: APT now reflects the policy that Pure Parallel observations are non-propriety with no exclusive access period by default. (91743)
      • Durations now calculated for pure parallels: Observation and visit level Science and Total Charged Durations are now populated for pure parallel proposals. (92071)

    The APT version 2020.3

    • Contained the following changes for JWST

    • Previous APT Versions and improvements

      • Review manually created MOS observations:  You can now send a manually created MOS observation to the MSA Planning Tool (MPT) for review in the Plans pane. Click the « Review in MPT » button in the observation and then go to MPT in the toolbar. (91955)
      • Timing changes: Minor timing changes (such as in dither patterns) have been introduced through resource file updates and so small changes may be seen by some users. (92171)
      • Upgrade to Java 11: APT contains its own Java library. It was updated in the HST release APT 2020.2.1 and so JWST users may be seeing this for the first time with APT 2020.3. Should be helpful for people who were getting security warnings about the previous Java. (91456)

    The APT version 2020.2

    • Contained the following changes for JWST

        • Overhead/Timing Changes: More work has been done to improve the fidelity of overheads. Your draft proposals may now report less « Charged Time » than in previous versions (due to the slew time for dithers being reduced).
        • Minor changes in graphical Timeline: Close examination of the graphical Timeline will likely show small changes in the way overheads are reported even if the total amount has not changed.
        • Change to names of Visit Planner constraints: If you need to examine the individual scheduling constraints reported in the Visit Planner you will find that the constraint names and order have changed to be more readily understandable and consistent with special requirement nomenclature. If needed, there is a Knowledge Article that explains all scheduling constraints.
        • New NIRCam WFSS Dither: A 2-point subpixel dither pattern has been added to the NIRCam WFSS template. (87291)
        • New NIRISS WFSS Dithers: 
          • Filter-dependent dithers have been implemented for the NIRISS WFSS template when GRISM=BOTH. (91506)
          • Optional 3-point “Direct Imaging” dithers have been implemented for the NIRISS WFSS template. (91741)
        • New Keywords: Debris Disks and Circumstellar Disks have been added to appropriate Science Keyword lists. (92027)

    The APT version 2020.1.2 

    • Contained the following changes for JWST

      • PDF Concatenation Error: Addresses a problem with creating the PDF Preview (or exporting the TAC PDF). Users with large image files within their Proposal PDF Attachment sometimes got a PDF Error when attempting to preview the full TAC view of their proposal. (91609)

    The APT version 2020.1.1

    • Contained the following changes for JWST

      • MPT Rewrite: There has been a major reengineering of the user experience of the MSA Planning Tool.
      • Timing Changes: The modeling of overheads has been better aligned with what has been seen in ground testing. Previous draft proposals may now report more or less  « Charged Time » than in previous versions.
      • New Coordinated Parallel options: There are three new supported prime/parallel pairings of templates available: NIRCam WFSS & MIRI Imaging, NIRCam WFSS & NIRISS Imaging, and NIRSpec MOS & MIRI Imaging.
      • Key for graphical Timeline: The graphical Timeline tool now has a link to a key (hosted in JDox) at the bottom of the display. (91536)
      • Joint HST/JWST programs: JWST Cycle 1 invites Joint Observatory Programs for HST and JWST. (91818)
      • Default Visit Planner Dates: The default date range for Visit Planner processing has been updated. For Cycle 1 the default range is now 01-Aug-2021 to 31-Mar-2023. (90480)
      • Example Science Programs: Eight more Example Science Programs have been added to the APT File Menu. (91612)
      • Optional MIRI Verification Image: For slitted MIRI LRS observations with a Target Acquisition there is now an option for a Verification Image. (91765)
      • Brighter targets for NIRCam: Support for acquisition of brighter targets by allowing additional filter choices in the NIRCam Time Series and Grism Time Series templates. (89141)
      • Additional Filter for NIRISS: The NIRISS SOSS template now allows the use of the F277W filter. (91758)
      • Was a major JWST release and had to be used for all HST and JWST GO programs. It contains the following changes for JWST:
      • MPT Rewrite: There has been a major reengineering of the user experience of the MSA Planning Tool.
      • Timing Changes: The modeling of overheads has been better aligned with what has been seen in ground testing. Previous draft proposals may now report more or less  « Charged Time » than in previous versions.
      • New Coordinated Parallel options: There are three new supported prime/parallel pairings of templates available: NIRCam WFSS & MIRI Imaging, NIRCam WFSS & NIRISS Imaging, and NIRSpec MOS & MIRI Imaging.
      • Key for graphical Timeline: The graphical Timeline tool now has a link to a key (hosted in JDox) at the bottom of the display. (91536)
      • Joint HST/JWST programs: JWST Cycle 1 invites Joint Observatory Programs for HST and JWST. (91818)
      • Default Visit Planner Dates: The default date range for Visit Planner processing has been updated. For Cycle 1 the default range is now 01-Aug-2021 to 31-Mar-2023. (90480)
      • Example Science Programs: Eight more Example Science Programs have been added to the APT File Menu. (91612)
      • Optional MIRI Verification Image: For slitted MIRI LRS observations with a Target Acquisition there is now an option for a Verification Image. (91765)
      • Brighter targets for NIRCam: Support for acquisition of brighter targets by allowing additional filter choices in the NIRCam Time Series and Grism Time Series templates. (89141)
      • Additional Filter for NIRISS: The NIRISS SOSS template now allows the use of the F277W filter. (91758)
      •  

    The APT 26.0.2

    • (May 14, 2018)

      • Pure Parallels: Improved the implementation of Pure Parallels
      • NIRSpec MSA Planning tool: Numerous updates to the NIRSpec MSA Planning tool
      • Data Volume: Corrections to data volume calculations and a check at 1/2 recorder size
      • Visit Coverage: Corrections to the visit coverage export file
      • Target Groups: Completed implementation of target groups

    The APT 25.4.4

    • (March 14, 2018)

      • Minor release – fixes a regression in Aladin; recommended for users of the Aladin tool.
      •  

    The APT 25.4.3

    • (Feb. 20, 2018)

      • Changes to the Visit Planner servers: There are now separate servers for Fixed and Solar System proposals. And Solar System proposals no longer check for guidestars.
        Fix for MIRI LRS Mapping: The spectral & spatial offsets for the mapping dither had been inverted in the Aladin display and reports.
        Improved opacity functionality in Aladin: There is now a master slider for the opacity of apertures in Aladin as well as a toggle to turn off the fill.
      •  

    The APT 25.4.2

    • (Jan. 16, 2018)

      • Timing model: Includes updates to the timing model, including revisions to the overheads for coordinated parallel observations and tight timing windows..
        MIRI No Acq option: The option for MIRI LRS and MRS observations to be executed with no Target Acquisition.
        MIRI MRS flexibility: The Wavelength and filter selection is now more flexible for MIRI MRS observations.

      • Version 25.4.2 had to be used to support JWST Early Release Science (ERS) and Guaranteed Time Observers (GTO) (and also HST Cycle 25 Phase I) submissions.
      •  

    The APT 25.4.1

    • (Dec. 5, 2017)

      • Background Noise Calculation: You can now specify (with a Special Requirement) that your observation is Background Limited and this will be considered in the Visit Planner processing.
        Operational PDF: The operational PDF has been updated to be a more complete view of your proposal. Helpful for reviewing the technical aspects of your proposal.
        ETC ID: There is now a place to record the ETC Workbook ID for each exposure specification.
        Aperture updates in Aladin: There have been changes in the representation in Aladin of many apertures.
        Data Volume: There have been many updates to the data volume calculations.
        Context Sensitive Help: With updates to JDox, CSH is mostly complete.
        Smart Accounting: You are now given feedback that Smart Accounting needs to be run and more ways to invoke it.
        NIRSpec MSA: Guidestar checking and smart accounting have been turned on for NIRSpec MSA observations.
        Processing dates: The default Visit Planner processing dates have been updates for the updated launch dates.

    The APT 25.4.01

    • (Nov. 20, 2017)

      • NIRSpec: Added Wide Aperture Target Acquisition (WATA)
        NIRSpec: Updated the NIRSpec MSA Planning Tool
        NIRSpec: Updated MSA metrology model
        NIRSpec: Updated dithers for Fixed Slit and IFU templates
        NIRCam: Updated dither for NIRCam Imaging
        NIRCam: Fixed aperture used for NIRCam Time Series
        MIRI: LRS template can now use SLOW mode
        NIRISS: TA can now use readout pattern NIS
        Aladin: Updated apertures and visualization
        Data Volume: Updated
        Timing Model: Updated (but no overheads yet for moving targets or coordinated parallels)
        Smart Accounting: Updated
        New Category: Added archival proposal category
        TSO: Added Time Series Observation special requirement (allows exposures longer than 10 ks for some templates)
        Guide stars: Catalog updated: news stars added
        Guide stars: Increased spoiler radius: some guide stars no longer viable)

    The ETC

    The Exposure Time Calculator

     

     

    it calculates the detailed performance of the observatory by modeling astronomical scenes consisting of single or multiple point and extended sources. It offers full support for all of the JWST observing modes.

    • Exemple of output from the ETC (here the signal-to-noise ratio)

    The JWST Exposure Time Calculator (ETC) version 1.5.1 was released on January 27, 2020. 

    As a note, when you login to this new version, your old workbooks will be marked « Out of Date ». They will open in Read-Only mode: this ensures that your previous results are not overwritten and remain available to you for reference. If you copy an out of date workbook, and load the copy, all its calculations will be automatically updated for you with the current version of the software.

    This new release contains late-breaking accuracy improvements, performance enhancements, and bug fixes, including:

    •  – Updating the cosmic ray model
    •  – Improving the mid-infrared thermal model
    •  – Fixing bugs for slit and slitless spectroscopy when the source is offset within the scene
    •  – Enhancing performance of the ETC during times of heavy use
    •  – Rotating PSFs to match the orientation on-sky
    •  – New and updated workbooks associated with the Example Science Programs in JDox
    •  – Addition of a narrow-band filter for NIRCam target acquisition (TA) to support observations of bright targets
    ETC Login

    Version 1.2 of the JWST ETC

    • had been released on December 2017
    • Previous Versions of ETC

       

        • – When you load them, they will open in Read-Only mode: this ensures that your previous results are not overwritten and remain available to you for reference.
        • – If you copy an out of date workbook, and load the copy, all its calculations will be automatically updated for you with the current version of the software.
        •  
        • For more information, see :
    ETC Releases and Out-of-Date Workbooks

      • In addition, JWST ETC version 1.2 features faster performance, accuracy improvements, usability enhancements, and more.

        The version 1.2.2 of the ETC had been released on March 19, 2018. This patch includes accuracy-related changes for several modes, as well as critical performance and robustness improvements.

    Accuracy Improvements
    • Calculations now treat « number of exposures » as « number of dithers ». This correctly decreases the residual flat field error for dithered observations.

    • Major accuracy improvements have been achieved for NIRCam and MIRI Coronagraphy modes, MIRI Coronagraphic Target Acquisition, and NIRISS long-wavelength Imaging and TA modes, by using a redesigned and better-sampled PSF Library.

    Simulated data sets

    MIRI

      • – MIRI Four Quadrant Phase Masks now include the effect of the quadrant boundaries on off-centered PSFs.
      • – The MIRI Lyot Coronagraphic Mask is now more appropriately sampled (positions of the pre-calculated PSFs).
      • – MIRI Coronagraphic Target Acquisition no longer erroneously has the coronagraph stops in the pupil plane.

    NIRCam

      • NIRCam Coronagraphy bar masks are now more appropriately sampled (positions of the pre-calculated PSFs).

    NIRISS

      • NIRISS Imaging in long-wavelength filters now include the pupil mask, leading to a ~16% reduction in flux. This affects the F277W filters and longer wavelengths, for Imaging and Target Acquisition modes.

    New features

      • – NIRSpec IFU and MIRI MRS modes now report saturations from both « Nod » positions independently.
      • – Coronagraphy modes now report saturations from both Science Scene and PSF subtraction source separatedly.
      • – The Coronagraphy Strategy has been enhanced by providing a total of four options under « PSF Subtraction ».
      • – « Optimal (PSF Autoscaling) » will automatically scale the PSF subtraction source to the flux of the central source before subtraction. This matches the ETC 1.2 behavior for « Optimal » subtraction.
      • – « Optimal (No PSF Autoscaling) » with no scaling of the PSF subtraction source. This matches the ETC 1.1.1 and earlier behavior for « Optimal » subtraction.
      • – « Unsubtracted Science Scene » displays only the science scene, with only the coronagraphic mask suppressing the central source.
      • – « PSF Subtraction Source only » displays the PSF subtraction source by itself, under the coronagraphic mask.

    Under the hood

      • – ETC 1.2.2 is installed on more powerful hardware, to better support heavy load as the deadlines for proposal submissions approach.
      • – Improvements have been made to database handling and resource management.
      • – Additional logging and monitoring has been added to facilitate problem investigation.
      • Note that the old workbooks from previous ETC versions are locked to facilitate comparisons..
      •  
      • – When you load them, they will open in read-only mode. This ensures that your previous results are not overwritten and remain available to you for reference.
      • – When you copy an out-of-date workbook and load the copy, all of its calculations will be automatically updated for you with the current version of the software.
      •  
      •  
      • See the Release Notes for details, and be sure to review the Known Issues for this release (and the previous ones).
    Release Notes
    Known Issues
      • Several JWST community oriented products and tools had been launched at the January 2017 AAS meeting and provided the following links to the main elements:
    JDOX
    ETC
    ERS
    JWST

  • Programs & Projects Accomplishments

  • The LABCOM INCLASS

  • Meetings and Conferences

  • Tools

  • Documents

  • Detectors

  • Pipeline

  • Data rate

  • High level data analysis tools

  • Simulator

  • Science Data for Webb’s First Images Now Available

    • Meetings and Conferences

    Centre

    BY OR RELEVANT TO JWST & MIRI

    Meetings and Conferences

    Early Science with JWST

    Centre

    BY OR RELEVANT TO JWST & MIRI

    Meetings and Conferences

    Early Science with JWST

    2018

    • JWST Data Analysis and Calibration 5 novembre 2018 - workshop at STScI, Baltimore (MD), on November 5th, 2018 Informations
    • JWST : Launch, Commissioning, and Cycle 1 Science 22 août 2018 - A science meeting to be held in Vienna, Austria, Aug. 20-22, 2018 during the IAU 2018 General Assembly
    • American Astronomical Society 232nd Meeting 3 juin 2018 - It will be held at Denver (CO) June 3-7, 2018. There will be a JWST booth, and DD-ERS special sessions AAS 2018
    • Early Science with JWS 1 avril 2018 - Critical to the success of the James Webb Space Telescope (JWST) mission is the ability to bring the scientific community quickly up to speed on the instruments and scientific capabilities of the observatory. EWASS 2018, taking place on 3-6 April 2018, offers a perfect opportunity to inform the European community of the status of the JWST mission, and discuss the scientific programs that will define the first months of operations, including the Guaranteed Time Observations (GTO) and the Early Release Science (ERS) programs. Now that the ERS programs have been selected, EWASS 2018 will offer a timely forum to engage with the ERS teams, as well as encourage scientific discussion of future JWST plans.As part of the science meeting, EWASS 2018 will host the « Early Science with JWST » symposium S1 on 3-4 April 2018.
    • Science with Precision Astrometry 13 mars 2018 - Precision astrometry is providing many advances in our understanding of the physics of the local universe, which will expand as the HST time baseline increases, the Gaia DR2 catalog is released, JWST is launched and new ground-based facilities come on-line. This workshop will address the state of our current and near-future facilities, the techniques that are needed to achieve precision astrometry, science results and the future landscape.
    • Social Media Q&A Session on Twitter 26 février 2018 - STScI held the first Q&A session on their JWST Observer Twitter account on Monday, February 26, 2018 to help the community prepare for the JWST Cycle 1 proposals. Another session will take place on Monday, March 5 at 3:00 pm (ET).
    • JWST Data Analysis and Calibration 5 février 2018 - Workshop at STScI, Baltimore (MD)

    2017

    2016

  • Programs & Projects Accomplishments

  • The LABCOM INCLASS

  • Meetings and Conferences

  • Tools

  • Documents

  • Detectors

  • Pipeline

  • Data rate

  • High level data analysis tools

  • Simulator

  • Science Data for Webb’s First Images Now Available

    • The LABCOM INCLASS

    The LABCOM INCLASS

    Le LabCom Innovative Common Laboratory For Space Spectroscopy (INCLASS) mis en place entre l’Institut d’Astrophysique Spatiale (IAS) et la PME ACRI-ST a pour but le  développement de nouvelles méthodologies pour la fusion des données d’imagerie et de spectroscopie.

    Ces méthodologies seront appliquées aux données de l’imageur et du spectrometre MRS de l’instrument MIRI du JWST, et des missions Sentinel 2 et 3 du programme européen Copernicus. Le LabCom a été créé le 1er mai 2021, et est financé par l’Agence nationale de la Recherche (ANR) pour une durée de quatre années.   Il apportera au centre d’expertise MICE des compétences complémentaires sur le spectromètre MRS, ainsi que sur la fusion des données imageur-MRS. 

     

    The Innovative Common Laboratory For Space Spectroscopy (INCLASS) set up between the Institut d’Astrophysique Spatiale (IAS) and the SME ACRI-ST aims to develop new methodologies for spectral-imaging data fusion.

      These methodologies will be applied to data taken by the imager and the spectrometer MRS of the JWST/MIRI instrument, and to data taken by the Sentinel 2 and 3 missions of the European Copernicus programme. 

     

    The LabCom was created on 1 May 2021, and is funded by the French National Research Agency (ANR) for a period of four years. It will provide the MICE centre of expertise with complementary expertise on the MRS spectrometer, as well as on MRS-imager data fusion.

     

    Fore more information see here if you have any questions.

    Retour

  • Programs & Projects Accomplishments

  • The LABCOM INCLASS

  • Meetings and Conferences

  • Tools

  • Documents

  • Detectors

  • Pipeline

  • Data rate

  • High level data analysis tools

  • Simulator

  • Science Data for Webb’s First Images Now Available

    • JWST