Explore Workflows

https://github.com/common-workflow-language/cwl-utils.git

Path: testdata/step_valuefrom5_wf_with_id_v1_0.cwl

Branch/Commit ID: 88ad2a6ad70d7124b094e0cb3e5f72b78078c7e2

https://github.com/lanl/BEE.git

Path: examples/cat-grep-tar/workflow.cwl

Branch/Commit ID: 77b1583234c1680c6b85a4048b1d642887bd718d

https://git.astron.nl/RD/LINC.git

Path: workflows/linc_target.cwl

Branch/Commit ID: dc7a4f725f6e8dde49b0b1db2e3fbde7fb19990a

https://git.astron.nl/RD/LINC.git

Path: workflows/linc_target/prep.cwl

Branch/Commit ID: dc7a4f725f6e8dde49b0b1db2e3fbde7fb19990a

Workflow runs group-isoforms.cwl tool using scatter for isoforms_file input. genes_filename and common_tss_filename inputs are ignored.

https://github.com/Barski-lab/workflows.git

Path: tools/group-isoforms-batch.cwl

Branch/Commit ID: b8e28a017f7b1a2900ec0fd3b3549f123f0c91b4

Landsat-8 pan-sharpening

https://github.com/cwl-for-eo/cwl-101.git

Path: tutorial-3/pan-sharpen.cwl

Branch/Commit ID: f41de311c6c77def3923f7a23f09b2dff46670af

Packed ID: main

https://github.com/common-workflow-language/cwltool.git

Path: tests/wf/mut3.cwl

Branch/Commit ID: a21728aa0e2dd0ffc1be39fdbf9bc76029e90c66

Camera calibration data (from telescope-level calibration events) will be recorded alongside science data during and around each observation night by ACADA. Different calibration event types will be recorded to the different streams at this stage. Interleaved flat-field and sky pedestal events are tagged at the telescope level, allowing the data to directly align with the functional decomposition of the CalibPipe and avoid the need of additional event-type filtering. Following this, pixel- and channel-wise camera calibration coefficients are calculated as a function of time. This process includes the computation of aggregated time-series statistics for the calibration events, as well as the detection of non-nominal pixels and time periods (UC-120-2.21). The aggregated statistics are further processed to derive the sky pedestal offsets per waveform sample, flat-fielding coefficients, and pixel timing corrections. Additionally, the CalibPipe calculates the absolute gain for each pixel and gain channel as a function of time. This process will ultimately yield a multiplicative coefficient for the absolute calibration of extracted charge into photoelectrons. To achieve accurate absolute gain and charge calibration, CalibPipe derives telescope-specific systematic corrections (UC-120-2.22) and the conversion factors from digital counts to single photoelectrons (UC-120-2.23).

https://gitlab.cta-observatory.org/cta-computing/dpps/calibrationpipeline/calibpipe.git

Path: workflows/telescope/camera/uc-120-2.20-perform-camera-calibration.cwl

Branch/Commit ID: rc-1.0

https://github.com/common-workflow-language/cwl-utils.git

Path: testdata/workflow_input_sf_expr_array.cwl

Branch/Commit ID: e413f9b185f0060ffbdd876062133d65daecb7da

Reverse the lines in a document, then sort those lines.

https://github.com/common-workflow-language/cwltool.git

Path: tests/wf/revsort.cwl

Branch/Commit ID: 526f36f93655bfb098f766ff020708b5a707513a