Explore Workflows

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

Path: testdata/scatter-wf1_v1_0.cwl

Branch/Commit ID: c1875d54dedc41b1d2fa08634dcf1caa8f1bc631

Assemble a set of reads using SKESA

https://github.com/ncbi/pgap.git

Path: assemble.cwl

Branch/Commit ID: 2afb5ebafd1353ba063cc74ee9a7eaf347afce5c

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

Path: testdata/workflow_input_format_expr.cwl

Branch/Commit ID: c1875d54dedc41b1d2fa08634dcf1caa8f1bc631

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

Path: testdata/scatter-wf2_v1_0.cwl

Branch/Commit ID: c1875d54dedc41b1d2fa08634dcf1caa8f1bc631

https://github.com/ncbi/pgap.git

Path: task_types/tt_fscr_calls_pass1.cwl

Branch/Commit ID: 2afb5ebafd1353ba063cc74ee9a7eaf347afce5c

When DPPS receives a new DL0 data product, the CalibPipe is triggered to process the calibration events. The CalibPipe performs charge integration and peak time extraction for the entire set of calibration events, and computes aggregated time-series statistics, including the mean, median, and standard deviation. Using these aggregated statistics, the CalibPipe identifies faulty camera pixels, such as those affected by starlight, by applying various outlier detection criteria. Time periods with a significant number of faulty pixels, exceeding a predefined threshold, are flagged as invalid. A refined treatment can then be applied to these time periods to account for the issues.

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

Path: workflows/telescope/camera/uc-120-2.21-assess-statistical-description.cwl

Branch/Commit ID: camcalib_cwl

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: 81949412f693d624e10883485ac2758c9067a50f

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: camcalib_cwl

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

Path: testdata/step_valuefrom5_wf_with_id_v1_0.cwl

Branch/Commit ID: c1875d54dedc41b1d2fa08634dcf1caa8f1bc631

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

Path: testdata/cond-wf-004.1.cwl

Branch/Commit ID: c1875d54dedc41b1d2fa08634dcf1caa8f1bc631