Campuses:
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| datachallenge [2017/07/20 14:48] – [Data Challenges] borrill | datachallenge [2018/02/14 17:27] (current) – [Subscribing to this Group's Mailing List] borrill | ||
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| - | ===== Subscribing to this Group' | ||
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| - | Send e-mail to: \\ | ||
| - | probedatachallenge+subscribe@umn.edu | ||
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| - | The subject and body of the e-mail can be empty. Within minutes you will receive an automated e-mail response asking you to click on a radio button to subscribe. The group' | ||
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| - | __**Important: | ||
| ===== Data Challenges ===== | ===== Data Challenges ===== | ||
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| We are at the very beginning stages of defining this data challenge. Nothing written here should be understood as finalized. Please feel free to contribute to the definition of the data challenge. | We are at the very beginning stages of defining this data challenge. Nothing written here should be understood as finalized. Please feel free to contribute to the definition of the data challenge. | ||
| - | Following the model used in CMB-S4, we will define Data Challenge X.Y as the application of Mission Model X to Sky Model Y. We anticipate the first iteration (DC_0.0) to be available in mid-July. This will primarily be a test case for the construction and analysis processes, with more detailed and representative models to follow. | + | Following the model used in CMB-S4, we will define Data Challenge X.Y as the application of Mission Model X to Sky Model Y. |
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| - | Details of specific mission and sky models are provided below. | + | |
| Data challenges will be made available at NERSC at / | Data challenges will be made available at NERSC at / | ||
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| * Focal plane layout | * Focal plane layout | ||
| * Noise model for each detector | * Noise model for each detector | ||
| + | * Cooler cycle frequency & duration (if any) | ||
| ===Observation Model=== | ===Observation Model=== | ||
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| and any polarization modulation | and any polarization modulation | ||
| * HWP rotation rate or stepping frequency and angle | * HWP rotation rate or stepping frequency and angle | ||
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| - | Given an observation and an advanced instrument model, we will use the TOAST tools to generate simulated hit and noise maps. | ||
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| - | [[https:// | ||
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| ====Sky Model==== | ====Sky Model==== | ||
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| A sky model comprises four elements: | A sky model comprises four elements: | ||
| * Scalar, tensor and non-Gaussian CMB | * Scalar, tensor and non-Gaussian CMB | ||
| - | * Extragalactic foregrounds | + | * Extragalactic foregrounds, including their lensing. |
| * Galactic foregrounds | * Galactic foregrounds | ||
| * Zodiacal emission | * Zodiacal emission | ||
| - | ==Sky Model 0== | ||
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| - | * Unlensed scalar and tensor CMB with zero and non-zero r | ||
| - | * PySM galactic foregrounds including AME, thermal dust, free-free & synchrotron (a2d7f1s3) | ||
| - | * No extragalactic foregrounds or lensing | ||
| - | * No zodiacal emission | ||