🎹
Hello
🎹
Hello
  • Crowrite
  • 2025
    • 0225-TODO
    • 0107-Convolution
    • 0115-file saving
    • 0118-recycling method factor
    • 0121-constraints on tensor-scalar ratio
    • 0122-better way to use my own code
    • 0124-r constraint
    • 0128-new r constraint
    • 0311-MCA
    • 0331-PSM simulation
  • 2024
    • 0209-Linux and git basic command
    • 0213-How to take notes for research
    • 0214-Scientific method
    • 0215-Scientific method
    • 0221-Statistical properties of polarized radio sources at high frequency... arxiv:1003.5846
    • 0223-Primordial B-mode Diagnostics and Self Calibrating the CMB Polarization arxiv:0912.3532
    • 0226-it is customary to mask detected point sources in order to eliminate this spurious contribution
    • 0227-(WMAP) Observations: Foreground Emission arxiv:0302208
    • 0228-Ali-first light
    • 0229-Masking versus removing point sources in CMB data: arxiv:1207.2315
    • 0301-Galactic cold Clump
    • 0305-constrained realization and CMB S4
    • 0306-BICEP setup
    • 0307-Bicep setup
    • 0308-QUIJOTE
    • 0311-SPT point source catelogue
    • 0312-Jaffe Thesis: Foreground Challenge to CMB Polarization: Present Methodologies and New Concepts
    • 0314-python logger
    • 0318-The radio source counts at 15 GHz and their implications for cm-wave CMB imaging
    • 0320-Component separation methods for the PLANCK mission
    • 0326-Low-$\ell$ CMB analysis and inpainting Starck 2013
    • 0328-Sparsity
    • 0329-Morphological component analysis on the sphere
    • 0410-Planck 2018 V Planck 2015 IX
    • 0411- Fan region and Gum nebula, Coma and Virgo cluster
    • 0417-vec.ctypes.data
    • 0419-Stokes parameter
    • 0430-PBH
    • 0520-ACT Extragalactic Point Sources in the Southern Surveys at 150, 220 and 280 GHz
    • 0521-Astrometry
    • 0522-AGN Two-season ACTPol Extragalactic Point Sources and their Polarization properties
    • 0523-classmethod and static method
    • 0528-ACT DR5 maps of 18 000 square degrees of the microwave sky from ACT 2008-2018 data
    • 0619-Gaussian profile
    • 0619-EB noise level
    • 0703-bias from wrong covariance matrix estimation
    • 0718-np.random.choice
    • 0807-ps rmv brainstorm
    • 0814-test-inline-formula
    • 0814-healpy lon lat scope
    • 0816-change $ to $$
    • 0821-len() for np.ndarray
    • 0821-angdist snippets and hp.ang2pix lonlat range
    • 0823-same name of some variable
    • 0828-purity and completeness
    • 0904-template fitting advantage over matched filter
    • 0910-FUTURE CODE
    • 0911-EB leakage test
    • 0918-add prior to chi square fitting
    • 0929-PS results comparison
    • 1002-apodization
    • 1011-power spectrum estimation for partial sky
    • 1015-215GHz and 95GHz / th noise power spectrum
    • 1015-conference
    • 1020-compare different method pipeline-star
    • 1029-mask small scale structure
    • 1030-smoothing maps precautions
    • 1031-inpainting debug
    • 1031-unit test
    • 1105-inpainting steps
    • 1108-git tag
    • 1114-cut how many number PS can give good estimate of other components
    • 1118-nested title in markdown
    • 1122-some markdown format
    • 1202-lmax for maps
    • 1203-theory noise level
    • 1205-python local variable
    • 1210-BAO
    • 1217-pandas index
    • 1225-multiunion and reduce lists
  • Biophysics
    • Claycomb
      • Terminology
  • QUATA
    • term
Powered by GitBook
On this page
  • First light [ CMB | MEETING ]
  • Matrix based pipeline
  • CROW
  • MEMO
Edit on GitHub
  1. 2024

0228-Ali-first light

Previous0227-(WMAP) Observations: Foreground Emission arxiv:0302208Next0229-Masking versus removing point sources in CMB data: arxiv:1207.2315

Last updated 7 months ago

First light [ CMB | MEETING ]

BICEP pipeline and their thesis ACT thesis

Matrix based pipeline

CROW

what is the model of point sources. (beam profile, effective beam? and what is the variance in the chi square.(CMB+NOISE?)) what do point sources catalog have in their data. how to consider its variability? why not using different ways to estimate the phetometry? \

MEMO

the method to reduce the ILC bias.(The Atacama Cosmology Telescope: High-resolution component-separated maps across one-third of the sky. arxiv:2307.01258)

pipeline_1
pipeline_2
pipeline_3
pipeline_4