Difference between revisions of "Coldspotz June Visit to Pasadena"
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'''Concepts Learnt:''' | '''Concepts Learnt:''' | ||
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1. Planck vision is not as sharp as WISE. Need WISE to get better position for source. W4 or W3 is the band of choice since | 1. Planck vision is not as sharp as WISE. Need WISE to get better position for source. W4 or W3 is the band of choice since | ||
they both sample dust emission. Sometimes multiple W4 or W3 sources might be within the Planck beam. If one of the sources is | they both sample dust emission. Sometimes multiple W4 or W3 sources might be within the Planck beam. If one of the sources is | ||
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4. Generating spectral energy distribution of a source (Brightness vs Wavelength). Different classes of objects show different spectral energy | 4. Generating spectral energy distribution of a source (Brightness vs Wavelength). Different classes of objects show different spectral energy | ||
| − | distributions. | + | distributions. Examples of object classes are asteroids, stars, stars with dust shells/disks, dusty nearby galaxies, planetary nebulae, supermassive black holes, distant star-forming galaxies. |
5. Using morphology of sources using SDSS or 2MASS to get independent confirmation of nature of source. Always remember to use the | 5. Using morphology of sources using SDSS or 2MASS to get independent confirmation of nature of source. Always remember to use the | ||
most accurate coordinates for the source - this is NOT the Planck coordinates. | most accurate coordinates for the source - this is NOT the Planck coordinates. | ||
Revision as of 19:25, 19 June 2012
Schedule during the Visit: Media:schedule.pdf
Concepts Learnt:
1. Planck vision is not as sharp as WISE. Need WISE to get better position for source. W4 or W3 is the band of choice since they both sample dust emission. Sometimes multiple W4 or W3 sources might be within the Planck beam. If one of the sources is exceptionally bright, that is most likely our counterpart. Otherwise, there could be multiple contributors to Planck flux densities.
2. Fitting a model to data and testing the accuracy of the model using additional data e.g. IRAS, 2MASS
3. Deriving a new model which fits all the data and using that to conclude nature of the source.
4. Generating spectral energy distribution of a source (Brightness vs Wavelength). Different classes of objects show different spectral energy distributions. Examples of object classes are asteroids, stars, stars with dust shells/disks, dusty nearby galaxies, planetary nebulae, supermassive black holes, distant star-forming galaxies.
5. Using morphology of sources using SDSS or 2MASS to get independent confirmation of nature of source. Always remember to use the most accurate coordinates for the source - this is NOT the Planck coordinates.
