CoolWiki - User contributions [en]

File:Aas cs2.JPG

2013-01-21T06:52:21Z

Chary:

File:Aas cs1.JPG

2013-01-21T06:50:05Z

Chary:

File:ColdSpotz6 17Dec w rrceits.xlsx

2013-01-16T02:24:30Z

Chary:

File:ColdSpotz Sci2013.pdf

2013-01-11T08:43:02Z

Chary:

File:COLD SPOTZ 12.14v2.xlsx

2012-12-15T02:40:22Z

Chary:

File:ColdSpotz v3.xls

2012-11-09T06:39:09Z

Chary:

File:ColdSpotz3.xlsx

2012-11-06T02:14:30Z

Chary:

Cold Spotz Current Research Activities

2012-09-25T01:12:12Z

Chary:

Coldspotz June Visit to Pasadena

2012-08-08T18:23:41Z

Chary:

'''Schedule during the Visit:''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

[[File:6.jpg|600px|Gang@JPL courtesy of Chelen]]

[[File:7.jpg|600px|Presenting results]]

[[File:8.jpg|600px|Welcome to Planck-land]]

[[File:9.jpg|400px|Tough work!]]

'''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 sources contributing to the Planck flux density.

2. Fitting a model to data and testing the accuracy of the model using additional data e.g. other Planck bands, IRAS, 2MASS

3. Deriving a new model which fits all the data and using that to conclude nature of the source. Normalization of the model to the measured flux densities is important to get the true best fit.

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.

6. Statistics - what is signal to noise, why is the measurement of uncertainty or noise important, how can one estimate whether a fit is good when there are multiple data points with different uncertainties.

Coldspotz June Visit to Pasadena

2012-08-08T18:23:26Z

Chary:

'''Schedule during the Visit:''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

[[File:6.jpg|600px|Gang@JPL courtesy of Chelen]]

[[File:7.jpg|600px|Presenting results]]

[[File:8.jpg|600px|Welcome to Planck-land]]

[[File:9.jpg|200px|Tough work!]]

'''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 sources contributing to the Planck flux density.

2. Fitting a model to data and testing the accuracy of the model using additional data e.g. other Planck bands, IRAS, 2MASS

3. Deriving a new model which fits all the data and using that to conclude nature of the source. Normalization of the model to the measured flux densities is important to get the true best fit.

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.

6. Statistics - what is signal to noise, why is the measurement of uncertainty or noise important, how can one estimate whether a fit is good when there are multiple data points with different uncertainties.

File:9.jpg

2012-08-08T18:22:43Z

Chary: i could tear my hair out!

i could tear my hair out!

Coldspotz June Visit to Pasadena

2012-08-08T18:20:47Z

Chary:

'''Schedule during the Visit:''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

[[File:6.jpg|600px|Gang@JPL courtesy of Chelen]]

[[File:7.jpg|600px|Presenting results]]

[[File:8.jpg|600px|Welcome to Planck-land]]

'''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 sources contributing to the Planck flux density.

2. Fitting a model to data and testing the accuracy of the model using additional data e.g. other Planck bands, IRAS, 2MASS

3. Deriving a new model which fits all the data and using that to conclude nature of the source. Normalization of the model to the measured flux densities is important to get the true best fit.

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.

6. Statistics - what is signal to noise, why is the measurement of uncertainty or noise important, how can one estimate whether a fit is good when there are multiple data points with different uncertainties.

File:7.jpg

2012-08-08T18:20:22Z

Chary: presenting results!

presenting results!

Coldspotz June Visit to Pasadena

2012-08-08T18:19:46Z

Chary:

'''Schedule during the Visit:''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

[[File:6.jpg|600px|Gang@JPL courtesy of Chelen]]

[[File:8.jpg|600px|Welcome to Planck-land]]

'''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 sources contributing to the Planck flux density.

2. Fitting a model to data and testing the accuracy of the model using additional data e.g. other Planck bands, IRAS, 2MASS

3. Deriving a new model which fits all the data and using that to conclude nature of the source. Normalization of the model to the measured flux densities is important to get the true best fit.

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.

6. Statistics - what is signal to noise, why is the measurement of uncertainty or noise important, how can one estimate whether a fit is good when there are multiple data points with different uncertainties.

File:8.jpg

2012-08-08T18:18:33Z

Chary: Welcome to the world of Planck

Welcome to the world of Planck

Coldspotz June Visit to Pasadena

2012-06-19T19:28:08Z

Chary:

'''Schedule during the Visit:''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

[[File:6.jpg|600px|Gang@JPL courtesy of Chelen]]

'''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 sources contributing to the Planck flux density.

2. Fitting a model to data and testing the accuracy of the model using additional data e.g. other Planck bands, IRAS, 2MASS

3. Deriving a new model which fits all the data and using that to conclude nature of the source. Normalization of the model to the measured flux densities is important to get the true best fit.

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.

6. Statistics - what is signal to noise, why is the measurement of uncertainty or noise important, how can one estimate whether a fit is good when there are multiple data points with different uncertainties.

Coldspotz June Visit to Pasadena

2012-06-19T19:25:25Z

Chary:

'''Schedule during the Visit:''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

[[File:6.jpg|600px|Gang@JPL courtesy of Chelen]]

'''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.

Coldspotz June Visit to Pasadena

2012-06-19T19:23:25Z

Chary:

Cold Spotz Current Research Activities

2012-06-19T19:17:50Z

Chary:

Cold Spotz Current Research Activities

2012-06-19T19:15:58Z

Chary:

[[File:ColdSpotz.jpg]]

=[[Cold Spotz Suggested Reading List]]=

=[[Cold Spotz Proposal]]=
This page will be used to assemble the pieces for the proposal we are writing. See [[2012 proposal instructions]] for, well, instructions!

=[[Cold Spotz Spring work]]=

=[[Coldspotz June Visit to Pasadena]]=

=Miscellaneous=

[[File:PlanckModel04.jpg]] [[File:IMG_7380.jpg]]

Project #1: Build your Planck model:
The paper parts for a Planck model can be found at [http://planck.cf.ac.uk/education/model]. Kat's model (the one furthest to the right above) actually has the reflection of the focal plane in the mirror the correct way up.

Project #2: Launch costs:
What is the relationship between launch cost and satellite size is. Does it cost more to go where Planck is, or to go where television satellites are, or to go where the international space station is?

Project #3: One Jansky is the flux density you receive if you hold a 60W light bulb at what distance?

Project #4: Take a look at Topic 5 on the Suggested Reading List

Project #5: February 27, 2012: There are 4 planets visible in the night sky - Jupiter, Mercury, Venus and Mars. Try to spot them. Mercury and Venus will be visible around sunset - Why? Jupiter and Mars will be visible through most of the evening. Use the
relative motion of the planets (i.e. the angular separation between the planets) to infer how far they are from us.

Project #6: The sun is red in the morning, whitish/yellow in the middle of the day and red again in the evening. Since color is related to temperature, does that mean the Sun is changing in temperature? No. Difference in color is due to light of a particular frequency being scattered away by the dust/molecules in the atmosphere. A dust grain most efficiently scatters wavelengths of its own size. There are more small grains than large grains, so shorter wavelengths (blue) get scattered more than larger wavelengths (red).

Project #7: If a star had a 40AU dust shell around it and was at a distance of 10pc what would the size of the dust shell be? Would it be extended as seen by WISE? No. It would be 4 arcsec while WISE has a spatial resolution of 12 arcsec at wavelengths where it can see dust emission.
If a galaxy of radius 10 kpc was at a distance of 10 Mpc, would it be extended as seen by WISE? Yes. It would be 412 arcseconds in diameter.

Wasnt that solar eclipse on May 20th cool?

Proposal Structure:
1. Title - Classification of Compact Submillimeter Sources in the Planck Archive

2. Goal: What are you going to do (Chelen)

3. Motivation: Why are you going to do it (Chris)

4. Methodology: How you are going to do it (Kat)

5. Timescale: What is the plan and what are the milestones (Denise)

6. Questions and concepts you expect to understand and share with the students. ("Involving students involved in the data analysis" is not a good answer - details please). Some ideas: what is a black body, using the peak wavelength as a measure of temperature, working with data in excel, how astronomers draw conclusions from data, how one can differentiate between galactic and extragalactic sources, why cant this be done with SOFIA, why do we need to launch Planck to L2?

7. What new teaching skills do you plan to develop based on this research program

8. We'll put in an abstract in the end which summarizes all this.

Figures for the proposal: all sky image and why we are looking outside the Galactic plane; cutouts of Planck, IRAS and WISE images of the same field with Planck beam overlaid; also, histogram of Planck/W1 flux density, and Planck/W2 and Planck/W3 and Planck/W4 flux density.

Cold Spotz Current Research Activities

2012-06-19T19:15:10Z

Chary:

[[File:ColdSpotz.jpg]]

=[[Cold Spotz Suggested Reading List]]=

=[[Cold Spotz Proposal]]=
This page will be used to assemble the pieces for the proposal we are writing. See [[2012 proposal instructions]] for, well, instructions!

=[[Cold Spotz Spring work]]=

=[[Cold Spotz June Visit to Pasadena]]=

=Miscellaneous=

[[File:PlanckModel04.jpg]] [[File:IMG_7380.jpg]]

Project #1: Build your Planck model:
The paper parts for a Planck model can be found at [http://planck.cf.ac.uk/education/model]. Kat's model (the one furthest to the right above) actually has the reflection of the focal plane in the mirror the correct way up.

Project #2: Launch costs:
What is the relationship between launch cost and satellite size is. Does it cost more to go where Planck is, or to go where television satellites are, or to go where the international space station is?

Project #3: One Jansky is the flux density you receive if you hold a 60W light bulb at what distance?

Project #4: Take a look at Topic 5 on the Suggested Reading List

Project #5: February 27, 2012: There are 4 planets visible in the night sky - Jupiter, Mercury, Venus and Mars. Try to spot them. Mercury and Venus will be visible around sunset - Why? Jupiter and Mars will be visible through most of the evening. Use the
relative motion of the planets (i.e. the angular separation between the planets) to infer how far they are from us.

Project #6: The sun is red in the morning, whitish/yellow in the middle of the day and red again in the evening. Since color is related to temperature, does that mean the Sun is changing in temperature? No. Difference in color is due to light of a particular frequency being scattered away by the dust/molecules in the atmosphere. A dust grain most efficiently scatters wavelengths of its own size. There are more small grains than large grains, so shorter wavelengths (blue) get scattered more than larger wavelengths (red).

Project #7: If a star had a 40AU dust shell around it and was at a distance of 10pc what would the size of the dust shell be? Would it be extended as seen by WISE? No. It would be 4 arcsec while WISE has a spatial resolution of 12 arcsec at wavelengths where it can see dust emission.
If a galaxy of radius 10 kpc was at a distance of 10 Mpc, would it be extended as seen by WISE? Yes. It would be 412 arcseconds in diameter.

Wasnt that solar eclipse on May 20th cool?

Proposal Structure:
1. Title - Classification of Compact Submillimeter Sources in the Planck Archive

2. Goal: What are you going to do (Chelen)

3. Motivation: Why are you going to do it (Chris)

4. Methodology: How you are going to do it (Kat)

5. Timescale: What is the plan and what are the milestones (Denise)

6. Questions and concepts you expect to understand and share with the students. ("Involving students involved in the data analysis" is not a good answer - details please). Some ideas: what is a black body, using the peak wavelength as a measure of temperature, working with data in excel, how astronomers draw conclusions from data, how one can differentiate between galactic and extragalactic sources, why cant this be done with SOFIA, why do we need to launch Planck to L2?

7. What new teaching skills do you plan to develop based on this research program

8. We'll put in an abstract in the end which summarizes all this.

Figures for the proposal: all sky image and why we are looking outside the Galactic plane; cutouts of Planck, IRAS and WISE images of the same field with Planck beam overlaid; also, histogram of Planck/W1 flux density, and Planck/W2 and Planck/W3 and Planck/W4 flux density.

Cold Spotz Current Research Activities

2012-06-19T19:14:40Z

Chary:

Cold Spotz Current Research Activities

2012-06-19T19:14:17Z

Chary:

[[File:ColdSpotz.jpg]]

=[[Cold Spotz Suggested Reading List]]=

=[[Cold Spotz Proposal]]=
This page will be used to assemble the pieces for the proposal we are writing. See [[2012 proposal instructions]] for, well, instructions!

=[[Cold Spotz Spring work]]=

=[[Coldspotz June Visit to Pasadena]]=

=...Plenty of space for anything you want=

[[File:PlanckModel04.jpg]] [[File:IMG_7380.jpg]]

Project #1: Build your Planck model:
The paper parts for a Planck model can be found at [http://planck.cf.ac.uk/education/model]. Kat's model (the one furthest to the right above) actually has the reflection of the focal plane in the mirror the correct way up.

Project #2: Launch costs:
What is the relationship between launch cost and satellite size is. Does it cost more to go where Planck is, or to go where television satellites are, or to go where the international space station is?

Project #3: One Jansky is the flux density you receive if you hold a 60W light bulb at what distance?

Project #4: Take a look at Topic 5 on the Suggested Reading List

Project #5: February 27, 2012: There are 4 planets visible in the night sky - Jupiter, Mercury, Venus and Mars. Try to spot them. Mercury and Venus will be visible around sunset - Why? Jupiter and Mars will be visible through most of the evening. Use the
relative motion of the planets (i.e. the angular separation between the planets) to infer how far they are from us.

Project #6: The sun is red in the morning, whitish/yellow in the middle of the day and red again in the evening. Since color is related to temperature, does that mean the Sun is changing in temperature? No. Difference in color is due to light of a particular frequency being scattered away by the dust/molecules in the atmosphere. A dust grain most efficiently scatters wavelengths of its own size. There are more small grains than large grains, so shorter wavelengths (blue) get scattered more than larger wavelengths (red).

Project #7: If a star had a 40AU dust shell around it and was at a distance of 10pc what would the size of the dust shell be? Would it be extended as seen by WISE? No. It would be 4 arcsec while WISE has a spatial resolution of 12 arcsec at wavelengths where it can see dust emission.
If a galaxy of radius 10 kpc was at a distance of 10 Mpc, would it be extended as seen by WISE? Yes. It would be 412 arcseconds in diameter.

Wasnt that solar eclipse on May 20th cool?

Proposal Structure:
1. Title - Classification of Compact Submillimeter Sources in the Planck Archive

2. Goal: What are you going to do (Chelen)

3. Motivation: Why are you going to do it (Chris)

4. Methodology: How you are going to do it (Kat)

5. Timescale: What is the plan and what are the milestones (Denise)

6. Questions and concepts you expect to understand and share with the students. ("Involving students involved in the data analysis" is not a good answer - details please). Some ideas: what is a black body, using the peak wavelength as a measure of temperature, working with data in excel, how astronomers draw conclusions from data, how one can differentiate between galactic and extragalactic sources, why cant this be done with SOFIA, why do we need to launch Planck to L2?

7. What new teaching skills do you plan to develop based on this research program

8. We'll put in an abstract in the end which summarizes all this.

Figures for the proposal: all sky image and why we are looking outside the Galactic plane; cutouts of Planck, IRAS and WISE images of the same field with Planck beam overlaid; also, histogram of Planck/W1 flux density, and Planck/W2 and Planck/W3 and Planck/W4 flux density.

Cold Spotz Current Research Activities

2012-06-19T19:14:05Z

Chary:

[[File:ColdSpotz.jpg]]

=[[Cold Spotz Suggested Reading List]]=

=[[Cold Spotz Proposal]]= This page will be used to assemble the pieces for the proposal we are writing. See [[2012 proposal instructions]] for, well, instructions!

=[[Cold Spotz Spring work]]=

=[[Coldspotz June Visit to Pasadena]]=

=...Plenty of space for anything you want=

[[File:PlanckModel04.jpg]] [[File:IMG_7380.jpg]]

Project #1: Build your Planck model:
The paper parts for a Planck model can be found at [http://planck.cf.ac.uk/education/model]. Kat's model (the one furthest to the right above) actually has the reflection of the focal plane in the mirror the correct way up.

Project #2: Launch costs:
What is the relationship between launch cost and satellite size is. Does it cost more to go where Planck is, or to go where television satellites are, or to go where the international space station is?

Project #3: One Jansky is the flux density you receive if you hold a 60W light bulb at what distance?

Project #4: Take a look at Topic 5 on the Suggested Reading List

Project #5: February 27, 2012: There are 4 planets visible in the night sky - Jupiter, Mercury, Venus and Mars. Try to spot them. Mercury and Venus will be visible around sunset - Why? Jupiter and Mars will be visible through most of the evening. Use the
relative motion of the planets (i.e. the angular separation between the planets) to infer how far they are from us.

Project #6: The sun is red in the morning, whitish/yellow in the middle of the day and red again in the evening. Since color is related to temperature, does that mean the Sun is changing in temperature? No. Difference in color is due to light of a particular frequency being scattered away by the dust/molecules in the atmosphere. A dust grain most efficiently scatters wavelengths of its own size. There are more small grains than large grains, so shorter wavelengths (blue) get scattered more than larger wavelengths (red).

Project #7: If a star had a 40AU dust shell around it and was at a distance of 10pc what would the size of the dust shell be? Would it be extended as seen by WISE? No. It would be 4 arcsec while WISE has a spatial resolution of 12 arcsec at wavelengths where it can see dust emission.
If a galaxy of radius 10 kpc was at a distance of 10 Mpc, would it be extended as seen by WISE? Yes. It would be 412 arcseconds in diameter.

Wasnt that solar eclipse on May 20th cool?

Proposal Structure:
1. Title - Classification of Compact Submillimeter Sources in the Planck Archive

2. Goal: What are you going to do (Chelen)

3. Motivation: Why are you going to do it (Chris)

4. Methodology: How you are going to do it (Kat)

5. Timescale: What is the plan and what are the milestones (Denise)

6. Questions and concepts you expect to understand and share with the students. ("Involving students involved in the data analysis" is not a good answer - details please). Some ideas: what is a black body, using the peak wavelength as a measure of temperature, working with data in excel, how astronomers draw conclusions from data, how one can differentiate between galactic and extragalactic sources, why cant this be done with SOFIA, why do we need to launch Planck to L2?

7. What new teaching skills do you plan to develop based on this research program

8. We'll put in an abstract in the end which summarizes all this.

Figures for the proposal: all sky image and why we are looking outside the Galactic plane; cutouts of Planck, IRAS and WISE images of the same field with Planck beam overlaid; also, histogram of Planck/W1 flux density, and Planck/W2 and Planck/W3 and Planck/W4 flux density.

Coldspotz June Visit to Pasadena

2012-06-18T18:00:02Z

Chary:

'''Plan for the Visit:''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

[[File:6.jpg|600px|Gang@JPL courtesy of Chelen]]

File:6.jpg

2012-06-18T17:59:24Z

Chary:

Coldspotz June Visit to Pasadena

2012-06-17T23:29:10Z

Chary:

Coldspotz June Visit to Pasadena

2012-06-17T23:28:18Z

Chary:

'''Plan for the Visit''' [[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

Coldspotz June Visit to Pasadena

2012-06-17T23:28:09Z

Chary:

'''Plan for the Visit'''[[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

Coldspotz June Visit to Pasadena

2012-06-17T23:26:05Z

Chary:

[[Media:schedule.pdf]]

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

File:Schedule.pdf

2012-06-17T23:25:27Z

Chary:

Coldspotz June Visit to Pasadena

2012-06-17T23:17:18Z

Chary:

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px|Chris, da' funny maan]]

[[File:5.jpg|600px|That iphone looks so delicious, I could eat it]]

Coldspotz June Visit to Pasadena

2012-06-17T23:15:19Z

Chary:

[[File:1.jpg|600px|SSC/Caltech Rooftop]]

[[File:2.jpg|600px|On the JPL Tour]]

[[File:3.jpg|600px|Chillin' after a hard weeks' work]]

[[File:4.jpg|400px]]

[[File:5.jpg|600px]]

Coldspotz June Visit to Pasadena

2012-06-17T23:14:32Z

Chary:

Coldspotz June Visit to Pasadena

2012-06-17T23:14:01Z

Chary:

Coldspotz June Visit to Pasadena

2012-06-17T23:12:22Z

Chary:

File:5.jpg

2012-06-17T23:12:16Z

Chary:

File:4.jpg

2012-06-17T23:11:39Z

Chary:

File:3.jpg

2012-06-17T23:10:39Z

Chary:

File:2.jpg

2012-06-17T23:09:23Z

Chary: JPL Tour

JPL Tour

Coldspotz June Visit to Pasadena

2012-06-17T23:08:38Z

Chary:

[[File:1.jpg|600px]]

Coldspotz June Visit to Pasadena

2012-06-17T23:06:53Z

Chary: Created page with "File:1.jpg"

[[File:1.jpg]]

File:1.jpg

2012-06-17T23:06:15Z

Chary: SSC/Caltech Rooftop

SSC/Caltech Rooftop

Cold Spotz Current Research Activities

2012-06-17T23:04:53Z

Chary:

[[File:ColdSpotz.jpg]]

=[[Cold Spotz Suggested Reading List]]=

Click on the link above!

=[[Cold Spotz Proposal]]=

This page will be used to assemble the pieces for the proposal we are writing. See [[2012 proposal instructions]] for, well, instructions!

=[[Cold Spotz Spring work]]=
This page will be used to collect information during our work in Spring.

=[[Coldspotz June Visit to Pasadena]]=

=...Plenty of space for anything you want=

[[File:PlanckModel04.jpg]] [[File:IMG_7380.jpg]]

Project #1: Build your Planck model:
The paper parts for a Planck model can be found at [http://planck.cf.ac.uk/education/model]. Kat's model (the one furthest to the right above) actually has the reflection of the focal plane in the mirror the correct way up.

Project #2: Launch costs:
What is the relationship between launch cost and satellite size is. Does it cost more to go where Planck is, or to go where television satellites are, or to go where the international space station is?

Project #3: One Jansky is the flux density you receive if you hold a 60W light bulb at what distance?

Project #4: Take a look at Topic 5 on the Suggested Reading List

Project #5: February 27, 2012: There are 4 planets visible in the night sky - Jupiter, Mercury, Venus and Mars. Try to spot them. Mercury and Venus will be visible around sunset - Why? Jupiter and Mars will be visible through most of the evening. Use the
relative motion of the planets (i.e. the angular separation between the planets) to infer how far they are from us.

Project #6: The sun is red in the morning, whitish/yellow in the middle of the day and red again in the evening. Since color is related to temperature, does that mean the Sun is changing in temperature? No. Difference in color is due to light of a particular frequency being scattered away by the dust/molecules in the atmosphere. A dust grain most efficiently scatters wavelengths of its own size. There are more small grains than large grains, so shorter wavelengths (blue) get scattered more than larger wavelengths (red).

Project #7: If a star had a 40AU dust shell around it and was at a distance of 10pc what would the size of the dust shell be? Would it be extended as seen by WISE? No. It would be 4 arcsec while WISE has a spatial resolution of 12 arcsec at wavelengths where it can see dust emission.
If a galaxy of radius 10 kpc was at a distance of 10 Mpc, would it be extended as seen by WISE? Yes. It would be 412 arcseconds in diameter.

Wasnt that solar eclipse on May 20th cool?

Proposal Structure:
1. Title - Classification of Compact Submillimeter Sources in the Planck Archive

2. Goal: What are you going to do (Chelen)

3. Motivation: Why are you going to do it (Chris)

4. Methodology: How you are going to do it (Kat)

5. Timescale: What is the plan and what are the milestones (Denise)

6. Questions and concepts you expect to understand and share with the students. ("Involving students involved in the data analysis" is not a good answer - details please). Some ideas: what is a black body, using the peak wavelength as a measure of temperature, working with data in excel, how astronomers draw conclusions from data, how one can differentiate between galactic and extragalactic sources, why cant this be done with SOFIA, why do we need to launch Planck to L2?

7. What new teaching skills do you plan to develop based on this research program

8. We'll put in an abstract in the end which summarizes all this.

Figures for the proposal: all sky image and why we are looking outside the Galactic plane; cutouts of Planck, IRAS and WISE images of the same field with Planck beam overlaid; also, histogram of Planck/W1 flux density, and Planck/W2 and Planck/W3 and Planck/W4 flux density.

Cold Spotz Suggested Reading List

2012-06-08T21:57:38Z

Chary:

'''1''' [http://www.bbc.co.uk/news/science-environment-12065464]Planck starts warming up Jan 14, 2012. This means we have observed the entire sky almost 5 times since launch in May 2009.

'''2''' [http://arxiv.org/abs/1101.2041]Example of what a research paper looks like. This has a lot of the information on the data you will be working with but is likely to be incomprehensible due to the jargon used. Do not be alarmed!

'''3''' [http://www.bbc.co.uk/news/education-16612100] I am appalled that parents cant answer these questions. Teachers, please teach your students these. Answers to the questions:
1. Moon reflects sunlight that is why it is bright. It rises and sets every day/night because of the Earth's rotation. At the same time, the Moon orbits around the Earth with a 28 day period. So the time it rises and sets changes depending on its position in its orbit.
2. The day sky is blue because the dust in the Earth's atmosphere scatters blue light more effectively (particles best scatter wavelengths of light of their size or smaller). It is the same reason why the sky is red at sunset.
3. We dont know. The Universe is very big and distances are large. There are most likely aliens out there but because of the large distances involved we may never discover them.
4. 6E24 Kg.
5. The air blowing over a planes wings has a different velocity above and below the wing. This difference in pressure results in a lift. This is why planes cannot fly in space - there is no air.

'''4''' [http://wise2.ipac.caltech.edu/docs/release/prelim/expsup/figures/sec4_3gt4.gif] WISE Zero Points to get flux densities from magnitudes.

'''5''' In the image below, each type of bulb emits the spectrum of light below it. Can you infer from this which light corresponds to the hottest temperature and which corresponds to the coldest?

[[File:Blackbody.jpg]]

'''6''' [http://www.mauinews.com/page/content.detail/id/557678.html] Chris and Kat in the local newspaper.

'''7''' [http://sci-ed.net/] Meet other passionate science teachers

'''8''' There are several interesting conferences happening next week (2/13/2012-2/17/2012). One is the Planck Intermediate Papers Conference in Bologna [http://www.iasfbo.inaf.it/events/planck-2012/index.php], a second is the WFIRST Conference in Pasadena [http://www.ipac.caltech.edu/wfir2012/index.shtml] and a third is a conference on the first galaxies in Santa Barbara [http://www.kitp.ucsb.edu/activities/dbdetails?acro=dwarfgal-c12]

'''9''' How one starts building a telescope on earth [http://www.space.com/15021-giant-magellan-telescope-construction-blast.html]. The Giant Magellan Telescope has competitors which are in the works as well - TMT and the European ELT.

'''10''' [http://www.latimes.com/news/opinion/commentary/la-oe-krauss-cosmology-design-universe-20120401,0,4136597.story] A well written article which touches on the cutting edge of astronomy

'''11''' [http://wiki.nasa.gov/cm/blog/NES_Teachers_Corner/posts/post_1334344076343.html] Get your students involved in high altitude ballooning for science!

'''12''' [http://www.nasa.gov/topics/universe/index.html] Get the news of the Universe from NASA.

'''13''' [http://www.nasa.gov/externalflash/goddardVT/] The life cycle of any space mission. Have a good idea? Get started now 'cause the entire life cycle can take 10 years or more.

'''14''' [http://profmattstrassler.com/articles-and-posts/particle-physics-basics/neutrinos/neutrinos-faster-than-light/opera-what-went-wrong/] This is a great article on how the process of science works (mistakes/corrections/human tendencies...). The take away message is check, check and check again and if all those cross-checks agree, make someone else repeat the experiment and reproduce your results.

Cold Spotz Suggested Reading List

2012-06-08T21:55:53Z

Chary:

Cold Spotz Current Research Activities

2012-05-21T19:12:29Z

Chary: /* ...Plenty of space for anything you want */

[[File:ColdSpotz.jpg]]

=[[Cold Spotz Suggested Reading List]]=

Click on the link above!

=[[Cold Spotz Proposal]]=

This page will be used to assemble the pieces for the proposal we are writing. See [[2012 proposal instructions]] for, well, instructions!

=[[Cold Spotz Spring work]]=
This page will be used to collect information during our work in Spring.

=...Plenty of space for anything you want=

[[File:PlanckModel04.jpg]] [[File:IMG_7380.jpg]]

Project #1: Build your Planck model:
The paper parts for a Planck model can be found at [http://planck.cf.ac.uk/education/model]. Kat's model (the one furthest to the right above) actually has the reflection of the focal plane in the mirror the correct way up.

Project #2: Launch costs:
What is the relationship between launch cost and satellite size is. Does it cost more to go where Planck is, or to go where television satellites are, or to go where the international space station is?

Project #3: One Jansky is the flux density you receive if you hold a 60W light bulb at what distance?

Project #4: Take a look at Topic 5 on the Suggested Reading List

Project #5: February 27, 2012: There are 4 planets visible in the night sky - Jupiter, Mercury, Venus and Mars. Try to spot them. Mercury and Venus will be visible around sunset - Why? Jupiter and Mars will be visible through most of the evening. Use the
relative motion of the planets (i.e. the angular separation between the planets) to infer how far they are from us.

Project #6: The sun is red in the morning, whitish/yellow in the middle of the day and red again in the evening. Since color is related to temperature, does that mean the Sun is changing in temperature? No. Difference in color is due to light of a particular frequency being scattered away by the dust/molecules in the atmosphere. A dust grain most efficiently scatters wavelengths of its own size. There are more small grains than large grains, so shorter wavelengths (blue) get scattered more than larger wavelengths (red).

Project #7: If a star had a 40AU dust shell around it and was at a distance of 10pc what would the size of the dust shell be? Would it be extended as seen by WISE? No. It would be 4 arcsec while WISE has a spatial resolution of 12 arcsec at wavelengths where it can see dust emission.
If a galaxy of radius 10 kpc was at a distance of 10 Mpc, would it be extended as seen by WISE? Yes. It would be 412 arcseconds in diameter.

Wasnt that solar eclipse on May 20th cool?

Proposal Structure:
1. Title - Classification of Compact Submillimeter Sources in the Planck Archive

2. Goal: What are you going to do (Chelen)

3. Motivation: Why are you going to do it (Chris)

4. Methodology: How you are going to do it (Kat)

5. Timescale: What is the plan and what are the milestones (Denise)

6. Questions and concepts you expect to understand and share with the students. ("Involving students involved in the data analysis" is not a good answer - details please). Some ideas: what is a black body, using the peak wavelength as a measure of temperature, working with data in excel, how astronomers draw conclusions from data, how one can differentiate between galactic and extragalactic sources, why cant this be done with SOFIA, why do we need to launch Planck to L2?

7. What new teaching skills do you plan to develop based on this research program

8. We'll put in an abstract in the end which summarizes all this.

Figures for the proposal: all sky image and why we are looking outside the Galactic plane; cutouts of Planck, IRAS and WISE images of the same field with Planck beam overlaid; also, histogram of Planck/W1 flux density, and Planck/W2 and Planck/W3 and Planck/W4 flux density.

Cold Spotz Spring work

2012-04-24T04:14:06Z

Chary:

'''''Our initial foray into the Planck archives:'''''
Here's the spreadsheet with our group data ... [[File:FirstData.xlsx]] --[[User:CJohnson|CJohnson]] 18:40, 13 February 2012 (PST)

Here's the spreadsheet with my data included. [[File:SecondData.xlsx]]
--[[User:CJohnson|CJohnson]] 18:23, 31 March 2012 (PDT)

Okay, here's a third version of our flux spreadsheet. Differences from previous versions ... inclusion of RA and Dec (to help when using SDSS to categorize our sources), Planck fluxes in Jy, slight corrections in WISE fluxes. [[File:FluxData_03April.xlsx]]
--[[User:CJohnson|CJohnson]] 08:47, 5 April 2012 (PDT)

[[File:FluxData_17April.xlsx]] Here is the file with my values for W4 and temperature. Please check to see why there are disagreements between my values and yours. RRC; 17 April 2012. Updated 23 April 2012 with values for Denise' sources.

----
Resource list from the proposal ...

'''''Articles specific to the Planck mission:'''''

'''Refereed journals'''

• Planck Early Results. I. The Planck mission. A&A 536: A7 (2011). http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201116464&Itemid=129

• Planck Early Results. VII. The Early Release Compact Source Catalog. A&A 536, A7 (2011). http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201116474&Itemid=129

'''Scientific American magazine'''

• Planck Telescope sees Universe’s cool stuff. http://www.scientificamerican.com/article.cfm?id=planck-telescope-sees-universe

• Planck’s new view of the cosmic theater http://www.scientificamerican.com/article.cfm?id=plancks-new-view-of-the-cosmic-thea

'''Sky and Telescope magazine'''

• Planck’s view of the Universe http://www.skyandtelescope.com/community/skyblog/newsblog/97960234.html

• Planck sees first light http://www.skyandtelescope.com/community/skyblog/newsblog/60242112.html

'''Astronomy magazine'''

• Planck steps closer to the cosmic blueprint http://www.astronomy.com/News-Observing/News/2012/02/Planck%20steps%20closer%20to%20the%20cosmic%20blueprint.aspx
Astronomical Society of the Pacific – Astronomy Beats!

• Issue #24. Planck Flies! 01 June 2009. [[File:AstroBeat2009-24.pdf]]

'''''Articles tailored to astronomy concepts:'''''

• '''Submillimeter astronomy:''' http://www.astronomycast.com/2009/04/episode-131-submillimeter-astronomy/

• '''Flux density:''' http://web.njit.edu/~gary/728/Lecture1.html

• '''LaGrangian points:''' http://www-spof.gsfc.nasa.gov/Education/wlagran.html

• '''Blackbody radiation:''' http://www.egglescliffe.org.uk/physics/astronomy/blackbody/bbody.html

• '''Distant, Dusty Galaxies:''' http://www.scientificamerican.com/article.cfm?id=distant-dusty-galaxies and http://www.universetoday.com/10312/spitzer-finds-hidden-galaxies/#.T0LgpC-Alao.mailto

• '''Star formation:''' http://www.sciencedaily.com/releases/2009/04/090422085832.htm#.T0LdoixLPbs.email

--[[User:CJohnson|CJohnson]] 15:25, 22 March 2012 (PDT)

File:FluxData 17April.xlsx

2012-04-24T04:10:12Z

Chary: uploaded a new version of "File:FluxData 17April.xlsx"

Cold Spotz Spring work

2012-04-17T18:46:28Z

Chary:

'''''Our initial foray into the Planck archives:'''''
Here's the spreadsheet with our group data ... [[File:FirstData.xlsx]] --[[User:CJohnson|CJohnson]] 18:40, 13 February 2012 (PST)

Here's the spreadsheet with my data included. [[File:SecondData.xlsx]]
--[[User:CJohnson|CJohnson]] 18:23, 31 March 2012 (PDT)

Okay, here's a third version of our flux spreadsheet. Differences from previous versions ... inclusion of RA and Dec (to help when using SDSS to categorize our sources), Planck fluxes in Jy, slight corrections in WISE fluxes. [[File:FluxData_03April.xlsx]]
--[[User:CJohnson|CJohnson]] 08:47, 5 April 2012 (PDT)

[[File:FluxData_17April.xlsx]] Here is the file with my values for W4 and temperature. Please check to see why there are disagreements between my values and yours. RRC; 17 April 2012

----
Resource list from the proposal ...

'''''Articles specific to the Planck mission:'''''

'''Refereed journals'''

• Planck Early Results. I. The Planck mission. A&A 536: A7 (2011). http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201116464&Itemid=129

• Planck Early Results. VII. The Early Release Compact Source Catalog. A&A 536, A7 (2011). http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201116474&Itemid=129

'''Scientific American magazine'''

• Planck Telescope sees Universe’s cool stuff. http://www.scientificamerican.com/article.cfm?id=planck-telescope-sees-universe

• Planck’s new view of the cosmic theater http://www.scientificamerican.com/article.cfm?id=plancks-new-view-of-the-cosmic-thea

'''Sky and Telescope magazine'''

• Planck’s view of the Universe http://www.skyandtelescope.com/community/skyblog/newsblog/97960234.html

• Planck sees first light http://www.skyandtelescope.com/community/skyblog/newsblog/60242112.html

'''Astronomy magazine'''

• Planck steps closer to the cosmic blueprint http://www.astronomy.com/News-Observing/News/2012/02/Planck%20steps%20closer%20to%20the%20cosmic%20blueprint.aspx
Astronomical Society of the Pacific – Astronomy Beats!

• Issue #24. Planck Flies! 01 June 2009. [[File:AstroBeat2009-24.pdf]]

'''''Articles tailored to astronomy concepts:'''''

• '''Submillimeter astronomy:''' http://www.astronomycast.com/2009/04/episode-131-submillimeter-astronomy/

• '''Flux density:''' http://web.njit.edu/~gary/728/Lecture1.html

• '''LaGrangian points:''' http://www-spof.gsfc.nasa.gov/Education/wlagran.html

• '''Blackbody radiation:''' http://www.egglescliffe.org.uk/physics/astronomy/blackbody/bbody.html

• '''Distant, Dusty Galaxies:''' http://www.scientificamerican.com/article.cfm?id=distant-dusty-galaxies and http://www.universetoday.com/10312/spitzer-finds-hidden-galaxies/#.T0LgpC-Alao.mailto

• '''Star formation:''' http://www.sciencedaily.com/releases/2009/04/090422085832.htm#.T0LdoixLPbs.email

--[[User:CJohnson|CJohnson]] 15:25, 22 March 2012 (PDT)