High resolution is 10 to the 4th (resolving individual lines).
Is the question "how do galaxies form stars, grow their central supermassive black holes, and make heavy elements over Cosmic time" agnostic? Yes.
This question, drives one to assess how OST is different, given that SPICA may be doing this already. OSTs differenciation is that we will study the dawn of galaxies and elements. Most data will be cosmic.
Suggested taking another round of votes/feedback for alternatives to this question.
Fractional lumniosity is 3%
Kartik J. Sheth asked is there a reason for even split (given Hubble or Spitzers wedding cake structure)? The split is not optimized to a high level of fidelity, this can be optimized further.
FIP surveys in the study? No slides on FIP surveys were included.
Can get these with Alma at 600 microns.
May need C cat in the future.
How will sources be detected? Detction of lines with lower wavelengths.
Follow up several hundreds of these sources as well.
Look at long wavelength cut off and establish justification of
How are wavelengths synergistic with Alma? ALma coverage in higher frequencies is spotty (this is an argument for justification of the extended wavelength to 600 microns).
Need to have a certain number of galaxies as the driving requirement.
How did we get here? Ted/Gary/Klaus/Stefanie - See PowerPoint presentation below for additional notes on this agenda item.
Bulk of the program are disks.
HERO follow up obtains spectrally resolved observations.
Need to get to 25 microns to to get wings of 40 microns ice feature.
You dont need 35 micron spectral resolution. We would use OSS with coarser resolution to get the ice feature.
Klaus Pontoppidan note that we do need high resolutions at shorter wavelength of 175 microns.
The FTS will provide higher resolution at shorter wavelengths.
Higher spectral resolution will be better (Klaus Pontoppidan's memo justifies and explains this)
We may not need the etelon. With HERO band working at HD, do we need OSS etalon at the high resolution to do the disk work? Sensitivity will give us more targetrs. Minimum, we could go to 112.
Reasonable descope with the heterodyne.
Requirement for 0.2 kilometers (km)second.
High res follow up for disks, 0.3 km per/second
0.2 kn/second is needed to do the water trail correctly.
Should talk about spectral resolving power and sensitivity. HERO would be sufficient to do the starless course.
May not need the etalon, with the HERO at high sensitivities. For sensitvities, should prove the factors and improvement gotten over Herschel. Run calculations (for 200 hours) of how many disks are gotten with the eltalon vs. HERO?
If the etalon is dropped how much descoping occurs? A few tens of kilograms. Infrastructure of columnated beam is already there.
Did calculations using modest detectors Matt Bradford can send these out.
Just got an email indicating that she is still waiting on yeilds.
Eric Neilson indicated that he is trying to calculate what kind of planet masses that can be estimated (for 10 to the minus, 4, 5, 6, 7 for 4.5 microns)
10 to the minus for - JWST is bette r
Still need to get clarification for the inner working (2 lambda over D) angle and outter working angle?
How many planets can be detected in 2000 hours?
What will be the determining factor for deciding whether we will keep these? Will be able to get different wavelengths over MIRI.
WIll the corographic mask be on the same wavelength filter? The coronograph mask will be like near cam, where it inserts into the array. Still need to figure this out in the optical design. If this is a separate design this will add to the risk and cost. Trying to keep costs low.
Study Center update (Dave)
JWST chilled design status
Have not heard anything. They are still working on it currently.
Target Due Date
Status (In progress/Completed)
Recalculate MISC surveys and (MISC survey needs recalculation to figure out if it is realistic)