Exoplanet Working Group Telecon Meeting Minutes - October 12, 2017


Subject:Exoplanet Working Group Telecon Date:10/12/2017
Purpose:To discuss science activities for exoplanet working group.Facilitator:Kevin Stevenson
Location/Time:

Telecon/Web-Ex Online: 

https://stsci.webex.com/stsci/j.php?MTID=m8758cbeba1b8f7c6a7633a990872001d

Meeting Number: 

1-855-244-8681 (toll free)

1-650-479-3207 Call-in number


Access code: 646 769 704 

Note Taker:Sydney Jones

Discussion Items 

  • Questions from Face-to-Face (F2F)
    • Concept 2 targets for 3.5 meter telescope
    • Looking for volunteer to give bio-signatures presentation at AAS, 15 minutes, working group can help to generate content and figures, including from white paper
      • Commitment includes giving presentations maybe once or twice
      • ACTION: Notify Kevin Stevenson if interested. 
      • ACTION: Kevin Stevenson to send Sydney Jones or entire exoplanet working group information or email info exoplanet working group members.
    • Is ~25 thousand (K) sufficient for high res transmission spectroscopy for MIRI? 
      • Concern is how many photons is needed at this mode.
      • Resolution at 100 get photon limited noise. Need to see science limitations at this mode.
      • Stick to 25K and do rough calculation of noise. 
      • Killer science case is habitable planets, exciting science is spectroscopy science case, should consider this in a broader context of non-habitable planets. 
      • May not be able to do high-res with habitable planets. 
      • Reach out to POC at University of Colorado who is working with Alexa. 
      • High resolution spectroscopy should consider stacking of lines. 
      • Not going to be bigger than anything on the ground, water or methane may shift to get out of windows. need good understanding of science capability for this. 
      • 2.3 microns has been done on the ground 
      • Can examine shape of disks through spectral resolution, are these science cases out of date?
        • Proto-planetary disks has a science case similar to this
        • Requirement is set at 25K
        • Cases aim at longer wavelengths sometimes for higher spectra resolution
        • Wavelength coverage should be determined to detect modules. Need provide preference of wavelength coverage.
      • Aliza Kemptons Response 
        • High res spectroscopy has been targeted at higher spectral resolution to detect wind and atmospheric dynamics. 25K would not be sufficient for kilometer scale. 
        • Need to get close to R ten to the 5 for dopler precision of kilometer per second. 
        • Key planetary targets are cooler. 
        • Are photon stars only received from the ground? This is true from the ground, using cross correlation model. Get signal in cross correlation but you don't get to see lines per say. 
        • For OST, how far can sigma noise be reduced to get something out of it? Eliza does not, but observers presumably do. 
          • ACTION: @Aliza Kempton to get answer for this. 
  • Reviewed Figures of Transmission and Emission 
    • MIRI Noise Floor
      • Concerns is that the MIRI LRS spectra do not have noise floor, which is why two data sets are comparable. 
      • Need to determine reasonable PPM and decide on this and introduce into the figures (deadline is in two weeks).
      • Zodi is 200 electrons per pixel, which is why things fall apart at longer wavelengths. Has background and detector noise. 
      • Roellig added that symbol sizes in plots are too close. Need different color scheme to differentiate between the two.
      • Pablo asked about the noise from spectrum. Can noise be included in the spectrum or just in the era bars? Transit number (plotting era bars with 100)?
        • Green added that he does not know the number for this. Some of the best noise performance with cold Spitzer were Heather's parcel phase curve of 189, getting 50 or 60 PPM noise total substantial amount of this is the noise floor. 50 PPM may be okay, it is pretty uncertain at the moment.
        • Total noise could be 60 PPM?
          • This was possible with cold Spitzer. May be able to do this with James Webb Space Telescope, which would then be possible with Spitzer and subsequently possible for OST. 
          • JWST may not do this object very well, but OST has a goal that we can work with. 
          • LRS for MIRI could be 30 PPM noise floor, that is achievable for MIRI. Could put in no noise for OST to show what the potential is? 
          • 30 PPM could be possible for MIRI detectors. 
          • 50 PPM is assuming we get SPITZER like performance. Reference the paper and say this is what Spitzer can do. Regardless of 50-30 PPM we cant do science that OST wants to do. 
          • 30 PPM for JWST and 0 for OST (technology development is needed and should be implied for OST)
          • OST will get longer wavelength coverage at PPM
          • ACTION: @Tom Greene do trapis at k = 8 
      • ACTION: Explore parameter space, planet size, stellar type and get reasonable assessment of parameter space. This will be good to help demonstrate that OST has done work to identify relative parameters of bio-signatures to difference planets that have an atmosphere and those that don't. Think about how to put together models and programs. Kevin Stevenson will revisit this at the next exoplanet working group meeting.
  • Discuss initial report due on 10/27/2017 
    • Good progress on figures
    • Text is progress will get copy in the next few days
  • White Paper - Lisa Kaltenegger
    • ACTION: People to review and provide comments at next exoplanet working group. 
    • Which emission model is best to use? 
      • Generate uncertainties for Pablo to create instance of simulated data. 
    • Benting for figures? R of 30 is possible.
    • ACTION: Kevin Stevenson will sent out hyperwall dates and times and write up documents/guidelines for AAS meeting. 

                                                                 Action Items 

No.Action Item(s)Owner Target Due date Status (In progress/Completed)

1.

Explore parameter space, planet size, stellar type and get reasonable assessment of parameter space. This will be good to help demonstrate that OST has done work to identify relative parameters of bio-signatures to difference planets that have an atmosphere and those that don't. 
Think about how to put together models and programs. Kevin Stevenson will revisit this at the next exoplanet working group meeting.
All Members of Exoplanet Working Group10/26/2017
2.

Get answer for OST how far can sigma noise be reduced to get something out of it? Eliza does not, but observers presumably do

@Aliza Kempton 10/26/2017
3.Figures of Transmission and Emission for MIRI do traps at K = 810/26/2017
4. Send email to Sydney Jones and all exoplanet meeting members regarding bio-signatures info for hyperwall dates and times and write up documents/guidelines for AAS meeting. 10/26/2017
5.Notify Kevin Stevensonif interested in presenting bio-sigantures hyperwall talk at AAS meeting. All Members of Exoplanet Working GroupBefore 10/26/2017
6.Review white paper from (Lisa Kaltenegger) and provide comments at the next exoplanet working group meeting. All Members of Exoplanet Working Group10/26/2017