The purpose of this page is to collect questions (and answers!) from the community regarding the Galactic Plane Survey.
The SOC will reach out to the relevant people to answer these questions, and once responses are available they will be posted here.
I am very curious about the feasibility of using the HK filter for measuring Paschen alpha. And similarly Paschen beta in J, Paschen gamma in K?
It was mentioned that Roman would be able to observe M dwarf stars out to the distance of the Galactic Center. Is that taking into account limitations from extinction toward the Central Molecular Zone and crowding from the high density of stars?
What are the chances of extending the allocated 700 hours?
Could Roman astrometry be used together with Gaia (where this is possible, in the less crowded Galactic plane regions) to get proper motions?
Where to obtain isochrones and modeling. I presume RGB tip saturated so only photometry a red clump, main sequence turnoff.
How are synergies with the GBTDS being considered? Are synergies with filters and such being considered?
For the simulation of different realizations of the GPS, how is noise being simulated? Is confusion being taken into account?
What is the planned cadence of the high cadence fields?
What would be the necessary exposure times to reach apparent magnitudes F129=23.5 and F213=19.7 with SNR=20 (these are the estimated oMSTO mags of the bulge, adopting E(J-K)=3). I estimated that 980s and 85s are the necessary exposure times. Could someone verify this? It is a very crowded region, so I guess a small aperture will be necessary and the background may be relatively bright.
I am wondering if in the Off-plane option we could test the grism capabilities
I would like to know the delta-time between filters of a given footprint -- what is the absolute minimum, and what is the likely minimum given wide-field survey science goals?
Is there any detailed plan on combining Galactic bulge time domain survey data with Plan survey data during the data redunction? In this case some bulge region could have improved astrometry.
I would like to learn more about how new person can join in, and learn more detail about the survey area and proper motion projects. Information about Galactic Plane Survey is not easily available.
There is available data simulated?
Will the exposure time (Texp) be fixed or we can propose Texp in function of our science? It would be interesting for us to know about the surface brightness (for large structures) that can be reached in a certain Texp for each filter, so we can assess the feasibility of our prospective project: Is there an ETC we could use (or do you already have this information) ?
- What data pipeline will be used to process the data from the Galactic Plane survey? Where will the data product be made available? What format will those data products be in, and will there be any simulated data available to the community for testing software?
