We should start up the task force to look at the observing strategy (cadence) simulations. This is urgent because many simulations already exist and reports may start as soon as January 2020. I understand that decisions about how often etc. to observe both high latitude and low latitude fields will be based on the suite of simulations.
The current status of the runs is available here:
I think what we really need are:
People to look at the output of the current simulations, there is a lot of info out there now that we can use.
People to write new metrics (MAF) IF ANY ARE NEEDED.
A discussion of what we think about the different proposals in terms of our science. That could lead to new “Figures of Merit” to express this conclusion.
I think it would be good to have this happen here on community rather than email for a variety of reasons.
Gasp. What a large inventory of cadences. Are there clues for the clueless as to which to look at first?
In the Bad Old Days, cadence output appeared in MySQL format. The current ones appear as .db files. Is there a pointer to documents on what platform is needed and how to proceed. Is this a Jupyter thing? Sorry that I don’t work LSST every day and the learning curve is steep.
Hi @dgmonet - the cadence outputs are now plain sqlite database files, not a full mysql database, hopefully this is even easier to access as you don’t have to set up a mysql database for yourself (see ‘sqlite’ at the command line or ‘import sqlite3’ in python).
But yes, I would definitely encourage you to use MAF (there are a lot of tutorials and links to more resources at https://github.com/LSST-nonproject/sims_maf_contrib/tree/master/tutorials) – especially if you want us to be able to recreate your analysis on any new runs in the future (there will be at least another one or two big sets of runs like this). It helps us a lot.
Hi @ljones cc @yoachim- I am attempting to use sims with Docker to try to short-cut the various dependency installations (machine is old). Is Owen Boberg’s Docker page still the place to look for instructions running sims within Docker, and does the sims version therein understand the latest round of OpSim outputs? https://hub.docker.com/r/oboberg/maf/
Hi @jgizis@pmmcgehee - I agree with John’s 3-point list in the message at the top of this thread about what is needed.
Perhaps a good way to jumpstart this process would be for the CF task force leads to contact the lead authors of the latest round of cadence whitepapers (cWPs) to check in about whether the existing MAFs are sufficient to assess observing strategies - and, if not, what precisely is needed to make the assessment on a timescale of a couple of months.
Some cWP groups already have run their MAFs on older sims (so in theory could be re-run on the latest round of OpSims), some still need the MAFs to be coded from specs in their whitepapers (and/or the target MAFs may have evolved or simplified since the cWPs were written). Given the time-frame, I think it’s likely that the latest round of MAFs will be produced by dissection of the nice set of tutorial notebooks @yoachim and @ljones have produced in maf_contrib on github (unless someone has had a PhD student working on metrics that we don’t know about).
I think the same goes for the SMWLV metrics in the COSEP - it should be determined which of those MAFs really are the critical ones for a Jan-2020 (!!) time-frame. The emphasis should be on simple metrics.
@jgizis , do you have a record of who volunteered to lead the task forces at the PCW in August?
"Here are some important updates from the LSST Project and Community Workshop held earlier this month in Tucson:
Crowded Field Photometry: The project is making a plan to process crowded stellar fields with a special deblender, i.e., a DAOPhot-like system integrated into the LSST DM pipeline, and not the same deblender being developed to deal with galaxies at high galactic latitude. They believe an in-house DM solution has significant advantages over using existing external codes. A document (plan) explaining their approach is expected around September 1. We will have two months to provide feedback. [See Task Forces below]
New “Task Forces” for 2019-2020: We had a meeting of SMWLV members. We decided to form a number of task forces which have a defined mission and finite lifetime. A number of volunteers, but we badly need more. Please sign up here:
The proposed task forces are:
CADENCE SIMULATIONS: Tasks: Review existing cadence metrics and identify new metrics. Work with “LSST MAF” group to implement metrics. Complete this within 4 months. After feedback from our collaboration, analyze results of simulations. Volunteers: Olsen, Clarkson, Leo, Marcio,
CROWDED FIELD: Read and comment on DM crowded field photometry plan by November. Volunteers: Clarkson, Nidever,Adriano Pieres
COMMISSIONING: Review LSST official document on commissioning tests. Lead discussion of tests that we feel are missing. Identify participants to directly participate in commissioning, early access sprints, data preview sprints. Many timescales, but reading and planning can occur in next six months. We anticipate most work is in 2020-2021. Volunteers: Olsen.
ASTROMETRY: Investigate Differential Color Refraction (DCR). Identify data and develop proposal if necessary. Volunteers: D. Monet, Jullio Camargo
CALIBRATION: Investigate water bands and calibration (y) filter. New calibration data expected in spring 2020, so start then. (Should also reach out to supernovae people). Volunteer: Pat Boeshaar.
DATA CHALLENGE: Plan sprint or data challenges of our own to do science. Volunteer: Clarkson.
Other task forces are welcome. The first three were considered the most urgent and important. Please volunteer!"
The Project intends to ask Science Collaborations to evaluate in-kind contributions from international contributors. What this means is yet to be worked out.
@pmmcgehee cc @jgizis aha, thanks! So in this present thread I think we’re talking about the “Cadence Simulations” task force, on which it looks like myself, @knutago , Leo and Marcio volunteered to work.
Oof, we haven’t kept up with generating docker images of sims … that said, I think this would still work (especially if you did a git pull of the MAF repo - the ‘pull_repos’ command mentioned on Owen’s page).
I’ll see if we can spend a bit of time generating a new docker image. It’ll have to move locations because Owen is no longer with LSST (he moved on to a great data scientist job in Indiana).
Hi all, just to clarify my place in this matter: I hope to look at the metrics for “non-variable stellar science”, more specifically at the expected distribution of limiting magnitudes, star counts, maximum reached distances, etc, for the different cases and filters, for single visits + stacks. My time is limited and work will not start before 2 weeks. And everything will depend very much on me being able to run MAF remotely (thanks Will for the instructions, which I still did not try).
One set of metrics/figure-of-merits I would like to explore would be based around the actual positions of star-forming-regions or open clusters or the bulge or known satellite galaxies or whatever [including both Northern and Southern Hemisphere. (It would also need depth, astrometry, or time coverage metrics for the various science case).
I think this would be valuable because it could be helpful in looking at the Big Sky Cadence, WFD, Galactic Plane both inner and anti-center, South Celestial Cap, etc. in a fair way.
do you have any news about simulations of the metrics/figure-of-merits described in our White paper ( “Investigating the population of Galactic star formation regions and star clusters within a Wide-Fast-Deep Coverage of the Galactic Plane”)?
We have several new simulations that would be relevant for the galactic plane survey strategy questions. However, I looked at the metrics in your white paper and have questions:
We can certainly just look at the limiting depth in each part of the sky, but this doesn’t seem to really be the thing that we should be measuring - because dust extinction is not included in that simple limiting magnitude. Your figures of merit included some additional conversion between simply the coadded depth and the final figures of merit, which included something I can’t quite decipher about the distribution of the stellar population and the distribution of dust. Can you help us make better metrics that will include both of these?