Rubin LSST SC’s feedback for draft Phase I report

SCOC Second Workshop, 2021 Nov 16-17

Session 2 (1045-1300 PST, Tues Nov 16)

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

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Who are we?

Rubin LSST Science Collaborations

• Rubin has no science-team

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• 8 self-managed self-governed science teams are preparing to do science with LSST data

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~2000 members,

physicists, astronomers,

data scientists, software engineers

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SC Coordinator: Federica Bianco fbianco@udel.edu

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

AGN Science Collaboration

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https://agn.science.lsst.org/

wnbrandt@gmail.com gtr@physics.drexel.edu

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Informatics and Statistics SC

loredo@astro.cornell.edu, cschafer@cmu.edu

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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AGN + ISSC Q/A

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Dark Energy Science Collaboration

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Quick intro

Science relies on various cosmology probes

• Static
• Primary: Weak Lensing, Large-Scale Structure, Clusters
• Transient
• Primary: Type Ia Supernovae, Strong Lensing
• Also: Kilonovae, Gravitational Wave sources
• Beyond just DESC, Astro2020 recommendations make Rubin transients a major focus!

Both WFD and DDFs are critical for both kinds of probes

Ongoing work in DESC Observing Strategy Working Group (see e.g., Lochner+2018, Scolnic+2018, Lochner+2021, DESC Cadence Note 2020) + collaborations/connections across SCs.

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Speaker: Humna Awan (DESC OSWG co-chair)

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lsst-desc-spokesperson@slac.stanford.edu

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Dark Energy Science Collaboration

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DESC is very happy about

• The decoupling of low-extinction WFD regions vs high-extinction

Why? Only the low-extinction regions of the sky are usable for DESC science since the science focus is extragalactic.

• Testing pushing the limits on declination bands

Why? DESC science would benefit greatly from overlap with DESI which is at higher declinations.

• Recognizing the critical role DDFs play in WFD science (aside from their role for transients)

Why? DESC science depends on photo-zs - calibration of these using the DDFs would be critical.

• Field revisit in different filters on the same night

Why? Always having a color measurement is significantly beneficial for supernova classification & distances.

• Revisiting dithering during commissioning

Why? Dithering (both translation and rotational) is critical but impacts of rotational dithers are difficult to quantify conclusively before commissioning.

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Speaker: Humna Awan (DESC OSWG co-chair)

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lsst-desc-spokesperson@slac.stanford.edu

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Dark Energy Science Collaboration

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Aspect of observing strategy that DESC is concerned about

• Rolling cadence

What? Rolling cadences have the potential to alleviate a lot of tensions when it comes to depth vs. area trade-off alongside improving cadence for transients. How rolling is implemented, however, will impact both static and transient science.

Would specifically like to quantify e.g. impacts of choosing buffers other than 1.5 years at the beginning and end of the survey since that impacts data releases; this aspect is currently missing in sims.

• Data releases

What? Rolling would impact the uniformity of the data releases => need to distinguish between comprehensive* vs. uniform releases. Will Data Management (DM) be able to produce both? If not, who will/can, and how?

• DDF optimization (* = i.e., with all data obtained so far)

What? DESC science suffers with DDF allocation < 5% (already assuming DESC-optimized cadence, filters, exposure times); would like more time. Cadence needs short-internight gaps; prefer only small dithers for DDFs.

Hear more (from DESC and other SCs) re their DDF needs at the community-led session tomorrow, 10.45a PT;

join #ddf on slack.

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Speaker: Humna Awan (DESC OSWG co-chair)

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lsst-desc-spokesperson@slac.stanford.edu

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

DESC Q/A

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Speaker: Humna Awan (DESC OSWG co-chair)

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lsst-desc-spokesperson@slac.stanford.edu

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Solar System Science Collaboration

Michael S. P. Kelley (University of Maryland)

for the SSSC

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Updated Footprint

The SSSC is happy with the updated footprint.

The North Ecliptic Spur (NES) is an SSSC priority, and happy to see that included in the 2.0 simulations. ��We still need to look at the wide variations on the number visits within the NES and their impact on our metrics and other science cases.

NES is crucial for Outer Solar System Science, Active Asteroid Population studies, Planet 9 Search.

Image Credit: SCOC report

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Solar System Science Collaboration

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Time recovered from potential efficiency gains?

Low Solar Elongation Twilight survey - enables niche science cases:

• Asteroids with orbits interior to the Earth.
• Sungrazing comets.
• NEO orbital phase space not covered in the Wide-Fast-Deep.

Any time that can be dedicated to observing low solar elongations at twilight will be useful.

"No compelling reasons why any of these proposals must be attempted during the first year of operations…"

• Achieving nominal WFD operations is a higher priority, but worth testing in commissioning.

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Solar System Science Collaboration

Longer u-band observations

Exposure times up to 1x50 s are advantageous for detection of CN gas around comets.

Filter allocations/pairs

SSOs are generally brightest in the redder filters: blue heavy distributions reduce SSO discovery rates.

Additional g-band observations can be beneficial to asteroidal and cometary science (e.g., gas emission), but we want to avoid impacts on Kuiper-belt object discovery and main-belt asteroid lightcurve inversion.

Image Credit: HSC Project NAOJ

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Solar System Science Collaboration

Nightly Pair Separation

The proposed 33-min separation (15 min during twilight) is expected to be the best balance for Solar System science, which relies on proper motion and source linking for object discovery.

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Solar System Science Collaboration

Long Gap Scenarios

We have concerns over potentially changing the separation between nightly pairs at the 5 year mark to accommodate the transient time gap.

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Not all Solar System objects are found in the first 2 years (i.e., main-belt statistics dominate numbers).

Nightly triplets did not strongly affect our metrics until the highest g-band limit in the previous set of simulations, so this may be the better way forward.

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Solar System Science Collaboration

SSSC Cadence Contacts:

Meg Schwamb (QUB; mschwamb.astro@gmail.com),

David Trilling (NAU; david.trilling@nau.edu)

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Rolling Cadence

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Need to do a full analysis on the rolling cadence variations.

We have concerns over more extreme rolling cadence scenarios, but the two-band N-S rolling cadence implemented, looks okay for Solar System Science.

Image Credit: Lynne Jones

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

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DESC + SSSC Q/A

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Strong Lensing Science Collaboration

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Chairs: Timo Anguita (Universidad Andres Bello), and �Graham Smith (University of Birmingham)

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Topics: “Static” lens finding (Timo)�Lensed NS-NS/KNe and deep Rubin ToOs (Graham)

Additional concerns

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gps@star.sr.bham.ac.uk/tanguita@gmail.com

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Strong Lensing Science Collaboration

Our “Static” SLSC Cadence Note

• Key Goals for finding lenses
1. Wide area with reasonable sensitivity in all bands
2. Good (sub-arcsecond) image quality in general, but particularly in the blue (g-band)
3. Blue sensitivity

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gps@star.sr.bham.ac.uk/tanguita@gmail.com

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Strong Lensing Science Collaboration

Cadence Note vs Recommendations

• Key Goals
• Wide area with reasonable sensitivity in all bands
• Good (sub-arcsecond) image quality in general, but particularly in the blue (g-band)
• Blue sensitivity

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• SCOC Draft Recommendations
• Optimize extinction area rather than just increase
• No image quality recommendations(?), but:
• Blue “skewed” (added depth) simulations available. (need to test)

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gps@star.sr.bham.ac.uk/tanguita@gmail.com

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Strong Lensing Science Collaboration

Lensed NS-NS/KNe and deep Rubin ToOs

• Deep Rubin ToOs will unlock gravitationally lensed gravitational wave science
• LIGO predicted to detect approaching one lensed NS-NS/year at A+ sensitivity (mid-2020s)
• Detection of lensed kilonova (KN) counterpart is required to localize the GW to a lens
• LIGO’s A+ sensitivity (2025) is well matched to early years of Rubin’s survey operations
• Lensed KN is detectable by Rubin with deep ToO follow-up (up to one hour per pointing)
• Recommend to include lensed NS-NS/KNe when testing impact of ToO micro-survey

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These slides summarize:�Smith, Nicholl, Ryczanowski et al., in prep.

See also:�Smith et al. arXiv:1902.05140

KN lightcurve models from: Nicholl et al. (2021)

gps@star.sr.bham.ac.uk/tanguita@gmail.com

Localize candidate lensed NS-NS to a lens* via deep ToOs

*Lenses span galaxies, groups and clusters (Robertson et al. 2020)

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Strong Lensing Science Collaboration

Lensed NS-NS/KNe and deep Rubin ToOs

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LIGO detection: �A+ sensitivity will enable detection of lensed NS-NS in mid-2020s

Candidate selection:�70% of lensed NS-NS are placed in the mass gap in low latency

Rubin follow-up:�Typical lensed KNe require deep ToOs within 1-2 days

Smith, Nicholl, Ryczanowski et al., in prep.; see also Smith et al. arXiv:1902.05140; KN lightcurve models from Nicholl et al. (2021)

gps@star.sr.bham.ac.uk/tanguita@gmail.com

Mass gap

z≈1-2

AT2017gfo-like lensed KN (⇒ optimistic)

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Strong Lensing Science Collaboration

Lensed NS-NS/KNe and deep Rubin ToOs

• Challenges and opportunities to collaborate (some relevant to SCOC, some not) include:
• Developing a workable approach to reference images, especially for early years
• Careful vetting of candidates, building on O3(+O4) experience
• Characterising the false positive population
• Testing recovery of faint lensed transients in difference imaging analysis (e.g. figures at right)
• Testing Scarlet deblender in cores of galaxy group/cluster-scale lenses

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Smith et al. (2019, MNRAS, 485, 5180)

80% of injected transients recovered down to nominal depth of data well inside tangential critical curve in locally optimized difference images

gps@star.sr.bham.ac.uk/tanguita@gmail.com

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Strong Lensing Science Collaboration

Additional concerns

• How is image quality measured / optimized? (e.g. variable exposure time simulations)
• Could we have a different image quality (gri) optimized strategy only for the first year? (see trilateral AGN/TVS/SL session tomorrow)
• Two band rolling baseline might be an issue for quasar time-delay measurements and microlensing (also see trilateral AGN/TVS/SL session).
• Recommend to include deep ToOs when simulating impact of ToO micro-survey on survey cadence and observing strategy

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gps@star.sr.bham.ac.uk/tanguita@gmail.com

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Galaxies Science Collaboration

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s.kaviraj@herts.ac.uk

SCOC report -- Generally looks good!

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• Longer u-band exposures are a high priority
• Greater overlap with Euclid is a high priority
• Nice to see Virgo Cluster Micro-survey included in future investigations

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Chairs: Sugata Kaviraj (Hertfordshire); Manda Banerji (Southampton)

https://tinyurl.com/lsstgalaxies

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Galaxies Science Collaboration

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s.kaviraj@herts.ac.uk

Consider year-1 optimization

Insurance policy for good start on static-sky catalogs

• At least 25% of r-band exposures taken in the top quartile of seeing on every field in year 1.
• Provides a minimum baseline for peak detection
• (This isn’t particularly ambitious -- weighting to even better seeing in r-band would be even better)
• At least a few u-band exposures taken in photometric conditions at low airmass.
• u-band photometric calibration is the most difficult
• Possibly a greater payoff from this than 50s vs 30s exposures?
• Difficult to construct simple high-level science metrics that would drive either of these.
• But easy to imagine adding weights to scheduling to give these priority.

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https://tinyurl.com/lsstgalaxies

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

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SLSC + Galaxies Q/A

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Stars, Milky Way, Local Volume SC

�Will Clarkson (wiclarks@umich.edu)

Broad science areas (by science working group)

1. The Solar Neighborhoods
2. Star Clusters
3. Variable Stars (STRONG overlap with TVS and DESC)
4. Galactic Structure and the ISM
5. The Galactic Bulge
6. The Magellanic Clouds
7. Near-field cosmology

Improved coverage of the bulge, plane, and Magellanic Clouds, has been a main request from the Galactic science community for some time.�

For much of SMWLV science, v2.0 represents a substantial improvement compared to previous baselines, particularly in moderately crowded regions. The new default footprint is a major improvement over v1.5 and v1.7.

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(In the list at left, entries in bold are generally improved by increased coverage of areas of high stellar density.)

Most groups* are still working on re-running their metrics on baseline v2, here follows some immediate feedback:

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Stars, Milky Way, Local Volume SC

Will Clarkson (wiclarks@umich.edu)

Example: proper motion uncertainty as a proxy for time sampling & depth:

Street et al. (2021 rubin cadence note)

v1.7.1_10yrs

v2.0_10yrs

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Stars, Milky Way, Local Volume SC

(Cool) brown dwarf detection not seriously compromised (metric described in Gizis et al. 2021 cadence note)

v1.7.1: 179k L7 brown dwarfs with y-band uncertainty <0.2 mag

v2.0: 168k L7 brown dwarfs with y-band uncertainty <0.2 mag

Will Clarkson (wiclarks@umich.edu)

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Stars, Milky Way, Local Volume SC

*For young stellar object discovery, v2 baseline is much better than v1.7.

Best choice: WFD Nvisits as in gp_smooth v1.5 (Loredana Prisinzano et al. 2021-11-13)

Will Clarkson (wiclarks@umich.edu)

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Stars, Milky Way, Local Volume SC

Filter balance in plane, bulge, MC’s? Static science → high accuracy in all filters, tradeoff vs variability?

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What about the plane outside the bulge (including the “dusty plane”)? Probably don’t want to go below 0.27 x WFD (~230 epochs per field, for variability, proper motion...). Some cases prefer 0.5 x WFD or more. Known metrics in preparation (e.g. YSOs): also, the ISM itself and Galactic structure?

�Rolling cadence: needs more exploration for Galactic variability studies → tradeoff against static science

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Short exposures: Required for calibration (bright foreground stars in many regions): needed in year 1? Commissioning? �Parallax tradeoff against other science cases?

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Seeing distribution needs to be incorporated into community metrics… e.g. 75 %-ile rather than best?

Developments during 2021

Open issues to be addressed via metrics into rubin_sim (“missing metrics” session)

• 3D extinction map + query tools are being prepared for incorporation into rubin_sim (led by Alessandro Mazzi)
• The rubin_sim-predicted spatial confusion limit probably *is* about right… to reproduce {grizy} DECam confusion-limited depth, can use CrowdingM5Metric() with crowding_error=0.25 mag or so (writeup in prep).

Will Clarkson (wiclarks@umich.edu)

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Stars, Milky Way, Local Volume SC

Filter balance in plane, bulge, MC’s? Static science → high accuracy in all filters, tradeoff vs variability?

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What about the plane outside the bulge (including the “dusty plane”)? Probably don’t want to go below 0.27 x WFD (~230 epochs per field, for variability, proper motion...). Some cases prefer 0.5 x WFD or more. Known metrics in preparation (YSOs): also, the ISM itself and Galactic structure?

�Rolling cadence: needs more exploration for Galactic variability studies → tradeoff against static science?

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Short exposures: Required for calibration (bright foreground stars in many regions): needed in year 1? Commissioning? �Parallax tradeoff against other science cases?

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Seeing distribution needs to be incorporated into community metrics… e.g. 75 %-ile rather than best?

Developments during 2021

Open issues to be addressed via metrics into rubin_sim (“missing metrics” session)

• A 3D extinction map + query tools are being prepared for incorporation into rubin_sim (led by Alessandro Mazzi)
• The rubin_sim-predicted spatial confusion limit probably *is* about right… to reproduce {grizy} DECam confusion-limited depth, can use CrowdingM5Metric() with crowding_error=0.25 mag or so.

Will Clarkson (wiclarks@umich.edu)

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Transients and Variable Stars SC

Rachel Street rstreet@lco.global

https://lsst-tvssc.github.io

Survey Strategy Task Force:

• 2020: Rachel Street, Rosanne DiStefano, Federica Bianco, Sara Bonito
• 2021: Rachel Street (Chair), Sara Bonito, Rosanne DiStefano, Claudia Raiteri, Igor Andreoni, Andjelka Kovacevic, Michael William Coughlin, Robert Szabo, Ilya Mandel, Ilaria Musella, Silvio Leccia, Dragana Ilic, Giulia De Somma, Marcella Marconi, Maribel Carnerero

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Credit

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We acknowledge consistent efforts by many TVS members and productive collaborations with other Science Collaborations

Phase 1 recommendations incorporate much of this community input

TVS appreciates the SCOC’s consideration, and gratefully acknowledges support from the MAF Team.

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Please see Rubin Cadence Notes - SMWLV + TVS Synthesis document

https://drive.google.com/file/d/1XoZVUVLCIaV2dbynbrWL9KSqSSHqjs0P/view

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q1: Are there any science drivers that would strongly argue for, or against, increasing the WFD footprint from 18,000 sq. deg. to 20,000 sq.deg.?

• Optimization of survey footprint and cadence by sky region strongly supported
• Value the added coverage of the Galactic Bulge and Magellanic Clouds
• Note that baseline v2.0 limits observations of a number of key regions
• We propose a set of pencilbeam fields to help area trade-offs

Pencilbeam fields

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q2: What is the best use of additional observing time?

• Recognize tensions between galactic and extra-galactic science
• Strongly value Galactic Plane, Magellanic Clouds minisurvey
• Stress the value of observations of SFRs
• Propose detailed discussion post-workshop (Bonito & Venuti et al.)
• Emphasize need for coordination with Roman for Bulge survey, and Euclid for DDFs

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q3: Arguments for and against changing the u-band exposure to 1x50s

• We recommend some fraction of shorter exposures to avoid saturation and extend dynamic range

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q4: Arguments for/against changing time allocated per band

• We recommend optimizing the time per filter allocation for the Galactic Plane and note this will occur in Phase 2
• We emphasize the value of u-band observations for metallicity measurements, and characterization of TDEs, young stars, but balance between filters is also important

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q5: Arguments for/against two observations per night in same or different filters

• We recognize the tensions between different science cases, which argue for both the same and different filters for subsequent observations
• Somewhat dependent on sky region; surveys could be optimized separately
• Fast transients, microlensing anomalies and more favors shorter intervals; but longer intervals still valuable for many science cases

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q5: Arguments for/against two observations per night in same or different filters

• Further evaluation of Presto-Color strategy needed
• Requires 3 obs/night in g, i with time gaps <1.5hrs and >4hrs
• Ming simulated strategy with PLAsTiCC data
• We recommend close coordination with F. Bianco/M.Lian to ensure implementation is correct

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q6: For or against rolling cadence?

• Beneficial for a lot of science but the length of the season (and gaps) will limit study of long-term phenomena
• Black hole lensing, t_E~100-300d, Miras etc)
• Coordination with other surveys (esp. Roman, Euclid) highly advisable
• Galactic Bulge, DDFs

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q7: For or against dithering?

• For astrometry, dithers need to be statistically uncorrelated with parallax factor and DCR.
• Most cadence notes did not express a strong preference for or against dithering; those that did, generally indicate that rotational or large translational dithers tend to improve the science.

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS Feedback on Phase 1 Recommendations

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Q7: For or against dithering?

• For astrometry, dithers need to be statistically uncorrelated with parallax factor and DCR.
• Most cadence notes did not express a strong preference for or against dithering; those that did, generally indicate that rotational or large translational dithers tend to improve the science.

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

TVS Response to SCOC Feedback

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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TVS White Paper submissions

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TVS members contributed 40% of the 2018 White Papers, representing the wide range of science we cover.

Many, but not all, included metrics

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Joint Metrics Spreadsheet

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64 community-contributed metrics from all Science Collaborations

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Joint Metrics Spreadsheet

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64 community-contributed metrics from all Science Collaborations

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

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ApJ Strategy Special Edition papers in prep/submitted

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Federica Bianco et al. Optimization of the Observing Cadene for the Rubin Observatory

Xiaolong Li et al. Preparing to discover the unknown with Rubin LSST I: Time domain

Fabio Ragosta et al. Preparing to discover the unknown with Rubin LSST II: Proper motion

Sara Bonito et al. Young stellar objects and their variability with Rubin Observatory LSST

Rachel Street et al. LSST Survey Footprint in the Galactic Plane and Magellanic Clouds

Claudia M. Raiteri et al. Blazar variability with the Vera C. Rubin Legacy Survey of Space and Time (LSST)

Loredana Prisinzano et al. Maximize volume and uniformity coverage of Star Forming Regions in the Galactic

Plane with Rubin LSST

Kresimir Tisanic et al. Simulations of multiband Lomb-Scargle-derived variable star periods

Piero Dal Tio et al. TRILEGAL simulation of the LSST stellar content

Igor Andreoni et al. Optimizing Cadences with Realistic Light Curve Filtering for Serendipitous Kilonova

Discovery with Vera Rubin Observatory

Will Clarkson et al. Saturation and bright objects

Will Clarkson et al. The Galactic Bulge with LSST

Andjelka Kovacevic et al. Photometric reverberation mapping in the era of LSST

Ilaria Musella, et al. Classical variable stars in different Galactic environments: pulsation behaviour recovery.

Natasha Abrams, et al. Microlensing Discovery, Alerts, and Characterization Efficiency at Different Timescales in

the Vera C. Rubin Legacy Survey of Space and Time

Nina Hernitschek et al. The Impact of Observing Strategy on Reliable Classification of Standard-Candle Variable Stars:

Detection of Amplitude, Period, and Phase Modulation (Blazhko Effect) with LSST

Eric Feigelson et al. A Rapid LSST Cadence for Variable Stars

Igor Andreoni et al. Target of Opportunity Observations of Gravitational Wave Events with

Vera C. Rubin Observatory

Eric Bellm et al. Give Me a Few Hours: Exploring Short Timescales in Rubin Observatory Cadence Simulations

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Questions and Concerns

• High-cadence intensive observations, esp SFR?
• Rubin ToOs
• Acquisition of templates/early science and commissioning
1. Should metrics for science cases provided in the TVS Commissioning Note be integrated in MAF?
2. Combine microsurvey & commissioning metrics? Some require different timescales
• 1-to-1 feedback for non-integrated metrics

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

Resources

• Spreadsheet of community metrics and metric packages
• Summary presentation describing community-contributed metrics
• Presentation on Galactic Plane and Magellanic Cloud Metric Package
• Metric package document for the Galactic Plane and Magellanic Clouds
• Metric package document for microlensing
• Metric package for transients
• Impact of LSST template image acquisition on
1. Time-critical science
2. Non-time critical science

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TVS Feedback presentation full slide deck

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Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

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SMWLV + TVS Q/A

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary

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THANK YOU!!

Rubin LSST Science Collaborations

Vera C. Rubin Observatory | SCOC Second Workshop | 16-17 November 2021

Acronyms & Glossary