Student-led Presentations & Discussions
The instructor will lead discussions for the first few weeks. Subsequently, each student (or perhaps small group of students) will lead at least one class discussion on a relevant topic of interest on their assigned date. All students will be expected to devote approximately one hour per week to reading and submitting questions/comments on the reading (typically via Perusall, see link from course webpage in Canvas). Reading questions and comments are due 24 hours before the start of class, so the presenter has time to incorporate these into their discussion plans. See the presentations section of the syllabus for details about what is expected and the timeline for preparing your presentation.
Schedule of Reading/Discussion Topics
| Week | Date | Leader | Topic | Reading |
|---|---|---|---|---|
| 1 | Aug 28 | Ford | Overview of Course & What is EPRV? | Crass et al. (2021), Exec Summary |
| 2 | Sep 4 | Ford | Intro to Precision RV Observations | Hara & Ford (2023), S1-2.3 |
| 3 | Sep 11 | Ford | Intro to RV Extraction | Harra & Ford (2023), S3 |
| 4 | Sep 18 | Ford | Intro to RV Analysis | Harra & Ford (2023), S4-4.5 |
| 5 | Sep 25 | HG | EPRV Instruments | Schwab et al. (2016) |
| 6 | Oct 2 | CR | EPRV Wavelength Calibration | HPF blog, Metcalf et al. (2019) |
| 7 | Oct 9 | KS | Stellar Variability: Magnetic Activity | Meunier et al. (2010), S1, 3.1; Meunier et al. (2019), S5 |
| 8 | Oct 16 | RZ | Classical Activity Indicators | Zechmeister et al. (2018), S3.1-4.4; Gomes da Silva et al. (2021), Appendix A2 |
| 9 | Oct 23 | EB | EPRV Survey Design | Crass et al. (2021), S 3-3.2.1, Table 3.3, S 4-4.2 |
| 10 | Oct 30 | AP | Significance of Exoplanet Detections | Hara & Ford (2023), S4, App C & D |
| 11 | Nov 6 | GM | Characterizing Masses & Orbits | Ford (2005): S 2-2.1, 4, Figs 2 & 4; Nelson et al. (2014): 4, 4.1 (skip 4.1.1-4.2), 4.2, (skip 4.2.1), Fig 2, Fig 4, S 6 |
| 12 | Nov 13 | GL | Rossiter-McLaughlin Effect | Gaudi & Winn(2018), S 2 & 6 |
| 13 | Nov 20 | KP | Mitigating Stellar Variability with ML | de Beurs et al. (2022) S 5-5.2, Figs 1, 2, 5, 11, 12 |
| Nov 27 | –- | Happy Thanksgiving | –- | |
| 14 | Dec 4 | SJF | Evaluating ML for EPRV | Zhao et al. (2022) S 3-5, Figs 4-6 |
| 15 | Dec 11 | EG | Sun-as-a-Star Observations | Lin et al. (2022) Sec 2.1, 2.2, 3.3; Ford et al. (2024) S 1 & 4 |
Suggestions for Potential Topics for Student-led Presentations & Discussions
PRV/EPRV data reduction
Spectral extraction
Wavelength calibration
RVs from Cross-Correlation Function (CCF)
RVs from template fitting
Exoplanet detection & modeling
Establishing the statistical significance of detections
Model fitting: Measuring exoplanet masses and orbits
Model fitting: Modeling multiple-planet systems
Correlated noise models
PRV/EPRV survey design
Target selection
Scheduling of observations
Requirements for detecting Earth-analogs
Stellar variability
Physics of stellar variabity
Magnetic activity
Stellar pulsations
Granulation
Other processes
Mitigating stellar variability
Classical stellar activity indicators
Line shape metrics
Data-driven/Machine-learning methods for mitigating stellar variability
Gaussian process models for correlated "noise"
EPRV Stellar Signals Project
Sun-as-a-Star Observations
EPRV instruments/surveys
Current/upcoming instruments: ESPRESSO, EXPRES, MAROON-X, NEID, KPF, iLocator
Calibration systems
Combing EPRV with other methods
Transit photometry
Rossiter-McLaughlin effect
Astrometry
Direct imaging
Students are welcome to propose one of the topics above, a combination or variation on one or two of the topics above, or an additional topic that is of particular interest to them. Students should suggest at least one source for them to read and select portions for other students to read. See the resources page to help get started finding some readings that might be relevant for your topic.