1. The SDSS-III MARVELS Survey: Overview and First Results Nathan De Lee and the MARVELS Team

2. De Lee, Shanghai 2009 MARVELS TEAM Principal investigator: Jian Ge (UF) Survey scientist: Holland Ford (JHU) Project manager: Fred Hearty (UF) Instrument scientist: Xiaoke Wan (UF) SWG chair: Eric Agol (UW) Data coordinator: Brian Lee (UF) MARVELS SWG Members: E. Agol, E. Ford, H. Ford, S. Gaudi, D. Schneider, J. Holtzman & S. Seager UF Staff and Postdocs: X. Wan, S. Mahadevan, B. Lee, B. Zhao, J. Groot, F. Hearty, K. Hanna, F. Varosi, J. van Eyken, S. Kane (UF and IPAC), L. Chang, Z. Chen, J. Liu, C. Murphey, S. Thirupathi, & N. De Lee UF Grads and Undergrads: S. Fleming, P. Guo, P. Jiang, M. Malik, A. Shelden, J. Crepp, J. Wang, A. Fletcher, P. Rohan, E. Costello, & S. McDowell Other collaborators: D. Eisenstein, D. Weinberg, J. Gunn, F. Leger, P. Harding, M. Blanton, J. E. Martin, Bochanski, A. Wolczczan, A. Niedzielski, D. Montes, S. Hawley, D. Schlegel, & S. Snedden

3. De Lee, Shanghai 2009 SDSS-III Since September 2008, SDSS III has been using the wide field Sloan 2.5m Telescope for up to 4 projects: All using massive fiber-fed spectroscopic surveys BOSS: A Baryon Oscillation Survey with a 1000 fiber spectrograph APOGEE: A NIR H band R~20k spectrograph to look at K giants SEGUE-2: Galactic Dynamics using current SDSS spectrographs MARVELS: Multi-Object APO Radial Velocity Exoplanet Large Area Survey

4. De Lee, Shanghai 2009 MARVELS Overview Monitor a total of 10,000 V=7.6-12 FGK dwarfs and subgiants Monitor a total of 1,000 V=7.6-10 G and K giants Both groups will be selected with minimal metallicity and age biases for detecting and characterizing ~200 giant planets. Use all of the bright time in 2008-2011 and share the bright time with APOGEE in 2011-2014 Approx. 120 fields will be monitored about 30 times over ~18 months Up to two multi-object Doppler instruments with a total of 120+ object capability The wavelength coverage ~ 500-570 nm Spectral resolution ~10,000

5. De Lee, Shanghai 2009 MARVELS Science Goals  To find a homogeneous sample of several hundreds of giant planets that can be used for statistical study of planet properties and comparison to theory Constrain formation, migration & dynamical evolution of planetary systems Discovery of rare systems (e.g. “Very Hot Jupiters”, short-period super-massive planets, short-period eccentric planets, transiting planets, highly eccentric planets, rapidly interacting multiple planet systems, planets orbiting low-metallicitiy host stars, planets around active and young stars, and other rare types of planets) Find signposts for lower-mass or more distant planets Quantify the brown dwarf desert

6. De Lee, Shanghai 2009 MARVELS Field Selection  Survey area is ~800 sq deg, a total of ~120 fields, mainly along the Galactic plane  About 80 fields will be shared with APOGEE in 2011-2014  Field selection is based on sufficient number of bright observable stars in each field, and some fields need to have known calibrators for initial instrument calibration  64 fields, including some calibration fields, have been selected for the first two years of operation A number of fields have also been selected to coincide with the one of the 21 CCD modules of the KEPLER space mission

7. De Lee, Shanghai 2009 Preselection Targets Targets initially selected from GSC2.3 catalog matched up with 2MASS for J, H, K colors SDSS spectroscopy pre-selection efficiently remove giants (e.g., log g 6250 K) from the initially color selected targets 25-35% of the ~500 candidates per field are acceptable targets Effective temperature and gravity plot of target candidates of 7 fields

8. De Lee, Shanghai 2009 Final Distribution of Targets Final distributions based on 41 of the 60 first season fields

9. De Lee, Shanghai 2009 Current Survey Status Number of Survey Observations: 489 Number of Plates Observed: 43 Total Number of stars: 2580

10. De Lee, Shanghai 2009 Current Error Estimates RMS errors based on current pipeline from the Instrument Acceptance Review.

11. De Lee, Shanghai 2009 Reference Star Fits HD 68988 V=8.21, G0, 1.9 M J, P=6.276 days, e=0.14 (Vogt et al. 2002) HIP 14810b V=8.52, G5, 3.84 M J, P=6.67 days, e=0.15 (Butler et al. 2006)

12. De Lee, Shanghai 2009 Brown Dwarf Candidate More information will be available in Lee et al. 2009 in preparation

13. De Lee, Shanghai 2009 MARVELS Pipeline Development To help reduce systematics in the MARVELS data, a number of avenues are being looked at: – PV Scale correction – Cosmic ray rejection – Distortion correction – Low flux spectra Dispersion direction

14. De Lee, Shanghai 2009 Summary and Future Work The MARVELS instrument is producing radial velocity data in survey mode. Continue work on the MARVELS Pipeline Look into methods to increase throughput Work on hardware upgrades / repairs Develop large scale RV fitting procedures Further the groundwork for the second instrument. Follow-up current candidates