Early y MARVELS Science Science Scott Gaudi The Ohio State - PowerPoint PPT Presentation

Early y MARVELS Science Science Scott Gaudi The Ohio State University The Ohio State University MARVELS Survey Scientist

MARVELS Discovery Space. Sensitivity down to ~100 m/s (eventually 20-40 m/s) for: • Large Number of Targets. Large Number of Targets. – Years 1+2 1680 stars with at least 15 epochs. • Homogeneous and Broad Sample of Homogeneous and Broad Sample of Targets. – V<11 5-12 Teff<6250K V<11.5 12, Teff<6250K – 70% dwarfs (40% F stars), 30% giants – No cut for binarity, youth, etc. y y

Number of Epochs.

Cadence.

RV Variability. 10 M 10 M J @ 30 days @ 30 days SNR>15 for 20 points SNR>15 for 20 points p

Detectability. K ~ 600 m/s for ~ 600 m/s for M M ~10 M ~10 M J , , P ~30d, ~30d, M * ~M ~M 

Science Enabled w ith Current Data. • Distributions of companion properties over two orders of magnitude in mass ratio and period. – Mass ratio distribution in one survey. – Period & eccentricity distribution through the BD desert. – Change in location of BD desert with primary Change in location of BD desert with primary mass. • Rare systems Rare systems. – e.g., Short period BD companions in the desert.

Synergy w ith Transit Surveys. Ground-based transit surveys target surveys target similar magnitudes as MARVELS as MARVELS. • Transiting Systems. • Eclipsing Binaries. • Intrinsic variability. Intrinsic variability. (Siverd et al., KELT RMSs) (Siverd et al., KELT RMSs)

Early Science. • Short-period BD discoveries (Fleming et al. 2010, Lee et al. 2010) • Several additional BDs and a rough measurement of the aridity of the BD desert. • Binary science, double-lined and eclipsing binaries.

The Brow n Dw arf Desert. (Grether & Lineweaver 2006) (Grether & Lineweaver 2006) • Known about for over 20 years, not well sampled. • Frequency of close BD companions ~0.1%.

TYC 2949-00557-1 •Marvels Pilot Project Discovery, Minimum mass ~ 64 M Marvels Pilot Project Discovery, Minimum mass ~ 64 M J , P~5.7d, Fleming et al. 2010. , P~5.7d, Fleming et al. 2010.

TYC 1240-00945-1

BD Candidate. • RV confirmation with SMARTS, HET. • P~5.9 days, K~2.5 km/s, circular. • Likely places this companion in the BD desert.

Host Star Characterization Host Star Characterization . • Multicolor absolute photometry (BVRIg’r’I’JHK). • Follow-up spectra (APO 3.5m, Follow up spectra (APO 3.5m, FEROS ESO 2.2m) – T eff ~6200 K – log g ~ 3 9 log g 3.9 – [Fe/H] ~ -0.15 – Vsin i ~2.2 km/s • Slightly evolved F8 star • Slightly evolved F8 star – M ~ 1.37 M  – R ~ 2.20 R  • Minimum mass ~ 28M J Mi i 28M • Transit Probability is high ~ 14%

KELT Data. •5036 data points over ~ 4 years, RMS of ~1% (V~10.5). 5036 data points over ~ 4 years, RMS of ~1% (V~10.5). •No evidence of intrinsic long No evidence of intrinsic long-term variability at few %. g term variability at few %. y •RMS of phased curve binned by 0.04 in phase is ~0.06%. RMS of phased curve binned by 0.04 in phase is ~0.06%. •Rule out transits at 95% c.l. for radii >1.2 R Rule out transits at 95% c.l. for radii >1.2 R J

True Companion Mass. • Minimum mass ~ 28M J • Near driest part of the p BD Desert. • True mass unknown. • Likely to be substellar for reasonable priors. • What we want to figure out!

Tidal Effects. • Mass, close companion - tidal effects are likely important. important. • Can spin up star and evolve to a synchronous state state. • Measurement and theoretical uncertainties muddle interpretation ddl i t t ti (analysis by Rory Barnes) (analysis by Rory Barnes) • Evolved state of host also complicated the • v sin sin i i ~ 2.2 km/s, ~ 2.2 km/s, R * * ~2.2 R ~2.2 R  , P * sin i ~ 50 d interpretation. • P comp ~ 5.9 d

Additional BD Candidates. •8 BD candidates 8 BD candidates •From ~1800 stars •From ~1800 stars From ~1800 stars From ~1800 stars •Broad Range of Broad Range of Properties Properties -Period 2 Period 2- -120d 120d -Mass 23 Mass 23- -90M 90M J -Range of Range of eccentricities eccentricities •See talk by Nathan See talk by Nathan y De Lee. De Lee.

Mapping the Shores of the Brow n Dw arf Desert

Binary Science. • Expect ~10% of targets to be spectroscopic bi binaries. i – Binary Frequency – Mass Ratio Distribution M R ti Di t ib ti – Period Distribution • Eclipsing binary science. E li i bi i – Few percent should be eclipsing. – Synergy with transit surveys very useful! S ith t it f l! – KELT covers 60% of MARVELS Y1-2 targets. – Cross reference of SB from MPP with WASP Cross reference of SB from MPP with WASP yeilded two EB (Fleming et al.).

Binaries from MARVELS.

Building Infrastructure. • Collecting and consolidating follow-up resources: Collecting and consolidating follow up resources: – Spectroscopic: KPNO, HET, SMARTS, APO, ESO, additional. – Photometric: HAO, KELT, WASP, numerous small telescopes. • Developing analysis tools: Developing analysis tools: – RV searching and fitting, transit analysis, host star characterization tools, interpretation tools. • Processes for applying these tools to new systems are being streamlined and upscaled. • New efforts underway (e g • New efforts underway (e.g., using MARVELS using MARVELS spectra for host star characterization.)

Summary. • MARVELS Discovery Space currently includes 2 orders of magnitude in companion mass period for ~1700 stars magnitude in companion mass, period for 1700 stars. – Pipeline improvements will allow another order of magnitude in mass. • Already allows for very interesting discoveries and science Al d ll f i t ti di i d i for BD and binary companions. • Detailed analysis of a ~28 Jupiter mass companion Detailed analysis of a 28 Jupiter mass companion highlights this potential. • Also illustrates: – Development and consolidation of collaboration resources, follow-up capabilities, and analysis infrastructure. – Excellent synergy with transit surveys. • With an additional 7 BD companions, we are beginning to map out the BD desert.