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 MJ @ 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 MJ, , 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 MJ, 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)

– Teff ~6200 K – log g ~ 3 9 log g 3.9 – [Fe/H] ~ -0.15 – Vsini ~2.2 km/s

• Slightly evolved F8 star
• Slightly evolved F8 star

– M ~ 1.37 M – R ~ 2.20 R

Mi i 28M

• Minimum mass ~ 28MJ
• 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 %. term variability at few %. g 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 RJ

True Companion Mass.

• Minimum mass ~ 28MJ
• Near driest part of the

p BD Desert.

• True mass unknown.
• Likely to be substellar

for reasonable priors.

• What we want to figure
• ut!

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 ddl i t t ti muddle interpretation

• Evolved state of host also

complicated the

• vsin

sini i ~ 2.2 km/s, ~ 2.2 km/s, R*

* ~2.2 R

~2.2 R, P* sini ~ 50 d (analysis by Rory Barnes) (analysis by Rory Barnes)

interpretation.

• Pcomp ~ 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

90MJ

• 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 i binaries.

– Binary Frequency M R ti Di t ib ti – Mass Ratio Distribution – Period Distribution

E li i bi i

• Eclipsing binary science.

– Few percent should be eclipsing. S ith t it f l! – Synergy with transit surveys very useful! – 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

using MARVELS

• New efforts underway (e.g., 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.

Al d ll f i t ti di i d i

• Already allows for very interesting discoveries and science

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.