WIDE BINARY SCIENCE USING PAN-STARRS1 NIALL DEACON (MPIA) MICHAEL LIU, EUGENE MAGNIER, WILL BEST, KIMBERLY ALLER, MICHAEL KOTSON (HAWAII), BRENDAN BOWLER.

WIDE BINARY SCIENCE USING PAN-STARRS1

NIALL DEACON (MPIA)

MICHAEL LIU, EUGENE MAGNIER, WILL BEST, KIMBERLY ALLER, MICHAEL KOTSON (HAWAII), BRENDAN BOWLER (CALTECH), ADAM KRAUS, TRENT DUPUY, ANDREW MANN (TEXAS)

BREAKING THE DEGENERACY

Saumon & Marley models

PSO 318-22:THE “LONELY PLANET”

Liu+ 2013

PSO J318.5−22 is the first free-floating object with the colors, spectra, magnitudes, luminosity, and mass that overlap the young dusty planets around HR 8799 and 2MASS J1207−39.

PS1 + 2MASS SEARCH FINDS SUBSTELLAR MEMBERS OF YOUNG MOVING GROUPS

Wavelength (μm)

Flu

x +

Con

stan

t

Incr

easi

ng A

ge

40 MJup

Kimberly Aller (IfA)

BENCHMARK SYSTEMSWide companions to main sequence stars

Age, distance and metallicity determined from primary

Break degeneracy

Formation mechanism for wide binaries uncertain

2MASS J

BENCHMARKSWHAT ARE THEY GOOD FOR?

Testing atmospheric models of ultracool dwarfs.

Deacon et al. (2012) Burningham et al. (2009)

Higher order multiples can also have masses measured.

Dupuy et al. (2009,2014)

Used to define metallicity relations for M dwarfs. Mann et al. (2014), Newton et al. (2014), Royas-Ayala et al. (2012)

Huh! GoodGodY’all!

Starr et al. 1969

SELECTING CANDIDATES

Input primary listHigh m Hipparcos starsM dwarfs from LSPM, rNLTT, Lepine & Gaidos (2011)

Search PS1 proper motions for objects with comparable proper motions (rmax = 10,000 AU or 20 arcmins)

Follow up companions with IRTF/SpeXHigh priority: zp1-yp1 > 0.8Back-up: J<15Preferentially followed up close (<5 arcmins) companions

DISCOVERY SUMMARY

58 new companions

31 known

24 new Ls

23 late Ms

Deacon et al. ApJ revised

Open: total knownSolid: Our contribution

Doubled

82% more

Deacon et al. ApJ revised

NEW ATMOSPHERIC MODELS REPRODUCE TEMPERATURES WELL

Deacon et al 2012

HIGHER ORDER MULTIPLICITY

8 of our objects are tertiary components

One companion showed usual water band absorption

Spectra suggest L1 + T3

See Burgasser (2007), Dupuy & Liu (2012) for methodology

Keck NIRC2 LGS/AO0.12” binary>300 yr period

WIDE COMPANIONS AND EXOPLANETS

Kaib et al. 2013

Full proper motion survey of the Kepler field using all available data

GOALS

Probe effect of wide binarity on planet occurrence

Wide binaries as tests of gyrochronology

Testing axial alignment of binaries

Powerful legacy dataset to characterise Kepler planet hosts

PS1 KEPLER STANDARD PROJECT

ASTROMETRIC ACCURACY

PROBLEM AREAS

Reduced Proper MotionHr = r +5 + 5log10mHr = Mr + 5log10vt + const

PS1 KEPLER STATUS

Combining PS1 + 2MASS + POSS I & II+ UKIRT + WISE+SDSS

Will rerun on corrected DVO database

Include Skyprobe data for bright KICs

High resolution spectroscopic follow-up at McDonald

Probabilistic binary selection

STS field

Run on K2 fields?

TO-DO

CLOSE BINARIES IN SYNOPTIC SURVEYS

Objects have ≈50 observations in PS1

True binaries will be more elliptical in better seeing

Can be used to identify >0.4’’ binaries in PS1 data

0.4” binary

First used on PTF data by Terziev et al. (2012)

Blue histogram: objects not resolved as binaries with AO

SUMMARY

Doubled the number of wide late M companions

82% increase in wide late L companions

Most successful survey for benchmark companions to date

PS1Kepler probing wide binary – planet connection

Synoptic surveys provide a wealth of data for discovering new multiple systems

COINCIDENT?

STABILITY

Deacon et al. ApJ revised