Gemini S peckle Imaging with DS S I at Gemini and the DCT - - PowerPoint PPT Presentation

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Gemini S peckle Imaging with DS S I at Gemini and the DCT - - PowerPoint PPT Presentation

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1 Gemini S peckle Imaging with DS S I at Gemini and the DCT Elliott Horch, S CS U DSSI 09.29.2016 ADeLA 2016 2 S peckle Imaging is S ingle-Aperture Interferometry In each exposure, t he effect of at mospheric t

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S peckle Imaging with DS S I at Gemini and the DCT

DSSI Gemini

Elliott Horch, S CS U

09.29.2016 ADeLA 2016 1

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S peckle Imaging is “ S ingle-Aperture” Interferometry

 In each exposure, t he effect of

at mospheric t urbulence is “ frozen.”

 If t he obj ect is double, t hen

t here are “ double speckles.”

 Image reconst ruct ion via

bispect ral analysis.

 Fast : no observing overhead.  Baselines are redundant .  S

peckle has been responsible for many high-qualit y binary st ar orbit s over t he years.

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EMCCDs

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Photon counting performance with high quantum efficiency. Clocking accumulated charge through a series of gain registers builds up signal prior to reading out through the charge amplifier  sub-electron read noise.

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S

  • me S

peckle Cameras in Current Use

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Tip-Tilt Mirrors (M1,M2) EMCCD 1 Telescope Focal Plane Collimat ing Lens (L1) Reimaging Lens (L2)

Electronics Bay

EMCCD 2 Dichroic Beam S plit t er (S1) Reimaging Lens (L3)

Filter (F2) Filter (F1) Space for Risley Prisms

A Uniquely Capable S peckle Imager Built at S CS U

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1 arcsec

What the DS S I Camera Does

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Gemini-N

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Used 2012-present, official visiting instrument, 4 different science projects on last run. (Jan 2016) WIYN Gemini

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Some Representative Projects

 K-Kids. Finding companions to K-type main sequence stars.  GOAL: G, M stars have been characterized but not K stars. If the rate of binarity is different for K stars, it will have implications for star formation. (T. Henry, E. Horch)  Kepler survey. Finding companions to KOIs and K2 objects.  GOAL: Characterize fraction of exoplanet systems that have stellar companions. (S. Howell, E. Horch)  Observing secondaries of known “wide” binaries – finding

  • companions. (A. Tokovinin, E. Horch)

 GOAL: will yield info on star formation processes.  Metal-Poor Binaries. (W. van Altena, P. Demarque ,E. Horch)  GOAL: Characterize “Second Parameters” of Mass-Luminosity Relation.

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K-Kids Poster Children of the Month

HIP 11565 Dist: 19.5 pc S eparation: 10 AU HIP 9603 Dist: 28.8 pc S eparation: 6 AU

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Data from Lowell Observatory’s Discovery Channel Telescope

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Companion Detection for Kepler

 TRILEGAL galaxy model.  Look in Kepler field at the appropriate distance range.  Use Raghavan 2010 binary/multiple star statistics from the field.  Ask with what frequency DSSI would detect Kepler star with a companion.

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Gemini: Kepler Stars with Companions

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KOI 3255

Kepler 437 =

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Error In Planet Radius

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Companion Detection for K2 using AO and speckle

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Crossfield et al. 2016, 5σ confidence limits

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Andrei’s “ BCs”

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Courtesy of Andrei Tokovinin, CTIO

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Metal-Poor Binaries

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What’s new? WIYNS PKL and GEMS PKL

 Two new “ facilit y” speckle cameras for WIYN and

Gemini-N  Dual-channel instruments, like DS

S I

 Both will have a “ speckle” mode and a “ wide-field” mode

(~1’ x1’ )

 Filters: narrowband speckle filters and S

loan griz.

 WIYNS

PKL (aka NES S I): engineering t ime t his Oct ober at

  • WIYN. S

hare port wit h Hydra, WHIRC.

 GEMS

PKL: engineering in Jan 2017? Will mount t o GCAL unit , will not t ake a current ly used port .

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What’s New? S peckle plus Wavefront S ensing

S imulation Results of Löbb, 2016.

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S peckle plus Wavefront S ensing

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What’s New: Gaia

 DR1 was released earlier this month.

 A few parallaxes of speckle binaries, but in preparing

  • bserving proposals for 2017A, I did not find not many.

 When will Gaia help with binaries and astrophysics?

 DR2 (current ly 2017) will cont ain more and bet t er parallaxes

t han DR1 but mainly single st ars.

 DR3 (current ly 2018) orbit s for short er period binaries.  DR4 (current ly 2019) first cat alog of non-singles.  DR5 (current ly 2022) full ast romet ric, phot omet ric, and RV

informat ion, final non-single cat alogs, exoplanet list .

 While speckle follow-up is unlikely at Gemini in a survey

mode, it is a possibility at WIYN, DCT and other 4-m class telescopes.

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S ummary

 S

peckle Imaging today:  S

uccess of DS S I has led t o t he cont ruct ion of t wo new speckle cameras available t o t he communit y at WIYN and Gemini.

 Many science proj ect s: S

t ars are import ant again!

 Biggest impact : finding and charact erizing st ellar

companions t o exoplanet syst ems.

 Can we make speckle even better?

 Incorporat e wavefront sensor informat ion.  Wide-field fast imaging.

 S

peckle follow-up can be used on Gaia binaries in the coming years.

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