CHARA

Meeting

Meudon 2018

nic scott

NASA ARC

Speckle interferometry at NASA ARC

Speckle...

the once and future interferometry?

  • Speckle Imaging Group
  • Instruments
    • Past
      • DSSI
    • Present
      • NESSI
      • `Alopeke
    • Future
      • Zorro
      • QWISSI, SEXSI (Gerard)
  • Techniques
    • Wide Field
    • Extended objects
  • Projects

2018 Speckle retreat, following the "Know thy Stars. Know thy Planet" meeting

DSSI

Author network

DSSI Papers

DSSI Reads

NESSI papers

Speckle

  • 10mas/pxl
  • mag limit ~17
  • contrast limit ~8

Wide Field

  • 73mas/pxl

Speckle

  • 18mas/pxl
  • mag limit ~14
  • contrast limit ~6

Wide Field

  • 81mas/pxl

0.011'' @u

0.026'' @832nm

0.025'' @u

0.060'' @832nm

6.7''

60''

19''

56''

Twin instruments in the North and South.

  • TESS follow-up
  • whole sky surveys
  • Quad-channel
  • Wave-front sensing
  • Possible near-IR channel?
  • DSSI heritage at the DCT+NPOI

QWSSI

observed

bound (simulated)

line-of-sight (simulated)

K2 binaries detectable with DSSI-

Matson et al. 2018 (submitted)

Companions of Kepler false positives

Furlan et al. 2017

Furlan & Howell 2017

Furlan & Howell 2017

Fulton

mini-neptunes

super-Earths

  • Large radius errors originally hid distribution features
  • Fulton gap revealed after CKS (10% stellar radius errors)
  • Accounting for binarity shifts gap in the distribution

brightest companion 1''

brightest companion 2''

Teske et al. (in prep.)

Shift from 1.8 to 2.2 

  • increased water/ice vs pure Si rock
R_E
RER_E

Seeing-limited

Reconstructed

42''

Two-color wide-field speckle reconstruction

  • 0.25'' resolution from 500 frames (20s)
  • compromise b/t angres and contrast
  • Seeing ~ 0.85''

Text

Text

M13

  • astrometry of clusters
  • very early results and little calibration or modelling over the FoV

Reconstructed

Seeing-limited

Abs astrometry residuals

~6-7 mas

4.2 mas

Further improvement possible to obtain ~0.02 pix (~0.4mas)

  • optics, dither, deeper obs

0.05 mag accuracy on aperture photometry

FWHM ~7pix (0.57'')

FWHM ~4pix (0.3'')

NEAs

  • sizes
    • radar typically quotes 40% uncertainties
    • albedo/radar size mismatch
  • shapes
    • adapt stellar surface modeling tools
    • light curve inversion/illumination model 

a~2.8AU

d~270km x 80km

(neck~50-65km)

model: Franck Marchis

Phaethon

Dec 2017 ~ 0.07AU

d~6km

Point source PS

Phaethon power spectrum (resolved)

Exozodis

JouFLU

  • Flux limited to 1.6% at 0.1''
  • Any companion T ≥ 2500K (M8V/M9V) is eliminated.

 

Open to the community

  • NOAO proposal process
  • NESSI - WIYN@KPNO
  • `Alopeke - Gemini-N
  • DSSI - Gemini-S
  • Transitioning from block queue operation to Facility Instrument status

NPP & internship opportunities: see me for details

Some other proposals so far:

  • Constrain NEA diameters. Image SS objects.
  • Determine multiplicity of nearby K and M-dwarfs, does it vary across spectral type?
  • Imaging of brown dwarfs and distant large planets, particularly around M dwarfs.
  • Investigate differences in planetary system architectures between multiple vs not (known) multiple host stars.
  • Examine long term RV trends/determine binarity of RV planet hosts.  
  • K2, TESS follow-up
  • Provide and unbiased sample for TESS, so statistical determinations of planet occurrence rates can be made.
  • Occultations, Transit photometry, Pulsar time scales, observe pulsating WDs at high cadence....

References

  • Scott, Howell, Horch, & Everett. PASP 2018 (accepted)
  • Horch et al. AJ 2012
  • Furlan et al. AJ 2017
  • Furlan & Howell AJ 2017
  • Horch & Casetti-Dinescu 2018 (in prep.)
  • Matson et al. 2018 (submitted)
  • Teske et al. 2018 (in prep.)
  • Fulton et al. AJ 2017