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)
- Past
- 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
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
CHARA meeting
By Nic Scott
