NESSI, 'Alopeke, and Zorro

Nic Scott

NASA ARC

BAEM 2018

3 new speckle imagers

DSSI/NESSI/`Alopeke/Zorro

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''

3-4x improvement over native seeing

40s

20min

Science Programs

40 total proposals

110.04 total nights

(NOAO 2016A to 2018B)

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 an 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

Some proposals so far:

optical, NIR imaging of host stars of KOIs
~ 90% of the confirmed and candidate exoplanet hosts
separations, PA, and dm for all detected, bound and LoS companion stars.
2297 companions around 1903 primary stars ~ 10% of the observed stars 1+ companions detected w/i 1”
correction factors for exoplanet radii caused by the dilution of the transit depth decreases the number of KOI planets with radii smaller than 2 Earth radii by 2% - 23%

Furlan's previous results applied to planets w/ known masses & radii, analyze the effects of a close stellar companion on planetary density.

50 planets orbiting 26 stars in the Kepler field
a transit dilution requires the planet radii to be revised upward, decreasing the density of the planet
if planet orbits a faint companion star, density may decrease by ~ 3x

The effect of close ~ 0.5” companions of Kepler and K2 planet candidate hosts had on the inferred exoplanet radius distribution.

Fulton gap is robust regarding undetected stellar companions
gap became broader & shallower when accounting for possible undetected stellar companions
core composition of super-Earth and sub-Neptune exoplanets may not have so strong a divide as is suggested initially
w/o high-resolution imaging of Kepler and TESS host stars, the exoplanet radius distribution will be incorrectly inferred.

(2018, in press)

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''

Shift from 1.8 to 2.2

increased water/ice vs pure Si rock

R_E

R_E

170 KOI companions < 2” using AO, speckle, lucky, or the HST
constrained their stellar properties and assessed the probability that the companions are physically bound
60 - 80% of companions < 1” & > 90% of companions < 0.5” were found to be bound
assuming the planet is equally likely to be orbiting the primary or secondary, unless they are vetted, nearly half of all Kepler planets may have radii underestimated by an average of 65%.

DSSI @ G-S
highest-resolution images to date
27 mas
imaging from 0.32 to 14.5 au
excludes all possible stellar and brown dwarf companions

Open to the community

NOAO proposal process
NESSI - WIYN@KPNO
`Alopeke - Gemini-N
DSSI -> Zorro - Gemini-S
Transitioning from visitor to ''Resident'' instrument

backup slides

Science Programs

40 total proposals

110.04 total nights

(NOAO 2016A to 2018B)

Title Text

Text

Publications

Text

blue bars are refereed citations to refereed papers

green bars are non-refereed citations to refereed papers

SAO/NASA ADS “Bumblebee” search: ‘‘speckle’’ - ‘‘speckle noise’’

limited to astronomy and refereed
removed AO speckle noise references
excluded AO and spectroscopic techniques
constrained to 1970+ sorted by citation count

This search returned 1,139 papers with 24,181 total citations

rise of EMCCDs & start of large speckle survey programs (& Kepler)?

672.9

mas

Seeing-limited

Reconstructed

42''

Two-color wide-field speckle reconstruction

from NESSI

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

Urban telescope WF speckle

Wide-field speckle techniques for small, urban telescopes, Nicole M. Granucci, Elliott P. Horch, Southern Connecticut State Univ. (USA) talk Tues (coming up next actually)[10701-20]

Pluto opposition

SOFIA occultation target duplicity

WF and speckle optics

Conv and EMCCD imaging

466/832 and g/i filters

New Horizons (not us.....yet)

TNO Varda ⌀~700km, d~50au

multiplicity is the single largest source of error to occultation path prediction

NEAs

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