review of the array

• 0.20 mas at R (650 nm)
• 0.52 mas at H (1.67 μm)
• 0.66 mas at K (2.13 μm)

TelAO

LabAO

staff changes

• Theo retired
• Larry the site manager retired
• Laszlo and Judit retired

New hires:

• Narsi Anugu
• Rob Ligon
• Nic Scott

...New Projects, new combiners

AO+6T observing is regular now, soon most nights may be 6T IR+VIS with MIRC-X, MYSTIC, & SPICA running simulataneously

CMAP

(CHARA Michelson Array Pathfinder)

Mobile Telescope Transport (TR116)

Ligon et al. 2022

S3

S4

The full Michelson Array would offer

12 total positions, creating 66 possible baselines.

1100m

600m

~17m

S3

S4

W5

current/new combiners

MIRX

MYSTIC

SILMARIL

SPICA

CHARIOT

PAVO

SPICA

VIS BEAMS

STS/STST

Lanthermann et al. 2022

SILMARIL

MIRCX

MIRC-X disperses light across several spectral channels and operates in the J and H-bands. MYSTIC operates in the  K-band. MIRC-X/MYSTIC can be used simultaneously to create images of stellar surfaces and circumstellar disks.  The precision closure phases are well suited to detecting faint binary companions.

Three spectral modes are currently available in the H-band: prism R=50 (8 spectral channels), prism R=102, and grism R=190. A higher resolution grism with R=1170 is available (with approval)

STS and STST

Anugu 2020

MYSTIC

MYSTIC, the Michigan Young STar Imager at CHARA is a K-band, cryogenic, 6-beam combiner. All-in-One 6T or high sensitivity 4T gravity chip

A 4-telescope mode for MYSTIC using an integrated optics component designed for the VLTI-GRAVITY experiment is under development and will provide better sensitivity for the faintest targets.

MYSTIC is available in the K-band using a low-resolution R=49 prism. Additional spectra modes (prism R=22, grism R=278, grism R=981, grism R=1724)

Setterholm et al. 2023

Pannetier et al. 2021

SPICA

(Stellar Parameters and Imaging with a Cophased Array)

SPICA-FT H-band 6-beam ABCD combiner by VLC Photonics, inspired by GRAVITY

low-resolution mode uses MIRC-X for fringe-tracking

The goal of the SPICA project is to provide a large and homogeneous set of stellar parameters across the HR-diagram. The survey aims to measure the angular diameters of 1000 stars.

Low-resolution spectrograph for measuring precise angular diameters (R=150, 50 channels over 650–950 nm).

For a sub-sample of bright stars, medium (R=4300) and high (R=13,200) spectral resolution modes will be available for spectral imaging of stellar surfaces and environments and kinematic studies.

spectrograph

CHARIOT

(CHARA Array Integrated Optics Testbed)

collaboration with Leibniz Institute for Astrophysics Potsdam (AIP)

ULI optics for JHK bands

(Siliprandi, Labadie, Madhav, Dinkelaker, Thompson, Benoît)

Currently have two injection stages, CRED1 arrives this year

Coupling ratio evolutions of (input coupling waveguide) and R2(λ) in blue diamonds of a writing beam combiner characterized by coupling input light in the two external PT1 and PT2 inputs to obtain two experimental measurements of the 3 dB asymmetric directional coupler (a, b) and one for each photometric asymmetric Tap directional couplers, as Tap 1 (c) and Tap 2 (d)

Siliprandi et al. 2022

science drivers

• multiple star systems
• time domain astronomy
• YSOs/planetary formation
• evolved stars
• starspots/surface imaging
• exozodis
• AGN
• HWO/PLATO
• exoplanet hosts

There are some 250 known exoplanets with host stars accessible to CHARA (Dec>-30 deg, V < 7). The new baselines will enable resolution of solar-like stars out to about 70pc in H-band. Numerical simulations of the transiting hot-Jupiter in HD189773 indicate that the shape of the silhouette of the planet can be measured in long baseline observations made during transits.

The Gaia orbits give the center-of-light motion of unresolved binaries, and a single resolved CHARA observation is sufficient to determine the full orbit and masses. High angular resolution observations also reveal how interacting stars are transformed by mass exchange.

NGC 4151

Early results from CHARA already show that the innermost dusty region in NGC 4151 is aligned perpendicularly to the jet axis.

• Explore the apparent variability of known exozodis
  • long-term monitoring
  • ​clues to source and formation of the dust
• ​Expand strong exozodi sample
  • ​leveraging LBTI and prior surveys​​
  • from ~100 \(\rightarrow\) ~1000 objects  
• Use spectral dispersion to resolve the thermal/scattered dilemma
• Risk mitigation for coronagraphy/starshade missions
• Target selection and characterization for mid/large missions (HWO, Plato, etc)
  • ​exozodis likely to be dominant noise source
• Precision diameters and fundamental astrophysics

following slides stolen from EXOPAG 23:

future plans

• Telescope dichroic replacement
• more automated alignment and tracking
• new/upgraded labAO system
• TEMA replacement
• new telescope drives, cylinder drives
• fibers to all telescopes (PM fused silica,          1550nm H-band 1st, 1350 nm – 1470 nm metrology)
• nuller "Achromatic photonic tricouplers for application in nulling interferometry" - Martinod et al. 2021
• W5/Channel 13 site (1100m)
  • 0.16 mas at H, 65 μas at R
• double-pass delay (90m tracking delay)

• Narcissus Mirror for SILMARIL

• The Michelson Array
• 2m central telescope?

• up to 300 nights over three years of open access time via (NOIRLab).

• Snapshot Imaging Mode to encourage new investigations. 

• Planewave:
  • 2-3 yrs until a 2 meter
  • $2.5 million ea
  • > 2 magnitudes deeper
  • move existing telescopes to CMAP sites?
    • 1m outriggers?
  • 6x2m + 4x1m array? 45 baselines!
• JWST plenary talk:
  • “imaging interferometers are coming online”
• How to get more hands at the Array/instrumentation interest
  • REU options
  • Shadow-a-Scientist programs
  • Collaborations/Partners
• Funding
  • NSF wants astronomers to compete for MSIPs with MSRI funds
  • Workshops on centers of excellence, partnerships with industry (TIP)
  • Could chara get solar panel funding?
  • Grow local and state politician interest/investment?

Some thoughts from AAS 241