The CHARA Array in 2040

Nic Scott

Telescope Systems Scientist

Horizons in Optical Long Baseline Interferometry

Jan 27th - 30th 2025 Meudon

Georgia State University, Atlanta
Director: Douglas Gies

CHARA Array
Mount Wilson Observatory, California
Director: Gail Schaefer
16 staff members onsite
Operations funded through the NSF, GSU, collaboration partners

Center for High Angular Resolution Astronomy

Not pictured yet: Heven, new operator

The CHARA Array in 2040?

but let's assume the best...

outline

The CHARA Array
- Array in 2010
- Array now
  - beam combiners
  - science highlights
  - current projects
- Array in 2040
  - future plans
  - science future goals
- Access and risks

the CHARA Array

The Array is capable of resolving details as small as 200 micro-arcseconds, equivalent to the angular size of a coin seen from a distance of 10,000 miles (16,000 km).

the CHARA Array

"the CHARA Array continues to offer exceptional opportunities for scientific discovery using the longest operating baselines in the world among optical/near-IR interferometers"

Eisenhauer et al 2023

CHARA Science meeting 2023 - Atlanta, GA

CHARA Science meeting 2024 - Tucson, AZ

Next meeting: April 28-30th Nice, France

CHARA timeline

1984 - "CHARA" established
1994 - NSF funding awarded
1996 - Mt. Wilson ground broken
1998 - Keck funding added
1999 - First fringes between S1/S2
2001 - First starlight fringes on longest baseline
2003 - Construction completed
2005 - First journal paper - dia. of Regulus (McAlister)
2007 - Image of surface of Altair (Monnier)
2010 - Open access program initiated
2025 - 272 paper published so far

" technical improvements in both hardware and software will continue indefinitely.

one rationale for the facility is to serve as a testbed for new developments in optical interferometry."

https://chara.gsu.edu/astronomers/journal-articles

2010		Band	Limits
TipTilt		R	10-11
Classic	2T	K	7.7-8.7
CLIMB	3T (commiss.)	K	6.5-8.1
FLUOR	2T	K	3-3.5
MIRC	4T	H	4.5
PAVO	2 or 3T	R	6-8.2
VEGA	4T	R	4-7.5

2024		Band	Limits typ (best)
AO		R	12-14
Classic	2T	K	8.5 (9.3)
MIRC-X/MYSTIC	6T	H/K	7.5 (8)
PAVO	2 or 3T	R	7
SPICA	6T	R	7-8
SILMARIL (com)	3T	HK	8.5 (9-12 expected)

2010 Science

Current Beam Combiners

CHARIOT - 2 beam, K-band IO testbed

Star spots

Evans et al. 2024, ApJ, 971, 190

Polaris

Roettenbacher et al., 2017, ApJ, 849, 120.

sigma Geminorum

Roettenbacher et al. 2016, Nature, 533, 217

zeta Andromedae

Recent Science -

Ashley Elliott 2024

Diameters of Stars

Angular Dia. + Parallax → Linear Radius
Diameter + Bolometric Flux → Teff
masses & ages from evolutionary tracks/isochrones
evolutionary models
color-magnitude relations
surface brightness relations
asteroseismic scaling relations

693 stars, σθ < 5%

Binary & Multiple Stars

Castor A and B

Torres et al. 2022

Ashley Elliott (LSU)

Resolved the inner binary components
Masses & 3D orbits
Mutual orientation of components

Imaging Luminous Stars

The cool hypergiant star RW Cep experienced a Great Dimming event in 2022:

Anugu et al. 2023

post-AGB star AC Her

Image credit: Dr Mark A. Garlick / markgarlick.com

If so, represents the first example of a polar circumbinary planet.

Anugu et al. 2023

Martin et al. 2023

Binary surrounded by large gas/dust disk
First 3D orbit for system
Cavity in the center not created by the tidal action of the central binary

Planet formed in disk would be relatively stable
Central cavity could be the result

H & K-band images asymmetric distribution, distorted shape
NIR spectroscopy: fading increased towards shorter wavelengths

→ implicates dust formation from stellar ejecta as explanation for the fading & unusual appearance.

Ibrahim et al. 2023

Disks Around Young Stars

T Tau type disks and other Young Stellar Objects (YSOs) are the birthplaces of planets.

Herbig Be star HD 190073

V1925 Aql

SU Aur

Labdon et al. 2023

YSO disk is viewed almost face-on (i<20°)
Clear view of the full extent of the inner gas disk.
Discovered bright spot in the disk that migrated by 27° over 32 days

Inclined & warped disk
Flux mainly from the far side of the disk
Near side partially obscures the central star
Dust emission indicates formation of a disk wind from the boundaries of the warped disk

NGC 4151

Active Galactic Nuclei

bright central region of the active galactic nucleus of the Seyfert galaxy NGC 4151.

Central structure resolved: 0.5 mas
Ring-like structure, i = 40°
Perpendicular to radio jet
K-band flux probably from dust sublimation region on the face of torus surrounding black hole

CMAP

(CHARA Michelson Array Pathfinder)

Ligon et al. 2022

Current CHARA

Projects

ALOHA – Univ. Limoges
Single-mode PM fibers
λ=810 nm, 240 m long
Laying on the ground
Connect S1+S2
On-sky fringes
Magri, J. et al., MNRAS, 536, 266 (2025)

CMAP
Single-mode PM fibers
λ=1.6 μm, 650 m long
Trench: 18 inches deep

Fibers to S1/S2/S3 laid

First lab fringes through CMAP fibers
New AO system software
STST integration - "offloading" DM corrections to beacon/M7/M10
New telescope drives and control software
New cylinder drives and control
"Minions" environmental sensing
Spycams - HD + audio

1100m

553m

~17m

Max spatial resolution

• 0.06 mas at R (650 nm)

• 0.16 mas at H (1.67 μm)

• 0.20 mas at K (2.13 μm)

17 to 1100m

36 possible baselines: array + CMAP [6+3]

Central 2m telescope
1m's → 2m's
Km+ baselines
AO/ople/lab upgrades
Off-target phase tracking
Nuller
Future beam transport
Michelson Array

(bigger future plans)

CHARA in 2040

Telescope dichroic upgrade
Automated alignment/tracking
Upgrade labAO system
Optimizing multi-wavelength simultaneous observations
Fibers to all telescopes
W5 site (1100m)
- extended/double-pass delay
Up to 300 nights over three years of open access time via NOIRLab.

(near future plans)

Known exoplanets from the NASA Exoplanet Archive. Over-plotted yellow rectangle region of planets that could be characterized with CHARA.

Dual-Star Phase Referencing at CHARA

Proven at VLTI already
expect gain ~ 6 magnitudes

Use MIRC-X + Mystic together
allows longer integration of science fringes ~ tens of mins

"Direct imaging of a hot Jupiter would require a new phase referencing mode of a nearby star."

Central 2m Telescope

Vacuum beam transport with fiber option
Bundled with Delay Line Upgrades

"A gain of one magnitude doubles the available sample of AGN."

7T Imaging improvements

AGN: dust sublimation and accretion disk could be resolved, binary black holes at the center?
High contrast/contact/interacting binaries - Outflow/ejection/dimming events, Be star circumstellar disks relations
Red giant ages
Star and planet formation: enabled by greater UV coverage, sensitivity, & longer baselines
Massive stars
Cool stars
HR diagram diameters: extended into late type stars
Solar System Science: Asteroids bright enough are too big for original Array,CMAP+Silmaril → break discrepancies between radar and reflectance measurements
Other mission support: HWO, JWST and ELT candidate finding and follow-up, Space mission technology testbeds?

"Priorities will include stellar system evolution: planetary formation and young stellar objects, imaging the sites of planet formation in the inner region of circumstellar disks, and measuring the contraction of pre-main sequence stars."

2040 CHARA Science Cases?

Taurus star forming region (d=140 pc)
Measure contraction of young stars to the main sequence.
Need < 0.2 mas to achieve this.

Angular Diameter of Pre-MS stars

Image an exoplanet during transit

There are some 250 known exoplanets with host stars accessible to CHARA.
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 silhouette of the planet can be measured in long baseline observations made during transits.

Verify diameter measurements between eclipsing binaries and singles
8% of M dwarfs are photometrically variable by 2% in V, R, I. 92% are stable
Study flares, spots
Magnetically active M dwarfs have very large spots that could be imaged

20pc sample → 600 M dwarfs

volume complete sample to 20pc
How many could chara resolve/image?

Diameters and resolved surfaces of M dwarfs

http://recons.org/published.annrev.pdf
https://aasnova.org/2018/07/11/3796/

The RECONS 25 Parsec Database

animation: Adric Riedel

https://www.youtube.com/embed/up_MqNBv0FE

Plan Outline:

Phase 0: AC at telescopes
Phase 0.1: new IR dichroics for beam samplers
- Improve multi-wavelength performance
- Wider bandwidth for better STST performance
  - CRED1, bluer for science, WFS on a single chip?
- Dual-star phase reference mode
Phase 0.5: upgrades of telAO
- Redesign M2, go to focal design?
Phase 1: central 2m + AO + OPLE upgrades
- LabWFS control new telDM,
- Longer delay + better metrology or double-decker carts
  - Visible-sensitivity, resolution, stability → needed for nulling
Phase 2: replace 1m's with 2m's
- Propagate upgrades from central 2m
Phase 3: full CMA - outer km baseline fiber array

(2024 Meeting on CHARA Future)

The full Michelson Array would offer 12 total positions, creating 66 possible baselines.

Review the current state of capabilities & techniques in optical/IR interferometry
Discuss quantum-enhanced methods for pushing current limitations on spatial resolution
Establish collaborations between the astronomy & quantum communities to address science requirements and technical challenges

Charting Quantum Horizons March 2024

"Performance of the Khabiboulline Configuration of Quantum Enhanced Long Baseline Optical Interferometry"- Mcclinton & Ridgeway (AAS 2025)

"Towards quantum-enhanced long-baseline optical/near-IR interferometry"

Rajagopal et al. (2024)

open-air or quantum-enhanced future beam transport?

NOIRLab Open access time

1000 ext applied?

2040

800 ext awarded?

300+ internal?

Total of 296 internal PI + CoI.

255 open access investigators awarded time
152 open access investigators applied but were not awarded time (potential untapped users).
Total ~ 700 investigators awarded or applied for time.

Risks:

very uncertain US environment

Funding options:

- NSF

- private: Heising-Simons Foundation, Keck, Kavli Instititute

- extend the consortium?

- other universities?

- National lab status?

- International partners?

Next generation of interferometrists:

the CHARA Array, VLTI, and other interferometers should continue to host educational workshops in the same vein as the VLTI and Michelson Schools.

Fire & climate change affects all facilities

backup slides

Meeting on CHARA Array future planning (2024)

Telescopes
- More/bigger apertures
  - <27% central obscuration, RC or Mersenne, f/2
- Planewave or AMOS
  - PW: 1-3 yrs until a 2m, ~$2.5 million ea, $100k for M4-6
  - questions on pupil stability and flexure of the PW scopes.
    - COTS hexapod might handle this (also option for current scopes)
- RC vs Mersenne
  - Easier for aligning telescope, acq setup easier, smaller DMs/optics, fiber injection or expand beam to inject into the light pipes
- Move existing telescopes to CMAP sites?
  - 1m outriggers? 6x2m + 4x1m array? 45 baselines!
  - need to expand OPLE....

OPLE
- Build up the 7th & 8th lines
  - Adapt STS/STST, metrology
  - "Stacked" upper level delay cart over the 7 & 8 line?
- Reduce lab vibrations
- Enable delay for fiber-fed telescope or open air too?
- Smaller delay optics? optimize for fiber?
- Upgrade opto-mechanical parts
- Carts go wireless
  - eliminate cable pulley/vibration issues.
- Test double pass cart scheme to allow more delay space for 1km+ baselines
- Use fixed open air delay to improve pop performance
- Extend existing rails to back of OPLE (through storage)?
  - new metrology system (current wouldn't reach beyond existing rail limit)

TELAO & TT
- New dichroic for better IR+vis simultaneous ops
- TELAO upgrade for visible wavelengths:
  - Keep the Andors but upgrade the lenslets and DMs
  - Benefits SPICA and science cases
- NIR TT tracking in the lab for red stars with a CRED1 camera
  - replace C-RED2 of STST
  - As we are targeting fainter stars, many science targets have V > 12
  - Having tip-tilt tracking in the near-infrared will allow us to access these targets, although without AO.
  - Beam stabilization in the lab is currently limited by CRED2 of STST.
- Silmaril/NIRO upgrade: include using NIRO for IR TT tracking
- Speed up/automate more on-sky alignment
  - Increase time on target

LabAO/STST
- Upgrade lab DM so we have a true "flat"
- Andor OCAM2: vis wfs camera in lab.
  - If sensitive enough camera, could correct off the star instead of blue beacon
  - Could use the same camera for multiple beams
- STST upgrade - cameras, beam sampler IR dichroic
  - Wider spectrum to STST
- Or eliminate labDM and just have fast TT in lab using starlight ....if you have better telDM
- Nuller in 5-6 yrs?
  - J or L-band
  - tri coupler (Tuthill/GLINT)
  - photonic lantern nuller (Xin 2024, JATIS)

MIRC-X/Mystic

MIRC-X

dispersed spectral channels
J and H-bands
MIRC-X/MYSTIC can be used simultaneously
images of stellar surfaces and circumstellar disks
precision closure phases
faint binary companions.

STS & STST

Anugu 2020

Setterholm et al. 2023

MYSTIC (the Michigan Young STar Imager at CHARA)

K-band, cryogenic, 6-beam combiner
All-in-One 6T or high sensitivity 4T gravity chip

Lanthermann et al. 2022

SILMARIL

Aug 2023 - First fringes

3T combiner (ten Brummelaar, Tuthill, Lanthermann)
Designed for high sensitivity and faint targets
CRED-1 in place

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. - measure the angular diameters of 1000 stars.