Future Prospects of Intensity Interferometry
from
Wednesday, October 30, 2024 (8:00 a.m.)
to
Friday, November 1, 2024 (5:00 p.m.)
Wednesday, October 30, 2024
8:30 a.m.
Registration
Registration
8:30 a.m. - 9:00 a.m.
9:00 a.m.
Opening Remarks
Opening Remarks
9:00 a.m. - 9:15 a.m.
Room: PI/4-405 - Bob Room
9:15 a.m.
Review of HBT
-
Robin Kaiser
(
Université Cote D'Azur
)
Review of HBT
Robin Kaiser
(
Université Cote D'Azur
)
9:15 a.m. - 10:15 a.m.
Room: PI/4-405 - Bob Room
10:15 a.m.
Break
Break
10:15 a.m. - 10:45 a.m.
Room: PI/1-119 - Atrium
10:45 a.m.
Intensity Interferometry with the H.E.S.S. telescopes
-
Naomi Vogel
(
ECAP, FAU Erlangen-Nürnberg
)
Intensity Interferometry with the H.E.S.S. telescopes
Naomi Vogel
(
ECAP, FAU Erlangen-Nürnberg
)
10:45 a.m. - 11:10 a.m.
Room: PI/4-405 - Bob Room
Intensity Interferometry (II) is a method that can achieve high angular resolution and was first employed in the 1960s by Robert Brown and Richard Q. Twiss (HBT). Since then, significant advancements have been made, particularly in the construction of telescopes with large light collection areas, such as Imaging Atmospheric Cherenkov Telescopes (IACTs), exemplified by instruments like H.E.S.S. , MAGIC and VERITAS. Our II setup was designed to be mounted on the lid of the Phase I H.E.S.S. telescopes in Namibia. In April 2022, our first observation campaign was conducted, during which two telescopes operated in a single wavelength band. In April-May 2023, a third telescope was added, and observations were performed in two colors simultaneously for the first time in II. In this contribution I will introduce our setup and compare the different configurations, as well as present the latest results of four southern hemisphere stars.
11:10 a.m.
Progress Toward Multi-Channel Intensity Interferometry with the Southern Connecticut Stellar Interferometer
-
Elliott Horch
(
Southern Connecticut State University
)
Progress Toward Multi-Channel Intensity Interferometry with the Southern Connecticut Stellar Interferometer
Elliott Horch
(
Southern Connecticut State University
)
11:10 a.m. - 11:35 a.m.
Room: PI/4-405 - Bob Room
The renaissance in stellar intensity interferometry has resulted in two main types of telescope arrays: those using large "light bucket" telescopes and photomultiplier tubes, such as CTA, VERITAS, MAGIC, and others, and those that instead use smaller, more traditional astronomical telescopes with high-grade optics, such as the systems at the Cote d'Azur and Asiago Observatories. To detect and timestamp photons, these latter systems have used single-photon avalanche diode (SPAD) detectors. This talk will focus on the latter type of instrument, which is also being pursued at Southern Connecticut State University. The current status of our instrument, the Southern Connecticut Stellar Interferometer (SCSI), will be reviewed, and prospects for improved sensitivity will be discussed. Principal among these is the use of SPAD arrays, which are increasingly available, to record different wavelengths simultaneously. If a sufficient number of channels can be employed, this type of intensity interferometer can reach much fainter magnitudes than currently possible. The talk will also briefly discuss work toward wireless intensity interferometry with SCSI, which will make larger baselines easier to set up and use, and ideas for quantum-assisted intensity interferometry that might be employed with SCSI in the future.
11:35 a.m.
Workshop Talk
-
David Kieda
(
The University of Utah
)
Workshop Talk
David Kieda
(
The University of Utah
)
11:35 a.m. - 12:00 p.m.
Room: PI/4-405 - Bob Room
12:00 p.m.
Lunch
Lunch
12:00 p.m. - 1:00 p.m.
Room: PI/2-251 - Upper Bistro
1:00 p.m.
The Multi Aperture Spectroscopic Telescope: Status and potential as an intensity interferometry facility
-
Sagi Ben Ami
(
Weizmann Institute of Science
)
The Multi Aperture Spectroscopic Telescope: Status and potential as an intensity interferometry facility
Sagi Ben Ami
(
Weizmann Institute of Science
)
1:00 p.m. - 1:25 p.m.
Room: PI/4-405 - Bob Room
The Multi-Aperture Spectroscopic Telescope is an array of 20x60cm prime-focus telescopes with single F/3 parabolic mirrors. The telescope array is being commissioned in the Negev Desert, with 10 telescopes expected to see first light by the end of the year. In the following talk, I will present the array, its various properties, including unique fiber coupling and imaging units, and its potential as an intensity interferometry facility.
1:25 p.m.
Intensity Interferometer Results on Sirius with 0.25 m Telescopes
-
Tom Mozdzen
(
Arizona State University
)
Intensity Interferometer Results on Sirius with 0.25 m Telescopes
Tom Mozdzen
(
Arizona State University
)
1:25 p.m. - 1:50 p.m.
Room: PI/4-405 - Bob Room
We present the design and initial results of a stellar intensity interferometer using small 0.25 m Newtonian-style telescopes in an urban backyard setting. The primary purpose of the interferometer is to measure the angular diameters of stars. Recent advances in low jitter time-tagging equipment and Single Photon Avalanche Detectors have made the detection of second-order correlation signals, necessary for Intensity Interferometry as demonstrated by Hanbury Brown and Twiss in 1956, feasible with small telescopes. Using Sirius as a target star, we observe a strong second-order correlation spike with an integrated signal to noise ratio (SNR) ∼7 after 13.55 h of integration over a three-night period using a 3.3 m baseline. The measured signal agrees with the theoretical estimates of both coherence time, 𝜏coh = 0.74 ± 0.26 ps and SNR. We discuss the future expansion of this technique with multiple wavelengths simultaneously via a prism grating and multiple detectors.
2:00 p.m.
Colloquium - Norm Murray
Colloquium - Norm Murray
2:00 p.m. - 3:00 p.m.
Room: PI/1-100 - Theatre
3:00 p.m.
Break
Break
3:00 p.m. - 3:30 p.m.
Room: PI/1-119 - Atrium
3:30 p.m.
Short Talks and Panel Discussion #1
-
Aaron Mueninghoff
(
Stony Brook University
)
Peng Kian Tan
(
Centre for Quantum Technologies, National University of Singapore
)
Federico Izraelevitch
(
University of San Martin and National Research Council of Argentina
)
Short Talks and Panel Discussion #1
Aaron Mueninghoff
(
Stony Brook University
)
Peng Kian Tan
(
Centre for Quantum Technologies, National University of Singapore
)
Federico Izraelevitch
(
University of San Martin and National Research Council of Argentina
)
3:30 p.m. - 4:30 p.m.
Room: PI/4-405 - Bob Room
Thursday, October 31, 2024
9:00 a.m.
Review of Photon Counters
-
Joshua Bienfang
(
National Institute of Standards and Technology
)
Karl Berggren
(
Massachusetts Institute of Technology
)
Review of Photon Counters
Joshua Bienfang
(
National Institute of Standards and Technology
)
Karl Berggren
(
Massachusetts Institute of Technology
)
9:00 a.m. - 10:15 a.m.
Room: PI/4-405 - Bob Room
10:15 a.m.
Break
Break
10:15 a.m. - 10:45 a.m.
Room: PI/1-119 - Atrium
10:45 a.m.
Workshop Talk
-
Verena Leopold
(
Quantum Optics and Quantum Information, FAU Erlangen
)
Workshop Talk
Verena Leopold
(
Quantum Optics and Quantum Information, FAU Erlangen
)
10:45 a.m. - 11:10 a.m.
Room: PI/4-405 - Bob Room
11:10 a.m.
Superconducting Nanowire Single Photon Detectors for Intensity Interferometry
-
Ioana Craiciu
(
Jet Propulsion Lab
)
Superconducting Nanowire Single Photon Detectors for Intensity Interferometry
Ioana Craiciu
(
Jet Propulsion Lab
)
11:10 a.m. - 11:35 a.m.
Room: PI/4-405 - Bob Room
Superconducting nanowire single photon detectors (SNSPDs) are of interest for intensity interferometry measurements because they have picosecond timing resolution. In addition, they work from the UV to mid-IR, with excellent eOiciency at visible and near-IR wavelengths, and are being fabricated into ever-larger detector arrays. On behalf of my colleagues in the JPL SNSPD group, I will present on the Deep Space Optical Communication (DSOC) demonstration, in which an SNSPD array was coupled to the 5 mHale telescope at Palomar, and received data at 267 Mbps from the Psyche spacecraft, the first optical communication between Earth and interplanetary space. The DSOC infrastructure at Palomar is suitable for intensity interferometry, as demonstrated by g(2) correlation (photon bunching) measurements of the stars Rigel and Procyon. I will also describe our current work on SNSPD array readout schemes, extending detector sensitivity into the mid-IR, and improving the system timing jitter of SNSPD arrays.
11:35 a.m.
Workshop Talk
-
Boris Korzh
(
Caltech
)
Workshop Talk
Boris Korzh
(
Caltech
)
11:35 a.m. - 12:00 p.m.
Room: PI/4-405 - Bob Room
12:00 p.m.
Lunch
Lunch
12:00 p.m. - 1:00 p.m.
Room: PI/2-251 - Upper Bistro
1:00 p.m.
Review of Astro
-
Charles Gammie
(
University of Illinois
)
Review of Astro
Charles Gammie
(
University of Illinois
)
1:00 p.m. - 2:00 p.m.
Room: PI/4-405 - Bob Room
2:00 p.m.
Workshop Talk
Workshop Talk
2:00 p.m. - 2:25 p.m.
Room: PI/4-405 - Bob Room
2:30 p.m.
Break
Break
2:30 p.m. - 3:00 p.m.
Room: PI/1-119 - Atrium
3:00 p.m.
Short Talks and Panel Discussion #2
-
Christopher Ingenhütt
(
ECAP, FAU Erlangen-Nürnberg
)
Sebastian Karl
(
QOQI, FAU Erlangen-Nürnberg
)
Roland Walter
(
University of Geneva
)
Short Talks and Panel Discussion #2
Christopher Ingenhütt
(
ECAP, FAU Erlangen-Nürnberg
)
Sebastian Karl
(
QOQI, FAU Erlangen-Nürnberg
)
Roland Walter
(
University of Geneva
)
3:00 p.m. - 4:00 p.m.
Room: PI/4-405 - Bob Room
4:00 p.m.
Social/Reception
Social/Reception
4:00 p.m. - 5:00 p.m.
Room: PI/2-251 - Upper Bistro
Friday, November 1, 2024
9:00 a.m.
Leveraging Intensity Interferometry Towards Understanding Massive Stars and Supernovae
-
Jared Goldberg
(
Flatiron Institute
)
Leveraging Intensity Interferometry Towards Understanding Massive Stars and Supernovae
Jared Goldberg
(
Flatiron Institute
)
9:00 a.m. - 9:25 a.m.
Room: PI/4-405 - Bob Room
9:25 a.m.
Supernova Morphology and Hubble Constant with Intensity Interferometer
-
I-Kai (Calvin) Chen
(
New York University
)
Supernova Morphology and Hubble Constant with Intensity Interferometer
I-Kai (Calvin) Chen
(
New York University
)
9:25 a.m. - 9:50 a.m.
Room: PI/4-405 - Bob Room
We demonstrate the ability to measure supernova morphology and distance using the P Cygni line profile with intensity interferometer.
9:50 a.m.
Workshop Talk
Workshop Talk
9:50 a.m. - 10:15 a.m.
Room: PI/4-405 - Bob Room
10:15 a.m.
Break
Break
10:15 a.m. - 10:45 a.m.
Room: PI/1-119 - Atrium
10:45 a.m.
Two-Photon Methods for Astrometric Gravitational Wave Detection
-
Paul Stankus
(
Brookhaven National Laboratory
)
Two-Photon Methods for Astrometric Gravitational Wave Detection
Paul Stankus
(
Brookhaven National Laboratory
)
10:45 a.m. - 11:10 a.m.
Room: PI/4-405 - Bob Room
With the observation of gravitational waves (GW's) at high, kilohertz frequencies by LIGO and the evidence for GW's at low, nanohertz frequencies from NANOGrav there is a new emphasis on exploring the GW landscape at intermediate frequency ranges. Beyond the two measurement methods used in these observations, i.e. laser metrology in LIGO and pulsar timing offsets in NANOGrav, we have been developing a third approach of observing astrometric GW signatures, which is very well suited to the intermediate microhertz frequency range. While astrometric GW observations have been discussed in the context of survey missions, e.g. GAIA, this presentation will exhibit a potentially superior approach using long baseline two-photon interferometry, with both space-based and ground-based platforms. The practicalities of a near-future experiment will be particularly highlighted
11:10 a.m.
Workshop Talk
-
Marios Galanis
(
Perimeter Institute
)
Workshop Talk
Marios Galanis
(
Perimeter Institute
)
11:10 a.m. - 11:35 a.m.
Room: PI/4-405 - Bob Room
11:35 a.m.
Workshop Talk
-
Michael Rubel
Workshop Talk
Michael Rubel
11:35 a.m. - 12:00 p.m.
Room: PI/4-405 - Bob Room
12:00 p.m.
Lunch
Lunch
12:00 p.m. - 1:00 p.m.
Room: PI/2-251 - Upper Bistro
1:00 p.m.
Bayesian Imaging for Intensity Interferometry with Deep Generative Priors
-
Biwei Dai
(
University of California, Berkeley
)
Bayesian Imaging for Intensity Interferometry with Deep Generative Priors
Biwei Dai
(
University of California, Berkeley
)
1:00 p.m. - 1:25 p.m.
Room: PI/4-405 - Bob Room
1:25 p.m.
Image Reconstruction From Intensity Interferometry
-
Albert Stebbins
(
Fermi National Accelerator Laboratory
)
Image Reconstruction From Intensity Interferometry
Albert Stebbins
(
Fermi National Accelerator Laboratory
)
1:25 p.m. - 1:50 p.m.
Room: PI/4-405 - Bob Room
Even with dense sampling of the uv plane intensity correlations only contain half the information required to reconstruct an image. Intensity correlations do contain the full information of the image power spectrum and therefore of the image 2-point correlation function. With some practice one can gain intuitive understanding in interpreting 2-point correlation function "images". This is illustrated with both toy examples and modeling of real astronomical images. In some assumptions one can even interpret these 2-point correlation function "images" with only a few baselines.
1:50 p.m.
Generative AI for Image Reconstruction: A First Attempt
-
Prasenjit Saha
(
University of Zurich
)
Generative AI for Image Reconstruction: A First Attempt
Prasenjit Saha
(
University of Zurich
)
1:50 p.m. - 2:15 p.m.
Room: PI/4-405 - Bob Room
In modern astronomy, artificial intelligence (AI) is increasingly utilized to analyze large volumes of data, significantly reducing the need for human computational resources and time. Machine learning (ML) techniques are at the forefront of revealing astronomical mysteries by analyzing observed data. Here, we will introduce the application of machine learning to Intensity Interferometry (II) data for high-resolution optical astronomy, aiming to overcome the limitations of traditional image reconstruction methods. In this presentation, we demonstrate successful image reconstruction of a fast-rotating star using conditional Generative Adversarial Networks (cGANs), a supervised machine learning approach. Simulations of II are based on an assembly of four telescopes similar to existing arrays. However, the sensitivity of the signal and high resolution are expected to improve with additional baselines. It makes the current and future Cherenkov Telescope Array Observatory (CTAO) an ideal candidate for II applications. Our approach is highly relevant and innovative, addressing key challenges in phase reconstruction and proposing novel solutions that could revolutionize high-resolution imaging in astronomy.
2:15 p.m.
Break
Break
2:15 p.m. - 2:45 p.m.
Room: PI/1-119 - Atrium
2:45 p.m.
Short Talks and Panel Discussion #3
-
Lifan Wang
(
Texas A&M University
)
Chad Bender
(
University of Arizona
)
Short Talks and Panel Discussion #3
Lifan Wang
(
Texas A&M University
)
Chad Bender
(
University of Arizona
)
2:45 p.m. - 3:30 p.m.
Room: PI/4-405 - Bob Room
3:30 p.m.
Closing Remarks
-
Phil Mauskopf
(
Arizona State Universtiy
)
Closing Remarks
Phil Mauskopf
(
Arizona State Universtiy
)
3:30 p.m. - 4:00 p.m.
Room: PI/4-405 - Bob Room
4:00 p.m.
Friday Social
Friday Social
4:00 p.m. - 5:00 p.m.
Room: PI/1-124 - Lower Bistro