Network Configurations for Astrophysical Observatories
Explore the intricate relationship between frequencies, sensitivities, and network configurations in astrophysical observatories through insightful diagrams and explanations. Gain valuable insights into the optimal setup for detecting phenomena such as black holes, neutron stars, continuous waves, and more.
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Presentation Transcript
Frequencies-Sensitivities Low vs High Salvo s and Stefan s personal views subject to updates MIT, Glasgow
Color code Blue: concerning black holes Magenta: concerning neutron stars Green: concerning CWs Yellow: concerning stochastic. Orange: bursts Dashed: the unexpected Some boxes are red and blue meaning that any combination of NS and/or BH is relevant. 3/18/2025 S.Vitale & S.Hild 2
Caveats This plot should be taken as an indication of what science topics rely on which frequency and the number of detectors It is not meant to be rigorous (at least in this version) It s something I put together to show clearly how the answer to what s the optimal network configuration strongly depends on the scientific question one is trying to answer I will try to keep this to date and improve it with suggestions I receive You are welcome to use this diagram, just please kindly credit it 3/18/2025 S.Vitale & S.Hild 3
More detectors The unexpected Early- warning localization CW Axions from 30M BH remnant Sky localization BNS Stochastic Tests of General relativity Source-frame masses IMBH or high-z BBH Distance/ Cosmology Inclination/ EM modeling NS post-merger Supernovae and other unmodeled transients Continuous waves Memory Aligned BH spins Precessing BH spins Eccentricity mass ratio NS Equation of state Ringdown S. Vitale, 2019 Better high-frequency Better bucket Better low-frequency 3/18/2025 S.Vitale & S.Hild 4
Caveats This plot should be taken as an indication of which technologies will enable which frequency sensitivity It is not meant to be rigorous The vertical axis is very indicative. Other dimensions to be considered are: Technical readiness, Risk etc 3/18/2025 S.Vitale & S.Hild 5
Observatory aspects and noises Complexity, Gain Underground facility to reduce atmospheric and seismic Newtonian noise Longer facilities Xylophone High powered, silicon interferometer Cryogenic test masses and suspensions Longer wavelength HF quantum noise configs Better coatings Larger + heavier testmasses Bigger Lasers, better TCS, better mirrors (optical) Newtonian subtraction Better squeezing Better high-frequency Better bucket S.Vitale & S.Hild Better low-frequency 3/18/2025 6
Observatory aspects and noises Complexity, Gain Underground facility to reduce atmospheric and seismic Newtonian noise Myriad of control noises, mystery noises and Scattering Longer facilities Xylophone High power commissioning is tough and takes time High powered, silicon interferometer Cryogenic test masses and suspensions Longer wavelength HF quantum noise configs Better coatings Larger + heavier testmasses Bigger Lasers, better TCS, better mirrors (optical) Newtonian subtraction Better squeezing Better high-frequency Better bucket S.Vitale & S.Hild Better low-frequency 3/18/2025 7
Some Questions to Muse about Broadband detectors vs specialised detectors covering only part of the frequency range? Static vs tunable detectors? What low frequency cut off to target at? N. De Lillo ET-D with different low frequency cut-offs (Equal Mass No Spinning CBC in Plank2015 Cosmology) 3/18/2025 S.Vitale & S.Hild 8
