Continuous Ultraviolet to Blue-Green Astrocomb
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arXiv
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| Auteurs principaux: | , , , , , , , , |
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| Format: | Preprint |
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2023
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| _version_ | 1866916144147857408 |
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| author | Cheng, Yuk Shan Dadi, Kamalesh Mitchell, Toby Thompson, Samantha Piskunov, Nikolai Wright, Lewis D. Gawith, Corin B. E. McCracken, Richard A. Reid, Derryck T. |
| author_facet | Cheng, Yuk Shan Dadi, Kamalesh Mitchell, Toby Thompson, Samantha Piskunov, Nikolai Wright, Lewis D. Gawith, Corin B. E. McCracken, Richard A. Reid, Derryck T. |
| contents | The characterization of Earth-like exoplanets and precision tests of cosmological models using next-generation telescopes such as the ELT will demand precise calibration of astrophysical spectrographs in the visible region, where stellar absorption lines are most abundant. Astrocombs--lasers providing a broadband sequence of ultra-narrow, drift-free, regularly spaced optical frequencies on a multi-GHz grid--promise an atomically-traceable, versatile calibration scale, but their realization is challenging because of the need for ultra-broadband frequency conversion of mode-locked infrared lasers into the blue-green region. Here, we introduce a new concept achieving a broad, continuous spectrum by combining second-harmonic generation and sum-frequency-mixing in an aperiodically-poled MgO:PPLN waveguide to generate gap-free 390-520 nm light from a 1 GHz Ti:sapphire laser frequency comb. We lock a low-dispersion Fabry-Perot etalon to extract a sub-comb of bandwidth from 392-472 nm with a spacing of 30 GHz, visualizing the thousands of resulting comb modes on a high resolution cross-dispersion spectrograph. Complementary experimental data and simulations demonstrate the effectiveness of the approach for eliminating the spectral gaps present in second-harmonic-only conversion, in which weaker fundamental frequencies are suppressed by the quadratic \{chi}^((2)) nonlinearity. Requiring only ~100 pJ pulse energies, our concept establishes a practical new route to broadband UV-visible generation at GHz repetition rates. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2306_13533 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Continuous Ultraviolet to Blue-Green Astrocomb Cheng, Yuk Shan Dadi, Kamalesh Mitchell, Toby Thompson, Samantha Piskunov, Nikolai Wright, Lewis D. Gawith, Corin B. E. McCracken, Richard A. Reid, Derryck T. Optics Instrumentation and Methods for Astrophysics The characterization of Earth-like exoplanets and precision tests of cosmological models using next-generation telescopes such as the ELT will demand precise calibration of astrophysical spectrographs in the visible region, where stellar absorption lines are most abundant. Astrocombs--lasers providing a broadband sequence of ultra-narrow, drift-free, regularly spaced optical frequencies on a multi-GHz grid--promise an atomically-traceable, versatile calibration scale, but their realization is challenging because of the need for ultra-broadband frequency conversion of mode-locked infrared lasers into the blue-green region. Here, we introduce a new concept achieving a broad, continuous spectrum by combining second-harmonic generation and sum-frequency-mixing in an aperiodically-poled MgO:PPLN waveguide to generate gap-free 390-520 nm light from a 1 GHz Ti:sapphire laser frequency comb. We lock a low-dispersion Fabry-Perot etalon to extract a sub-comb of bandwidth from 392-472 nm with a spacing of 30 GHz, visualizing the thousands of resulting comb modes on a high resolution cross-dispersion spectrograph. Complementary experimental data and simulations demonstrate the effectiveness of the approach for eliminating the spectral gaps present in second-harmonic-only conversion, in which weaker fundamental frequencies are suppressed by the quadratic \{chi}^((2)) nonlinearity. Requiring only ~100 pJ pulse energies, our concept establishes a practical new route to broadband UV-visible generation at GHz repetition rates. |
| title | Continuous Ultraviolet to Blue-Green Astrocomb |
| topic | Optics Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2306.13533 |