The Askaryan Radio Array (ARA) is an in-ice ultrahigh energy (UHE) neutrino experiment at the South Pole. ARA aims to detect the radio emissions from neutrino-induced particle showers using in-ice clusters of antennas buried ${sim}200$ m deep on a roughly cubical lattice with side length of ${sim}10$ m. ARA has five such independent stations which have collectively accumulated ${sim}30$ station-years of livetime through 2023. The fifth station of ARA has an additional sub-detector, known as the phased array, which pioneered an interferometric trigger constructed by beamforming the signals of $7$ tightly packed, vertically-polarized antennas. This scheme has been demonstrated to significantly improve the trigger efficiency for low SNR signals. In this talk, we will present the current state of the first array-wide diffuse neutrino search using $24$ station-years of data (through 2021). We anticipate that this analysis will result in the first UHE neutrino observation or world-leading limits from a radio neutrino detector below $100$ EeV. Additionally, this analysis will demonstrate the feasibility for multi-station in-ice radio arrays to successfully conduct an array-wide neutrino search -- paving the way for future, large detector arrays such as RNO-G and IceCube-Gen2 Radio.
{"title":"Progress towards an array-wide diffuse UHE neutrino search with the Askaryan Radio Array","authors":"Marco Stein Muziofor the ARA Collaboration","doi":"arxiv-2409.03854","DOIUrl":"https://doi.org/arxiv-2409.03854","url":null,"abstract":"The Askaryan Radio Array (ARA) is an in-ice ultrahigh energy (UHE) neutrino\u0000experiment at the South Pole. ARA aims to detect the radio emissions from\u0000neutrino-induced particle showers using in-ice clusters of antennas buried\u0000${sim}200$ m deep on a roughly cubical lattice with side length of ${sim}10$\u0000m. ARA has five such independent stations which have collectively accumulated\u0000${sim}30$ station-years of livetime through 2023. The fifth station of ARA has\u0000an additional sub-detector, known as the phased array, which pioneered an\u0000interferometric trigger constructed by beamforming the signals of $7$ tightly\u0000packed, vertically-polarized antennas. This scheme has been demonstrated to\u0000significantly improve the trigger efficiency for low SNR signals. In this talk,\u0000we will present the current state of the first array-wide diffuse neutrino\u0000search using $24$ station-years of data (through 2021). We anticipate that this\u0000analysis will result in the first UHE neutrino observation or world-leading\u0000limits from a radio neutrino detector below $100$ EeV. Additionally, this\u0000analysis will demonstrate the feasibility for multi-station in-ice radio arrays\u0000to successfully conduct an array-wide neutrino search -- paving the way for\u0000future, large detector arrays such as RNO-G and IceCube-Gen2 Radio.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217491","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Manon Lallement, Sylvestre Lacour, Elsa Huby, Guillermo Martin, Kevin Barjot, Guy Perrin, Daniel Rouan, Vincent Lapeyrere, Sebastien Vievard, Olivier Guyon, Julien Lozi, Vincent Deo, Takayuki Kotani, Cecil Pham, Cedric Cassagnettes, Adrien Billat, Nick Cvetojevic, Franck Marchis
Integrated optics are used to achieve astronomical interferometry inside robust and compact materials, improving the instruments stability and sensitivity. In order to perform differential phase measurements at the H$alpha$ line (656.3 nm) with the 600-800 nm spectro-interferometer FIRST, a photonic integrated circuit (PIC) is being developed. This PIC performs the visible combination of the beams coming from the telescope pupil sub-apertures. In this work, TEEM Photonics waveguides fabricated by $K_+:Na_+$ ion exchange in glass are characterized in terms of single-mode range and mode field diameter. The waveguide diffused index profile is modeled on Beamprop software. FIRST beam combiner building blocks are simulated, especially achromatic directional couplers and passive $pi/2$ phase shifters for a potential ABCD interferometric combination.
{"title":"Photonic chip for visible interferometry: laboratory characterization and comparison with the theoretical model","authors":"Manon Lallement, Sylvestre Lacour, Elsa Huby, Guillermo Martin, Kevin Barjot, Guy Perrin, Daniel Rouan, Vincent Lapeyrere, Sebastien Vievard, Olivier Guyon, Julien Lozi, Vincent Deo, Takayuki Kotani, Cecil Pham, Cedric Cassagnettes, Adrien Billat, Nick Cvetojevic, Franck Marchis","doi":"arxiv-2409.03808","DOIUrl":"https://doi.org/arxiv-2409.03808","url":null,"abstract":"Integrated optics are used to achieve astronomical interferometry inside\u0000robust and compact materials, improving the instruments stability and\u0000sensitivity. In order to perform differential phase measurements at the\u0000H$alpha$ line (656.3 nm) with the 600-800 nm spectro-interferometer FIRST, a\u0000photonic integrated circuit (PIC) is being developed. This PIC performs the\u0000visible combination of the beams coming from the telescope pupil sub-apertures.\u0000In this work, TEEM Photonics waveguides fabricated by $K_+:Na_+$ ion exchange\u0000in glass are characterized in terms of single-mode range and mode field\u0000diameter. The waveguide diffused index profile is modeled on Beamprop software.\u0000FIRST beam combiner building blocks are simulated, especially achromatic\u0000directional couplers and passive $pi/2$ phase shifters for a potential ABCD\u0000interferometric combination.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217492","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Manon Lallement, Elsa Huby, Sylvestre Lacour, Guillermo Martin, Kevin Barjot, Guy Perrin, Daniel Rouan, Vincent Lapeyrere, Sebastien Vievard, Olivier Guyon, Julien Lozi, Vincent Deo, Takayuki Kotani, Cecil Pham, Cedric Cassagnettes, Adrien Billat, Nick Cvetojevic, Franck Marchis
Integrated optics are used to achieve astronomical interferometry inside robust and compact materials, improving the instrument's stability and sensitivity. In order to perform differential phase measurements at the H$alpha$ line (656.3 nm) with the 600-800 nm spectro-interferometer FIRST, a photonic integrated circuit (PIC) is being developed in collaboration with TEEM Photonics. This PIC performs the interferometric combination of the beams coming from sub-apertures selected in the telescope pupil, thus implementing the pupil remapping technique to restore the diffraction limit of the telescope. In this work, we report on the latest developments carried out within the FIRST project to produce a high performance visible PIC. The PICs are manufactured by TEEM Photonics, using their technology based on $K_+:Na_+$ ion exchange in glass. The first part of the study consists in the experimental characterization of the fundamental properties of the waveguides, in order to build an accurate model, which is the basis for the design of more complex functions. In the second part, theoretical designs and their optimization for three types of combiner architectures are presented: symmetric directional coupler, asymmetric directional couplers and ABCD cells including achromatic phase shifters.
{"title":"Photonic beam-combiner for visible interferometry with SCExAO/FIRST: laboratory characterization and design optimization","authors":"Manon Lallement, Elsa Huby, Sylvestre Lacour, Guillermo Martin, Kevin Barjot, Guy Perrin, Daniel Rouan, Vincent Lapeyrere, Sebastien Vievard, Olivier Guyon, Julien Lozi, Vincent Deo, Takayuki Kotani, Cecil Pham, Cedric Cassagnettes, Adrien Billat, Nick Cvetojevic, Franck Marchis","doi":"arxiv-2409.03476","DOIUrl":"https://doi.org/arxiv-2409.03476","url":null,"abstract":"Integrated optics are used to achieve astronomical interferometry inside\u0000robust and compact materials, improving the instrument's stability and\u0000sensitivity. In order to perform differential phase measurements at the\u0000H$alpha$ line (656.3 nm) with the 600-800 nm spectro-interferometer FIRST, a\u0000photonic integrated circuit (PIC) is being developed in collaboration with TEEM\u0000Photonics. This PIC performs the interferometric combination of the beams\u0000coming from sub-apertures selected in the telescope pupil, thus implementing\u0000the pupil remapping technique to restore the diffraction limit of the\u0000telescope. In this work, we report on the latest developments carried out\u0000within the FIRST project to produce a high performance visible PIC. The PICs\u0000are manufactured by TEEM Photonics, using their technology based on $K_+:Na_+$\u0000ion exchange in glass. The first part of the study consists in the experimental\u0000characterization of the fundamental properties of the waveguides, in order to\u0000build an accurate model, which is the basis for the design of more complex\u0000functions. In the second part, theoretical designs and their optimization for\u0000three types of combiner architectures are presented: symmetric directional\u0000coupler, asymmetric directional couplers and ABCD cells including achromatic\u0000phase shifters.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217497","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
B. Buralli, M. N'Diaye, R. Pourcelot, M. Carbillet, E. H. Por, I. Laginja, L. Canas, S. Steiger, P. Petrone, M. M. Nguyen, B. Nickson, S. F. Redmond, A. Sahoo, L. Pueyo, M. D. Perrin, R. Soummer
We study a mid-order wavefront sensor (MOWFS) to address fine cophasing errors in exoplanet imaging with future large segmented aperture space telescopes. Observing Earth analogs around Sun-like stars requires contrasts down to $10^{-10}$ in visible light. One promising solution consists of producing a high-contrast dark zone in the image of an observed star. In a space observatory, this dark region will be altered by several effects, and among them, the small misalignments of the telescope mirror segments due to fine thermo-mechanical drifts. To correct for these errors in real time, we investigate a wavefront control loop based on a MOWFS with a Zernike sensor. Such a MOWFS was installed on the high-contrast imager for complex aperture telescopes (HiCAT) testbed in Baltimore in June 2023. The bench uses a 37-segment Iris-AO deformable mirror to mimic telescope segmentation and some wavefront control strategies to produce a dark zone with such an aperture. In this contribution, we first use the MOWFS to characterize the Iris-AO segment discretization steps. For the central segment, we find a minimal step of 125,$pm$31,pm. This result will help us to assess the contribution of the Iris-AO DM on the contrast in HiCAT. We then determine the detection limits of the MOWFS, estimating wavefront error amplitudes of 119 and 102,pm for 10,s and 1,min exposure time with a SNR of 3. These values inform us about the measurement capabilities of our wavefront sensor on the testbed. These preliminary results will be useful to provide insights on metrology and stability for exo-Earth observations with the Habitable Worlds Observatory.
{"title":"Mid-order wavefront control for exoplanet imaging: preliminary characterization of the segmented deformable mirror and Zernike wavefront sensor on HiCAT","authors":"B. Buralli, M. N'Diaye, R. Pourcelot, M. Carbillet, E. H. Por, I. Laginja, L. Canas, S. Steiger, P. Petrone, M. M. Nguyen, B. Nickson, S. F. Redmond, A. Sahoo, L. Pueyo, M. D. Perrin, R. Soummer","doi":"arxiv-2409.03411","DOIUrl":"https://doi.org/arxiv-2409.03411","url":null,"abstract":"We study a mid-order wavefront sensor (MOWFS) to address fine cophasing\u0000errors in exoplanet imaging with future large segmented aperture space\u0000telescopes. Observing Earth analogs around Sun-like stars requires contrasts\u0000down to $10^{-10}$ in visible light. One promising solution consists of\u0000producing a high-contrast dark zone in the image of an observed star. In a\u0000space observatory, this dark region will be altered by several effects, and\u0000among them, the small misalignments of the telescope mirror segments due to\u0000fine thermo-mechanical drifts. To correct for these errors in real time, we\u0000investigate a wavefront control loop based on a MOWFS with a Zernike sensor.\u0000Such a MOWFS was installed on the high-contrast imager for complex aperture\u0000telescopes (HiCAT) testbed in Baltimore in June 2023. The bench uses a\u000037-segment Iris-AO deformable mirror to mimic telescope segmentation and some\u0000wavefront control strategies to produce a dark zone with such an aperture. In\u0000this contribution, we first use the MOWFS to characterize the Iris-AO segment\u0000discretization steps. For the central segment, we find a minimal step of\u0000125,$pm$31,pm. This result will help us to assess the contribution of the\u0000Iris-AO DM on the contrast in HiCAT. We then determine the detection limits of\u0000the MOWFS, estimating wavefront error amplitudes of 119 and 102,pm for 10,s\u0000and 1,min exposure time with a SNR of 3. These values inform us about the\u0000measurement capabilities of our wavefront sensor on the testbed. These\u0000preliminary results will be useful to provide insights on metrology and\u0000stability for exo-Earth observations with the Habitable Worlds Observatory.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217499","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Emma V. Turtelboom, Jamie Dietrich, Courtney D. Dressing, Caleb K. Harada
Multi-planet system architectures are frequently used to constrain possible formation and evolutionary pathways of observed exoplanets. Therefore, understanding the predictive and descriptive power of empirical models of these systems is critical to understanding their formation histories. Additionally, if empirical models can reproduce architectures over a range of scales, transit and radial velocity observations can be more easily and effectively used to inform future microlensing, astrometric, and direct imaging surveys. We analyze 52 TESS multi-planet systems previously studied using Dynamite (Dietrich & Apai 2020), who used TESS data alongside empirical models based on Kepler planets to predict additional planets in each system. We analyze additional TESS data to search for these predicted planets. We thereby evaluate the degree to which these models can be used to predict planets in TESS multi-planet systems. Specifically, we study whether a period ratio method or clustered period model is more predictive. We find that the period ratio model predictions are most consistent with the planets discovered since 2020, accounting for detection sensitivity. However, neither model is highly predictive, highlighting the need for additional data and nuanced models to describe the full population. Improved eccentricity and dynamical stability prescriptions incorporated into Dynamite provide a modest improvement in the prediction accuracy. We also find that the current sample of 183 TESS multi-planet systems are are highly dynamically packed, and appear truncated relative to detection biases. These attributes are consistent with the Kepler sample, and suggest a highly efficient formation process.
{"title":"Searching for Additional Planets in TESS Multi-Planet Systems: Testing Empirical Models Based on Kepler Data","authors":"Emma V. Turtelboom, Jamie Dietrich, Courtney D. Dressing, Caleb K. Harada","doi":"arxiv-2409.03852","DOIUrl":"https://doi.org/arxiv-2409.03852","url":null,"abstract":"Multi-planet system architectures are frequently used to constrain possible\u0000formation and evolutionary pathways of observed exoplanets. Therefore,\u0000understanding the predictive and descriptive power of empirical models of these\u0000systems is critical to understanding their formation histories. Additionally,\u0000if empirical models can reproduce architectures over a range of scales, transit\u0000and radial velocity observations can be more easily and effectively used to\u0000inform future microlensing, astrometric, and direct imaging surveys. We analyze\u000052 TESS multi-planet systems previously studied using Dynamite (Dietrich & Apai\u00002020), who used TESS data alongside empirical models based on Kepler planets to\u0000predict additional planets in each system. We analyze additional TESS data to\u0000search for these predicted planets. We thereby evaluate the degree to which\u0000these models can be used to predict planets in TESS multi-planet systems.\u0000Specifically, we study whether a period ratio method or clustered period model\u0000is more predictive. We find that the period ratio model predictions are most\u0000consistent with the planets discovered since 2020, accounting for detection\u0000sensitivity. However, neither model is highly predictive, highlighting the need\u0000for additional data and nuanced models to describe the full population.\u0000Improved eccentricity and dynamical stability prescriptions incorporated into\u0000Dynamite provide a modest improvement in the prediction accuracy. We also find\u0000that the current sample of 183 TESS multi-planet systems are are highly\u0000dynamically packed, and appear truncated relative to detection biases. These\u0000attributes are consistent with the Kepler sample, and suggest a highly\u0000efficient formation process.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"75 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217495","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Jean Le Graët, Aurélia Secroun, Marie Tourneur-Silvain, Éric Kajfasz, Jean-Luc Atteia, Olivier Boulade, Alix Nouvel de la Flèche, Hervé Geoffray, William Gillard, Stéphanie Escoffier, Francis Fortin, Nicolas Fourmanoit, Smaïn Kermiche, Hervé Valentin, Julien Zoubian
With the expanding integration of infrared instruments in astronomical missions, accurate per-pixel flux estimation for near-infrared hybrid detectors has become critical to the success of these missions. Based on CPPM's involvement in both SVOM/Colibri and Euclid missions, this study introduces universally applicable methods and framework for characterizing IR hybrid detectors and decorrelating their intrinsic properties. The characterization framework, applied to the ALFA detector and Euclid's H2RG, not only validates the proposed methods but also points out subtle behaviors inherent to each detector.
{"title":"Toward a universal characterization methodology for conversion gain measurement of CMOS APS: application to Euclid and SVOM","authors":"Jean Le Graët, Aurélia Secroun, Marie Tourneur-Silvain, Éric Kajfasz, Jean-Luc Atteia, Olivier Boulade, Alix Nouvel de la Flèche, Hervé Geoffray, William Gillard, Stéphanie Escoffier, Francis Fortin, Nicolas Fourmanoit, Smaïn Kermiche, Hervé Valentin, Julien Zoubian","doi":"arxiv-2409.03374","DOIUrl":"https://doi.org/arxiv-2409.03374","url":null,"abstract":"With the expanding integration of infrared instruments in astronomical\u0000missions, accurate per-pixel flux estimation for near-infrared hybrid detectors\u0000has become critical to the success of these missions. Based on CPPM's\u0000involvement in both SVOM/Colibri and Euclid missions, this study introduces\u0000universally applicable methods and framework for characterizing IR hybrid\u0000detectors and decorrelating their intrinsic properties. The characterization\u0000framework, applied to the ALFA detector and Euclid's H2RG, not only validates\u0000the proposed methods but also points out subtle behaviors inherent to each\u0000detector.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217500","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
N. Godoy, E. Choquet, L. Altinier, A. Lau, R. Mayer, A. Vigan, D. Mary
In this study, we explored the fundamental contrast limit of NIRCam coronagraphy observations, representing the achievable performance with post-processing techniques. This limit is influenced by photon noise and readout noise, with complex noise propagation through post-processing methods like principal component analysis. We employed two approaches: developing a formula based on simplified scenarios and using Markov Chain Monte Carlo (MCMC) methods, assuming Gaussian noise properties and uncorrelated pixel noise. Tested on datasets HIP,65426, AF,Lep, and HD,114174, the MCMC method provided accurate but computationally intensive estimates. The analytical approach offered quick, reliable estimates closely matching MCMC results in simpler scenarios. Our findings showed the fundamental contrast curve is significantly deeper than the current achievable contrast limit obtained with post-processing techniques at shorter separations, being 10 times deeper at $0.5''$ and 4 times deeper at $1''$. At greater separations, increased exposure time improves sensitivity, with the transition between photon and readout noise dominance occurring between $2''$ and $3''$. We conclude the analytical approach is a reliable estimate of the fundamental contrast limit, offering a faster alternative to MCMC. These results emphasize the potential for greater sensitivity at shorter separations, highlighting the need for improved or new post-processing techniques to enhance JWST NIRCam sensitivity or contrast curve.
{"title":"ESCAPE project: fundamental detection limits of JWST/NIRCam coronographic observations","authors":"N. Godoy, E. Choquet, L. Altinier, A. Lau, R. Mayer, A. Vigan, D. Mary","doi":"arxiv-2409.03485","DOIUrl":"https://doi.org/arxiv-2409.03485","url":null,"abstract":"In this study, we explored the fundamental contrast limit of NIRCam\u0000coronagraphy observations, representing the achievable performance with\u0000post-processing techniques. This limit is influenced by photon noise and\u0000readout noise, with complex noise propagation through post-processing methods\u0000like principal component analysis. We employed two approaches: developing a\u0000formula based on simplified scenarios and using Markov Chain Monte Carlo (MCMC)\u0000methods, assuming Gaussian noise properties and uncorrelated pixel noise.\u0000Tested on datasets HIP,65426, AF,Lep, and HD,114174, the MCMC method\u0000provided accurate but computationally intensive estimates. The analytical\u0000approach offered quick, reliable estimates closely matching MCMC results in\u0000simpler scenarios. Our findings showed the fundamental contrast curve is\u0000significantly deeper than the current achievable contrast limit obtained with\u0000post-processing techniques at shorter separations, being 10 times deeper at\u0000$0.5''$ and 4 times deeper at $1''$. At greater separations, increased exposure\u0000time improves sensitivity, with the transition between photon and readout noise\u0000dominance occurring between $2''$ and $3''$. We conclude the analytical\u0000approach is a reliable estimate of the fundamental contrast limit, offering a\u0000faster alternative to MCMC. These results emphasize the potential for greater\u0000sensitivity at shorter separations, highlighting the need for improved or new\u0000post-processing techniques to enhance JWST NIRCam sensitivity or contrast\u0000curve.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217521","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Ansgar Reiners, Michael Debus, Sebastian Schäfer, Eberhard Tiemann, Mathias Zechmeister
Astronomical spectrographs require frequency calibration through sources like hollow-cathode lamps or absorption-gas cells. Laser frequency combs (LFCs) provide highest accuracy but are facing operational challenges. We aim to provide a precise and accurate frequency solution for the spectrum of molecular iodine absorption by referencing to an LFC that does not cover the same frequency range. We used a Fourier Transform Spectrometer (FTS) to produce a consistent frequency scale for the combined spectrum from an iodine absorption cell at 5200--6200AA and an LFC at 8200AA. We used 17,807 comb lines to determine the FTS frequency offset and compared the calibrated iodine spectrum to a synthetic spectrum computed from a molecular potential model. In a single scan, the frequency offset was determined from the comb spectrum with an uncertainty of $sim$1 cm s$^{-1}$. The distribution of comb line frequencies is consistent with no deviation from linearity. The iodine observation matches the model with an offset of smaller than the model uncertainties of $sim$1 m s$^{-1}$, which confirms that the FTS zero point is valid outside the range covered by the LFC, and that the frequencies of the iodine absorption model are accurate. We also report small systematic effects regarding the iodine model's energy scale. We conclude that Fourier Transform Spectrometry can transfer LFC accuracy into frequency ranges not originally covered by the comb. This allows us to assign accurate frequency scales to the spectra of customized wavelength calibrators. The calibrators can be optimized for individual spectrograph designs regarding resolution and spectral bandwidth, and requirements on their long-term stability are relaxed because FTS monitoring can be performed during operation. This provides flexibility for the design and operation of calibration sources for high-precision Doppler experiments.
{"title":"Accurate calibration spectra for precision radial velocities -- Iodine absorption referenced by a laser frequency comb","authors":"Ansgar Reiners, Michael Debus, Sebastian Schäfer, Eberhard Tiemann, Mathias Zechmeister","doi":"arxiv-2409.02631","DOIUrl":"https://doi.org/arxiv-2409.02631","url":null,"abstract":"Astronomical spectrographs require frequency calibration through sources like\u0000hollow-cathode lamps or absorption-gas cells. Laser frequency combs (LFCs)\u0000provide highest accuracy but are facing operational challenges. We aim to\u0000provide a precise and accurate frequency solution for the spectrum of molecular\u0000iodine absorption by referencing to an LFC that does not cover the same\u0000frequency range. We used a Fourier Transform Spectrometer (FTS) to produce a\u0000consistent frequency scale for the combined spectrum from an iodine absorption\u0000cell at 5200--6200AA and an LFC at 8200AA. We used 17,807 comb lines to\u0000determine the FTS frequency offset and compared the calibrated iodine spectrum\u0000to a synthetic spectrum computed from a molecular potential model. In a single\u0000scan, the frequency offset was determined from the comb spectrum with an\u0000uncertainty of $sim$1 cm s$^{-1}$. The distribution of comb line frequencies\u0000is consistent with no deviation from linearity. The iodine observation matches\u0000the model with an offset of smaller than the model uncertainties of $sim$1 m\u0000s$^{-1}$, which confirms that the FTS zero point is valid outside the range\u0000covered by the LFC, and that the frequencies of the iodine absorption model are\u0000accurate. We also report small systematic effects regarding the iodine model's\u0000energy scale. We conclude that Fourier Transform Spectrometry can transfer LFC\u0000accuracy into frequency ranges not originally covered by the comb. This allows\u0000us to assign accurate frequency scales to the spectra of customized wavelength\u0000calibrators. The calibrators can be optimized for individual spectrograph\u0000designs regarding resolution and spectral bandwidth, and requirements on their\u0000long-term stability are relaxed because FTS monitoring can be performed during\u0000operation. This provides flexibility for the design and operation of\u0000calibration sources for high-precision Doppler experiments.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"43 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217505","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Sumit Dahal, Peter A. R. Ade, Christopher J. Anderson, Alyssa Barlis, Emily M. Barrentine, Jeffrey W. Beeman, Nicholas Bellis, Alberto D. Bolatto, Victoria Braianova, Patrick C. Breysse, Berhanu T. Bulcha, Giuseppe Cataldo, Felipe A. Colazo, Lee-Roger Chevres-Fernandez, Chullhee Cho, Danny S. Chmaytelli, Jake A. Connors, Nicholas P. Costen, Paul W. Cursey, Negar Ehsan, Thomas M. Essinger-Hileman, Jason Glenn, Joseph E. Golec, James P. Hays-Wehle, Larry A. Hess, Amir E. Jahromi, Trevian Jenkins, Mark O. Kimball, Alan J. Kogut, Samuel H. Kramer, Nicole Leung, Luke N. Lowe, Philip D. Mauskopf, Jeffrey J. McMahon, Vilem Mikula, Mona Mirzaei, Samuel H. Moseley, Jonas W. Mugge-Durum, Jacob Nellis, Omid Noroozian, Kate Okun, Trevor Oxholm, Tatsat Parekh, Ue-Li Pen, Anthony R. Pullen, Maryam Rahmani, Mathias M. Ramirez, Cody Roberson, Samelys Rodriguez, Florian Roselli, Deepak Sapkota, Konrad Shire, Gage L. Siebert, Faizah Siddique, Adrian K. Sinclair, Rachel S. Somerville, Ryan Stephenson, Thomas R. Stevenson, Eric R. Switzer, Jared Termini, Peter T. Timbie, Justin Trenkamp, Carole E. Tucker, Elijah Visbal, Carolyn G. Volpert, Joseph Watson, Eric Weeks, Edward J. Wollack, Shengqi Yang, Aaron Yung
The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) is a balloon-borne telescope designed to survey star formation over cosmological time scales using intensity mapping in the 420 - 540 GHz frequency range. EXCLAIM uses a fully cryogenic telescope coupled to six on-chip spectrometers featuring kinetic inductance detectors (KIDs) to achieve high sensitivity, allowing for fast integration in dark atmospheric windows. The telescope receiver is cooled to $approx$ 1.7 K by immersion in a superfluid helium bath and enclosed in a superfluid-tight shell with a meta-material anti-reflection coated silicon window. In addition to the optics and the spectrometer package, the receiver contains the magnetic shielding, the cryogenic segment of the spectrometer readout, and the sub-Kelvin cooling system. A three-stage continuous adiabatic demagnetization refrigerator (CADR) keeps the detectors at 100 mK while a $^4$He sorption cooler provides a 900 mK thermal intercept for mechanical suspensions and coaxial cables. We present the design of the EXCLAIM receiver and report on the flight-like testing of major receiver components, including the superfluid-tight receiver window and the sub-Kelvin coolers.
{"title":"Superfluid-tight cryogenic receiver with continuous sub-Kelvin cooling for EXCLAIM","authors":"Sumit Dahal, Peter A. R. Ade, Christopher J. Anderson, Alyssa Barlis, Emily M. Barrentine, Jeffrey W. Beeman, Nicholas Bellis, Alberto D. Bolatto, Victoria Braianova, Patrick C. Breysse, Berhanu T. Bulcha, Giuseppe Cataldo, Felipe A. Colazo, Lee-Roger Chevres-Fernandez, Chullhee Cho, Danny S. Chmaytelli, Jake A. Connors, Nicholas P. Costen, Paul W. Cursey, Negar Ehsan, Thomas M. Essinger-Hileman, Jason Glenn, Joseph E. Golec, James P. Hays-Wehle, Larry A. Hess, Amir E. Jahromi, Trevian Jenkins, Mark O. Kimball, Alan J. Kogut, Samuel H. Kramer, Nicole Leung, Luke N. Lowe, Philip D. Mauskopf, Jeffrey J. McMahon, Vilem Mikula, Mona Mirzaei, Samuel H. Moseley, Jonas W. Mugge-Durum, Jacob Nellis, Omid Noroozian, Kate Okun, Trevor Oxholm, Tatsat Parekh, Ue-Li Pen, Anthony R. Pullen, Maryam Rahmani, Mathias M. Ramirez, Cody Roberson, Samelys Rodriguez, Florian Roselli, Deepak Sapkota, Konrad Shire, Gage L. Siebert, Faizah Siddique, Adrian K. Sinclair, Rachel S. Somerville, Ryan Stephenson, Thomas R. Stevenson, Eric R. Switzer, Jared Termini, Peter T. Timbie, Justin Trenkamp, Carole E. Tucker, Elijah Visbal, Carolyn G. Volpert, Joseph Watson, Eric Weeks, Edward J. Wollack, Shengqi Yang, Aaron Yung","doi":"arxiv-2409.02847","DOIUrl":"https://doi.org/arxiv-2409.02847","url":null,"abstract":"The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) is a\u0000balloon-borne telescope designed to survey star formation over cosmological\u0000time scales using intensity mapping in the 420 - 540 GHz frequency range.\u0000EXCLAIM uses a fully cryogenic telescope coupled to six on-chip spectrometers\u0000featuring kinetic inductance detectors (KIDs) to achieve high sensitivity,\u0000allowing for fast integration in dark atmospheric windows. The telescope\u0000receiver is cooled to $approx$ 1.7 K by immersion in a superfluid helium bath\u0000and enclosed in a superfluid-tight shell with a meta-material anti-reflection\u0000coated silicon window. In addition to the optics and the spectrometer package,\u0000the receiver contains the magnetic shielding, the cryogenic segment of the\u0000spectrometer readout, and the sub-Kelvin cooling system. A three-stage\u0000continuous adiabatic demagnetization refrigerator (CADR) keeps the detectors at\u0000100 mK while a $^4$He sorption cooler provides a 900 mK thermal intercept for\u0000mechanical suspensions and coaxial cables. We present the design of the EXCLAIM\u0000receiver and report on the flight-like testing of major receiver components,\u0000including the superfluid-tight receiver window and the sub-Kelvin coolers.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"54 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217504","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Lei Wang, Xiaoming Zhang, Chunhai Bai, Haiwen Xie, Juan Li, Jiayi Ge, Jianfeng Wang, Xianqun Zeng, Jiantao Sun, Xiaojun Jiang
Optically observing and monitoring moving objects, both natural and artificial, is important to human space security. Non-sidereal tracking can improve the system's limiting magnitude for moving objects, which benefits the surveillance. However, images with non-sidereal tracking include complex background, as well as objects with different brightness and moving mode, posing a significant challenge for accurate multi-object detection in such images, especially in wide field of view (WFOV) telescope images. To achieve a higher detection precision in a higher speed, we proposed a novel object detection method, which combines the source feature extraction and the neural network. First, our method extracts object features from optical images such as centroid, shape, and flux. Then it conducts a naive labeling based on those features to distinguish moving objects from stars. After balancing the labeled data, we employ it to train a neural network aimed at creating a classification model for point-like and streak-like objects. Ultimately, based on the neural network model's classification outcomes, moving objects whose motion modes consistent with the tracked objects are detected via track association, while objects with different motion modes are detected using morphological statistics. The validation, based on the space objects images captured in target tracking mode with the 1-meter telescope at Nanshan, Xinjiang Astronomical Observatory, demonstrates that our method achieves 94.72% detection accuracy with merely 5.02% false alarm rate, and a processing time of 0.66s per frame. Consequently, our method can rapidly and accurately detect objects with different motion modes from wide-field images with non-sidereal tracking.
{"title":"Rapid Automatic Multiple Moving Objects Detection Method Based on Feature Extraction from Images with Non-sidereal Tracking","authors":"Lei Wang, Xiaoming Zhang, Chunhai Bai, Haiwen Xie, Juan Li, Jiayi Ge, Jianfeng Wang, Xianqun Zeng, Jiantao Sun, Xiaojun Jiang","doi":"arxiv-2409.02405","DOIUrl":"https://doi.org/arxiv-2409.02405","url":null,"abstract":"Optically observing and monitoring moving objects, both natural and\u0000artificial, is important to human space security. Non-sidereal tracking can\u0000improve the system's limiting magnitude for moving objects, which benefits the\u0000surveillance. However, images with non-sidereal tracking include complex\u0000background, as well as objects with different brightness and moving mode,\u0000posing a significant challenge for accurate multi-object detection in such\u0000images, especially in wide field of view (WFOV) telescope images. To achieve a\u0000higher detection precision in a higher speed, we proposed a novel object\u0000detection method, which combines the source feature extraction and the neural\u0000network. First, our method extracts object features from optical images such as\u0000centroid, shape, and flux. Then it conducts a naive labeling based on those\u0000features to distinguish moving objects from stars. After balancing the labeled\u0000data, we employ it to train a neural network aimed at creating a classification\u0000model for point-like and streak-like objects. Ultimately, based on the neural\u0000network model's classification outcomes, moving objects whose motion modes\u0000consistent with the tracked objects are detected via track association, while\u0000objects with different motion modes are detected using morphological\u0000statistics. The validation, based on the space objects images captured in\u0000target tracking mode with the 1-meter telescope at Nanshan, Xinjiang\u0000Astronomical Observatory, demonstrates that our method achieves 94.72%\u0000detection accuracy with merely 5.02% false alarm rate, and a processing time of\u00000.66s per frame. Consequently, our method can rapidly and accurately detect\u0000objects with different motion modes from wide-field images with non-sidereal\u0000tracking.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"13 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217510","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：