Noura IbrahimUniversity of Michigan, Mayra GutierrezUniversity of Michigan, John D. MonnierUniversity of Michigan, Stefan KrausUniversity of Exeter, Jean-Baptiste Le BouquinIPAG, Narsireddy AnuguThe CHARA Array, Theo ten BrummelaarThe CHARA Array, Sorabh ChhabraUniversity of Exeter, Isabelle CodronUniversity of Exeter, Julien DejongheObservatoire de la Côte d'Azur, Aaron LabdonEuropean Southern Observatory, Daniel LecronObservatoire de la Côte d'Azur, Daniel MortimerMax-Planck-Institut für Astronomie, Denis MourardObservatoire de la Côte d'Azur, Gail SchaeferThe CHARA Array, Benjamin SetterholmMax-Planck-Institut für Astronomie, Manuela ArnóINAF, Andrea BiancoINAF, Michele FrangiamoreINAF, Laurent JocouIPAG
MIRC-X and MYSTIC are six-telescope near-infrared beam (1.08-2.38 ${mu}$m) combiners at the CHARA Array on Mt Wilson CA, USA. Ever since the commissioning of MIRC-X (J and H bands) in 2018 and MYSTIC (K bands) in 2021, they have been the most popular and over-subscribed instruments at the array. Observers have been able to image stellar objects with sensitivity down to 8.1 mag in H and 7.8 mag in K-band under the very best conditions. In 2022 MYSTIC was upgraded with a new ABCD mode using the VLTI/GRAVITY 4-beam integrated optics chip, with the goal of improving the sensitivity and calibration. The ABCD mode has been used to observe more than 20 T Tauri stars; however, the data pipeline is still being developed. Alongside software upgrades, we detail planned upgrades to both instruments in this paper. The main upgrades are: 1) Adding a motorized filter wheel to MIRC-X along with new high spectral resolution modes 2) Updating MIRC-X optics to allow for simultaneous 6T J+H observations 3) Removing the warm window between the spectrograph and the warm optics in MYSTIC 4) Adding a 6T ABCD mode to MIRC-X in collaboration with CHARA/SPICA 5) Updating the MIRC-X CRED-ONE camera funded by Prof. Kraus from U. Exeter 6) Carrying out science verification of the MIRC-X polarization mode 7) Developing new software for ABCD-mode data reduction and more efficient calibration routines. We expect these upgrades to not only improve the observing experience, but also increase the sensitivity by 0.4 mag in J+H-bands, and 1 mag in K-band.
{"title":"Recent and Upcoming Upgrades for MIRC-X and MYSTIC on the CHARA Array","authors":"Noura IbrahimUniversity of Michigan, Mayra GutierrezUniversity of Michigan, John D. MonnierUniversity of Michigan, Stefan KrausUniversity of Exeter, Jean-Baptiste Le BouquinIPAG, Narsireddy AnuguThe CHARA Array, Theo ten BrummelaarThe CHARA Array, Sorabh ChhabraUniversity of Exeter, Isabelle CodronUniversity of Exeter, Julien DejongheObservatoire de la Côte d'Azur, Aaron LabdonEuropean Southern Observatory, Daniel LecronObservatoire de la Côte d'Azur, Daniel MortimerMax-Planck-Institut für Astronomie, Denis MourardObservatoire de la Côte d'Azur, Gail SchaeferThe CHARA Array, Benjamin SetterholmMax-Planck-Institut für Astronomie, Manuela ArnóINAF, Andrea BiancoINAF, Michele FrangiamoreINAF, Laurent JocouIPAG","doi":"arxiv-2408.04038","DOIUrl":"https://doi.org/arxiv-2408.04038","url":null,"abstract":"MIRC-X and MYSTIC are six-telescope near-infrared beam (1.08-2.38 ${mu}$m)\u0000combiners at the CHARA Array on Mt Wilson CA, USA. Ever since the commissioning\u0000of MIRC-X (J and H bands) in 2018 and MYSTIC (K bands) in 2021, they have been\u0000the most popular and over-subscribed instruments at the array. Observers have\u0000been able to image stellar objects with sensitivity down to 8.1 mag in H and\u00007.8 mag in K-band under the very best conditions. In 2022 MYSTIC was upgraded\u0000with a new ABCD mode using the VLTI/GRAVITY 4-beam integrated optics chip, with\u0000the goal of improving the sensitivity and calibration. The ABCD mode has been\u0000used to observe more than 20 T Tauri stars; however, the data pipeline is still\u0000being developed. Alongside software upgrades, we detail planned upgrades to\u0000both instruments in this paper. The main upgrades are: 1) Adding a motorized\u0000filter wheel to MIRC-X along with new high spectral resolution modes 2)\u0000Updating MIRC-X optics to allow for simultaneous 6T J+H observations 3)\u0000Removing the warm window between the spectrograph and the warm optics in MYSTIC\u00004) Adding a 6T ABCD mode to MIRC-X in collaboration with CHARA/SPICA 5)\u0000Updating the MIRC-X CRED-ONE camera funded by Prof. Kraus from U. Exeter 6)\u0000Carrying out science verification of the MIRC-X polarization mode 7) Developing\u0000new software for ABCD-mode data reduction and more efficient calibration\u0000routines. We expect these upgrades to not only improve the observing\u0000experience, but also increase the sensitivity by 0.4 mag in J+H-bands, and 1\u0000mag in K-band.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"36 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947582","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}
Konstantinos Platanitis, Miguel Arana-Catania, Leonardo Capicchiano, Saurabh Upadhyay, Leonard Felicetti
This paper presents a machine learning approach to estimate the inertial parameters of a spacecraft in cases when those change during operations, e.g. multiple deployments of payloads, unfolding of appendages and booms, propellant consumption as well as during in-orbit servicing and active debris removal operations. The machine learning approach uses time series clustering together with an optimised actuation sequence generated by reinforcement learning to facilitate distinguishing among different inertial parameter sets. The performance of the proposed strategy is assessed against the case of a multi-satellite deployment system showing that the algorithm is resilient towards common disturbances in such kinds of operations.
{"title":"Spacecraft inertial parameters estimation using time series clustering and reinforcement learning","authors":"Konstantinos Platanitis, Miguel Arana-Catania, Leonardo Capicchiano, Saurabh Upadhyay, Leonard Felicetti","doi":"arxiv-2408.03445","DOIUrl":"https://doi.org/arxiv-2408.03445","url":null,"abstract":"This paper presents a machine learning approach to estimate the inertial\u0000parameters of a spacecraft in cases when those change during operations, e.g.\u0000multiple deployments of payloads, unfolding of appendages and booms, propellant\u0000consumption as well as during in-orbit servicing and active debris removal\u0000operations. The machine learning approach uses time series clustering together\u0000with an optimised actuation sequence generated by reinforcement learning to\u0000facilitate distinguishing among different inertial parameter sets. The\u0000performance of the proposed strategy is assessed against the case of a\u0000multi-satellite deployment system showing that the algorithm is resilient\u0000towards common disturbances in such kinds of operations.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"90 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947587","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}
Y. Takasefor the LiteBIRD Collaboration, L. Vacherfor the LiteBIRD Collaboration, H. Ishinofor the LiteBIRD Collaboration, G. Patanchonfor the LiteBIRD Collaboration, L. Montierfor the LiteBIRD Collaboration, S. L. Steverfor the LiteBIRD Collaboration, K. Ishizakafor the LiteBIRD Collaboration, Y. Naganofor the LiteBIRD Collaboration, W. Wangfor the LiteBIRD Collaboration, J. Aumontfor the LiteBIRD Collaboration, K. Aizawafor the LiteBIRD Collaboration, A. Anandfor the LiteBIRD Collaboration, C. Baccigalupifor the LiteBIRD Collaboration, M. Ballardinifor the LiteBIRD Collaboration, A. J. Bandayfor the LiteBIRD Collaboration, R. B. Barreirofor the LiteBIRD Collaboration, N. Bartolofor the LiteBIRD Collaboration, S. Basakfor the LiteBIRD Collaboration, M. Bersanellifor the LiteBIRD Collaboration, M. Bortolamifor the LiteBIRD Collaboration, T. Brinckmannfor the LiteBIRD Collaboration, E. Calabresefor the LiteBIRD Collaboration, P. Campetifor the LiteBIRD Collaboration, E. Carinosfor the LiteBIRD Collaboration, A. Caronesfor the LiteBIRD Collaboration, F. J. Casasfor the LiteBIRD Collaboration, K. Cheungfor the LiteBIRD Collaboration, L. Clermontfor the LiteBIRD Collaboration, F. Columbrofor the LiteBIRD Collaboration, A. Coppolecchiafor the LiteBIRD Collaboration, F. Cuttaiafor the LiteBIRD Collaboration, P. de Bernardisfor the LiteBIRD Collaboration, T. de Haanfor the LiteBIRD Collaboration, E. de la Hozfor the LiteBIRD Collaboration, S. Della Torrefor the LiteBIRD Collaboration, P. Diego-Palazuelosfor the LiteBIRD Collaboration, G. D'Alessandrofor the LiteBIRD Collaboration, H. K. Eriksenfor the LiteBIRD Collaboration, J. Errardfor the LiteBIRD Collaboration, F. Finellifor the LiteBIRD Collaboration, U. Fuskelandfor the LiteBIRD Collaboration, G. Gallonifor the LiteBIRD Collaboration, M. Gallowayfor the LiteBIRD Collaboration, M. Gervasifor the LiteBIRD Collaboration, T. Ghignafor the LiteBIRD Collaboration, S. Giardiellofor the LiteBIRD Collaboration, C. Gimeno-Amofor the LiteBIRD Collaboration, E. Gjerløwfor the LiteBIRD Collaboration, R. González Gonzálezfor the LiteBIRD Collaboration, A. Gruppusofor the LiteBIRD Collaboration, M. Hazumifor the LiteBIRD Collaboration, S. Henrot-Versilléfor the LiteBIRD Collaboration, L. T. Hergtfor the LiteBIRD Collaboration, K. Ikumafor the LiteBIRD Collaboration, K. Kohrifor the LiteBIRD Collaboration, L. Lamagnafor the LiteBIRD Collaboration, M. Lattanzifor the LiteBIRD Collaboration, C. Leloupfor the LiteBIRD Collaboration, M. Lembofor the LiteBIRD Collaboration, F. Levrierfor the LiteBIRD Collaboration, A. I. Lonappanfor the LiteBIRD Collaboration, M. López-Caniegofor the LiteBIRD Collaboration, G. Luzzifor the LiteBIRD Collaboration, B. Maffeifor the LiteBIRD Collaboration, E. Martínez-Gonzálezfor the LiteBIRD Collaboration, S. Masifor the LiteBIRD Collaboration, S. Matarresefor the LiteBIRD Collaboration, F. T. Matsudafor the LiteBIRD Collaboration, T. Matsumurafor the LiteBIRD Collaboration, S. Michelifor the LiteBIRD Collaboration, M. Migliacciofor the LiteBIRD Collaboration, M. Monellifor the LiteBIRD Collaboration, G. Morgantefor the LiteBIRD Collaboration, B. Motfor the LiteBIRD Collaboration, R. Nagatafor the LiteBIRD Collaboration, T. Namikawafor the LiteBIRD Collaboration, A. Novellifor the LiteBIRD Collaboration, K. Odagirifor the LiteBIRD Collaboration, S. Ogurifor the LiteBIRD Collaboration, R. Omaefor the LiteBIRD Collaboration, L. Paganofor the LiteBIRD Collaboration, D. Paolettifor the LiteBIRD Collaboration, F. Piacentinifor the LiteBIRD Collaboration, M. Pincherafor the LiteBIRD Collaboration, G. Polentafor the LiteBIRD Collaboration, L. Porcellifor the LiteBIRD Collaboration, N. Raffuzzifor the LiteBIRD Collaboration, M. Remazeillesfor the LiteBIRD Collaboration, A. Ritaccofor the LiteBIRD Collaboration, M. Ruiz-Grandafor the LiteBIRD Collaboration, Y. Sakuraifor the LiteBIRD Collaboration, D. Scottfor the LiteBIRD Collaboration, Y. Sekimotofor the LiteBIRD Collaboration, M. Shiraishifor the LiteBIRD Collaboration, G. Signorellifor the LiteBIRD Collaboration, R. M. Sullivanfor the LiteBIRD Collaboration, H. Takakurafor the LiteBIRD Collaboration, L. Terenzifor the LiteBIRD Collaboration, M. Tomasifor the LiteBIRD Collaboration, M. Tristramfor the LiteBIRD Collaboration, B. van Tentfor the LiteBIRD Collaboration, P. Vielvafor the LiteBIRD Collaboration, I. K. Wehusfor the LiteBIRD Collaboration, B. Westbrookfor the LiteBIRD Collaboration, G. Weymann-Despresfor the LiteBIRD Collaboration, E. J. Wollackfor the LiteBIRD Collaboration, M. Zannonifor the LiteBIRD Collaboration, Y. Zhoufor the LiteBIRD Collaboration
Large angular scale surveys in the absence of atmosphere are essential for measuring the primordial $B$-mode power spectrum of the Cosmic Microwave Background (CMB). Since this proposed measurement is about three to four orders of magnitude fainter than the temperature anisotropies of the CMB, in-flight calibration of the instruments and active suppression of systematic effects are crucial. We investigate the effect of changing the parameters of the scanning strategy on the in-flight calibration effectiveness, the suppression of the systematic effects themselves, and the ability to distinguish systematic effects by null-tests. Next-generation missions such as LiteBIRD, modulated by a Half-Wave Plate (HWP), will be able to observe polarisation using a single detector, eliminating the need to combine several detectors to measure polarisation, as done in many previous experiments and hence avoiding the consequent systematic effects. While the HWP is expected to suppress many systematic effects, some of them will remain. We use an analytical approach to comprehensively address the mitigation of these systematic effects and identify the characteristics of scanning strategies that are the most effective for implementing a variety of calibration strategies in the multi-dimensional space of common spacecraft scan parameters. We also present Falcons, a fast spacecraft scanning simulator that we developed to investigate this scanning parameter space.
{"title":"Multi-dimensional optimisation of the scanning strategy for the LiteBIRD space mission","authors":"Y. Takasefor the LiteBIRD Collaboration, L. Vacherfor the LiteBIRD Collaboration, H. Ishinofor the LiteBIRD Collaboration, G. Patanchonfor the LiteBIRD Collaboration, L. Montierfor the LiteBIRD Collaboration, S. L. Steverfor the LiteBIRD Collaboration, K. Ishizakafor the LiteBIRD Collaboration, Y. Naganofor the LiteBIRD Collaboration, W. Wangfor the LiteBIRD Collaboration, J. Aumontfor the LiteBIRD Collaboration, K. Aizawafor the LiteBIRD Collaboration, A. Anandfor the LiteBIRD Collaboration, C. Baccigalupifor the LiteBIRD Collaboration, M. Ballardinifor the LiteBIRD Collaboration, A. J. Bandayfor the LiteBIRD Collaboration, R. B. Barreirofor the LiteBIRD Collaboration, N. Bartolofor the LiteBIRD Collaboration, S. Basakfor the LiteBIRD Collaboration, M. Bersanellifor the LiteBIRD Collaboration, M. Bortolamifor the LiteBIRD Collaboration, T. Brinckmannfor the LiteBIRD Collaboration, E. Calabresefor the LiteBIRD Collaboration, P. Campetifor the LiteBIRD Collaboration, E. Carinosfor the LiteBIRD Collaboration, A. Caronesfor the LiteBIRD Collaboration, F. J. Casasfor the LiteBIRD Collaboration, K. Cheungfor the LiteBIRD Collaboration, L. Clermontfor the LiteBIRD Collaboration, F. Columbrofor the LiteBIRD Collaboration, A. Coppolecchiafor the LiteBIRD Collaboration, F. Cuttaiafor the LiteBIRD Collaboration, P. de Bernardisfor the LiteBIRD Collaboration, T. de Haanfor the LiteBIRD Collaboration, E. de la Hozfor the LiteBIRD Collaboration, S. Della Torrefor the LiteBIRD Collaboration, P. Diego-Palazuelosfor the LiteBIRD Collaboration, G. D'Alessandrofor the LiteBIRD Collaboration, H. K. Eriksenfor the LiteBIRD Collaboration, J. Errardfor the LiteBIRD Collaboration, F. Finellifor the LiteBIRD Collaboration, U. Fuskelandfor the LiteBIRD Collaboration, G. Gallonifor the LiteBIRD Collaboration, M. Gallowayfor the LiteBIRD Collaboration, M. Gervasifor the LiteBIRD Collaboration, T. Ghignafor the LiteBIRD Collaboration, S. Giardiellofor the LiteBIRD Collaboration, C. Gimeno-Amofor the LiteBIRD Collaboration, E. Gjerløwfor the LiteBIRD Collaboration, R. González Gonzálezfor the LiteBIRD Collaboration, A. Gruppusofor the LiteBIRD Collaboration, M. Hazumifor the LiteBIRD Collaboration, S. Henrot-Versilléfor the LiteBIRD Collaboration, L. T. Hergtfor the LiteBIRD Collaboration, K. Ikumafor the LiteBIRD Collaboration, K. Kohrifor the LiteBIRD Collaboration, L. Lamagnafor the LiteBIRD Collaboration, M. Lattanzifor the LiteBIRD Collaboration, C. Leloupfor the LiteBIRD Collaboration, M. Lembofor the LiteBIRD Collaboration, F. Levrierfor the LiteBIRD Collaboration, A. I. Lonappanfor the LiteBIRD Collaboration, M. López-Caniegofor the LiteBIRD Collaboration, G. Luzzifor the LiteBIRD Collaboration, B. Maffeifor the LiteBIRD Collaboration, E. Martínez-Gonzálezfor the LiteBIRD Collaboration, S. Masifor the LiteBIRD Collaboration, S. Matarresefor the LiteBIRD Collaboration, F. T. Matsudafor the LiteBIRD Collaboration, T. Matsumurafor the LiteBIRD Collaboration, S. Michelifor the LiteBIRD Collaboration, M. Migliacciofor the LiteBIRD Collaboration, M. Monellifor the LiteBIRD Collaboration, G. Morgantefor the LiteBIRD Collaboration, B. Motfor the LiteBIRD Collaboration, R. Nagatafor the LiteBIRD Collaboration, T. Namikawafor the LiteBIRD Collaboration, A. Novellifor the LiteBIRD Collaboration, K. Odagirifor the LiteBIRD Collaboration, S. Ogurifor the LiteBIRD Collaboration, R. Omaefor the LiteBIRD Collaboration, L. Paganofor the LiteBIRD Collaboration, D. Paolettifor the LiteBIRD Collaboration, F. Piacentinifor the LiteBIRD Collaboration, M. Pincherafor the LiteBIRD Collaboration, G. Polentafor the LiteBIRD Collaboration, L. Porcellifor the LiteBIRD Collaboration, N. Raffuzzifor the LiteBIRD Collaboration, M. Remazeillesfor the LiteBIRD Collaboration, A. Ritaccofor the LiteBIRD Collaboration, M. Ruiz-Grandafor the LiteBIRD Collaboration, Y. Sakuraifor the LiteBIRD Collaboration, D. Scottfor the LiteBIRD Collaboration, Y. Sekimotofor the LiteBIRD Collaboration, M. Shiraishifor the LiteBIRD Collaboration, G. Signorellifor the LiteBIRD Collaboration, R. M. Sullivanfor the LiteBIRD Collaboration, H. Takakurafor the LiteBIRD Collaboration, L. Terenzifor the LiteBIRD Collaboration, M. Tomasifor the LiteBIRD Collaboration, M. Tristramfor the LiteBIRD Collaboration, B. van Tentfor the LiteBIRD Collaboration, P. Vielvafor the LiteBIRD Collaboration, I. K. Wehusfor the LiteBIRD Collaboration, B. Westbrookfor the LiteBIRD Collaboration, G. Weymann-Despresfor the LiteBIRD Collaboration, E. J. Wollackfor the LiteBIRD Collaboration, M. Zannonifor the LiteBIRD Collaboration, Y. Zhoufor the LiteBIRD Collaboration","doi":"arxiv-2408.03040","DOIUrl":"https://doi.org/arxiv-2408.03040","url":null,"abstract":"Large angular scale surveys in the absence of atmosphere are essential for\u0000measuring the primordial $B$-mode power spectrum of the Cosmic Microwave\u0000Background (CMB). Since this proposed measurement is about three to four orders\u0000of magnitude fainter than the temperature anisotropies of the CMB, in-flight\u0000calibration of the instruments and active suppression of systematic effects are\u0000crucial. We investigate the effect of changing the parameters of the scanning\u0000strategy on the in-flight calibration effectiveness, the suppression of the\u0000systematic effects themselves, and the ability to distinguish systematic\u0000effects by null-tests. Next-generation missions such as LiteBIRD, modulated by\u0000a Half-Wave Plate (HWP), will be able to observe polarisation using a single\u0000detector, eliminating the need to combine several detectors to measure\u0000polarisation, as done in many previous experiments and hence avoiding the\u0000consequent systematic effects. While the HWP is expected to suppress many\u0000systematic effects, some of them will remain. We use an analytical approach to\u0000comprehensively address the mitigation of these systematic effects and identify\u0000the characteristics of scanning strategies that are the most effective for\u0000implementing a variety of calibration strategies in the multi-dimensional space\u0000of common spacecraft scan parameters. We also present Falcons, a fast\u0000spacecraft scanning simulator that we developed to investigate this scanning\u0000parameter space.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"21 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947589","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}
Fluorescence telescopes are important instruments widely used in modern experiments for registering ultraviolet radiation from extensive air showers (EASs) generated by cosmic rays of ultra-high energies. We present a proof-of-concept convolutional neural network aimed at reconstruction of energy and arrival directions of primary particles using model data for two telescopes developed by the international JEM-EUSO collaboration. We also demonstrate how a simple convolutional encoder-decoder can be used for EAS track recognition. The approach is generic and can be adopted for other fluorescence telescopes.
荧光望远镜是现代实验中广泛使用的重要仪器，用于记录由超高能量宇宙射线产生的大范围空气淋浴（EAS）的紫外线辐射。我们介绍了一个概念验证卷积神经网络，旨在利用国际 JEM-EUSO 合作组织开发的两台望远镜的模型数据重建原生粒子的能量和到达方向。我们还演示了如何将简单的卷积编码器-解码器用于 EAS 轨迹识别。该方法具有通用性，可用于其他荧光望远镜。
{"title":"Reconstruction of energy and arrival directions of UHECRs registered by fluorescence telescopes with a neural network","authors":"Mikhail Zotovfor the JEM-EUSO Collaboration","doi":"arxiv-2408.02440","DOIUrl":"https://doi.org/arxiv-2408.02440","url":null,"abstract":"Fluorescence telescopes are important instruments widely used in modern\u0000experiments for registering ultraviolet radiation from extensive air showers\u0000(EASs) generated by cosmic rays of ultra-high energies. We present a\u0000proof-of-concept convolutional neural network aimed at reconstruction of energy\u0000and arrival directions of primary particles using model data for two telescopes\u0000developed by the international JEM-EUSO collaboration. We also demonstrate how\u0000a simple convolutional encoder-decoder can be used for EAS track recognition.\u0000The approach is generic and can be adopted for other fluorescence telescopes.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947667","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}
Julia Saleh-Natur, Ehud Behar, Omer Reich, Shlomit Tarem, Zvika Tarem, Alex Vdovin, Amir Feigenboim, Roi Rahin, Avner Kaidar, Hovhannes Agalarian, Alon Osovizky, Max Ghelman
We present a full-size engineering model of GALI - The GAmma-ray burst Localizing Instrument, composed of 362 CsI(Tl) small cubic scintillators, distributed within a small volume of $sim2$l, and read out by silicon photo-multipliers. GALI can provide directional information about GRBs with high angular accuracy from angle-dependent mutual obstruction between its scintillators. Here, we demonstrate GALI's laboratory experiments with an $^{241}$Am source, which achieved directional reconstruction of $<$3$^circ$ accuracy, in agreement with our Monte-Carlo simulations. GALI has a wide field view of the unobstructed sky. With its current cubic configuration, GALI's effective area varies between 97 cm$^2$ (face on) and 138 cm$^2$ (from the corners at 45$^circ$), which is verified in the current experiment.
{"title":"GALI -- A GAmma-ray burst Localizing Instrument: Results from Full Size Engineering Model","authors":"Julia Saleh-Natur, Ehud Behar, Omer Reich, Shlomit Tarem, Zvika Tarem, Alex Vdovin, Amir Feigenboim, Roi Rahin, Avner Kaidar, Hovhannes Agalarian, Alon Osovizky, Max Ghelman","doi":"arxiv-2408.02144","DOIUrl":"https://doi.org/arxiv-2408.02144","url":null,"abstract":"We present a full-size engineering model of GALI - The GAmma-ray burst\u0000Localizing Instrument, composed of 362 CsI(Tl) small cubic scintillators,\u0000distributed within a small volume of $sim2$l, and read out by silicon\u0000photo-multipliers. GALI can provide directional information about GRBs with\u0000high angular accuracy from angle-dependent mutual obstruction between its\u0000scintillators. Here, we demonstrate GALI's laboratory experiments with an\u0000$^{241}$Am source, which achieved directional reconstruction of $<$3$^circ$\u0000accuracy, in agreement with our Monte-Carlo simulations. GALI has a wide field\u0000view of the unobstructed sky. With its current cubic configuration, GALI's\u0000effective area varies between 97 cm$^2$ (face on) and 138 cm$^2$ (from the\u0000corners at 45$^circ$), which is verified in the current experiment.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"63 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947591","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}
Phil Cigan, Valeri Makarov, Nathan Secrest, David Gordon, Megan Johnson, Sebastien Lambert
Using very long baseline interferometry data for the sources that comprise the third International Celestial Reference Frame (ICRF3), we examine the quality of the formal source position uncertainties of ICRF3 by determining the excess astrometric variability (unexplained variance) for each source as a function of time. We also quantify multiple qualitatively distinct aspects of astrometric variability seen in the data, using a variety of metrics. Average position offsets, statistical dispersion measures, and coherent trends over time as explored by smoothing the data are combined to characterize the most and least positionally stable ICRF3 sources. We find a notable dependence of the excess variance and statistical variability measures on declination, as is expected for unmodeled ionospheric delay errors and the northern hemisphere dominated network geometries of most astrometric and geodetic observing campaigns.
{"title":"Metrics of Astrometric Variability in the International Celestial Reference Frame: I. Statistical analysis and selection of the most variable sources","authors":"Phil Cigan, Valeri Makarov, Nathan Secrest, David Gordon, Megan Johnson, Sebastien Lambert","doi":"arxiv-2408.01373","DOIUrl":"https://doi.org/arxiv-2408.01373","url":null,"abstract":"Using very long baseline interferometry data for the sources that comprise\u0000the third International Celestial Reference Frame (ICRF3), we examine the\u0000quality of the formal source position uncertainties of ICRF3 by determining the\u0000excess astrometric variability (unexplained variance) for each source as a\u0000function of time. We also quantify multiple qualitatively distinct aspects of\u0000astrometric variability seen in the data, using a variety of metrics. Average\u0000position offsets, statistical dispersion measures, and coherent trends over\u0000time as explored by smoothing the data are combined to characterize the most\u0000and least positionally stable ICRF3 sources. We find a notable dependence of\u0000the excess variance and statistical variability measures on declination, as is\u0000expected for unmodeled ionospheric delay errors and the northern hemisphere\u0000dominated network geometries of most astrometric and geodetic observing\u0000campaigns.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"90 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947594","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}
Gerard T. van Belle, David Ciardi, Daniel Hillsberry, Anders Jorgensen, John Monnier, Krista Lynne Smith, Tabetha Boyajian, Kenneth Carpenter, Catherine Clark, Gioia Rau, Gail Schaefer
MoonLITE (Lunar InTerferometry Explorer) is an Astrophysics Pioneers proposal to develop, build, fly, and operate the first separated-aperture optical interferometer in space, delivering sub-mas science results. MoonLITE will leverage the Pioneers opportunity for utilizing NASA's Commercial Lunar Payload Services (CLPS) to deliver an optical interferometer to the lunar surface, enabling unprecedented discovery power by combining high spatial resolution from optical interferometry with deep sensitivity from the stability of the lunar surface. Following landing, the CLPS-provided rover will deploy the pre-loaded MoonLITE outboard optical telescope 100 meters from the lander's inboard telescope, establishing a two-element interferometric observatory with a single deployment. MoonLITE will observe targets as faint as 17th magnitude in the visible, exceeding ground-based interferometric sensitivity by many magnitudes, and surpassing space-based optical systems resolution by a factor of 50 times. The capabilities of MoonLITE open a unique discovery space that includes direct size measurements of the smallest, coolest stars and substellar brown dwarfs; searches for close-in stellar companions orbiting exoplanet-hosting stars that could confound our understanding and characterization of the frequency of Earth-like planets; direct size measurements of young stellar objects and characterization of the terrestrial planet-forming regions of these young stars; measurements of the inner regions and binary fraction of active galactic nuclei; and a probe of the very nature of spacetime foam itself. A portion of the observing time will also be made available to the broader community via a guest observer program. MoonLITE takes advantage of the CLPS opportunity and delivers an unprecedented combination of sensitivity and angular resolution at the remarkably affordable cost point of Pioneers.
{"title":"MoonLITE: a CLPS-delivered NASA Astrophysics Pioneers lunar optical interferometer for sensitive, milliarcsecond observing","authors":"Gerard T. van Belle, David Ciardi, Daniel Hillsberry, Anders Jorgensen, John Monnier, Krista Lynne Smith, Tabetha Boyajian, Kenneth Carpenter, Catherine Clark, Gioia Rau, Gail Schaefer","doi":"arxiv-2408.01392","DOIUrl":"https://doi.org/arxiv-2408.01392","url":null,"abstract":"MoonLITE (Lunar InTerferometry Explorer) is an Astrophysics Pioneers proposal\u0000to develop, build, fly, and operate the first separated-aperture optical\u0000interferometer in space, delivering sub-mas science results. MoonLITE will\u0000leverage the Pioneers opportunity for utilizing NASA's Commercial Lunar Payload\u0000Services (CLPS) to deliver an optical interferometer to the lunar surface,\u0000enabling unprecedented discovery power by combining high spatial resolution\u0000from optical interferometry with deep sensitivity from the stability of the\u0000lunar surface. Following landing, the CLPS-provided rover will deploy the\u0000pre-loaded MoonLITE outboard optical telescope 100 meters from the lander's\u0000inboard telescope, establishing a two-element interferometric observatory with\u0000a single deployment. MoonLITE will observe targets as faint as 17th magnitude\u0000in the visible, exceeding ground-based interferometric sensitivity by many\u0000magnitudes, and surpassing space-based optical systems resolution by a factor\u0000of 50 times. The capabilities of MoonLITE open a unique discovery space that\u0000includes direct size measurements of the smallest, coolest stars and substellar\u0000brown dwarfs; searches for close-in stellar companions orbiting\u0000exoplanet-hosting stars that could confound our understanding and\u0000characterization of the frequency of Earth-like planets; direct size\u0000measurements of young stellar objects and characterization of the terrestrial\u0000planet-forming regions of these young stars; measurements of the inner regions\u0000and binary fraction of active galactic nuclei; and a probe of the very nature\u0000of spacetime foam itself. A portion of the observing time will also be made\u0000available to the broader community via a guest observer program. MoonLITE takes\u0000advantage of the CLPS opportunity and delivers an unprecedented combination of\u0000sensitivity and angular resolution at the remarkably affordable cost point of\u0000Pioneers.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"47 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947595","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}
A. Donaldson, C. Snodgrass, R. Kokotanekova, A. Rożek
The Legacy Survey of Space and Time (LSST) at Vera C. Rubin Observatory will deliver high-quality, temporally-sparse observations of millions of Solar System objects on an unprecedented scale. Such datasets will likely enable the precise estimation of small body properties on a population-wide basis. In this work, we consider the possible applications of photometric data points from the LSST to the characterisation of Jupiter-family comet (JFC) nuclei. We simulate sparse-in-time lightcurve points with an LSST-like cadence for the orbit of a JFC between 2024-2033. Convex lightcurve inversion is used to assess whether the simulation input parameters can be accurately reproduced for a sample of nucleus rotation periods, pole orientations, activity onsets, shapes and sizes. We find that the rotation period and pole direction can be reliably constrained across all nucleus variants tested, and that the convex shape models, while limited in their ability to describe complex or bilobed nuclei, are effective for correcting sparse photometry for rotational modulation to improve estimates of nucleus phase functions. Based on this analysis, we anticipate that LSST photometry will significantly enhance our present understanding of the spin-state and phase function distributions of JFC nuclei.
Vera C. Rubin 天文台的时空遗产巡天（LSST）将以前所未有的规模对数百万太阳系天体进行高质量、时间稀疏的观测。这样的数据集将有可能在整个群体的基础上实现对小天体特性的精确估算。在这项工作中，我们考虑了将来自LSST的测光数据点应用于描述木星眷属彗星（JFC）核特性的可能性。我们以类似于 LSST 的节奏模拟了 2024-2033 年间木星彗星轨道上的实时光曲线点。我们发现，旋转周期和极点方向可以在所有测试过的彗核变体中得到可靠的约束，而凸形模型虽然在描述复杂或双叶彗核方面能力有限，但却可以有效地校正稀疏的旋转调制光度，从而改进对彗核相位函数的估计。基于上述分析，我们预计 LSST 光度测量将大大提高我们目前对 JFC 核的自旋态和相位函数分布的认识。
{"title":"Predictions for Sparse Photometry of Jupiter-Family Comet Nuclei in the LSST Era","authors":"A. Donaldson, C. Snodgrass, R. Kokotanekova, A. Rożek","doi":"arxiv-2408.01315","DOIUrl":"https://doi.org/arxiv-2408.01315","url":null,"abstract":"The Legacy Survey of Space and Time (LSST) at Vera C. Rubin Observatory will\u0000deliver high-quality, temporally-sparse observations of millions of Solar\u0000System objects on an unprecedented scale. Such datasets will likely enable the\u0000precise estimation of small body properties on a population-wide basis. In this\u0000work, we consider the possible applications of photometric data points from the\u0000LSST to the characterisation of Jupiter-family comet (JFC) nuclei. We simulate\u0000sparse-in-time lightcurve points with an LSST-like cadence for the orbit of a\u0000JFC between 2024-2033. Convex lightcurve inversion is used to assess whether\u0000the simulation input parameters can be accurately reproduced for a sample of\u0000nucleus rotation periods, pole orientations, activity onsets, shapes and sizes.\u0000We find that the rotation period and pole direction can be reliably constrained\u0000across all nucleus variants tested, and that the convex shape models, while\u0000limited in their ability to describe complex or bilobed nuclei, are effective\u0000for correcting sparse photometry for rotational modulation to improve estimates\u0000of nucleus phase functions. Based on this analysis, we anticipate that LSST\u0000photometry will significantly enhance our present understanding of the\u0000spin-state and phase function distributions of JFC nuclei.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"59 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947596","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}
We systematically investigate the variability of polarized X-rays on a timescale of a few seconds in the low/hard state of the black hole binary Cygnus X-1. The correlation between polarization degrees and angles with X-Ray intensity was analyzed using data collected by the Imaging X-ray Polarimetry Explorer (IXPE) in June 2022. Given that X-Ray variability in the low/hard state of Cygnus X-1 is non-periodic, flux peaks were aggregated to suppress statistical fluctuations. We divided the temporal profiles of these aggregated flux peaks into seven time segments and evaluated the polarization for each segment. The results reveal that the polarization degree was 4.6%$pm$1.2 and 5.3%$pm$1.2 before and after the peak, respectively, but decreased to 3.4%$pm$1.1 and 2.7%$pm$1.1 in the segments including and immediately following the peak. Furthermore, the polarization angle exhibited a slight shift from approximately 30$^{circ}$ to $sim$40$^{circ}$ before and after the peak. These findings suggest that the accretion disk contracts with increasing X-Ray luminosity, and the closer proximity of the X-Ray emitting gas to the black hole may lead to reduced polarization.
{"title":"Polarized X-rays Correlated with Short--Timescale Variability of Cygnus X-1","authors":"Kaito Ninoyu, Yuusuke Uchida, Shinya Yamada, Takayoshi Kohmura, Taichi Igarashi, Ryota Hayakawa, Tenyo Kawamura","doi":"arxiv-2408.00980","DOIUrl":"https://doi.org/arxiv-2408.00980","url":null,"abstract":"We systematically investigate the variability of polarized X-rays on a\u0000timescale of a few seconds in the low/hard state of the black hole binary\u0000Cygnus X-1. The correlation between polarization degrees and angles with X-Ray\u0000intensity was analyzed using data collected by the Imaging X-ray Polarimetry\u0000Explorer (IXPE) in June 2022. Given that X-Ray variability in the low/hard\u0000state of Cygnus X-1 is non-periodic, flux peaks were aggregated to suppress\u0000statistical fluctuations. We divided the temporal profiles of these aggregated\u0000flux peaks into seven time segments and evaluated the polarization for each\u0000segment. The results reveal that the polarization degree was 4.6%$pm$1.2 and\u00005.3%$pm$1.2 before and after the peak, respectively, but decreased to\u00003.4%$pm$1.1 and 2.7%$pm$1.1 in the segments including and immediately\u0000following the peak. Furthermore, the polarization angle exhibited a slight\u0000shift from approximately 30$^{circ}$ to $sim$40$^{circ}$ before and after\u0000the peak. These findings suggest that the accretion disk contracts with\u0000increasing X-Ray luminosity, and the closer proximity of the X-Ray emitting gas\u0000to the black hole may lead to reduced polarization.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"64 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947669","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}
The Big Fringe Telescope (BFT) is a facility concept under development for a next-generation, kilometer-scale optical interferometer. Observations over the past two decades from routinely operational facilities such as CHARA and VLTI have produced groundbreaking scientific results, reflecting the mature state of the techniques in optical interferometry. However, routine imaging of bright main sequence stars remains a surprisingly unexplored scientific realm. Additionally, the three-plus decade old technology infrastructure of these facilities leads to high operations & maintenance costs, and limits performance. We are developing the BFT, based upon robust, modern, commercially-available, automated technologies with low capital construction and O&M costs, in support of kilometer-scale optical interferometers that will open the door to regular `snapshot' imaging of main sequence stars. Focusing on extreme angular resolution for bright objects leads to substantial reductions in expected costs through use of COTS elements and simplified infrastructure.
{"title":"The Big Fringe Telescope","authors":"Gerard T. van Belle, Anders M. Jorgensen","doi":"arxiv-2408.01386","DOIUrl":"https://doi.org/arxiv-2408.01386","url":null,"abstract":"The Big Fringe Telescope (BFT) is a facility concept under development for a\u0000next-generation, kilometer-scale optical interferometer. Observations over the\u0000past two decades from routinely operational facilities such as CHARA and VLTI\u0000have produced groundbreaking scientific results, reflecting the mature state of\u0000the techniques in optical interferometry. However, routine imaging of bright\u0000main sequence stars remains a surprisingly unexplored scientific realm.\u0000Additionally, the three-plus decade old technology infrastructure of these\u0000facilities leads to high operations & maintenance costs, and limits\u0000performance. We are developing the BFT, based upon robust, modern,\u0000commercially-available, automated technologies with low capital construction\u0000and O&M costs, in support of kilometer-scale optical interferometers that will\u0000open the door to regular `snapshot' imaging of main sequence stars. Focusing on\u0000extreme angular resolution for bright objects leads to substantial reductions\u0000in expected costs through use of COTS elements and simplified infrastructure.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"63 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947665","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}
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