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EP250108a/SN 2025kg: A Broad-Line Type Ic Supernova Associated with a Fast X-ray Transient Showing Evidence of Extended CSM Interaction

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arXiv 2025年

作者： Srinivasaragavan, Gokul P. Hamidani, Hamid Schroeder, Genevieve Sarin, Nikhil Ho, Anna Y.Q. Piro, Anthony L. Cenko, S. Bradley Anand, Shreya Sollerman, Jesper Perley, Daniel A. Maeda, Keiichi O’Connor, Brendan Kuncarayakti, Hanindyo Miller, M. Coleman Ahumada, Tomás Vail, Jada Duffell, Paul Dastidar, Ranadeep Andreoni, Igor Bochenek, Aleksandra Brennan, Seán J. Carney, Jonathan Chen, Ping Freeburn, James Gal-Yam, Avishay Jacobson-Galán, Wynn Kasliwal, Mansi M. Li, Jiaxuan Li, Maggie L. Sravan, Niharika Warshofsky, Daniel E. Department of Astronomy University of Maryland College ParkMD20742 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Astrophysics Science Division NASA Goddard Space Flight Center 8800 Greenbelt Rd GreenbeltMD20771 United States Astronomical Institute Graduate School of Science Tohoku University Sendai980-8578 Japan Department of Astronomy Cornell University IthacaNY14853 United States Oskar Klein Centre for Cosmoparticle Physics Department of Physics Stockholm University AlbaNova StockholmSE-106 91 Sweden Nordita Stockholm University KTH Royal Institute of Technology Hannes Alfvéns vg 12 StockholmSE-106 91 Sweden The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Department of Astronomy The Oskar Klein Center Stockholm University AlbaNova Stockholm10691 Sweden Astrophysics Research Institute Liverpool John Moores University Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan McWilliams Center for Cosmology Department of Physics Carnegie Mellon University PittsburghPA15213 United States Tuorla Observatory Department of Physics and Astronomy University of Turku FI-20014 Finland Finnish Centre for Astronomy ESO FINCA University of Turku FI-20014 Finland Division of Physics Mathematics and Astronomy California Institute of Technology PasadenaCA91125 United States Department of Physics and Astronomy Purdue University 525 Northwestern Avenue West LafayetteIN47907 United States Department of Physics and Astronomy University of North Carolina at Chapel Hill Chapel HillNC27599-3255 United States

We present optical, radio, and X-ray observations of EP250108a/SN 2025kg, a broad-line Type Ic supernova (SN Ic-BL) accompanying an Einstein Probe (EP) fast X-ray transient (FXT) at z = 0.176. EP250108a/SN 2025kg possesses a double-peaked optical light curve and its spectrum transitions from a blue underlying continuum to a typical SN Ic-BL spectrum over time. We fit a radioactive decay model to the second peak of the optical light curve and find SN parameters that are consistent with the SNe Ic-BL population, while its X-ray and radio properties are consistent with those of low-luminosity GRB (LLGRB) 060218/SN 2006aj. We explore three scenarios to understand the system’s multi-wavelength emission – (a) SN ejecta interacting with an extended circumstellar medium (CSM), (b) the shocked cocoon of a collapsar-driven jet choked in its stellar envelope, and (c) the shocked cocoon of a collapsar-driven jet choked in an extended CSM. All three models can explain the optical light curve and are also consistent with the radio and X-ray observations. We favor models (a) and (c) because they self-consistently explain both the X-ray prompt emission and first optical peak, but we do not rule out model (b). From the properties of the first peak in models (a) and (c), we find evidence that EP250108a/SN 2025kg interacts with an extended CSM, and infer an envelope mass Me ∼ 0.1 M☉ and radius Re ∼ 4 × 1013 cm. EP250108a/SN 2025kg’s multi-wavelength properties make it a close analog to LLGRB 060218/SN 2006aj, and highlight the power of early follow-up observations in mapping the environments of massive stars prior to core collapse. Copyright © 2025, The Authors. All rights reserved.

关键词： Supernovae

Dark Matter Direct Detection with Quantum Dots

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arXiv 2022年

作者： Blanco, Carlos Essig, Rouven Fernandez-Serra, Marivi Ramani, Harikrishnan Slone, Oren Department of Physics Princeton University PrincetonNJ08544 United States Stockholm University The Oskar Klein Centre for Cosmoparticle Physics Alba Nova Stockholm10691 Sweden C. N. Yang Institute for Theoretical Physics Stony Brook University United States Department of Physics and Astronomy Stony Brook University Stony BrookNY11794-3800 United States Institute for Advanced Computational Science Stony Brook University Stony BrookNY11794-3800 United States Stanford Institute for Theoretical Physics Department of Physics Stanford University StanfordCA94305 United States Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY10003 United States

We propose using Quantum Dots as novel targets to probe sub-GeV dark matter-electron interactions. Quantum dots are nanocrystals of semiconducting material, which are commercially available, with gram-scale quantities suspended in liter-scale volumes of solvent. Quantum dots can be efficient scintillators, with near unity single-photon quantum yields, and their band-edge electronic properties are determined by their characteristic size, which can be precisely tuned. Examples include lead sulfide (PbS) and lead selenide (PbSe) quantum dots, which can be tuned to have sub-eV optical gaps. A dark-matter interaction can generate one or more electron-hole pairs (excitons), with the multi-exciton state decaying via the emission of two photons with an efficiency of about 10% of the single-photon quantum yield. An experimental setup using commercially available quantum dots and two photo-multiplier-tubes (PMTs) for detecting the coincident two-photon signal can already improve on existing dark-matter bounds, while using photodetectors with lower dark-count rates can improve on current constraints by orders of magnitude. © 2022, CC BY.

关键词： Lead compounds

From Halos to Galaxies. IX. Estimate of halo assembly history for SDSS galaxy groups

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arXiv 2024年

作者： Lyu, Cheqiu Peng, Yingjie Jing, Yipeng Yang, Xiaohu Ho, Luis C. Renzini, Alvio Zhao, Dingyi Mannucci, Filippo Mo, Houjun Wang, Kai Wang, Bitao Xu, Bingxiao Dou, Jing Gallazzi, Anna R. Gu, Qiusheng Maiolino, Roberto Wang, Enci Yuan, Feng Department of Astronomy School of Physics Peking University 5 Yiheyuan Road Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University 5 Yiheyuan Road Beijing100871 China Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Tsung-Dao Lee Institute Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai Jiao Tong University Shanghai200240 China INAF–Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy INAF–Osservatorio Astrofisico di Arcetri Largo Enrico Fermi 5 FirenzeI-50125 Italy Department of Astronomy University of Massachusetts AmherstMA01003 United States School of Astronomy and Space Science Nanjing University Nanjing210093 China Cavendish Laboratory University of Cambridge 19 J.J. Thomson Avenue CambridgeCB3 0HE United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China Center for Astronomy and Astrophysics Department of Physics Fudan University Shanghai200438 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China University of Chinese Academy of Sciences No. 19A Yuquan Road Beijing100049 China

The properties of the galaxies are tightly connected to their host halo mass and halo assembly history. Accurate measurement of the halo assembly history in observation is challenging but crucial to the understanding of galaxy formation and evolution. The stellar-to-halo mass ratio (M*/Mh) for the centrals has often been used to indicate the halo assembly time th,50 of the group, where th,50 is the lookback time at which a halo has assembled half of its present-day virial mass. Using mock data from the semi-analytic models, we find that M*/Mh shows a significant scatter with th,50, with a strong systematic difference between the group with a star-forming central (blue group) and passive central (red group). To improve the accuracy, we develop machine-learning models to estimate th,50 for galaxy groups using only observable quantities in the mocks. Since star-formation quenching will decouple the co-growth of the dark matter and baryon, we train our models separately for blue and red groups. Our models have successfully recovered th,50, within an accuracy of ~ 1.09 Gyr. With careful calibrations of individual observable quantities in the mocks with SDSS observations, we apply the trained models to the SDSS Yang et al. groups and derive the th,50 for each group for the first time. The derived SDSS th,50 distributions are in good agreement with that in the mocks, in particular for blue groups. The derived halo assembly history, together with the halo mass, make an important step forward in studying the halo-galaxy connections in observation. Copyright © 2024, The Authors. All rights reserved.

关键词： Galaxies

Compact representation of uncertainty in hierarchical clustering

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arXiv 2020年

作者： Greenberg, Craig S. Macaluso, Sebastian Monath, Nicholas Lee, Ji-Ah Flaherty, Patrick Cranmer, Kyle McGregor, Andrew McCallum, Andrew College of Information and Computer Sciences University of Massachusetts Amherst United States National Institute of Standards and Technology United States Center for Cosmology and Particle Physics & Center for Data Science New York University United States Department of Mathematics and Statistics University of Massachusetts Amherst United States

Hierarchical clustering is a fundamental task often used to discover meaningful structures in data, such as phylogenetic trees, taxonomies of concepts, subtypes of cancer, and cascades of particle decays in particle physics. When multiple hierarchical clusterings of the data are possible, it is useful to represent uncertainty in the clustering through various probabilistic quantities. Existing approaches represent uncertainty for a range of models;however, they only provide approximate inference. This paper presents dynamic-programming algorithms and proofs for exact inference in hierarchical clustering. We are able to compute the partition function, MAP hierarchical clustering, and marginal probabilities of sub-hierarchies and clusters. Our method supports a wide range of hierarchical models and only requires a cluster compatibility function. Rather than scaling with the number of hierarchical clusterings of n elements (ω(nn!/2n−1)), our approach runs in time and space proportional to the significantly smaller powerset of n. Despite still being large, these algorithms enable exact inference in small-data applications and are also interesting from a theoretical perspective. We demonstrate the utility of our method and compare its performance with respect to existing approximate methods. Copyright © 2020, The Authors. All rights reserved.

关键词： Genome

Erratum to: Constraining primordial black holes as dark matter using AMS-02 data

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The European Physical Journal C 2024年第8期84卷 1-1页

作者： Su, Bing-Yu Pan, Xu Wang, Guan-Sen Zu, Lei Yang, Yupeng Feng, Lei Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing China School of Astronomy and Space Science University of Science and Technology of China Hefei China School of Physics and Physical Engineering Qufu Normal University Qufu China Joint Center for Particle Nuclear Physics and Cosmology Nanjing University-Purple Mountain Observatory Nanjing China

MoEDAL search in the CMS beam pipe for magnetic monopoles produced via the Schwinger effect

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arXiv 2024年

作者： Acharya, B. Alexandre, J. Behera, S.C. Benes, P. Bergmann, B. Bertolucci, S. Bevan, A. Brancaccio, R. Branzas, H. Burian, P. Campbell, M. Cecchini, S. Cho, Y.M. de Montigny, M. De Roeck, A. Ellis, J.R. Fairbairn, M. Felea, D. Frank, M. Gould, O. Hays, J. Hirt, A.M. Ho, D.L.-J. Hung, P.Q. Janecek, J. Kalliokoski, M. Lacarrère, D.H. Leroy, C. Levi, G. Margiotta, A. Maselek, R. Maulik, A. Mauri, N. Mavromatos, N.E. Millward, L. Mitsou, V.A. Musumeci, E. Ostrovskiy, I. Ouimet, P.-P. Papavassiliou, J. Patrizii, L. Pavalaş, G.E. Pinfold, J.L. Popa, L.A. Popa, V. Pozzato, M. Pospisil, S. Rajantie, A. Ruiz de Austri, R. Sahnoun, Z. Sakellariadou, M. Sakurai, K. Sarkar, S. Semenoff, G. Shaa, A. Sirri, G. Sliwa, K. Soluk, R. Spurio, M. Staelens, M. Suk, M. Tenti, M. Togo, V. Tuszynski, J.A. Upreti, A. Vento, V. Vives, O. Theoretical Particle Physics & Cosmology Group Physics Dept. King's College London United Kingdom Department of Physics and Astronomy University of Alabama TuscaloosaAL United States IEAP Czech Technical University Prague Czech Republic INFN Section of Bologna Bologna Italy School of Physics and Astronomy Queen Mary University of London United Kingdom INFN Section of Bologna Department of Physics & Astronomy University of Bologna Italy Institute of Space Science Bucharest - Magurele Romania Experimental Physics Department CERN Geneva Switzerland Center for Quantum Spacetime Sogang University Seoul Korea Republic of Physics Department University of Alberta EdmontonAB Canada Theoretical Physics Department CERN Geneva Switzerland Department of Physics Concordia University MontrealQC Canada University of Nottingham Nottingham United Kingdom Department of Earth Sciences Swiss Federal Institute of Technology Zurich Switzerland Department of Physics Imperial College London United Kingdom Department of Physics University of Virginia CharlottesvilleVA United States Helsinki Institute of Physics University of Helsinki Helsinki Finland Departement de Physique Universite de Montreal Quebec Canada Institute of Theoretical Physics University of Warsaw Warsaw Poland IFIC Universitat de Valencia - CSIC Valencia Spain Physics Department University of Regina ReginaSK Canada Department of Physics University of British Columbia VancouverBC Canada Department of Physics and Astronomy Tufts University MedfordMA United States Int. Centre for Theoretical Physics Trieste Italy Department of Physics School of Applied Mathematical and Physical Sciences National Technical University of Athens Athens Greece

We report on a search for magnetic monopoles (MMs) produced in ultraperipheral Pb-Pb collisions during Run-1 of the LHC. The beam pipe surrounding the interaction region of the CMS experiment was exposed to 184.07 µb−1 of Pb-Pb collisions at 2.76 TeV center-of-mass energy per collision in December 2011, before being removed in 2013. It was scanned by the MoEDAL experiment using a SQUID magnetometer to search for trapped MMs. No MM signal was observed. The two distinctive features of this search are the use of a trapping volume very close to the collision point and ultrahigh magnetic fields generated during the heavy-ion run that could produce MMs via the Schwinger effect. These two advantages allowed setting the first reliable, world-leading mass limits on MMs with high magnetic charge. In particular, the established limits are the strongest available in the range between 2 and 45 Dirac units, excluding MMs with masses of up to 80 GeV at 95% confidence level. Copyright © 2024, The Authors. All rights reserved.

关键词： Heavy ions

Hunting the gamma-ray emission from Fast Radio Burst with Fermi-LAT

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arXiv 2023年

作者： Principe, Giacomo Lalla, Niccolò Di Venere, Leonardo Di Negro, Michela Longo, Francesco Universitá di Trieste Dipartimento di Fisica TriesteI-34127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Trieste TriesteI-34127 Italy Istituto Nazionale di Astrofisica - Istituto di Radioastronomia BolognaI-40129 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy University of Maryland Baltimore County BaltimoreMD21250 United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA/GSFC GreenbeltMD20771 United States

Fast radio bursts (FRBs) are one of the most exciting new mysteries of astrophysics. Their origin is still unknown, but recent observations seem to link them to soft gamma repeaters and, in particular, to magnetar giant flares (MGFs). The recent detection of a MGF at GeV energies by the Fermi Large Area Telescope (LAT) motivated the search for GeV counterparts to the >100 currently known FRBs. To date, none of these has a known gamma-ray counterpart. Taking advantage of more than 12 years of Fermi-LAT data, we perform a search for gamma-ray emission from almost all the reported repeating and non-repeating FRBs. We analyze on different time scales the Fermi-LAT data for each individual source separately and perform a cumulative analysis on the repeating ones. In addition, we perform the first stacking analysis at GeV energies of this class of sources in order to constrain the gamma-ray properties of the FRBs. The stacking analysis is a powerful method that allows for a possible detection from below-threshold FRBs providing important information on these objects. In this proceeding we present preliminary results of our study and we discuss their implications for the predictions of gamma-ray emission from this class of sources. © 2023, CC BY.

关键词： Gamma rays

Application of the nitrogen laser calibration system in LHAASO-WFCTA

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Application of the nitrogen laser calibration system in LHAA...

37th International Cosmic Ray Conference, ICRC 2021

作者： Chen, Long Li, Xin Ge, Lisi Liu, Hu Sun, Qinning Wang, Yang Xia, Junji Zhu, Fengrong Zhang, Yong Cao, Zhen Aharonian, F. An, Q. Axikegu Bai, L.X. Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Cai, H. Cai, J.T. Cao, Zhe Chang, J. Chang, J.F. Chen, B.M. Chen, E.S. Chen, J. Chen, Liang Chen, Liang Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, X.L. Chen, Y. Cheng, N. Cheng, Y.D. Cui, S.W. Cui, X.H. Cui, Y.D. D’Ettorre Piazzoli, B. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu della Volpe, D. Dong, X.J. Duan, K.K. Fan, J.H. Fan, Y.Z. Fan, Z.X. Fang, J. Fang, K. Feng, C.F. Feng, L. Feng, S.H. Feng, Y.L. Gao, B. Gao, C.D. Gao, L.Q. Gao, Q. Gao, W. Ge, M.M. Geng, L.S. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, J.G. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. He, H.H. He, H.N. He, J.C. He, S.L. He, X.B. He, Y. Heller, M. Hor, Y.K. Hou, C. Hu, H.B. Hu, S. Hu, S.C. Hu, X.J. Huang, D.H. Huang, Q.L. Huang, W.H. Huang, X.T. Huang, X.Y. Huang, Z.C. Ji, F. Ji, X.L. Jia, H.Y. Jiang, K. Jiang, Z.J. Jin, C. Ke, T. Kuleshov, D. Levochkin, K. Li, B.B. Li, Cheng Li, Cong Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, K. Li, W.L. Li, X.R. Li, Xin Li, Xin Li, Y. Li, Y.Z. Li, Zhe Li, Zhuo Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, D. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, J.S. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Liu, Z.X. Long, W.J. Lu, R. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Masood, A. Min, Z. Mitthumsiri, W. Montaruli, T. Nan, Y.C. Pang, B.Y. Pattarakijwanich, P. Pei, Z.Y. Qi, M.Y. Qi, Y.Q. Qiao, B.Q. Qin, J.J. Ruffolo, D. Rulev, V. Sáiz, A. Shao, L. Shchegolev, O. Sheng, X.D. Shi, J.Y. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Sun, Q.N. Sun, X.N. School of Physical Science and Technology Southwest Jiaotong University No.111 North Section 1 Second Ring Road Chengdu China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan RoadShijingshan District Beijing China Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu China Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin Ireland Max-Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg69029 Germany State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Anhui Hefei230026 China School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Sichuan Chengdu610031 China College of Physics Sichuan University Sichuan Chengdu610065 China School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210023 China Center for Astrophysics Guangzhou University Guangdong Guangzhou510006 China School of Physics and Technology Wuhan University Hubei Wuhan430072 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Hebei Normal University Hebei Shijiazhuang050024 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Ministry of Education Tibet Lhasa850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Sun Yat-sen University Guangdong Zhuhai519000 China Dipartimento di Fisica dell’Università di Napoli `‘Federico II" Complesso Universitario di Monte Sant’Angelo via Cinthia Napoli80126 Italy Sc

The nitrogen laser calibration system for the Wide Field of View Cherenkov Telescope Array (WFCTA) is one of the most important components of the Large High Altitude Air Shower Observatory (LHAASO). This calibration system is composed of three parts, including a high-precision 3D lifting and rotating platform (HiRoP), a nitrogen laser and the wide field of view Cherenkov telescope prototypes. The accuracy of the HiRoP is of great importance for the precise calibration of WFCTA since it controls the laser beam’s pointing direction. A home-made HiRoP was introduced and the measurements implies that the angular and lifting accuracies of HiRoP are better than 0.003° and 0.075 mm, respectively. Furthermore, the pulse energy stability of the nitrogen laser beam is another remarkably important factor. The nitrogen laser system with a wavelength of 337.1 nm located in a high-precision temperature and humidity’s controlling container, resulting in a pulse energy fluctuation less than 3 percent. Besides, the method of a standard zero point verification is employed to improve the long-term accuracy of the beam pointing direction. © Copyright owned by the author(s).

关键词： Laser beams

Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation

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arXiv 2024年

作者： Kanodia, Shubham Cañas, Caleb I. Mahadevan, Suvrath Ford, Eric B. Helled, Ravit Anderson, Dana E. Boss, Alan Cochran, William D. Delamer, Megan Han, Te Libby-Roberts, Jessica E. Lin, Andrea S.J. Müller, Simon Robertson, Paul Stefánsson, Guðmundur Teske, Johanna Earth and Planets Laboratory Carnegie Institution for Science 5241 Broad Branch Road NW WashingtonDC20015 United States NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Department of Astronomy & Astrophysics 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Center for Exoplanets and Habitable Worlds 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Center for Astrostatistics 525 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Center for Theoretical Astrophysics & Cosmology University of Zurich Winterthurerstr. 190 ZurichCH-8057 Switzerland McDonald Observatory Department of Astronomy The University of Texas Austin United States Center for Planetary Systems Habitability The University of Texas Austin United States Department of Physics & Astronomy The University of California Irvine IrvineCA92697 United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08540 United States

Recent discoveries of transiting giant exoplanets around M-dwarf stars (GEMS), aided by the all-sky coverage of TESS, are starting to stretch theories of planet formation through the core-accretion scenario. Recent upper limits on their occurrence suggest that they decrease with lower stellar masses, with fewer GEMS around lower-mass stars compared to solar-type. In this paper, we discuss existing GEMS both through confirmed planets, as well as protoplanetary disk observations, and a combination of tests to reconcile these with theoretical predictions. We then introduce the Searching for GEMS survey, where we utilize multi-dimensional nonparameteric statistics to simulate hypothetical survey scenarios to predict the required sample size of transiting GEMS with mass measurements to robustly compare their bulk-density with canonical hot-Jupiters orbiting FGK stars. Our Monte-Carlo simulations predict that a robust comparison requires about 40 transiting GEMS (compared to the existing sample of ∼ 15) with 5-σ mass measurements. Furthermore, we discuss the limitations of existing occurrence estimates for GEMS, and provide a brief description of our planned systematic search to improve the occurrence rate estimates for GEMS. © 2024, CC BY.

关键词： Monte Carlo methods