Nature Astronomy最新文献

{"title":"Future astrophysics funding requires both ambition and accountability","authors":"Thomas H. Zurbuchen","doi":"10.1038/s41550-025-02656-x","DOIUrl":"10.1038/s41550-025-02656-x","url":null,"abstract":"Current funding challenges in astrophysics present an opportunity to secure its future through ambition, accountability and readiness for a world where breakthrough science is increasingly done in big teams.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"9 9","pages":"1282-1283"},"PeriodicalIF":14.3,"publicationDate":"2025-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145032171","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Catching ΛCDM in the act","authors":"Themiya Nanayakkara","doi":"10.1038/s41550-025-02662-z","DOIUrl":"https://doi.org/10.1038/s41550-025-02662-z","url":null,"abstract":"Two new studies provide potential evidence for the formation of the unexpectedly bright and massive galaxy populations that have been detected with JWST in the early Universe.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"39 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145017448","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A complete measurement of a black-hole recoil through higher-order gravitational-wave modes","authors":"Juan Calderón Bustillo, Samson H. W. Leong, Koustav Chandra","doi":"10.1038/s41550-025-02632-5","DOIUrl":"https://doi.org/10.1038/s41550-025-02632-5","url":null,"abstract":"<p>General relativity predicts that gravitational waves (GWs) carry linear momentum. Consequently, the remnant black hole of a black-hole merger can inherit a recoil velocity or ‘kick’ of crucial implications in, for example, black-hole formation scenarios. While the kick magnitude is determined by the mass ratio and spins of the source, estimating its direction requires a measurement of the two orientation angles of the source. While the orbital inclination angle is commonly reported in GW observations, the scientific potential of the azimuthal one has not been exploited so far. Here we show how the presence of more than one GW emission mode allows one to constrain this angle and, consequently, the kick direction of a real GW event. We analyse the GW190412 signal, which contains higher-order modes, with a numerical relativity surrogate waveform model for black-hole mergers. We rule out kick magnitudes below the typical escape velocity of dense globular clusters <i>v</i>_esc ≈ 50 km s⁻¹ with a Bayes factor of ~21 (or ~95% probability). The kick forms angles <span>({theta }_{{mathrm{KL}}}^{-100M}=3{2}_{-14}^{+35},text{deg})</span> with the orbital angular momentum defined at a reference time <i>t</i>_ref = −100 <i>M</i> before merger (with <i>M</i> denoting the system mass in geometric units), <span>({theta }_{{{KN}}}=4{4}_{-17}^{+19},text{deg})</span> with the line of sight and <span>({phi }_{{{KN}}}^{-100M}=6{9}_{-38}^{+33},text{deg})</span> with the projection of the latter onto the former, all quoted at a 90% credible level. We anticipate that complete characterization of black-hole recoils will aid in evaluating candidate multi-messenger observations of black-hole mergers in active galactic nuclei, by testing the consistency of observed signals with proposed electromagnetic emission mechanisms.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"87 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145017596","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Different arrival times of CM- and CI-like bodies from the outer Solar System in the asteroid belt","authors":"Sarah E. Anderson, Pierre Vernazza, Miroslav Brož","doi":"10.1038/s41550-025-02635-2","DOIUrl":"https://doi.org/10.1038/s41550-025-02635-2","url":null,"abstract":"<p>Understanding the birthplace of meteoritic materials is critical for reconstructing the early Solar System and contextualizing recent sample-return missions. Here, we use <i>N</i>-body simulations to investigate the influence of giant-planet growth and inward type I migration on the delivery of outer Solar System bodies to the asteroid belt. We find that the radial distribution of planetesimals reflects that of the gas in the disk at the moment of implantation. Since chondrule-rich CM- and chondrule-poor CI-like bodies with diameters greater than 100 km have different radial distributions, they must have been implanted at different times. CM-like bodies probably originate from the Saturn formation region and were implanted by aerodynamic drag into the belt during Saturn’s growth phase, while CI- and comet-like bodies probably formed in the primordial trans-Uranian disk and were scattered inwards by the formation and migration of Uranus and Neptune driven by remaining planetesimals. Our results support a formation zone for chondrules interior to the ice giants (≤10 <span>au</span>), and suggest that CM-like bodies contributed to the water budget of the telluric planets.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"68 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145008943","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The rise and fall of massive galaxies in the early Universe","authors":"Francesco D’Eugenio","doi":"10.1038/s41550-025-02658-9","DOIUrl":"https://doi.org/10.1038/s41550-025-02658-9","url":null,"abstract":"An analysis of two post-starburst galaxies at high redshift indicates the presence of ongoing feedback between the stellar material and the supermassive black hole.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"33 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144995558","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A collisional history of the L chondrite parent bodies","authors":"Marine Ciocco, Mathieu Roskosz, Béatrice Doisneau, Etienne Deloule, Guillaume Fiquet, Marco Delbo, Matthieu Gounelle","doi":"10.1038/s41550-025-02615-6","DOIUrl":"https://doi.org/10.1038/s41550-025-02615-6","url":null,"abstract":"<p>L chondrites are some of the most common meteorites retrieved on Earth. Their Ar–Ar collision ages indicate a major disruption of their parent body ~470 million years ago (Ma), which was followed by an intense meteorite shower on Earth that is linked to the Ordovician biological crisis. However, recent but previously scarce chronological and geochemical data on a few L chondrites hint at a more complex evolution of the parent body than a single, one-stage 470 Ma break-up. Here we conducted a unique coordinated mineralogical and geochronological study on eight shocked L chondrites, which showed a wide distribution of collisional ages at 4,500, 4,470, ~700, 470 and ~10 Ma. The lower-limit sizes of the parent body derived from shock timescales, combined with the orbital parameters and the aforementioned ages of the meteorites, indicate a complex collisional cascade endured by the parent body of the L chondrites, pointing towards several L chondrite sources in the asteroid main belt, namely, the Nysa–Polana, Juno, Gefion 2 and potentially Massalia asteroid families.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"30 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144995559","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Evidence for polycyclic aromatic hydrocarbons detected in sulfates at Jezero crater by the Perseverance rover","authors":"Teresa Fornaro, Sunanda Sharma, Ryan S. Jakubek, Giovanni Poggiali, John Robert Brucato, Rohit Bhartia, Andrew Steele, Ashley E. Murphy, Michael M. Tice, Mitchell D. Schulte, Kevin P. Hand, Marc D. Fries, William J. Abbey, Andrew Alberini, Daniela Alvarado-Jiménez, Kathleen C. Benison, Eve L. Berger, Sole Biancalani, Adrian J. Brown, Adrian P. Broz, Wayne P. Buckley, Denise K. Buckner, Aaron S. Burton, Sergei V. Bykov, Emily L. Cardarelli, Edward A. Cloutis, Stephanie A. Connell, Cristina Garcia-Florentino, Felipe Gómez, Nikole C. Haney, Carina Lee, Valeria Lino, Paola Manini, Francis M. McCubbin, Michelle E. Minitti, Richard V. Morris, Yu Yu Phua, Nicolas Randazzo, Joseph Razzell Hollis, Francesco Renzi, Sandra Siljeström, Justin I. Simon, Anushree Srivastava, Nicola Tasinato, Kyle Uckert, Roger C. Wiens, Amy J. Williams","doi":"10.1038/s41550-025-02638-z","DOIUrl":"https://doi.org/10.1038/s41550-025-02638-z","url":null,"abstract":"<p>The search for organic molecules on Mars is central to understanding the planet’s past habitability and potential for ancient life. Although organic molecules have previously been detected on Mars, their nature, origin and preservation mechanisms remain debated. On the floor of the Jezero crater—an ancient delta–lake system on Mars—the Perseverance rover detected Raman features that may be due to organic compounds spatially associated with sulfates, although their origin is uncertain. Here we report the detection of similar Raman features in the Jezero fan top and attribute them to polycyclic aromatic hydrocarbons based on comparisons with laboratory data. We propose that these polycyclic aromatic hydrocarbons may have formed through endogenous igneous processes and were subsequently preserved by sulfate precipitation. These findings align with previous studies on Martian meteorites and at Gale crater, underscoring the role of sulfates in preserving organic matter on Mars. Returning these samples to Earth would be key to assess their astrobiological relevance.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"24 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144987480","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A high fraction of close massive binary stars at low metallicity","authors":"H. Sana,&nbsp;T. Shenar,&nbsp;J. Bodensteiner,&nbsp;N. Britavskiy,&nbsp;N. Langer,&nbsp;D. J. Lennon,&nbsp;L. Mahy,&nbsp;I. Mandel,&nbsp;S. E. de Mink,&nbsp;L. R. Patrick,&nbsp;J. I. Villaseñor,&nbsp;M. Dirickx,&nbsp;M. Abdul-Masih,&nbsp;L. A. Almeida,&nbsp;F. Backs,&nbsp;S. R. Berlanas,&nbsp;M. Bernini-Peron,&nbsp;D. M. Bowman,&nbsp;V. A. Bronner,&nbsp;P. A. Crowther,&nbsp;K. Deshmukh,&nbsp;C. J. Evans,&nbsp;M. Fabry,&nbsp;M. Gieles,&nbsp;A. Gilkis,&nbsp;G. González-Torà,&nbsp;G. Gräfener,&nbsp;Y. Götberg,&nbsp;C. Hawcroft,&nbsp;V. Hénault-Brunet,&nbsp;A. Herrero,&nbsp;G. Holgado,&nbsp;R. G. Izzard,&nbsp;A. de Koter,&nbsp;S. Janssens,&nbsp;C. Johnston,&nbsp;J. Josiek,&nbsp;S. Justham,&nbsp;V. M. Kalari,&nbsp;J. Klencki,&nbsp;J. Kubát,&nbsp;B. Kubátová,&nbsp;R. R. Lefever,&nbsp;J. Th. van Loon,&nbsp;B. Ludwig,&nbsp;J. Mackey,&nbsp;J. Maíz Apellániz,&nbsp;G. Maravelias,&nbsp;P. Marchant,&nbsp;T. Mazeh,&nbsp;A. Menon,&nbsp;M. Moe,&nbsp;F. Najarro,&nbsp;L. M. Oskinova,&nbsp;R. Ovadia,&nbsp;D. Pauli,&nbsp;M. Pawlak,&nbsp;V. Ramachandran,&nbsp;M. Renzo,&nbsp;D. F. Rocha,&nbsp;A. A. C. Sander,&nbsp;F. R. N. Schneider,&nbsp;A. Schootemeijer,&nbsp;E. C. Schösser,&nbsp;C. Schürmann,&nbsp;K. Sen,&nbsp;S. Shahaf,&nbsp;S. Simón-Díaz,&nbsp;L. A. C. van Son,&nbsp;M. Stoop,&nbsp;S. Toonen,&nbsp;F. Tramper,&nbsp;R. Valli,&nbsp;A. Vigna-Gómez,&nbsp;J. S. Vink,&nbsp;C. Wang,&nbsp;R. Willcox","doi":"10.1038/s41550-025-02610-x","DOIUrl":"10.1038/s41550-025-02610-x","url":null,"abstract":"At high metallicity, a majority of massive stars have at least one close stellar companion. The evolution of such binaries is subject to strong interaction processes, which heavily impact the characteristics of their life-ending supernova and compact remnants. For the low-metallicity environments of high-redshift galaxies, constraints on the multiplicity properties of massive stars over the separation range leading to binary interaction are crucially missing. Here we show that the presence of massive stars in close binaries is ubiquitous, even at low metallicity. Using the Very Large Telescope, we obtained multi-epoch radial velocity measurements of a representative sample of 139 massive O-type stars across the Small Magellanic Cloud, which has a metal content of about one-fifth of the solar value. We find that 45% of them show radial velocity variations that demonstrate that they are members of close binary systems, and predominantly have orbital periods shorter than 1 year. Correcting for observational biases indicates that at least $$7{0}_{-6}^{+11}%$$ of the O stars in our sample are in close binaries, and that at least $$6{8}_{-8}^{+7}%$$ of all O stars interact with a companion star during their lifetime. We found no evidence supporting a statistically significant trend of the multiplicity properties with metallicity. Our results indicate that multiplicity and binary interactions govern the evolution of massive stars and determine their cosmic feedback and explosive fates. The analysis of radial velocity variations of O-type stars in the Small Magellanic Cloud reveals a large fraction of close binaries, suggesting that binary physics also plays a prominent role in the low-metallicity environment of the distant Universe.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"9 9","pages":"1337-1346"},"PeriodicalIF":14.3,"publicationDate":"2025-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144928222","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Quo vadis galaxy evolution? A conference to reflect, and to chart the course of extragalactic astronomy","authors":"Dominika Wylezalek,&nbsp;Eduardo Bañados","doi":"10.1038/s41550-025-02650-3","DOIUrl":"10.1038/s41550-025-02650-3","url":null,"abstract":"A conference at the International Academic Forum of Heidelberg University, Germany, brought together 80 experts across various disciplines to recount recent breakthroughs in extragalactic astrophysics and ask, where are you going, galaxy evolution?","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"9 9","pages":"1290-1291"},"PeriodicalIF":14.3,"publicationDate":"2025-08-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144906004","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Chemical evolution imprints in the rare isotopes of nearby M dwarfs","authors":"Darío González Picos, Ignas Snellen, Sam de Regt","doi":"10.1038/s41550-025-02641-4","DOIUrl":"https://doi.org/10.1038/s41550-025-02641-4","url":null,"abstract":"<p>Elements heavier than hydrogen and helium, collectively termed metals, were created inside stars and dispersed through space at the final stages of stellar evolution. The relative amounts of different isotopes (variants of the same element with different masses) in stellar atmospheres provide clues about how our galaxy evolved chemically over billions of years. M dwarfs are small, cool, long-lived stars that comprise three-quarters of all stars in our galaxy. Their spectra exhibit rich fingerprints of their composition, making them potential tracers of chemical evolution. Here we measure rare carbon and oxygen isotopes in 32 nearby M dwarfs spanning a range of metallicities using high-resolution infrared spectroscopy. We find that stars with higher metal content have lower ¹²C/¹³C ratios, indicating they formed from material progressively enriched in ¹³C over time. This pattern is consistent with models where novae eruptions contributed significant amounts of ¹³C to the interstellar medium over the past few billion years. Our measurements of the ¹⁶O/¹⁸O ratio align with theoretical predictions and indicate that metal-rich stars attain significantly lower ¹⁶O/¹⁸O ratios than the Sun. These results establish M dwarfs as tracers of chemical evolution throughout cosmic history.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"51 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-08-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144900150","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}