The Astrophysical Journal最新文献

{"title":"COSMOS-Web: The Role of Galaxy Interactions and Disk Instabilities in Producing Starbursts at z < 4","authors":"Andreas L. Faisst, Lilan Yang, M. Brinch, C. M. Casey, N. Chartab, M. Dessauges-Zavadsky, N. E. Drakos, S. Gillman, G. Gozaliasl, C. C. Hayward, O. Ilbert, P. Jablonka, A. Kaminsky, J. S. Kartaltepe, A. M. Koekemoer, V. Kokorev, E. Lambrides, D. Liu, C. Maraston, C. L. Martin, A. Renzini, B. E. Robertson, D. B. Sanders, Z. Sattari, N. Scoville, C. M. Urry, A. P. Vijayan, J. R. Weaver, H. B. Akins, N. Allen, R. C. Arango-Toro, O. R. Cooper, M. Franco, F. Gentile, S. Harish, M. Hirschmann, A. A. Khostovan, C. Laigle, R. L. Larson, M. Lee, Z. Liu, A. S. Long, G. Magdis, R. Massey, H. J. McCracken, J. McKinney, L. Paquereau, J. Rhodes, R. M. Rich, M. Shuntov, J. D. Silverman, M. Talia, S. Toft, J. A. Zavala","doi":"10.3847/1538-4357/ada566","DOIUrl":"https://doi.org/10.3847/1538-4357/ada566","url":null,"abstract":"We study of the role of galaxy–galaxy interactions and disk instabilities in producing starburst activity in galaxies out to <italic toggle=\"yes\">z</italic> = 4. For this, we use a sample of 387 galaxies with robust total star formation rate measurements from Herschel, gas masses from the Atacama Large Millimeter/submillimeter Array, stellar masses and redshifts from multiband photometry, and JWST/NIRCam rest-frame optical imaging. Using mass-controlled samples, we find an increased fraction of interacting galaxies in the starburst regime at all redshifts out to <italic toggle=\"yes\">z</italic> = 4. This increase correlates with star formation efficiency (SFE) but not with gas fraction. However, the correlation is weak (and only significant out to <italic toggle=\"yes\">z</italic> = 2), which could be explained by the short duration of SFE increase during interaction. In addition, we find that isolated disk galaxies make up a significant fraction of the starburst population. The fraction of such galaxies with star-forming clumps (“clumpy disks”) is significantly increased compared to the main-sequence disk population. Furthermore, this fraction directly correlates with SFE. This is direct observational evidence for a long-term increase of SFE maintained due to disk instabilities, contributing to the majority of starburst galaxies in our sample and hence to substantial mass growth in these systems. This result could also be of importance for explaining the growth of the most massive galaxies at <italic toggle=\"yes\">z </italic>&gt; 6.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"42 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417423","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}

{"title":"Observations of the X-Ray Millihertz Quasiperiodic Oscillations in Hercules X-1","authors":"Wen Yang, Wei Wang","doi":"10.3847/1538-4357/adae8f","DOIUrl":"https://doi.org/10.3847/1538-4357/adae8f","url":null,"abstract":"With a systematic timing investigation of the persistent X-ray binary pulsar Her X-1 based on a large number of Insight-HXMT observations between 2017 and 2019, we confirm the presence of X-ray millihertz quasiperiodic oscillations (mHz QPOs) at ∼0.01 Hz. By applying wavelet analysis in our data analysis procedures, we first identify ∼0.005–0.009 Hz QPOs coexisting with the ∼0.01 Hz QPOs. Wavelet analysis suggests that these QPO features show transient behaviors, that the frequencies of mHz QPOs evolve in short timescales. There exists a positive relation between QPO centroid frequency (from ∼0.005 to 0.009 Hz) and X-ray luminosity, while the 10 mHz QPO frequencies remain nearly constant for different luminosities, which suggests different physical mechanisms for the two types of mHz QPOs. The 10 mHz QPOs in both X-ray and UV bands would have the same origin related to the beat frequency where the Alfvén radius is close to the corotation radius, and the 5 mHz QPOs may originate from magnetic disk precession.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"31 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417432","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}

{"title":"Energy Extraction from a Black Hole by a Strongly Magnetized Thin Accretion Disk","authors":"Prasun Dhang, Jason Dexter, Mitchell C. Begelman","doi":"10.3847/1538-4357/ada76e","DOIUrl":"https://doi.org/10.3847/1538-4357/ada76e","url":null,"abstract":"The presence of a strong, large-scale magnetic field in an accretion flow leads to the extraction of the rotational energy of the black hole (BH) through the Blandford–Znajek (BZ) process, believed to power relativistic jets in various astrophysical sources. We study rotational energy extraction from a BH surrounded by a highly magnetized thin disk by performing a set of 3D global GRMHD simulations. We find that the saturated flux threading the BH has a weaker dependence on BH spin, compared to highly magnetized hot (geometrically thick) accretion flows. Also, we find that only a fraction (10%–70%) of the extracted BZ power is channeled into the jet, depending on the spin parameter. The remaining energy is potentially used to launch winds or contribute to the radiative output of the disk or corona. Our simulations reveal that the presence of a strong magnetic field enhances the radiative efficiency of the disk, making it more luminous than its weakly magnetized counterpart or the standard disk model. We attribute this excess luminosity primarily to the enhanced magnetic dissipation in the intra-ISCO region. Our findings have implications for understanding X-ray corona formation and BH spin measurements, and interpreting BH transient phenomena.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143418370","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}

{"title":"Swift-BAT GUANO Follow-up of Gravitational-wave Triggers in the Third LIGO–Virgo–KAGRA Observing Run","authors":"Gayathri Raman, Samuele Ronchini, James Delaunay, Aaron Tohuvavohu, Jamie A. Kennea, Tyler Parsotan, Elena Ambrosi, Maria Grazia Bernardini, Sergio Campana, Giancarlo Cusumano, Antonino D’Aì, Paolo D’Avanzo, Valerio D’Elia, Massimiliano De Pasquale, Simone Dichiara, Phil Evans, Dieter Hartmann, Paul Kuin, Andrea Melandri, Paul O’Brien, Julian P. Osborne, Kim Page, David M. Palmer, Boris Sbarufatti, Gianpiero Tagliaferri, Eleonora Troja, The LIGO Scientific Collaboration, The Virgo Collaboration, and The KAGRA Collaboration, A. G. Abac, R. Abbott, H. Abe, I. Abouelfettouh, F. Acernese, K. Ackley, C. Adamcewicz, S. Adhicary, N. Adhikari, R. X. Adhikari, V. K. Adkins, V. B. Adya, C. Affeldt, D. Agarwal, M. Agathos, O. D. Aguiar, I. Aguilar, L. Aiello, A. Ain, T. Akutsu, S. Albanesi, R. A. Alfaidi, A. Al-Jodah, C. Alléné, A. Allocca, S. Al-Shammari, P. A. Altin, S. Alvarez-Lopez, A. Amato, L. Amez-Droz, A. Amorosi, C. Amra, S. Anand, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, T. Andrade, N. Andres, M. Andrés-Carcasona, T. Andrić, J. Anglin, S. Ansoldi, J. M. Antelis, S. Antier, M. Aoumi, E. Z. Appavuravther, S. Appert, S. K. Apple, K. Arai, A. Araya, M. C. Araya, J. S. Areeda, N. Aritomi, F. Armato, N. Arnaud, M. Arogeti, S. M. Aronson, G. Ashton, Y. Aso, M. Assiduo, S. Assis de Souza Melo, S. M. Aston, P. Astone, F. Aubin, K. AultONeal, G. Avallone, S. Babak, F. Badaracco, C. Badger, S. Bae, S. Bagnasco, E. Bagui, Y. Bai, J. G. Baier, R. Bajpai, T. Baka, M. Ball, G. Ballardin, S. W. Ballmer, S. Banagiri, B. Banerjee, D. Bankar, P. Baral, J. C. Barayoga, B. C. Barish, D. Barker, P. Barneo, F. Barone, B. Barr, L. Barsotti, M. Barsuglia, D. Barta, S. D. Barthelmy, M. A. Barton, I. Bartos, S. Basak, A. Basalaev, R. Bassiri, A. Basti, M. Bawaj, P. Baxi, J. C. Bayley, A. C. Baylor, M. Bazzan, B. Bécsy, V. M. Bedakihale, F. Beirnaert, M. Bejger, D. Belardinelli, A. S. Bell, V. Benedetto, D. Beniwal, W. Benoit, J. D. Bentley, M. Ben Yaala, S. Bera, M. Berbel, F. Bergamin, B. K. Berger, S. Bernuzzi, M. Beroiz, C. P. L. Berry, D. Bersanetti, A. Bertolini, J. Betzwieser, D. Beveridge, N. Bevins, R. Bhandare, U. Bhardwaj, R. Bhatt, D. Bhattacharjee, S. Bhaumik, S. Bhowmick, A. Bianchi, I. A. Bilenko, G. Billingsley, A. Binetti, S. Bini, O. Birnholtz, S. Biscoveanu, A. Bisht, M. Bitossi, M.-A. Bizouard, J. K. Blackburn, C. D. Blair, D. G. Blair, F. Bobba, N. Bode, G. Bogaert, G. Boileau, M. Boldrini, G. N. Bolingbroke, A. Bolliand, L. D. Bonavena, R. Bondarescu, F. Bondu, E. Bonilla, M. S. Bonilla, A. Bonino, R. Bonnand, P. Booker, A. Borchers, V. Boschi, S. Bose, V. Bossilkov, V. Boudart, A. Boumerdassi, A. Bozzi, C. Bradaschia, P. R. Brady, M. Braglia, A. Branch, M. Branchesi, M. Breschi, T. Briant, A. Brillet, M. Brinkmann, P. Brockill, E. Brockmueller, A. F. Brooks, D. D. Brown, M. L. Brozzetti, S. Brunett, G. Bruno, R. Bruntz, J. Bryant, F. Bucci, J. Buchanan, O. Bulashenko, T. Bulik, H. J. Bulten, A. Buonanno, K. Burtnyk, R. Buscicchio, D. Buskulic, C. Buy, R. L. Byer, G. S. Cabourn Davies, G. Cabras, R. Cabrita, L. Cadonati, G. Cagnoli, C. Cahillane, J. Calderón Bustillo, J. D. Callaghan, T. A. Callister, E. Calloni, J. B. Camp, M. Canepa, G. Caneva Santoro, M. Cannavacciuolo, K. C. Cannon, H. Cao, Z. Cao, L. A. Capistran, E. Capocasa, E. Capote, G. Carapella, F. Carbognani, M. Carlassara, J. B. Carlin, M. Carpinelli, G. Carrillo, J. J. Carter, G. Carullo, J. Casanueva Diaz, C. Casentini, G. Castaldi, S. Y. Castro-Lucas, S. Caudill, M. Cavaglià, R. Cavalieri, G. Cella, P. Cerdá-Durán, E. Cesarini, W. Chaibi, P. Chakraborty, S. Chalathadka Subrahmanya, C. Chan, J. C. L. Chan, K. H. M. Chan, M. Chan, W. L. Chan, K. Chandra, R.-J. Chang, P. Chanial, S. Chao, C. Chapman-Bird, E. L. Charlton, P. Charlton, E. Chassande-Mottin, C. Chatterjee, Debarati Chatterjee, Deep Chatterjee, M. Chaturvedi, S. Chaty, A. Chen, A. H.-Y. Chen, D. Chen, H. Chen, H. Y. Chen, K. H. Chen, X. Chen, Yi-Ru Chen, Yanbei Chen, Yitian Chen, H. P. Cheng, P. Chessa, H. T. Cheung, H. Y. Chia, F. Chiadini, C. Chiang, G. Chiarini, A. Chiba, R. Chiba, R. Chierici, A. Chincarini, M. L. Chiofalo, A. Chiummo, C. Chou, S. Choudhary, N. Christensen, S. S. Y. Chua, K. W. Chung, G. Ciani, P. Ciecielag, M. Cieślar, M. Cifaldi, A. A. Ciobanu, R. Ciolfi, F. Clara, J. A. Clark, T. A. Clarke, P. Clearwater, S. Clesse, F. Cleva, E. Coccia, E. Codazzo, P.-F. Cohadon, M. Colleoni, C. G. Collette, J. Collins, S. Colloms, A. Colombo, M. Colpi, C. M. Compton, L. Conti, S. J. Cooper, T. R. Corbitt, I. Cordero-Carrión, S. Corezzi, N. J. Cornish, A. Corsi, S. Cortese, C. A. Costa, R. Cottingham, M. W. Coughlin, A. Couineaux, J.-P. Coulon, S. T. Countryman, J.-F. Coupechoux, B. Cousins, P. Couvares, D. M. Coward, M. J. Cowart, D. C. Coyne, R. Coyne, K. Craig, R. Creed, J. D. E. Creighton, T. D. Creighton, P. Cremonese, A. W. Criswell, J. C. G. Crockett-Gray, M. Croquette, R. Crouch, S. G. Crowder, J. R. Cudell, T. J. Cullen, A. Cumming, E. Cuoco, M. Cusinato, P. Dabadie, T. Dal Canton, S. Dall’Osso, G. Dálya, B. D’Angelo, S. Danilishin, S. D’Antonio, K. Danzmann, K. E. Darroch, L. P. Dartez, A. Dasgupta, S. Datta, V. Dattilo, A. Daumas, N. Davari, I. Dave, A. Davenport, M. Davier, T. F. Davies, D. Davis, L. Davis, M. C. Davis, E. J. Daw, M. Dax, J. De Bolle, M. Deenadayalan, J. Degallaix, M. De Laurentis, S. Deléglise, V. Del Favero, F. De Lillo, D. Dell’Aquila, W. Del Pozzo, F. De Marco, F. De Matteis, V. D’Emilio, N. Demos, T. Dent, A. Depasse, N. DePergola, R. De Pietri, R. De Rosa, C. De Rossi, R. De Simone, A. Dhani, S. Dhurandhar, R. Diab, M. C. Díaz, M. Di Cesare, G. Dideron, N. A. Didio, T. Dietrich, L. Di Fiore, C. Di Fronzo, F. Di Giovanni, M. Di Giovanni, T. Di Girolamo, D. Diksha, A. Di Michele, J. Ding, S. Di Pace, I. Di Palma, F. Di Renzo, Divyajyoti, A. Dmitriev, Z. Doctor, E. Dohmen, P. P. Doleva, L. Donahue, L. D’Onofrio, F. Donovan, K. L. Dooley, T. Dooney, S. Doravari, O. Dorosh, M. Drago, J. C. Driggers, Y. Drori, J.-G. Ducoin, L. Dunn, U. Dupletsa, D. D’Urso, H. Duval, P.-A. Duverne, S. E. Dwyer, C. Eassa, M. Ebersold, T. Eckhardt, G. Eddolls, B. Edelman, T. B. Edo, O. Edy, A. Effler, J. Eichholz, H. Einsle, M. Eisenmann, R. A. Eisenstein, A. Ejlli, M. Emma, E. Engelby, A. J. Engl, L. Errico, R. C. Essick, H. Estellés, D. Estevez, T. Etzel, M. Evans, T. Evstafyeva, B. E. Ewing, J. M. Ezquiaga, F. Fabrizi, F. Faedi, V. Fafone, S. Fairhurst, P. C. Fan, A. M. Farah, B. Farr, W. M. Farr, G. Favaro, M. Favata, M. Fays, M. Fazio, J. Feicht, M. M. Fejer, E. Fenyvesi, D. L. Ferguson, I. Ferrante, T. A. Ferreira, F. Fidecaro, A. Fiori, I. Fiori, M. Fishbach, R. P. Fisher, R. Fittipaldi, V. Fiumara, R. Flaminio, S. M. Fleischer, L. S. Fleming, E. Floden, E. M. Foley, H. Fong, J. A. Font, B. Fornal, P. W. F. Forsyth, K. Franceschetti, N. Franchini, S. Frasca, F. Frasconi, A. Frattale Mascioli, Z. Frei, A. Freise, O. Freitas, R. Frey, W. Frischhertz, P. Fritschel, V. V. Frolov, G. G. Fronzé, M. Fuentes-Garcia, S. Fujii, I. Fukunaga, P. Fulda, M. Fyffe, W. E. Gabella, B. Gadre, J. R. Gair, S. Galaudage, S. Gallardo, B. Gallego, R. Gamba, A. Gamboa, D. Ganapathy, A. Ganguly, S. G. Gaonkar, B. Garaventa, J. Garcia-Bellido, C. García-Núñez, C. García-Quirós, J. W. Gardner, K. A. Gardner, J. Gargiulo, A. Garron, F. Garufi, C. Gasbarra, B. Gateley, V. Gayathri, G. Gemme, A. Gennai, J. George, R. George, O. Gerberding, L. Gergely, N. Ghadiri, Archisman Ghosh, Shaon Ghosh, Shrobana Ghosh, Suprovo Ghosh, Tathagata Ghosh, L. Giacoppo, J. A. Giaime, K. D. Giardina, D. R. Gibson, D. T. Gibson, C. Gier, P. Giri, F. Gissi, S. Gkaitatzis, J. Glanzer, A. E. Gleckl, F. Glotin, J. Godfrey, P. Godwin, N. L. Goebbels, E. Goetz, J. Golomb, S. Gomez Lopez, B. Goncharov, G. González, P. Goodarzi, A. W. Goodwin-Jones, M. Gosselin, A. S. Göttel, R. Gouaty, D. W. Gould, S. Goyal, B. Grace, A. Grado, V. Graham, A. E. Granados, M. Granata, V. Granata, L. Granda Argianas, S. Gras, P. Grassia, C. Gray, R. Gray, G. Greco, A. C. Green, S. M. Green, S. R. Green, A. M. Gretarsson, E. M. Gretarsson, D. Griffith, W. L. Griffiths, H. L. Griggs, G. Grignani, A. Grimaldi, C. Grimaud, H. Grote, A. S. Gruson, D. Guerra, D. Guetta, G. M. Guidi, A. R. Guimaraes, H. K. Gulati, F. Gulminelli, A. M. Gunny, H. Guo, W. Guo, Y. Guo, Anchal Gupta, Anuradha Gupta, Ish Gupta, N. C. Gupta, P. Gupta, S. K. Gupta, T. Gupta, N. Gupte, R. Gurav, J. Gurs, N. Gutierrez, F. Guzman, D. Haba, M. Haberland, L. Haegel, G. Hain, S. Haino, E. D. Hall, R. Hamburg, E. Z. Hamilton, G. Hammond, W.-B. Han, M. Haney, J. Hanks, C. Hanna, M. D. Hannam, O. A. Hannuksela, A. G. Hanselman, H. Hansen, J. Hanson, R. Harada, T. Harder, K. Haris, T. Harmark, J. Harms, G. M. Harry, I. W. Harry, B. Haskell, C.-J. Haster, J. S. Hathaway, K. Haughian, H. Hayakawa, K. Hayama, J. Healy, A. Heffernan, A. Heidmann, M. C. Heintze, J. Heinze, J. Heinzel, H. Heitmann, F. Hellman, P. Hello, A. F. Helmling-Cornell, G. Hemming, M. Hendry, I. S. Heng, E. Hennes, J.-S. Hennig, M. Hennig, C. Henshaw, A. Hernandez, T. Hertog, M. Heurs, A. L. Hewitt, S. Higginbotham, S. Hild, P. Hill, S. Hill, Y. Himemoto, A. S. Hines, N. Hirata, C. Hirose, J. Ho, S. Hoang, S. Hochheim, D. Hofman, N. A. Holland, K. Holley-Bockelmann, I. J. Hollows, Z. J. Holmes, D. E. Holz, C. Hong, J. Hornung, S. Hoshino, J. Hough, S. Hourihane, E. J. Howell, C. G. Hoy, D. Hoyland, C. A. Hrishikesh, H.-F. Hsieh, C. Hsiung, H. C. Hsu, S.-C. Hsu, W.-F. Hsu, P. Hu, Q. Hu, H. Y. Huang, Y.-J. Huang, Y. Huang, Y. T. Huang, A. D. Huddart, B. Hughey, D. C. Y. Hui, V. Hui, R. Hur, S. Husa, R. Huxford, T. Huynh-Dinh, G. A. Iandolo, A. Iess, K. Inayoshi, Y. Inoue, G. Iorio, J. Irwin, M. Isi, M. A. Ismail, Y. Itoh, M. Iwaya, B. R. Iyer, V. JaberianHamedan, P.-E. Jacquet, S. J. Jadhav, S. P. Jadhav, T. Jain, A. L. James, P. A. James, R. Jamshidi, A. Z. Jan, K. Jani, L. Janiurek, J. Janquart, K. Janssens, N. N. Janthalur, S. Jaraba, P. Jaranowski, P. Jasal, R. Jaume, W. Javed, A. Jennings, W. Jia, J. Jiang, H.-B. Jin, K. Johansmeyer, G. R. Johns, N. A. Johnson, R. Johnston, N. Johny, D. H. Jones, D. I. Jones, R. Jones, S. Jose, P. Joshi, L. Ju, K. Jung, J. Junker, V. Juste, T. Kajita, C. Kalaghatgi, V. Kalogera, M. Kamiizumi, N. Kanda, S. Kandhasamy, G. Kang, J. B. Kanner, S. J. Kapadia, D. P. Kapasi, S. Karat, C. Karathanasis, S. Karki, R. Kashyap, M. Kasprzack, W. Kastaun, J. Kato, T. Kato, S. Katsanevas, E. Katsavounidis, W. Katzman, T. Kaur, R. Kaushik, K. Kawabe, D. Keitel, J. Kelley-Derzon, J. Kennington, R. Kesharwani, J. S. Key, S. Khadka, F. Y. Khalili, F. Khan, I. Khan, T. Khanam, M. Khursheed, W. Kiendrebeogo, N. Kijbunchoo, C. Kim, J. C. Kim, K. Kim, M. H. Kim, S. Kim, W. S. Kim, Y.-M. Kim, C. Kimball, N. Kimura, M. Kinley-Hanlon, M. Kinnear, J. S. Kissel, T. Kiyota, S. Klimenko, T. Klinger, A. M. Knee, N. Knust, P. Koch, S. M. Koehlenbeck, G. Koekoek, K. Kohri, K. Kokeyama, S. Koley, P. Kolitsidou, M. Kolstein, K. Komori, A. K. H. Kong, A. Kontos, M. Korobko, R. V. Kossak, X. Kou, A. Koushik, N. Kouvatsos, M. Kovalam, N. Koyama, D. B. Kozak, S. L. Kranzhoff, V. Kringel, N. V. Krishnendu, A. Królak, G. Kuehn, P. Kuijer, S. Kulkarni, A. Kulur Ramamohan, A. Kumar, Praveen Kumar, Prayush Kumar, Rahul Kumar, Rakesh Kumar, J. Kume, K. Kuns, S. Kuroyanagi, S. Kuwahara, K. Kwak, K. Kwan, G. Lacaille, P. Lagabbe, D. Laghi, S. Lai, A. H. Laity, M. H. Lakkis, E. Lalande, M. Lalleman, M. Landry, B. B. Lane, R. N. Lang, J. Lange, B. Lantz, A. La Rana, I. L. Rosa, A. Lartaux-Vollard, P. D. Lasky, J. Lawrence, M. Laxen, A. Lazzarini, C. Lazzaro, P. Leaci, S. LeBohec, Y. K. Lecoeuche, H. M. Lee, H. W. Lee, K. Lee, R.-K. Lee, R. Lee, S. Lee, Y. Lee, I. N. Legred, J. Lehmann, L. Lehner, A. Lemaître, M. Lenti, M. Leonardi, E. Leonova, M. Lequime, N. Leroy, M. Lesovsky, N. Letendre, M. Lethuillier, C. Levesque, Y. Levin, K. Leyde, A. K. Y. Li, K. L. Li, T. G. F. Li, X. Li, Chien-Yu Lin, Chun-Yu Lin, E. T. Lin, F. Lin, H. Lin, L. C.-C. Lin, F. Linde, S. D. Linker, T. B. Littenberg, A. Liu, G. C. Liu, Jian Liu, F. Llamas, J. Llobera-Querol, R. K. L. Lo, J.-P. Locquet, L. London, A. Longo, D. Lopez, M. Lopez Portilla, M. Lorenzini, V. Loriette, M. Lormand, G. Losurdo, T. P. Lott IV, J. D. Lough, H. A. Loughlin, C. O. Lousto, M. J. Lowry, H. Lück, D. Lumaca, A. P. Lundgren, A. W. Lussier, L.-T. Ma, S. Ma, M. Ma’arif, R. Macas, M. MacInnis, R. R. Maciy, D. M. Macleod, I. A. O. MacMillan, A. Macquet, D. Macri, K. Maeda, S. Maenaut, I. Magaña Hernandez, S. S. Magare, C. Magazzù, R. M. Magee, E. Maggio, R. Maggiore, M. Magnozzi, M. Mahesh, S. Mahesh, M. Maini, S. Majhi, E. Majorana, C. N. Makarem, J. A. Malaquias-Reis, S. Maliakal, A. Malik, N. Man, V. Mandic, V. Mangano, B. Mannix, G. L. Mansell, M. Manske, M. Mantovani, M. Mapelli, F. Marchesoni, D. Marín Pina, F. 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N. Nelson, M. Nery, A. Neunzert, S. Ng, C. Nguyen, P. Nguyen, L. Nguyen Quynh, S. A. Nichols, A. B. Nielsen, G. Nieradka, A. Niko, Y. Nishino, A. Nishizawa, S. Nissanke, E. Nitoglia, W. Niu, F. Nocera, M. Norman, C. North, J. Novak, J. F. Nuño Siles, G. Nurbek, L. K. Nuttall, K. Obayashi, J. Oberling, J. O’Dell, M. Oertel, A. Offermans, G. Oganesyan, J. J. Oh, K. Oh, S. H. Oh, T. O’Hanlon, M. Ohashi, M. Ohkawa, F. Ohme, H. Ohta, A. S. Oliveira, R. Oliveri, V. Oloworaran, B. O’Neal, K. Oohara, B. O’Reilly, N. D. Ormsby, M. Orselli, R. O’Shaughnessy, Y. Oshima, S. Oshino, S. Ossokine, C. Osthelder, D. J. Ottaway, A. Ouzriat, H. Overmier, B. J. Owen, A. E. Pace, R. Pagano, M. A. Page, A. Pai, S. A. Pai, A. Pal, S. Pal, M. A. Palaia, M. Pálfi, P. P. Palma, C. Palomba, K. C. Pan, P. K. Panda, L. Panebianco, P. T. H. Pang, F. Pannarale, B. C. Pant, F. H. Panther, C. D. Panzer, F. Paoletti, A. Paoli, A. Paolone, E. E. Papalexakis, L. Papalini, G. Papigkiotis, A. Parisi, J. Park, W. Parker, G. Pascale, D. Pascucci, A. Pasqualetti, R. Passaquieti, D. Passuello, O. Patane, M. Patel, D. Pathak, M. Pathak, A. Patra, B. Patricelli, A. S. Patron, S. Paul, E. Payne, T. Pearce, M. Pedraza, R. Pegna, A. Pele, F. E. Peña Arellano, S. Penn, M. D. Penuliar, A. Perego, A. Pereira, J. J. Perez, C. Périgois, C. C. Perkins, G. Perna, A. Perreca, J. Perret, S. Perriès, J. W. Perry, D. Pesios, C. Petrillo, H. P. Pfeiffer, H. Pham, K. A. Pham, K. S. Phukon, H. Phurailatpam, O. J. Piccinni, M. Pichot, M. Piendibene, F. Piergiovanni, L. Pierini, G. Pierra, V. Pierro, M. Pietrzak, M. Pillas, F. Pilo, L. Pinard, C. Pineda-Bosque, I. M. Pinto, M. Pinto, B. J. Piotrzkowski, M. Pirello, M. D. Pitkin, A. Placidi, E. Placidi, M. L. Planas, W. Plastino, R. Poggiani, E. Polini, L. Pompili, J. Poon, E. Porcelli, J. Portell, E. K. Porter, C. Posnansky, R. Poulton, J. Powell, M. Pracchia, B. K. Pradhan, T. Pradier, A. K. Prajapati, K. Prasai, R. Prasanna, P. Prasia, G. Pratten, M. Principe, G. A. Prodi, L. Prokhorov, P. Prosposito, L. Prudenzi, A. Puecher, J. Pullin, M. Punturo, F. Puosi, P. Puppo, M. Pürrer, H. Qi, J. Qin, G. Quéméner, V. Quetschke, C. Quigley, P. J. Quinonez, R. Quitzow-James, F. J. Raab, G. Raaijmakers, N. Radulesco, P. Raffai, S. X. Rail, S. Raja, C. Rajan, B. Rajbhandari, D. S. Ramirez, K. E. Ramirez, F. A. Ramis Vidal, A. Ramos-Buades, D. Rana, E. Randel, S. Ranjan, P. Rapagnani, B. Ratto, S. Rawat, A. Ray, V. Raymond, M. Razzano, J. Read, M. Recaman Payo, T. Regimbau, L. Rei, S. Reid, S. W. Reid, D. H. Reitze, P. Relton, A. Renzini, P. Rettegno, B. Revenu, A. Reza, M. Rezac, A. S. Rezaei, F. Ricci, M. Ricci, D. Richards, C. J. Richardson, J. W. Richardson, A. Rijal, K. Riles, H. K. Riley, S. Rinaldi, J. Rittmeyer, C. Robertson, F. Robinet, M. Robinson, A. Rocchi, L. Rolland, J. G. Rollins, M. Romanelli, A. E. Romano, R. Romano, A. Romero, I. M. Romero-Shaw, J. H. Romie, T. J. Roocke, L. Rosa, T. J. Rosauer, C. A. Rose, D. Rosińska, M. P. Ross, M. Rossello, S. Rowan, S. K. Roy, S. Roy, D. Rozza, P. Ruggi, E. Ruiz Morales, K. Ruiz-Rocha, S. Sachdev, T. Sadecki, J. Sadiq, P. Saffarieh, M. R. Sah, S. S. Saha, T. Sainrat, S. Sajith Menon, K. Sakai, M. Sakellariadou, T. Sako, S. Sakon, O. S. Salafia, F. Salces-Carcoba, L. Salconi, M. Saleem, F. Salemi, M. Sallé, S. Salvador, A. Sanchez, E. J. Sanchez, J. H. Sanchez, L. E. Sanchez, N. Sanchis-Gual, J. R. Sanders, E. M. Sänger, T. R. Saravanan, N. Sarin, A. Sasli, P. Sassi, B. Sassolas, H. Satari, R. Sato, S. Sato, Y. Sato, O. Sauter, R. L. Savage, T. Sawada, H. L. Sawant, S. Sayah, D. Schaetzl, M. Scheel, J. Scheuer, M. G. Schiworski, P. Schmidt, S. Schmidt, R. Schnabel, M. Schneewind, R. M. S. Schofield, K. Schouteden, H. Schuler, B. W. Schulte, B. F. Schutz, E. Schwartz, J. Scott, S. M. Scott, T. C. Seetharamu, M. Seglar-Arroyo, Y. Sekiguchi, D. Sellers, A. S. Sengupta, D. Sentenac, E. G. Seo, J. W. Seo, V. Sequino, M. Serra, G. Servignat, Y. Setyawati, T. Shaffer, U. S. Shah, M. S. Shahriar, M. A. Shaikh, B. Shams, L. Shao, A. K. Sharma, P. Sharma, S. Sharma-Chaudhary, P. Shawhan, N. S. Shcheblanov, B. Shen, Y. Shikano, M. Shikauchi, K. Shimode, H. Shinkai, J. Shiota, D. H. Shoemaker, D. M. Shoemaker, R. W. Short, S. ShyamSundar, A. Sider, H. Siegel, M. Sieniawska, D. Sigg, L. Silenzi, M. Simmonds, L. P. Singer, A. Singh, D. Singh, M. K. Singh, A. Singha, A. M. Sintes, V. Sipala, V. Skliris, B. J. J. Slagmolen, T. J. Slaven-Blair, J. Smetana, J. R. Smith, L. Smith, R. J. E. Smith, W. J. Smith, J. Soldateschi, S. N. Somala, K. Somiya, K. Soni, S. Soni, V. Sordini, F. Sorrentino, N. Sorrentino, R. Soulard, T. Souradeep, A. Southgate, E. Sowell, V. Spagnuolo, A. P. Spencer, M. Spera, P. Spinicelli, A. K. Srivastava, F. Stachurski, D. A. Steer, J. Steinlechner, S. Steinlechner, N. Stergioulas, P. Stevens, M. StPierre, L. C. Strang, G. Stratta, M. D. Strong, A. Strunk, R. Sturani, A. L. Stuver, M. Suchenek, S. Sudhagar, N. Sueltmann, A. G. Sullivan, K. D. Sullivan, L. Sun, S. Sunil, A. Sur, J. Suresh, P. J. Sutton, Takamasa Suzuki, Takanori Suzuki, B. L. Swinkels, A. Syx, M. J. Szczepańczyk, P. Szewczyk, M. Tacca, H. Tagoshi, S. C. Tait, H. Takahashi, R. Takahashi, A. Takamori, K. Takatani, H. Takeda, M. Takeda, C. J. Talbot, C. Talbot, M. Tamaki, N. Tamanini, D. Tanabe, K. Tanaka, S. J. Tanaka, T. Tanaka, A. J. Tanasijczuk, D. Tang, S. Tanioka, D. B. Tanner, L. Tao, R. D. Tapia, E. N. Tapia San Martín, R. Tarafder, C. Taranto, A. Taruya, J. D. Tasson, M. Teloi, R. Tenorio, H. Themann, A. Theodoropoulos, M. P. Thirugnanasambandam, L. M. Thomas, M. Thomas, P. Thomas, J. E. Thompson, S. R. Thondapu, K. A. Thorne, E. Thrane, J. Tissino, A. Tiwari, Shubhanshu Tiwari, Srishti Tiwari, V. Tiwari, M. R. Todd, A. M. Toivonen, K. Toland, A. E. Tolley, T. Tomaru, K. Tomita, T. Tomura, C. Tong-Yu, A. Toriyama, N. Toropov, A. Torres-Forné, C. I. Torrie, M. Toscani, I. Tosta e Melo, E. Tournefier, A. A. Trani, A. Trapananti, F. Travasso, G. Traylor, J. Trenado, M. Trevor, M. C. Tringali, A. Tripathee, L. Troiano, A. Trovato, L. Trozzo, R. J. Trudeau, T. T. L. Tsang, R. Tso, S. Tsuchida, L. Tsukada, T. Tsutsui, K. Turbang, M. Turconi, C. Turski, H. Ubach, A. S. Ubhi, N. Uchikata, T. Uchiyama, R. P. Udall, T. Uehara, K. Ueno, C. S. Unnikrishnan, T. Ushiba, A. Utina, M. Vacatello, H. Vahlbruch, N. Vaidya, G. Vajente, A. Vajpeyi, G. Valdes, J. Valencia, M. Valentini, S. A. Vallejo-Peña, S. Vallero, V. Valsan, N. van Bakel, M. van Beuzekom, M. van Dael, J. F. J. van den Brand, C. Van Den Broeck, D. C. Vander-Hyde, M. van der Sluys, A. Van de Walle, J. van Dongen, K. Vandra, H. van Haevermaet, J. V. van Heijningen, J. Vanosky, M. H. P. M. van Putten, Z. van Ranst, N. van Remortel, M. Vardaro, A. F. Vargas, V. Varma, M. Vasúth, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, S. Venikoudis, J. Venneberg, P. Verdier, D. Verkindt, B. Verma, P. Verma, Y. Verma, S. M. Vermeulen, D. Veske, F. Vetrano, A. Veutro, A. M. Vibhute, A. Viceré, S. Vidyant, A. D. Viets, A. Vijaykumar, A. Vilkha, V. Villa-Ortega, E. T. Vincent, J.-Y. Vinet, S. Viret, A. Virtuoso, S. Vitale, H. Vocca, D. Voigt, E. R. G. von Reis, J. S. A. von Wrangel, S. P. Vyatchanin, L. E. Wade, M. Wade, K. J. Wagner, R. C. Walet, M. Walker, G. S. Wallace, L. Wallace, H. Wang, J. Z. Wang, W. H. Wang, Z. Wang, G. Waratkar, R. L. Ward, J. Warner, M. Was, T. Washimi, N. Y. Washington, D. Watarai, K. E. Wayt, B. Weaver, C. R. Weaving, S. A. Webster, M. Weinert, A. J. Weinstein, R. Weiss, C. M. Weller, R. A. Weller, F. Wellmann, L. Wen, P. Weßels, K. Wette, J. T. Whelan, D. D. White, B. F. Whiting, C. Whittle, J. B. Wildberger, O. S. Wilk, D. Wilken, K. Willetts, D. Williams, M. J. Williams, N. S. Williams, J. L. Willis, B. Willke, M. Wils, C. C. Wipf, G. Woan, J. Woehler, J. K. Wofford, N. E. Wolfe, D. Wong, H. T. Wong, H. W. Y. Wong, I. C. F. Wong, J. L. Wright, M. Wright, C. Wu, D. S. Wu, H. Wu, D. M. Wysocki, L. Xiao, V. A. Xu, Y. Xu, N. Yadav, H. Yamamoto, K. Yamamoto, M. Yamamoto, T. S. Yamamoto, T. Yamamoto, S. Yamamura, R. Yamazaki, S. Yan, T. Yan, F. W. Yang, F. Yang, K. Z. Yang, L.-C. Yang, Y. Yang, Z. Yarbrough, S.-W. Yeh, A. B. Yelikar, S. M. C. Yeung, X. Yin, J. Yokoyama, T. Yokozawa, J. Yoo, H. Yu, H. Yuzurihara, A. Zadrożny, A. J. Zannelli, M. Zanolin, M. Zeeshan, T. Zelenova, J.-P. Zendri, M. Zeoli, M. Zerrad, M. Zevin, A. C. Zhang, J. Zhang, L. Zhang, R. Zhang, T. Zhang, Y. Zhang, C. Zhao, Yue Zhao, Yuhang Zhao, Y. Zheng, H. Zhong, S. Zhong, R. Zhou, Z.-H. Zhu, A. B. Zimmerman, M. E. Zucker, J. Zweizig","doi":"10.3847/1538-4357/ad9749","DOIUrl":"https://doi.org/10.3847/1538-4357/ad9749","url":null,"abstract":"We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO–Virgo–KAGRA network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received with low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wave Transient Catalogs (GWTC-3). Targeted searches were carried out on the entire GW sample using the maximum-likelihood Non-imaging Transient Reconstruction and Temporal Search pipeline on the BAT data made available via the GUANO infrastructure. We do not detect any significant electromagnetic emission that is temporally and spatially coincident with any of the GW candidates. We report flux upper limits in the 15–350 keV band as a function of sky position for all the catalog candidates. For GW candidates where the Swift-BAT false alarm rate is less than 10⁻³ Hz, we compute the GW–BAT joint false alarm rate. Finally, the derived Swift-BAT upper limits are used to infer constraints on the putative electromagnetic emission associated with binary black hole mergers.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"47 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417426","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}

{"title":"UNCOVERing the Faint End of the z ∼ 7 [O iii] Luminosity Function with JWST’s F410M Medium Bandpass Filter","authors":"Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, John R. Weaver, Bingjie Wang","doi":"10.3847/1538-4357/ada8a6","DOIUrl":"https://doi.org/10.3847/1538-4357/ada8a6","url":null,"abstract":"Strong emission from doubly ionized oxygen is a beacon for some of the most intensely star-forming galaxies. JWST enables the search for this beacon in the early Universe with unprecedented sensitivity. Using UNCOVER DR1 JWST/NIRCam and Hubble Space Telescope (HST) imaging data of A2744, we identify strong (rest-frame EW &gt; 500Å) [O &lt;sc&gt;iii&lt;/sc&gt;]&lt;sub&gt;5008&lt;/sub&gt; emitters at &lt;italic toggle=\"yes\"&gt;z&lt;/italic&gt; ∼ 7 based on excess F410M flux. We find &lt;italic toggle=\"yes\"&gt;N&lt;/italic&gt; = 68 &lt;italic toggle=\"yes\"&gt;z&lt;/italic&gt; ∼ 7 [O &lt;sc&gt;iii&lt;/sc&gt;] candidates, including &lt;italic toggle=\"yes\"&gt;N&lt;/italic&gt; = 33 with deep HST coverage required to rule out lower-redshift interlopers (13.68 arcmin&lt;sup&gt;2&lt;/sup&gt; with F814W 5&lt;italic toggle=\"yes\"&gt;σ&lt;/italic&gt; depth &gt;28 AB). Such strong emission lines can produce very red colors often misinterpreted as evidence for old, massive stellar populations, but are shown to be emission lines where we have spectra. Using this deep HST sample, we derive a new [O &lt;sc&gt;iii&lt;/sc&gt;] luminosity function (LF) spanning &lt;inline-formula&gt;\u0000&lt;tex-math&gt;\u0000&lt;?CDATA $41.1lt {{rm{log}}}_{10}(L/{{rm{erg}},{rm{s}}}^{-1})lt 42.4$?&gt;\u0000&lt;/tex-math&gt;\u0000&lt;mml:math overflow=\"scroll\"&gt;&lt;mml:mn&gt;41.1&lt;/mml:mn&gt;&lt;mml:mo&gt;&lt;&lt;/mml:mo&gt;&lt;mml:msub&gt;&lt;mml:mrow&gt;&lt;mml:mi mathvariant=\"normal\"&gt;log&lt;/mml:mi&gt;&lt;/mml:mrow&gt;&lt;mml:mrow&gt;&lt;mml:mn&gt;10&lt;/mml:mn&gt;&lt;/mml:mrow&gt;&lt;/mml:msub&gt;&lt;mml:mo stretchy=\"false\"&gt;(&lt;/mml:mo&gt;&lt;mml:mi&gt;L&lt;/mml:mi&gt;&lt;mml:mo&gt;/&lt;/mml:mo&gt;&lt;mml:msup&gt;&lt;mml:mrow&gt;&lt;mml:mi mathvariant=\"normal\"&gt;erg&lt;/mml:mi&gt;&lt;mml:mspace width=\"0.25em\"&gt;&lt;/mml:mspace&gt;&lt;mml:mi mathvariant=\"normal\"&gt;s&lt;/mml:mi&gt;&lt;/mml:mrow&gt;&lt;mml:mrow&gt;&lt;mml:mo&gt;−&lt;/mml:mo&gt;&lt;mml:mn&gt;1&lt;/mml:mn&gt;&lt;/mml:mrow&gt;&lt;/mml:msup&gt;&lt;mml:mo stretchy=\"false\"&gt;)&lt;/mml:mo&gt;&lt;mml:mo&gt;&lt;&lt;/mml:mo&gt;&lt;mml:mn&gt;42.4&lt;/mml:mn&gt;&lt;/mml:math&gt;\u0000&lt;inline-graphic xlink:href=\"apjada8a6ieqn1.gif\"&gt;&lt;/inline-graphic&gt;\u0000&lt;/inline-formula&gt;, an order of magnitude deeper than previous &lt;italic toggle=\"yes\"&gt;z&lt;/italic&gt; ∼ 6 studies. This LF is fit by a power law with a faint-end slope of &lt;inline-formula&gt;\u0000&lt;tex-math&gt;\u0000&lt;?CDATA $alpha =-2.0{7}_{-0.23}^{+0.22}$?&gt;\u0000&lt;/tex-math&gt;\u0000&lt;mml:math overflow=\"scroll\"&gt;&lt;mml:mi&gt;α&lt;/mml:mi&gt;&lt;mml:mo&gt;=&lt;/mml:mo&gt;&lt;mml:mo&gt;−&lt;/mml:mo&gt;&lt;mml:mn&gt;2.0&lt;/mml:mn&gt;&lt;mml:msubsup&gt;&lt;mml:mrow&gt;&lt;mml:mn&gt;7&lt;/mml:mn&gt;&lt;/mml:mrow&gt;&lt;mml:mrow&gt;&lt;mml:mo&gt;−&lt;/mml:mo&gt;&lt;mml:mn&gt;0.23&lt;/mml:mn&gt;&lt;/mml:mrow&gt;&lt;mml:mrow&gt;&lt;mml:mo&gt;+&lt;/mml:mo&gt;&lt;mml:mn&gt;0.22&lt;/mml:mn&gt;&lt;/mml:mrow&gt;&lt;/mml:msubsup&gt;&lt;/mml:math&gt;\u0000&lt;inline-graphic xlink:href=\"apjada8a6ieqn2.gif\"&gt;&lt;/inline-graphic&gt;\u0000&lt;/inline-formula&gt;. Our results are consistent with the &lt;italic toggle=\"yes\"&gt;z&lt;/italic&gt; ∼ 7 FRESCO [O &lt;sc&gt;iii&lt;/sc&gt;] LF across the overlapping 0.5 dex range, &lt;inline-formula&gt;\u0000&lt;tex-math&gt;\u0000&lt;?CDATA $41.9gt {{rm{log}}}_{10}(L/{{rm{erg}},{rm{s}}}^{-1})gt 42.4$?&gt;\u0000&lt;/tex-math&gt;\u0000&lt;mml:math overflow=\"scroll\"&gt;&lt;mml:mn&gt;41.9&lt;/mml:mn&gt;&lt;mml:mo&gt;&gt;&lt;/mml:mo&gt;&lt;mml:msub&gt;&lt;mml:mrow&gt;&lt;mml:mi mathvariant=\"normal\"&gt;log&lt;/mml:mi&gt;&lt;/mml:mrow&gt;&lt;mml:mrow&gt;&lt;mml:mn&gt;10&lt;/mml:mn&gt;&lt;/mml:mrow&gt;&lt;/mml:msub&gt;&lt;mml:mo stretchy=\"false\"&gt;(&lt;/mml:mo&gt;&lt;mml:mi&gt;L&lt;/mml:mi&gt;&lt;mml:mo&gt;/&lt;/mml:mo&gt;&lt;mml:msup&gt;&lt;mml:mrow&gt;&lt;mml:mi mathvariant=\"normal\"&gt;erg&lt;/mml:mi&gt;&lt;mml:mspac","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417427","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}

{"title":"Three-dimensional Transport of Solids in a Protoplanetary Disk Containing a Growing Giant Planet","authors":"Eric Van Clepper, Ellen M. Price, Fred J. Ciesla","doi":"10.3847/1538-4357/ada8a4","DOIUrl":"https://doi.org/10.3847/1538-4357/ada8a4","url":null,"abstract":"We present the results of combined hydrodynamic and particle tracking post-processing modeling to study the transport of small dust in a protoplanetary disk containing an embedded embryo in three dimensions. We use a suite of FARGO3D hydrodynamic simulations of disks containing a planetary embryo varying in mass up to 300 <italic toggle=\"yes\">M</italic>_⊕ on a fixed orbit in both high- and low-viscosity disks. We then simulate solid particles through the disk as a post-processing step using a Monte Carlo integration, allowing us to track the trajectories of individual particles as they travel throughout the disk. We find that gas advection onto the planet can carry small, well-coupled solids across the gap opened in the disk by the embedded planet for planetary masses above the pebble isolation mass. This mixing between the inner and outer disk can occur in both directions, with solids in the inner disk mixing to the outer disk as well. Additionally, in low-viscosity disks, multiple dust pile-ups in the outer disk may preserve isotopic heterogeneities, possibly providing an outermost tertiary isotopic reservoir. Throughout Jupiter's growth, the extent of mixing between isotopic reservoirs varied depending on dust size, gas turbulence, and the Jovian embryo mass.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"27 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417429","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}

{"title":"Magnetic Activities of AD Leonis: Flares in TESS Data and Optical Spectra","authors":"Diya Ram, Soumen Mondal, Dusmanta Patra, Samrat Ghosh, Rajib Khumbhakar","doi":"10.3847/1538-4357/adabc3","DOIUrl":"https://doi.org/10.3847/1538-4357/adabc3","url":null,"abstract":"We studied the flaring activities of M4.5 dwarf AD Leo to understand its stellar atmospheres and magnetic activities. We present new observational results on this highly active star, using nonsimultaneous measurement of Transiting Exoplanet Survey Satellite (TESS) data, time-series optical spectra, and Giant Meter Radio Telescope 325 MHz radio data. We revisited the rotation period of 2.23 ± 0.04 days from TESS, which matches well with previously measured literature values. We estimated an extremely rare high-energy superflare of 4.9 × 10³⁵ erg and ∼400 minute duration with a high magnetic field strength of 1.2 kG. Interestingly, we correlated the duration of a flare event with its energy, <italic toggle=\"yes\">τ</italic> ∝ <inline-formula>\u0000<tex-math>\u0000<?CDATA ${E}_{mathrm{bol}}^{0.60pm 0.02}$?>\u0000</tex-math>\u0000<mml:math overflow=\"scroll\"><mml:msubsup><mml:mi>E</mml:mi><mml:mi>bol</mml:mi><mml:mrow><mml:mn>0.60</mml:mn><mml:mo>±</mml:mo><mml:mn>0.02</mml:mn></mml:mrow></mml:msubsup></mml:math>\u0000<inline-graphic xlink:href=\"apjadabc3ieqn1.gif\"></inline-graphic>\u0000</inline-formula>, and noticed a discrepancy between stellar and solar flares suggesting a difference in coronal magnetic field strength. From time-series spectra, we observed H<italic toggle=\"yes\">α</italic> spectral flares in the range of 10³⁰–10³¹ erg. A 12 minute delay in a spectral flare event was observed between the emission of the H<italic toggle=\"yes\">α</italic> and Ca <sc>ii</sc> H and K lines, possibly due to their origination at different spatial locations in the chromosphere. We noticed the deviation in flare rate distribution and orbital phases indicates the presence of highly active regions. Furthermore, an occasional radio detection with a flux density of 9.46 ± 1.63 mJy at a frequency of 325 MHz might be coherent emission in the presence of the magnetic field, giving a hint of star–planet interaction.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"79 6 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143417436","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}

{"title":"Relative Alpha in the Magnetohydrodynamics with Open Magnetic Field Boundary and Its Application to the Solar Eruption","authors":"Shangbin Yang, Jörg Büchner, Jean Carlo Santos, Jan Skála, Hongqi Zhang","doi":"10.3847/1538-4357/ada278","DOIUrl":"https://doi.org/10.3847/1538-4357/ada278","url":null,"abstract":"An instability criterion in the magnetohydrodynamics (MHD) with the open boundary of a magnetic field is proposed in this paper. We use a series of linear force-free extrapolation fields, in which the normal part of the magnetic field is fixed, to obtain the linear fitting coefficient called relative alpha by using the cojoined value of magnetic free energy and magnetic flux at the open boundary (<italic toggle=\"yes\">E</italic>_{<italic toggle=\"yes\">f</italic>}Φ²) and the square of relative magnetic helicity (<inline-formula>\u0000<tex-math>\u0000<?CDATA ${H}_{R}^{2}$?>\u0000</tex-math>\u0000<mml:math overflow=\"scroll\"><mml:msubsup><mml:mrow><mml:mi>H</mml:mi></mml:mrow><mml:mrow><mml:mi>R</mml:mi></mml:mrow><mml:mrow><mml:mn>2</mml:mn></mml:mrow></mml:msubsup></mml:math>\u0000<inline-graphic xlink:href=\"apjada278ieqn1.gif\"></inline-graphic>\u0000</inline-formula>). We calculate this coefficient of the magnetic field above active regions NOAA 8210 and NOAA 11429 obtained by the photospheric-data-driven MHD model. It is found that the fitting coefficient is a good proxy of the criterion to indicate the occurrence of instability after which the magnetic reconnection happens and causes the fast release of magnetic energy. We also applied this method to the continuous evolution of the three-dimensional magnetic field of NOAA 11158 based on the measurement of the photospheric vector magnetic field of Solar Dynamics Observatory/Helioseismic and Magnetic Imager by the nonlinear force-free extrapolation method. The calculated coefficient when the major flare happened based on the extrapolation data is very close to the expected ones, which perfectly reflects the occurrence of instability, and the difference is even less than 7%. This relative alpha is very helpful to evaluate how far it is from the instability in the MHD and quantitatively estimate the occurrence of solar eruption in the space weather forecast.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"51 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143418369","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}

{"title":"Flux-rope-mediated Turbulent Magnetic Reconnection","authors":"Alexander J. B. Russell","doi":"10.3847/1538-4357/adac61","DOIUrl":"https://doi.org/10.3847/1538-4357/adac61","url":null,"abstract":"We present a new model of magnetic reconnection in the presence of turbulence. The new model differs from the Lazarian–Vishniac turbulent reconnection theory by emphasizing the role of locally coherent magnetic structures, whose existence is shown to be permitted by the properties of magnetic field line separation in turbulent plasma. Local coherence allows storage of magnetic helicity inside the reconnection layer in the form of locally coherent twisted flux ropes. We then introduce the “Alfvén horizon” to explain why the global reconnection rate can be governed by locally coherent magnetic field structure instead of by field line wandering, formally extending to 3D the principle that reconnection can be made fast by fragmentation of the global current layer. Coherence is shown to dominate over field line dispersion if the anisotropy of the turbulence at the perpendicular scale matching the thickness of a marginally stable current layer exceeds the aspect ratio of the current layer. Finally, we conjecture that turbulence generated within the reconnection layer may produce a critically balanced state that maintains the system in the flux-rope-mediated regime. The new model successfully accounts for the major features of 3D numerical simulations of self-generated turbulent reconnection, including reconnection rates of 0.01 in resistive MHD and 0.1 with collisionless physics.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"47 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143401765","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}

{"title":"Exploring the Key Features of Repeating Fast Radio Bursts with Machine Learning","authors":"Wan-Peng Sun, Ji-Guo Zhang, Yichao Li, Wan-Ting Hou, Fu-Wen Zhang, Jing-Fei Zhang and Xin Zhang","doi":"10.3847/1538-4357/adad6a","DOIUrl":"https://doi.org/10.3847/1538-4357/adad6a","url":null,"abstract":"Fast radio bursts (FRBs) are enigmatic high-energy events with unknown origins, which are observationally divided into two categories, i.e., repeaters and nonrepeaters. However, there are potentially a number of nonrepeaters that may be misclassified, as repeating bursts are missed due to the limited sensitivity and observation periods, thus misleading the investigation of their physical properties. In this work, we propose a repeater identification method based on the t-distributed Stochastic Neighbor Embedding algorithm and apply the classification to the first Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) catalog. We find that the spectral morphology parameters, specifically spectral running (r), represent the key features for identifying repeaters from the nonrepeaters. Also, the results suggest that repeaters are more biased toward narrowband emission, whereas nonrepeaters are inclined toward broadband emission. We provide a list of 163 repeater candidates, five of which are confirmed with an updated repeater catalog from CHIME/FRB. Our findings improve our understanding of the various properties underlying repeaters and nonrepeaters, as well as guidelines for future FRB detection and categorization.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143401770","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}