@article{MTMT:34722940,
	title = {Serendipitous detection of the dusty Type IIL SN 1980K with JWST/MIRI},
	url = {https://m2.mtmt.hu/api/publication/34722940},
	author = {Zsíros, Szanna and Szalai, Tamás and De, Looze Ilse and Sarangi, Arkaprabha and Shahbandeh, Melissa and Fox, Ori D. and Temim, Tea and Milisavljevic, Dan and Van, Dyk Schuyler D. and Smith, Nathan and Filippenko, Alexei V. and Brink, Thomas G. and Zheng, WeiKang and Dessart, Luc and Jencson, Jacob and Johansson, Joel and Pierel, Justin and Rest, Armin and Tinyanont, Samaporn and Niculescu-Duvaz, Maria and Barlow, M. J. and Wesson, Roger and Andrews, Jennifer and Clayton, Geoff and De, Kishalay and Dwek, Eli and Engesser, Michael and Foley, Ryan J. and Gezari, Suvi and Gomez, Sebastian and Gonzaga, Shireen and Kasliwal, Mansi and Lau, Ryan and Marston, Anthony and O'Steen, Richard and Siebert, Matthew and Skrutskie, Michael and Strolger, Lou and Wang, Qinan and Williams, Brian and Williams, Robert and Xiao, Lin},
	doi = {10.1093/mnras/stae507},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {529},
	unique-id = {34722940},
	issn = {0035-8711},
	abstract = {We present mid-infrared (mid-IR) imaging of the Type IIL supernova (SN) 1980K with the JWST more than 40 yr post-explosion. SN 1980K, located in the nearby (D ≈ 7 Mpc) 'SN factory' galaxy NGC 6946, was serendipitously captured in JWST/MIRI images taken of the field of SN 2004et in the same galaxy. SN 1980K serves as a promising candidate for studying the transitional phase between young SNe and older SN remnants and also provides a great opportunity to investigate its the close environment. SN 1980K can be identified as a clear and bright point source in all eight MIRI filters from F560W up to F2550W. We fit analytical dust models to the mid-IR spectral energy distribution that reveal a large amount (Md ≈ 0.002 M⊙) of Si-dominated dust at $T_\\rm {dust}\\approx 150$ K (accompanied by a hotter dust/gas component), and also computed numerical SED dust models. Radiative transfer modelling of a late-time optical spectrum obtained recently with Keck discloses that an even larger (~0.24-0.58 M⊙) amount of dust is needed in order for selective extinction to explain the asymmetric line profile shapes observed in SN 1980K. As a conclusion, with JWST, we may see i) pre-existing circumstellar dust heated collisionally (or, partly radiatively), analogous to the equatorial ring of SN 1987A, or ii) the mid-IR component of the presumed newly-formed dust, accompanied by much more colder dust present in the ejecta (as suggested by the late-time the optical spectra).},
	keywords = {extinction; DUST; Astrophysics - Solar and Stellar Astrophysics; infrared: stars; supernovae: general; Astrophysics - High Energy Astrophysical Phenomena; Astrophysics - Astrophysics of Galaxies; supernovae: individual: SN 1980K},
	year = {2024},
	eissn = {1365-2966},
	pages = {155-168}
}

@article{MTMT:34579602,
	title = {GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run},
	url = {https://m2.mtmt.hu/api/publication/34579602},
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	doi = {10.1103/PhysRevD.109.022001},
	journal-iso = {PHYS REV D},
	journal = {PHYSICAL REVIEW D},
	volume = {109},
	unique-id = {34579602},
	issn = {2470-0010},
	year = {2024},
	eissn = {2470-0029},
	orcid-numbers = {Gergely, Árpád László/0000-0003-3146-6201}
}

@article{MTMT:34547808,
	title = {Ground-based and JWST Observations of SN 2022pul. I. Unusual Signatures of Carbon, Oxygen, and Circumstellar Interaction in a Peculiar Type Ia Supernova},
	url = {https://m2.mtmt.hu/api/publication/34547808},
	author = {Siebert, M.R. and Kwok, L.A. and Johansson, J. and Jha, S.W. and Blondin, S. and Dessart, L. and Foley, R.J. and Hillier, D.J. and Larison, C. and Pakmor, R. and Temim, T. and Andrews, J.E. and Auchettl, K. and Badenes, C. and Barna, Barnabás and Bostroem, K.A. and Brenner, Newman M.J. and Brink, T.G. and Bustamante-Rosell, M.J. and Camacho-Neves, Y. and Clocchiatti, A. and Coulter, D.A. and Davis, K.W. and Deckers, M. and Dimitriadis, G. and Dong, Y. and Farah, J. and Filippenko, A.V. and Flörs, A. and Fox, O.D. and Garnavich, P. and Gonzalez, E.P. and Graur, O. and Hambsch, F.-J. and Hosseinzadeh, G. and Howell, D.A. and Hughes, J.P. and Kerzendorf, W.E. and Le, Saux X.K. and Maeda, K. and Maguire, K. and McCully, C. and Mihalenko, C. and Newsome, M. and O'Brien, J.T. and Pearson, J. and Pellegrino, C. and Pierel, J.D.R. and Polin, A. and Rest, A. and Rojas-Bravo, C. and Sand, D.J. and Schwab, M. and Shahbandeh, M. and Shrestha, M. and Smith, N. and Strolger, L.-G. and Szalai, Tamás and Taggart, K. and Terreran, G. and Terwel, J.H. and Tinyanont, S. and Valenti, S. and Vinkó, József and Wheeler, J.C. and Yang, Y. and Zheng, W. and Ashall, C. and DerKacy, J.M. and Galbany, L. and Hoeflich, P. and Hsiao, E. and de, Jaeger T. and Lu, J. and Maund, J. and Medler, K. and Morrell, N. and Shappee, B.J. and Stritzinger, M. and Suntzeff, N. and Tucker, M. and Wang, L.},
	doi = {10.3847/1538-4357/ad0975},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {960},
	unique-id = {34547808},
	issn = {1538-4357},
	year = {2024},
	eissn = {0004-637X},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@misc{MTMT:34542680,
	title = {Development of an ultrathin liquid leaf target system for deuteron acceleration at 10 Hz repetition rate (Conference Presentation)},
	url = {https://m2.mtmt.hu/api/publication/34542680},
	author = {Füle, Miklós Jenő and Gilinger, Tibor and Nagyillés, Bálint G. and Karnok, Máté and Gaál, Péter and Figul, Stephan and Marowsky, Gerd and Kovács, Attila Pál and Osvay, Károly},
	doi = {10.1117/12.2665573},
	editor = {Schroeder, Carl B. and Schreiber, Jörg and Hur, Min Sup and Bulanov, Stepan S. and Jaroszynski, Dino A.},
	unique-id = {34542680},
	year = {2023},
	pages = {30},
	orcid-numbers = {Füle, Miklós Jenő/0000-0001-6996-2329; Kovács, Attila Pál/0000-0001-9754-5573; Osvay, Károly/0000-0002-3468-8312}
}

@article{MTMT:34539610,
	title = {GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run},
	url = {https://m2.mtmt.hu/api/publication/34539610},
	author = {Abbott, R. and Abbott, T.D. and Acernese, F. and Ackley, K. and Adams, C. and Adhikari, N. and Adhikari, R.X. and Adya, V.B. and Affeldt, C. and Agarwal, D. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O.D. and Aiello, L. and Ain, A. and Ajith, P. and Akcay, S. and Akutsu, T. and Albanesi, S. and Allocca, A. and Altin, P.A. and Amato, A. and Anand, C. and Anand, S. and Ananyeva, A. and Anderson, S.B. and Anderson, W.G. and Ando, M. and Andrade, T. and Andres, N. and Andrić, T. and Angelova, S.V. and Ansoldi, S. and Antelis, J.M. and Antier, S. and Appert, S. and Arai, K. and Arai, K. and Arai, Y. and Araki, S. and Araya, A. and Araya, M.C. and Areeda, J.S. and Arène, M. and Aritomi, N. and Arnaud, N. and Arogeti, M. and Aronson, S.M. and Arun, K.G. and Asada, H. and Asali, Y. and Ashton, G. and Aso, Y. and Assiduo, M. and Aston, S.M. and Astone, P. and Aubin, F. and Austin, C. and Babak, S. and Badaracco, F. and Bader, M.K.M. and Badger, C. and Bae, S. and Bae, Y. and Baer, A.M. and Bagnasco, S. and Bai, Y. and Baiotti, L. and Baird, J. and Bajpai, R. and Ball, M. and Ballardin, G. and Ballmer, S.W. and Balsamo, A. and Baltus, G. and Banagiri, S. and Bankar, D. and Barayoga, J.C. and Barbieri, C. and Barish, B.C. and Barker, D. and Barneo, P. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M. and Barta, Dániel and Bartlett, J. and Barton, M.A. and Bartos, I. and Bassiri, R. and Basti, A. and Bawaj, M. and Bayley, J.C. and Baylor, A.C. and Bazzan, M. and Bécsy, B. and Bedakihale, V.M. and Bejger, M. and Belahcene, I. and Benedetto, V. and Beniwal, D. and Bennett, T.F. and Bentley, J.D. and Benyaala, M. and Bergamin, F. and Berger, B.K. and Bernuzzi, S. and Berry, C.P.L. and Bersanetti, D. and Bertolini, A. and Betzwieser, J. and Beveridge, D. and Bhandare, R. and Bhardwaj, U. and Bhattacharjee, D. and Bhaumik, S. and Bilenko, I.A. and Billingsley, G. and Bini, S. and Birney, R. and Birnholtz, O. and Biscans, S. and Bischi, M. and Biscoveanu, S. and Bisht, A. and Biswas, B. and Bitossi, M. and Bizouard, M.-A. and Blackburn, J.K. and Blair, C.D. and Blair, D.G. and Blair, R.M. and Bobba, F. and Bode, N. and Boer, M. and Bogaert, G. and Boldrini, M. and Bonavena, L.D. and Bondu, F. and Bonilla, E. and Bonnand, R. and Booker, P. and Boom, B.A. and Bork, R. and Boschi, V. and Bose, N. and Bose, S. and Bossilkov, V. and Boudart, V. and Bouffanais, Y. and Bozzi, A. and Bradaschia, C. and Brady, P.R. and Bramley, A. and Branch, A. and Branchesi, M. and Brandt, J. and Brau, J.E. and Breschi, M. and Briant, T. and Briggs, J.H. and Brillet, A. and Brinkmann, M. and Brockill, P. and Brooks, A.F. and Brooks, J. and Brown, D.D. and Brunett, S. and Bruno, G. and Bruntz, R. and Bryant, J. and Bulik, T. and Bulten, H.J. and Buonanno, A. and Buscicchio, R. and Buskulic, D. and Buy, C. and Byer, R.L. and Davies, G.S.C. and Cadonati, L. and Cagnoli, G. and Cahillane, C. and Bustillo, J.C. and Callaghan, J.D. and Callister, T.A. and Calloni, E. and Cameron, J. and Camp, J.B. and Canepa, M. and Canevarolo, S. and Cannavacciuolo, M. and Cannon, K.C. and Cao, H. and Cao, Z. and Capocasa, E. and Capote, E. and Carapella, G. and Carbognani, F. and Carlin, J.B. and Carney, M.F. and Carpinelli, M. and Carrillo, G. and Carullo, G. and Carver, T.L. and Diaz, J.C. and Casentini, C. and Castaldi, G. and Caudill, S. and Cavaglià, M. and Cavalier, F. and Cavalieri, R. and Ceasar, M. and Cella, G. and Cerdá-Durán, P. and Cesarini, E. and Chaibi, W. and Chakravarti, K. and Subrahmanya, S.C. and Champion, E. and Chan, C.-H. and Chan, C. and Chan, C.L. and Chan, K. and Chan, M. and Chandra, K. and Chanial, P. and Chao, S. and Chapman-Bird, C.E.A. and Charlton, P. and Chase, E.A. and Chassande-Mottin, E. and Chatterjee, C. and Chatterjee, D. and Chatterjee, D. and Chaturvedi, M. and Chaty, S. and Chatziioannou, K. and Chen, C. and Chen, H.Y. and Chen, J. and Chen, K. and Chen, X. and Chen, Y.-B. and Chen, Y.-R. and Chen, Z. and Cheng, H. and Cheong, C.K. and Cheung, H.Y. and Chia, H.Y. and Chiadini, F. and Chiang, C.-Y. and Chiarini, G. and Chierici, R. and Chincarini, A. and Chiofalo, M.L. and Chiummo, A. and Cho, G. and Cho, H.S. and Choudhary, R.K. and Choudhary, S. and Christensen, N. and Chu, H. and Chu, Q. and Chu, Y.-K. and Chua, S. and Chung, K.W. and Ciani, G. and Ciecielag, P. and Cieślar, M. and Cifaldi, M. and Ciobanu, A.A. and Ciolfi, R. and Cipriano, F. and Cirone, A. and Clara, F. and Clark, E.N. and Clark, J.A. and Clarke, L. and Clearwater, P. and Clesse, S. and Cleva, F. and Coccia, E. and Codazzo, E. and Cohadon, P.-F. and Cohen, D.E. and Cohen, L. and Colleoni, M. and Collette, C.G. and Colombo, A. and Colpi, M. and Compton, C.M. and Constancio, M. 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Farinon, S. and Farr, B. and Farr, W.M. and Farrow, N.W. and Fauchon-Jones, E.J. and Favaro, G. and Favata, M. and Fays, M. and Fazio, M. and Feicht, J. and Fejer, M.M. and Fenyvesi, Edit and Ferguson, D.L. and Fernandez-Galiana, A. and Ferrante, I. and Ferreira, T.A. and Fidecaro, F. and Figura, P. and Fiori, I. and Fishbach, M. and Fisher, R.P. and Fittipaldi, R. and Fiumara, V. and Flaminio, R. and Floden, E. and Fong, H. and Font, J.A. and Fornal, B. and Forsyth, P.W.F. and Franke, A. and Frasca, S. and Frasconi, F. and Frederick, C. and Freed, J.P. and Frei, Zsolt and Freise, A. and Frey, R. and Fritschel, P. and Frolov, V.V. and Fronzé, G.G. and Fujii, Y. and Fujikawa, Y. and Fukunaga, M. and Fukushima, M. and Fulda, P. and Fyffe, M. and Gabbard, H.A. and Gabella, W.E. and Gadre, B.U. and Gair, J.R. and Gais, J. and Galaudage, S. and Gamba, R. and Ganapathy, D. and Ganguly, A. and Gao, D. and Gaonkar, S.G. and Garaventa, B. and García, F. and García-Núñez, C. and García-Quirós, 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and Hernandez, Vivanco F. and Heurs, M. and Hild, S. and Hill, P. and Himemoto, Y. and Hines, A.S. and Hiranuma, Y. and Hirata, N. and Hirose, E. and Hochheim, S. and Hofman, D. and Hohmann, J.N. and Holcomb, D.G. and Holland, N.A. and Holley-Bockelmann, K. and Hollows, I.J. and Holmes, Z.J. and Holt, K. and Holz, D.E. and Hong, Z. and Hopkins, P. and Hough, J. and Hourihane, S. and Howell, E.J. and Hoy, C.G. and Hoyland, D. and Hreibi, A. and Hsieh, B.-H. and Hsu, Y. and Huang, G.-Z. and Huang, H.-Y. and Huang, P. and Huang, Y.-C. and Huang, Y.-J. and Huang, Y. and Hübner, M.T. and Huddart, A.D. and Hughey, B. and Hui, D.C.Y. and Hui, V. and Husa, S. and Huttner, S.H. and Huxford, R. and Huynh-Dinh, T. and Ide, S. and Idzkowski, B. and Iess, A. and Ikenoue, B. and Imam, S. and Inayoshi, K. and Ingram, C. and Inoue, Y. and Ioka, K. and Isi, M. and Isleif, K. and Ito, K. and Itoh, Y. and Iyer, B.R. and Izumi, K. and Jaberianhamedan, V. and Jacqmin, T. and Jadhav, S.J. and Jadhav, S.P. 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	doi = {10.1103/PhysRevX.13.041039},
	journal-iso = {PHYS REV X},
	journal = {PHYSICAL REVIEW X},
	volume = {13},
	unique-id = {34539610},
	issn = {2160-3308},
	year = {2023},
	eissn = {2160-3308},
	orcid-numbers = {Barta, Dániel/0000-0001-6841-550X; Dálya, Gergely/0000-0003-3258-5763; Frei, Zsolt/0000-0002-0181-8491; Gergely, Árpád László/0000-0003-3146-6201; Raffai, Péter/0000-0001-7576-0141}
}

@inproceedings{MTMT:34515150,
	title = {Characterisation of a 200 nm Thick Liquid Jet Sheet for Ion Acceleration},
	url = {https://m2.mtmt.hu/api/publication/34515150},
	author = {Kovács, Attila Pál and Karnok, Máté and Gilinger, Tibor and Füle, Miklós Jenő and Osvay, Károly},
	booktitle = {2023 Conference on Lasers and Electro-Optics Europe & European Quantum Electronics Conference (CLEO/Europe-EQEC)},
	doi = {10.1109/CLEO/Europe-EQEC57999.2023.10232186},
	unique-id = {34515150},
	year = {2023},
	pages = {1-1},
	orcid-numbers = {Kovács, Attila Pál/0000-0001-9754-5573; Füle, Miklós Jenő/0000-0001-6996-2329; Osvay, Károly/0000-0002-3468-8312}
}

@article{MTMT:34447016,
	title = {The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX)},
	url = {https://m2.mtmt.hu/api/publication/34447016},
	author = {Liu, Chenxu and Chen, Xinlei and Er, Xinzhong and Zeimann, Gregory R. and Vinkó, József and Wheeler, J. Craig and Cooper, Erin Mentuch and Davis, Dustin and Farrow, Daniel J. and Gebhardt, Karl and Guo, Helong and Hill, Gary J. and House, Lindsay and Kollatschny, Wolfram and Kong, Fanchuan and Kumar, Brajesh and Liu, Xiangkun and Tuttle, Sarah and Endl, Michael and Duke, Parker and Cochran, William D. and Zhang, Jinghua and Liu, Xiaowei},
	doi = {10.3847/2041-8213/ad0da8},
	journal-iso = {ASTROPHYS J LETT},
	journal = {ASTROPHYSICAL JOURNAL LETTERS},
	volume = {958},
	unique-id = {34447016},
	issn = {2041-8205},
	abstract = {Supernova (SN) 2023ixf was discovered on 2023 May 19. The host galaxy, M101, was observed by the Hobby-Eberly Telescope Dark Energy Experiment collaboration over the period 2020 April 30-2020 July 10, using the Visible Integral-field Replicable Unit Spectrograph (3470 less than or similar to lambda less than or similar to 5540 angstrom) on the 10 m Hobby-Eberly Telescope. The fiber filling factor within +/- 30 '' of SN 2023ixf is 80% with a spatial resolution of 1 ''. The r < 5 ''.5 surroundings are 100% covered. This allows us to analyze the spatially resolved preexplosion local environments of SN 2023ixf with nebular emission lines. The two-dimensional maps of the extinction and the star formation rate (SFR) surface density (Sigma(SFR)) show weak increasing trends in the radial distributions within the r < 5 ''.5 regions, suggesting lower values of extinction and SFR in the vicinity of the progenitor of SN 2023ixf. The median extinction and that of the surface density of SFR within r < 3 '' are E( B - V) = 0.06 +/- 0.14, and Sigma(SFR) = 10(-5.44 +/- 0.66) M-circle dot yr(-1) arcsec(-2). There is no significant change in extinction before and after the explosion. The gas metallicity does not change significantly with the separation from SN 2023ixf. The metal-rich branch of the R-23 calculations indicates that the gas metallicity around SN 2023ixf is similar to the solar metallicity (similar to Z(circle dot)). The archival deep images from the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) show a clear detection of the progenitor of SN 2023ixf in the z band at 22.778 +/- 0.063 mag, but nondetections in the remaining four bands of CFHTLS (u, g, r, i). The results suggest a massive progenitor of approximate to 22 M-circle dot.},
	year = {2023},
	eissn = {2041-8213},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:34416888,
	title = {Search for Gravitational Waves Associated with Fast Radio Bursts Detected by CHIME/FRB during the LIGO-Virgo Observing Run O3a},
	url = {https://m2.mtmt.hu/api/publication/34416888},
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Bagnasco, S. and Bai, Y. and Baiotti, L. and Baird, J. and Bajpai, R. and Ball, M. and Ballardin, G. and Ballmer, S.W. and Balsamo, A. and Baltus, G. and Banagiri, S. and Bankar, D. and Barayoga, J.C. and Barbieri, C. and Barish, B.C. and Barker, D. and Barneo, P. and Barone, F. and Barr, B. and Barsotti, L. and Barsuglia, M. and Barta, D. and Bartlett, J. and Barton, M.A. and Bartos, I. and Bassiri, R. and Basti, A. and Bawaj, M. and Bayley, J.C. and Baylor, A.C. and Bazzan, M. and Bécsy, B. and Bedakihale, V.M. and Bejger, M. and Belahcene, I. and Benedetto, V. and Beniwal, D. and Bennett, T.F. and Bentley, J.D. and BenYaala, M. and Bergamin, F. and Berger, B.K. and Bernuzzi, S. and Berry, C.P.L. and Bersanetti, D. and Bertolini, A. and Betzwieser, J. and Beveridge, D. and Bhandare, R. and Bhardwaj, U. and Bhattacharjee, D. and Bhaumik, S. and Bilenko, I.A. and Billingsley, G. and Bini, S. and Birney, R. and Birnholtz, O. and Biscans, S. and Bischi, M. and Biscoveanu, S. and Bisht, 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	doi = {10.3847/1538-4357/acd770},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {955},
	unique-id = {34416888},
	issn = {1538-4357},
	year = {2023},
	eissn = {0004-637X},
	orcid-numbers = {Dálya, Gergely/0000-0003-3258-5763; Frei, Zsolt/0000-0002-0181-8491; Gergely, Árpád László/0000-0003-3146-6201; Raffai, Péter/0000-0001-7576-0141}
}

@{MTMT:34415284,
	title = {A Variable Output 100 Hz Laser System With Few-cycle and TW Pulses},
	url = {https://m2.mtmt.hu/api/publication/34415284},
	author = {Gaál, P. and Nagyillés, B. and Karnok, M. and Kovács, Attila Pál and Gilinger, T. and Füle, Miklós Jenő and Király, C. and Nagymihály, Roland Sándor and Seres, Imre and Tóth, Szabolcs and Osvay, Károly},
	booktitle = {2023 Conference on Lasers and Electro-Optics Europe & European Quantum Electronics Conference (CLEO/Europe-EQEC)},
	doi = {10.1109/CLEO/EUROPE-EQEC57999.2023.10232576},
	unique-id = {34415284},
	abstract = {High repetition rate target systems are inevitable to exploit fully the capabilities recent high average power high peak power laser systems [1]. The special requirements of such target systems [2] are calling for frequent experimental testing with appropriate laser sources. Ultrashort pulse laser systems operational in large scale facilities like ELI -ALPS [3] are heavily booked for secondary source developments and user experiments. Here we present a versatile laser system, which is ideal for the development of high repetition rate target systems. One arm of the system capable to provide pulses with tens ofmI energy, while the broadband few-cycle pulses from the other arm can be used for probing of the interaction area. Moreover, the temporally compressed pulses of both arms make the system ideal for generation of high harmonics and driving other secondary sources as well as for pump-probe studies of ultrafast phenomena in University environment. © 2023 IEEE.},
	keywords = {Optical pumping; Few-cycle; Laser systems; Pulse repetition rate; Secondary sources; High average power; Target systems; high repetition rate; Laser sources; Experimental testing; High peak power; Power laser systems},
	year = {2023},
	orcid-numbers = {Kovács, Attila Pál/0000-0001-9754-5573; Füle, Miklós Jenő/0000-0001-6996-2329; Tóth, Szabolcs/0000-0002-8516-3962; Osvay, Károly/0000-0002-3468-8312}
}

@article{MTMT:34271995,
	title = {Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf},
	url = {https://m2.mtmt.hu/api/publication/34271995},
	author = {Bostroem, K. Azalee and Pearson, Jeniveve and Shrestha, Manisha and Sand, David J. and Valenti, Stefano and Jha, Saurabh W. and Andrews, Jennifer E. and Smith, Nathan and Terreran, Giacomo and Green, Elizabeth and Lundquist, Michael and Haislip, Joshua and Hoang, Emily T. and Hosseinzadeh, Griffin and Janzen, Daryl and Jencson, Jacob E. and Kouprianov, Vladimir and Paraskeva, Emmy and Retamal, Nicolas E. Meza and Reichart, Daniel E. and Arcavi, Iair and Bonanos, Alceste Z. and Coughlin, Michael W. and Dobson, Ross and Farah, Joseph and Galbany, Lluis and Gutierrez, Claudia and Hawley, Suzanne and Hebb, Leslie and Hiramatsu, Daichi and Howell, D. Andrew and Iijima, Takashi and Ilyin, Ilya and Jhass, Kiran and McCully, Curtis and Moran, Sean and Morris, Brett M. and Mura, Alessandra C. and Mueller-Bravo, Tomas E. and Munday, James and Newsome, Megan and Pabst, Maria Th. and Ochner, Paolo and Gonzalez, Estefania Padilla and Pastorello, Andrea and Pellegrino, Craig and Piscarreta, Lara and Ravi, Aravind P. and Reguitti, Andrea and Salo, Laura and Vinkó, József and de Vos, Kellie and Wheeler, J. C. and Williams, G. Grant and Wyatt, Samuel},
	doi = {10.3847/2041-8213/acf9a4},
	journal-iso = {ASTROPHYS J LETT},
	journal = {ASTROPHYSICAL JOURNAL LETTERS},
	volume = {956},
	unique-id = {34271995},
	issn = {2041-8205},
	abstract = {We present the optical spectroscopic evolution of SN 2023ixf seen in subnight cadence spectra from 1.18 to 15 days after explosion. We identify high-ionization emission features, signatures of interaction with material surrounding the progenitor star, that fade over the first 7 days, with rapid evolution between spectra observed within the same night. We compare the emission lines present and their relative strength to those of other supernovae with early interaction, finding a close match to SN 2020pni and SN 2017ahn in the first spectrum and SN 2014G at later epochs. To physically interpret our observations, we compare them to CMFGEN models with confined, dense circumstellar material around a red supergiant (RSG) progenitor from the literature. We find that very few models reproduce the blended N iii (lambda lambda 4634.0,4640.6)/C iii (lambda lambda 4647.5,4650.0) emission lines observed in the first few spectra and their rapid disappearance thereafter, making this a unique diagnostic. From the best models, we find a mass-loss rate of 10-3-10-2 M circle dot yr-1, which far exceeds the mass-loss rate for any steady wind, especially for an RSG in the initial mass range of the detected progenitor. These mass-loss rates are, however, similar to rates inferred for other supernovae with early circumstellar interaction. Using the phase when the narrow emission features disappear, we calculate an outer dense radius of circumstellar material R CSM,out approximate to 5 x 1014 cm, and a mean circumstellar material density of rho = 5.6 x 10-14 g cm-3. This is consistent with the lower limit on the outer radius of the circumstellar material we calculate from the peak H alpha emission flux, R CSM,out greater than or similar to 9 x 1013 cm.},
	year = {2023},
	eissn = {2041-8213},
	orcid-numbers = {Dobson, Ross/0000-0001-5903-8159; Jhass, Kiran/0009-0007-5240-6861; Munday, James/0000-0002-1872-5398; Vinkó, József/0000-0001-8764-7832}
}