@article{MTMT:34618837,
	title = {Cosmological Distance Measurement of Twelve Nearby Supernovae IIP with ROTSE-IIIb},
	url = {https://m2.mtmt.hu/api/publication/34618837},
	author = {Dhungana, G. and Kehoe, R. and Staten, R. and Vinkó, József and Wheeler, J. C. and Akerlof, C. and Doss, D. and Ferrante, F. V. and Gibson, C. A. and Lasker, J. and Marion, G. H. and Pandey, S. B. and Quimby, R. M. and Rykoff, E. and Smith, D. and Yuan, F. and Zheng, W.},
	doi = {10.3847/1538-4357/ad17bc},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {962},
	unique-id = {34618837},
	issn = {1538-4357},
	abstract = {We present cosmological analysis of 12 nearby (z < 0.06) Type IIP supernovae (SNe IIP) observed with the ROTSE-IIIb telescope. To achieve precise photometry, we present a new image-differencing technique that is implemented for the first time on the ROTSE SN photometry pipeline. With this method, we find up to a 20% increase in the detection efficiency and significant reduction in residual rms scatter of the SN lightcurves when compared to the previous pipeline performance. We use the published optical spectra and broadband photometry of well-studied SNe IIP to establish temporal models for ejecta velocity and photospheric temperature evolution for our SNe IIP population. This study yields measurements that are competitive with other methods even when the data are limited to a single epoch during the photospheric phase of SNe IIP. Using the fully reduced ROTSE photometry and optical spectra, we apply these models to the respective photometric epochs for each SN in the ROTSE IIP sample. This facilitates the use of the Expanding Photosphere Method (EPM) to obtain distance estimates to their respective host galaxies. We then perform cosmological parameter fitting using these EPM distances, from which we measure the Hubble constant to be 72.9(-4.3)(+5.7)kms(-1)Mpc(-1) , which is consistent with the standard Lambda CDM model values derived using other independent techniques.},
	year = {2024},
	eissn = {0004-637X},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@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}
}

@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:34391454,
	title = {Uncovering a population of gravitational lens galaxies with magnified standard candle SN Zwicky (Jun, 10.1038/s41550-023-01981-3, 2023)},
	url = {https://m2.mtmt.hu/api/publication/34391454},
	author = {Goobar, Ariel and Johansson, Joel and Schulze, Steve and Arendse, Nikki and Carracedo, Ana Sagues and Dhawan, Suhail and Moertsell, Edvard and Fremling, Christoffer and Yan, Lin and Perley, Daniel and Sollerman, Jesper and Joseph, Remy and Hinds, K-Ryan and Meynardie, William and Andreoni, Igor and Bellm, Eric and Bloom, Josh and Collett, Thomas E. and Drake, Andrew and Graham, Matthew and Kasliwal, Mansi and Kulkarni, Shri R. and Lemon, Cameron and Miller, Adam A. and Neill, James D. and Nordin, Jakob and Pierel, Justin and Richard, Johan and Riddle, Reed and Rigault, Mickael and Rusholme, Ben and Sharma, Yashvi and Stein, Robert and Stewart, Gabrielle and Townsend, Alice and Vinkó, József and Wheeler, J. Craig and Wold, Avery},
	doi = {10.1038/s41550-023-02034-5},
	journal-iso = {NAT ASTRON},
	journal = {NATURE ASTRONOMY},
	volume = {7},
	unique-id = {34391454},
	issn = {2397-3366},
	year = {2023},
	eissn = {2397-3366},
	pages = {1137-1138},
	orcid-numbers = {Schulze, Steve/0000-0001-6797-1889; Fremling, Christoffer/0000-0002-4223-103X; Hinds, K-Ryan/0000-0002-0129-806X; Bellm, Eric/0000-0001-8018-5348; Sharma, Yashvi/0000-0003-4531-1745; Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:34351616,
	title = {Uncovering a population of gravitational lens galaxies with magnified standard candle SN Zwicky},
	url = {https://m2.mtmt.hu/api/publication/34351616},
	author = {Goobar, Ariel and Johansson, Joel and Schulze, Steve and Arendse, Nikki and Carracedo, Ana Sagués and Dhawan, Suhail and Mörtsell, Edvard and Fremling, Christoffer and Yan, Lin and Perley, Daniel and Sollerman, Jesper and Joseph, Rémy and Hinds, K. -Ryan and Meynardie, William and Andreoni, Igor and Bellm, Eric and Bloom, Josh and Collett, Thomas E. and Drake, Andrew and Graham, Matthew and Kasliwal, Mansi and Kulkarni, Shri R. and Lemon, Cameron and Miller, Adam A. and Neill, James D. and Nordin, Jakob and Pierel, Justin and Richard, Johan and Riddle, Reed and Rigault, Mickael and Rusholme, Ben and Sharma, Yashvi and Stein, Robert and Stewart, Gabrielle and Townsend, Alice and Vinkó, József and Wheeler, J. Craig and Wold, Avery},
	doi = {10.1038/s41550-023-01981-3},
	journal-iso = {NAT ASTRON},
	journal = {NATURE ASTRONOMY},
	volume = {7},
	unique-id = {34351616},
	issn = {2397-3366},
	abstract = {Detecting gravitationally lensed supernovae is among the biggest challenges in astronomy. It involves a combination of two very rare phenomena: catching the transient signal of a stellar explosion in a distant galaxy and observing it through a nearly perfectly aligned foreground galaxy that deflects light towards the observer. Here we describe how high-cadence optical observations with the Zwicky Transient Facility, with its unparalleled large field of view, led to the detection of a multiply imaged type Ia supernova, SN Zwicky, also known as SN 2022qmx. Magnified nearly 25-fold, the system was found thanks to the standard candle nature of type Ia supernovae. High-spatial-resolution imaging with the Keck telescope resolved four images of the supernova with very small angular separation, corresponding to an Einstein radius of only θE = 0.167″ and almost identical arrival times. The small θE and faintness of the lensing galaxy are very unusual, highlighting the importance of supernovae to fully characterize the properties of galaxy-scale gravitational lenses, including the impact of galaxy substructures.},
	year = {2023},
	eissn = {2397-3366},
	pages = {1098-1107},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@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}
}

@article{MTMT:34232492,
	title = {SN 2021gno: a calcium-rich transient with double-peaked light curves},
	url = {https://m2.mtmt.hu/api/publication/34232492},
	author = {Ertini, K. and Folatelli, G. and Martinez, L. and Bersten, M. C. and Anderson, J. P. and Ashall, C. and Baron, E. and Bose, S. and Brown, P. J. and Burns, C. and DerKacy, J. M. and Ferrari, L. and Galbany, L. and Hsiao, E. and Kumar, S. and Lu, J. and Mazzali, P. and Morrell, N. and Orellana, M. and Pessi, P. J. and Phillips, M. M. and Piro, A. L. and Polin, A. and Shahbandeh, M. and Shappee, B. J. and Stritzinger, M. and Suntzeff, N. B. and Tucker, M. and Elias-Rosa, N. and Kuncarayakti, H. and Gutiérrez, C. P. and Kozyreva, A. and Müller-Bravo, T. E. and Chen, T. -W. and Hinkle, J. T. and Payne, A. V. and Székely, Péter and Szalai, Tamás and Barna, Barnabás and Könyves-Tóth, Réka and Bánhidi, D. and Bíró, I. B. and Csányi, István and Kriskovics, Levente and Pál, András and Szabó, Zs and Szakáts, Róbert and Vida, Krisztián and Vinkó, József and Gromadzki, M. and Harvey, L. and Nicholl, M. and Paraskeva, E. and Young, D. R. and Englert, B.},
	doi = {10.1093/mnras/stad2705},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {526},
	unique-id = {34232492},
	issn = {0035-8711},
	abstract = {We present extensive ultraviolet (UV) and optical photometric and optical spectroscopic follow-up of supernova (SN) 2021gno by the 'Precision Observations of Infant Supernova Explosions' (POISE) project, starting less than 2 d after the explosion. Given its intermediate luminosity, fast photometric evolution, and quick transition to the nebular phase with spectra dominated by [Ca II] lines, SN 2021gno belongs to the small family of Calcium-rich transients. Moreover, it shows double-peaked light curves, a phenomenon shared with only four other Calcium-rich events. The projected distance from the centre of the host galaxy is not as large as other objects in this family. The initial optical light-curve peaks coincide with a very quick decline of the UV flux, indicating a fast initial cooling phase. Through hydrodynamical modelling of the bolometric light curve and line velocity evolution, we found that the observations are compatible with the explosion of a highly stripped massive star with an ejecta mass of $0.8\\, M_\\odot$ and a 56Ni mass of 0.024 M⊙. The initial cooling phase (first light-curve peak) is explained by the presence of an extended circumstellar material comprising ~$10^{-2}\\, {\\rm M}_{\\odot }$ with an extension of $1100\\, R_{\\odot }$. We discuss if hydrogen features are present in both maximum-light and nebular spectra, and their implications in terms of the proposed progenitor scenarios for Calcium-rich transients.},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; supernovae: general; Astrophysics - High Energy Astrophysical Phenomena; stars: massive; supernovae: individual: SN 2021gno},
	year = {2023},
	eissn = {1365-2966},
	pages = {279-298},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:34221293,
	title = {Three is the magic number: Distance measurement of NGC 3147 using SN 2021hpr and its siblings},
	url = {https://m2.mtmt.hu/api/publication/34221293},
	author = {Barna, Barnabás and Nagy, Andrea and Bora, Zs. and Czavalinga, Donát Róbert and Könyves-Tóth, Réka and Szalai, Tamás and Székely, Péter and Zsíros, Szanna and Banhidi, D. and Biro, I. B. and Csanyi, I. and Kriskovics, Levente and Pál, András and Szabo, Zs. M. and Szakáts, Róbert and Vida, Krisztián and Bodola, Zsófia Réka and Vinkó, József},
	doi = {10.1051/0004-6361/202346395},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {677},
	unique-id = {34221293},
	issn = {0004-6361},
	abstract = {Context. The nearby spiral galaxy NGC 3147 hosted three Type Ia supernovae (SNe Ia) in the past decades that have been the subjects of intense follow-up observations. Simultaneous analysis of their data provides a unique opportunity for testing different methods of light curve fitting and distance estimation.Aims. The detailed optical follow-up of SN 2021hpr allows us to revise the previous distance estimations to NGC 3147 and compare the widely used light curve fitting algorithms to each other. After the combination of the available and newly published data of SN 2021hpr, its physical properties can also be estimated with higher accuracy.Methods. We present and analyse new BVgriz and Swift photometry of SN 2021hpr to constrain its general physical properties. Together with its siblings, SNe 1997bq and 2008fv, we cross-compared the individual distance estimates of these three SNe given by the Spectral Adaptive Lightcurve Template (SALT) code, and we also checked their consistency with the results from the Multi-Color Light Curve Shape (MLCS) code. The early spectral series of SN 2021hpr was also fit with the radiative spectral code TARDIS to verify the explosion properties and constrain the chemical distribution of the outer ejecta.Results. After combining the distance estimates for the three SNe, the mean distance to their host galaxy, NGC 3127, is 42.5 +/- 1.0 Mpc, which matches with the distance inferred by the most up-to-date light curve fitters, SALT3 and BayeSN. We confirm that SN 2021hpr is a Branch-normal Type Ia SN that ejected -1.12 +/- 0.28 M-circle dot from its progenitor white dwarf and synthesized -0.44 +/- 0.14 M-circle dot of radioactive Ni-56.},
	keywords = {radiative transfer; supernovae: general; Galaxies: distances and redshifts; supernovae: individual: SN 2021hpr},
	year = {2023},
	eissn = {1432-0746},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:34212437,
	title = {Fitting Optical Light Curves of Tidal Disruption Events with TiDE},
	url = {https://m2.mtmt.hu/api/publication/34212437},
	author = {Kovács-Stermeczky, Zsófia Valéria and Vinkó, József},
	doi = {10.1088/1538-3873/acf8f8},
	journal-iso = {PUBL ASTRON SOC PAC},
	journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC},
	volume = {135},
	unique-id = {34212437},
	issn = {0004-6280},
	abstract = {A Tidal Disruption Event (TDE) occurs when a supermassive black hole tidally disrupts a nearby passing star. The fallback accretion rate of the disrupted star may exceed the Eddington limit, which induces a supersonic outflow and a burst of luminosity, similar to an explosive event. Thus, TDEs can be detected as very luminous transients, and the number of observations for such events is increasing rapidly. In this paper we fit 20 TDE light curves with TiDE, a new public, object-oriented code designed to model optical TDE light curves. We compare our results with those obtained by the popular MOSFiT and the recently developed TDEmass codes, and discuss the possible sources of differences.},
	year = {2023},
	eissn = {1538-3873},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:34203486,
	title = {From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion},
	url = {https://m2.mtmt.hu/api/publication/34203486},
	author = {Hiramatsu, Daichi and Tsuna, Daichi and Berger, Edo and Itagaki, Koichi and Goldberg, Jared A. and Gomez, Sebastian and Kishalay, De and Hosseinzadeh, Griffin and Bostroem, K. Azalee and Brown, Peter J. and Arcavi, Iair and Bieryla, Allyson and Blanchard, Peter K. and Esquerdo, Gilbert A. and Farah, Joseph and Howell, D. Andrew and Matsumoto, Tatsuya and McCully, Curtis and Newsome, Megan and Gonzalez, Estefania Padilla and Pellegrino, Craig and Rhee, Jaehyon and Terreran, Giacomo and Vinkó, József and Wheeler, J. Craig},
	doi = {10.3847/2041-8213/acf299},
	journal-iso = {ASTROPHYS J LETT},
	journal = {ASTROPHYSICAL JOURNAL LETTERS},
	volume = {955},
	unique-id = {34203486},
	issn = {2041-8205},
	abstract = {We present the discovery of the Type II supernova SN 2023ixf in M101 and follow-up photometric and spectroscopic observations, respectively, in the first month and week of its evolution. Our discovery was made within a day of estimated first light, and the following light curve is characterized by a rapid rise (≈5 days) to a luminous peak ( M V ≈ − 18.2 mag) and plateau ( M V ≈ − 17.6 mag) extending to 30 days with a fast decline rate of ≈0.03 mag day −1 . During the rising phase, U − V color shows blueward evolution, followed by redward evolution in the plateau phase. Prominent flash features of hydrogen, helium, carbon, and nitrogen dominate the spectra up to ≈5 days after first light, with a transition to a higher ionization state in the first ≈2 days. Both the U − V color and flash ionization states suggest a rise in the temperature, indicative of a delayed shock breakout inside dense circumstellar material (CSM). From the timescales of CSM interaction, we estimate its compact radial extent of ∼(3–7) × 10 14 cm. We then construct numerical light-curve models based on both continuous and eruptive mass-loss scenarios shortly before explosion. For the continuous mass-loss scenario, we infer a range of mass-loss history with 0.1–1.0 M ⊙ yr −1 in the final 2−1 yr before explosion, with a potentially decreasing mass loss of 0.01–0.1 M ⊙ yr −1 in ∼0.7–0.4 yr toward the explosion. For the eruptive mass-loss scenario, we favor eruptions releasing 0.3–1 M ⊙ of the envelope at about a year before explosion, which result in CSM with mass and extent similar to the continuous scenario. We discuss the implications of the available multiwavelength constraints obtained thus far on the progenitor candidate and SN 2023ixf to our variable CSM models.},
	year = {2023},
	eissn = {2041-8213},
	orcid-numbers = {Hiramatsu, Daichi/0000-0002-1125-9187; Tsuna, Daichi/0000-0002-6347-3089; Berger, Edo/0000-0002-9392-9681; Goldberg, Jared A./0000-0003-1012-3031; Gomez, Sebastian/0000-0001-6395-6702; Kishalay, De/0000-0002-8989-0542; Hosseinzadeh, Griffin/0000-0002-0832-2974; Bostroem, K. Azalee/0000-0002-4924-444X; Brown, Peter J./0000-0001-6272-5507; Arcavi, Iair/0000-0001-7090-4898; Bieryla, Allyson/0000-0001-6637-5401; Blanchard, Peter K./0000-0003-0526-2248; Esquerdo, Gilbert A./0000-0002-9789-5474; Farah, Joseph/0000-0003-4914-5625; Howell, D. Andrew/0000-0003-4253-656X; Matsumoto, Tatsuya/0000-0002-9350-6793; McCully, Curtis/0000-0001-5807-7893; Newsome, Megan/0000-0001-9570-0584; Gonzalez, Estefania Padilla/0000-0003-0209-9246; Pellegrino, Craig/0000-0002-7472-1279; Rhee, Jaehyon/0000-0001-9214-7437; Terreran, Giacomo/0000-0003-0794-5982; Vinkó, József/0000-0001-8764-7832; Wheeler, J. Craig/0000-0003-1349-6538}
}