@article{MTMT:35999842,
	title = {Can circumstellar interaction explain the strange light-curve features of Type Ib/c supernovae?},
	url = {https://m2.mtmt.hu/api/publication/35999842},
	author = {Nagy, Andrea and Bodola, Zsófia Réka},
	doi = {10.1051/0004-6361/202348689},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {695},
	unique-id = {35999842},
	issn = {0004-6361},
	abstract = {The evolution and surrounding of the progenitors of stripped-envelope supernovae are still debated: some studies suggest single-star progenitors, but others prefer massive binary progenitors. Moreover, the basic physical properties of the exploding star and its interaction with circumstellar matter could significantly modify the overall light-curve features of these objects. To better understand the effect of stellar evolution and circumstellar interaction, systematic hydrodynamic calculations are needed. We test the hypothesis that circumstellar matter generated by an extreme episodic η Carinae-like eruption that occurs days or weeks before the supernova explosion may explain the differences related to the general light-curve features of stripped-envelope supernovae. We present our bolometric light-curve calculations of single-star and binary progenitors generated by hydrodynamic simulations via MESA and SNEC . We also studied the effect of an interaction with close low-mass circumstellar matter assumed to be created just a few days or weeks before the explosion. In addition to generating a model light-curve grid, we compared our results with some observational data. We found that the shape of the supernova light curve alone can indicate that the cataclysmic death of the massive star occurred in a binary system or was related to the explosion of a single star. Moreover, our study also shows that confined dense circumstellar matter may cause the strange light-curve features (bumps, rebrightening, or steeper tail) of some Type Ib/c supernovae.},
	year = {2025},
	eissn = {1432-0746}
}

@article{MTMT:36163694,
	title = {Modeling the circumstellar interaction around SN 2004gq},
	url = {https://m2.mtmt.hu/api/publication/36163694},
	author = {Nagy, Andrea and Pál, Boróka Hanga and Szalai, Tamás},
	doi = {10.1051/0004-6361/202347285},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {697},
	unique-id = {36163694},
	issn = {0004-6361},
	abstract = {Context. The relationship between the mass-loss history and final evolutionary stage of massive stars and the properties of the observable supernova (SN) is still under debate. This is especially true for stripped-envelope (Type Ib/c) SNe, where the progenitor ejects a considerably large amount of material during its evolution, which can lead to a circumstellar medium relatively close to the exploding star. Moreover, when the star explodes as a SN, this matter may contribute significantly to the generated luminosity because of the interaction. However, the trace of this circumstellar interaction can only be investigated for a couple of Type Ib/c SNe, and the nature of a close (within around 1015 cm) circumstellar matter (CSM) has also been largely unexplored for these objects. Aims. We present the results of our radio and bolometric light curve (LC) analysis related to SN 2004gq. We describe a combined model that explains the unusual LC properties of this event and supports the circumstellar interaction scenario. Methods. We computed the quasi-bolometric LC of the SN and fit this with a multicomponent model to gain information on the progenitor and the surrounding circumstellar medium. We also analyzed the available radio LCs (taken at 1.4, 4.9 and 8.5 GHz) of SN 2004gq to verify our estimated average mass-loss rate, which is one of the most crucial physical properties related to CSM models. Results. We infer reasonable parameters for SN 2004gq using radioactive decay and magnetar energy input. To power the entire LC, we must also add an extra energy source related to the CSM. We determine the most essential parameter of this medium: the average mass-loss rate from both LC and radio data fitting. We find that the suggested hidden circumstellar interaction is a viable mechanism that provides the required energy deficiency and that it can be estimated using a simple semi-analytic model. © 2025 The Authors.},
	keywords = {GIANT STARS; LIGHT CURVES; methods: analytical; PROPERTY; circumstellar matter; Supernovae; Mass loss; Circumstellar matters; circumstellar; mass loss rate; supernovae: individual: SN 1987A; methods:analytical; Supernovae: individual: SN 2004gq; Evolutionary stage; Supernova: individual: supernova 2004gq},
	year = {2025},
	eissn = {1432-0746}
}

@article{MTMT:36413344,
	title = {SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling},
	url = {https://m2.mtmt.hu/api/publication/36413344},
	author = {Vinkó, József and Bodola, Zsófia Réka and Gődény, Ákos and Csák, Szelina Fruzsina and Könyves-Tóth, Réka and Nagy, Andrea and Szalai, Tamás and Bánhidi, Dominik and Bíró, Imre Barna and Bódi, Attila and Bora, Zsófia and Csányi, István and Cseh, Borbála and Hegedüs, Tibor and Horti-Dávid, Ágoston and Joó, András Péter and Kalup, Csilla and Kriskovics, Levente and Mochnács, Erika and Pál, András and Regály, Zsolt and Seli, Bálint Attila and Sódor, Ádám and Szabó, Olivér Norton and Szakáts, Róbert and Székely, Péter and Varga, Vázsony and Vida, Krisztián},
	doi = {10.3847/1538-4357/ae0614},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {993},
	unique-id = {36413344},
	issn = {1538-4357},
	abstract = {We present new photometric observations of the core-collapse supernova SN 2023ixf occurred in M101, taken with the RC 80 and BRC80 robotic telescopes in Hungary. The initial nickel mass from the late-phase bolometric light curve extending up to 400 days after explosion, is inferred as M Ni  = 0.046 ± 0.007 M ⊙ . The comparison of the bolometric light curve with models from hydrodynamical simulations as well as semi-analytic radiative diffusion codes reveals a relatively low-mass ejecta of M ej  ≲ 9 M ⊙ , contrary to SN 2017eaw, another H-rich core-collapse event, which had M ej  ≳ 15 M ⊙ .},
	year = {2025},
	eissn = {0004-637X},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832; Gődény, Ákos/0009-0001-3178-603X; Csák, Szelina Fruzsina/0009-0000-0914-130X; Bódi, Attila/0000-0002-8585-4544; Bora, Zsófia/0000-0001-6232-9352; Horti-Dávid, Ágoston/0009-0008-2052-8474; Joó, András Péter/0000-0001-5203-434X; Seli, Bálint Attila/0000-0002-3658-2175; Szakáts, Róbert/0000-0002-1698-605X}
}

@article{MTMT:35207604,
	title = {The story of SN 2021aatd: A peculiar 1987A-like supernova with an early-phase luminosity excess},
	url = {https://m2.mtmt.hu/api/publication/35207604},
	author = {Szalai, Tamás and Könyves-Tóth, Réka and Nagy, Andrea and Hiramatsu, D. and Arcavi, I. and Bostroem, A. and Howell, D. A. and Farah, J. and McCully, C. and Newsome, M. and Padilla, Gonzalez E. and Pellegrino, C. and Terreran, G. and Berger, E. and Blanchard, P. and Gomez, S. and Székely, Péter and Bánhidi, Dominik and Bíró, Imre Barna and Csányi, István and Pál, András and Rho, J. and Vinkó, József},
	doi = {10.1051/0004-6361/202348548},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {690},
	unique-id = {35207604},
	issn = {0004-6361},
	abstract = {There is a growing number of peculiar events that cannot be assigned to any of the main supernova (SN) classes. SN 1987A and a handful of similar objects, thought to be explosive outcomes of blue supergiant stars, belong to them: while their spectra closely resemble those of H-rich (IIP) SNe, their light-curve (LC) evolution is very different. Here we present the detailed photometric and spectroscopic analysis of SN 2021aatd, a peculiar Type II explosion: while its early-time evolution resembles that of the slowly evolving, double-peaked SN 2020faa (however, at a lower luminosity scale), after $\\sim$40 days, its LC shape becomes similar to that of SN 1987A-like explosions. Beyond comparing LCs, color curves, and spectra of SN 2021aatd to that of SNe 2020faa, 1987A, and of other objects, we compare the observed spectra with our own SYN++ models and with the outputs of published radiative transfer models. We also modeled the pseudo-bolometric LCs of SNe 2021aatd and 1987A assuming a two-component (core+shell) ejecta, and involving the rotational energy of a newborn magnetar in addition to radioactive decay. We find that both the photometric and spectroscopic evolution of SN 2021aatd can be well described with the explosion of a $\\sim$15 $M_\\odot$ blue supergiant star. Nevertheless, SN 2021aatd shows higher temperatures and weaker Na ID and Ba II 6142 A lines than SN 1987A, which is reminiscent of rather to IIP-like atmospheres. With the applied two-component ejecta model (counting with both decay and magnetar energy), we can successfully describe the bolometric LC of SN 2021aatd, including the first $\\sim$40-day long phase showing an excess compared to 87A-like SNe but being strikingly similar to that of the long-lived SN 2020faa. Nevertheless, finding a unified model that also explains the LCs of more luminous events (like SN 2020faa) is still a matter of concern.},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; Astrophysics - High Energy Astrophysical Phenomena},
	year = {2024},
	eissn = {1432-0746},
	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 Bánhidi, Dominik and Bíró, Imre Barna and Csányi, István 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 = {Szakáts, Róbert/0000-0002-1698-605X; Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:32541555,
	title = {Rescued from oblivion: detailed analysis of archival Spitzer data of SN 1993J},
	url = {https://m2.mtmt.hu/api/publication/32541555},
	author = {Zsíros, Szanna and Nagy, Andrea and Szalai, Tamás},
	doi = {10.1093/mnras/stab3075},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {509},
	unique-id = {32541555},
	issn = {0035-8711},
	abstract = {We present an extensive analysis of the late-time mid-infrared (mid-IR) evolution of the Type IIb SN 1993J from 10-26 yr post-explosion based on archival - mostly previously unpublished - photometric data from the Spitzer Space Telescope in conjunction with an archival InfraRed Spectrograph spectrum. SN 1993J is one of the best-studied supernovae (SNe) with an extensive decade-long multiwavelength data set published in various papers; however, its detailed late-time mid-IR analysis is still missing from the literature. Mid-IR data follow not just the continuously cooling SN ejecta but also late-time dust-formation and circumstellar-interaction processes. We provide evidence that the observed late-time mid-IR excess of SN 1993J can be described by the presence of two-component local dust with a dust mass of ~(3.5-6.0) × 10-3 M⊙ in the case of a partly silicate-based dust composition. The source of these components could be either newly formed dust grains or heating of pre-existing dust via ongoing circumstellar matter interaction also detected at other wavelengths. If it is newly formed, the dust is assumed to be located both in the unshocked inner ejecta and in the outer cold dense shell, just as in the Cassiopeia A remnant and also assumed in other dust-forming SNe a few years after explosion.},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; circumstellar matter; infrared: stars; supernovae: general; Astrophysics - High Energy Astrophysical Phenomena; supernovae: individual: SN 1993J},
	year = {2022},
	eissn = {1365-2966},
	pages = {3235-3246}
}

@article{MTMT:32944850,
	title = {SN 2019va: a Type IIP Supernova with Large Influence of Nickel-56 Decay on the Plateau-phase Light Curve},
	url = {https://m2.mtmt.hu/api/publication/32944850},
	author = {Zhang, Xinghan and Wang, Xiaofeng and Sai, Hanna and Mo, Jun and Nagy, Andrea and Zhang, Jicheng and Cai, Yongzhi and Lin, Han and Zhang, Jujia and Baron, Eddie and DerKacy, James M. and Zhang, Tianmeng and Li, Zhitong and Graham, Melissa and Huang, Fang},
	doi = {10.1093/mnras/stac1166},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {513},
	unique-id = {32944850},
	issn = {0035-8711},
	abstract = {We present multiband photometric and spectroscopic observations of the type II supernova, (SN) 2019va, which shows an unusually flat plateau-phase evolution in its V-band light curve. Its pseudo-bolometric light curve even shows a weak brightening towards the end of the plateau phase. These uncommon features are related to the influence of Ni-56 decay on the light curve during the plateau phase, when the SN emission is usually dominated by cooling of the envelope. The inferred Ni-56 mass of SN 2019va is 0.088 +/- 0.018 M-circle dot, which is significantly larger than most SNe II. To estimate the influence of Ni-56 decay on the plateau-phase light curve, we calculate the ratio (dubbed as eta(Ni)) between the integrated time-weighted energy from Ni-56 decay and that from envelope cooling within the plateau phase, obtaining a value of 0.8 for SN 2019va, which is the second largest value among SNe II that has been measured. After removing the influence of Ni-56 decay on the plateau-phase light curve, we found that the progenitor/explosion parameters derived for SN 2019va are more reasonable. In addition, SN 2019va is found to have weaker metal lines in its spectra compared to other SNe IIP at similar epochs, implying a low-metallicity progenitor, which is consistent with the metal-poor environment inferred from the host-galaxy spectrum. We further discuss the possible reasons that might lead to SN 2019va-like events.},
	keywords = {supernovae: general; supernovae: individual (SN 2019va); galaxies: individual (UGC 08577)},
	year = {2022},
	eissn = {1365-2966},
	pages = {4556-4572}
}

@article{MTMT:31395641,
	title = {A low-luminosity core-collapse supernova very similar to SN 2005cs},
	url = {https://m2.mtmt.hu/api/publication/31395641},
	author = {Jäger, Zoltán and Vinkó, József and Bíró, Imre Barna and Hegedüs, Tibor and Borkovits, Tamás and Jäger, Zoltán Sr. and Nagy, Andrea and Molnár, László and Kriskovics, Levente},
	doi = {10.1093/mnras/staa1743},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {496},
	unique-id = {31395641},
	issn = {0035-8711},
	abstract = {We present observations and analysis of PSN J17292918+7542390, a low-luminosity Type II-P supernova (LL SN IIP). The observed sample of such events is still low, and their nature is still under debate. Such SNe are similar to SN 2005cs, a well-observed LL Type II-P event, having low expansion velocities, and small ejected 56Ni mass. We have developed a robust and relatively fast Monte Carlo code that fits semi-analytic models to light curves of core-collapse SNe. This allows the estimation of the most important physical parameters, like the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others. PSN J17292918+7542390 has $R_0 = 91_{-70}^{+119} \times 10^{11} \, \text{cm}$, $M_\text{ej} = 9.89_{-1.00}^{+2.10} \, \mathrm{ M}_{\odot }$, $E_{\mbox{kin}} = 0.65_{-0.18}^{+0.19} \, \text{foe}$, and $v_{\mbox{exp}} = 3332_{-347}^{+216}$ km s−1, for its progenitor radius, ejecta mass, kinetic energy, and expansion velocity, respectively. The initial nickel mass of the PSN J17292918+7542390 turned out to be $1.55_{-0.70}^{+0.75} \times 10^{-3} \, \mathrm{M}_{\odot }$. The measured photospheric velocity at the earliest observed phase is 7000 km s−1. As far as we can tell based on the small population of observed LL SNe IIP, the determined values are typical for these events.},
	keywords = {methods: data analysis; methods: numerical; Astrophysics - Solar and Stellar Astrophysics; techniques: photometric; Astrophysics - Instrumentation and Methods for Astrophysics; Astrophysics - High Energy Astrophysical Phenomena; instrumentation: photometers; 2012aw; supernovae: individual: PSN J17292918+7542390; 1997D; 1999em; 2004et; 2009md; 2005cs},
	year = {2020},
	eissn = {1365-2966},
	pages = {3725-3740},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832; Borkovits, Tamás/0000-0002-8806-496X}
}

@article{MTMT:30682388,
	title = {The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase},
	url = {https://m2.mtmt.hu/api/publication/30682388},
	author = {Szalai, Tamás and Vinkó, József and Könyves-Tóth, Réka and Nagy, Andrea and Bostroem, K. Azalee and Sárneczky, Krisztián and Brown, Peter J. and Pejcha, Ondrej and Bódi, Attila and Cseh, Borbála and Csörnyei, Géza and Dencs, Zoltán and Hanyecz, Ottó and Ignácz, Bernadett and Kalup, Csilla and Kriskovics, Levente and Ordasi, András and Pál, András and Seli, Bálint and Sódor, Ádám and Szakáts, Róbert and Vida, Krisztián and Zsidi, Gabriella and Konkoly, team and Arcavi, Iair and Ashall, Chris and Burke, Jamison and Galbany, Lluís and Hiramatsu, Daichi and Hosseinzadeh, Griffin and Hsiao, Eric Y. and Howell, D. Andrew and McCully, Curtis and Moran, Shane and Rho, Jeonghee and Sand, David J. and Shahbandeh, Melissa and Valenti, Stefano and Wang, Xiaofeng and Wheeler, J. Craig and Supernova, Project Global},
	doi = {10.3847/1538-4357/ab12d0},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {876},
	unique-id = {30682388},
	issn = {1538-4357},
	abstract = {The nearby SN 2017eaw is a Type II-P (“plateau”) supernova (SN) showing early-time, moderate CSM interaction. We present a comprehensive study of this SN, including the analysis of high-quality optical photometry and spectroscopy covering the very early epochs up to the nebular phase, as well as near-ultraviolet and near-infrared spectra and early-time X-ray and radio data. The combined data of SNe 2017eaw and 2004et allow us to get an improved distance to the host galaxy, NGC 6946, of D ∼ 6.85 ± 0.63 Mpc; this fits into recent independent results on the distance of the host and disfavors the previously derived (30% shorter) distances based on SN 2004et. From modeling the nebular spectra and the quasi-bolometric light curve, we estimate the progenitor mass and some basic physical parameters for the explosion and ejecta. Our results agree well with previous reports on a red supergiant progenitor star with a mass of ∼15–16 M ⊙. Our estimation of the pre-explosion mass-loss rate (\\dot{M}∼ 3× {10}-7{--}1× {10}-6{M}ȯ yr‑1) agrees well with previous results based on the opacity of the dust shell enshrouding the progenitor, but it is orders of magnitude lower than previous estimates based on general light-curve modeling of Type II-P SNe. Combining late-time optical and mid-infrared data, a clear excess at 4.5 μm can be seen, supporting the previous statements on the (moderate) dust formation in the vicinity of SN 2017eaw.},
	keywords = {supernovae: general; supernovae: individual: SN 2017eaw},
	year = {2019},
	eissn = {0004-637X},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832; Bódi, Attila/0000-0002-8585-4544; Szakáts, Róbert/0000-0002-1698-605X}
}

@article{MTMT:3366737,
	title = {Absolute Distances to Nearby Type Ia Supernovae via Light Curve Fitting Methods},
	url = {https://m2.mtmt.hu/api/publication/3366737},
	author = {Vinkó, József and Ordasi, A and Szalai, Tamás and Sarneczky, K and Banyai, E and Bíró, Imre Barna and Borkovits, Tamás and Hegedüs, Tibor and Hodosan, G and Kelemen, J and Klagyivik, Péter and Kriskovics, Levente and Kun, Emma and Marion, GH and Marschalkó, Gábor and Molnar, L and Nagy, Andrea and Pal, A and Silverman, JM and Szakáts, Róbert and Szegedi-Elek, E and Székely, Péter and Szing, Attila and Vida, K and Wheeler, JC},
	doi = {10.1088/1538-3873/aab258},
	journal-iso = {PUBL ASTRON SOC PAC},
	journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC},
	volume = {130},
	unique-id = {3366737},
	issn = {0004-6280},
	abstract = {We present a comparative study of absolute distances to a sample of very nearby, bright Type Ia supernovae (SNe) derived from high cadence, high signal-to-noise, multi-band photometric data. Our sample consists of four SNe: 2012cg, 2012ht, 2013dy and 2014J. We present new homogeneous, high-cadence photometric data in Johnson-Cousins BVRI and Sloan g' r' i' z' bands taken from two sites (Piszkesteto and Baja, Hungary), and the light curves are analyzed with publicly available light curve fitters (MLCS2k2, SNooPy2 and SALT2.4). When comparing the best-fit parameters provided by the different codes, it is found that the distance moduli of moderately reddened SNe Ia agree within less than or similar to 0.2 mag, and the agreement is even better (less than or similar to 0.1 mag) for the highest signal-to-noise BVRI data. For the highly reddened SN 2014J the dispersion of the inferred distance moduli is slightly higher. These SN-based distances are in good agreement with the Cepheid distances to their host galaxies. We conclude that the current state-of-the-art light curve fitters for Type Ia SNe can provide consistent absolute distance moduli having less than similar to 0.1-0.2 mag uncertainty for nearby SNe. Still, there is room for future improvements to reach the desired similar to 0.05 mag accuracy in the absolute distance modulus.},
	keywords = {photometry; CONSTRAINTS; extinction; ULTRAVIOLET; DUST; MAGNITUDES; DARK ENERGY; HUBBLE-SPACE-TELESCOPE; CONSTANT; HOST GALAXIES; Distances and redshifts; supernovae: individual (SN 2012cg, SN 2012ht, SN 2013dy, SN 2014J)},
	year = {2018},
	eissn = {1538-3873},
	orcid-numbers = {Vinkó, József/0000-0001-8764-7832; Borkovits, Tamás/0000-0002-8806-496X; Kun, Emma/0000-0003-2769-3591; Marschalkó, Gábor/0000-0002-7989-2704; Szakáts, Róbert/0000-0002-1698-605X}
}