@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:34672842,
	title = {Ionized regions in the central arcsecond of NGC 1068 YJHK spatially resolved spectroscopy},
	url = {https://m2.mtmt.hu/api/publication/34672842},
	author = {Vermot, P. and Barna, Barnabás and Ehlerova, S. and Morris, M. R. and Palous, J. and Wunsch, R.},
	doi = {10.1051/0004-6361/202347227},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {678},
	unique-id = {34672842},
	issn = {0004-6361},
	keywords = {Ism: clouds; Galaxies: active; galaxies: nuclei; infrared: ISM; galaxies: individual: NGC 1068},
	year = {2023},
	eissn = {1432-0746}
}

@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:34116921,
	title = {Over 500 Days in the Life of the Photosphere of the Type Iax Supernova SN 2014dt},
	url = {https://m2.mtmt.hu/api/publication/34116921},
	author = {Camacho-Neves, Yssavo and Jha, Saurabh W. and Barna, Barnabás and Dai, Mi and Filippenko, Alexei V. and Foley, Ryan J. and Hosseinzadeh, Griffin and Howell, D. Andrew and Johansson, Joel and Kelly, Patrick L. and Kerzendorf, Wolfgang E. and Kwok, Lindsey A. and Larison, Conor and Magee, Mark R. and McCully, Curtis and O'Brien, John T. and Pan, Yen-Chen and Pandya, Viraj and Singhal, Jaladh and Stahl, Benjamin E. and Szalai, Tamás and Wieber, Meredith and Williamson, Marc},
	doi = {10.3847/1538-4357/acd558},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {951},
	unique-id = {34116921},
	issn = {1538-4357},
	abstract = {Type Iax supernovae (SNe Iax) are the largest known class of peculiar white dwarf SNe, distinct from normal Type Ia supernovae (SNe Ia). The unique properties of SNe Iax, especially their strong photospheric lines out to extremely late times, allow us to model their optical spectra and derive the physical parameters of the long-lasting photosphere. We present an extensive spectral timeseries, including 21 new spectra, of SN Iax 2014dt from +11 to +562 days after maximum light. We are able to reproduce the entire timeseries with a self-consistent, nearly unaltered deflagration explosion model from Fink et al. using TARDIS, an open source radiative-transfer code. We find that the photospheric velocity of SN 2014dt slows its evolution between +64 and +148 days, which closely overlaps the phase when we see SN 2014dt diverge from the normal spectral evolution of SNe Ia (+90 to +150 days). The photospheric velocity at these epochs, ~400-1000 km s-1, may demarcate a boundary within the ejecta below which the physics of SNe Iax and normal SNe Ia differ. Our results suggest that SN 2014dt is consistent with a weak deflagration explosion model that leaves behind a bound remnant and drives an optically thick, quasi-steady-state wind creating the photospheric lines at late times. The data also suggest that this wind may weaken at epochs past +450 days, perhaps indicating a radioactive power source that has decayed away.},
	keywords = {radiative transfer; Astrophysics - Solar and Stellar Astrophysics; Supernovae; Astrophysics - High Energy Astrophysical Phenomena; Type Ia supernovae; 1728; 1668; Radiative transfer simulations; Supernova dynamics; 1335; 1967; 1664},
	year = {2023},
	eissn = {0004-637X}
}

@article{MTMT:34116920,
	title = {Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg},
	url = {https://m2.mtmt.hu/api/publication/34116920},
	author = {Singh, Mridweeka and Sahu, Devendra. K. and Dastidar, Raya and Barna, Barnabás and Misra, Kuntal and Gangopadhyay, Anjasha and Howell, D. Andrew and Jha, Saurabh W. and Im, Hyobin and Taggart, Kirsty and Andrews, Jennifer and Hiramatsu, Daichi and Teja, Rishabh Singh and Pellegrino, Craig and Foley, Ryan J. and Joshi, Arti and Anupama, G. C. and Bostroem, K. Azalee and Burke, Jamison and Camacho-Neves, Yssavo and Dutta, Anirban and Kwok, Lindsey A. and McCully, Curtis and Pan, Yen-Chen and Siebert, Matt and Srivastav, Shubham and Szalai, Tamás and Swift, Jonathan J. and Yang, Grace and Zhou, Henry and DiLullo, Nico and Scheer, Jackson},
	doi = {10.3847/1538-4357/acd559},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {953},
	unique-id = {34116920},
	issn = {1538-4357},
	abstract = {We present the optical photometric and spectroscopic analysis of two Type Iax supernovae (SNe), 2018cni and 2020kyg. SN 2018cni is a bright Type Iax SN (M V,peak = -17.81 ± 0.21 mag), whereas SN 2020kyg (M V,peak = -14.52 ± 0.21 mag) is a faint one. We derive 56Ni mass of 0.07 and 0.002 M ⊙ and ejecta mass of 0.48 and 0.14 M ⊙ for SNe 2018cni and 2020kyg, respectively. A combined study of the bright and faint Type Iax SNe in R/r-band reveals that the brighter objects tend to have a longer rise time. However, the correlation between the peak luminosity and decline rate shows that bright and faint Type Iax SNe exhibit distinct behavior. Comparison with standard deflagration models suggests that SN 2018cni is consistent with the deflagration of a CO white dwarf, whereas the properties of SN 2020kyg can be better explained by the deflagration of a hybrid CONe white dwarf. The spectral features of both the SNe point to the presence of similar chemical species but with different mass fractions. Our spectral modeling indicates stratification at the outer layers and mixed inner ejecta for both of the SNe.},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; Supernovae; Astrophysics - High Energy Astrophysical Phenomena; 1668},
	year = {2023},
	eissn = {0004-637X}
}

@article{MTMT:34095108,
	title = {A 3D model for the stellar populations in the nuclei of NGC 1433, NGC 1566, and NGC 1808. NIR photometry, CO absorption lines, and line-of-sight velocity and its dispersion},
	url = {https://m2.mtmt.hu/api/publication/34095108},
	author = {Vermot, P. and Palouš, J. and Barna, Barnabás and Ehlerová, S. and Morris, M. R. and Wünsch, R.},
	doi = {10.1051/0004-6361/202245627},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {674},
	unique-id = {34095108},
	issn = {0004-6361},
	abstract = {Aims. We aim to characterize the properties of the stellar populations in the central few hundred parsecs of nearby galactic nuclei; specifically their age, mass, and 3D geometry.},
	year = {2023},
	eissn = {1432-0746},
	orcid-numbers = {Vermot, P./0000-0002-6126-3264}
}

@article{MTMT:33601645,
	title = {A JWST Near- and Mid-Infrared Nebular Spectrum of the Type Ia Supernova 2021aefx},
	url = {https://m2.mtmt.hu/api/publication/33601645},
	author = {Kwok, Lindsey A. and Jha, Saurabh W. and Temim, Tea and Fox, Ori D. and Larison, Conor and Camacho-Neves, Yssavo and Brenner, Newman Max J. and Pierel, Justin D. R. and Foley, Ryan J. and Andrews, Jennifer E. and Badenes, Carles and Barna, Barnabás and Bostroem, K. Azalee and Deckers, Maxime and Flors, Andreas and Garnavich, Peter and Graham, Melissa L. and Graur, Or and Hosseinzadeh, Griffin and Howell, D. Andrew and Hughes, John P. and Johansson, Joel and Kendrew, Sarah and Kerzendorf, Wolfgang E. and Maeda, Keiichi and Maguire, Kate and McCully, Curtis and O'Brien, John T. and Rest, Armin and Sand, David J. and Shahbandeh, Melissa and Strolger, Louis-Gregory and Szalai, Tamás and Ashall, Chris and Baron, E. and Burns, Chris R. and DerKacy, James M. and Mera, Evans Tyco and Fisher, Alec and Galbany, Lluis and Hoeflich, Peter and Hsiao, Eric and de, Jaeger Thomas and Karamehmetoglu, Emir and Krisciunas, Kevin and Kumar, Sahana and Lu, Jing and Maund, Justyn and Mazzali, Paolo A. and Medler, Kyle and Morrell, Nidia and Phillips, Mark. M. and Shappee, Benjamin J. and Stritzinger, Maximilian and Suntzeff, Nicholas and Telesco, Charles and Tucker, Michael and Wang, Lifan},
	doi = {10.3847/2041-8213/acb4ec},
	journal-iso = {ASTROPHYS J LETT},
	journal = {ASTROPHYSICAL JOURNAL LETTERS},
	volume = {944},
	unique-id = {33601645},
	issn = {2041-8205},
	abstract = {We present JWST near- and mid-infrared spectroscopic observations of the nearby normal Type Ia supernova SN 2021aefx in the nebular phase at $+255$ days past maximum light. Our Near Infrared Spectrograph (NIRSpec) and Mid Infrared Instrument (MIRI) observations, combined with ground-based optical data from the South African Large Telescope (SALT), constitute the first complete optical $+$ NIR $+$ MIR nebular SN Ia spectrum covering 0.3$-$14 $\\mu$m. This spectrum unveils the previously unobserved 2.5$-$5 $\\mu$m region, revealing strong nebular iron and stable nickel emission, indicative of high-density burning that can constrain the progenitor mass. The data show a significant improvement in sensitivity and resolution compared to previous Spitzer MIR data. We identify numerous NIR and MIR nebular emission lines from iron-group elements and as well as lines from the intermediate-mass element argon. The argon lines extend to higher velocities than the iron-group elements, suggesting stratified ejecta that are a hallmark of delayed-detonation or double-detonation SN Ia models. We present fits to simple geometric line profiles to features beyond 1.2 $\\mu$m and find that most lines are consistent with Gaussian or spherical emission distributions, while the [Ar III] 8.99 $\\mu$m line has a distinctively flat-topped profile indicating a thick spherical shell of emission. Using our line profile fits, we investigate the emissivity structure of SN 2021aefx and measure kinematic properties. Continued observations of SN 2021aefx and other SNe Ia with JWST will be transformative to the study of SN Ia composition, ionization structure, density, and temperature, and will provide important constraints on SN Ia progenitor and explosion models.},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; Astrophysics - High Energy Astrophysical Phenomena},
	year = {2023},
	eissn = {2041-8213}
}

@article{MTMT:33641343,
	title = {FLASH-light on the RING: hydrodynamic simulations of expanding supernova shells near supermassive black holes},
	url = {https://m2.mtmt.hu/api/publication/33641343},
	author = {Barna, Barnabás and Palouš, J. and Ehlerová, S. and Wünsch, R. and Morris, M. R. and Vermot, P.},
	doi = {10.1093/mnras/stab3723},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {510},
	unique-id = {33641343},
	issn = {0035-8711},
	abstract = {The way supermassive black holes (SMBHs) in Galactic Centres (GCs) accumulate their mass is not completely determined. At large scales, it is governed by galactic encounters, mass inflows connected to spirals arms and bars, or due to expanding shells from supernova (SN) explosions in the central parts of galaxies. The investigation of the latter process requires an extensive set of gas dynamical simulations to explore the multidimensional parameter space needed to frame the phenomenon. The aims of this paper are to extend our investigation of the importance of SNe for inducing accretion on to an SMBH and carry out a comparison between the fully hydrodynamic code FLASH and the much less computationally intensive code RING, which uses the thin shell approximation. We simulate 3D expanding shells in a gravitational potential similar to that of the GC with a variety of homogeneous and turbulent environments. In homogeneous media, we find convincing agreement between FLASH and RING in the shapes of shells and their equivalent radii throughout their whole evolution until they become subsonic. In highly inhomogeneous, turbulent media, there is also a good agreement of shapes and sizes of shells, and of the times of their first contact with the central 1-pc sphere, where we assume that they join the accretion flow. The comparison supports the proposition that an SN occurring at a galactocentric distance of 5 pc typically drives 1-3 M⊙ into the central 1 pc around the GC.},
	keywords = {galaxies: ISM; galaxies: evolution; Galaxies: active; ISM: supernova remnants; Astrophysics - Astrophysics of Galaxies; Galaxy: centre; transients: supernovae},
	year = {2022},
	eissn = {1365-2966},
	pages = {5266-5279}
}

@article{MTMT:33641342,
	title = {How to create Sgr A East. Where did the supernova explode?},
	url = {https://m2.mtmt.hu/api/publication/33641342},
	author = {Ehlerová, S. and Palouš, J. and Morris, M. R. and Wünsch, R. and Barna, Barnabás and Vermot, P.},
	doi = {10.1051/0004-6361/202244682},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {668},
	unique-id = {33641342},
	issn = {0004-6361},
	abstract = {Context. Sgr A East is the supernova remnant closest to the centre of the Milky Way. Its age has been estimated to be either very young, around 1-2 kyr, or about 10 kyr, and its exact origin remains unclear. Aims: We aspire to create a simple model of a supernova explosion that reproduces the shape, size, and location of Sgr A East. Methods: Using a simplified hydrodynamical code, we simulated the evolution of a supernova remnant in the medium around the Galactic centre. The latter consists of a nearby massive molecular cloud with which Sgr A East is known to be interacting and a wind from the nuclear star cluster. Results: Our preferred models of the Sgr A East remnant are compatible with an age of around 10 kyr. We also find suitable solutions for older ages, but not for ages younger than 5 kyr. Our simulations predict that the supernova exploded at a distance of about 3.5 pc from the Galactic centre, below the Galactic plane, slightly eastwards from the centre and 3 pc behind it.},
	keywords = {ISM: supernova remnants; Galaxy: center; Astrophysics - Astrophysics of Galaxies; ISM: individual objects: Sgr A East},
	year = {2022},
	eissn = {1432-0746}
}