TY - JOUR AU - Barna, Barnabás AU - Nagy, Andrea AU - Bora, Zs. AU - Czavalinga, Donát Róbert AU - Könyves-Tóth, Réka AU - Szalai, Tamás AU - Székely, Péter AU - Zsíros, Szanna AU - Banhidi, D. AU - Biro, I. B. AU - Csanyi, I. AU - Kriskovics, Levente AU - Pál, András AU - Szabo, Zs. M. AU - Szakáts, Róbert AU - Vida, Krisztián AU - Bodola, Zsófia Réka AU - Vinkó, József TI - Three is the magic number: Distance measurement of NGC 3147 using SN 2021hpr and its siblings JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 677 PY - 2023 PG - 16 SN - 0004-6361 DO - 10.1051/0004-6361/202346395 UR - https://m2.mtmt.hu/api/publication/34221293 ID - 34221293 AB - 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. LA - English DB - MTMT ER - TY - JOUR AU - Zhang, Xinghan AU - Wang, Xiaofeng AU - Sai, Hanna AU - Mo, Jun AU - Nagy, Andrea AU - Zhang, Jicheng AU - Cai, Yongzhi AU - Lin, Han AU - Zhang, Jujia AU - Baron, Eddie AU - DerKacy, James M. AU - Zhang, Tianmeng AU - Li, Zhitong AU - Graham, Melissa AU - Huang, Fang TI - SN 2019va: a Type IIP Supernova with Large Influence of Nickel-56 Decay on the Plateau-phase Light Curve JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY J2 - MON NOT R ASTRON SOC VL - 513 PY - 2022 IS - 3 SP - 4556 EP - 4572 PG - 17 SN - 0035-8711 DO - 10.1093/mnras/stac1166 UR - https://m2.mtmt.hu/api/publication/32944850 ID - 32944850 AB - 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. LA - English DB - MTMT ER - TY - JOUR AU - Zsíros, Szanna AU - Nagy, Andrea AU - Szalai, Tamás TI - Rescued from oblivion: detailed analysis of archival Spitzer data of SN 1993J JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY J2 - MON NOT R ASTRON SOC VL - 509 PY - 2022 SP - 3235 EP - 3246 PG - 12 SN - 0035-8711 DO - 10.1093/mnras/stab3075 UR - https://m2.mtmt.hu/api/publication/32541555 ID - 32541555 AB - 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. LA - English DB - MTMT ER - TY - JOUR AU - Jäger, Zoltán AU - Vinkó, József AU - Bíró, Imre Barna AU - Hegedüs, Tibor AU - Borkovits, Tamás AU - Jäger, Zoltán Sr. AU - Nagy, Andrea AU - Molnár, László AU - Kriskovics, Levente TI - A low-luminosity core-collapse supernova very similar to SN 2005cs JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY J2 - MON NOT R ASTRON SOC VL - 496 PY - 2020 IS - 3 SP - 3725 EP - 3740 PG - 16 SN - 0035-8711 DO - 10.1093/mnras/staa1743 UR - https://m2.mtmt.hu/api/publication/31395641 ID - 31395641 N1 - Funding Agency and Grant Number: European Union [GINOP 2.3.2-15-2016-00033]; Premium Postdoctoral Research Program of the Hungarian Academy of Sciences; Lendulet grant of the Hungarian Academy of Sciences [LP2018-7]; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; Center for High-Performance Computing at the University of Utah Funding text: This work is part of the project 'Transient Astrophysical Objects' GINOP 2.3.2-15-2016-00033 of the National Research, Development and Innovation Office (NKFIH), Hungary, funded by the European Union.; Laszlo Molnar was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has received funding from the LP2018-7 Lendulet grant of the Hungarian Academy of Sciences.; Funding for the SDSS-IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org. LA - English DB - MTMT ER - TY - JOUR AU - Szalai, Tamás AU - Vinkó, József AU - Könyves-Tóth, Réka AU - Nagy, Andrea AU - Bostroem, K. Azalee AU - Sárneczky, Krisztián AU - Brown, Peter J. AU - Pejcha, Ondrej AU - Bódi, Attila AU - Cseh, Borbála AU - Csörnyei, Géza AU - Dencs, Zoltán AU - Hanyecz, Ottó AU - Ignácz, Bernadett AU - Kalup, Csilla AU - Kriskovics, Levente AU - Ordasi, András AU - Pál, András AU - Seli, Bálint AU - Sódor, Ádám AU - Szakáts, Róbert AU - Vida, Krisztián AU - Zsidi, Gabriella AU - Konkoly, team AU - Arcavi, Iair AU - Ashall, Chris AU - Burke, Jamison AU - Galbany, Lluís AU - Hiramatsu, Daichi AU - Hosseinzadeh, Griffin AU - Hsiao, Eric Y. AU - Howell, D. Andrew AU - McCully, Curtis AU - Moran, Shane AU - Rho, Jeonghee AU - Sand, David J. AU - Shahbandeh, Melissa AU - Valenti, Stefano AU - Wang, Xiaofeng AU - Wheeler, J. Craig AU - Supernova, Project Global TI - The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase JF - ASTROPHYSICAL JOURNAL J2 - ASTROPHYS J VL - 876 PY - 2019 IS - 1 SN - 1538-4357 DO - 10.3847/1538-4357/ab12d0 UR - https://m2.mtmt.hu/api/publication/30682388 ID - 30682388 N1 - eprint: arXiv:1903.09048 eprint: arXiv:1903.09048; AB - 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. LA - English DB - MTMT ER - TY - CHAP AU - Nagy, Andrea ED - Benkő, József ED - Mizser, A TI - Az SN 1987A harminc éve, avagy a jó, a rossz és csúf szupernóva T2 - Meteor Csillagászati Évkönyv 2018. PB - Magyar Csillagászati Egyesület (MCSE) CY - Budapest PY - 2018 SP - 235 UR - https://m2.mtmt.hu/api/publication/30605340 ID - 30605340 LA - Hungarian DB - MTMT ER - TY - JOUR AU - Nagy, Andrea TI - Average Opacity Calculation for Core-collapse Supernovae JF - ASTROPHYSICAL JOURNAL J2 - ASTROPHYS J VL - 862 PY - 2018 IS - 2 PG - 11 SN - 1538-4357 DO - 10.3847/1538-4357/aace56 UR - https://m2.mtmt.hu/api/publication/3400842 ID - 3400842 AB - Supernovae (SNe) are among the most intensely studied objects of modern astrophysics, but due to their complex physical nature, theoretical models are essential to better understand these exploding stars, as well as the properties of the variation of the emitted radiation. One possibility for modeling SNe light curves (LCs) is the construction of a simplified semianalytic model, which can be used for getting order-of magnitude estimates of the SN properties. One of the strongest simplifications in most of these LC models is the assumption of the constant Thomson-scattering opacity that can be determined as the average opacity of the ejecta. Here we present a systematic analysis for estimating the average opacity in different types of core-collapse supernovae that can be used as the constant opacity of the ejecta in simplified semianalytic models. To use these average opacities self-consistently during LC fit, we estimate their values from hydrodynamic simulations. In this analysis, we first generate MESA stellar models with different physical parameters (initial mass, metallicity, and rotation), which determine the mass-loss history of the model star. Then we synthesize SN LCs from these models with the SNEC hydrodynamic code and calculate the Rosseland mean opacity in every mass element. Finally, we compute the average opacities by integrating these Rosseland mean opacities. As a result, we find that the average opacities from our calculations show adequate agreement with the opacities generally used in previous studies. LA - English DB - MTMT ER - TY - JOUR AU - Vinkó, József AU - Ordasi, A AU - Szalai, Tamás AU - Sarneczky, K AU - Banyai, E AU - Bíró, Imre Barna AU - Borkovits, Tamás AU - Hegedus, T AU - Hodosan, G AU - Kelemen, J AU - Klagyivik, Péter AU - Kriskovics, Levente AU - Kun, Emma AU - Marion, GH AU - Marschalkó, Gábor AU - Molnar, L AU - Nagy, Andrea AU - Pal, A AU - Silverman, JM AU - Szakáts, Róbert AU - Szegedi-Elek, E AU - Székely, Péter AU - Szing, A AU - Vida, K AU - Wheeler, JC TI - Absolute Distances to Nearby Type Ia Supernovae via Light Curve Fitting Methods JF - PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC J2 - PUBL ASTRON SOC PAC VL - 130 PY - 2018 IS - 988 PG - 23 SN - 0004-6280 DO - 10.1088/1538-3873/aab258 UR - https://m2.mtmt.hu/api/publication/3366737 ID - 3366737 AB - 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. LA - English DB - MTMT ER - TY - JOUR AU - Nagy, Andrea TI - Calculating the average opacity for core-collapse supernovae JF - MEMORIE DELLA SOCIETA ASTRONOMICA ITALIANA - JOURNAL OF THE ITALIAN ASTRONOMICAL SOCIETY J2 - MEMOR SOC ASTRONOM ITAL VL - 88 PY - 2017 IS - 3 SP - 274 EP - 277 PG - 4 SN - 0037-8720 UR - https://m2.mtmt.hu/api/publication/3414249 ID - 3414249 LA - English DB - MTMT ER - TY - JOUR AU - Jäger, Zoltán AU - Nagy, Andrea AU - Bíró, Imre Barna AU - Vinkó, József TI - A new supernova light curve modeling program JF - ROMANIAN ASTRONOMICAL JOURNAL J2 - ROMANIAN ASTRONOM J VL - 27 PY - 2017 SP - 203 EP - 210 PG - 8 SN - 1220-5168 UR - https://m2.mtmt.hu/api/publication/3330281 ID - 3330281 AB - Supernovae are extremely energetic explosions that highlight the violent deaths of various types of stars. Studying such cosmic explosions may be important because of several reasons. Supernovae play a key role in cosmic nucleosynthesis processes, and they are also the anchors of methods of measuring extragalactic distances. Several exotic physical processes take place in the expanding ejecta produced by the explosion. We have developed a fast and simple semi-analytical code to model the the light curve of core collapse supernovae. This allows the determination of their most important basic physical parameters, like the the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others. LA - English DB - MTMT ER -