TY  - JOUR
AU  - Hansen, Terese T.
AU  - Simon, Joshua D.
AU  - Li, Ting S.
AU  - Sharkey, Domani
AU  - Ji, Alexander P.
AU  - Thompson, Ian B.
AU  - Reggiani, Henrique M.
AU  - Galarza, Jhon Yana
TI  - Chemical Diversity on Small Scales: Abundance Analysis of the Tucana V Ultrafaint Dwarf Galaxy
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 968
PY  - 2024
SP  - 21
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad3a52
UR  - https://m2.mtmt.hu/api/publication/35220812
ID  - 35220812
AB  - The growing number of Milky Way satellites detected in recent years has introduced a new focus for stellar abundance analysis. Abundances of stars in satellites have been used to probe the nature of these systems and their chemical evolution. However, for most satellites, only centrally located stars have been examined. This paper presents an analysis of three stars in the Tucana V system, one in the inner region and two at ∼10‧ (7–10 half-light radii) from the center. We find a remarkable chemical diversity between the stars. One star exhibits enhancements in rapid neutron-capture elements (an r-I star), and another is highly enhanced in C, N, and O but with low neutron-capture abundances (a CEMP-no star). The metallicities of the stars analyzed span more than 1 dex from [Fe/H] = ‑3.55 to ‑2.46. This, combined with a large abundance range of other elements like Ca, Sc, and Ni, confirms that Tuc V is an ultrafaint dwarf (UFD) galaxy. The variation in abundances, highlighted by [Mg/Ca] ratios ranging from +0.89 to ‑0.75, among the stars demonstrates that the chemical enrichment history of Tuc V was very inhomogeneous. Tuc V is only the second UFD galaxy in which stars located at large distances from the galactic center have been analyzed, along with Tucana II. The chemical diversity seen in these two galaxies, driven by the composition of the noncentral member stars, suggests that distant member stars are important to include when classifying faint satellites and that these systems may have experienced more complex chemical enrichment histories than previously anticipated.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Arellano-Córdova, Karla Z.
AU  - Berg, Danielle A.
AU  - Mingozzi, Matilde
AU  - James, Bethan L.
AU  - Rogers, Noah S. J.
AU  - Skillman, Evan D.
AU  - Cullen, Fergus
AU  - Alexander, Ryan K.
AU  - Amorín, Ricardo O.
AU  - Chisholm, John
AU  - Hayes, Matthew
AU  - Heckman, Timothy
AU  - Hernandez, Svea
AU  - Kumari, Nimisha
AU  - Leitherer, Claus
AU  - Martin, Crystal L.
AU  - Maseda, Michael
AU  - Nanayakkara, Themiya
AU  - Parker, Kaelee
AU  - Ravindranath, Swara
AU  - Strom, Allison L.
AU  - Vincenzo, Fiorenzo
AU  - Wofford, Aida
TI  - CLASSY. IX. The Chemical Evolution of the Ne, S, Cl, and Ar Elements
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 968
PY  - 2024
SP  - 98
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad34cf
UR  - https://m2.mtmt.hu/api/publication/35220811
ID  - 35220811
AB  - To study the chemical evolution across cosmic epochs, we investigate Ne, S, Cl, and Ar abundance patterns in the Cosmic Origins Spectrograph Legacy Archive Spectroscopic SurveY (CLASSY). CLASSY comprises local star-forming galaxies (SFGs; 0.02 < z < 0.18) with enhanced star formation rates, making them strong analogues to high-z SFGs. With direct measurements of electron temperature, we derive accurate ionic abundances for all elements and assess ionization correction factors (ICFs) to account for unseen ions and derive total abundances. We find Ne/O, S/O, Cl/O, and Ar/O exhibit constant trends with gas-phase metallicity for 12+log(O/H) < 8.5 but significant correlation for Ne/O and Ar/O with metallicity for 12+log(O/H) > 8.5, likely due to ICFs. Thus, the applicability of the ICFs to integrated spectra of galaxies could bias results, underestimating true abundance ratios. Using CLASSY as a local reference, we assess the evolution of Ne/O, S/O, and Ar/O in galaxies at z > 3, finding no cosmic evolution of Ne/O, while the lack of direct abundance determinations for S/O and Ar/O can bias the interpretation of the evolution of these elements. We determine the fundamental metallicity relationship (FMR) for CLASSY and compare to the high-redshift FMR, finding no evolution. Finally, we perform the first mass–neon relationship analysis across cosmic epochs, finding a slight evolution to high Ne at later epochs. The robust abundance patterns of CLASSY galaxies and their broad range of physical properties provide essential benchmarks for interpreting the chemical enrichment of the early galaxies observed with the JWST.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Barth, Nicholas
AU  - Privon, George C.
AU  - Ezzeddine, Rana
AU  - Evans, Aaron S.
AU  - Treister, Ezequiel
TI  - Stellar Abundances at the Center of Early-type Galaxies with Fine Structure
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 968
PY  - 2024
SP  - 127
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad41b5
UR  - https://m2.mtmt.hu/api/publication/35220809
ID  - 35220809
AB  - Our understanding of early-type galaxies (ETGs) has grown in the past decade with the advance of full-spectrum fitting techniques used to infer the properties of the stellar populations that make up the galaxy. We present ages, central velocity dispersions, and abundance ratios relative to Fe of C, N, O, Mg, Si, Ca, Ti, Cr, Mn, Co, Ni, Cu, Sr, Ba, and Eu, derived using full-spectrum fitting techniques for three ETGs, NGC 2865, NGC 3818, and NGC 4915. Each of these three galaxies were selected because they have optical, disturbed structures (fine structure) that are linked to major merger events that occurred 1, 7, and 6 Gyr ago, respectively. Two of the ETGs, NGC 3818 and NGC 4915, show chemical signatures similar to ETGs without fine structure, which is consistent with a gas-poor merger of elliptical galaxies in which substantial star formation is not expected. For NGC 2865, we find a statistically higher abundance of Ca (an α element) and Cr and Mn (Fe-peak elements). We show that for NGC 2865, a simple gas-rich merger scenario fails to explain the larger abundance ratios compared to ETGs without fine structure. These three ETGs with fine structure exhibit a range of abundances, suggesting ETGs with fine structure can form via multiple pathways and types of galaxy mergers.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Manea, Catherine
AU  - Hawkins, Keith
AU  - Ness, Melissa K.
AU  - Buder, Sven
AU  - Martell, Sarah L.
AU  - Zucker, Daniel B.
TI  - Chemical Doppelgangers in GALAH DR3: The Distinguishing Power of Neutron-capture Elements among Milky Way Disk Stars
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 972
PY  - 2024
SP  - 69
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad58d9
UR  - https://m2.mtmt.hu/api/publication/35220757
ID  - 35220757
AB  - The observed chemical diversity of Milky Way stars places important constraints on Galactic chemical evolution and the mixing processes that operate within the interstellar medium. Recent works have found that the chemical diversity of disk stars is low. For example, the Apache Point Observatory Galactic Evolution Experiment (APOGEE) "chemical doppelganger rate," or the rate at which random pairs of field stars appear as chemically similar as stars born together, is high, and the chemical distributions of APOGEE stars in some Galactic populations are well-described by two-dimensional models. However, limited attention has been paid to the heavy elements (Z > 30) in this context. In this work, we probe the potential for neutron-capture elements to enhance the chemical diversity of stars by determining their effect on the chemical doppelganger rate. We measure the doppelganger rate in GALactic Archaeology with HERMES DR3, with abundances rederived using The Cannon, and find that considering the neutron-capture elements decreases the doppelganger rate from ∼2.2% to 0.4%, nearly a factor of 6, for stars with ‑0.1 < [Fe/H] < 0.1. While chemical similarity correlates with similarity in age and dynamics, including neutron-capture elements does not appear to select stars that are more similar in these characteristics. Our results highlight that the neutron-capture elements contain information that is distinct from that of the lighter elements and thus add at least one dimension to Milky Way abundance space. This work illustrates the importance of considering the neutron-capture elements when chemically characterizing stars and motivates ongoing work to improve their atomic data and measurements in spectroscopic surveys.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Lee, Sieun
AU  - Lee, Jeong-Eun
AU  - Contreras, Peña Carlos
AU  - Johnstone, Doug
AU  - Herczeg, Gregory
AU  - Lee, Seonjae
TI  - Mid-infrared Variability of Young Stellar Objects on Timescales of Days to Years
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 962
PY  - 2024
SP  - 38
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad14f8
UR  - https://m2.mtmt.hu/api/publication/34996543
ID  - 34996543
AB  - Variability in the brightness of young stellar objects (YSOs) is a common phenomenon that can be caused by changes in various factors, including accretion, extinction, disk morphology, interactions between the disk and the stellar photosphere, and the rotation of hot or cold magnetic spots on the stellar photosphere. Analyzing the variability on different timescales provides insight into the mechanisms driving the changes in the brightness of YSOs. We investigate the variability of YSOs on both long and short timescales using two mid-IR data sets: the Near-Earth Object Wide-field Infrared Survey Explorer (NEOWISE) 7.5 yr W2 (4.6 μm) data and the YSOVAR 40 day Spitzer/IRAC2 (4.5 μm) data, respectively. We classify the variability types in each timescale following Park et al. We find a higher detection rate of variable sources in the short term (77.6%) compared to the long term (43.0%) due to the higher sensitivity of the Spitzer observations. In addition, the higher cadence of the YSOVAR data results in the weeks-long short-term variability being mostly secular, while the years-long long-term variability explored with the coarsely sampled NEOWISE data is mostly stochastic. By crossmatching the two catalogs, we statistically analyze the variability types exhibited by YSOs across both timescales. The long-term variability amplitude is mostly three times (up to 10 times) greater than the short-term variability. Furthermore, we evaluate variability on very short (1–2 days) timescales and recover a trend of the increasing amplitude of variability as the timescales increase. By comprehensively analyzing the variability of YSOs over various timescales, we contribute to a deeper understanding of the underlying mechanisms driving their variability.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - El-Abd, Samer J.
AU  - Brogan, Crystal L.
AU  - Hunter, Todd R.
AU  - Lee, Kin Long Kelvin
AU  - Loomis, Ryan A.
AU  - McGuire, Brett A.
TI  - An Automated Chemical Exploration of NGC 6334I at 340 au Resolution
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 965
PY  - 2024
SP  - 14
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad283f
UR  - https://m2.mtmt.hu/api/publication/34996516
ID  - 34996516
AB  - Much of the information gleaned from observations of star-forming regions comes from the analysis of their molecular emission spectra, particularly in the radio regime. The time-consuming nature of fitting synthetic spectra to observations interactively for such line-rich sources, however, often results in such analysis being limited to data extracted from a single-dish observation or a handful of pixels from an interferometric observation. Yet, star-forming regions display a wide variety of physical conditions that are difficult, if not impossible, to accurately characterize with such a limited number of spectra. We have developed an automated fitting routine that visits every pixel in the field of view of an Atacama Large Millimeter/submillimeter Array (ALMA) data cube and determines the best-fit physical parameters, including excitation temperature and column densities, for a given list of molecules. In this proof-of-concept work, we provide an overview of the fitting routine and apply it to 0.″26, 1.1 km s‑1 resolution ALMA observations of two sites of massive star formation in NGC 6334I. Parameters were found for 21 distinct molecules by generating synthetic spectra across 7.48 GHz of spectral bandwidth between 280 and 351 GHz. Spatial images of the derived parameters for each of the >8000 pixels are presented with special attention paid to the C2H4O2 isomers and their relative variations. We highlight the greater scientific utility of the column density and velocity images of individual molecules compared to traditional moment maps of single transitions.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Li, Hui
AU  - Jiang, Wence
AU  - Yang, Zhongwei
AU  - Liu, Xiaodong
AU  - Verscharen, Daniel
AU  - Wang, Chi
TI  - Pickup Ion Modulation on Plateau-like Turbulence in the Martian Magnetosheath
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 967
PY  - 2024
SP  - 76
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad3d49
UR  - https://m2.mtmt.hu/api/publication/34889348
ID  - 34889348
AB  - The distribution of magnetic energy across scales, represented by the turbulence spectrum, provides insights into magnetic field dynamics in astrophysical and space plasma. While the Earth’s magnetosheath exhibits a conventional two-slope spectrum, the Martian magnetosheath often displays a prominent plateau-like spectrum. However, the underlying physical mechanism remains unresolved. Based on MAVEN observations, we present appealing evidence of pickup ions (PUIs) modulating the plateau-like spectrum through proton cyclotron waves (PCWs). PCWs, driven by unstable pickup H+ ion distributions, significantly influence the formation of plateau-like spectra. Both case and statistical studies suggest that the spectral evolution is affected by the relative abundance of pickup O+ ions. A substantial presence of pickup O+ ions can suppress PCWs driven by pickup H+ ions, resulting in a decline in the slope of the plateau spectrum. Particle-in-cell simulations confirm the role of PUI-modulated PCWs in the plateau-range energy injection. Our results provide new insight into the impact of PUIs on magnetic turbulence evolution and associated energy transfer processes in space and astrophysical plasma.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Morrell, N.
AU  - Phillips, M. M.
AU  - Folatelli, G.
AU  - Stritzinger, M. D.
AU  - Hamuy, M.
AU  - Suntzeff, N. B.
AU  - Hsiao, E. Y.
AU  - Taddia, F.
AU  - Burns, C. R.
AU  - Hoeflich, P.
AU  - Ashall, C.
AU  - Contreras, C.
AU  - Galbany, L.
AU  - Lu, J.
AU  - Piro, A. L.
AU  - Anais, J.
AU  - Baron, E.
AU  - Burrow, A.
AU  - Busta, L.
AU  - Campillay, A.
AU  - Castellón, S.
AU  - Corco, C.
AU  - Diamond, T.
AU  - Freedman, W. L.
AU  - Gonzalez, C.
AU  - Krisciunas, K.
AU  - Kumar, S.
AU  - Persson, S. E.
AU  - Serón, J.
AU  - Shahbandeh, M.
AU  - Torres, S.
AU  - Uddin, S. A.
AU  - Anderson, J. P.
AU  - Baltay, C.
AU  - Gall, C.
AU  - Goobar, A.
AU  - Hadjiyska, E.
AU  - Holmbo, S.
AU  - Kasliwal, M.
AU  - Lidman, C.
AU  - Marion, G. H.
AU  - Mazzali, P. A.
AU  - Nugent, P.
AU  - Perlmutter, S.
AU  - Pignata, G.
AU  - Rabinowitz, D.
AU  - Roth, M.
AU  - Ryder, S. D.
AU  - Shappee, B. J.
AU  - Vinkó, József
AU  - Wheeler, J. C.
AU  - de, Jaeger T.
AU  - Lira, P.
AU  - Ruiz, M. T.
AU  - Rich, J. A.
AU  - Prieto, J. L.
AU  - Di, Mille F.
AU  - Osip, D.
AU  - Blanc, G.
AU  - Palunas, P.
TI  - Optical Spectroscopy of Type Ia Supernovae by the Carnegie Supernova Projects I and II
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 967
PY  - 2024
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad38af
UR  - https://m2.mtmt.hu/api/publication/34883207
ID  - 34883207
AB  - We present the second and final release of optical spectroscopy of Type Ia supernovae (SNe Ia) obtained during the first and second phases of the Carnegie Supernova Project (CSP-I and CSP-II). The newly released data consist of 148 spectra of 30 SNe Ia observed in the course of CSP-I and 234 spectra of 127 SNe Ia obtained during CSP-II. We also present 216 optical spectra of 46 historical SNe Ia, including 53 spectra of 30 SNe Ia observed by the Calán/Tololo Supernova Survey. We combine these observations with previously published CSP data and publicly available spectra to compile a large sample of measurements of spectroscopic parameters at maximum light, consisting of pseudo-equivalent widths and expansion velocities of selected features for 232 CSP and historical SNe Ia (including more than 1000 spectra). Finally, we review some of the strongest correlations between spectroscopic and photometric properties of SNe Ia. Specifically, we define two samples: one consisting of SNe Ia discovered by targeted searches (most of them CSP-I objects) and the other composed of SNe Ia discovered by untargeted searches, which includes most of the CSP-II objects. The analyzed correlations are similar for both samples. We find a larger incidence of SNe Ia belonging to the cool and broad-line Branch subtypes among the events discovered by targeted searches, shallow-silicon SNe Ia are present with similar frequencies in both samples, while core normal SNe Ia are more frequent in untargeted searches.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Kwok, Lindsey A.
AU  - Siebert, Matthew R.
AU  - Johansson, Joel
AU  - Jha, Saurabh W.
AU  - Blondin, Stéphane
AU  - Dessart, Luc
AU  - Foley, Ryan J.
AU  - Hillier, D. John
AU  - Larison, Conor
AU  - Pakmor, Rüdiger
AU  - Temim, Tea
AU  - Andrews, Jennifer E.
AU  - Auchettl, Katie
AU  - Badenes, Carles
AU  - Barna, Barnabás
AU  - Bostroem, K. Azalee
AU  - Brenner, Newman Max J.
AU  - Brink, Thomas G.
AU  - Bustamante-Rosell, María José
AU  - Camacho-Neves, Yssavo
AU  - Clocchiatti, Alejandro
AU  - Coulter, David A.
AU  - Davis, Kyle W.
AU  - Deckers, Maxime
AU  - Dimitriadis, Georgios
AU  - Dong, Yize
AU  - Farah, Joseph
AU  - Filippenko, Alexei V.
AU  - Flörs, Andreas
AU  - Fox, Ori D.
AU  - Garnavich, Peter
AU  - Padilla, Gonzalez Estefania
AU  - Graur, Or
AU  - Hambsch, Franz-Josef
AU  - Hosseinzadeh, Griffin
AU  - Howell, D. Andrew
AU  - Hughes, John P.
AU  - Kerzendorf, Wolfgang E.
AU  - Saux, Xavier K.
AU  - Maeda, Keiichi
AU  - Maguire, Kate
AU  - McCully, Curtis
AU  - Mihalenko, Cassidy
AU  - Newsome, Megan
AU  - O'Brien, John T.
AU  - Pearson, Jeniveve
AU  - Pellegrino, Craig
AU  - Pierel, Justin D. R.
AU  - Polin, Abigail
AU  - Rest, Armin
AU  - Rojas-Bravo, César
AU  - Sand, David J.
AU  - Schwab, Michaela
AU  - Shahbandeh, Melissa
AU  - Shrestha, Manisha
AU  - Smith, Nathan
AU  - Strolger, Louis-Gregory
AU  - Szalai, Tamás
AU  - Taggart, Kirsty
AU  - Terreran, Giacomo
AU  - Terwel, Jacco H.
AU  - Tinyanont, Samaporn
AU  - Valenti, Stefano
AU  - Vinkó, József
AU  - Wheeler, J. Craig
AU  - Yang, Yi
AU  - Zheng, WeiKang
AU  - Ashall, Chris
AU  - DerKacy, James M.
AU  - Galbany, Lluís
AU  - Hoeflich, Peter
AU  - de, Jaeger Thomas
AU  - Lu, Jing
AU  - Maund, Justyn
AU  - Medler, Kyle
AU  - Morell, Nidia
AU  - Shappee, Benjamin J.
AU  - Stritzinger, Maximilian
AU  - Suntzeff, Nicholas
AU  - Tucker, Michael
AU  - Wang, Lifan
TI  - Ground-based and JWST Observations of SN 2022pul. II. Evidence from Nebular Spectroscopy for a Violent Merger in a Peculiar Type Ia Supernova
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 966
PY  - 2024
PG  - 18
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad2c0d
UR  - https://m2.mtmt.hu/api/publication/34842798
ID  - 34842798
AB  - We present an analysis of ground-based and JWST observations of SN 2022pul, a peculiar "03fg-like" (or "super-Chandrasekhar") Type Ia supernova (SN Ia), in the nebular phase at 338 days postexplosion. Our combined spectrum continuously covers 0.4–14 μm and includes the first mid-infrared spectrum of a 03fg-like SN Ia. Compared to normal SN Ia 2021aefx, SN 2022pul exhibits a lower mean ionization state, asymmetric emission-line profiles, stronger emission from the intermediate-mass elements (IMEs) argon and calcium, weaker emission from iron-group elements (IGEs), and the first unambiguous detection of neon in a SN Ia. A strong, broad, centrally peaked [Ne II] line at 12.81 μm was previously predicted as a hallmark of "violent merger" SN Ia models, where dynamical interaction between two sub-M Ch white dwarfs (WDs) causes disruption of the lower-mass WD and detonation of the other. The violent merger scenario was already a leading hypothesis for 03fg-like SNe Ia; in SN 2022pul it can explain the large-scale ejecta asymmetries seen between the IMEs and IGEs and the central location of narrow oxygen and broad neon. We modify extant models to add clumping of the ejecta to reproduce the optical iron emission better, and add mass in the innermost region (<2000 km s‑1) to account for the observed narrow [O I] λ λ6300, 6364 emission. A violent WD–WD merger explains many of the observations of SN 2022pul, and our results favor this model interpretation for the subclass of 03fg-like SNe Ia.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Martínez-Rodríguez, Héctor
AU  - Galbany, Lluís
AU  - Badenes, Carles
AU  - Anderson, Joseph P.
AU  - Domínguez, Inmaculada
AU  - Kuncarayakti, Hanindyo
AU  - Lyman, Joseph D.
AU  - Sánchez, Sebastián F.
AU  - Vílchez, José M.
AU  - Smith, Nathan
AU  - Milisavljevic, Dan
TI  - Recovering Lost Light: Discovery of Supernova Remnants with Integral Field Spectroscopy
JF  - ASTROPHYSICAL JOURNAL
J2  - ASTROPHYS J
VL  - 963
PY  - 2024
SP  - 125
SN  - 1538-4357
DO  - 10.3847/1538-4357/ad1bcf
UR  - https://m2.mtmt.hu/api/publication/34832424
ID  - 34832424
N1  - Department of Physics and Astronomy and Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, United States            
            Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, Barcelona, E-08193, Spain            
            Institut d’Estudis Espacials de Catalunya (IEEC), c. Gran Capità, 2-4, Barcelona, E-08034, Spain            
            European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla, Santiago, 190001, Chile            
            Millennium Institute of Astrophysics MAS, Nuncio Monsenor Sotero Sanz 100, Off. 104, Santiago, Chile            
            Departamento de Física Teórica y del Cosmos, Universidad de Granada, Granada, E-18071, Spain            
            Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Vaisalantie 20, Piikkiö, FI-21500, Finland            
            Department of Physics, University of Warwick, Coventry, CV4 7AL, United Kingdom            
            Instituto de Astronomía, Universidad Nacional Autóonoma de México, A.P. 70-264 D.F., México, C.P. 04510, Mexico            
            Instituto de Astrofísica de Andalucía—CSIC, Glorieta de la Astronomía s.n., Granada, E-18008, Spain            
            Steward Observatory, University of Arizona, 933 N. Cherry Aveue, Tucson, AZ 85721, United States            
            Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, United States            
            Integrative Data Science Initiative, Purdue University, West Lafayette, IN 47907, United States            
            Export Date: 18 July 2024
AB  - We present results from a systematic search for broad (≥ 400 km s‑1) Hα emission in integral field spectroscopy data cubes of ∼1200 nearby galaxies obtained with PMAS and MUSE. We found 19 unique regions that pass our quality cuts, four of which match the locations of previously discovered supernovae (SNe): one Type IIP and three Type IIn, including the well-known SN 2005ip. We suggest that these objects are young Supernova remnants (SNRs), with bright and broad Hα emission powered by the interaction between the SN ejecta and dense circumstellar material. The stellar ages measured at the locations of these SNR candidates are systematically lower by about 0.5 dex than those measured at the locations of core-collapse (CC) SNe, implying that their progenitors might be shorter lived and therefore more massive than a typical CCSN progenitor. The methods laid out in this work open a new window into the study of nearby SNe with integral field spectroscopy.
LA  - English
DB  - MTMT
ER  -