Imagen (Image).

Supernova

Memoria Digital Vasca = Euskal Memoria Digitala
oai:www.memoriadigitalvasca.eus:10357/42903
Memoria Digital Vasca = Euskal Memoria Digitala
  • Toledo, Manuel
Exposición, Técnica: Esmalte, Materia-soporte: Tablex, Fecha de ejecución: 1978, Obra abstracta, manchas blancas sobre fondo rojo y figuras en la parte inferior., Firmado y fechado en ángulo inferior izquierdo.
 
DOI: http://hdl.handle.net/10357/42903
Memoria Digital Vasca = Euskal Memoria Digitala
oai:www.memoriadigitalvasca.eus:10357/42903

HANDLE: http://hdl.handle.net/10357/42903
Memoria Digital Vasca = Euskal Memoria Digitala
oai:www.memoriadigitalvasca.eus:10357/42903
 
Ver en: http://hdl.handle.net/10357/42903
Memoria Digital Vasca = Euskal Memoria Digitala
oai:www.memoriadigitalvasca.eus:10357/42903

Recercat. Dipósit de la Recerca de Catalunya
oai:recercat.cat:2072/49988
Artículo científico (article).

SUPERNOVA MATTER: A SEMICLASSICAL APPROACH

Recercat. Dipósit de la Recerca de Catalunya
  • Pi Pericay, Martí
  • Viñas Gausí, Xavier
  • Barranco Gómez, Manuel
  • Polls Martí, Artur
  • Pérez-Canyellas, A.
A well-established semiclassical method is used to systematically study the properties of hot dense matter in the conditions prevailing during the gravitational collapse of massive stars. Different semiclassical kinetic energy and entropy densities are discussed. Detailed results for different nuclear forces having different nucleon effective mass and nuclear incompressibility are presented. Plasma effects (translational and vibrational energies and Coulomb excess) are considered for a typical adiabat. The results presented here cover a wide range in entropy per baryon and electron concentration per baryon, for baryon densities ranging from 0.001/cu fm to 0.3/cu fm.




Recercat. Dipósit de la Recerca de Catalunya
oai:recercat.cat:2072/368810
Artículo científico (article).

INTERACTION OF HEMISPHERICAL BLAST WAVES WITH INHOMOGENEOUS SPHERES: PROBING THE COLLISION OF A SUPERNOVA EJECTA WITH A NEARBY COMPANION STAR IN THE LABORATORY

Recercat. Dipósit de la Recerca de Catalunya
  • García Senz, Domingo
  • Velarde, Pedro
  • Suzuki Vidal, Francisco
  • Stehlé, Chantal
  • Cotelo Ferreiro, Manuel
  • Portillo García, David
  • Plewa, Tomasz
  • Pak, Arthur
Past laboratory experiments at high energy density have provided insights into the physics of supernovae, supernovaremnants, and the destruction of interstellar clouds. In a typical experimental setting, a laser-driven planar blast waveinteracts with a compositionally homogeneous spherical or cylindrical target. In this work we propose a new laboratoryplatform that accounts for curvature ofthe impacting shock and density stratification of the target. Both characteristicsreflect the conditions expected to exist shortly after a supernova explosion in a close binary system. We provide detailsof a proposed experimental design(laser drive, target configuration, diagnostic system), optimized to capture the keyproperties of recent ejecta–companion interaction models.Good qualitative agreement found between our experimentalmodels and their astrophysical counterparts highlights the strong potential of the proposed design to probe details of theejecta–companion interaction for broad classes of objects by means of laboratory experiments at high energy density, Peer Reviewed




Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/146412
Artículo científico (article). 2017

NEARBY SUPERNOVA HOST GALAXIES FROM THE CALIFA SURVEY: II. SUPERNOVA ENVIRONMENTAL METALLICITY

Digital.CSIC. Repositorio Institucional del CSIC
  • Galbany, Lluís
  • García-Benito, Rubén
  • González Delgado, Rosa M.
  • Kehrig, C.
  • Pérez Jiménez, Enrique
  • Vílchez Medina, José Manuel
The metallicity of a supernova progenitor, together with its mass, is one of the main parameters that can rule the progenitor's fate. We present the second study of nearby supernova (SN) host galaxies (0.005 <z< 0.03) using integral field spectroscopy (IFS) from the CALIFA survey. We analyze the metallicity of 115 galaxies, which hosted 132 SNe within and 10 SNe outside the field of view (FoV) of the instrument. Another 18 galaxies, which hosted only SNe outside the FoV, were also studied. Using the O3N2 calibrator that was described elsewhere, we found no statistically significant differences between the gas-phase metallicities at the locations of the three main SN types - Ia, Ib/c and II; they all have 12 + log (O/H) ≃ 8.50 within 0.02 dex. The total galaxy metallicities are also very similar, and we argue that the reason is that our sample only consists of SNe discovered in massive galaxies (log (M/M) > 10 dex) by targeted searches. We neither found evidence that the metallicity at the SN location differs from the average metallicity at the galactocentric distance of the SNe. By extending our SN sample with published metallicities at the SN location, we are able to study the metallicity distributions for all SN subtypes split into SN discovered in targeted and untargeted searches. We confirm a bias toward higher host masses and metallicities in the targeted searches. By combining data from targeted and untargeted searches, we found a sequence from higher to lower local metallicity: SN Ia, Ic, and II show the highest metallicity, which is significantly higher than those of SN Ib, IIb, and Ic-BL. Our results support the scenario according to which SN Ib result from binary progenitors. Additionally, at least part of the SN Ic are the result of single massive stars that were stripped of their outer layers by metallicity-driven winds. We studied several proxies of the local metallicity that are frequently used in the literature and found that the total host metallicity allows estimating the metallicity at the SN location with an accuracy better than 0.08 dex and very small bias. In addition, weak AGNs that cannot be seen in the total spectrum may weakly bias (by 0.04 dex) the metallicity estimate that is derived from the galaxy-integrated spectrum. © ESO, 2016., This work was partly funded by FCT with the research grant PTDC/CTE-AST/112582/2009. Support for L.G. is partially provided by FCT, by CONICYT through FONDECYT grant 3140566, and from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics (MAS). V.S. acknowledges financial support from Fundacao para a Ciencia e a Tecnologia (FCT) under program Ciencia 2008. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912., Peer Reviewed

Proyecto: EC/FP7/303912



Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/164473
Artículo científico (article). 2018

ELEMENTAL GAS-PHASE ABUNDANCES OF INTERMEDIATE REDSHIFT TYPE IA SUPERNOVA STAR-FORMING HOST GALAXIES

Digital.CSIC. Repositorio Institucional del CSIC
  • Moreno-Raya, M.E.
  • Galbany, Lluís
  • López-Sánchez, R.
  • Mollá, M.
  • González-Gaitán, Santiago
  • Vílchez Medina, José Manuel
  • Carnero, A.
The maximum luminosity of type Ia supernovae (SNe Ia) depends on the oxygen abundance of the regions of the host galaxies, where they explode. This metallicity dependence reduces the dispersion in the Hubble diagram (HD) when included with the traditional two-parameter calibration of SN Ia light-curve parameters and absolute magnitude. In this work, we use empirical calibrations to carefully estimate the oxygen abundance of galaxies hosting SNe Ia from the SDSS-II/SN (Sloan Digital Sky Survey-II Supernova) survey at intermediate redshift by measuring their emission-line intensities. We also derive electronic temperature with the direct method for a small fraction of objects for consistency. We find a trend of decreasing oxygen abundance with increasing redshift for the most massive galaxies. Moreover, we study the dependence of the HD residuals (HR) with galaxy oxygen abundance obtaining a correlation in line with those found in other works. In particular, the HR versus oxygen abundance shows a slope of -0.186± 0.123 mag dex (1.52σ) in good agreement with theoretical expectations. This implies smaller distance modulii after corrections for SNe Ia in metal-rich galaxies. Based on our previous results on local SNe Ia, we propose this dependence to be due to the lower luminosity of the SNe Ia produced in more metal-rich environments.© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society., This work has been supported by Direccion General de Investigacion Cientifica y Tecnica (DGICYT) and Ministerio de Economia y Competitividad (MINECO) grants AYA2010-21887-C04-02 and AYA2013-47742-C4-4-P., Peer Reviewed




Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/214121
Artículo científico (article). 2020

PISCO: THE PMAS/PPAK INTEGRAL-FIELD SUPERNOVA HOSTS COMPILATION

Digital.CSIC. Repositorio Institucional del CSIC
  • Galbany, Lluís
  • Anderson, Joseph P.
  • Sánchez, S. F.
  • Kuncarayakti, Hanindyo
  • Pedraz, S.
  • González-Gaitán, Santiago
  • Stanishev, V.
  • Domínguez, I.
  • Moreno-Raya, M.E.
  • Wood-Vasey, W. M.
  • Mourão, A. M.
  • Ponder, K. A.
  • Badenes, C.
  • Mollá, M.
  • López-Sánchez, A.R.
  • Rosales-Ortega, F. F.
  • Vílchez Medina, José Manuel
  • García-Benito, Rubén
  • Marino, R.A.
We present the PMAS/PPak Integral-field Supernova hosts COmpilation (PISCO), which comprises integral field spectroscopy (IFS) of 232 supernova (SN) host galaxies that hosted 272 SNe, observed over several semesters with the 3.5 m telescope at the Calar Alto Observatory (CAHA). PISCO is the largest collection of SN host galaxies observed with wide-field IFS, totaling 466,347 individual spectra covering a typical spatial resolution of ∼380 pc. Focused studies regarding specific SN Ia-related topics will be published elsewhere; this paper aims to present the properties of the SN environments, using stellar population (SP) synthesis, and the gas-phase interstellar medium, providing additional results separating stripped-envelope SNe into their subtypes. With 11,270 H ii regions detected in all galaxies, we present for the first time a statistical analysis of H ii regions, which puts H ii regions that have hosted SNe in context with all other star-forming clumps within their galaxies. SNe Ic are associated with environments that are more metal-rich and have higher EW(Hα) and higher star formation rate within their host galaxies than the mean of all H ii regions detected within each host. This in contrast to SNe IIb, which occur in environments that are very different compared to other core-collapse SNe types. We find two clear components of young and old SPs at SNe IIn locations. We find that SNe II fast decliners tend to explode at locations where the Σ is more intense. Finally, we outline how a future dedicated IFS survey of galaxies in parallel to an untargeted SN search would overcome the biases in current environmental studies.© 2018. The American Astronomical Society. All rights reserved., We are greatly in debt to the Calar Alto Observatory staff because without their kindness and interest for this project, most of the observations would have not been possible. We are greatly thankful to Yao-Yuan Mao for being behind most of the Python coding developed for plotting our results, as well as to Or Graur for useful discussions. L.G. and W.M.W.-V. were supported in part by the US National Science Foundation under Grant AST-1311862. I.D. is funded by the MINECO-FEDER AYA2015-63588-P grant. Escrit en la seva major part a cavall de la Biblioteca de Palafrugell i la Platgeta de Calella. Based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie (MPIA) and the Instituto de Astrofisica de Andalucia (CSIC). This study makes use of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://www.caha.es/CALIFA/). The STARLIGHT project is supported by the Brazilian agencies CNPq, CAPES, and FAPESP, and by the France-Brazil CAPES/Cofecub program. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and data products from the SDSS and Pan-STARRS surveys. Funding for the Sloan Digital Sky Survey 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. http://www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofisica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur Astronomie (MPIA Heidelberg), Max-Planck-Institut fur Astrophysik (MPA Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatario Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autonoma de Mexico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.




Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/275115
Artículo científico (article). 2022

APERTURE-CORRECTED SPECTROSCOPIC TYPE IA SUPERNOVA HOST GALAXY PROPERTIES

Digital.CSIC. Repositorio Institucional del CSIC
  • Galbany, Lluís
  • Smith, Mathew
  • Duarte Puertas, Salvador
  • González-Gaitán, Santiago
  • Pessa, Ismael
  • Sako, Masao
  • Iglesias-Páramo, J.
  • López-Sánchez, A.R.
  • Mollá, Mercedes
  • Vílchez Medina, José Manuel
We use type Ia supernova (SN Ia) data obtained by the Sloan Digital Sky Survey-II Supernova Survey (SDSS-II SNS) in combination with the publicly available SDSS DR16 fiber spectroscopy of supernova (SN) host galaxies to correlate SN Ia light-curve parameters and Hubble residuals with several host galaxy properties. Fixed-aperture fiber spectroscopy suffers from aperture effects: the fraction of the galaxy covered by the fiber varies depending on its projected size on the sky, and thus measured properties are not representative of the whole galaxy. The advent of integral field spectroscopy has provided a way to correct the missing light, by studying how these galaxy parameters change with the aperture size. Here we study how the standard SN host galaxy relations change once global host galaxy parameters are corrected for aperture effects. We recover previous trends on SN Hubble residuals with host galaxy properties, but we find that discarding objects with poor fiber coverage instead of correcting for aperture loss introduces biases into the sample that affect SN host galaxy relations. The net effect of applying the commonly used g-band fraction criterion is that intrinsically faint SNe Ia in high-mass galaxies are discarded, thus artificially increasing the height of the mass step by 0.02 mag and its significance. Current and next-generation fixed-aperture fiber-spectroscopy surveys, such as OzDES, DESI, or TiDES with 4MOST, that aim to study SN and galaxy correlations must consider, and correct for, these effects. © ESO 2022., L.G. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Social Fund (ESF) “Investing in your future” under the 2019 Ramón y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, and from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016. M.S. is funded by the European Reearch Council (ERC) under the European Union’s Horizon 2020 Research and Innovation program (grant agreement no 759194 – USNAC). S.D.P. is grateful to the Fonds de Recherche du Québec – Nature et Technologies. SGG acknowledges support by FCT under Project CRISP PTDC/FIS-AST-31546/2017 and Project No. UIDB/00099/2020. S.D.P., J.I.P., J.M.V. acknowledge support from the Spanish Ministerio de Economía y Competitividad under grant PID2019-107408GB-C44, and Junta de Andalucía Excellence Project P18-FR-2664, and from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). Escrit en part al Bellver, prop del mugró del Tagamanent, sobre la vall de ciment malalta (J.G., center forward)., Peer reviewed




Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/357729
Artículo científico (article). 2024

RECOVERING LOST LIGHT: DISCOVERY OF SUPERNOVA REMNANTS WITH INTEGRAL FIELD SPECTROSCOPY

Digital.CSIC. Repositorio Institucional del CSIC
  • Martínez-Rodríguez, Héctor
  • Galbany, Lluís
  • Badenes, Carles
  • Anderson, Joseph P.
  • Domínguez, Inmaculada
  • Kuncarayakti, Hanindyo
  • Lyman, Joseph D.
  • Sánchez, Sebastián F.
  • Vílchez Medina, José Manuel
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., We acknowledge useful discussions with Sedona Price and Evan Schneider. H.M.-R. and C.B. are funded by the NASA ADAP grant NNX15AM03G S01. H.M.-R. also acknowledges support from a PITT PACC, a Zaccheus Daniel and a Kenneth P. Dietrich School of Arts & Sciences Predoctoral Fellowship. L.G. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, the European Social Fund (ESF) "Investing in your future," under the 2019 Ramón y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. J.D.L. acknowledges support from a UK Research and Innovation Future Leaders Fellowship (MR/T020784/1). This work was funded by ANID, Millennium Science Initiative, ICN12_009. I.D. is supported by the project PID2021-123110NB-I00 financed by MCIN/AEI/10.13039/501100011033/FEDER, UE. Based on observations collected at the Centro Astronómico Hispano en Andalucía (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC). Based on observations made with ESO Telescopes at the Cerro Paranal Observatory under program IDs 095.D-0091(A), 095.D-0091(B), 096.D-0296(A), 097.D-0408(A), 098.D-0115(A), 099.D-0022(A), 0100.D-0341(A), 0101.D-0748(A), 0101.D-0748(B), 0102.D-0095(A), 0103.D-0440(A), 0104.D-0498(A), and 0104.D-0498(B). This research was supported in part by the University of Pittsburgh Center for Research Computing, RRID:SCR 022735, through the resources provided. Specifically, this work used the H2P cluster, which is supported by NSF award No. OAC-2117681., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2020-001058-M)., Peer reviewed




Dipòsit Digital de la UB
oai:diposit.ub.edu:2445/9180
Artículo científico (article). 1986

SUPERNOVA MATTER: A SEMICLASSICAL APPROACH

Dipòsit Digital de la UB
  • Pi Pericay, Martí
  • Viñas Gausí, Xavier
  • Barranco Gómez, Manuel
  • Polls Martí, Artur
  • Pérez-Canyellas, A.
A well-established semiclassical method is used to systematically study the properties of hot dense matter in the conditions prevailing during the gravitational collapse of massive stars. Different semiclassical kinetic energy and entropy densities are discussed. Detailed results for different nuclear forces having different nucleon effective mass and nuclear incompressibility are presented. Plasma effects (translational and vibrational energies and Coulomb excess) are considered for a typical adiabat. The results presented here cover a wide range in entropy per baryon and electron concentration per baryon, for baryon densities ranging from 0.001/cu fm to 0.3/cu fm.




UPCommons. Portal del coneixement obert de la UPC
oai:upcommons.upc.edu:2117/175411
Artículo científico (article). 2020

INTERACTION OF HEMISPHERICAL BLAST WAVES WITH INHOMOGENEOUS SPHERES: PROBING THE COLLISION OF A SUPERNOVA EJECTA WITH A NEARBY COMPANION STAR IN THE LABORATORY

UPCommons. Portal del coneixement obert de la UPC
  • García Senz, Domingo|||0000-0001-5197-7100
  • Velarde, Pedro
  • Suzuki Vidal, Francisco
  • Stehlé, Chantal
  • Cotelo Ferreiro, Manuel
  • Portillo García, David
  • Plewa, Tomasz
  • Pak, Arthur
Past laboratory experiments at high energy density have provided insights into the physics of supernovae, supernovaremnants, and the destruction of interstellar clouds. In a typical experimental setting, a laser-driven planar blast waveinteracts with a compositionally homogeneous spherical or cylindrical target. In this work we propose a new laboratoryplatform that accounts for curvature ofthe impacting shock and density stratification of the target. Both characteristicsreflect the conditions expected to exist shortly after a supernova explosion in a close binary system. We provide detailsof a proposed experimental design(laser drive, target configuration, diagnostic system), optimized to capture the keyproperties of recent ejecta–companion interaction models.Good qualitative agreement found between our experimentalmodels and their astrophysical counterparts highlights the strong potential of the proposed design to probe details of theejecta–companion interaction for broad classes of objects by means of laboratory experiments at high energy density, Peer Reviewed





Zaguán. Repositorio Digital de la Universidad de Zaragoza
oai:zaguan.unizar.es:134611
Artículo científico (article). 2024

SUPERNOVA ENVIRONMENTS IN J-PLUS

Zaguán. Repositorio Digital de la Universidad de Zaragoza
  • González-Díaz, Raúl
  • Galbany, Lluís
  • Kangas, Tuomas
  • García-Benito, Rubén
  • Anderson, Joseph P.
  • Lyman, Joseph
  • Varela, Jesús
  • Oltra, Lamberto
  • García, Rafael Logroño
  • Rojo, Gonzalo Vilella
  • López-Sanjuan, Carlos
  • Pérez-Torres, Miguel Ángel
  • Rosales-Ortega, Fabián
  • Mattila, Seppo
  • Kuncarayakti, Hanindyo
  • James, Phil
  • Habergham, Stacey
  • Vílchez, José Manuel
  • Alcaniz, Jailson
  • Angulo, Raul E.
  • Cenarro, Javier
  • Cristóbal-Hornillos, David
  • Dupke, Renato
  • Ederoclite, Alessandro
  • Hernández-Monteagudo, Carlos
  • Marín-Franch, Antonio
  • Moles, Mariano
  • Sodré, Laerte
  • Ramió, Héctor Vázquez
We investigated the local environmental properties of 418 supernovae (SNe) of all types using data from the Javalambre Photometric Local Universe Survey (J-PLUS), which includes five broad-band and seven narrow-band imaging filters. Our study involves two independent analyses: (1) the normalized cumulative-rank (NCR) method, which utilizes all 12 single bands along with five continuum-subtracted narrow-band emission and absorption bands, and (2) simple stellar population (SSP) synthesis, where we build spectral energy distributions (SED) of the surrounding 1 kpc2 SN environment using the 12 broad- and narrow-band filters. Improvements on previous works include: (i) the extension of the NCR technique to other filters (broad and narrow) and the use a set of homogeneous data (same telescope and instruments); (ii) a correction for extinction to all bands based on the relation between the g − i color and the color excess E(B − V); and (iii) a correction for the contamination of the [N II] λ6583 line that falls within the Hα filter. All NCR distributions in the broad-band filters, tracing the overall light distribution in each galaxy, are similar to each other. The main difference is that type Ia, II, and IIb SNe are preferably located in redder environments than the other SN types. The radial distribution of the SNe shows that type IIb SNe seem to have a preference for occurring in the inner regions of galaxies, whereas other types of SNe occur throughout the galaxies without a distinct preference for a specific location. For the Hα filter we recover the sequence from SNe Ic, which has the highest NCR, to SNe Ia, which has the lowest; this is interpreted as a sequence in progenitor mass and age. All core-collapse SN types are strongly correlated to the [O II] emission, which also traces star formation rate (SFR), following the same sequence as in Hα. The NCR distributions of the Ca II triplet show a clear division between II-IIb-Ia and Ib-Ic-IIn subtypes, which is interpreted as a difference in the environmental metallicity. Regarding the SSP synthesis, we found that including the seven J-PLUS narrow filters in the fitting process has a more significant effect on the core-collapse SN environmental parameters than for SNe Ia, shifting their values toward more extincted, younger, and more star-forming environments, due to the presence of strong emission lines and stellar absorptions in those narrow bands.



Memoria Digital Vasca = Euskal Memoria Digitala
oai:www.memoriadigitalvasca.eus:10357/42903
Imagen (Image). 2016

SUPERNOVA

Memoria Digital Vasca = Euskal Memoria Digitala
  • Toledo, Manuel
Exposición, Técnica: Esmalte, Materia-soporte: Tablex, Fecha de ejecución: 1978, Obra abstracta, manchas blancas sobre fondo rojo y figuras en la parte inferior., Firmado y fechado en ángulo inferior izquierdo.