EL PAPEL DE LOS BROTES DE FORMACION ESTELAR EN LA FORMACION Y EVOLUCION DE GALAXIAS
AYA2013-47742-C4-4-P
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Nombre agencia financiadora Ministerio de Economía y Competitividad
Acrónimo agencia financiadora MINECO
Programa Programa Estatal de Fomento de la Investigación Científica y Técnica de Excelencia
Subprograma Subprograma Estatal de Generación del Conocimiento
Convocatoria Proyectos de I+D dentro del Subprograma Estatal de Generación del Conocimiento (2013)
Año convocatoria 2013
Unidad de gestión Dirección General de Investigación Científica y Técnica
Centro beneficiario CENTRO DE INVESTIGACIONES ENERGÉTICAS, MEDIOAMBIENTALES Y TECNOLÓGICAS (CIEMAT)
Centro realización DEPARTAMENTO DE INVESTIGACION BASICA
Identificador persistente http://dx.doi.org/10.13039/501100003329
Publicaciones
Found(s) 3 result(s)
Found(s) 1 page(s)
Found(s) 1 page(s)
SN 2014J at M82 - I. A middle-class Type Ia supernova by all spectroscopic metrics
Digital.CSIC. Repositorio Institucional del CSIC
- Galbany, Lluís
- Moreno-Raya, M.E.
- Ruiz-Lapuente, Pilar
- González Hernández, Jonay I.
- Méndez, J.
- Vallely, P.
- Barón, E.
- Domínguez, I.
- Hamuy, M.
- López-Sánchez, A.R.
- Mollá, M.
- Catalán, S.
- Cooke, E. A.
- Fariña, C.
- Génova-Santos, R.
- Karjalainen, R.
- Lietzen, H.
- McCormac, J.
- Riddick, F. C.
- Rubiño-Martín, J. A.
- Skillen, I.
- Tudor, V.
- Vaduvescu, O.
13 págs.; 10 figs.; 4 tabs., We present the intensive spectroscopic follow up of the Type Ia supernova (SN Ia) 2014J in the starburst galaxy M82. Twenty-seven optical spectra have been acquired from 2014 January 22 to September 1 with the Isaac Newton and William Herschel Telescopes. After correcting the observations for the recession velocity of M82 and for MilkyWay and host galaxy extinction, we measured expansion velocities from spectral line blueshifts and pseudo-equivalent width of the strongest features in the spectra, which gives an idea on how elements are distributedwithin the ejecta.We position SN 2014J in the Benetti, Branch et al. andWang et al. diagrams. These diagrams are based on properties of the Si II features and provide dynamical and chemical information about the SN ejecta. The nearby SN 2011fe, which showed little evidence for reddening in its host galaxy, is shown as a reference for comparisons. SN 2014J is a border-line object between the Core-normal and Broad-line groups, which corresponds to an intermediate position between low-velocity gradient and high-velocity gradient objects. SN 2014J follows the R(Si II)-Δm15 correlation, which confirms its classification as a relatively normal SN Ia. Our description of the SN Ia in terms of the evolution of the pseudo-equivalent width of various ions as well as the position in the various diagrams put this specific SN Ia into the overall sample of SN Ia.
2016 The Authors ; Published by Oxford University Press on behalf of the Royal Astronomical Society, Based on service observations (programme
SW2014a08) made with the WHT, and on discretionary and Spanish
CAT service observations made with the INT, both operated on
the island of La Palma by the ING in the Spanish Observatorio del
Roque de los Muchachos of the Instituto de Astrofısica de Canarias.
Support for LG and MH is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. LG
acknowledges support by CONICYT through FONDECYT grant
3140566. Support for MEMR and MM is provided by DGICYT
grant AYA2010-21887-C04-02. This work is partially funded by
DGICYT grant AYA2013-47742-C4-4-P. JIG-H, HL and JAR-M
acknowledge financial support from the Spanish Ministry of Economy
and Competitiveness (MINECO) under the 2011 Severo Ochoa
programme MINECO SEV-2011-0187 JIG-H also acknowledge the
2013 Ramon y Cajal programme MINECO RYC-2013-14875, and
the Spanish ministry project MINECO AYA2014-56359-P. EAC
acknowledges the support of the STFC., Peer Reviewed
2016 The Authors ; Published by Oxford University Press on behalf of the Royal Astronomical Society, Based on service observations (programme
SW2014a08) made with the WHT, and on discretionary and Spanish
CAT service observations made with the INT, both operated on
the island of La Palma by the ING in the Spanish Observatorio del
Roque de los Muchachos of the Instituto de Astrofısica de Canarias.
Support for LG and MH is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. LG
acknowledges support by CONICYT through FONDECYT grant
3140566. Support for MEMR and MM is provided by DGICYT
grant AYA2010-21887-C04-02. This work is partially funded by
DGICYT grant AYA2013-47742-C4-4-P. JIG-H, HL and JAR-M
acknowledge financial support from the Spanish Ministry of Economy
and Competitiveness (MINECO) under the 2011 Severo Ochoa
programme MINECO SEV-2011-0187 JIG-H also acknowledge the
2013 Ramon y Cajal programme MINECO RYC-2013-14875, and
the Spanish ministry project MINECO AYA2014-56359-P. EAC
acknowledges the support of the STFC., Peer Reviewed
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
Using the local gas-phase oxygen abundances to explore a metallicity dependence in SNe Ia luminosities
Digital.CSIC. Repositorio Institucional del CSIC
- Moreno-Raya, M. E.
- López-Sánchez, Á. R.
- Mollá, M.
- Galbany, L.
- Vílchez Medina, José Manuel
- Carnero, A.
We present an analysis of the gas-phase oxygen abundances of a sample of 28 galaxies in the local Universe (z < 0.02) hosting Type Ia supernovae (SNe Ia). The data were obtained with the 4.2 m William Herschel Telescope. We derive local oxygen abundances for the regions where the SNe Ia exploded by calculating oxygen gradients through each galaxy (when possible) or assuming the oxygen abundance of the closest HII region. The sample selection only considered galaxies for which distances not based on the SN Ia method are available. Then, we use a principal component analysis to study the dependence of the absolute magnitudes on the colour of the SN Ia, the oxygen abundances of the region where they exploded and the stretch of the SN light curve. We demonstrate that our previous result suggesting a metallicity dependence on the SN Ia luminosity for non-reddened SNe Ia can be extended to our whole sample. These results reinforce the need of including a metallicity proxy, such as the oxygen abundance of the host galaxy, to minimize the systematic effect induced by the metallicity dependence of the SN Ia luminosity in future studies of SNe Ia at cosmological distances. © 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society., We acknowledge the anonymous referee for his/her helpful comments. We thank Miguel Cárdenas-Montes, Santiago González-Gaitán, Inma Domínguez and Brad Gibson for their inestimable comments and help. Based on observations made with the 4.2 m WHT operated on the islands of La Palma by the Isaac Newton Group of Telescopes in the Spanish observatory of Roque de Los Muchachos of the Instituto de Astrofísica de Canarias. MEMR thanks the hospitality of the staff at both the Australian Astronomical Observatory (Australia) and Departamento de Astronomía of the Universidad de Chile (Chile) during his stay in 2013 and 2014, respectively. ARL-S thanks the support of the ‘Study of Emission-Line Galaxies with Integral-Field Spectroscopy’ (SELGIFS) programme, funded by the EU (FP7-PEOPLE-2013-IRSES-612701). This work has been partially supported by MINECO-FEDER grant AYA2010-21887-C04-02 and AYA2013-47742-C4-4-P. Support for LG is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009 awarded to the Millennium Institute of Astrophysics (MAS), and CONICYT through FONDECYT grant 3140566. ACR acknowledges financial support provided by the PAPDRJ CAPE/FAPERJ Fellowship. 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.