| Full text | |
| Author(s): Show less - |
Sasdelli, Michele
[1]
;
Hillebrandt, W.
[1]
;
Aldering, G.
[2]
;
Antilogus, P.
[3]
;
Aragon, C.
[2]
;
Bailey, S.
[2]
;
Baltay, C.
[4]
;
Benitez-Herrera, S.
[1]
;
Bongard, S.
[3]
;
Buton, C.
[5, 6]
;
Canto, A.
[3]
;
Cellier-Holzem, F.
[3]
;
Chen, J.
[7]
;
Childress, M.
[2, 8]
;
Chotard, N.
[9, 7]
;
Copin, Y.
[10]
;
Fakhouri, H. K.
[2, 8]
;
Feindt, U.
[5, 6]
;
Fink, M.
[1]
;
Fleury, M.
[3]
;
Fouchez, D.
[11]
;
Gangler, E.
[10]
;
Guy, J.
[3]
;
Ishida, E. E. O.
[12, 1]
;
Kim, A. G.
[2]
;
Kowalski, M.
[5, 6]
;
Kromer, M.
[1, 13, 14]
;
Lombardo, S.
[5, 6]
;
Mazzali, P. A.
[15, 1, 16]
;
Nordin, J.
[2, 17]
;
Pain, R.
[3]
;
Pecontal, E.
[18]
;
Pereira, R.
[10]
;
Perlmutter, S.
[2, 8]
;
Rabinowitz, D.
[4]
;
Rigault, M.
[5, 6]
;
Runge, K.
[2]
;
Saunders, C.
[2]
;
Scalzo, R.
[19]
;
Smadja, G.
[10]
;
Suzuki, N.
[2]
;
Tao, C.
[7, 11]
;
Taubenberger, S.
[1]
;
Thomas, R. C.
[20]
;
Tilquin, A.
[11]
;
Weaver, B. A.
[21]
Total Authors: 46
|
| Affiliation: Show less - | [1] Max Planck Inst Astrophys, D-85741 Garching - Germany
[2] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 - USA
[3] Univ Paris 07, Univ Paris 06, Lab Phys Nucl & Hautes Energies, CNRS IN2P3, F-75252 Paris 05 - France
[4] Yale Univ, Dept Phys, New Haven, CT 06520 - USA
[5] Humboldt Univ, Inst Phys, D-12489 Berlin - Germany
[6] Bond Univ, Inst Phys, D-53115 Bonn - Germany
[7] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084 - Peoples R China
[8] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 - USA
[9] Chinese Acad Sci, Natl Astron Observ, Beijing 100012 - Peoples R China
[10] Univ Lyon 1, Inst Phys Nucl Lyon, CNRS IN2P3, F-69622 Villeurbanne - France
[11] Aix Marseille Univ, Ctr Phys Particules Marseille, CNRS IN2P3, CPPM UMR 7346, F-13288 Marseille - France
[12] Univ Sao Paulo, IAG, BR-05508900 Sao Paulo - Brazil
[13] Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm - Sweden
[14] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm - Sweden
[15] INAF Osservatorio Astron Padova, I-35122 Padua - Italy
[16] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside - England
[17] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 - USA
[18] Univ Lyon 1, Ctr Rech Astron Lyon, F-69561 St Genis Laval - France
[19] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611 - Australia
[20] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Computat Cosmol Ctr, Berkeley, CA 94720 - USA
[21] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 - USA
Total Affiliations: 21
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 447, n. 2, p. 1247-1266, FEB 21 2015. |
| Web of Science Citations: | 8 |
| Abstract | |
We develop a new framework for use in exploring Type Ia supernovae (SNe Ia) spectra. Combining principal component analysis (PCA) and partial least square (PLS) analysis we are able to establish correlations between the principal components (PCs) and spectroscopic/photometric SNe Ia features. The technique was applied to similar to 120 SN and similar to 800 spectra from the Nearby Supernova Factory. The ability of PCA to group together SNe Ia with similar spectral features, already explored in previous studies, is greatly enhanced by two important modifications: (1) the initial data matrix is built using derivatives of spectra over the wavelength, which increases the weight of weak lines and discards extinction, and (2) we extract time evolution information through the use of entire spectral sequences concatenated in each line of the input data matrix. These allow us to define a stable PC parameter space which can be used to characterize synthetic SN Ia spectra by means of real SN features. Using PLS, we demonstrate that the information from important previously known spectral indicators (namely the pseudo-equivalent width of Si II 5972 angstrom/Si II 6355 angstrom and the line veloci of S II 5640 angstrom/Si II 6355 angstrom) at a given epoch is contained within the PC space and can be determined through a linear combination of the most important PCs. We also show that the PC space encompasses photometric features like B/V magnitudes, B - V colours and SALT2 parameters c and x(1). The observed colours and magnitudes, which are heavily affected by extinction, cannot be reconstructed using this technique alone. All the above-mentioned applications allowed us to construct a metric space for comparing synthetic SN Ia spectra with observations. (AU) | |
| FAPESP's process: | 11/09525-3 - Analysis of type IA supernovae in wide-field galaxy surveys |
| Grantee: | Emille Eugenia de Oliveira Ishida |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |