TY  - JOUR
A1  - Christensen, Lise Bech
A1  - Becker, Thomas
A1  - Jahnke, Knud
A1  - Kelz, A.
A1  - Roth, Martin M.
A1  - Sanchez, S. S.
A1  - Wisotzki, Lutz
T1  - Integral field spectroscopy of SN 2002er with PMAS
N2  - sent observations of the Type Ia supernova SN 2002er during the brightening phase. The observations were performed with the Potsdam Multi Aperture Spectrophotometer (PMAS) integral field instrument. Due to the 8arcsecx8 arcsec field of view of the spectrograph an accurate background subtraction was possible. Results from analyses of the evolution of absorption features in comparisons with other SNe show that SN 2002er is a fairly bright Type Ia supernova with a peak brightness of MB=-19.6+/-0.1.
Y1  - 2003
ER  - 
TY  - JOUR
A1  - Wisotzki, Lutz
A1  - Becker, Thomas
A1  - Christensen, Lise Bech
A1  - Helms, Andreas
A1  - Jahnke, Knud
A1  - Kelz, A.
A1  - Roth, Martin M.
A1  - Sanchez, Sebastian F.
T1  - Integral-field spectrophotometry of the quadruple QSO HE 0435-1223 : Evidence for microlensing
N2  - We present the first spatially resolved spectroscopic observations of the recently discovered quadruple QSO and gravitational lens HE 0435-1223. Using the Potsdam Multi-Aperture Spectrophotometer (PMAS), we show that all four QSO components have very similar but not identical spectra. In particular, the spectral slopes of components A, B, and D are indistinguishable, implying that extinction due to dust plays no major role in the lensing galaxy. While also the emission line profiles are identical within the error bars, as expected from lensing, the equivalent widths show significant differences between components. Most likely, microlensing is responsible for this phenomenon. This is also consistent with the fact that component D, which shows the highest relative continuum level, has brightened by 0.07 mag since Dec. 2001. We find that the emission line flux ratios between the components are in better agreement with simple lens models than broad band or continuum measurements, but that the discrepancies between model and data are still unacceptably large. Finally, we present a detection of the lensing galaxy, although this is close to the limits of the data. Comparing with a model galaxy spectrum, we obtain a redshift estimate of zlens=0.44+/- 0.02.
Y1  - 2003
ER  -