2000/06/12 by F. Courbin, C. Lidman, Courbin, F. +9
Earth and Planetary Sciences · Physics and Astronomy · #Adaptive optics and wavefront sensing #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Geophysics and Gravity Measurements #Pulsars and Gravitational Waves Research #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0006168
to be published in A&A, 8 pages, 9 postscript figures
arxiv created 2000/06/12 · openalex publication_date 2000/06/12 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
(Abridged) A new technique for the spatial deconvolution of spectra is\napplied to near-IR (0.95 - 2.50 micron) NTT/SOFI spectra of the lensed,\nradio-quiet quasar HE 1104-1805. The continuum of the lensing galaxy is\nrevealed between 1.5 and 2.5 micron. It is used in combination with previous\noptical and IR photometry to infer a plausible redshift in the range 0.8 < z <\n1.2. Modeling of the system shows that the lens is probably composed of the red\ngalaxy seen between the quasar images and a more extended component associated\nwith a galaxy cluster with fairly low velocity dispersion (~ 575 km/s). The\nspectra of the two lensed images of the source show no trace of reddening at\nthe redshift of the lens nor at the redshift of the source. Additionally, the\ndifference between the spectrum of the brightest component a nd that of a\nscaled version of the faintest component is a featureless continuum. Broad and\nnarrow emission lines, including the FeII features, are perfectly subtracted.\nThe very good quality of our spectrum makes it possible to fit precisely the\noptical Fe II feature, taking into account the underlying continuum over a wide\nwavelength range. HE 1104-1805 can be classified as a weak Fe II emitter.\nFinally, the slope of the continuum in the brightest image is steeper than the\ncontinuum in the faintest image and supports the finding by Wisotzki et al.\n(1993) that the brightest image is microlensed. This is particularly\ninteresting in view of the new source reconstruction methods from\nmultiwavelength photometric monitoring.\n