Volume 468, Number 3, June IV 2007
Extended baselines for the IRAM Plateau de Bure interferometer: First results
|Page(s)||L53 - L56|
|Published online||11 April 2007|
Letter to the Editor
Distribution of the molecular absorption in front of the quasar B0218+357
Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), PO Box 23–141, Taipei, 106 Taiwan e-mail: firstname.lastname@example.org
2 Institut de Radio Astronomie Millimétrique (IRAM), 300 rue de la piscine, 38406 St Martin d'Hères, France
3 Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014 Paris, France
4 ESA Space Telescope Division, STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA
Accepted: 3 April 2007
The line of sight to the quasar B0218+357, one of the most studied lensed systems, intercepts a spiral galaxy, which splits its image into two main components A and B, separated by ca. 0.3″, and gives rise to molecular absorption. Although the main absorption component has been shown to arise in front of image A, it is not established whether some absorption from other velocity components is also occuring in front of image B. To tackle this question, we have observed the HCO+(2–1) absorption line during the commissioning phase of the new very extended configuration of the Plateau de Bure Interferometer, in order to trace the position of the absorption as a function of frequency. Visibility fitting of the self-calibrated data allowed us to achieve position accuracy between ~12 and 80 mas per velocity component. Our results clearly demonstrate that all the different velocity components of the HCO+(2–1) absorption arise in front of the south-west image A of the quasar. We estimate a flux ratio at 106 GHz.
Key words: galaxies: quasars: individual: B0218+357 / galaxies: quasars: absorption lines / techniques: interferometric
© ESO, 2007
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