# Distribution of the molecular absorption in front of the quasar B0218+357

## TL;DR

This study uses high-resolution interferometric observations to determine that all molecular absorption components in the line of sight to quasar B0218+357 occur in front of one specific lensed image, clarifying the distribution of molecular gas.

## Contribution

It provides the first precise positional analysis of molecular absorption components, confirming they originate solely in front of image A of the lensed quasar.

## Key findings

- All velocity components of HCO+(2-1) absorption are in front of image A.
- Estimated flux ratio between images A and B is approximately 4.2.
- High positional accuracy achieved with interferometric data.

## Abstract

The line of sight to the quasar B0218+357, one of the most studied lensed systems, intercepts a z=0.68 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 fA/fB = 4.2 (-1.0;+1.8 at 106 GHz.