Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{1541fig1.eps} \end{figure}$ Figure 1: Continuum at 3 mm ( left panel), integrated CO(2-1) line emission ( middle panel) and the spectral CO(2-1) profiles observed toward CO-A, CO-B and at the 3 mm position of the radio jet ( right panel). Offset position (0, 0) is at the assumed position of the lens, i.e. at $\alpha _{\rm J2000}=10$ :01:21.0, $\delta _{\rm J2000}=$ +55:53:50.5. Contour levels are from $5\sigma = 1.1$ to 4.7 mJy beam^-1 in steps of 0.6 mJy beam^-1 for the 3.1 mm continuum and from 3 $\sigma = 0.33$ to 0.77 Jy km s^-1 in steps of 0.11 Jy km s^-1 for the line emission. The synthesized beam of $3.2 ''\times 3.0''$ at PA $87^\circ$ is shown in the lower left corner (1'' corresponds to 9 kpc at an angular-size distance $D_{\rm A} = 1.87$ Gpc). The white stars indicate the optical positions of the A and B image. The rms noise per 10 MHz channel is $\sim$ 0.65 mJy. The spectrum at the position of the jet is indicative of the noise level. Velocities are relative to the redshift at z = 1.4141.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1541fig2.eps} \end{figure}$ Figure 2: $\chi ^2$ results for the continuum ( upper panel) and blueshifted line ( lower panel) position fits based on the FGSE+CL model. Shown here are different positions in the source plane for the blueshifted line emission and the continuum depending on the $\chi ^2$ -test including the observed intensity ratios between the two lensed images and the observed position. Assumed values for the 3 mm continuum: $\rm A/B=1.5$ ; blueshifted line: $\rm A/B=0.4$ . Positions for the A, B (continuum) and CO-A and CO-B can be found in Table 1. Contour levels are from 0.1 to 1.0 in steps of 0.1. The region with a value close to 1.0 in this map corresponds to the best-fit position.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1541fig3.eps} \i... ...4.eps} \includegraphics[angle=-90,width=8.5cm,clip]{1541fig5.eps} \end{figure}$ Figure 3: $\chi ^2$ results of the size fit for the line emission. The FWHM of the Gaussian profile are plotted with the respective $\chi ^2$ . We also varied the position angle (PA) from 5 to 60 $^\circ$ but we restricted the presentation to the PA with the lowest $\chi ^2$ . Upper panel: blueshifted emission centered on the nucleus. $\chi ^2$ values based on the A-blue/B-blue ratio. Lowest $\chi ^2$ for $\rm PA=20^\circ$ . Contour levels start at 0.56 to 1.0 in steps of 0.04. Middle panel: blueshifted emission centered at a fixed off-nuclear position closer to the tangential caustic ( $\equiv$ position of line emission in Table 2). $\chi ^2$ based on the A-blue/B-blue ratio. Lowest $\chi ^2$ for $\rm PA=20^\circ$ . Contour levels are from 0.1 to 1.0 by 0.1. Lower panel: red- and blueshifted emission centered on the nucleus. $\chi ^2$ values based on the (A-blue+A-red)/B-blue ratio. PAs of $50\pm 10^\circ$ all result in a low $\chi ^2$ . Contour levels are from 0.6 to 1.0 in steps of 0.08.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17cm,clip]{1541fig6.eps} \end{figure}$ Figure 4: The line-free continuum at 95 GHz ( upper left panel) and the ¹²CO(2 $\rightarrow$ 1) line emission ( upper middle panel) as observed with the IRAM interferometer from both data sets. The lower panels show the simulated radio continuum ( left) and line emission ( middle) convolved with the synthesized beam and the critical lines ( grey lines). In the right panel the location of the unlensed line emissions ( $\rm r~\equiv~$ A-red, b $~\equiv~$ B-blue $~\equiv~$ A-blue) as well as the unlensed radio continuum (J $~\equiv~$ jet, Q $~\equiv~$ quasar) is shown together with the radial and tangential caustics with respect to the assumed position of the lensing galaxy ( grey lines). The offset position (0, 0) of each map corresponds to the position of the lensing galaxy. Contour levels for the data are as Fig. 1. We have also used the same contour levels for the simulated maps. The white stars indicate the optical positions of the A and B image. The parameters used for the model ( FGSE+CL) are listed in Table 2. Changes in the velocity dispersion of the lens of $\sim$ 1% or in the source positions of $\sim$ 0.1'' produce a difference in the time delay of the FGSE+CL model of $\sim$ 5%.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1541fig7.eps} \end{figure}$ Figure 5: HST image in the H-band of the host galaxy in Q0957+561 (Keeton et al. 2000) with contour levels from Fig. 4 of the velocity integrated CO(2-1) emission. Separation of the tick marks is 1''.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1541fig7.eps} \end{figure}$	Figure 5: HST image in the H-band of the host galaxy in Q0957+561 (Keeton et al. 2000) with contour levels from Fig. 4 of the velocity integrated CO(2-1) emission. Separation of the tick marks is 1''.
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