Molecular Absorption in PMN 0134-0931

ALMA Observations of Molecular Absorption in the Gravitational Lens PMN 0134-0931


We report the detection of molecular absorption lines at =0.7645 towards the radio-loud QSO PMN 0134-0931. The CO J=2–1 and HCO J=2–1 lines are seen in absorption along two different lines of sight to lensed images of the background QSO. The lines of sight are separated by 07, corresponding to 5 kpc in the lens plane. PMN 0134-0931 represents one out of only five known molecular absorption line systems at cosmologically significant distances. Moreover, it is also one of three such systems where the absorption occurs in a galaxy acting as a gravitational lens. The absorption lines through the two lines of sight are shifted by 215 8 km s, possibly representing rotational motion in one of the lensing galaxies. The absorption profiles are wide, 200 km s, suggesting that the absorption occurs in a highly inclined disk galaxy with a flat rotation curve and a cloud-cloud velocity dispersion 30 km s. Gravitational lens models require two equal mass galaxies to account for the observed configuration of lensed images. The presence of two galaxies in close proximity means that they might be interacting and potentially merging and the kinematics of the molecular gas may not reflect ordered rotational motion. The column densities of both CO and HCO are normal for diffuse molecular gas towards one of the lensed images, but significantly higher towards the other. Also, the abundance ratio is times higher than in typical diffuse molecular gas. It is plausible that the second line of sight probes denser molecular gas than what is normally the case for absorption.

ISM: general, molecules — galaxies: general, high redshift, ISM — (galaxies:) quasars: absorption lines — submillimeter: ISM



Tommy Wiklind

0000-0002-0786-7307]Tommy Wiklind


Observatoire de Paris, LERMA,
College de France, CNRS, PSL Univ, Sorbonne University, UPMC
75014 Paris, France


National Centre for Radio Astrophysics
TIFR, Post Bag 3, Ganeshkhind
Pune 411 007, India

1 Introduction

Molecular absorption lines seen towards flat-spectrum radio-loud QSOs provide an opportunity to study the molecular interstellar medium (ISM) in high redshift galaxies in much greater detail than what is possible with emission lines. Emission studies of molecular gas in high redshift galaxies have mostly been carried out using rotational transitions of CO (e.g. Carilli & Walter 2013). Such studies have provided crucial information on the most massive redshifted systems, ultra-luminous and luminous infrared galaxies, sub-mm galaxies and high- quasars (e.g. Walter et al. 2003; Daddi et al. 2008; Combes et al. 2013; Tacconi et al. 2013). Emission line strengths decrease with the inverse square of the luminosity distance and it becomes increasingly difficult to detect CO emission in high-redshift galaxies.

Absorption lines have the advantage that they remain observable at practically any distance, with the sensitivity determined only by the strength of the background source. Absorption lines can therefore be used to obtain detailed information about the physical conditions in molecular gas in galaxies at any redshift. In addition, while molecular emission studies are sensitive to dense and warm molecular gas, prevalent in actively star forming galaxies, absorption lines is more likely to arise in the excitationally cold gas, which is prevalent in less active galaxies. Molecular absorption studies towards background continuum sources thus provide a powerful probe of the evolution of normal galaxies and their interstellar medium (e.g. Wiklind & Combes 1995, 1997; Kanekar & Chengalur 2002; Menten et al. 2008; Henkel et al. 2009; Muller et al. 2014).

Once molecular absorption lines have been detected in a galaxy, deeper studies of accesible molecular lines allow detailed characterization of the physical and chemical conditions in the absorbing gas (e.g. Henkel et al. 2005; Bottinelli et al. 2009; Muller et al. 2014). The relative strengths of different absorption transitions of species where the excitation is dominated by the cosmic microwave background (CMB), can be used to determine the CMB temperature (e.g. Wiklind & Combes 1997; Muller et al. 2013). Comparison between the redshifts of different molecular transitions in an absorber can be used to test for cosmological evolution in the fundamental constants of physics (e.g. Wiklind & Combes 1997; Kanekar 2011; Kanekar et al. 2012; 2015b, 2018). Finally, redshifted absorbers provide the opportunity to study molecules whose transitions fall outside atmospheric transparency windows (e.g. molecular oxygen, water vapor, LiH, etc; Combes & Wiklind 1995; Combes et al. 1995; Combes & Wiklind 1997a,b; Kanekar & Meier 2015a).

The main obstacle to using molecular absorption lines to study molecular gas at high redshift is the scarcity of such systems. Only five molecular absorption line systems at cosmological distances are known. The rarity of these systems is mainly due to the fact that molecular gas is usually found only in the central regions of galaxies, necessitating a small impact parameter with a background continuum source. Hence, molecular absorption is more likely to be found in the host galaxy of an AGN than in an arbitrary intervening galaxy. In addition, a prior knowledge of the redshift is usually necessary to facilitate a search for absorption lines. Of the five known high-redshift molecular absorption line systems, only one was found in a blind search, PKS1830-211 (Wiklind & Combes 1996b). A blind search for redshifted molecular absorption towards 36 radio continuum sources using the Green Bank Telescope (Kanekar et al. 2014) probed redshifts 0.85 but provided only upper limits. A sensitive facility like ALMA can in principle allow a large scale search for molecular absorption line systems at high-, but unfortunately the presently available observing modes makes such an endeavour unfeasible.

The requirement of a small impact parameter means that when absorption do occur in an intervening galaxy, and the intervening galaxy is sufficiently massive, it acts as a gravitational lens of the background source. Of the five known high redshift molecular absorption line systems, including PMN 0134-0931 discussed in this paper, two have the absorption occurring in the host galaxy of the continuum source: PKS1413+135 at (Wiklind & Combes 1994; 1997a) and B1504+377 at (Wiklind & Combes 1996a). The remaining three absorption systems occur in galaxies acting as a strong gravitational lens to a background AGN: B0218+357 at (Wiklind & Combes 1995), PKS1830-211 at (Wiklind & Combes 1996b; 1998; Muller et al. 2014) and PMN 0134-0934 (Kanekar et al. 2005). Apart from providing detailed information on the interstellar medium itself, the kinematical information obtained when the absorption occurs in a gravitational lens can also provide information that can be used in modeling the lens itself.

In this paper we describe the detection of CO J=2–1 and HCO J=2–1 molecular absorption at towards the gravitationally lensed QSO PMN 0134-0931. Our Atacama Large Millimeter/submillimeter Array (ALMA) observations and data analysis are described in 2, the peculiar gravitational lens PMN 0134-0931 is described in 3. The results obtained with the ALMA data are presented in 4 and discussed in 5. In this paper we use concordance cosmological parameters from the Planck Collaboration (2016): km s Mpc; ; .

2 Observations

We observed the CO J=2–1 and HCO J=2–1 transitions, redshifted into ALMA bands 3 and 4, respectively (hereafter B3 and B4). The observations were done in three separate visits on September 9 (B4), September 17 and 19 (B3), 2016 under ALMA Cycle 3 project 2015.1.00582.S. The two B3 observations were both done with 40 antennas and PWV10.5 and 2.0 mm, respectively. The longest baseline was 3.14 km, resulting in a nominal angular resolution2 of 035. The total on-source time was 52 minutes. The B4 observations were done with 38 antennas on a single occasion, with PWV0.48 mm. The longest baseline was 2.48 km, with a nominal angular resolution of 028. The total on-source time for the B4 observation was 67 minutes.

The correlator setup for our B3 and B4 observations are shown in Table 1. For each band we used two basebands of width 1.875 GHz and 1920 channels giving a spectral resolution of 976.563 kHz. In the rest frame of the absorber, this corresponds to a velocity resolution of 2.90 km s in B3 and 2.23 km s in B4. In addition, we used two spectral basebands of width 2 GHz with 128 channels in continuum mode. The high resolution basebands were centered on 101.007 and 130.276 GHz, for CO J=2–1 and HCO J=2–1, respectively. The continuum channels were centered at 91 GHz and 140 GHz, for B3 and B4, each with a combined bandwidth of 4 GHz. The continuum data was used to construct images of the PMN 0134-0931 system. Since these were obtained at different frequency settings than the high spectral resolution basebands, we used continuum levels obtained from the high spectral resolution data in the analysis of the absorption lines.

The data reduction and calibration was done with the CASA3 package following standard procedures. The bright quasar J0006-0623 was used as both bandpass and flux calibrator. The flux calibration was bootstrapped to results from Solar system objects. The overall flux accuracy is better than 10% in both B3 and B4. Phase calibration was done with J0141-0928 for both B3 and B4.

In addition to the CO J=2–1 and HCO J=2–1 transitions, the high spectral resolution observations covered the redshifted transitions of HCN J=2–1 ( GHz), HNC J=2–1 ( GHz) and HO J=3 ( GHz).

3 The Gravitational Lens PMN 0134-0931

The gravitational lens nature of PMN 0134-0931 was discovered independently by Winn et al. (2002) in a survey of radio continuum sources and by Gregg et al. (2002) in a survey of red QSOs. High resolution radio continuum observations reveal six compact components with a maximum separation of 07 (Winn et al. 2003). The lens itself has not been reliably detected as it is overpowered by the glare of the background, =2.2 QSO (Gregg et al. 2002; Winn & Keeton 2003). Five of the six radio components (A–E)4 have the same spectral index from 1.7 to 43 GHz (, where ), while a sixth component (F) has a much steeper spectral index and is only seen in the 8.4 GHz radio data. Hence, the F component is likely to arise from a second emission component in the background QSO, physically distinct from the flat spectrum component. Differential extinction between the lensed QSO images indicates that the lens contains significant amount of dust (Gregg et al. 2002; Winn & Keeton 2003) with components C, E and D+F being more extincted than components A and B. Hall et al. (2002) detected Ca II absorption corresponding to =0.7645 in a Sloan Digital Sky Survey spectrum, interpreted as originating in the lens.

The large number of image components of PMN 0134-0931 makes it a unique gravitational lens and it presents a formidable challenge to lens modeling. Keeton & Winn (2003) did a detailed study of this system and concluded that more than one lensing galaxy is needed to account for the five flat-spectrum components. In order to model the steep spectrum component, a second distinct background source is needed. In their best model, a total of eight lens component is expected, of which six are detected: five images of a flat-spectrum radio core (A–E) and three images of a steep spectrum component (F + two unseen images). The two lensing galaxies, called Gal-N and Gal-S in Keeton & Winn (2003), are of similar mass, with 120 km s. Gal-N is centered 02 south of lens component E and Gal-S is centered 015 south of component C. The projected separation of the two galaxies is only 04 (3.2 kpc at the lens redshift ). The models suggest that the two galaxies are either both oriented in the east-west direction, or the north-south direction, and highly flattened. The presence of high extinction as well as ionized gas, inferred through scatter broadening of the radio images at low frequencies (Winn & Keeton 2003), suggests that the lensing galaxies are gas and dust rich and therefore likely to be spiral galaxies.

Absorption of the HI 21cm line was first detected in the lens of PMN 0134-0931 by Kanekar & Briggs (2003). The 21cm profile shows two broad components, with the strongest HI component matching the Ca II absorption profile of Hall et al. (2002). The total HI column density is cm, assuming a spin temperature of 200 K and a covering factor of unity. The total velocity coverage of the HI absorption components is 500 km s. Kanekar et al. (2005) searched for HCO J=2–1 absorption with the IRAM 30m telescope, the 6 cm ground state HCO doublet lines with the Green Bank Telescope (GBT) and the 2 cm first rotationally excited state of HCO with both the GBT and the Very large Array, as well as 18cm OH absorption towards PMN 0134-0931 using the GBT. While the HCO and HCO lines remained undetected, the two main OH lines at 1665 and 1667 MHz, and the two satellite lines at 1612 and 1720 MHz, were detected. The main OH lines have the same overall shape as the HI 21cm absorption. The two satellite lines are in conjugate absorption and emission, indicating a high OH column density, and can be used to probe the evolution of fundamental constants over a look-back time of 6.7 Gyr (Kanekar et al. 2005).

4 Results

4.1 Millimeter Continuum

Our ALMA continuum images of PMN 0134-0931 obtained with our ALMA data are shown in Fig. 1. The highest angular resolution (024018) is obtained at 140 GHz using uniform weighting (right panel in Fig. 1). This high resolution continuum image shows the lens components A,B and C as an extended but not resolved component. The D component is clearly separated from the A-C image by 07 and the E component is seen close to the A-C complex. We did not detect the F image which has a steep spectrum and is not likely to contribute to the continuum at millimeter wavelengths. The locations and derived parameters of the continuum components are listed in Table 2 and a comparison with the location of radio continuum images from Winn & Keeton (2003) is shown in Fig. 2. The average spectral index is () which is steeper than at radio wavelengths. This suggests that dust emission from the background source provides a negligible contribution to the rest frame submm continuum. The 140 GHz observations probe the 670m emission from the background QSO and if it had a detectable dust continuum this should make the measured spectral index flatter.

The high angular resolution continuum image is compared with the gravitational lens components in Fig. 2. The location and relative flux levels are taken from Winn & Keeton (2003). We assume that the D component is co-located with the second brightest millimeter continuum region. The other lens components line up very well with the rest of the mm continuum emission. The A, B and C components are not resolved but the mm continuum is extended, consistent with three blended sources, dominated by the A component. The flux ratios should be the same as at low radio frequencies, as long as differential lensing doesn’t affect the measured fluxes. Differential lensing could be present if the emission regions of long wavelength radio continuum do not coincide with the millimeter continuum in the background source. The flux ratio between the D and E components is at 140 GHz and at 15 GHz (Winn & Keeton 2003). The error of the mm continuum flux ratio takes a 10% absolute calibration uncertainty into account. If we add the A-C flux contributions at 15 GHz and take the ratio with the D component, we get (Winn & Keeton 2003). The corresponding flux ratio at 140 GHz is . The flux ratio at 91 GHz is slightly lower , but here the A-C and D components are not entirely resolved, making the flux ratio measurement less certain (see Fig. 1). Overall, the flux ratios seen at radio frequencies are consistent with our results at millimeter wavelengths and we detect no significant effect of differential magnification.

4.2 Molecular Absorption

We used an aperture with the same size as the restoring beam to extract spectra towards the continuum images A-C and D in PMN 0134-0931. The data cubes used for extracting the spectra were cleaned using Briggs weighting with the robustness set to 0.5. This results in slightly lower angular resolution than that obtained using uniform weighting, but is necessary to maximize the sensitivity while still retaining sufficient angular resolution to separate the continuum components. A uniform weighting produced noisy spectral data and we were not able to definitively assess the absorption properties towards the E component separate from the A-C image.

We detect absorption of CO J=2–1 and HCO J=2–1 towards both the A-C and D components. The spectra are shown in Fig. 3. The absorption profiles cover a total velocity range of 400 km s and consist of several distinct components. The depth of the absorption profiles is 10% of the continuum towards components A-C while it is 40% and 30% towards the weaker D component for CO and HCO, respectively. Overall, the absorption profiles of CO and HCO are similar, suggesting that they originate in the same molecular gas. Both the CO and HCO absorption profiles consist of a ‘narrow’ profile (seen to the right in Fig. 3), and a ‘wider’ profile. We fit Gaussian profiles to the absorption lines. The best result is obtained with three Gaussian components for the D component, one for the ‘wide’ and one for the ‘narrow’ profile. The A-C component only requires two Gaussian components to give a good fit. The results from the Gaussian fits are given in Table 3. The combined width of the ‘narrow’ and ‘wide’ CO and HCO absorption profiles is 200 km s towards both the A-C and D images. The CO profile towards the D component is even wider, approaching 250 km  s. The overall shapes of the profiles are similar towards the A-C and the D continuum components, despite probing molecular gas separated by 5 kpc in the lens plane.

While the overall shapes of the absorption profiles are comparable towards the A-C and the D continuum components, they do shift in velocity by a significant amount. The difference in intensity weighted velocity across the entire absorption profile for the CO and HCO lines along the two sight lines towards the A-C and D lens images is 2126 km . Fitting two Gaussian profiles to each absorption profile gives a velocity difference of 2158 km s. Combining a Gaussian fit to the ‘narrow’ absorption components and an intensity weighted velocity for the ‘broad’ absorption profiles gives a slightly larger velocity difference of 2188 km s. All of these estimates are consistent with each other within the errors and we adopt v = 215 km s as the velocity difference between the molecular absorption along the A-C and D lines of sight to PMN 0134-0931.

The observed opacity can be directly derived from the normalized flux shown in Fig. 3 as . If the absorption is saturated and only a lower limit to the column density can be derived. The absorption profiles towards PMN 0134-0931 do not appear to be saturated although the true opacity of the absorbing gas may be higher than if the filling factor of absorbing gas, , is less than unity:


Assuming that and consequently, , a lower limit to the column density of both CO and HCO can be derived from


where is the statistical weight of level , is the Einstein coefficient for transition , and the function is


In local thermal equilibrium (LTE), the partition function , where is the energy of level and is the excitation temperature of the molecule in question. The observed quantity needed for deriving the column density is the velocity integrated opacity .

The results for CO and HCO are given in Table 4 for the A-C and D components. It is clear that the opacities of both CO and HCO are significantly higher towards the D component. This is consistent with the optical reddening reported by Hall et al. (2002). In particular, the CO opacity towards the D component is one of the highest values seen in molecular absorption line systems. This is largely due to the large width of the absorbing profile and not just its depth. The ratio of is 500 towards the A-C component and 1500 towards the D component. Typical column density ratios seen in other absorption line systems range from 670 (B1504+377; Wiklind & Combes 1995) to 800 (PKS1413+135; Wiklind & Combes 1997). In the other absorption systems the CO and/or the HCO lines are saturated and no estimate of the abundance ratio can be obtained. The high CO-to-HCO abundance ratio towards the D component suggests that either the molecular gas seen here is of a different nature than the typical diffuse gas observed or that the covering factor for the HCO absorption.

The J=2–1 transitions of HCN and HNC are included in the high frequency resolution bandpasses in our ALMA observations. None of these lines are, however, detected at a 3 level. The HO J=3 transition is located at the very edge of our B3 data. Although a potential line is seen at 5 towards the D continuum component, the proximity to the band edge makes this line less reliable. The HO line is not detected toward the A-C component.

4.3 Molecular Emission

Since at least one of the lensing galaxies is gas-rich we searched for CO J=2–1 in emission. We extracted a spectrum from the data cube using a circular aperture with a diameter of 10 (7.48 kpc at the redshift of the lens) centered halfway between components A-C and D. We binned the spectrum to a velocity resolution of 13.4 km s, resulting in a channel to channel noise rms is 95Jy/beam. No emission was detected and assuming a velocity width of 200 km s the 5 upper limit to the molecular mass is M. The molecular mass was estimated using


where is expressed in Jy km s, the luminosity distance in Mpc and in GHz. We used M (km s pc) for the conversion between CO luminosity and H mass.

5 Discussion

5.1 Kinematics

Both the CO J=2–1 and HCO J=2–1 absorption lines toward the A-C lens components extend for 200 km s, divided into two main absorption components. A similar total width is seen for HCO towards the D lens component. The CO J=2–1 absorption towards the D component is even wider, extending over 250 km s. While the absorption seen towards the A-C component may be composed of contributions towards all three continuum images of the background QSO, separated by up to 1.3 kpc in the lens plane, the D component represents a very narrow line of sight through the lens, probably 1 pc. In other molecular absorption line systems the line widths range from a few km s to tens of km s (e.g. Wiklind & Combes 1997; Wiklind & Combes 1998). Only PKS1830-211 has molecular absorption lines approaching 100 km s in width (Wiklind & Combes 1996b, 1998; Muller et al. 2014). This system is also gravitationally lensed and provides two lines of sight through the disk of a spiral galaxy. Molecular absorption is seen along both sightlines, with a velocity separation 148 km s, providing a measure of the rotational motion of the lensing galaxy. The absorption profiles seen along the two lines of sight in PKS1830-211 are very different in shape and width and the 100 km s line widths are caused by highly saturated absorption lines. The molecular absorption seen towards the QSO B1504+377 at =0.67 also consists of two distinct absorption lines, separated by 330 km s (Wiklind & Combes 1996a). In this system the absorption occurs in the host galaxy of the QSO and the two absorption lines occur along a single line of sight. The HI 21cm absorption profile extends across the two molecular absorption complexes and shows that this is one continuous absorption system with a total velocity extent approaching 600 km s (Kanekar & Chengalur 2008). In this case, both the molecular and atomic absorption is likely to be associated with a fast neutral gas outflow, similar to those seen in lower redshift AGNs (Morganti et al. 2005).

Large line widths, such as the molecular absorption profiles seen towards PMN 0134-0931, can arise if the line of sight passes through an inclined gas-rich disk. The velocity envelope of the absorbing gas obtained by integrating along a line of sight through an axisymmetric disk depends on the inclination of the galaxy, the shape of the rotation curve, the radial extent of the absorbing gas and its velocity dispersion (Kregel & van der Kruit 2004, 2005). A velocity dispersion of 30 km s, a flat rotation curve and an inclination produce a velocity profile of width 200 km s. These parameters can be relaxed by making the radial extent of the gas distribution larger. Of course, molecular gas is not smoothly distributed but exists in discrete clouds and clumps. The velocity profile obtained by integrating along a line of sight represents an envelope and the fact that it is largely ‘filled’ with absorbing molecular gas indicates that there are several absorbing clouds along the lines of sight to PMN 0134-0931. Another possibility is that the absorbing profiles are caused by lines of sight penetrating the disk of two galaxies, which happens to have similar relative velocities. The lens models, however, do not favor such a scenario. The presence of two galaxies, with a projected distance of only 3 kpc in the lens plane (Keeton & Winn 2003) means that there is a possibility that the lensing galaxies are engaged in a merger process, with disturbed kinematics and non-circular motion, possibly with tidal arms crossing the line of sight to the background QSO.

The velocity difference between the absorption towards the A-C and D lens components is 215 km s(see Sect. 4). This difference is also seen in the HI 21cm and OH 18cm absorption (Kanekar & Briggs 2003; Kanekar et al. 2005; Fig. 4), although in these cases the background continuum sources were not resolved. The two-galaxy configuration implied by the lens model (Keeton & Winn 2003) has one of the galaxies centered just south of lens component C. If this galaxy extends across the A-C and D components, the molecular absorption may probe the rotation of a disk. In this case the absorption can be used to estimate the dynamical mass of one of the lensing galaxies. This, however, requires knowledge of the exact location and orientation of the lensing galaxy. Currently, neither observational data nor the lens models provide such information. A minimum mass can be derived by assuming that the center of the lens is mid-way between the A-C and D components and that the velocity separation probes the rotational velocity of the disk: M. However, as discussed above, due to the small projected distance between the two lensing galaxies, they may be gravitationally interacting and, hence, the kinematics of this system may not represent ordered motion.

5.2 Column Density

The high CO column density seen towards the D lens component is unusual among the molecular absorption systems observed to date, both in distant galaxies as well as in our own Galaxy (Lucas & Liszt 1996). The column density ratio is 2 times higher than earlier estimates along Galactic and high- sightlines, and 3 times higher than what is seen towards the A-C component in PMN 0134-0931. This high abundance ratio does not seem to be due to an anomalously low . The column density of HCO along the D component is cm (Table 4), significantly higher than what is typically seen in absorption of diffuse molecular gas. Lucas & Liszt (1996) found an average column density of of cm in a sample of 17 line of sights through diffuse molecular gas in the Milky Way galaxy, almost a factor of ten lower than the column density we derive for HCO along the D component. Our estimate is, however, similar to the average HCO column density of cm seen in Infrared Dark Clouds (Sanhueza et al. 2012). The CO column density is also significantly higher than any previously value derived from unsaturated absorption lines. This suggests that the absorption towards the D component occurs in a dense molecular cloud core rather than the typical diffuse molecular gas.

This interpretation is corroborated by the HI 21cm absorption profile (Kanekar & Briggs 2005). In Fig. 4 we compare the HI 21cm absorption profile of Kanekar et al. (2012) with that of the HCO J=2–1 absorption profile presented in this paper. The HI profile has the same broad character as seen in the molecular absorption, with similar overall velocity spread. The HI 21cm observations did not resolve the lensing components but comparing the HI profile with the molecular profiles it is possible to distinguish which part of the HI 21cm absorption is associated with the A-C and the D components, respectively (Fig. 4). There are two interesting differences between the mm-wave molecular and atomic absorption profiles; towards the A-C lens component, the CO and HCO absorption consists of two distinct line components while the HI 21cm absorption consists of a single smooth profile. Still, the overall widths are the same. This suggests that the absorbing gas consists of two denser molecular clumps embedded in a smooth atomic component. Towards the D lens component, on the other hand, the CO and HCO absorption profiles consist of three distinct profiles, two of which are much less pronounced in the HI 21cm absorption and in the case of the ‘narrow’ molecular absorption, essentially without any HI absorption altogether. This suggests that this absorption arises in a gas component that is completely molecular. This is consistent with this being a dense molecular cloud, as inferred from the high column density ratio. The OH 1665 MHz absorption towards PMN 0134-0931 closely follows that of HI (Kanekar et al. 2005), with a pronounced absence of OH in two of the HCO and CO absorption components towards the D image. Since line widths of CO and HCO in dark molecular clouds are typically only a few km s (Lucas & Liszt 1996; Sanhueza et al. 2012), the overall large line widths seen in PMN 0134-0931 as well as the large and values are simply due to a large number of absorbing molecular clouds lined up along the line of sight.

Kanekar et al. (2012) provide a 4-component Gaussian fit to their OH 1667 MHz spectrum, with two components at positive velocities (relative to ) and two at negative velocities. We use this to infer the OH column density towards lens components A-C and D, assuming that, like the mm-wave absorption, the positive velocity OH absorption arises against A-C and the negative velocity absorption against D. The OH column density estimate also requires the covering factors of the A-C and D components. For this, we use the flux densities of the different components measured by Winn & Keeton (2003) and the low-frequency spectral index of (Winn & Keeton 2003) to estimate the fraction of the total flux density at 945 MHz (the redshifted OH 1667 MHz line frequency) in components A-C and component D. We obtain flux density fractions of in components A-C and in component D, assuming that the other components do not contribute significantly to the 945 MHz flux density. For a typical OH line excitation temperature of 10 K, this then yields OH column densities of N cm and  cm against components A-C and D, respectively, assuming that the covering fractions of components A-C and D are the same as their fractional contribution to the total flux density. Comparing these to the HCO column densities along the two sightlines yields HCO to OH column density ratios of and towards A-C and D, respectively. The former is similar to estimates of this ratio () in diffuse gas in both the Milky Way and high- galaxies (e.g. Lucas & Liszt 1996; Kanekar & Chengalur 2002), but the latter is significantly lower. This reinforces our suspicion that the sightline towards component D is very different from typical sightlines through spiral galaxies.

To summarize, the gravitational lens PMN 0134-0931 consists of two galaxies at with a small projected separation on the sky. The lensing configuration gives rise to six lensed images. Absorption of ionized, atomic and molecular gas probe kinematically distinct lines of sight through this system. The molecular absorption is seen towards two lines of sight, separated by 5 kpc in the lens plane. The absorption lines shift by 215 8 km s between the two lines of sight, possibly due to the rotational motion of one of the lensing galaxies. The width of the absorption profiles is 200 km s. This suggests that the absorption occurs in an inclined gas-rich disk with an approximately flat rotation curve and a cloud-cloud velocity dispersion of 30 km s. The column densities of CO and HCO towards the A-C component are similar to other extragalactic molecular absorption systems but it is unusually high towards the D component. This is likely due to the presence of molecular gas more dense than the diffuse molecular gas most commonly seen in absorption. The data on the ISM and its kinematics can potentially be used to further refine the lens modeling and help to understand the nature of this intriguing gravitational lens system. The interpretation is currently hampered by the lack of accurate information on the location and orientation of the lensing galaxies.

This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00582.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NK acknowledges support from the Department of Science and Technology via a Swarnajayanti Fellowship (DST/SJF/PSA-01/2012-13).
ALMA BW nchan v
band GHz GHz MHz km s
B3 89.151 2.0 128 15.24 51.23
91.023 2.0 128 15.24 50.18
101.068 1.875 1920 0.98 2.90
103.007 1.875 1920 0.98 2.84
B4 128.318 1.875 1920 0.98 2.28
130.276 1.875 1920 0.98 2.25
140.318 2.0 128 15.24 32.54
142.206 2.0 128 15.24 32.12

Note. – denotes the central frequency of a each spectral window.

Table 1: ALMA Correlator Setup
Component RA DEC Integrated flux Peak flux Deconvolved size PA
GHz J2000.0 mJy mJy/beam mas deg
A–C 90.09 01:34:35.668 -09:31:02.909 52.202.7 44.21.4 21956191102 1768
141.3 01:34:35.667 -09:31:02.886 27.540.87 20.740.41 146148027 4212
D 90.09 01:34:35.701 -09:31:03.263 7.920.17 6.970.08 2402512136 15711
141.26 01:34:35.701 -09:31:03.275 3.570.14 3.620.08
E 90.09
141.26 01:34:35.684 -09:31:02.680 2.100.26 1.360.11 17450128116 4575

Note. – Component D: 141.26 GHz is an unresolved point source; Component E: 90.09 GHz, angular resolution not sufficient to resolve component.

Table 2: PMN 0134-0931 Continuum components
Component HCO(2-1) CO(2-1)
Peak Peak
mJy/beam km s km s mJy/beam km s km s
A–C 0.076 0.015 73.80 6.41 39.70 9.14 0.228 0.009 70.38 0.96 30.17 1.35
0.064 0.024 169.69 4.74 15.05 6.72 0.159 0.013 171.83 0.91 13.15 1.28
D 0.216 0.016 -166.65 3.12 36.21 4.76 0.299 0.047 -161.21 14.99 53.10 16.45
0.330 0.020 -115.65 1.59 15.05 2.26 0.356 0.136 -117.96 2.88 15.25 6.51
0.232 0.030 -46.22 1.10 22.85 1.64 0.468 0.064 -48.46 2.85 22.75 4.10

Note. – The error estimates of the Gaussian components are derived from the covariance matrix of the non-linear fit.

Table 3: Gaussian fit parameters
Transition Component v N
km s km s cm
CO(J=2-1) A–C 4.48 0.017 5.25 1.20
D 4.48 0.013 70.26 6.96
HCO(J=2-1) A–C 5.79 0.036 7.20 0.65
D 5.79 0.070 35.14 3.21

Note. – refers to the 1 noise in the opacity measured from the normalized flux.

Table 4: Opacity and column densities
Figure 1: Continuum emission from the background QSO PMN 0134-0701. Left: 90 GHz continuum, Right: 141 GHz continuum. The highest angular resolution is achieved with the 141 GHz image, done with uniform weighting. In this case the restoring beam is 024018 with a position angle of . The 90 GHz image has a restoring beam of 05400.45 with a position angle of .
Figure 2: The 141 GHz continuum image of PMN 0134-0931 with uniform weighting. The lens components A–E from Winn & Keeton (2003) are shown. The overlay was done by fixing the D component to the unresolved millimeter continuum below the main continuum component. The relative offsets of the lens components from Winn & Keeton (2003) were then used for the A–C and E components. The F component is not shown as it is a steep spectrum radio source and unlikely to contribute any continuum at 141 GHz. The size of the lens components corresponds to the approximate continuum strength at long radio wavelength and may not reflect the true relative strength at mm wavelengths. The separation between A and D is 068, corresponding to 5 kpc in the lens plane.
Figure 3: The J=2–1 absorption spectra of CO and HCO towards the A-C lens component (top panels) and the D lens component (bottom panels). The velocity scale is relative to a redshift and the continuum levels have been normalized to unity.
Figure 4: Comparison of the HI 21cm absorption (blue line) from Kanekar & Briggs (2003) with the HCO(2-1) absorption observed with ALMA (red line) seen through the two continuum components A-C and D.


  1. Precipitable water vapor
  2. The actual angular resolution depends on the uv-weighting applied in the CLEAN process.
  3. Common Astronomy Software Applications:
  4. We use the same designation of the lens components as in Winn & Keeton (2003).


  1. Bottinelli, S., Hughes, A.M., van Dishoeck, E.F., et al. 2009, ApJ, 690, 130
  2. Carilli, C.L. & Walter, F. 2013, ARA&A, 51, 105
  3. Combes, F. & Wiklind, T. 1995, A&A, 303, L61
  4. Combes, F. & Wiklind, T. 1997a, A&A, 486, L79
  5. Combes, F. & Wiklind, T. 1997b, A&A, 334, L81
  6. Combes, F., García-Burillo, S., Braine, J., et al. 2011, A&A, 528, 124
  7. Combes, F., García-Burillo, S., Braine, J., et al. 2013, A&A, 550, 41
  8. Daddi, E., Dannerbauer, H., Elbaz, D., et al., 2008, ApJ, 673, 21
  9. González-López, J., Barrientos, L. F., Gladders, M. D., et al. 2017, ApJ, 846, 22
  10. Gregg, M.D., Lacy, M., White, R.L., et al. 2002, ApJ, 564, 133
  11. Hall, P.B., Richards, G.T., York, D.G., et al. 2002, ApJ, 575, 51
  12. Henkel, C., Jethava, N., Kraus, A., et al. 2005, A&A, 440, 893
  13. Henkel, C, Menten, K.M., Murphy, M.T., et al. 2009, A&A, 500, 725
  14. Kanekar, N. & Chengalur, J.N. 2002, A&A, 381, L73
  15. Kanekar, N. & Briggs, F.H. 2003, A&A, 412, L29
  16. Kanekar, N. Carilli, C.L., Langston, G.I., et al. 2005, Phys. Rev. Lett., 95, 1301
  17. Kanekar, N. & Chengalur, J.N. 2008, MNRAS, 384, L6
  18. Kanekar, N. 2011, ApJ, 728, 12
  19. Kanekar, N., Langston, G.I., Stocke, J.T., Carilli, C.L., Menten K.M. 2012, ApJ, 746, 16
  20. Kanekar, N., Gupta, A., Carilli, C.L., Stocke, J.T., Willett, K.W. 2014, ApJ, 782, 56
  21. Kanekar, N. & Meier, D.S. 2015a, ApJ, 811, 23
  22. Kanekar, N., Ubachs, W., Menten, K.M., etal. 2015b, MNRAS, 448, L104
  23. Kanekar, N., Gosh, T., Chengalur, J.N. 2018, Phys. Rev. Lett., 120, 1302
  24. Keeton, C.R. & Winn, J.N. 2003, ApJ, 590, 39
  25. Kregel, M & van der Kruit, P.C. 2004, MNRAS, 352, 787
  26. Kregel, M & van der Kruit, P.C. 2005, MNRAS, 358, 481
  27. Lucas, R. & Liszt, H. 1996, A&A, 307, 237
  28. Menten, K.M., Güsten, R., Leurini, S., et al. 2008, A&A, 492, 725
  29. Morganti, R., Tadhunter, C.N., Oosterloo, T. 2005, A&A, 444, L9
  30. Muller, S., Beelen, A., Black, J.H., et al. 2013, A&A, 551, 109
  31. Muller, S., Combes, F., Guélin, M., et al. 2014, A&A, 566, 112
  32. Muller, S., Muller, H.S.P., Black, J.H., et al. 2016, A&A, 595, 128
  33. Muller, S., Muller, H.S.P., Black, J.H., et al. 2017, A&A, 606, 109
  34. Planck Collaboration, et al. 2016, A&A, 594, 13
  35. Sanhueza, P., Jackson, M., Foster, J.B., et al. 2012, ApJ, 756, 60
  36. Tacconi, L.J., Neri. R., Genzel, R., et al. 2013, ApJ, 768, 74
  37. Walter, F., Bertoldi, F., Carilli, C., et al., 2003, Nature, 424, 406
  38. Wiklind, T. & Combes, F. 1994, A&A, 286, L9
  39. Wiklind, T. & Combes, F. 1995, A&A, 299, 382
  40. Wiklind, T. & Combes, F. 1996a, A&A, 315, 86
  41. Wiklind, T. & Combes, F. 1996b, Nature, 379, 139
  42. Wiklind, T. & Combes, F. 1997a, A&A, 328, 48
  43. Wiklind, T. & Combes, F. 1997b, ApJ, 500, 129
  44. Winn, J.N., Lovell, J.E.J., Chen, H.-W., et al. 2002, ApJ, 564, 143
  45. Winn, J.N., Kochanek, C.S., Keeton, C.R., Lovell, J.E.J. 2003, ApJ, 590, 26
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Comments 0
Request comment
The feedback must be of minumum 40 characters
Add comment
Loading ...

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description