ALMA observations of a metal-rich damped Lyα absorber at z = 2.5832: evidence for strong galactic winds in a galaxy group
J. P. U. Fynbo, K. E. Heintz, M. Neeleman, L. Christensen, M. Dessauges-Zavadsky, N. Kanekar, P. Moller, J. X. Prochaska, N. H. P. Rhodin, M. Zwaan
MMNRAS , 1–7 (2018) Preprint 6 June 2018 Compiled using MNRAS L A TEX style file v3.0
ALMA observations of a metal-rich damped Ly α absorber at z = . : evidence for strong galactic winds in a galaxy group (cid:63) J. P. U. Fynbo, , K. E. Heintz, , , M. Neeleman, L. Christensen, M. Dessauges-Zavadsky, N. Kanekar, P. Møller, J. X. Prochaska, N. H. P. Rhodin, M. Zwaan The Cosmic Dawn Center, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavík, Iceland Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg, Germany Observatoire de Genéve, Université de Genéve, 51 Ch. des Maillettes, 1290 Versoix, Switzerland Swarnajayanti Fellow; National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune 411007, India European Southern Observatory, Karl-Schwarzschild Strasse 2, D-85748 Garching, Germany
Accepted 2018 May 29. Received 2018 May 28; in original form 2018 May 1.
ABSTRACT
We report on the results of a search for CO(3-2) emission from the galaxy counterpartof a high-metallicity Damped Ly α Absorber (DLA) at z = . + M gas / M (cid:63) is in the low end of the range found for DLAgalaxies, but is still consistent with what is found for other star-forming galaxies at similarredshifts. Instead we detect CO(3-2) emission from another intensely star-forming galaxy atan impact parameter of 117 kpc from the line-of-sight to the quasar and 131 km s − redshiftedrelative to the velocity centroid of the DLA in the quasar spectrum. In the velocity profile ofthe low- and high-ionisation absorption lines of the DLA there is an absorption componentconsistent with the redshift of this CO-emitting galaxy. It is plausible that this componentis physically associated with a strong outflow in the plane of the sky from the CO-emittinggalaxy. If true, this would be further evidence, in addition to what is already known fromstudies of Lyman-break galaxies, that galactic outflows can be traced beyond 100 kpc fromstar-forming galaxies. The case of this z = .
583 structure is an illustration of this in a groupenvironment.
Key words: galaxies: ISM – ISM: molecules – quasar: absorption lines – quasars: individual(Q 0918 + (cid:63) This paper makes use of the following ALMA data:ADS / JAO.ALMA / NRAO and NAOJ.Based on observations made with the Nordic Optical Telescope, operatedby the Nordic Optical Telescope Scientific Association at the Observa-torio del Roque de los Muchachos, La Palma, Spain, of the Instituto deAstrofisica de Canarias. Based on observations made with the NASA / ESAHubble Space Telescope, obtained at the Space Telescope Science In-stitute (STScI), which is operated by the Association of Universities forResearch in Astronomy, Inc., under NASA contract NAS 5-26555. Theseobservations are associated with programme 12553.
The most hydrogen rich class of quasar absorption systems, theDLAs (defined to have N (H i ) ≥ × cm − , Wolfe et al. 2005),remain one of the most compelling ways to probe the properties ofgalaxies, in particular at redshifts 2 – 5 (see Wolfe et al. 2005, for areview). This class of absorbers gives access to detailed informationabout chemical evolution. The technique is obviously limited togas-rich galaxies, but is otherwise not limited to only the brightestgalaxies as most other techniques are (Fynbo et al. 2008).Early on in the studies of DLAs, it was realized that it is im-portant to determine the emission properties of the DLAs in orderto connect the information collected from absorption studies withthe rapidly growing body of information on high- z galaxies basedon emission studies. The Atacama Large Millimeter / sub-millimeterArray, ALMA, has opened up a new possibility to do this at sub- c (cid:13) a r X i v : . [ a s t r o - ph . GA ] J un millimeter wavelengths. An advantage of this approach is that thecontrast between the bright background quasar and the faint DLAgalaxy at these wavelengths typically is much smaller than in theoptical or near-IR bands. The first pilot studies of DLAs withALMA have given quite interesting results. Møller et al. (2018)studied a single system at z = .
716 and found a surprisingly largemolecular mass and for that mass surprisingly low star-formationrate placing the object away from the normal galactic scaling rela-tions for these quantities. Kanekar et al. (2018) studied a sample ofDLAs at similar redshifts and found a surprisingly large detectionrate of CO-emission from the galaxy counterparts of the absorbers.The first reported detection of CO-emission from a study targettingthe field of a z > z = . (cid:48)(cid:48) (30 kpc) from the quasar sightline.In this paper we present new observations of the field of the z = . + / H] = − . ± .
05 and [S / H] = − . ± .
05. The system also shows ab-sorption features from H molecules with a column density withinthe range of N (H ) = . × − . × cm − (the large uncer-tainty reflecting that the individual absorption components of theH lines are not resolved in the X-shooter spectrum). The galaxycounterpart is detected at a projected distance of 1.98 arcsec fromthe quasar (i.e. 16.2 kpc at z = . ii ], [O iii ], H β and H α are seen in the combined X-shooterspectrum, and using emission line diagnostics, Fynbo et al. (2013,hereafter F13) found a metallicity of 12 + log(O / H) = . ± . / H] em = . ± . ff erence betweenthe absorption and emission redshift amounts to only 36 ±
20 kms − (F13). From an Spectral Energy Distribution (SED) fit to theoptical and near-IR photometric data, F13 derived a stellar massof log( M (cid:63) / M (cid:12) ) = . + . − . and a star-formation rate (SFR) of27 + − M (cid:12) yr − for the DLA emission counterpart. In addition, theSED fit infers a dust attenuation of A V = . + . − . mag. These prop-erties made the system a promising target for our ALMA study ofmetal-rich DLAs at z (cid:38) − = − Mpc − , Ω m = Ω Λ = The field surrounding Q0918 + + + −
2) line at 96.5 GHz with a fre-quency resolution of 3.9 MHz. The remaining three spectral win-dows were set up to measure continuum emission of the field.The initial data were calibrated using the ALMA pipeline,which is part of the Common Astronomy Software Applications(CASA; McMullin et al. 2007) package. After this initial round of calibration, additional flagging was performed in CASA. Thecontinuum image was generated from the three continuum spectralwindows, using natural weighting, resulting in a synthesized beamof 3 . (cid:48)(cid:48) × . (cid:48)(cid:48) ◦ . The resulting root mean square (RMS) noiseof the continuum image is 14.3 µ Jy beam − , no sources were de-tected in this image at high signal-to-noise (S / N > σ ).Using the task TCLEAN in CASA, a spectral cube was madefrom the spectral window centered on the CO(3 −
2) emission atthe redshift of the z = . − , resulting in a RMS noise of 0.24 mJy beam − per48.5 km s − channel. The spectral cube spans a velocity window of ± − around the DLA redshift. The full ALMA spectral cube was searched for line emission. Onlya single line source was detected at a S / N >
7. We do detect oneother possible line emission line at 5 . σ centered at −
700 km s − and 35 (cid:48)(cid:48) south-west of the quasar, but no optical counterpart in the HST imaging is seen at this position. Assuming Gaussian noisecharacteristics, the chance probability of such a signal to occur inthe full data cube due to noise fluctuations is 7 × − . We note thatthe signal is detected at > σ in two consecutive, independent (24km s − ) channels, suggesting the emission is real. However, with-out a clear optical counterpart, it is hard to interpret this tentativedetection. At the location of the previously identified DLA galaxy counter-part —2 arcsec west of the quasar— no emission was seen in eitherthe spectral cube or continuum emission. In the top panel of Fig. 2we show the ALMA spectrum around the expected position of theCO(3-2) line. The 1 σ RMS noise for a 100 km s − channel is 0.167mJy / beam. Assuming a similar line width for the emission profilegives a 3 σ upper limit on the velocity-integrated line flux of 0 . × ( ∆ V /
100 km s − ) / Jy km s − . At z = . L (cid:48) CO(3 − < . × K km s − pc , usingthe conversion formula from Solomon & Vanden Bout (2005). Toestimate the molecular mass, we assume L (cid:48) CO(3 − / L (cid:48) CO(1 − = . conversion of α CO = . M (cid:12) (K km s − pc ) − (Bolatto et al. 2013), which resultsin an upper limit on the molecular gas mass of M mol < . × M (cid:12) .Given the stellar mass of M ∗ = . + . − . × M (cid:12) (from F13) theratio of M mol / M (cid:63) is still consistent with the general redshift evo-lution of gas-to-stellar mass inferred from main-sequence galaxies(e.g., Magdis et al. 2012b).For comparison, the z ∼ . . − . × M (cid:12) ,with two non-detections below a molecular mass of 5 × M (cid:12) . Inaddition, the molecular mass of a z = .
101 galaxy-absorber pair is M mol = (4 . ± . × M (cid:12) (Neeleman et al. 2016) and the galaxyassociated with a z = .
193 DLA discussed in Neeleman et al.(2018) has a molecular mass of (1 . ± . × M (cid:12) . MNRAS , 1–7 (2018)
LMA observations of a metal-rich DLA at z = .
583 3 z=3.088 QSO z=2.412 z=2.583z~2.9 z=2.584
Right Ascension D ec li n a ti on F105W
F160W
F606W
Figure 1.
Top panels: Integrated CO(3 −
2) emission (red contours) and dust continuum (yellow contours) overlaid on the HST / F160W image. The left panelshows the full field of view of the ALMA observation and the right panel a zoom on the region around the quasar. No CO emission is detected down to0 . × ( ∆ V /
100 km s − ) / Jy km s − at the position of the previously identified galaxy counterpart 2 arcsec west of the quasar. The CO-emitting galaxy islocated at a projected distance of 14.2 arcsec (117 kpc at z = . −
2) emission (red contours) anddust continuum (orange contours) overlaid on the HST F606W, F105W and F160W images from F13 from the galaxy located at a distance of 14.2 arcsec (117kpc at z = . ∆ v = km s − While no CO(3 −
2) line emission is detected at the position of thepreviously identified DLA counterpart, we do detect a strong CO-emitting galaxy at a projected distance of 14.2 arcsec (117 physicalkpc at z = . ± µ Jy. The in-tegrated CO(3-2) and dust continuum emission from the ALMAobservations are shown in Fig. 1, overlaid on the
HST images ofthe galaxy from F13.In the
HST
F160W image there are multiple emission com-ponents near the position of the ALMA source. Unfortunately, theresolution of the spectral cube emission is insu ffi cient to resolvethe CO emission. Together with the known o ff set in absolute as-trometry between ALMA and HST (e.g., Dunlop et al. 2017), wecannot establish if this is a chance projection of several galaxies atdi ff erent redshift or emission from regions in the same galaxy. Inthe following, we will assume the latter. As Fig. 1 shows, the CO emission is co-spatial with a very red component that is only seenin the F160W band.From the CO spectral cube, we have extracted a line profileat the position of the CO emission, which is shown in the bottompanel in Fig. 2. The spectrum shows that the CO emission is red-shifted from the centroid of the DLA at z = . − .There is marginal evidence for a "boxy" or double-horned line pro-file (Davis et al. 2011), similar to the CO(2 −
1) and CO(1 −
0) lineprofiles observed for two other, low- z absorbing galaxies (Neele-man et al. 2016; Møller et al. 2018). This indicates that this galaxyhas some degree of a rotational support and / or emission from sev-eral sub-clumps.The velocity-integrated flux density of the CO(3-2) emissionline is 0 . ± .
08 Jy km s − . This corresponds to a luminosity of L (cid:48) CO(3 − = (2 . ± . × K km s − pc .The star-formation rate of this galaxy (see Sect. 3.2.3) issimilar to the galaxy discussed in Neeleman et al. (2018), wherewe assumed an α CO = M (cid:12) (K km s − pc ) − conversion fac-tor and L (cid:48) CO(3 − / L (cid:48) CO(1 − = .
57. To facilitate comparison, wewill use similar values here, although recent work suggest some
MNRAS000
MNRAS000 , 1–7 (2018)
DLA Galaxy
CO(3-2) GalaxyVelocity relative to z = 2.5832 (km s ) F l u x D e n s i t y ( m J y ) Figure 2.
CO flux density as a function of velocity, where v rel = − corresponds to z DLA = . ff set of δ v =
131 km s − relative to z DLA . absorption-selected galaxies might show more starburst-like inter-stellar medium conditions (Klitsch et al. 2018). To account for thisuncertainty, the lower uncertainty on the mass includes the assump-tion of starburst-like conditions. Using these conversion factorsthen yields a molecular gas mass of M mol = (1 . + . − . ) × M (cid:12) . In Fig. 3 we show the normalized quasar spectrum in regionsaround selected low- and high-ionisation metal lines from the z = . ∆ v =
131 kms − in the low-ionisation lines and in the high-ionisation lines thereis quite strong absorption.C iv and Si iv absorption indicates > the presence of a warm-hot plasma in galaxy halos or in the IGM and is observed in mostquasar and GRB-DLAs (e.g. Fox et al. 2008, 2009, and Heintz etal., submitted). The large extent of the C iv and Si iv absorptionline profiles are therefore expected since this gas traces a more ex-tended medium than the galaxy ISM. In Fig. 3 we also look forextended Mg ii absorption due the large stellar mass of the CO-emitting galaxy (see Sect. 3.2.3 below) since the extent of the Mg ii absorbing gas is found to scale with stellar mass and specific star-formation rate (Chen et al. 2010). We do also see extended absorp-tion in the region of Mg ii λλ ff ected by strong emission lines from airglow).There is also indications of absorption from N v and O vi in thespectrum, but both features are heavily blended. It is intriguing thatthe high-ionisation metal lines might originate in the IGM betweena group of galaxies at z = . absorption in the quasar spectrum isdistributed over about 55 km − in velocity space centred aroundthe mean peak of low-ionisation absorption (see the lower panel inFig. 4 in Fynbo et al. 2011). Hence, the H absorption is most likelyassociated with gas originating in the DLA galaxy counterpart 16kpc from the quasar.
0 1 0 1
SiII λ
0 1
CIV λ
0 1
SiIV λ
0 1
FeII λ −400 −200 0 200 400 0 1 MgII λ N o r m a li s ed F l u x −400 −200 0 200 400 0 1 AlIII λ N o r m a li s ed F l u x Relative velocity [km s −1 ] Figure 3.
Sections from the normalized X-shooter spectrum ofQ 0918 + z DLA = . ff set of 131 km s − measured from the centroid of the CO(3-2)emission line from the galaxy 117 kpc from the quasar. Table 1.
Photometric data for the three galaxies in the field at z ≈ . E ( B − V ) = .
022 mag (Schlafly & Finkbeiner2011).Band Source(Mag AB ) DLA galaxy CO galaxy Gal. at z phot = . + . − . F W . ± .
13 26 . ± .
25 27 . ± . F W . ± .
09 24 . ± .
13 25 . ± . F W . ± .
06 23 . ± .
07 23 . ± . u > . σ ) > . σ ) > . σ ) g . ± . > . σ ) > . σ ) K s > . σ ) > . σ ) > . σ ) The field of Q 0918 + HST in the F W , F W , and F W filters, and with the Andalucia Faint Object Spectrographand Camera (ALFOSC) and the Nordic Optical Telescope near-infrared Camera and spectrograph (NOTCam) at the NOT (see F13for details). From the NOT we obtained u and g SDSS filter imagesusing ALFOSC and a K s band image using NOTCam. Using theseimaging data we measure the magnitudes in circular apertures witha diameter of 2 arcsec for the CO galaxy and report them in Table 1.For comparison we also list the magnitudes for the DLA emissioncounterpart (from F13) and for a galaxy that has been photomet-rically determined to be possibly located at a similar redshift (seeSect. 3.3 below). This galaxy is not detected in the ALMA data.To determine the physical properties of the CO-emitting MNRAS , 1–7 (2018)
LMA observations of a metal-rich DLA at z = .
583 5
Table 2.
Physical properties of the CO galaxy from SED fitting and fromthe ALMA observations.Parameter ValueAge (Myr) 217 + − A V (mag) 1 . + . − . SFR ( M (cid:12) yr − ) 112 + − log( M (cid:63) / M (cid:12) ) 10 . + . − . log( L dust / L (cid:12) ) 12 . + . − . log( M dust / M (cid:12) ) 7 . + . − . log( M mol / M (cid:12) ) 11 . + . − . Figure 4.
The broad-band optical to near-infrared SED of the CO-emittinggalaxy. The red points denotes the measured photometric data points andupper limits (arrows). From blue to red wavelengths: ALFOSC u and g bands, HST / WFC3 F W , F W and F W bands, the NOTCam K s band, and the ALMA continuum detection. The best-fit galaxy model isshown as the black line. The stellar component without dust-extinction isshown with a blue line. galaxy we use M ag P hys (da Cunha et al. 2008), with the photom-etry in Table 1 but corrected for the Galactic foreground extinctionof E ( B − V ) = .
022 mag (Schlafly & Finkbeiner 2011). M ag -P hys is a tool that fits the photometric data to stellar population anddust emission synthesis models, assuming a Chabrier (2003) IMFto generate the output galaxy models. We also include the detec-tion of the continuum flux determined from the ALMA data. Theresults of the spectral energy distribution (SED) fits are provided inTable 2 and the generated galaxy model is illustrated in Fig. 4. Theage, extinction and stellar mass of the CO-emitting galaxy are allsimilar with those inferred for the DLA galaxy. The SFR, however,is almost an order of magnitude higher than that of the DLA galaxy.We stress that this photometric modeling is only the best possiblewith the data in hand. Looking at the morphology of the object itclearly consists of multiple components with di ff erent colours solikely both age, the SFR and the dust vary across the object. + In order to search for other possible members of the z = . Figure 5.
The ratio of gas mass to stellar mass as a function of redshiftfor various emission (small circles) and absorption selected galaxy samples(gray symbols). The upper limit for the DLA counterpart and the detetionfor the CO-emitting galaxy in the Q0918 + z = .
583 (the point for the CO-galaxy has been shifted slightly tothe left to increase visibility). For both the DLA counterpart and the CO-galaxy we show M gas / M (cid:63) assuming α CO = .
3, but the error-bar includesthe possibility for α CO =
1. The measurements from other star-forminggalaxies are taken from Leroy et al. (2009); Geach et al. (2011); Magnelliet al. (2012); Daddi et al. (2010); Tacconi et al. (2010, 2013); Riecherset al. (2010), and Magdis et al. (2012a). The data for DLA galaxies arefrom Neeleman et al. (2016, 2018); Møller et al. (2018), and Kanekar et al.(2018). The dashed curve follows M gas / M (cid:63) = . × (1 + z ) (e.g., Geachet al. 2011; Carilli & Walter 2013). region of the HST and NOT imaging data. One additional object(marked with z ∼ . To place the measurements from the field of Q0918 + M gas / M (cid:63) as a function of red-shift (following Carilli & Walter (2013)). For comparison, we showmeasurements from a range of studies of both starformation and ab-sorption selected galaxies. The upper limit on the M gas / M (cid:63) ratio isin the low end of the range found for DLA galaxies, but is other-wise consistent with what has been found for star-forming galaxiesin general. The non-detection of CO(3-2) emission is therefore notvery surprising for the DLA and it seems that a detection will bepossibly with a slightly fainter detection limit.With the detection of the CO-emitting galaxy we can probethis z = . MNRAS000
1. The measurements from other star-forminggalaxies are taken from Leroy et al. (2009); Geach et al. (2011); Magnelliet al. (2012); Daddi et al. (2010); Tacconi et al. (2010, 2013); Riecherset al. (2010), and Magdis et al. (2012a). The data for DLA galaxies arefrom Neeleman et al. (2016, 2018); Møller et al. (2018), and Kanekar et al.(2018). The dashed curve follows M gas / M (cid:63) = . × (1 + z ) (e.g., Geachet al. 2011; Carilli & Walter 2013). region of the HST and NOT imaging data. One additional object(marked with z ∼ . To place the measurements from the field of Q0918 + M gas / M (cid:63) as a function of red-shift (following Carilli & Walter (2013)). For comparison, we showmeasurements from a range of studies of both starformation and ab-sorption selected galaxies. The upper limit on the M gas / M (cid:63) ratio isin the low end of the range found for DLA galaxies, but is other-wise consistent with what has been found for star-forming galaxiesin general. The non-detection of CO(3-2) emission is therefore notvery surprising for the DLA and it seems that a detection will bepossibly with a slightly fainter detection limit.With the detection of the CO-emitting galaxy we can probethis z = . MNRAS000 , 1–7 (2018) rich and H -bearing DLA in the quasar spectrum at z = . − at an impact parameter of 16.2 kpc relative to the DLA and nowthe CO-emitting galaxy redshifted by 131 km s − at an impact pa-rameter of 117 physical kpc from the DLA. Photometric redshiftsindicate that there could be other luminous members of the group.There is evidence from the kinematics that a minor part of the low-ionisation absorption and a larger fraction of the high-ionisationabsorption in the DLA could caused by gas associated with theCO-emitting galaxy. Whereas we cannot rule out that the matchis a chance e ff ect, a causal relation seems plausible. The impactparameter of 117 kpc combined with the age of the star-burst as es-timated from SED-fitting requires a galactic wind velocity of sev-eral hundred km s − , which is not unreasonable (e.g., Geach et al.2014). Together, this shows that the system is a likely part of agalaxy group and the galactic winds from at least the two identifiedgalaxies are enriching the group-environment with metals, neutralhydrogen, dust and molecules (see also Sommer-Larsen & Fynbo2017).High- z DLAs have previously been found in environmentswith other nearby galaxies (e.g., Macchetto et al. 1993; Møller& Warren 1993; Francis & Hewett 1993; Warren & Møller 1996;Møller & Warren 1998; Fynbo et al. 2003; Schulze et al. 2012). Inthe work of Møller & Warren (1993) and Warren & Møller (1996) agroup of three galaxies were found within 20 arcsec correspondingto about 150 kpc from the quasar line-of-sight. In this case the DLAis a proximate DLA so the quasar itself should be included in thestructure. The study of Fynbo et al. (2003) found a large pancake-like structure marked out by 23 Lyman- α emitters in the field of anintervening DLA at z = .
85 towards Q2138 − ff erent other lines of research thatgalaxies must expel large amounts of metals into their environ-ments. In clusters of galaxies the metals can be directly inferredfrom observations in the X-ray band of the intracluster medium(e.g., Arnaud et al. 1992; Renzini 1997). The evidence supportsa scenario, in which the metals in the intracluster medium wasexpelled from galaxies at early times (e.g., Ettori 2005; Mantzet al. 2017). The extent of halos of high-ionisation gas has previ-ously been explored for Lyman-break galaxies at redshifts of 2.5–3.5 (Adelberger et al. 2005). This study found that strongly star-forming galaxies, with typical star-formation rates of several tensof solar masses per year, are generally associated with haloes ofionised gas traced by C iv out to ∼
80 kpc for N C iv (cid:38) cm − .This work was extended by Steidel et al. (2010) who studied bothhigh- and low-ionisation absorption lines traceable out to impactparameters of about 100 kpc from z = − ±
140 kpc for H i absorbers with column densities in the range N H i = . − . cm − . Finally we note that, the DLA studiedby Neeleman et al. (2017) also shows evidence for a galactic windgiven the large impact parameter of the identified galaxy counter-part (45 kpc) and a large velocity spreads in the low-ionizationmetal lines.We know less about the presence of molecules in the circum-galatic medium at these redshifts. In the present case we know thereis H at z = . z = . z = .
47 extendingover more than 40 kpc.The fact that both the low- and high-ionisation lines in thequasar spectrum appear to have contributions from several galaxies,including some at impact parameters beyond 100 kpc, in a groupenvironment may be part of the reason why simulations of DLAkinematics have had di ffi culties matching the large line-widths ofDLAs (Prochaska & Wolfe 1997; Ledoux et al. 1998; Pontzen et al.2008; Barnes & Haehnelt 2009; Bird et al. 2015). The relativelystrong correlation between metallicity and absorption line widths(Ledoux et al. 2006; Møller et al. 2013; Neeleman et al. 2013;Christensen et al. 2014), may in addition to a mass-metallicity re-lation, also be partly influenced by the e ff ect of environment: highmetallicity systems will preferentially trace more biased regions ofthe Universe with a higher than average galactic density. We finallynote that strong feedback, especially for halo masses in the range10 -10 h − M (cid:12) is required to match the column density distribu-tion of DLAs (Bird et al. 2014). In summary, we do not detect CO emission from the previouslyidentified DLA galaxy counterpart. This non-detection is still con-sistent with the distribution of M gas / M (cid:63) found for other star-forming galaxies. Instead we detect CO(3-2) from another intenselystar-forming galaxy at an impact parameter of 117 kpc from theline-of-sight to the quasar and 131 km s − redshifted relative to thevelocity centroid of the DLA in the quasar spectrum. In the velocityprofile of the low- and high-ionisation absorption lines of the DLAthere is an absorption component consistent with the redshift of theCO-emitting galaxy. It is plausible that this component is physi-cally associated with a strong outflow in the plane of the sky fromthe CO-emitting galaxy. If true, this would be further evidence, inaddition to what is already known from studies of Lyman-breakgalaxies, of strong galactic outflows traceable to impact parametersof at least 100 kpc. ACKNOWLEDGEMENTS
We thank the anonymous referee for a very constructive and help-ful report. We thank Georgios Magdis for helpful discussions dur-ing the preparation of this manuscript. The Cosmic Dawn cen-ter is funded by the DNRF. KEH acknowledges support by aProject Grant (162948–051) from The Icelandic Research Fund.The National Radio Astronomy Observatory is a facility of the Na-tional Science Foundation operated under cooperative agreementby Associated Universities, Inc. LC and NHR are supported byDFF-4090-00079. MN acknowledges support from ERC AdvancedGrant 740246 (Cosmic_Gas).
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LMA observations of a metal-rich DLA at z = .
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