arXiv:1210.5524v1 [astro-ph.CO] 19 Oct 2012 2018 September 6 o.Nt .Ato.Soc. Astron. R. Not. Mon. e Blitz, Leo h ATLAS The ahrn Alatalo, Katherine galaxies early-type rcEmsellem, Eric Cappellari, Michele al Serra, Paolo hrtnNaab, Thorsten ireYe Lablanche, Pierre-Yves 18 17 16 15 14 13 12 9 2 8 1 7 11 10 3 6 5 4 c aoaor I ai-aly E/RUSp–CR Univer – CNRS – CEA/IRFU/SAp Paris-Saclay, AIM Laboratoire AAHrce cec etr aionaIsiueo Tech of Institute California Center, Science Herschel NASA bevtied ai,LRAadCR,6 v el’Observato de Av. 61 CNRS, and LERMA Paris, de Observatoire eateto srnm,Has il ne,Uiest of University Annex, Field Hearst Astronomy, of Department hsc eatet nvriyo oeo 81W Bancroft W. 2801 Toledo, of University Department, Physics uoenSuhr bevtr,Karl-Schwarzschild-Str. Observatory, Southern European eateto srnm,LdreGaut eerhTwrB Tower Research Graduate Lederle Astronomy, of Department hsc eatet e eioIsiueo iigadTech and Mining of Institute Mexico New Department, Physics u-eateto srpyis eateto hsc,Un Physics, of Department Astrophysics, of Sub-department vneCalsAd´,F620SitGnsLvl France Laval, Saint-Genis Andr´e, F-69230 Charles avenue 9 ulpIsiuefrAtooy&Atohsc,University Astrophysics, & Astronomy for Institute Uni Dunlap Swinburne Supercomputing, and Astrophysics for Hertfords Centre of University Research, Astrophysics A‘o for N. Centre 670 Centre, Operations Northern Observatory, Gemini Groningen, of University Institute, Astronomical Postb Kapteyn (ASTRON), Astronomy Radio for Institute Box Netherlands PO Physik, f¨ur Extraterrestrische Institut Planck Max nvri´ yn1 bevtied yn eted Recherc de Centre Lyon, de Observatoire 1, 2300 Universit´e Lyon 9513, Postbus University, Leiden Leiden, Sterrewacht 02RAS 2012 1 lsnF Crocker, F. Alison 13 n neMreWeijmans Anne-Marie and 000 3 12 3D , 11 –2(02 rne etme 08(NL (MN 2018 September 6 Printed (2012) 1–52 , o Oosterloo, Tom 1 rjc VI.CRAC mgn uvyof survey imaging CO CARMA XVIII. – project aehKhochfar, Sadegh , 2 4 ⋆ oe .Davies, L. Roger ioh .Davis, A. Timothy 3 , 11 afel Morganti, Raffaella 6 , 7 sel Bayet, Estelle ,878Grhn,Germany Garching, 85748 2, 13 ie afil,HrsA19B UK 9AB, AL1 Herts Hatfield, hire, otu 0,90 VGoign h Netherlands The Groningen, AV 9700 800, Postbus ooy 7 .Wlo v. aaea A915 USA 91125, CA Pasadena, Ave., Wilson S. 770 nology, 32 -57 acig Germany Garching, D-85478 1312, vriyo xod ey ikno ulig el od O Road, Keble Building, Wilkinson Denys Oxford, of iversity oeo H USA OH, Toledo, , fTrno 0S.Gog tet oot,O 5 H,Canada 3H4, M5S ON Toronto, Street, George St. 50 Toronto, of ALie,TeNetherlands The Leiden, RA aiona ekly A97031,USA 94720-3411, CA Berkeley, California, eAtohsqed ynadEoeNraeSpeiued Ly Sup´erieure de Normale Ecole and Lyon de Astrophysique he , s2 90A wneo,TeNetherlands The Dwingeloo, AA 7990 2, us est fTcnlg,Hwhr,Vcoi 12 Australia 3122, Victoria Hawthorn, Technology, of versity 14 ooy oor,N 70,USA 87801, NM Socorro, nology, ouPae io I970 USA 96720, HI Hilo, Place, hoku 1E nvriyo ascuet,Ahrt A003 USA 01003, MA Amherst, Massachusetts, of University 619E, 12 r,F704Prs France Paris, F-75014 ire, i´ ai ieo,911GfsrYet ee,France Cedex, Gif-sur-Yvette 91191 Diderot, sit´e Paris acSarzi, Marc 4 ao Krajnovi Davor .T eZeeuw, de T. P. 3 18 atnBureau, Martin † 4 13 aieBois, Maxime A , T 14 E 16 tl l v2.2) file style X ihr .McDermid, M. Richard ihlsScott, Nicholas c, 3 ´ , 10 3 4 aadKuntschner, Harald ireAanDuc, Pierre-Alain iaM Young, M. Lisa 8 Fr ed ´ 17 fr X R,UK 3RH, OX1 xford rcBournaud, eric ´ on, 5 15 9 3 9 2 K. Alatalo and the ATLAS3D team

ABSTRACT We present the Combined Array for Research in Millimeter Astronomy (CARMA) ATLAS3D molecular gas imaging survey, a systematic study of the distribution and kinematics of molec- ular gas in CO-rich early-type galaxies. Our full sample of 40 galaxies (30 newly mapped and 10 taken from the literature) is complete to a 12CO(1–0) integrated flux of 18.5 Jy km s−1‡, and it represents the largest, best-studied sample of its type to date. A comparison of the CO distribution of each galaxy to the g − r color image (representing dust) shows that the molecular gas and dust distributions are in good agreement and trace the same underly- ing interstellar medium. The galaxies exhibit a variety of CO morphologies, including discs (50%), rings (15%), bars+rings (10%), spiral arms (5%), and mildly (12.5%) and strongly (7.5%) disrupted morphologies. There appear to be weak trends between galaxy mass and CO morphology, whereby the most massive galaxies in the sample tend to have molecular gas in a disc morphology. We derive a lower limit to the total accreted molecular gas mass across 10 8 the sample of 2.48 × 10 M⊙, or approximately 8.3 × 10 M⊙ per minor merger within the sample, consistent with minor merger stellar mass ratios. Key words: galaxies : elliptical and lenticular, cD – galaxies : kinematics and dynamics – galaxies : evolution – galaxies : ISM – radio lines : galaxies – galaxies : star formation – ISM : molecules – surveys

1 INTRODUCTION hereafter Paper IV), and 65% of the sample has been observed in H I with the Westerbork Synthesis Radio Telescope (WSRT; The bimodality in the morphological classification of galaxies has Morganti et al. 2006; Oosterloo et al. 2010; Serra et al. 2012, here- long been known (Hubble 1926). Late-type galaxies (LTGs) typ- after Paper XIII). For studies of the cold and warm interstellar ically have exponential discs, spiral structure and blue colours. medium (ISM), the ATLAS3D sample is thus one of the largest and Early-type galaxies (ETGs) are more ellipsoidal, with smoother best-observed samples of local ETGs available. isophotes and red colours. One scenario for producing this galaxy Of the 260 ETGs in the ATLAS3D sample, 56 were detected bimodality is via mergers. Simulations have shown that a merger in CO (22% detection rate; Paper IV). However, despite emerging between two LTGs often creates an ETG (Toomre & Toomre 1972; evidence that a non-negligible fraction of ETGs contain molecular Springel et al. 2005). ETGs are also much more likely to be found gas, little is known about its origin and evolution, although various on the “red sequence” portion of the color-magnitude diagram scenarios have been put forth (see e.g. Davis et al. 2011b, hereafter (CMD; Baldry et al. 2004; Faber et al. 2007), presumably due to Paper X1). The three most prominent scenarios are outlined here. the loss of most of their star-forming material. First, it is possible that the gas survived the galaxy’s transforma- ETGs have been shown to be deficient in star formation tion into an ETG and was not completely consumed subsequently relative to LTGs at a given mass (Visvanathan & Sandage 1977; through secular evolution. Second, the molecular gas may have ac- Bower et al. 1992), and therefore should be molecular and atomic cumulated internally through stellar mass loss (Faber & Gallagher gas-poor (Lees et al. 1991). Recently, it has however become clear 1976). In the ATLAS3D sample, it is expected that each galaxy pro- that they are not devoid of cold gas, containing reservoirs of −1 duces on average 0.1 M⊙ yr of ISM through mass loss from the dust (e.g. Hawarden et al. 1981; Jura 1986; Knapp et al. 1989), old stellar population alone (Ciotti et al. 1991). Third, it is possi- neutral atomic gas (e.g. Knapp et al. 1985; Sage & Welch 2006; ble that the molecular gas was accreted from an external source, Oosterloo et al. 2010) and molecular gas (e.g. Sage & Wrobel through tidal stripping events, cold accretion and/or minor mergers 1989; Welch & Sage 2003; Combes et al. 2007). with gas-rich companions. The minor merger (1:4 – 1:10 mass ra- The ATLAS3D sample is a complete, volume-limited sample tios) rate calculated by Lotz et al. (2008, 2011) suggests that there of 260 local ETGs brighter than MK = 21.5, covering distances are approximately 0.12 minor mergers per galaxy per Gyr, so the to 42 Mpc with some restrictions on declination− and Galactic lati- ETGs of the ATLAS3D sample as a whole should have undergone tude (Cappellari et al. 2011a, hereafter Paper I). The survey was de- a total of 30 minor mergers in the last Gyr. It is also possible signed to help us understand ETG formation and evolution. Optical that this molecular≈ gas is leftover from major mergers that have integral-field spectroscopy with SAURON on the William Herschel taken place, but minor mergers dominate in number. Determining Telescope (WHT) has been obtained over the central 41′′ 33′′ re- the origin of the molecular gas therefore requires a detailed anal- gion of all ATLAS3D galaxies, revealing their internal stellar× kine- ysis of its distribution and kinematics (e.g. angular momentum), matics, stellar population properties and ionized gas distributions only available from interferometric maps, and a comparison to the and kinematics. The ATLAS3D sample has also been completely stellar kinematics (as done in Paper X). observed in CO J=1–0 and J=2–1 with the Institut de Radioas- How the properties of the molecular gas depend on the en- tronomie Millimetrique (IRAM) 30m telescope (Young et al. 2011, vironment of the host galaxy is an open question. For instance, galaxies in clusters may well be unable to acquire cold external gas, ⋆ email: [email protected] specifically atomic hydrogen (H I), due to the presence of the hot † Dunlap Fellow ‡ 18.5 Jy km s−1 is drawn from the IRAM 30m survey, and as the inter- ferometric data indicate that the 30m molecular gas masses are generally 1 The current paper presents in detail the observations used in Paper X to underestimates, the true limit is likely slightly higher. discuss the origin of the CO.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 3 intracluster medium (ICM) and associated ram pressure stripping distances from 13.4 Mpc to 45.8 Mpc2. Six of the 30 galaxies be- (Cayatte et al. 1990; B¨ohringer et al. 1994; Paper X). A first effort long to the Virgo cluster. All galaxies but three (IC 719, NGC 1222 towards studying the molecular gas properties of ETGs with multi- and NGC 7465) are regular rotators according to their stellar kine- ple molecular transitions (including 13CO, HCN and HCO+ in ad- matics (Krajnovi´cet al. 2011, hereafter Paper II). NGC 1222, clas- dition to 12CO; Crocker et al. 2012, hereafter Paper XI) shows that sified as a non-regular rotator, is known to be undergoing a strong the molecular gas properties widely vary amoung ETGs, probably interaction with a neighbour. NGC 7465 is undergoing an inter- due to 12CO optical thickness variations linked to the dynamical action with NGC 7464 and NGC 7463, and has a kinematically- state of the gas. decoupled core. IC 719 does show ordered rotation in its stellar It is also not well determined whether the properties of in- component, but is recognized as a 2σ (double-peaked) galaxy when dividual galaxies are the determining factors in the behavior of the velocity dispersion map is considered, indicating two counter- the molecular gas, or whether the molecular gas in ETGs fol- rotating stellar discs. Further properties of the sample galaxies are lows the same star-formation relations as in spirals (e.g. Kennicutt listed in Table 1. 1998; Bigiel et al. 2008; Shapiro et al. 2010; Wei et al. 2010a; Crocker et al. 2011). To completely understand star formation in ETGs, it is vital to study in a spatially-resolved way the molecular gas in an unbiased sample of molecular-gas rich ETGs. Therefore, 3 OBSERVATIONS, CALIBRATION AND DATA as part of the ATLAS3D project, we performed the present imag- REDUCTION ing survey with the Combined Array for Research in Millimeter 3.1 CARMA observations Astronomy (CARMA), the first of its kind capable of providing 12 significant conclusions about the state of molecular gas in ordinary Observations for this survey were taken in the CO(1–0) line at ETGs from interferometric imaging. CARMA over the course of five semesters, beginning in Autumn In 2, we describe the selection criteria used to define the 2008 and finishing in November 2010. Galaxies were always first CARMA§ sample. In 3, we describe the observational strategy, the observed with the CARMA D array, with 11 – 150m baselines, cor- ′′ data calibration and§ reduction, and the analysis techniques. In 4, responding to observable angular scales of 3.5 – 48 at CO(1–0). we investigate the properties of the molecular gas in the sample,§ in- NGC 2697 and NGC 7465, that appeared to have significant flux cluding the range of morphologies present and their relationships to resolved out, were followed up with the more compact E array (8 other host galaxy properties. We conclude briefly in 5. Appendix – 66m baselines). NGC 1266 was spatially unresolved in D array, A describes the CO data of individual galaxies in§ the CARMA and was followed up with the CARMA B and A arrays (a detailed ATLAS3D sample. Appendix B presents CO literature data of CO- discussion of NGC 1266 can be found in Alatalo et al. 2011). The 3D imaged ATLAS3D galaxies, that will be included in the official data CARMA ATLAS survey had a surface brightness sensitivity (1σ −1 −2 release in a uniform manner. in 100 km s linewidth) ranging from 12 to 369 M⊙ pc , with −2 median a sensitivity of 84 M⊙ pc . On average, 100 hours of observations were obtained each semester. Observational≈ parame- ters are listed in Table 2. 2 THECARMA SAMPLE Upgrades to the CARMA correlator and receivers were tak- 3D The sample of ETGs chosen for the CARMA survey was extracted ing place while the ATLAS survey was ongoing, so data taken from the ATLAS3D survey. All ATLAS3D galaxies were observed later in the programme have larger bandwidths and simultane- ous observations of 12CO(1–0) and 13CO(1–0). A handful of with the IRAM 30m telescope in CO(1–0) and CO(2–1), mostly 3D 13 by Combes et al. (2007) and Paper IV, though a few were observed ATLAS galaxies thus also have CO maps that will be pre- sented in an upcoming paper. The galaxies with large line widths by Welch & Sage (2003). The CARMA sample consists of 30 of −1 the CO-detected ATLAS3D galaxies (see Table 1). NGC 2697 and (∆v & 420 km s ) were observed only after the CARMA corre- NGC 4292, removed from the ATLAS3D sample because of evi- lator was upgraded, providing sufficient bandwidth and channel dence of spiral structure in optical images and of a lack of SAURON resolution to properly cover and sample the line. We were able data, respectively, were also imaged with CARMA. We present to reliably image 3mm continuum in three sources (NGC 1266, their maps in Appendix C, but will not use them in any statistical NGC 3665 and NGC 5866), and Table 3 lists those fluxes as well work discussed in 4. We will refer to the 30 CO-rich ATLAS3D as upper limits for the other galaxies. galaxies with CARMA§ data as the CARMA ATLAS3D sample. Including 10 CO-detected sample galaxies that have already been interferometrically-mapped (see 3.5). The total number of 3.2 Calibration and imaging 3D § ATLAS galaxies with interferometric observations discussed in Raw CARMA visibility data were reduced in the usual way, using 3D this paper is 40. This sample of CO-imaged ATLAS galaxies the Multichannel Image Reconstruction Image Analysis and Dis- is complete for the 33 brightest objects, down to an integrated play (MIRIAD) package (Sault et al. 1995). For each source and −1 CO(1–0) flux limit of 18.5 Jy km s (corresponding to the flux track, the raw data were first Hanning-smoothed in velocity. Then of NGC 3182). Two galaxies with fluxes below this threshold also the phase vs. time behaviour of the calibrator was checked to search have CARMA CO images, UGC 05408 and NGC 5173. Five other for decorrelations over baselines, which were flagged out. Next, CO-faint galaxies have CO maps in the literature (NGC 4550 by the data were corrected for differences in the lengths of the fiber Crocker et al. 2009; NGC 2768, NGC 4477 and NGC 3489 by optic lines between the antennas and the correlator. The bandpass Crocker et al. 2011; NGC 2685 by Schinnerer & Scoville 2002). The faintest detections from Paper IV were not observed due to observing time restrictions. 2 UGC 05408 was kept in the ATLAS3D survey because its estimated dis- 3D Objects in the CARMA ATLAS sample have total absolute tance is within 42 Mpc when errors in the distance estimate are taken into K-band magnitudes ranging from MK = 21.57 to 25.09, and account (Paper I) − − c 2012 RAS, MNRAS 000, 1–52 4 K. Alatalo and the ATLAS3D team

Table 1. CARMA ATLAS3D galaxy sample.

α δ v i φ d Virgo Name sys mol (J2000) (J2000) (km s−1) (deg) (deg) (Mpc) membership IC 676 11 12 39.84 +09 03 20.7 1429 69 16.5 24.6 0 IC 719 11 40 18.52 +09 00 35.6 1833 74 229.0 29.4 0 IC 1024 14 31 27.07 +03 00 30.0 1479 72 24.5 24.2 0 NGC 1222 03 08 56.76 −02 57 19.3 2422 41 33.0c 33.3 0 NGC 1266 03 16 00.79 −02 25 38.6 2170 26 270 29.9 0 NGC 2764 09 08 17.44 +21 26 35.8 2706 65 202.5 39.6 0 NGC 2824 09 19 02.22 +26 16 12.3 2758 61 161.5 40.7 0 NGC 3182 10 19 33.02 +58 12 21.0 2118 35 331.5 34.0 0 NGC 3607 11 16 54.54 +18 03 07.1 942 34 302.5 22.2 0 NGC 3619 11 19 21.60 +57 45 28.3 1560 48 74.5 26.8 0 NGC 3626 11 20 03.78 +18 21 25.6 1486 67 169.5 19.5 0 NGC 3665 11 24 43.64 +38 45 46.2 2069 64 219.5 33.1 0 NGC 4119 12 08 09.60 +10 22 44.7 1656 69 296.0 16.5 1 NGC 4150 12 10 33.65 +30 24 05.5 208 54 146.0 13.4 0 NGC 4324 12 23 06.17 +05 15 02.8 1665 62 232.0 16.5 1 NGC 4429 12 27 26.56 +11 06 27.3 1104 68 82.0 16.5 1 NGC 4435 12 27 40.49 +13 04 44.3 791 52 201.0 16.7 1 NGC 4694 12 48 15.10 +10 59 01.3 1171 69 155.5 16.5 1 NGC 4710 12 49 39.36 +15 10 11.7 1102 86 207.0 16.5 1 NGC 4753 12 52 22.07 −01 11 57.9 1163 75 93.0 22.9 0 NGC 5173 13 28 25.29 +46 35 29.9 2424 24 100c 38.4 0 NGC 5379 13 55 34.35 +59 44 34.3 1774 64 66 30.0 0 NGC 5866 15 06 29.60 +55 45 48.0 755 89 127 14.9 0 NGC 6014 15 55 57.39 +05 55 54.7 2381 22 139.5 35.8 0 NGC 7465 23 02 00.96 +15 57 53.3 1960 70 106.0 29.3 0 PGC 029321 10 05 51.18 +12 57 40.7 2816 38 76 40.9 0 PGC 058114 16 26 04.29 +02 54 23.6 1507 71 94.5 23.8 0 UGC 05408 10 03 51.86 +59 26 10.2 2998 31 315c 45.8 0 UGC 06176 11 07 24.68 +21 39 25.6 2677 68 201.0 40.1 0 UGC 09519 14 46 21.12 +34 22 14.2 1631 41 177.5 27.6 0 NGC 2697a 08 54 59.40 −02 59 15.2 1814b 30 301.5 22.0 0 NGC 4292a 12 21 16.49 +04 35 44.3 2258b 50 230 29.8 0

a Removed from the ATLAS3D sample, but the CO data are presented in Appendix C. b From the HYPERLEDA catalog, due to the absence of SAURON data. c Not originally in Paper V. Notes: Column (1): Principle designation from LEDA, used as the standard designation. Column (2): Right ascension (J2000), from LEDA. Column (3): Declination (J2000), from LEDA. Column (4): Optical stellar heliocentric velocity, from Paper I. Column (5): Best-determined CO inclination angle, from Paper V. Column (6): Kinematic position angle of the molecular gas, from Paper X. Column (7): Average distance to each galaxy, from Paper I, originally from Tonry et al. (2001) and Mei et al. (2007). Column (8): Virgo membership of each galaxy, from Paper I.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 5

Table 2. Observational parameters of CARMA galaxies

Gain Total θ × θ ∆V Bandwidth Name Semester maj min calibrator hours (arcsec) (km s−1) (km s−1) IC 676 2009B 1058+015 3.75 3.8 × 3.3 10 410 IC 719 2010A 3C273 13.17 3.9 × 2.8 20 580 IC 1024 2008B 3C279 4.68 3.9 × 3.0 10 420 NGC 1222 2008B 0339-017 5.20 3.6 × 3.2 5 420 NGC 1266 2008B 0339-017 5.43 4.2 × 3.3 10 410 NGC 2764 2009B 0854+201 4.43 3.5 × 2.9 10 410 NGC 2824 2008B 0956+252 8.79 4.3 × 4.0 25 400 NGC 3182 2009A 0927+390 7.42 5.2 × 4.1 30 390 NGC 3607 2010B 1058+015 9.30 5.6 × 5.0 20 900 NGC 3619 2010B 0958+655 24.44 4.4 × 3.9 40 880 NGC 3626 2009B 1159+292 7.50 3.9 × 3.7 25 400 NGC 3665 2010B 1159+292 16.59 4.3 × 4.2 10 910 NGC 4119 2008B 3C273 3.67 5.0 × 4.0 10 410 NGC 4150 2010A 1159+292 6.74 5.3 × 4.1 10 560 NGC 4324 2009A 3C273 20.18 4.7 × 3.9 20 400 NGC 4429 2010B 3C273 8.83 4.7 × 3.7 10 840 NGC 4435 2010B 3C273 8.48 3.9 × 3.4 10 920 NGC 4694 2010A 3C273 5.38 3.9 × 3.1 10 390 NGC 4710 2009A 3C273 5.10 3.9 × 3.2 10 410 NGC 4753 2010B 3C273 10.38 5.6 × 4.1 15 735 NGC 5173 2009Ba 1310+323 7.06 3.9 × 3.5 20 240 NGC 5379 2010A 1642+689 5.33 5.2 × 3.6 10 410 NGC 5866 2010B 1419+543 3.52 3.6 × 3.1 10 920 NGC 6014 2008B 1751+096 3.85 4.2 × 3.9 10 350 2008B NGC 7465 3C454.3 15.02 6.6 × 5.6 10 410 2009Ab PGC 029321 2009B 1058+015 4.52 3.8 × 3.7 10 410 PGC 058114 2009A 1549+026 3.62 4.4 × 3.8 10 410 UGC 05408 2009A 0927+390 2.00 4.6 × 3.5 25 196 UGC 06176 2009A 1159+292 4.08 3.5 × 2.8 15 735 UGC 09519 2008B 1310+323 3.75 3.4 × 2.9 10 410 2008B NGC 2697 0927+390 14.33 6.8 × 5.1 20 380 2009Ab NGC 4292 2008B 3C273 19.86 4.1 × 3.3 10 410 a Observed both in C- and D-arrays b Observed in D-array in 2008B and E-array in 2009A. Notes: Column (1): Rrinciple designation from LEDA, used as the standard designation. Column (2): Semester in which the observations were taken at CARMA. Column (3): Gain calibrator used. Column (4): Total on-source observing time in hours. Column (5): FWHM of the major and minor axes of the synthesized beam. Column (6): Final velocity channel width. Column (7): Velocity bandwidth covering the line.

c 2012 RAS, MNRAS 000, 1–52 6 K. Alatalo and the ATLAS3D team was then determined using a high signal-to-noise ratio (S/N) ob- smoothed spatially (with a FWHM equal to that of the beam), and servation of a bright calibrator, and used to correct for instrumen- masks were created by selecting all pixels above fixed flux thresh- tal spectral fluctuations. The atmospheric phase offsets present in olds, adjusted to recover as much flux as possible in the moment the data were determined using a phase calibrator, usually a quasar maps while minimising the noise (generally about 2–3 times the within 20◦ of the source, observed at regular ( 15 minutes) in- rms noise in the smoothed channels). The moment maps were then tervals. Amplitude calibration was performed using≈ the phase cal- created using the unsmoothed cubes within the masked regions ibrator. A catalog of the most up-to-date fluxes of each calibrator only. is maintained at CARMA, both through monitoring of calibrator All data products were converted into Flexible Image Trans- fluxes during science tracks and through dedicated flux calibration port System (FITS) files using MIRIAD. Tables 2 and 3 list some tracks taken on a weekly basis, and is updated weekly using all datacube properties for each of the ATLAS3D CARMA galax- tracks that include a primary calibrator (e.g. a planet), used to in- ies. Figure 1 shows the CO moment0 contours of each CARMA fer the secondary calibrator fluxes (Bauermeister et al. 2012). Flux ATLAS3D sample galaxy overlaid on an r-band image, either from calibration uncertainties are assumed to be 20%, which is standard the Sloan Digital Sky Survey (SDSS) or the Isaac Newton Tele- for millimeter observations using planetary models (Petric et al., in scope (INT) when SDSS imaging is unavailable (Scott et al. 2012, prep). After the data were satisfactorily processed, the gain solu- submitted, hereafter Paper XXI). Figure 2 displays the moment1 tions derived from the nearby calibrator were applied to the source. maps of the 30 sample galaxies. Figure 3 shows the CO moment0 The calibrated source data of all observations of each source were contours overlaid on unsharp-masked optical images, to enhance then combined into one visibility file for imaging. dust features (see 4.1). Figure 4 displays position-velocity dia- § We then used MIRIAD to convert all visibility files to three- grams (PVDs) of galaxies whose kinematics are not well repre- dimensional (3D) data cubes. When possible, a zeroth order con- sented with moment1 maps, due to multiple velocity components tinuum fit to the uv-data was made using channels free of line along the line-of-sight (NGC 2764, NGC 4710 and NGC 5866). emission, and was subtracted from all channels. Only galaxies Appendix A contains multiple figures for each CARMA ATLAS3D observed after the correlator was upgraded (bandwidth > 420 galaxy, including a r-band-moment0 overlay, moment0 map, mo- km s−1) had sufficient bandwidth for a reliable continuum fit. ment1 map, a comparison of the CARMA and IRAM 30m spectra, Galaxies with narrower bandwidths were not continuum-subtracted a PVD along the kinematic position angle determined in Paper X, (continuum emission generally adds < 10% extra flux to each and individual channel maps. A more detailed analysis of the PVD, galaxy, much less than the total flux calibration uncertainties, and as well as a comparison to the stellar and ionized gas kinematics is this is usually confined to the central beam in each galaxy). The available in Davis et al. (2012, hereafter Paper XIV). continuum-subtracted uv-datasets were then transformed into RA- The continuum measurement or upper limit for each galaxy Dec-velocity space (with velocities determined from the line be- depended on the correlator configuration. For narrow-band (band- ing imaged, mainly 12CO but also occasionally 13CO). Channel width 420 km s−1) galaxies that did not include 13CO in the ≈ widths were chosen to achieve at least a 3σ detection in each chan- lower sideband, the full lower sideband was used to calculate the nel where flux was present, and were always larger (by at least a continuum (bandwidth 186 MHz). For narrow-band galaxies that 13 ≈ factor of 2) than the original spectral resolution of the uv-data. Pix- included CO observations, the edges of the band in the lower els of 1′′ 1′′ were chosen as a compromise between spatial sam- sideband were used (bandwidth 124 MHz). Galaxies that were ≈ pling and× resolution, typically giving approximately 4 pixels across observed with the upgraded correlator were treated individually, the the beam major axis. A constant pixel size was chosen to maintain continuum being modeled in line-free channels only, which varied uniform spatial sampling across the sample. One arcsecond corre- from galaxy to galaxy. The continuum upper limit was taken to be sponds to a physical scale between 72 and 222 pc, depending on three times the rms noise of the dirty map produced by inverting the the distance of the source. The areas imaged were generally cho- combined line-free channels. Galaxies where a continuum source sen to be within the primary beam of the 10m antennas ( 54′′), was detected (NGC 1266, NGC 3665 and NGC 5866), the flux was but in the cases of sources that extend beyond this (NGC≈ 4324, measured from the detected point source, and the rms noise was NGC 4710 and NGC 5866), the area imaged was taken to be closer measured in the flux-free regions of the cleaned maps. to the primary beam of the 6m antennas ( 90′′). In these cases, the MIRIAD imaging task INVERT was run≈ with the mosaicking op- 3.3 Measurements from the data tion, to properly scale the data and account for the different primary beam widths. To calculate the noise level, σrms of each data cube, we selected Robust=0 weighting was used by default, but was changed all the pixels within each cube outside the region known to contain if the size and make-up of the source dictated it. Natural weighting flux, and calculated the standard deviation. The total flux per chan- (robust = 1) was used for sources where large scale features nel was then calculated by using the region of the moment0 map presented in the initial (robust = 0) channel maps, and we sus- that contained flux, then summing over all pixels in each channel pected that some flux might be resolved out (NGC 3619, NGC 3626 located within that region. The statistical noise per channel is calcu- and NGC 4324). The dirty cubes were cleaned in regions of source lated as σrms √Nb , where Nb is the number of beam areas in the emission to a threshold equal to the rms of the dirty channels. The region with identified∗ emission. The CARMA integrated spectra clean components were then added back and re-convolved using a presented in Appendix A have been constructed using this method. Gaussian beam of full-width at half maximum (FWHM) equal to The integrated fluxes in the channel maps were converted from the that of the dirty beam. This produced the final, reduced and fully native Jansky beam−1 units into Jansky by dividing out the total calibrated data cube for each galaxy. beam area in pixels, and are given in Table 3. The 3D data cubes were then used to create moment maps of PVDs were created by taking thin (5 pixel) slices through the each galaxy: a zeroth moment (moment0) or integrated intensity data cubes, positioned to intersect the centre of the CO emission, map, and a first moment (moment1) or mean velocity map. The and using the kinematic position angle determined in Paper X. Ta- data cubes were first Hanning-smoothed in velocity and Gaussian- ble 1 also lists the kinematic position angles of galaxies not orig-

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 7

Table 3. Data parameters of CARMA ATLAS3Dgalaxies

M σrms Continuum FCARMA H2 FCARMA Morph. Name −1 −1 −1 log M (mJy bm ) (mJybm ) (Jykms ) ⊙ F30m class. IC 676 30.6 < 3.09 66.3 ± 2.5 8.71 ± 0.04 1.2 ± 0.05 D IC 719 6.63 < 0.351 20.4 ± 1.0 8.34 ± 0.05 1.2 ± 0.12 D IC 1024 19.4 < 3.06 94.6 ± 1.7 8.87 ± 0.02 1.8 ± 0.04 D NGC 1222 23.1 < 1.97 147.6 ± 1.6 9.33 ± 0.01 1.8 ± 0.04 X NGC 1266 22.8 7.49 ± 1.96 162.9 ± 0.7 9.28 ± 0.01 1.0 ± 0.03 D NGC 2764 12.9 < 1.85 85.4 ± 1.5 9.23 ± 0.02 1.1 ± 0.04 B+R NGC 2824 10.2 < 2.21 37.8 ± 0.8 8.91 ± 0.02 1.8 ± 0.08 D NGC 3182 8.16 < 1.68 16.4 ± 0.7 8.41 ± 0.04 1.2 ± 0.12 R NGC 3607 7.50 < 0.830 58.0 ± 0.8 8.50 ± 0.01 1.2 ± 0.04 D NGC 3619 3.23 < 0.327 15.2 ± 0.4 8.28 ± 0.03 0.7 ± 0.12 M NGC 3626 5.34 < 1.48 43.2 ± 0.9 8.32 ± 0.02 1.3 ± 0.10 D NGC 3665 10.2 8.98 ± 0.42 94.3 ± 1.2 9.11 ± 0.01 1.6 ± 0.06 D NGC 4119 20.2 < 2.64 39.3 ± 0.9 8.14 ± 0.02 1.8 ± 0.07 R NGC 4150 9.41 < 1.87 20.5 ± 0.4 7.82 ± 0.02 0.7 ± 0.08 M NGC 4324 4.30 < 0.974 27.2 ± 0.6 7.97 ± 0.02 1.9 ± 0.12 R NGC 4429 9.53 < 0.375 70.8 ± 0.9 8.39 ± 0.01 2.2 ± 0.08 D NGC 4435 11.5 < 0.375 31.6 ± 1.0 8.05 ± 0.03 1.5 ± 0.10 R NGC 4694 9.30 < 0.512 21.7 ± 0.6 8.01 ± 0.03 0.7 ± 0.07 X NGC 4710 14.0 < 5.20 351.2 ± 1.7 9.08 ± 0.01 2.3 ± 0.03 B+R NGC 4753 11.1 < 0.521 74.7 ± 1.1 8.70 ± 0.01 1.4 ± 0.06 M NGC 5173 8.16 < 1.46 12.5 ± 0.2 8.36 ± 0.02 1.2 ± 0.14 X NGC 5379 10.8 < 0.450 18.5 ± 0.8 8.53 ± 0.04 1.6 ± 0.15 B+R NGC 5866 17.6 4.02 ± 0.54 258.2 ± 3.4 8.75 ± 0.01 1.9 ± 0.02 B+R NGC 6014 22.4 < 3.61 34.5 ± 1.0 8.77 ± 0.03 1.0 ± 0.07 S NGC 7465 9.71 < 1.39 93.6 ± 0.4 9.02 ± 0.01 1.7 ± 0.04 M PGC 029321 13.1 < 2.09 18.3 ± 0.7 8.61 ± 0.04 1.2 ± 0.09 D PGC 058114 15.7 < 2.21 73.7 ± 0.9 8.75 ± 0.01 1.4 ± 0.04 D UGC 05408 13.6 < 2.83 6.1 ± 0.5 8.32 ± 0.08 0.8 ± 0.18 D UGC 06176 10.8 < 0.524 28.5 ± 0.8 8.76 ± 0.03 1.5 ± 0.10 D UGC 09519 19.5 < 2.27 51.4 ± 1.4 8.77 ± 0.03 0.9 ± 0.04 M NGC 2697 9.89 < 1.36 48.2 ± 0.7 8.61 ± 0.01 2.3 ± 0.11 R NGC 4292 9.58 < 1.05 13.8 ± 0.5 7.74 ± 0.04 1.2 ± 0.14 R Notes: Column (1): Principle designation from LEDA, used as the standard designation. Column (2): Root mean square noise level per channel, measured in regions devoid of line emission. Column (3): Continuum emission or upper limit (see text). Column (4): Total CO flux from CARMA. 20 −1 −1 −2 Column (5): Total molecular gas mass from the CARMA observations using XCO = 3 × 10 (K km s ) cm (as in Paper IV) Column (6): Fraction of CO flux recovered by CARMA (with respect to the IRAM 30m telescope). Column (7): CO morphological classification, based on the moment0 and moment1 maps: D = disc, X = strongly disrupted, R = ring, M = mildly disrupted, B = bar/ring, S=spiral. inally listed in Paper X, but subsequently had kinematic position As discussed above, all galaxies detected with the IRAM 30m angles fitted using the same methods. were also detected at CARMA. However, the IRAM 30m selec- tion for the current CARMA survey does imply that galaxies with molecular gas exclusively beyond the 30m beam (e.g. rings, arms 3.4 Comparison to the 30m data and tidal features beyond a radius of 12′′) would have been ≈ The integrated spectra from CARMA and the IRAM 30m telescope missed. It is impossible to estimate the incidence of these objects are overlaid in Figs. A1–A30. Millimeter measurements are as- based on the CO data alone, but the Galaxy Evolution Explorer sumed to have 20% absolute flux uncertainties (errors reported on (GALEX) ultraviolet imaging survey of the SAURON sample (trac- the measured parameters listed in Table 3 only include the random ing the associated star formation) suggests that they are very rare errors on the measurement itself, not the systematic flux calibration (of 34 ETGs, only one has such features, NGC 2974; Jeong et al. error), so flux ratios between 0.78 and 1.28 indicate fluxes in agree- 2009). Lower density neutral hydrogen is however fairly common ment within the uncertainties. The spectra from the IRAM 30m at large radii (Paper XIII). agree with the CARMA ones for 15/30 galaxies. In all cases where there is disagreement, CARMA actually recovers more flux than the 30m. Most discrepant galaxies either extend beyond, or fill the Because the molecular gas in many (> 75%) galaxies extends majority of the single-dish beam, with two large ratios (NGC 4435 beyond the single-dish beam, it is likely that the CARMA flux more and UGC 06176) likely due to a slight off-center pointing of the accurately reflects the total molecular gas mass in each galaxy, and single dish. In fact, only 7 of the galaxies within the CARMA therefore we adopt the CARMA derived molecular gas masses for ATLAS3D sample are well contained within the 21.6′′ IRAM beam. the remainder of this paper.

c 2012 RAS, MNRAS 000, 1–52 8 K. Alatalo and the ATLAS3D team

IC 676 IC 719 IC 1024 NGC 1222 NGC 1266

10″ = 1.2 kpc 10″ = 1.4 kpc 10″ = 1.2 kpc 10″ = 1.6 kpc 10″ = 1.4 kpc

NGC 3607 NGC 3619 NGC 2764 NGC 2824 NGC 3182

″ ″ ″ ″ ″ 10 = 1.9 kpc 10 = 2.0 kpc 10 = 1.6 kpc 10 = 1.1 kpc 10 = 1.3 kpc

NGC 3626 NGC 3665 NGC 4119 NGC 4150 NGC 4324

10″ = 0.95 kpc 10″ = 1.6 kpc 10″ = 0.80 kpc 10″ = 0.65 kpc 10″ = 0.80 kpc

NGC 4429 NGC 4435 NGC 4694 NGC 4710 NGC 4753

″ ″ ″ ″ ″ 10 = 0.80 kpc 10 = 0.81 kpc 10 = 0.80 kpc 10 = 0.80 kpc 10 = 1.1 kpc

NGC 5173 NGC 5379 NGC 5866 NGC 6014 NGC 7465

10″ = 1.9 kpc 10″ = 1.5 kpc 10″ = 0.72 kpc 10″ = 1.7 kpc 10″ = 1.4 kpc

PGC 029321 PGC 058114 UGC 05408 UGC 06176 UGC 09519

10″ = 2.0 kpc 10″ = 1.2 kpc 10″ = 2.2 kpc 10″ = 1.9 kpc 10″ = 1.3 kpc

Figure 1. r-band images (grayscale and black contours) overlaid with integrated CO(1–0) contours (yellow) at [10%, 30%, 50%, 70%, 90%] of the peak intensity for the 30 galaxies in the ATLAS3D CARMA sample. The r-band images were either taken from the SDSS or a dedicated program with the INT (Paper XXI) The CO synthesized beam is shown in the bottom-right corner of each panel. A bar in the bottom left corner of each panel indicates the scale of 10′′, as well as the equivalent physical scale at the distance of the galaxy.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 9

IC 676 IC 719 IC 1024 NGC 1222 NGC 1266

5″=0.60 kpc 5″=0.71 kpc 5″=0.59 kpc 5″=0.81 kpc 5″=0.72 kpc

NGC 2764 NGC 2824 NGC 3182 NGC 3607 NGC 3619

5″=0.96 kpc 5″=0.99 kpc 5″=0.82 kpc 5″=0.54 kpc 5″=0.65 kpc

NGC 3626 NGC 3665 NGC 4119 NGC 4150 NGC 4324

″ 5″=0.80 kpc 5″=0.40 kpc 5″=0.32 kpc ″ 5 =0.47 kpc 5 =0.40 kpc

NGC 4429 NGC 4435 NGC 4694 NGC 4710 NGC 4753

5″=0.40 kpc 5″=0.40 kpc 5″=0.40 kpc ″ 5″=0.56 kpc 5 =0.40 kpc

NGC 5173 NGC 5379 NGC 5866 NGC 6014 NGC 7465

5″=0.93 kpc 5″=0.73 kpc 5″=0.36 kpc 5″=0.87 kpc 5″=0.71 kpc

PGC 029321 PGC 058114 UGC 05408 UGC 06176 UGC 09519

″ ″ ″ ″ ″ 5 =0.99 kpc 5 =0.58 kpc 5 =1.1 kpc 5 =0.97 kpc 5 =0.67 kpc

Figure 2. Mean CO(1–0) velocity maps of the 30 galaxies of the ATLAS3D CARMA sample. Iso-velocity contours (black) are overlaid at 20 km s−1 intervals, as are contours from the moment0 map (white). The CO synthesized beam is shown at the bottom-right corner of each panel. A bar in the bottom left corner of each panel indicates the scale of 5′′, as well as the equivalent physical scale at the distance of the galaxy.

c 2012 RAS, MNRAS 000, 1–52 10 K. Alatalo and the ATLAS3D team

3.5 Literature data Table 4. Properties of the ATLAS3D literature galaxies 3D Twelve galaxies of the ATLAS sample already have in- Distance Morph. Virgo Name Reference terferometric CO data available in the literature. Those (Mpc) class.a membership galaxies are: NGC 4710 (Wrobel et al. 1992), NGC 2685 NGC 524 23.3 D 0 6 (Schinnerer & Scoville 2002), and the ten galaxies that will NGC 2685 16.7 R 0 1 be part of the ATLAS3D data release: NGC 4476 (Young NGC 2768 21.8 D 0 4 2002); NGC 3032, NGC 4150, NGC 4459 and NGC 4526 NGC 3032 21.4 D 0 3 (Young, Bureau & Cappellari 2008); NGC 2768 (Crocker et al. NGC 3489 11.7 S 0 6 2008); NGC 4550 (Crocker et al. 2009); NGC 524, NGC 3489 NGC 4459 16.1 D 1 3 and NGC 4477 (Crocker et al. 2011). Names, distances, Virgo NGC 4476 17.6 D 1 2 NGC 4477 16.5 R 1 6 membership, CO morphological classes and references of these NGC 4526 16.4 D 1 3 galaxies are listed in Table 4. When required, data for each of NGC 4550 15.5 D 1 5 the galaxies were provided by the original authors for use in this References: (1) Schinnerer & Scoville (2002); (2) Young (2002); work. Moment maps and dust comparisons appear in Figure B1 (3) Young, Bureau & Cappellari (2008); (4) Crocker et al. (2008); (5) for the galaxies whose data will be included in the data release. Crocker et al. (2009); (6) Crocker et al. (2011) Both NGC 4710 and NGC 4150 were re-observed as part of the Notes: a CARMA ATLAS3D survey, and we only present these updated CO morphological classification based on the moment0 and moment1 data in this paper. maps. D = disc, X = strongly disrupted, R = ring, M = mildly disrupted, B = bar/ring, S=spiral.

3D 3.6 Catalog of ATLAS interferometric CO data ing g r colour SDSS images (and for NGC 1222 and NGC 7465, − The CARMA data archive3 will include CARMA data for all 30 for which SDSS images are unavailable, on INT images, and for galaxies, as well as data for the 10 previously published galaxies NGC 1266, on CTIO b and r band images from the SINGS survey; and the two non-ATLAS3D sources. The data products provided Kennicutt et al. 2003). In order to create the g r images, the God- − will include data cubes and moment0 and moment1 maps in FITS dard IDL library task SKY was used to determine the background format. The data will also be reachable from the ATLAS3Dproject sky level, then subtracted from the images. The g r colour im- − website4. ages were then created by dividing the sky-subtracted g-band image from the sky-subtracted r-band image. The g r imaging enhances the visibility of dust features by directly tracing− extinction and pro- 4 DISCUSSION vides a qualitative view of the distribution of the filamentary dust in each galaxy of the ATLAS3D CARMA sample. This dust, for Figures 1 and 2 show the 30 ETGs imaged as part of the the most part, is a reasonable indicator of the distribution of the CARMA ATLAS3D survey. Before the survey was complete molecular gas. (which includes the 10 literature galaxies mentioned in 3.5), For simplicity we refer to the g r colour images as “dust § 16 ETGs had spatially-resolved CO maps (Wrobel et al. 1992; images” for the remaining text, even if− they are intrinsically only Schinnerer & Scoville 2002; Young 2002, 2005; Wei et al. 2010a; representations of stronger dust-obscured regions. Indeed, the CO Young, Bureau & Cappellari 2008; Crocker et al. 2011), most ob- is nearly always (28/29 instances) associated with evidence of tained as part of individual or small-sample studies. The addi- dust obscuration. It is evident that the converse is not true, as a tion of the CO-imaged ATLAS3D sources increases this amount Hubble Space Telescope (HST) survey of nearby ellipticals re- to over 50, and provides a largely unbiased sample. Combined with vealed that they contain dust in nearly half the cases (Tran et al. the maps from the SAURON integral-field spectrograph, the CO- 2001; Lauer et al. 2005), much more than the CO detection rate mapped ATLAS3D galaxies thus provide the most robust picture of of ATLAS3D. Additional dust is seen beyond the limits of the de- molecular gas-rich ETGs. tected CO emission in most galaxies, but notably in NGC 1266, We now focus our analysis on the CO-rich ATLAS3D ETGs NGC 3619, NGC 4150, NGC 4694 and NGC 4753. However, there only, adding the ten ATLAS3D galaxies imaged in CO with the is no noticeable dust beyond the detected extent of the CO in oth- Berkeley-Illinois-Maryland Array (BIMA), the Owens Valley Ra- ers. It thus appears that in most cases where the dust and CO are dio Observatory (OVRO) and the Plateau de Bure Interferometer co-spatial, dust provides a good, high spatial resolution rendering (PdBI) prior to the CARMA effort. Between the 30 CARMA galax- of the molecular gas structure. Where dust is more extended than ies and 10 previously published galaxies (excluding two overlap- the CO, it could simply be that the outer CO is below our detec- ping objects; see Table 4), we imaged 40 galaxies or 65% of the tion threshold, or that the ISM is not molecular at all (for instance, CO detections in Paper IV, more than 90% of the total molecular it could be atomic or warm). With this caveat in mind, we use the gas mass in those detections, and are complete down to a CO(1–0) dust images as a useful guide to the morphological structures in integrated flux of 18.5 Jy km s−1 . which the cold ISM resides. We exploit this fact below when the CO morphological class is difficult to determine (e.g. IC 676 and NGC 4435). 4.1 Comparison to the dust Figure 3 shows the CO moment0 contours of each galaxy overlaid on a g r colour image. The dust distributions are shown by creat- 4.2 Morphologies of the molecular gas − The CO-imaged ATLAS3D survey illustrates that the molecular 3 http://carma-server.ncsa.uiuc.edu:8181/ gas in ETGs comes in a large variety of morphologies. We have 4 http://purl.org/atlas3d identified six different morphologies, including smooth discs (D),

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 11

IC 676 IC 719 IC 1024 NGC 1222 NGC 1266

10″ 10″ 10″ 10″ 10″

NGC 2764 NGC 2824 NGC 3182 NGC 3607 NGC 3619

10″ 10″ 10″ 10″ 10″

NGC 3626 NGC 3665 NGC 4119 NGC 4150 NGC 4324

10″ 10″ 10″ 10″ 10″

NGC 4429 NGC 4435 NGC 4694 NGC 4710 NGC 4753

10″ 10″ 10″ 10″ 10″

NGC 5173 NGC 5379 NGC 5866 NGC 6014 NGC 7465

10″ 10″ 10″ 10″ 10″

PGC 029321 PGC 058114 UGC 05408 UGC 06176 UGC 09519

10″ 10″ 10″ 10″ 10″

Figure 3. Comparison of the integrated CO(1–0) distribution (magenta contours) and the dust distribution as represented by g − r colour images (grayscale) for the 30 galaxies of the ATLAS3D CARMA sample. It appears that galaxies with disrupted CO morphologies also exhibit disturbance in the dust distribution, and overall the molecular gas in the galaxies traces the filamentary dust.

c 2012 RAS, MNRAS 000, 1–52 12 K. Alatalo and the ATLAS3D team

Table 5. CO morphologies of the ATLAS3D interferometric The NGC 4753 dust structure is well explained by a precessing sample. twisted disc after the accretion of a gas-rich dwarf companion (Steiman-Cameron et al. 1992). The original BIMA observations Morphological Number Fraction Symbol of NGC 4150 (Young, Bureau & Cappellari 2008) show a pro- configuration (out of 40) (%) nounced low-surface density elongated tail that was not recovered Disc D 20 50 by CARMA, both due to a smaller field of view and higher spa- Spiral S 2 5 tial resolution. A study of the gas-phase metallicity of NGC 4150 Ring R 6 15 also show it to be sub-Solar (Z 0.3 0.5 Z⊙), therefore the Bar+Ring B+R 4 10 ≈ − Mild disruption M 5 12.5 molecular gas is likely to originate from an external accretion event Strong disruption X 3 7.5 (Crockett et al. 2011). It appears that field galaxies are far more likely to exhibit disrupted morphologies than Virgo cluster galaxies, with 24 8% spirals (S), rings (R), bars+rings (B+R), as bars are always found (7/29) of field galaxies classified as either M or X as opposed± to with rings, never alone, mildly disrupted objects (M), and strongly 9 9% (1/11) for Virgo galaxies. This is not surprising given the disrupted objects (X). These classifications are strictly for the results± of Paper X, which suggested that galaxies virialised within molecular gas, as all galaxies are optically-classified as ETGs. The the cluster are unable to replenish their stores of molecular gas via CO morphological classification of each galaxy was based on an external accretion, and thus only longer-lived phenomena survive, analysis of its moment0 and dust maps (Fig. 3), moment1 map such as bars and rings. Overall, the M- and X-class objects seem to (Fig. 2) and major-axis PVD (Figs. A1-30). In many cases the mo- host gas that has an external origin, and they are probably dynami- ment0 and moment1 map allowed us to unambiguously classify cally younger than the other objects, explaining the dearth of such a galaxy. For ambiguous cases, the PVD was used to search for objects within Virgo. distinct kinematic signatures. Finally, the dust map was used as a higher spatial resolution proxy for the molecular gas. The criteria for each CO morphological class are as follows. 4.2.2 Molecular rings and bars Galaxies classified as discs (D) show regular rotation and a smooth Rings (R) and bars+rings (B+R) also make up a non-negligible elliptical shape. The PVD of D-class objects also show smooth ve- fraction of the ATLAS3D molecular gas morphologies, represent- locity variations with no discontinuity. Galaxies classified as spi- ing about a fifth (8/40) of the CO sample. It is of note that cold rals (S) show regular rotation, but the moment0 and/or dust maps gas in barred galaxies accumulates in rings associated with the ma- exhibit discrete spiral arms. Galaxies classified as rings (R), like jor resonances (e.g. Buta & Combes 1996), so it is possible that discs, exhibit regular rotation, but unlike discs, the PVD of R-class bar+ring systems are simply in an early stage of an evolution- objects include a solid-body component and/or a discontinuity in ary sequence, whereby the bar funnels gas into the centre (e.g. velocity. Well-resolved rings show a central hole in the moment0 Bournaud & Combes 2002), evacuating the central (but not nu- map. In the most ambiguous cases, the dust map was consulted to clear) regions of molecular gas, and later leaving the ring struc- search for a dust ring (e.g. NGC 4119 and NGC 4435). Bar+Ring ture intact, without a molecular gas-rich bar. This scenario would systems (B+R) were identified either directly from the moment1 explain why bars are only seen with rings, but not the converse. map, when the bar and ring are both distinctly visible, or using the Figure 4 shows the PVDs of three galaxies (NGC 2764, PVD and searching for an X-shaped pattern (in the case of edge-on NGC 4710 and NGC 5866) that possess two velocity components systems; see 4.2.2). Galaxies classified as mildly disrupted (M) along the line-of-sight. All three galaxies are edge-on, and the char- have mainly regular§ disc morphologies, but include small devia- acteristic X-shaped PVDs observed are normally associated with tions in their moment0 and moment1 maps. Finally, a galaxy is the kinematic signature of a bar in an edge-on disc. The mate- classified as strongly disrupted (X) for showing strong irregulari- rial in the inner rapidly-rising component of each PVD is asso- ties in the CO kinematics. . ciated with gas on x2 orbits (elongated perpendicular to the bar and located within the inner Lindblad resonance, ILR), while the material in the outer slowly-rising component is associated with 4.2.1 Strongly and mildly disrupted objects gas on nearly circular orbits beyond corotation. The intermediate The origin of the strongly disrupted (X) objects is the most easily region has been largely swept free of gas by the bar, due to in- explained. These galaxies show highly irregular CO distributions flows toward the ILR (see Sellwood et al. 1993 for a review of bar and kinematics, that are normally characteristic of interacting sys- dynamics). The signature is analogous to that of the Milky Way tems, a fact often confirmed by observations at other wavelengths. bar in a Galactic longitude-velocity diagram. It was first proposed In the case of NGC 1222 and NGC 4694, it is clear that they ac- in external galaxies by Kuijken & Merrifield (1995), later refined quired their gas via external accretion (see Beck et al. 2007 and by Bureau & Athanassoula (1999) and Athanassoula & Bureau Duc et al. 2007 for details on each galaxy). NGC 5173 is known to (1999), who both identified multiple examples observationally host a large misaligned H I disk (Paper XIII). (Merrifield & Kuijken 1999; Bureau & Freeman 1999). The bar Mildly disrupted CO distributions (M) also appear to be signatures in NGC 2764 and NGC 5866 are observed here for the in less relaxed systems than the rest. In some cases, there is first time, but that in NGC 4710 was previously observed in CO strong evidence that the gas is being acquired externally, such by Wrobel et al. (1992). The link between bars and boxy-shaped as in NGC 7465 (Li & Seaquist 1994), which is accreting from bulges (such as that in NGC 4710) has long been established, but an external H I reservoir via a close interaction with other galax- the presence of a bar in NGC 5866 is rather unexpected given its ies. NGC 3619 and UGC 09519 are known to host large mis- large classical bulge (see Athanassoula 2005 for the different bulge aligned H I discs (Paper XIII), providing a likely source for the types and the bar-boxy bulge relationship). molecular gas. The irregular dust filaments in NGC 4753 are The fraction of molecular gas-rich ETGs (6/40) that contain a the main reason that the CO is classified as an M morphology. ring structure is also a factor of 2 larger than that of LTGs, based ≈ c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 13

0.91 1300 3.3 1.5 1000 2800 0.67 2.7 1.1 ) ) ) 900 -1 -1 -1 1200 0.43 2.0 0.73 800 2700 (K) 0.19 (K) 1.4 (K) 0.35 B B 1100 B T T T 700 -0.048 0.76 -0.021 Velocity (km s Velocity (km s Velocity (km s 2600 1000 600 -0.29 0.13 -0.39

″ beam = 3.5″ ″ 500 beam = 3.3 -0.53 900 beam = 3.7 -0.50 -0.77 0 10 20 30 40 50 0 10 20 30 40 50 60 0 10 20 30 40 50 60 Offset (arcsec), p.a. = 203.° Offset (arcsec), p.a. = 207.° Offset (arcsec), p.a. = 127.° Figure 4. Position-velocity diagrams of the three CARMA ATLAS3D ETGs with clear two-component velocity profiles, that are not properly represented by the moment1 maps. The galaxies are NGC 2764 (left), NGC 4710 (middle) and NGC 5866 (right). All 3 galaxies are edge-on or almost edge-on and show the characteristic X-shaped PVD signature of an edge-on bar (see §4.2.2) on the BIMA Survey of Nearby Galaxies (SONG) sample (3/39; and may thus prevent gravitational instabilities linked to spiral arms Sheth et al. 2002; Helfer et al. 2003) modified to match the average from developing (Toomre Q parameter; e.g. Toomre 1981). noise and redshift of the ATLAS3D sample (as in Paper XIV and It is also possible that some of the D morphologies would 4.2.3). Also, unlike for LTGs, the molecular gas morphology does have been classified otherwise with observations of better sensi- § not necessarily follow the stellar morphology, most notably stellar tivity and/or spatial resolution. For instance, much higher spatial bars. Galaxies with stellar bars identified in Paper II are as likely to resolution CO observations of NGC 1266 presented in Alatalo et al. have a disc-like (D) CO morphology as R and B+R morphologies. (2011) reveal a disrupted nuclear disc and a molecular outflow, both It also appears that Virgo cluster galaxies are slightly more of which are unresolved here. In addition, if only the peak of a spi- likely to have R and B+R structures than field galaxies, with ral structure were detected, and convolved with a large beam, it 45 15% (5/11) of Virgo galaxies classified as either R or B+R, as could well be classified as a disc. In fact, as much as half of BIMA ± opposed to 17 7% (5/29) for field galaxies. Paper X has shown SONG spirals (Helfer et al. 2003) would be classified as D if they that the molecular± gas in ETGs is preferentially kinematically- were located at the average distance of the ATLAS3D sample, with aligned with the stars in Virgo galaxies, so it is perhaps not surpris- similar noise properties and beam sizes (see Paper XIV for a full ing to find relatively more bars and rings there, where the gas has discussion of properly redshifting the BIMA SONG data to match been under the influence of secular processes without external gas ATLAS3D). However, even assuming that half of the current CO- interference for some time. This may also point to these morpholo- rich ETGs classified as D actually harbour spatially-unresolved spi- gies being long-lived, as opposed to the M and X morphologies rals, the spiral fraction of ATLAS3D galaxies would be 30 7%, discussed above. It is also quite possible that the slightly higher de- still much lower than the spiral fraction of BIMA SONG galaxi± es tection rate of R and B+R structures in Virgo with respect to the (62 10%). field galaxies is due to a spatial resolution effect, as Virgo galax- ±While obtaining higher resolution molecular gas maps is the ies are closer on average (D 16.5 Mpc; Mei et al. 2007) than only rigorous way to directly break the S/D degeneracy, we use here ≈ the field galaxies in the sample (D 28 Mpc). If we redshift the the unsharp-masked dust images as proxies. As mentioned in 4.1, Virgo galaxies to the average distance≈ of field galaxies, the detec- the molecular gas morphology follows the dust morphology fa§ith- tion rate of R and B+R structures drops from 45 to 18% and is then fully in the majority of cases. The unsharp-masked images there- statistically consistent with the field rate (NGC 4119, NGC 4435 fore may be utilized to provide the higher spatial resolution and and NGC 4477 become unresolved). Higher resolution and deeper sensitivity required to separate the S and D classifications. The dust imaging is required to determine whether the higher rate in Virgo comparison indicates that in the majority of cases (with the possible is truly a resolution effect or an intrinsic property. exceptions of NGC 3619, NGC 3626 and NGC 3665), and contrary to LTGs, a disc morphology without distinct spiral arms is indeed the most common morphology for the molecular gas in ETGs. 4.2.3 Molecular discs and spirals Smooth molecular discs make up the largest fraction of the CO 4.2.4 Summary of the gas morphologies morphologies that are seen in the CO-imaged ATLAS3D galaxies, while spirals make up the smallest fraction. This relative dearth Table 5 lists the total number of ATLAS3D ETGs within each CO of discrete spirals as compared to smooth discs seems to indicate morphological class. Overall, it thus appears that the CO in ETGs that there is something fundamentally different about the way in is most likely to be in a settled morphology, either in regular discs which molecular gas behaves within an ETG as opposed to a LTG. (comprising 50% of the galaxies) or ring, bar+ring and spiral mor- A caveat to this scenario is that galaxies with dominant molecular phologies (comprising another 30% of the sample). This means that gas spirals (and associated star formation) would likely be classi- the majority (80%) of ETGs have a dynamically settled molecu- fied as LTGs, and thus be excluded from the sample. lar gas morphology. The dynamically unsettled (M and X) systems It is possible that molecular gas in ETGs remains in a smooth comprise the remaining 20%, and just over half of those are only distribution and lacks distinct spiral arms for dynamical reasons. mildly disrupted. Of course, the CO structures observed here are For example, the steep potential wells in the central parts of ETGs rather compact spatially, with an average extent of only 1 kpc (Pa- (where the molecular gas resides) yield high epicyclic frequencies, per XIV), and have correspondingly small dynamical timescales

c 2012 RAS, MNRAS 000, 1–52 14 K. Alatalo and the ATLAS3D team

Asymmetric H I spectra generally trace lopsided spatial distri- butions, and lopsided molecular gas discs are likely a result of the molecular gas responding to a change in the gravitational poten- tial. In particular, long-lived lopsided H I discs are well reproduced in models where the gas is off-centre with respect to the galactic halo (e.g. Levine & Sparke 1998). Other possible causes for lop- sidedness include responding to an interaction (e.g. Jog & Combes 2009), or possibly an internal instability that perturbs both the m = 1 (lopsided) and m = 2 (barred) modes (Masset & Tagger 1997; Bournaud et al. 2005; Jog & Combes 2009). In the strongest case of asymmetry (IC 1024), it is likely that the molecular gas disc is responding to a tidal interaction, which is also seen in the optical data (Paper II). IC 1024, despite being lopsided, is dynami- cally relaxed (Paper XIV) and shows regular kinematics and a CO disc morphology in the moment0 map. This may suggest that the tidal interaction happened sufficiently long ago for any detectable morphological and kinematic disturbance of the molecular gas to subside, while preserving the spectral asymmetry. In the context of H I, the structures are well resolved, ex- tended, and clearly “lopsided”, and the H I cloud size is small 3D Figure 5. Color-magnitude diagram of the CO-imaged ATLAS galaxies, compared to the global structure, and thus inferences can be made sorted based on the CO morphological classifications. The contours (black) in most cases that the driver of the asymmetries are global, on a are from the SDSS Data Release 8 (DR8; Aihara et al. 2011), and repre- long timescale. Structures traced by the CO distributions are much sent all galaxies with redshift z > 0.08. Data for the ATLAS3D ETGs less extended compared to the rest of the galaxy (Paper XIV), and are either from the SDSS DR8 u, r and Mr catalog products or the INT (NGC 524, NGC 3489 and NGC 7465; Paper XXI). Colour information is thus the interpretation of CO asymmetries is less straightforward. A unavailable for NGC 1222 and NGC 1266 due to poor u-band photometry, more comprehensive study of asymmetries and lopsidedness in CO for PGC 058114 because of the presence of a bright star less than a degree distributions within galaxies would likely address these issues, as from the galaxy, and for NGC 4710 due to erroneous SDSS photometry. well as uncover many other yet unstudied properties of molecular gas distributions in galaxies, but is beyond the scope of this paper.

(107 108 yrs). The CO distributions are thus expected to relax and reach− equilibrium rapidly. Figure 5 shows the u r vs. Mr color-magnitude diagram 4.4 Mass of externally-acquired molecular gas in ETGs − 3D (CMD) of the CO-imaged ATLAS sample, from SDSS and INT Paper X discusses the origins of the molecular gas in ETGs, and data, overlaid upon the SDSS Data Release 8 distribution of all identifies galaxies that likely have externally-acquired gas. Using galaxies with redshift z > 0.08 (Aihara et al. 2011). There is no the criteria set forth in Paper X, that the kinematic major axis of clear separation of the morphological groups, although some trends the ionized gas must be misaligned with the kinematic major axis do appear. The brightest objects (Mr < 21) tend to be classified ◦ 3D − of the stars by at least 30 , at least thirteen CO-imaged ATLAS as D galaxies, with the exception of NGC 4753, which was dis- galaxies are identified as having externally-acquired gas: IC 719, cussed in 4.2.1. The CO discs in these massive galaxies are also § NGC 1266, NGC 2685, NGC 2768, NGC 3032, NGC 3626, generally well-resolved, limiting the chance that these objects are NGC 4694, NGC 5173, NGC 7465, PGC 029321, PGC 058114 and poorly resolved rings or spirals. It also appears that although B+R UGC 09519. NGC 3619 is classified as M in this work, exhibiting galaxies can be found throughout the CMD, galaxies classified as an unsettled CO morphology, but the origin of the CO is difficult to R only seem to cluster on the red sequence, perhaps indicating a determine, with a kinematic misalignment angle of only 24 3◦, later evolutionary stage. right at the boundary of being classified as external (Paper± X), and the galaxy contains a kinematically-misaligned H I disc (Paper XIII). Although it is possible that the CO indeed has an external 4.3 CO spectral asymmetries origin, there is no conclusive measurement to classify it as such, It is worth mentioning that a fraction of the CO spectra exhibit and NGC 3619 will not be considered as having external CO in the asymmetries, and have representatives in many CO morphologi- following discussion. The CO of NGC 4150 is included here as be- cal classes (as opposed to solely M and X-class objects). Although ing external in origin, as studies show that its gas-phase metallicity asymmetries detected from a single-dish spectrum could be due to is sub-Solar, and thus is very likely from the accretion of a gas-rich a slightly offset pointing, interferometric identifications of spec- companion in a minor merger (Crockett et al. 2011). NGC 4753 is tral asymmetries are more robust. Asymmetric spectra have long classified as M in this work, and Steiman-Cameron et al. (1992) been known within H I discs (Baldwin et al. 1980). Within the make a compelling argument that the molecular disc is unsettled, Westerbork H I sample of Spiral and Irregular Galaxies (WHISP) and must come from an external source. For this reason, we in- at least 80% of all galaxies contain some amount of asymmetry clude here NGC 4753 in the category of gas acquired externally. (van Eymeren et al. 2011). In fact, asymmetries are found at small The disrupted stellar and gas kinematics of NGC 1222 (CO class radii in at least 60% of H I discs from the WHISP survey. Despite X), which is currently undergoing a strong three-way interaction the different dynamical timescales at the radii where the CO has (Beck et al. 2007), also suggest that the molecular gas is likely to been found, finding a few asymmetric objects within the CARMA be of external origin. Including these three additions, 15 (38%) of ATLAS3D sample is unsurprising. the 40 gas-rich CARMA ETGs contain external gas, in good agree-

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 15 ment with the fraction of externally-acquired gas estimated in Paper 5 CONCLUSIONS X (36%). We have presented millimeter-wave data products as part of the CARMA ATLAS3D survey of galaxies, an imaging survey of the The fact that the majority of galaxies with unsettled gas mor- CO J = 1–0 emission of 30 nearby CO-rich ETGs, part of the phologies are identified as having an external gas origin is un- ATLAS3D survey. The main conclusions drawn from these data are: surprising, as a parcel of gas falling into a galaxy takes time to virialise, which is not the case for internal gas (stellar mass loss). 1. The CO-imaged ATLAS3D survey is the largest CO imag- The rest of the galaxies with external gas have disc morphologies ing survey of ETGs to date, and provides the most detailed view of (IC 719, NGC 3032, NGC 3626, PGC 029321 and PGC 058114), the nature of molecular gas in ETGs. represented at about the same rate as in the sample as a whole. 2. The molecular gas found in ETGs appears to be co-spatial NGC 2685 and NGC 2768 are both known polar rings/discs, with dust features (as traced by g r colour images), though the and are discussed in detail in Schinnerer & Scoville (2002) and dust features often appear to be more− extended, likely because we Crocker et al. (2008), respectively. are unable to trace small molecular gas surface densities. 3. The molecular gas present in ETGs comes in a variety of We use the H masses from CARMA, where available, and 2 morphologies: 50% of the objects have their CO in inclined gas find that the sum of the molecular gas masses in the 15 sources with 9 20 discs or is poorly resolved structures (D), 5% show spiral arms external CO is 8.26 10 M⊙, assuming XCO = 3 10 (K km −1 −1 −2 × × or spiral structure (S), 15% have resolved rings (R), 10% have s ) cm (Dickman, Snell & Schloerb 1986), and accounts for bar+ring systems (B+R), 12.5% have mildly disrupted distributions 44% of the total molecular gas mass in our sample of 40 CO-rich (M) and 7.5% have strongly disrupted distributions (X). galaxies with interferometric maps. There is reasonable agreement 4. The CO morphology does not show a strong correlation between the external number (38%) and mass (44%) fractions. We with the u r color or total magnitude of the galaxy, although there note that these fractions are lower limits, due to the fact that we appear to be− weak trends. For example, the most massive galaxies can only unambiguously assign galaxies with misaligned stellar in this sample tend to have D CO morphologies, and R morpholo- and gas kinematics as external accretors, while some fraction of gies tend to lie on the red sequence whereas B+R morphologies aligned galaxies are also likely to be so. tend to also be present in the blue cloud. 9 5. We currently observe a total of 8.26 10 M⊙ of molecular Galaxies that were originally detected in molecular gas (Paper gas that is likely of external origin in 15/40× of our galaxies. Using IV) but were not mapped interferometrically have a higher rate of the correction factor derived in Kaviraj et al. (2012), we estimate ionised gas kinematically-aligned with the stars, compared to those that the total externally acquired molecular gas prior to the con- actually mapped here (i.e. brighter CO; see Paper X). This likely 10 sumption of some of it by star formation was 2.48 10 M⊙. means that the un-imaged CO-detected ETGs contribute negligibly In conjunction with the minor merger rate of Lotz≈ et al.× (2008) and (< %) to the total external molecular gas mass. It is also likely 6 assumptions about gas mass fractions, this amount of externally ac- that undetected galaxies do not contribute significantly to the total 9 creted molecular gas is consistent with a minor merger origin. gas mass, with an upper limit to the contribution of M , 3D 3 10 6. The CARMA ATLAS (as well as 9 additional literature assuming that 42.5% upper limits in undetected field≈ galaxie× s are⊙ galaxy) data products including data cubes and moment0 and mo- due to an external phenomenon (Paper X). ment1 maps in FITS format, will be publicly released and hosted through the CARMA data archive5 and will be reachable from our Assuming the molecular gas is depleted through star for- project website6. mation and reasonable gas depletion timescales ( 1 Gyr; Saintonge et al. 2011) and star formation histories (allowi≈ ng us to adopt the mean current-to-initial molecular gas mass correc- tion factor calculated by Kaviraj et al. 2012 for ETGs with promi- ACKNOWLEDGMENTS nent dust lanes), we can infer the amount of molecular gas each galaxy acquired before star formation activity consumed some of We thank the anonymous referee for insightful comments and sug- the molecular gas. The total amount of molecular gas originally gestions. K.A. thanks C. Heiles, K. Nyland, G. Graves, R. Plam- acquired externally within the ATLAS3D sample is then approxi- beck, E. Rosolowsky and J. Carpenter for useful conversations. 10 mately 2.48 10 M⊙. At the rate of 30 minor mergers in the K.A. also wants to thank Lisa Wei in particular for collabora- sample detailed× in 1 and from the rate of Lotz et al. (2008), this tion on NGC 5173. The research of K. Alatalo is supported by § 8 would mean approximately 8.3 10 M⊙ of H2 per minor merger the NSF grants AST-0838258 and AST-0908572. The research per molecular gas depletion time× (1 Gyr; Saintonge et al. 2011). We of K. Alatalo is also supported by NASA grant HST-GO-12526. derive an average stellar mass ratio for these minor mergers by first MC acknowledges support from a STFC Advanced Fellowship converting the molecular gas mass to an atomic mass using the 1:3 (PP/D005574/1) and a Royal Society University Research Fellow- H2-to-H I ratio seen in the Milky Way (Wolfire et al. 2003). We ship. PS is a NWO/Veni fellow. RMcD is supported by the Gem- then use the average H I-to-stellar mass fraction of minor merger ini Observatory, which is operated by the Association of Universi- companions from Kannappan (2004) of 20% to calculate the av- ties for Research in Astronomy, Inc., on behalf of the international 10 erage stellar mass of the accreted companions, 1.25 10 M⊙. Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, For the mass of the accreting galaxy, we take the average× stellar the United Kingdom, and the United States of America. RLD and mass of the non-Virgo ETGs in the CO-imaged ATLAS3D sample, MB are supported by the rolling grants ‘Astrophysics at Oxford’ 10 6.5 10 M⊙. This results in a merger stellar mass ratio of 1:5.2,≈ consistent× with the minor merger stellar mass ratios we ex- pect. We therefore conclude that our results are in good agreement 5 http://carma-server.ncsa.uiuc.edu:8181/ with the origin of the external gas being due to minor mergers. 6 http://purl.org/atlas3d

c 2012 RAS, MNRAS 000, 1–52 16 K. Alatalo and the ATLAS3D team

PP/E001114/1 and ST/H002456/1 from the UK Research Coun- Duc, P.-A. et al., 2011, MNRAS, 417, 863; Paper IX cils. RLD acknowledges travel and computer grants from Christ Faber, S. M., Gallagher, J. S., 1976, ApJ, 204, 365 Church, Oxford and support from the Royal Society in the form of Faber, S. M. et al., 2007, ApJ, 665, 265 a Wolfson Merit Award 502011.K502/jd. TN acknowledges sup- Giovanelli, R. et al., 2005, AJ, 130, 2598 port from the DFG Cluster of Excellence: ”Origin and Structure Harker, J. J., Schiavon, R. P., Weiner, B. J. Faber, S. M., 2006, of the Universe.” Support for CARMA construction was derived ApJL, 647, L103 from the states of California, Illinois, and Maryland, the James S. Hawarden, T. G. et al., 1981, MNRAS, 196, 747 McDonnell Foundation, the Gordon and Betty Moore Foundation, Helfer, T. T. et al., 2003, ApJS, 145, 259 the Kenneth T. and Eileen L. Norris Foundation, the University of Hubble, E., 1926, ApJ, 64, 321 Chicago, the Associates of the California Institute of Technology, Jeong, H. et al., 2009, MNRAS, 398, 2028 and the National Science Foundation. Ongoing CARMA develop- Jura, M., 1986, ApJ, 306, 483 ment and operations are supported by the National Science Foun- Jog, C. J., Combes, F. 2009, Physics Reports, 471, 75 dation under a cooperative agreement, and by the CARMA partner Kannappan, S. J., 2004, ApJL, 611, 89 universities. This paper is partly based on observations carried out Kaviraj, S., et al. 2012, MNRAS, 423, 49 with the IRAM 30m telescope. IRAM is supported by INSU/CNRS Kennicutt, R. C., 1998, ApJ, 498, 541 (France), MPG (Germany) and ING (Spain). We acknowledge use Kennicutt, R. C. et al. 2003 PASP, 115, 928 of the HYPERLEDA database (http://leda.univ-lyon1.fr) and the Knapp, G. R., Turner, E. L., Cunniffe, P. E., 1985, AJ, 90, 3 NASA/IPAC Extragalactic Database (NED) which is operated by Knapp, G. R., Guhathukarta, P., Kim, D.-W., Jura, M., 1989, the Jet Propulsion Laboratory, California Institute of Technology, ApJS, 70, 329 under contract with the National Aeronautics and Space Adminis- Krajnovi´c, D. et al., 2011, MNRAS, 414, 2923 tration. Kuijken K., Merrifield M. R., 1995, ApJ, 443, L13 Lauer, T. R. et al. 2005, AJ, 129, 2138 Lees, J. F., Knapp, G. R., Rupen, M. P., Phillips, T. G. 1991, ApJ, REFERENCES 379, 177 Levine, S. E., Sparke, L. S. 1998, ApJL, 496, 13 Aihara H., Allende Prieto C., An D., et al., 2011, ApJS, 193, 29 Li, J. J., Seaquist, E. R., 1994, AJ, 107, 1953 Alatalo, K. et al., 2011, ApJ, 735, 88 Lotz, J. M. et al., 2008, ApJ, 672, 177 Athanassoula, E., 2005, MNRAS, 358, 1477 Lotz J. M. et al., 2011, ApJL, 742, 103 Athanassoula, E., Bureau, M., 1999, ApJ, 522, 699 Martig, M., Bournaud, F., Teyssier, R., Dekel, A., 2009, ApJ, 707, Baldry, I. K. et al., 2004, ApJ, 600, 681 250 Baldwin, J. E., Lynden-Bell, D., Sancisi, R. 1980, MNRAS, 193, Masset, F, Tagger, M. 1997, A&A, 322, 442 313 Mei, S. et al. 2007, ApJ, 655, 144 Bauermeister, A., et al. 2012, CARMA Memo, No. 59 Merrifield M. R., Kuijken K., 1999, A&A, 345, L47 (http://www.mmarray.org/memos/carma memo59.pdf) Morganti, R. et al., 2006, MNRAS, 371, 157 Beck, S. C., Turner, J. L., Kloosterman, J., 2007, AJ, 134, 1237 Oosterloo, T. et al., 2010, MNRAS, 409, 500 Bigiel, F. et al., 2008, AJ, 136, 2846 B¨ohringer, H. et al., 1994, Nature, 368, 828 Sage, L. J., Wrobel, J. M., 1989, ApJ, 344, 204 Bournaud, F., Combes, F., 2002, A&A, 392, 83 Sage, L. J., Galletta, G., 1993, ApJ, 419, 544 Bournaud, F., Combes, F., Jog, C. J., Puerari, I., 2005, A&A, 438, Sage, L. J., Welch, G. A., 2006, ApJ, 644, 850 507 Sage, L. J., Welch, G. A., Young, L. M., 2007, ApJ, 657, 232 Bower, R. G., Lucey, J. J., Ellis, R. S., 1991, MNRAS, 254, 601 Saintonge, A. et al. 2011, MNRAS, 415, 61 Bureau M., Athanassoula E., 1999, ApJ, 522, 686 Sault, R. J., Teuben, P. J., Wright, M. C. H., 1995, ASPC, 77, 433 Bureau M., Freeman K. C., 1999, AJ, 118, 126 Schinnerer, E., Scoville, N., 2002, ApJL, 577, 103 Buta, R., Combes, F., 1996, FCPh, 17, 95 Sellwood J. A., Wilkinson A., 1993, Reports Prog. Phys., 56, 173 Cappellari, M. et al., 2011a, MNRAS, 413, 813; Paper I Serra, P., et al., 2012, MNRAS, 422, 1835; Paper XIII Cappellari, M. et al., 2011b, MNRAS, 416, 1680; Paper VII Shapiro, K. L. et al., 2010, MNRAS, 402, 2140 Cayatte, V., van Gorkom, J. H., Balkowski, C., Kotanyi, C., 1990, Sheth, K. et al. 2002, AJ, 124, 2581 AJ, 100, 604 Springel, V., Di Matteo, T., Hernquist, L., 2005, MNRAS, 361, Ciotti, L., D’Ercole, A., Pellegrini, S., Renzini, A., 1991, ApJ, 776 376, 380 Steiman-Cameron, T. Y., Kormendy, J., Durisen, R. H., 1992, AJ, Combes, F., Young, L. M., Bureau, M., 2007, MNRAS, 377, 1795 104, 4 Crocker, A. C., Bureau, M., Young, L. M., Combes, F., 2008, MN- Tonry, J. L. et al. 2001, ApJ, 546, 681 RAS, 368, 1811 Toomre, A., Toomre, J., 1972, ApJ, 178, 623 Crocker, A. C. et al., 2009, MNRAS, 393, 1255 Toomre, A. 1981, in The Structure and Evolution of Normal Crocker, A. C. et al., 2011, MNRAS, 410, 1197 Galaxies, ed. S. M. Fall & D. Lynden-Bell (Cambridge : Cam- Crocker, A. C. et al., 2012, MNRAS, 421, 1298; Paper XI bridge Univ. Press), 111 Crockett, R. M. et al., 2011, ApJ, 727, 115 Tran, H. D. et al., 2001, AJ, 191, 2928 Davis, T. A. et al., 2011a, MNRAS, 414, 968; Paper V van Eymeren, J., J¨utte, E., Jog, C. J., Stein, Y., Dettmar, R.-J. Davis, T. A. et al., 2011b, MNRAS, 417, 882; Paper X 2011, A&A, 530, 29 Dickman, R. L., Snell, R. L., Schloerb, F. P. 1986, ApJ, 309, 326 Visvanathan, N., Sandage, A., 1977, ApJ, 216, 214 Duc, P.-A., Braine, J., Lisenfeld, U., Brinks, E., Boquien, M., Wei, L. H., Vogel, S. N., Kannappan, S. J., Baker, A. J., Stark, 2007, A&A, 475, 187 D. V., Laine, S., 2010, ApJL, 725, 62

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 17

Wei, L. H., Kannappan, S. J., Vogel, S. N., Baker, A. J., 2010, ApJ, 708, 841 Welch, G. A., Sage, L. J., 2003, ApJ, 584, 260 Welch, G. A., Sage, L. J., Young, L. M., 2010, ApJ, 735, 100 Wolfire, M. G., McKee, C. F., Hollenbach, D., Tielens, A. G. G. M., 2003, ApJ, 587, 278 Wrobel, J. M., Kenney, J. D. P. 1992, ApJ, 399, 94 Young, L. M., 2002, AJ, 124, 788 Young, L. M., 2005, ApJ, 258, 271 Young, L. M., Bureau, M., Cappellari, M., 2008, ApJ, 676, 317 Young, L. M., Bendo, G. J., Lucero, D. M., 2009, AJ, 137, 3053 Young, L. M. et al., 2011, MNRAS, 414, 940; Paper IV

c 2012 RAS, MNRAS 000, 1–52 18 K. Alatalo and the ATLAS3D team

APPENDIX A: CO CARMA DATA OF ATLAS3D GALAXIES For each galaxy of the CARMA ATLAS3D sample, we provide six figures:

Top-left: r-band image (grayscale) either from SDSS or from the INT, overlaid with black contours. The CO integrated intensity (moment0) map is also overlaid (cyan contours corresponding to 20, 40, 60, 80 and 100% of the peak). The cyan box corresponds to the size of the individual moment maps in the middle-left and middle-centre panels.

Top-right: Comparison of the single-dish IRAM 30m CO(1–0) integrated flux (black) and the CARMA integrated flux (red). The total integrated CARMA flux is obtained by summing all flux above a given threshold (see 3.3). The grey dashed vertical lines indicate the total spectral range of CARMA. Both heliocentric velocities and velocities with respect to§ systemic (taken from Paper I) are indicated. The rms noise is shown as a single error bar in black for the IRAM 30m and red for CARMA.

Middle-left: CO(1–0) integrated intensity (moment0) map (colorscale), overlaid with black and grey contours (at equal increments of 20% of the peak). The colour table on the right provides the integrated flux scale. The dot-dashed gray circle corresponds to the 21′′. 6 primary beam of the IRAM 30m telescope. The CARMA synthesized beam is shown in the bottom-right corner (black ellipse).

Middle-center: CO(1–0) mean velocity (moment1) map (colorscale and black contours at 20 km s−1 intervals unless otherwise stated). The colour table on the right provides the velocity scale with respect to the systemic velocity (taken from Paper I and indicated in the top-left corner of the panel). The dot-dashed gray circle corresponds to the 21′′. 6 primary beam of the IRAM 30m telescope. The CARMA synthesized beam is shown in the bottom-right corner (black ellipse).

Middle-right: CO(1–0) position-velocity diagram (PVD) taken over a one synthesized beam width (5 pixels) slice at the position angle indicated in the top-right corner inset and at the bottom of the panel (see 3.3). Velocities are heliocentric. The synthesized beam along the § PV slice direction is indicated in the bottom-right corner. Contours are spaced by 1σ starting at 3σ (unless otherwise stated), where σ is the rms noise in an individual channel multiplied by √5, to account for the summation over the synthesized beam width.

Bottom: CO(1–0) channel maps. The panels for velocity channels with flux are color-coded based on their velocity with respect to systemic (taken from Paper I). The mean velocity offset is listed in the top-left corner of each panel. The cross indicates a fixed reference position in all panels. Contours are spaced by 1σ beginning at 2σ (unless otherwise stated), where 1σ is the rms noise in an individual channel. Grey contours are negative. The CARMA synthesized beam± is shown in the lower-right corner of the first panel (black ellipse).

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 19

1200 1300 1400 1500 1600 1700 IC 676 04′ 00″ 0.8

0.6 ″ 30 0.4

0.2 Flux (Jy) 03′ 00″ 0.0

-0.2 09° 02′ 30″ -300 -200 -100 0 100 200 -1 11h 12m 43 s 41s 39s 37s Velocity (km s )

129 -1 51 1.6 vsys = 1429 km s 1500 ) )

107 -1 31 -1 1.1 )

″ ″ -1 30 86 30 11 1450 0.72

64 -9 0.30 (K) B v (K km s T ∆ ″ ″ 20 20 1400 -0.13 43 mb -29 Velocity (km s T Velocity (km s 21 -49 -0.56

09° 03′ 10″ 09° 03′ 10″ 1350 beam = 3.7″ 0 -69 -0.98 h m s s s h m s s s 0 5 10 15 20 25 11 12 40.8 40.4 40.0 11 12 40.8 40.4 40.0 Offset (arcsec), p.a. = 16.5°

-84 -74 -64 -54 -44 30″

20″

09° 03′ 10″

-34 -24 -14 -4 6

16 26 36 46 56

11h 12m 40.8 s 40.4s 40.0s

Figure A1. IC 676 is a field regular rotator (MK = -22.27) with a bar and ring stellar morphology. It has a dust filament. The moment0 peak is 17 Jy beam−1 km s−1. The moment1 contours are placed at 10km s−1 intervals and the PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 20 K. Alatalo and the ATLAS3D team

IC 719 1600 1800 2000 2200 ′ ″ 01 00 0.15

0.10 ″ 40 0.05

Flux (Jy) 0.00 20″ -0.05 -0.10 09° 00′ 00″ -200 0 200 400 -1 11h 40m 20.5s 19.5s Velocity (km s )

22 v = 1833 km s-1 187 0.29 50″ 50″ sys 2000 18 120 0.20 ) ) -1

-1 ) 15 54 -1 1900 0.11 40″ 40″

0.021 (K) 11 -13 1800 B T v (K km s ∆ 30″ 7 30″ -80 -0.070 Velocity (km s

mb 1700 Velocity (km s 4 T -146 -0.16

° ′ ″ ° ′ ″ beam = 3.0″ 09 00 20 0 09 00 20 -213 1600 -0.25 h m s s s h m s s s 0 5 10 15 20 25 30 11 40 19.6 19.2 18.8 11 40 19.6 19.2 18.8 Offset (arcsec), p.a. = 229.°

50″ -263 -243 -223 -203 -183 -163 -143

40″

30″

09° 00′ 20″ -123 -103 -83 -63 -43 -23 -3

17 37 57 77 97 117 137

157 177 197 217 237

11h 40m 19.6 s 19.2s 18.8s

Figure A2. IC 719 is a field 2σ non-regular rotator (MK = -22.70) with normal stellar morphology. It contains a dusty disc. The 2σ peak is the signature of two counter-rotating stellar discs with opposite angular momenta. The molecular gas is co-rotating with a kinematically decoupled core, and counter-rotating with respect to the dominant stellar component. The moment0 peak is 2.6 Jy beam−1 km s−1. The moment1 contours are placed at 25km s−1 intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 21

IC 1024 1100 1200 1300 1400 1500 1600 1700 01′ 00″ 0.6

40″ 0.4

0.2 Flux (Jy) 20″ 0.0

03° 00′ 00″ -300 -200 -100 0 100 200 -1 14h 31m 29.5s 28.5s Velocity (km s )

1600 1.4 94 v = 1479 km s-1 86 sys 1.1 78 1550 ) 51 ) ) -1 -1 ″ -1 40 40″ 0.75 61 16 1500

0.43 (K) 45 B -19 1450 T

30″ v (K km s 30″

∆ 0.11 29

-54 Velocity (km s mb 1400 T 12 -89 Velocity (km s -0.21 ° ′ ″ ° ′ ″ 03 00 20 03 00 20 1350 beam = 3.9″ -4 -124 -0.53 h m s s h m s s 0 5 10 15 20 25 14 31 28.2 27.8 14 31 28.2 27.8 ° Offset (arcsec), p.a. = 24.5

-139 -129 -119 -109 -99 -89 -79 40″

30″

03° 00′ 20″

-69 -59 -49 -39 -29 -19 -9

1 11 21 31 41 51 61

71 81 91 101 111 121

14h 31m 28.2s 27.8s

Figure A3. IC 1024 is a field regular rotator (MK = -21.85) with stellar morphology that shows interaction features as well as a dust filament. The moment0 peak is 14 Jy beam−1 km s−1. The channel map and PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 22 K. Alatalo and the ATLAS3D team

2200 2300 2400 2500 2600 2700 NGC 1222 00″ 1.0

0.8 10″ 0.6 20″ 0.4 Flux (Jy) 0.2 30″ 0.0

-02° 57′ 40″ -200 -100 0 100 200 300 -1 03h 08m 58.0 s 57.0s 56.0s Velocity (km s )

139 2500 1.8 v = 2422 km s-1 55 sys 115 26 1.3 ) ) 2450 -1 -1 10″ 10″ ) 91 -3 -1 0.90 2400

0.46 (K)

67 -33 B ″ ″ T 20 v (K km s 20

∆ 2350 43 -62 0.019 Velocity (km s

mb Velocity (km s T 19 -91 2300 -0.42 ° ′ ″ ° ′ ″ -02 57 30 -02 57 30 ″ -5 -120 beam = 3.5 -0.86 h m s s h m s s 0 5 10 15 03 08 57.8 57.4 ° 03 08 57.8 57.4 Offset (arcsec), p.a. = 33.0

-133 -128 -123 -118 -113 -108 -103 -98 -93

10″

20″

-02° 57′ 30″

-88 -83 -78 -73 -68 -63 -58 -53 -48

-43 -38 -33 -28 -23 -18 -13 -8 -3

2 7 12 17 22 27 32 37 42

47 52 57 62 67 72 77

03h 08m 57.8 s57.4s

Figure A4. NGC 1222 is a field non-regular rotator (MK = -22.71) with stellar morphology that shows interaction features as well as dust filaments. It is a well-known interaction, and cross-identified as Markarian 603 (Beck et al. 2007). The moment0 peak is 18 Jy beam−1 km s−1. The PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 23

1900 2000 2100 2200 2300 2400 2500 NGC 1266 1.4 ″ 00 1.2 1.0

25′ 30″ 0.8 0.6

Flux (Jy) 0.4 00″ 0.2

0.0 -02° 26′ 30″ -200 -100 0 100 200 300 -1 03h 16m 04s 02s 00s Velocity (km s )

4.1 687 -1 85 v = 2160 km s sys 2300 30″ 573 30″ 55 3.3 ) ) 2250 -1 -1 ) -1 34″ 458 34″ 25 2200 2.5

38″ 38″ 2150 1.8 (K) 344 -5 B T v (K km s 2100 42″ ∆ 42″ 1.0 229 -35 Velocity (km s

mb 2050 Velocity (km s ″ T ″ 46 115 46 -65 0.24

2000 beam = 3.3″ -02° 25′ 50″ 0 -02° 25′ 50″ -95 -0.53 h m s s s s h m s s s s 0 5 10 15 20 03 16 1.4 1.0 0.6 0.2 03 16 1.4 1.0 0.6 0.2 Offset (arcsec), p.a. = 270.°

-180 -170 -160 -150 -140 -130 -120 -110 32″

38″

44″

-02° 25′ 50″

-100 -90 -80 -70 -60 -50 -40 -30

-20 -10 0 10 20 30 40 50

60 70 80 90 100 110 120 130

03h 16m 1.4 s 0.8s 0.2s

Figure A5. NGC 1266 is a field regular rotator (MK = -22.93) with normal stellar morphology. It is also observed to have a dust filament. Not only was it the brightest detection in the sample, but it had the largest linewidths observed. It was initially unresolved in CARMA D-array, thus was observed in the much higher resolution arrays. NGC 1266 hosts a massive molecular outflow that appears to be driven by an AGN. Further details can be found in Alatalo et al. 2011. The moment0 peak is 100 Jy beam−1. The moment1 contours are placed at 10km s−1 intervals. The channel map contours are placed at 2σ intervals and the PVD contours are placed at 3σ intervals.

c 2012 RAS, MNRAS 000, 1–52 24 K. Alatalo and the ATLAS3D team

2400 2500 2600 2700 2800 2900 3000 NGC 2764

0.4 50″ 0.3

0.2

30″ Flux (Jy) 0.1

0.0

-0.1 21° 26′ 10″ -300 -200 -100 0 100 200 300 -1 09h 08m 19.5s 18.5s Velocity (km s )

163 0.91 -1 128 vsys = 2706 km s 133 0.67 ) 80

) 2800 -1 -1 ″ ″ ) 45 45 -1 104 32 0.43

2700 ″ 74 0.19 (K) 35 35″ -16 B T v (K km s

∆ 45 -65 -0.048 Velocity (km s 25″ mb 25″ 2600 T Velocity (km s -0.29 15 -113 beam = 3.5″ 21° 26′ 15″ -14 21° 26′ 15″ -161 -0.53 h m s s h m s s 0 10 20 30 40 50 09 08 19.0 17.0 ° 09 08 19.0 17.0 Offset (arcsec), p.a. = 203.

-171 -161 -151 -141 -131 -121 -111 -101 45″

35″

25″

21° 26′ 15″

-91 -81 -71 -61 -51 -41 -31 -21

-11 -1 9 19 29 39 49 59

69 79 89 99 109 119 129 139

09h 08m 19.0 s 17.0s

Figure A6. NGC 2764 is a field regular rotator (MK = -23.19) with stellar morphology that indicates interaction. It is also observed to contain a blue nucleus and dust filaments. The moment0 peak is 18 Jy beam−1 km s−1. The PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 25

2500 2600 2700 2800 2900 3000 30″ NGC 2824 0.15 20″ 0.10

10″ 0.05 Flux (Jy) 0.00 16′ 00″

-0.05 26° 15′ 50″ -300 -200 -100 0 100 200 -1 09h 19m 4.0 s 3.0s 2.0s 1.0s Velocity (km s )

46 -1 134 2900 0.24 vsys = 2758 km s 38 ) 77 0.17 )

-1 -1

) 2800 30 21 -1 15″ 15″ 0.096 21 -36 0.025 (K) 2700 B v (K km s T ∆ 13 -93 -0.045 mb

Velocity (km s T 5 -149 Velocity (km s 2600 26° 16′ 00″ 26° 16′ 00″ -0.12 -4 -206 beam = 4.1″ h m s s -0.19 09 19 3.0 2.0 h m s s 09 19 3.0 2.0 0 5 10 15 20 25 Offset (arcsec), p.a. = 162.°

-239 -214 -189 -164 -139 -114 20″

10″

26° 16′ 00″

-89 -64 -39 -14 11 36

61 86 111 136

09h 19m 3.0s 2.0s

−1 Figure A7. NGC 2824 is a field regular rotator (MK = -22.93) with a ring stellar morphology. It contains a dust disc. The moment0 peak is 8.6 Jy beam km s−1.

c 2012 RAS, MNRAS 000, 1–52 26 K. Alatalo and the ATLAS3D team

NGC 3182 1900 2000 2100 2200 2300 2400 50″ 0.15

0.10 30″ 0.05

12′ 10″ Flux (Jy) 0.00

-0.05 58° 11′ 50″ -300 -200 -100 0 100 200 -1 10h 19m 35s 33s Velocity (km s )

14 96 0.17 v = 2118 km s-1 12 sys 59 2200 0.12 ) ) -1 -1 ) 25″ 10 25″ 23 -1 2150 0.070

2100 0.022 (K)

7 -14 B T v (K km s

∆ 2050 15″ 5 15″ -51 -0.026 Velocity (km s mb Velocity (km s T 2000 -0.074 2 -87 beam = 4.7″ 58° 12′ 05″ 0 58° 12′ 05″ -124 1950 -0.12 h m s s s h m s s s 0 5 10 15 20 10 19 34.0 33.6 33.2 10 19 34.0 33.6 33.2 Offset (arcsec), p.a. = 332.°

-129 -99 -69 -39 -9

25″

15″

58° 12′ 05″

21 51 81 111

10h 19m 34.0s 33.6s 33.2s

Figure A8. NGC 3182 is a field regular rotator (MK = -23.19) with normal stellar morphology and contains a dust bar and ring. It is one of the faintest detections within the sample, thus it is likely much of the CO emission in this system is below the noise in the channel maps. The moment0 peak is 3.3 Jy beam−1 km s−1.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 27

400 600 800 1000 1200 1400 NGC 3607 0.25

04 0.20

0.15 0.10 03

Flux (Jy) 0.05

0.00

18° 02′ -0.05 -400 -200 0 200 400 -1 11h 17m 00s 16m 56s 52s Velocity (km s )

57 258 0.30 v = 942. km s-1 20″ 20″ sys 1200 47 161 0.24 ) ) -1 -1 ) 1100 37 65 -1 0.17 10″ 10″ 1000

0.10 (K) 27 -32 900 B

T v (K km s ∆ 03′ 00″ 17 03′ 00″ -129 800 0.033 Velocity (km s mb Velocity (km s 7 T -225 700 -0.035 ° ′ ″ ° ′ ″ beam = 5.4″ 18 02 50 -3 18 02 50 -322 600 -0.10 h m s s s h m s s s 0 10 20 30 40 11 16 55.5 54.5 53.5 11 16 55.5 54.5 53.5 Offset (arcsec), p.a. = 303.°

20″ -312 -292 -272 -252 -232 -212 -192 -172

10″

03′ 00″

18° 02′ 50″ -152 -132 -112 -92 -72 -52 -32 -12

8 28 48 68 88 108 128 148

168 188 208 228 248 268 288

11h 16m 55.5 s 53.5s

Figure A9. NGC 3607 is a field regular rotator (MK = -24.74) with normal stellar morphology. It contains a dust disc. The moment0 peak is 17 Jy beam−1 km s−1. The moment1 contours are placed at 40km s−1 intervals and the PVD contours are placed at 3σ intervals.

c 2012 RAS, MNRAS 000, 1–52 28 K. Alatalo and the ATLAS3D team

1200 1400 1600 1800 2000 NGC 3619 0.10

46′ 00″ 0.05

30″ 0.00

Flux (Jy)

45′ 00″ -0.05

57° 44′ 30″ -400 -200 0 200 400 -1 11h 19m 25s 23s 21s 19s Velocity (km s )

37 230 0.11 v = 1560 km s-1 sys 1800 40″ 31 40″ 150 0.081 ) ) -1 -1 ) 1700 -1 25 71 0.048 30″ 30″ 1600

0.015 (K) 19 -9 B 1500 T v (K km s

″ ∆ ″

-0.017 20 13 20 -88 1400 Velocity (km s mb Velocity (km s T 7 -168 1300 -0.050 ° ′ ″ ° ′ ″ 57 45 10 57 45 10 ″ 1 -247 1200 beam = 4.2 -0.083 h m s s s h m s s s 0 5 10 15 20 11 19 22.5 21.5 20.5 11 19 22.5 21.5 20.5 Offset (arcsec), p.a. = 74.5°

40″ -260 -220 -180 -140 -100 -60 -20

25″

57° 45′ 10″

20 60 100 140 180 220 260

300 340 380 420

11h 19m 22.5 s 20.5s

Figure A10. NGC 3619 is a field regular rotator (MK = -23.57) with a shell stellar morphology. It contains dust filaments, bars and rings. It is very likely that CARMA has resolved out what is possibly an extended gas disc. Observations that are sensitive to larger size scales is required to confirm this. The moment0 peak is 6.9 Jy beam−1 km s−1. The moment1 contours are placed at 40km s−1 intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 29

NGC 3626 1200 1300 1400 1500 1600 1700 1800 0.25

0.20

22 0.15

0.10 0.05 21 Flux (Jy) 0.00

-0.05 18° 20′ -200 -100 0 100 200 300 -1 11h 20m 10s 06s 02s Velocity (km s )

0.28 27 v = 1486 km s-1 167 sys 23 108 0.21 ) ″ ″ ) 35 -1 35 1600 -1 ) 18 49 -1 0.14 ″ ″ 1500

25 25 0.064 (K)

14 -10 B T

v (K km s ∆

-0.0082 9 -69 1400 15″ 15″ Velocity (km s mb Velocity (km s 5 T -128 -0.080

1300 ″ 18° 21′ 05″ 0 18° 21′ 05″ -187 beam = 3.8 -0.15 h m s s s h m s s s 0 10 20 30 40 11 20 5.0 4.0 3.0 11 20 5.0 4.0 3.0 Offset (arcsec), p.a. = 170.°

-200 -175 -150 -125 -100 -75 35″

20″

18° 21′ 05″ -50 -25 0 25 50 75

100 125 150 175

11h 20m 5.0 s 4.0s 3.0s

Figure A11. NGC 3626 is a group regular rotator (MK = -23.30) that includes a double maximum velocity feature, with ring stellar morphology. It contains a dust disc. Unfortunately the central velocity of the observations were offset from vsys, and due to its large linewidth, a small amount of the blueshifted spectrum was not within the 420 km s−1 CARMA window. The moment0 peak is 4.3 Jy beam−1 km s−1. The moment1 contours are placed at 30km s−1 intervals and PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 30 K. Alatalo and the ATLAS3D team

1600 1800 2000 2200 2400 2600 NGC 3665

46′ 30″ 0.2

0.1 ′ ″

45 30 Flux (Jy) 0.0

38° 44′ 30″ -400 -200 0 200 400 -1 11h 24m 48s 44s 40s Velocity (km s )

125 v = 2069 km s-1 316 2400 0.50 46′ 00″ 46′ 00″ sys 104 204 0.38 ) )

-1 -1 )

-1 2200 50″ 83 50″ 91 0.26

0.14 (K)

63 -22 B

2000 T v (K km s

″ ∆ ″ 40 42 40 -134 0.017 Velocity (km s mb Velocity (km s T 21 -247 1800 -0.10 38° 45′ 30″ 38° 45′ 30″ beam = 4.3″ 0 -359 -0.22 h m s s s h m s s s 0 5 10 15 20 25 11 24 44.8 44.4 44.0 11 24 44.8 44.4 44.0 Offset (arcsec), p.a. = 220.°

46′ 00″ -349 -339 -329 -319 -309 -299 -289 -279 -269 -259 -249 -239

50″

40″

38° 45′ 30″ -229 -219 -209 -199 -189 -179 -169 -159 -149 -139 -129 -119

-109 -99 -89 -79 -69 -59 -49 -39 -29 -19 -9 1

11 21 31 41 51 61 71 81 91 101 111 121

131 141 151 161 171 181 191 201 211 221 231 241

251 261 271 281 291 301 311 321 331

11h 24m 44.8 44.2s s

Figure A12. NGC 3665 is a group regular rotator (MK = -24.92) with normal stellar morphology. It contains a dust disc. The moment0 peak is 24 Jy beam−1 km s−1. The moment1 contours are placed at 50 km s−1 intervals and the PVD contours are placed at 2σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 31

1400 1500 1600 1700 1800 1900 NGC 4119 24 0.3

0.2 23

0.1

Flux (Jy) 22 0.0

-0.1 10° 21′ -200 -100 0 100 200 300 -1 12h 08m 16s 12s 08s 04s Velocity (km s )

36 -1 54 0.62 vsys = 1656 km s

30 32 0.46 ) ) 1700 -1 -1 ″ ″ ) 50 50 -1 24 10 0.30 1650

0.14 (K)

18 -12 B T

40″ v (K km s 40″ ∆ 12 -34 1600 -0.022 Velocity (km s mb Velocity (km s 6 T -56 -0.18 ° ′ ″ ° ′ ″ 1550 10 22 30 10 22 30 beam = 4.1″ 0 -78 -0.34 h m s s s h m s s s 0 5 10 15 20 25 12 08 10.6 10.2 9.8 12 08 10.6 10.2 9.8 Offset (arcsec), p.a. = 296.°

-96 -86 -76 -66 -56 -46 -36 50″

40″

10° 22′ 30″ -26 -16 -6 4 14 24 34

44 54 64 74

12h 08m 10.6 s 10.2s 9.8s

Figure A13. NGC 4119 is a Virgo regular rotator (MK = -22.60) with normal stellar morphology. It contains a dust disc. The moment0 peak is 8.1 Jy beam−1 km s−1. The PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 32 K. Alatalo and the ATLAS3D team

0 200 400 600 NGC 4150 0.20 40″ 0.15

20″ 0.10

0.05 24′ 00″ Flux (Jy) 0.00 40″ -0.05

30° 23′ 20″ -200 0 200 400 -1 12h 10m 37s 35s 33s Velocity (km s )

48 -1 97 400 0.28 vsys = 208. km s 40 69 0.21 ) ) -1 -1 ) 300 10″ 32 10″ 40 -1 0.13

0.056 (K) 24 12 200 B T v (K km s

′ ″ ∆ ′ ″ 24 00 16 24 00 -16 -0.019 Velocity (km s mb Velocity (km s T 100 8 -45 -0.093

beam = 4.8″ 30° 23′ 50″ 0 30° 23′ 50″ -73 -0.17 h m s s h m s s 0 5 10 15 20 25 30 12 10 34.6 34.2 12 10 34.6 34.2 Offset (arcsec), p.a. = 146.°

-178 -168 -158 -148 -138 -128 -118 -108

′ ″

24 05

30° 23′ 50″ -98 -88 -78 -68 -58 -48 -38 -28

-18 -8 2 12 22 32 42 52

62 72 82 92 102 112 122 132

142 152 162 172 182 192

12h 10m 34.6 s 34.0s

Figure A14. NGC 4150 is a Virgo regular rotator (MK = -21.65) with normal stellar morphology. The moment0 peak is 9.9 Jy beam−1 km s−1. The PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 33

1400 1500 1600 1700 1800 1900 NGC 4324 0.20 45″

0.15

15′ 15″ 0.10

0.05 45″ Flux (Jy) 0.00

-0.05 05° 14′ 15″ -300 -200 -100 0 100 200 -1 12h 23m 10s 08s 06s 04s Velocity (km s )

10 -1 150 0.20 vsys = 1665 km s ″ ″ 1800 20 8 20 89 0.15 ) ) -1 -1 ) 10″ 7 10″ 28 -1 0.097 1700

0.046 (K) ′ ″ 5 ′ ″ -32 B

15 00 15 00 T v (K km s

∆ 1600 3 -93 -0.0055 ″ ″ Velocity (km s 50 mb 50 Velocity (km s 2 T -154 -0.057 ″ 05° 14′ 40″ 05° 14′ 40″ 1500 beam = 4.5 0 -215 -0.11 h m s s h m s s 0 10 20 30 40 50 60 12 23 7.5 5.5 12 23 7.5 5.5 Offset (arcsec), p.a. = 232.°

25″ -185 -165 -145 -125 -105 -85

15′ 10″

55″

05° 14′ 40″

-65 -45 -25 -5 15 35

55 75 95 115 135 155

12h 23m 7.5 s 5.5s

Figure A15. NGC 4324 is a field regular rotator (MK = -21.61) that includes two velocity maxima. It contains a ring stellar morphology, as well as a dust disc, bar, and ring. The moment0 peak is 2.0 Jy beam−1 km s−1. The PVD contours are placed at 2σ intervals.

c 2012 RAS, MNRAS 000, 1–52 34 K. Alatalo and the ATLAS3D team

600 800 1000 1200 1400 NGC 4429

07′ 30″ 0.2

0.1 06′ 30″

Flux (Jy) 0.0 05′ 30″

-0.1 ° ′ ″ 11 04 30 -400 -200 0 200 400 -1 12h 27m 34s 30s Velocity (km s )

45″ 74 45″ -1 276 1400 0.38 vsys = 1104 km s 61 1300 0.28 ) 182 ) -1 -1 )

35″ 35″ -1 49 87 1200 0.19

1100 0.090 (K)

37 -7 B ″ ″ T 25 v (K km s 25

∆ 1000 25 -102 -0.0067 Velocity (km s

mb T Velocity (km s 900 -0.10 11° 06′ 15″ 12 11° 06′ 15″ -196 beam = 4.2″ 0 -291 800 -0.20 h m s s s h m s s s 0 10 20 30 12 27 27.6 27.2 26.8 12 27 27.6 27.2 26.8 Offset (arcsec), p.a. = 82.0°

40″ -289 -279 -269 -259 -249 -239 -229 -219 -209 -199 -189

25″

11° 06′ 10″ -179 -169 -159 -149 -139 -129 -119 -109 -99 -89 -79

-69 -59 -49 -39 -29 -19 -9 1 11 21 31

41 51 61 71 81 91 101 111 121 131 141

151 161 171 181 191 201 211 221 231 241 251

261 271 281

12h 27m 27.6 s 27.0s

Figure A16. NGC 4429 is a Virgo regular rotator (MK = -24.32) that includes two velocity maxima, with a bar and ring stellar morphology. It contains a dust disc. The moment0 peak is 14 Jy beam−1 km s−1. The moment1 contours are at 40 km s−1 intervals and the PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 35

400 600 800 1000 1200 NGC 4435 20″ 0.20 0.15 ′ ″ 05 00 0.10

0.05 40″ Flux (Jy) 0.00 20″ -0.05

-0.10 13° 04′ 00″ -400 -200 0 200 400 -1 12h 27m 43s 41s 39s Velocity (km s )

-1 0.57 137 v = 791 km s 179 1000 sys 114 111 0.42 ″ ) ″ 54 54 ) -1 -1

) 900

-1 50″ 91 50″ 42 0.27 800 ″ ″ 0.12 (K) 46 68 46 -26 B T

v (K km s ∆ 42″ 46 42″ -94 700 -0.028 Velocity (km s mb Velocity (km s ″ T ″ -0.18 38 23 38 -163 600 beam = 3.9″ 13° 04′ 34″ 0 13° 04′ 34″ -231 -0.33 h m s s h m s s 0 5 10 15 12 27 41.2 40.8 12 27 41.2 40.8 Offset (arcsec), p.a. = 201.°

-226 -216 -206 -196 -186 -176 -166 -156 -146 -136 50″

″ 44

38″

13° 04′ 32″

-126 -116 -106 -96 -86 -76 -66 -56 -46 -36

-26 -16 -6 4 14 24 34 44 54 64

74 84 94 104 114 124 134 144 154 164

174 184 194 204 214

12h 27m 41.2 s 40.8s

Figure A17. NGC 4435 is a Virgo regular rotator (MK = -23.82) that includes two velocity maxima, with a normal stellar morphology. It contains a dust disc. The moment0 peak is 20 Jy beam−1 km s−1. The moment1 contours are at 30 km s−1 intervals.

c 2012 RAS, MNRAS 000, 1–52 36 K. Alatalo and the ATLAS3D team

900 1000 1100 1200 1300 1400 40″ NGC 4694 0.4

20″ 0.3

0.2 59′ 00″

Flux (Jy) 0.1 40″ 0.0

10° 58′ 20″ -0.1 -200 -100 0 100 200 300 -1 12h 48m 18s 16s 14s Velocity (km s )

0.76 48 v = 1171 km s-1 39 sys 1240 40 27 0.56 ) 15″ 15″ ) 1220 -1 -1 ) 32 14 -1 1200 0.36 ′ ″ ′ ″ 59 05 59 05 1180

0.16 (K)

24 2 B

T

v (K km s 1160 ∆ 55″ 16 55″ -11 -0.036 Velocity (km s 1140 mb Velocity (km s T 8 -23 -0.23 ° ′ ″ ° ′ ″ 1120 10 58 45 10 58 45 ″ 0 -36 1100 beam = 3.5 -0.43 h m s s h m s s 0 5 10 15 20 25 12 48 16.0 14.0 12 48 16.0 14.0 Offset (arcsec), p.a. = 156.°

-66 -56 -46 -36 -26 15″

59′ 00″

10° 58′ 45″

-16 -6 4 14 24

34 44 54 64

12h 48m 16.0 s 14.0s

Figure A18. NGC 4694 is a Virgo regular rotator (MK = -22.15) with normal stellar morphology. It appears to be on its first approach into Virgo. It contains a dust filaments and bars. The moment0 peak is 6.0 Jy beam−1 km s−1. The moment1 contours are placed at 10km s−1 intervals and the PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 37

NGC 4710 900 1000 1100 1200 1300 1400 1.4

1.2 11 1.0

0.8

10 0.6

Flux (Jy) 0.4 09 0.2 0.0 ° ′ 15 08 -200 -100 0 100 200 300 -1 12h 49m 46s 42s Velocity (km s )

3.3 -1 1300 479 vsys = 1102 km s 118 399 73 2.7 ) ) ) -1 -1 ′ ″ ′ ″ -1 1200 10 10 319 10 10 28 2.0

1.4 (K) 239 -17 1100 B T

50″ v (K km s 50″

∆ 0.76 160 -62 Velocity (km s

mb 1000 Velocity (km s 80 T -107 0.13 ° ′ ″ ° ′ ″ 15 09 30 15 09 30 beam = 3.7″ 0 -152 900 -0.50 h m s s h m s s 0 10 20 30 40 50 60 12 49 41.0 40.0 12 49 41.0 40.0 Offset (arcsec), p.a. = 207.°

-197 -187 -177 -167 -157 -147 -137 -127 -117

′ ″

10 00

15° 09′ 30″

-107 -97 -87 -77 -67 -57 -47 -37 -27

-17 -7 3 13 23 33 43 53 63

73 83 93 103 113 123 133 143 153

163 173 183 193 203 213

12h 49m 41.0 s 40.0s

Figure A19. NGC 4710 is a Virgo regular rotator (MK = -23.52) with normal stellar morphology. It appears to be on the outskirts of Virgo and is likely to be on its first approach. It contains a dust disc, and is one of the nearest to edge-on systems in the sample. The moment0 peak is 62 Jy beam−1 km s−1. Channel map and PVD contours are placed at 3σ intervals.

c 2012 RAS, MNRAS 000, 1–52 38 K. Alatalo and the ATLAS3D team

NGC 4753 800 1000 1200 1400 1600 11 0.2

0.1 12 Flux (Jy) 0.0

-01° 13′ -0.1 -400 -200 0 200 400 -1 12h 52m 28s 24s 20s Velocity (km s )

0.38 49 -1 297 40″ 40″ vsys = 1163 km s 1400 40 206 0.28 )

) -1 -1 )

11′ 50″ 11′ 50″ -1 1300 32 115 0.19 1200

″ ″ 0.096 (K) 00 24 00 25 B T v (K km s 1100 ∆ 16 -66 0.0017 ″ ″ Velocity (km s

10 mb 10 1000 Velocity (km s 8 T -157 -0.092 900 -01° 12′ 20″ -01° 12′ 20″ beam = 5.5″ 0 -248 -0.19 h m s s h m s s 0 10 20 30 40 50 12 52 23.5 21.5 12 52 23.5 21.5 Offset (arcsec), p.a. = 93.0°

-316 -301 -286 -271 -256 -241 -226 -211 -196 -181

11′ 50″

05″

-01° 12′ 20″ -166 -151 -136 -121 -106 -91 -76 -61 -46 -31

-16 -1 14 29 44 59 74 89 104 119

134 149 164 179 194 209 224 239 254 269

284 299

12h 52m 23.5 s 21.5s

Figure A20. NGC 4753 is a field regular rotator (MK = -25.09) that includes two velocity maxima, with stellar morphology consistent with interaction. It contains a dust filament. It is also the most massive galaxy in the CARMA ATLAS3D survey. The moment0 peak is 12 Jy beam−1 km s−1. Moment1 contours are placed at 40km s−1 intervals and PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 39

2200 2300 2400 2500 2600 NGC 5173 0.15

0.10 40″ 0.05

Flux (Jy) 20″ 0.00

-0.05

46° 35′ 00″ -200 -100 0 100 200 -1 13h 28m 27.0s 26.0s Velocity (km s )

0.26 32 v = 2424 km s-1 78 40″ 40″ sys 2500 26 47 0.18 ) ) -1 -1 ) 2450 -1 21 16 0.099 ″ ″

30 30 2400 0.021 (K)

16 -15 B T v (K km s ∆ 11 -45 2350 -0.057 Velocity (km s mb Velocity (km s 46° 35′ 20″ 5 T 46° 35′ 20″ -76 -0.13 2300 beam = 3.6″ 0 -107 -0.21 h m s s h m s s 0 5 10 15 20 25 30 13 28 26.2 25.8 13 28 26.2 25.8 Offset (arcsec), p.a. = 100.°

-137 -117 -97 -77 -57 40″

30″

46° 35′ 20″ -37 -17 3 23 43

63 83

13h 28m 26.2 s 25.8s

Figure A21. NGC 5173 is a group regular rotator (MK = -22.88) with normal stellar morphology. It contains a dust bar. NGC 5173 was observed in CARMA D- and C- arrays, and the data were shared between this survey, and the work of Wei et al. 2010b, and thus uses the smaller pixel size of 0.4′′, to reflect the superior resolution of the observations. The moment0 peak is 4.6 Jy beam−1 km s−1. PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 40 K. Alatalo and the ATLAS3D team

1500 1600 1700 1800 1900 2000 NGC 5379 45′ 10″ 0.3

50″ 0.2

30″ 0.1 Flux (Jy) 44′ 10″ 0.0

59° 43′ 50″ -300 -200 -100 0 100 200 300 -1 13h 55m 37s 35s 33s Velocity (km s )

28 -1 126 0.56 vsys = 1774 km s 1900 50″ 50″ 23 83 0.43 ) ) -1

-1 ) 1850 40″ 18 40″ 39 -1 0.30 1800

0.17 (K) ″ 14 ″ -4 B 30 30 T v (K km s 1750 ∆ 9 -47 0.040 Velocity (km s 20″ mb 20″ Velocity (km s T 1700 -0.089 5 -91 beam = 3.9″ 59° 44′ 10″ 0 59° 44′ 10″ -134 1650 -0.22 h m s s h m s s 0 10 20 30 40 50 13 55 35.5 33.5 13 55 35.5 33.5 Offset (arcsec), p.a. = 66.°

-119 -109 -99 -89 -79 -69 -59

40″

25″

59° 44′ 10″

-49 -39 -29 -19 -9 1 11

21 31 41 51 61 71 81

91 101 111 121 131

13h 55m 35.5 s33.5s

Figure A22. NGC 5379 is a group regular rotator (MK = -22.08) with ring stellar morphology. It contains a dust bar, ring, and filaments. The moment0 peak is 5.7 Jy beam−1 km s−1. PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 41

200 400 600 800 1000 1200 NGC 5866 47 0.6

0.4 46

0.2

Flux (Jy)

45 0.0

-0.2 55° 44′ -600 -400 -200 0 200 400 -1 15h 06m 36s 32s 28s Velocity (km s )

440 1.5 v = 745 km s-1 295 sys 1000 367 1.1 ) 200 ) -1 -1 ′ ″ ′ ″ ) 900 46 00 46 00 -1 293 105 0.73 800

0.35 (K)

220 10 B T 40″ v (K km s 40″ 700 ∆ 147 -85 -0.021 Velocity (km s

mb 600 T Velocity (km s 73 -180 -0.39 ° ′ ″ ° ′ ″ 500 beam = 3.3″ 55 45 20 0 55 45 20 -275 -0.77 h m s s h m s s 0 10 20 30 40 50 60 15 06 31.5 30.5 15 06 31.5 30.5 Offset (arcsec), p.a. = 127.°

-270 -260 -250 -240 -230 -220 -210 -200 -190 -180

50″

55° 45′ 20″ -170 -160 -150 -140 -130 -120 -110 -100 -90 -80

-70 -60 -50 -40 -30 -20 -10 0 10 20

30 40 50 60 70 80 90 100 110 120

130 140 150 160 170 180 190 200 210 220

230 240 250 260 270 280 290

15h 06m 31.5 s 30.5s

Figure A23. NGC 5866 is a field regular rotator (MK = -24.00) with normal stellar morphology. It contains a dust disc. The molecular gas also strongly suggests that this galaxy contains a bar. The moment0 peak is 54 Jy beam−1 km s−1. Moment1 contours are placed at 40km s−1 intervals. Channel map contours are placed at 2σ intervals and PVD contours are placed at 2σ intervals.

c 2012 RAS, MNRAS 000, 1–52 42 K. Alatalo and the ATLAS3D team

2200 2300 2400 2500 2600 2700 NGC 6014 0.4 30″ 0.3 56′ 10″ 0.2

50″ 0.1 Flux (Jy)

0.0 30″ -0.1 ° ′ ″ 05 55 10 -200 -100 0 100 200 300 -1 15h 56m 00s 55m 58s 56s Velocity (km s )

0.80 78 v = 2381 km s-1 63 sys 56′ 04″ 65 56′ 04″ 41 0.57 )

) 2450

-1 -1 )

-1 58″ 52 58″ 20 0.35 2400

0.12 (K)

39 -2 B 52″ 52″ T v (K km s

∆ 2350 26 -24 -0.11 Velocity (km s ″ mb ″ Velocity (km s 46 T 46 -0.34 13 -45 2300

05° 55′ 40″ 0 05° 55′ 40″ -67 beam = 4.0″ -0.56 h m s s h m s s 0 5 10 15 20 25 15 55 58.2 57.6 15 55 58.2 57.6 Offset (arcsec), p.a. = 140.°

56′ 06″ -102 -92 -82 -72 -62 -52

58″

50″

05° 55′ 42″

-42 -32 -22 -12 -2 8

18 28 38 48 58 68

78 88 98

15h 55m 58.2 s 57.6s

Figure A24. NGC 6014 is a field regular rotator (MK = -22.99) with normal stellar morphology. It contains a dust bar, ring and filaments. The moment0 peak is 14 Jy beam−1 km s−1. PVD contours are placed at 1.5σ intervals.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 43

1700 1800 1900 2000 2100 2200

NGC 7465 30″ 0.8

0.6 58′ 10″

0.4 50″ Flux (Jy) 0.2 30″ 0.0 15° 57′ 10″ -300 -200 -100 0 100 200 300 23h 02m 04s 01s Velocity (km s-1)

″ 66 ″ -1 50 0.65 15 15 vsys = 1960 km s 2100 55 31 0.53 ) )

-1 2050 -1 58′ 05″ 58′ 05″ ) 44 12 -1 0.40 2000 ″ ″ 55 55 0.28 (K)

33 -7 B

1950 T

v (K km s ∆ ″ 22 ″ -27 0.15 45 45 Velocity (km s 1900 mb Velocity (km s T 11 -46 0.024 15° 57′ 35″ 15° 57′ 35″ 1850 beam = 5.6″ 0 -65 -0.10 h m s s s h m s s s 0 10 20 30 40 50 23 02 2.5 1.5 0.5 23 02 2.5 1.5 0.5 Offset (arcsec), p.a. = 106.°

-125 -115 -105 -95 -85 -75 -65

58′ 00″

45″

15° 57′ 30″

-55 -45 -35 -25 -15 -5 5

15 25 35 45 55 65 75

85 95 105 115

23h 02m 2.5 s 0.5s

Figure A25. NGC 7465 is a field non-regular rotator (MK = -22.82) with a kinematically-decoupled core (KDC) with stellar morphology indicative of interaction. It contains dust filaments. The moment0 peak is 26 Jy beam−1 km s−1. Channel map contours are placed at 2σ intervals and PVD contours are placed at 4σ intervals.

c 2012 RAS, MNRAS 000, 1–52 44 K. Alatalo and the ATLAS3D team

2600 2700 2800 2900 3000 3100 PGC 029321 55″ 0.2

45″ 0.1

″ Flux (Jy) 35 0.0

12° 57′ 25″ -0.1 -200 -100 0 100 200 300 10h 05m 52.5s 51.5s 50.5s Velocity (km s-1)

0.68 55 v = 2816 km s-1 9 sys 2850 ″ 46 ″ -5 0.51 48 ) 48 ) -1 -1 ) -1 0.34 36 -19 2800 42″ 42″

0.17 (K) 27 -34 B T

v (K km s ∆ 36″ 18 36″ -48 2750 0.0033 Velocity (km s mb Velocity (km s 9 T -62 -0.17 12° 57′ 30″ 12° 57′ 30″ beam = 3.7″ 0 -76 2700 -0.33 h m s s h m s s 0 5 10 15 10 05 52.0 51.4 10 05 52.0 51.4 Offset (arcsec), p.a. = 76.0°

48″ -111 -101 -91 -81 -71 -61

42″

36″

12° 57′ 30″

-51 -41 -31 -21 -11 -1

9 19

10h 05m 52.0 s 51.4s

Figure A26. PGC 029321 is a field regular rotator (MK = -21.66) with normal stellar morphology. It contains dust filaments. The moment0 peak is 8.5 Jy beam−1 km s−1.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 45

1200 1300 1400 1500 1600 1700 1800 PGC 058114 0.6 40″

0.4

0.2 20″ Flux (Jy)

0.0

02° 54′ 00″ -300 -200 -100 0 100 200 300 -1 16h 26m 5.5 s 4.5s 3.5s Velocity (km s )

158 -1 83 1650 1.3 36″ 36″ v = 1507 km s sys 132 51 1.1 ) 1600 ) -1 -1 ″ ″ )

30 30 -1 0.78 106 20 1550

24″ 24″ 0.50 (K) 79 -12 B 1500 T v (K km s

∆ 53 -44 0.21 18″ 18″ Velocity (km s

mb 1450 Velocity (km s T -0.073 26 -75 ° ′ ″ ° ′ ″ 1400 beam = 4.2″ 02 54 12 0 02 54 12 -107 -0.36 h m s s h m s s 0 5 10 15 20 16 26 5.0 4.6 16 26 5.0 4.6 Offset (arcsec), p.a. = 94.5°

36″ -112 -102 -92 -82 -72 -62 -52

30″

24″

18″

02° 54′ 12″

-42 -32 -22 -12 -2 8 18

28 38 48 58 68 78 88

98 108 118

16h 26m 5.0 s 4.6s

Figure A27. PGC 058114 is a field galaxy (MK = -21.57) with unknown kinematic structure or morphology. The moment0 peak is 28 Jy beam−1 km s−1. Channel map and PVD contours are placed at 2σ intervals.

c 2012 RAS, MNRAS 000, 1–52 46 K. Alatalo and the ATLAS3D team

2800 2900 3000 3100 UGC 05408 0.10

15″ 0.05

Flux (Jy) 0.00 26′ 05″

-0.05

59° 25′ 55″ -200 -100 0 100 -1 10h 03m 52.5s 51.5s Velocity (km s )

0.26 23 v = 2998 km s-1 -68 sys 19 -77 0.17 ″ ) ″ 16 16 ) -1 -1 ) -50 -1 15 -87 0.078 10″ 10″

-0.012 (K) 11 -97 B -100 T v (K km s ∆ ′ ″ 8 ′ ″ -106 -0.10 26 04 26 04 Velocity (km s mb Velocity (km s T -0.19 4 -116 -150 ° ′ ″ ° ′ ″ beam = 3.8″ 59 25 58 0 59 25 58 -126 -0.28 h m s s h m s s 0 5 10 15 10 03 52.6 52.0 10 03 52.6 52.0 Offset (arcsec), p.a. = 315.°

-188 -163 -139 -114 16″

10″

26′ 04″

59° 25′ 58″

-89 -65 -40 -16

10h 03m 52.6 s52.2s 51.8s

Figure A28. UGC 05408 is a field regular rotator (MK = -22.03) with a bar stellar morphology. It contains a dust bar and filaments. At a distance 45.8 Mpc, it is the most distant detection in the CARMA ATLAS3D survey. The moment0 peak is 3.5 Jy beam−1 km s−1.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 47

2400 2600 2800 3000 UGC 06176 50″ 0.15

0.10 30″ 0.05

Flux (Jy) 0.00 39′ 10″ -0.05

21° 38′ 50″ -400 -200 0 200 400 -1 11h 07m 27.0s 26.0s Velocity (km s )

127 -1 102 0.75 vsys = 2680 km s 2800 106 59 0.56 ) ″ ″ )

32 -1 32 -1 ) 2750 85 15 -1 0.37 2700 26″ 26″ 0.18 (K)

64 -28 B 2650 T v (K km s ∆ ″ 42 ″ -71 -0.0031 20 20 Velocity (km s

mb 2600 Velocity (km s T 21 -115 -0.19 2550 ° ′ ″ ° ′ ″ beam = 3.4″ 21 39 14 0 21 39 14 -158 -0.38 h m s s h m s s 0 2 4 6 8 10 11 07 25.4 24.8 11 07 25.4 24.8 Offset (arcsec), p.a. = 201.°

-151 -136 -121 -106 -91 -76 -61

32″

26″

20″

21° 39′ 14″

-46 -31 -16 -1 14 29 44

59 74 89 104 119 134

11h 07m 25.4 s 25.0s

Figure A29. UGC 06176 is a field regular rotator (MK = -22.66) with bar and ring stellar morphology. It contains a dust bar, ring, and filaments. The moment0 peak is 14 Jy beam−1 km s−1.

c 2012 RAS, MNRAS 000, 1–52 48 K. Alatalo and the ATLAS3D team

1500 1600 1700 1800 1900 2000 UGC 09519 0.4 30″ 0.3

0.2

22′ 10″ 0.1 Flux (Jy) 0.0

-0.1 34° 21′ 50″ -200 -100 0 100 200 300 -1 14h 46m 23.0s 22.0s Velocity (km s )

171 105 1.4 -1 vsys = 1631 km s 142 67 1.1 ) ″ ″ ) 1800

20 -1 20 -1 ) 114 29 -1 0.72

14″ 14″ 1750 0.37 (K)

85 -10 B

T v (K km s

∆ 57 -48 1700 0.024 08″ 08″ Velocity (km s mb Velocity (km s T -0.32 28 -87 1650 ° ′ ″ ° ′ ″ beam = 3.4″ 34 22 02 0 34 22 02 -125 -0.67 h m s s s h m s s s 0 2 4 6 8 14 46 21.8 21.2 20.6 14 46 21.8 21.2 20.6 Offset (arcsec), p.a. = 178.°

-140 -130 -120 -110 -100 -90 -80 -70

20″

14″

08″

34° 22′ 02″ -60 -50 -40 -30 -20 -10 0 10

20 30 40 50 60 70 80 90

100 110 120 130 140

14h 46m 21.8 s 21.2s 20.6s

Figure A30. UGC 09519 is a field regular rotator (MK = -21.98) with normal stellar morphology. It contains dust filaments. The moment0 peak is 18 Jy beam−1 km s−1.

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 49

1.6 180 50 ʺ NGC 524 1.3 ) 120 -1

)

-1

1.1 kms 60

30 ʺ -1

20 ʺ 0.79 20 ʺ 0

32 ʹ 10ʺ 0.53 -60

(kms Velocity

0.26 (Jybm Intensity -120 09 ° 31ʹ 50ʺ 09 ° 32ʹ 10ʺ 09 ° 32 ʹ 10 ʺ 10 ʺ 0.0 -180 01 h 24m 50s 48 s 46 s 01 h 24m 48.6 s 48.2s 47.8s 47.4s 01 h 24 m 48.6 s 48.2 s 47.8 s 47.4 s

1.2 130 NGC 2768 1.0 80 -1 45″ ) -1

0.80 km s 30

-1 15″ 15″ 02′ 15″ 0.60 -20

0.40 -70

45″ Velocity (km s Intensity Jy bm 60° 02′ 05″ 0.20 60° 02′ 05″ -120 ° ′ ″ 10″ 60 01 15 0.0 -170 09h 11m 41s 39s 09h 11m 38.2 s 37.8s 37.4s 09h 11m 38.2 s 37.8s 37.4s

18 1628 NGC 3032

15 ) 1604 -1 20″ 20″ ) -1

″ 12 km s 1580 20 -1 ″ ″ 10 10 10 1555

14′ 00″ 7 1531

14′ 00″ 14′ 00″ Velocity (km s

4 Intensity (Jy bm 1507 29° 13′ 40″ 10″ 29° 13′ 50″ 1 29° 13′ 50″ 1483 09h 52m 10s 08s 09h 52m 9.5s 8.5s 7.5s 09h 52m 9.5s 8.5s 7.5s

″ 1.3 ″ 130 NGC 3489 20 20 45″ 1.0 83 -1

) ″ ″ -1

10 0.83 km s 10 37 54′ 15″ -1

0.63 -10

54′ 00″ 54′ 00″ 45″ 0.42 -57 Velocity (km s

0.21 Intensity Jy bm -103 ° ′ ″ ° ′ ″ ° ′ ″ 13 53 50 13 53 50 13 53 15 10″ 0.0 -150 11h 00m 22s 20s 18s 11h 00m 19.5s 18.5s 11h 00m 19.5s 18.5s

Figure B1. Interferometric CO(1–0) data from ATLAS3D in the literature. From top-to-bottom, NGC 524 (Crocker et al. 2011), NGC 2768 (Crocker et al. 2008), NGC 3032 (Young, Bureau & Cappellari 2008), NGC 3489 (Crocker et al. 2011), NGC 4459 (Young, Bureau & Cappellari 2008), NGC 4476 (Young 2002), NGC 4477 (Crocker et al. 2011), NGC 4526 (Young, Bureau & Cappellari 2008) and NGC 4550 (Crocker et al. 2009). For each galaxy, from left-to- right, the panels show the r-band image overlaid with the CO(1–0) integrated intensity (moment0) contours (cyan), the color-scale and contours of the CO integrated intensity (moment0) map overlaid with the IRAM 30m telescope beam (gray), the color-scale of the CO mean velocity (moment1) map overlaid with isovelocity contours and the IRAM 30m telescope beam (gray), and the g − r colour image overlaid with the CO(1–0) moment0 contours (magenta). For comparisons to unsharp-masked HST data of these galaxies, see the papers cited above.

APPENDIX B: INTERFEROMETRIC CO DATA FROM THE LITERATURE APPENDIX C: GALAXIES OBSERVED WITH CARMA NOT IN THE ATLAS3D SURVEY

c 2012 RAS, MNRAS 000, 1–52 50 K. Alatalo and the ATLAS3D team

21 1357

20″ NGC 4459 18 ) 1302 55″ -1 55″

)

′ ″ -1

59 00 14 km s 1248 -1 45″ 45″ ″ 11 1193 40

35″ 7 35″ 1138 20″ Velocity (km s

4 Intensity (Jy bm 1084 ° ′ ″ ° ′ ″ 13° 58′ 00″ 13 58 25 13 58 25 10″ 0 1029 12h 29m 03s 01s 28m 59s 12h 29m 1.2s 0.8s 0.4s 12h 29m 1.2s 0.8s 0.4s

12 2050

NGC 4476 10 ) 2015 30″ -1 21′ 05″ 21′ 05″ ) -1

8 km s 1980

-1 21′ 00″ ″ ″ 55 6 55 1945

″ 4 1910 30 45″ 45″ Velocity (km s

2 Intensity (Jy bm 1875 ° ′ ″ ° ′ ″ ° ′ ″ 10″ 12 20 00 12 20 35 0 12 20 35 1840 12h 30m 03s 01s 29m 59s 57s 12h 30m 0.4s 0.0s 29m 59.6s 12h 30m 0.4s 0.0s 29m 59.6s

3.6 105 NGC 4477

3.0 ) 72 45″ -1 ) -1

2.4 km s 38 -1 38′ 15″ 10″ 1.8 10″ 5

1.2 -28 45″ Velocity (km s

0.60 Intensity (Jy bm -62 13° 38′ 00″ 13° 38′ 00″ 10″ 13° 37′ 15″ 0.0 -95 12h 30m 06s 04s 02s 00s 12h 30m 3.0 s 2.6s 2.2s 1.8s 12h 30m 3.0 s 2.6s 2.2s 1.8s

37 950 43′ 00″ NGC 4526

32 ) 828 -1 ″

30 )

42′ 05″ 42′ 05″ -1

26 km s 707

-1 ′ ″ 42 00 21 585 55″ 55″ 30″ 16 463 Velocity (km s

10 Intensity (Jy bm 342 ° ′ ″ ° ′ ″ ° ′ ″ 07 41 00 07 41 45 07 41 45 10″ 5 220 12h 34m 07s 05s 12h 34m 4.2s 3.8s 12h 34m 4.2s 3.8s

1.7 ) 115 NGC 4550 30″ -1 30″

1.4 89 km s

-1 14′ 00″ ) ″ 1.1 ″ 63 -1 20 20

30″ 0.83 37

10″ 10″ 0.55 12 Velocity (km s 13′ 00″ 0.28 -14 ° ′ ″ ° ′ ″ 12 13 00 12 13 00 10″ ° ′ ″ 12 12 30 0.0 Integrated Intensity (Jy bm -40 12h 35m 34s 32s 30s 12h 35m 31.8s 31.4s 31.0s 12h 35m 31.8s 31.4s 31.0s

Figure B1. Continued

c 2012 RAS, MNRAS 000, 1–52 The CARMA ATLAS3D CO survey of ETGs 51

1500 1600 1700 1800 1900 2000 NGC 2697 58′ 50″ 0.3

0.2 10″ 0.1

Flux (Jy) 30″ 0.0

-0.1 -02° 59′ 50″ -300 -200 -100 0 100 200 -1 08h 55m 02s 00s Velocity (km s )

13 126 0.22 -1 58′ 55″ 58′ 55″ vsys = 1814 km s 11 74 0.16 ) )

-1 1900 -1 )

-1 9 23 0.11 10″ 10″

1800 0.049 (K)

6 -29 B T

v (K km s ∆ ″ 4 ″ -81 -0.0069

25 25 Velocity (km s mb 1700 Velocity (km s T 2 -132 -0.063

-02° 59′ 40″ 0 -02° 59′ 40″ -184 beam = 6.8″ -0.12 h m s m s h m s m s 0 10 20 30 40 50 60 08 55 1.0 54 59.0 08 55 1.0 54 59.0 Offset (arcsec), p.a. = 302.°

58′ 55″ -184 -164 -144 -124 -104 -84

10″

25″

-02° 59′ 40″

-64 -44 -24 -4 16 36

56 76 96 116 136

08h 55m 1.0 54s m 59.0 s

Figure C1. NGC 2697 (MK = -22.19) was removed from the sample as being mis-classified and containing spiral structure in the stellar isophotes. The moment0 peak is 4.1 Jy beam−1 km s−1.

c 2012 RAS, MNRAS 000, 1–52 52 K. Alatalo and the ATLAS3D team

2000 2100 2200 2300 2400 2500 NGC 4292 0.20

0.15 36′ 10″

0.10

50″ 0.05 Flux (Jy) 0.00 30″ -0.05

04° 35′ 10″ -300 -200 -100 0 100 200 -1 12h 21m 19s 17s 15s Velocity (km s )

0.61 56″ 29 56″ v = 2258 km s-1 72 2350 sys 24 46 0.46 )

) -1 -1 50″ 50″ ) 2300 19 20 -1 0.32

44″ 44″ 2250 0.18 (K) 15 -6 B T v (K km s ∆ 10 -31 0.032 ″ ″ Velocity (km s 2200

38 mb 38 Velocity (km s 5 T -57 -0.11

2150 beam = 3.8″ 04° 35′ 32″ 0 04° 35′ 32″ -83 -0.26 h m s s h m s s 0 2 4 6 8 10 12 14 12 21 17.2 16.6 12 21 17.2 16.6 Offset (arcsec), p.a. = 230.°

56″ -123 -113 -103 -93 -83 -73 -63

50″

44″

38″

04° 35′ 32″

-53 -43 -33 -23 -13 -3 7

17 27 37 47 57 67 77

87 97 107

12h 21m 17.2s 16.8s

3D Figure C2. NGC 4292 is a Virgo cluster galaxy (MK = -23.2). It was removed from the ATLAS sample based on its not being observed with SAURON, and thus lacks stellar kinematic data. The moment0 peak is 4.3 Jy beam−1 km s−1.

c 2012 RAS, MNRAS 000, 1–52