PHIBSS2: survey design and z=0.5-0.8 results. Molecular gas reservoirs during the winding-down of star formation

Following the success of the Plateau de Bure high-z Blue Sequence Survey (PHIBSS), we present the PHIBSS2 legacy program, a survey of the molecular gas properties of star-forming galaxies on and around the star formation main sequence (MS) at different redshifts using NOEMA. This survey significantly extends the existing sample of star-forming galaxies with CO molecular gas measurements, probing the peak epoch of star formation (z=1-1.6) as well as its building-up (z=2-3) and winding-down (z=0.5-0.8) phases. The targets are drawn from the GOODS, COSMOS, and AEGIS deep fields and uniformly sample the MS in the stellar mass (M*) - star formation rate (SFR) plane with log(M*/Msun) = 10-11.8. We describe the survey strategy and sample selection before focusing on the results obtained at z=0.5-0.8, where we report 60 CO(2-1) detections out of 61 targets. We determine their molecular gas masses and separately obtain disc sizes and bulge-to-total (B/T) luminosity ratios from HST I-band images. The median molecular gas-to-stellar mass ratio, gas fraction, and depletion time as well as their dependence with M* and offset from the MS follow published scaling relations for a much larger sample of galaxies spanning a wider range of redshifts. The galaxy-averaged Kennicutt-Schmidt (KS) relation between molecular gas and SFR surface densities is strikingly linear, pointing towards similar star formation timescales within galaxies at any given epoch. In terms of morphology, the molecular gas content, the SFR, the disc stellar mass, and the disc molecular gas fraction do not seem to correlate with B/T and the stellar surface density, which suggests an ongoing supply of fresh molecular gas to compensate for the build-up of the bulge. Our measurements do not yield any significant variation of the depletion time with B/T and hence no strong evidence for morphological quenching within the scatter of the MS.


Introduction
The main sequence of star formation Observed massive galaxies in the distant universe form stars at much higher rates than their local counterparts, with a peak epoch of star formation in the range z = 1 − 3 (Noeske et al. 2007;Daddi et al. 2007;Reddy & Steidel 2009;Bouwens et al. 2010;Cucciati et al. 2012;Lilly et al. 2013;Madau & Dickinson 2014). At each epoch, there is a bimodality between red passive galaxies on one side and blue star-forming galaxies on the other, most of the latter lying on a relatively tight, almost linear relation between their stellar mass (M ) and star formation rate (SFR), known as the star formation 'main sequence' (MS; Baldry et al. 2004;Brinchmann et al. 2004;Noeske et al. 2007;Elbaz et al. 2007Elbaz et al. , 2011Daddi et al. 2007;Schiminovich et al. 2007;Damen et al. 2009;Santini et al. 2009;Rodighiero et al. 2010Rodighiero et al. , 2011Peng et al. 2010b;Wuyts et al. 2011b;Sargent et al. 2012;Whitaker et al. 2012Whitaker et al. , 2014Speagle et al. 2014;Renzini & Peng 2015;Schreiber et al. 2015). About 90% of the cosmic star formation history since z = 2.5 took place near this MS. The ≤ 0.3 dex scatter of the MS, the rotating disc morphology of most galaxies that constitute it (Förster Schreiber et al. 2006Genzel et al. 2006Genzel et al. , 2008Stark et al. 2008;Daddi et al. 2010a;Wuyts et al. 2011b) and the long star formation cycles inferred from the number of star-forming galaxies observed at z = 1 − 2 (Daddi et al. 2005Caputi et al. 2006) argue in favour of a relatively smooth mode of star formation. The large molecular gas reservoirs fueling star formation (Erb et al. 2006;Daddi et al. 2010a;Tacconi et al. 2010Tacconi et al. , 2013 are thought to be maintained by a continuous supply of fresh gas from the cosmic web and minor mergers (Birnboim & Dekel 2003;Kereš et al. 2005Kereš et al. , 2009Dekel & Birnboim 2006;Cattaneo et al. 2006;Ocvirk et al. 2008;Dekel et al. 2009a;Genel et al. 2010). Typical star-forming galaxies are expected to progress along the MS in a slowly evolving gas-regulated quasi equilibrium between inflows, outflows, and star formation Davé et al. 2011bDavé et al. , 2012Feldmann 2013;Lilly et al. 2013;Dekel et al. 2013;Peng & Maiolino 2014;Dekel & Mandelker 2014) until their star formation is quenched when they enter denser environments or grow past the Schechter mass (M ∼ 10 10.8−11 M ; Conroy & Wechsler 2009;Peng et al. 2010b), and then to rapidly transit down to the red sequence. Episodes of gas compaction, depletion, and replenishment could confine them within the scatter of the MS before the final quenching occurs (Dekel & Burkert 2014;Zolotov et al. 2015;Tacchella et al. 2016a,b). Quenching might be due to a combination of factors, including gas removal by winds driven by supernovae or active galactic nuclei (AGNs), gas streams from the cosmic web that stop penetrating galactic Article number, page 1 of 28 arXiv:1812.08180v3 [astro-ph.GA] 17 Jan 2019 haloes above a critical halo mass, a sudden drop in the gas cooling, a change in morphology, and/or environmental effects.
The equilibrium model predicts strong correlations between the specific SFR (sSFR = SFR/M star ) and the gas fraction (or equivalently, the gas-to-stellar mass ratio µ gas = M gas /M star , where M gas is either the total or the molecular gaseous mass of the galaxy) as they evolve with redshift, while the gas compaction scenario further implies gradients of the central gas density, gas fraction, and depletion time (t depl = M gas /SFR) across the MS. Measurements of these quantities at different redshifts thus provide crucial observational tests to understand the building-up and the winding-down phases of normal MS starforming galaxies. The depletion time, which measures the star formation efficiency (SFE), has notably been suggested to decrease with redshift up to z = 1 (Combes et al. 2011. The Kennicutt-Schmidt (KS) relation between the molecular gas and SFR surface densities, Σ SFR ∝ (Σ gas ) N , further characterises the SFE averaged over entire galaxies or subregions within them. It has been shown to be near linear on galactic and subgalactic scales for Σ gas > 10 M pc −2 , with an exponent N = 0.9 − 1.3 and a scatter of ±0.3 − 0.4 dex (Schmidt 1959;Kennicutt 1998b;Bigiel et al. 2008Bigiel et al. , 2011Leroy et al. 2008Leroy et al. , 2013Daddi et al. 2010a,b;Saintonge et al. 2011a;Schruba et al. 2011;Kennicutt & Evans 2012), indicating relatively uniform molecular gas depletion times around 1 − 2 Gyr.

The PHIBSS survey up to now
The Plateau de Bure High-z Blue Sequence Survey (PHIBSS, PI: L. Tacconi & F. Combes) carried out at the IRAM Plateau de Bure interferometer (PdBI; Guilloteau et al. 1992;Cox 2011) aimed at better understanding the winding-down of star formation within normal MS star-forming galaxies from the point of view of their molecular gas reservoirs. It focused on the massive tail of the MS at z = 1.2 and 2.2, with log(M /M ) 10.4 and log(SFR/M yr −1 ) 1.5, and comprised 52 CO (3-2) detections and 8 higher-resolution imaging observations with beam sizes in the range 0.3 − 1 . It uncovered large molecular gas reservoirs, with mean molecular gas fractions f gas = M gas /(M gas + M ) of 33% at z = 1.2 and 47% at z = 2.2 , when they only reach 7-10% in local giant spirals Saintonge et al. 2011a), showing that the cosmic evolution of the SFR is mainly due to the diminishing molecular gas content. Tacconi et al. (2013) further showed that f gas decreases with M , which can be interpreted in terms of feedback models where the first generations of stars remove part of the gas or in terms of a mass dependence of the accretion effiency or the SFE, since µ gas = sSFR × t depl (e.g. Bouché et al. 2010;Davé et al. 2011a). The PHIBSS also obtained a near linear KS relation lying in the continuity of low redshift measurements, albeit with a slightly lower mean depletion time Tacconi et al. 2013). The sub-arcsecond follow-up observations enabled to obtain good-quality rotation curves and resolved velocity dispersion maps, showing an increased turbulent support compared to low redshift which is compatible with models where cosmic streams feed the disc and trigger violent gravitational instabilities (e.g. Dekel et al. 2009b). Resolved kinematics also enabled to separate smoothed ensembles of clumps due to their different velocities, and to obtain a resolved KS relation at sub-galactic scale for four galaxies of the sample (Freundlich et al. 2013). Genzel et al. (2013) further obtained a pixel by pixel KS relation for one typical z = 1.53 massive star-forming galaxy from the PHIBSS sample.

The PHIBSS2 legacy program
Built on the success of the PHIBSS, the IRAM PHIBSS2 legacy program (PIs: F. Combes, S. García-Burillo, R. Neri & L. Tacconi) intends to extend these results to a wider range of redshifts and to better sample the M -SFR plane at each redshift. This four-year program was phased to optimise and exploit the NOrthern Extended Millimeter Array (NOEMA; Schuster 2014) capabilities as they came online at the PdBI, which enabled a significant statistical gain with the smaller integration times and the increased sensitivity. PHIBSS2 has measured mean molecular gas fractions and depletion times in different redshift bins and across the MS, with the aim of studying the connection between star formation and molecular gas reservoirs and its evolution with redshift. Genzel et al. (2015) and Tacconi et al. (2018) already use PHIBSS2 detections together with other measurements to quantify precisely how the depletion time and the gas fraction depend on redshift, stellar mass, and the offset from the MS reference line. They notably find that while the gas fraction decreases steeply with time, the depletion time slowly increases. They show how the gas fraction progressively increases above the MS and decreases below and how the depletion time follows the opposite trend without depending much on the stellar mass.
In this paper, we present the PHIBSS2 strategy and its results at z = 0.5 − 0.8. In this redshift bin, we report 60 CO  detections within a sample of 61 star-forming galaxies, hence constituting the first systematic census of the molecular gas in this redshift range. This sample bridges the gap between observations of the molecular gas in the nearby universe and at the peak epoch of star formation, probing the crucial period of the winding-down of star formation in the last 10 Gyr of the history of the universe. Until now, paradoxically, the molecular gas content of galaxies in this redshift range has not been studied as much as that of higher-redshift galaxies, partly because the CO line flux increase with frequency makes high CO rotational transitions more easily observable at higher redshifts (Combes et al. 1999). We determine the molecular gas content, the sizes and morphology of these galaxies and describe the star-formation conditions within them in terms of gas fraction, depletion time, and surface densities. Section 2 presents the general PHIBSS2 strategy, the sample selection and its implementation with the IRAM Plateau de Bure interferometer and its NOEMA upgrade. Section 3 reports the CO molecular gas measurements we obtain at z = 0.5−0.8 and the results of our morphological study. In section 4, we interpret our results in terms of molecular gas fraction and depletion time, their dependence on morphology and the KS relation. We conclude in Section 5. Throughout this paper, we assume a flat ΛCDM universe with Ω m = 0.3, Ω Λ = 1 − Ω m and H 0 = 70 km.s −1 .Mpc −1 .

Survey goals and strategy
The PHIBSS2 four-year legacy program is designed as a comprehensive and systematic study of the CO molecular gas content of galaxies during the build-up (z = 2−3), peak (z = 1−1.6), and subsequent winding-down (z = 0.5 − 0.8) phases of star formation in the universe. As shown in Fig. 1, it targets more than 120 sources over three redshift bins sampling the M -SFR plane in the well-studied GOODS-North, COSMOS, and AEGIS cosmological fields on and around the MS. It significantly expands the first PHIBSS sample, which focused on galaxies at z = 1.2 and 2.2, doubles the number of CO measurements available at z > 2, systematically probes the winding-down epoch at z = 0.5 − 0.8 Fig. 1: Location of the PHIBSS2 sample in the three redshift ranges z = 0.5 − 0.8, z = 1 − 1.6 and z = 2 − 3 as a function of stellar mass M and SFR. The PHIBSS2 galaxies at z = 0.5−0.8 presented in this paper and the targets in the other redshift ranges are all marked as plain red circles. The PHIBSS sample  is indicated as plain blue squares while other existing CO measurements in the same redshift ranges are displayed as open triangles, including ULIRGs at z = 0.5 − 0.8 observed with the IRAM 30m telescope (Combes et al. 2011, near MS star-forming galaxies in the range z = 0.5 − 3 (Daddi et al. 2010a;Magdis et al. 2012b;Magnelli et al. 2012), above MS submillimeter galaxies in the range z = 1.2 − 3 (Greve et al. 2005;Tacconi et al. 2006Tacconi et al. , 2008Bothwell et al. 2013) and lensed MS galaxies in the range z = 1.2 − 3 observed with the IRAM PdBI (Saintonge et al. 2013, and references therein), as well as additional sources between z = 1 and z = 2.5 observed with ALMA and NOEMA (Silverman et al. 2015;Decarli et al. 2016, Genzel et al. in prep.). The upper panel also shows sources observed by Geach et al. (2011) at z ∼ 0.4 as open diamonds and Bauermeister et al. (2013) at z ∼ 0.5 as open squares. The background data points correspond to 3D-HST galaxies in the AEGIS, GOODS-North, COSMOS and UDS fields Momcheva et al. 2016), while the solid line highlights the mean MS line from Speagle et al. (2014) in each redshift range. The shaded area corresponds to the 0.3 dex scatter of the MS and the dashed line to ±1 dex. and includes measurements below the MS at z = 1 − 1.6. The interconnected science goals of the PHIBSS2 survey are as follows.
1. Firstly, we aim to follow the evolution of the molecular gas fraction and the depletion time in normal MS star-forming galaxies at different epochs to establish quantitatively whether the evolution of the cosmic SFR is mostly driven by the available molecular gas reservoirs.
2. Secondly, we aim to characterise the dependence of the gas fraction and the depletion time on the sSFR to compare the galaxy population on, above, and below the MS. Quantifying this dependence will allow us to investigate whether "out of equilibrium" systems above the MS are fundamentally different from MS galaxies, how the quenching of star formation occurs below it, and in future studies to estimate gas fractions and depletion times directly from SFR data.
3. We futher intend to quantify the dependence of the gas fraction on the stellar mass to test feedback and quenching models. PHIBSS2 indeed enables to confirm and quantify the decrease of the gas fraction with stellar mass uncovered by PHIBSS over a broader range of stellar masses log(M /M ) = 10 − 11.6 spanning from the stellar feedback regime to the quenching regime.
4. Subsequently, we want to test the impact of AGNs, environment, and morphology on quenching using a purely mass-selected sample above the Schechter mass. PHIBSS and PHIBSS2 together indeed provide a large enough sample of about 50 star-forming galaxies with log(M /M ) > 10.8 to test how gas properties correlate with the presence of an AGN, environment, and morphological indicators such as the bulge-to-total ratio and the stellar mass surface density.

5.
We also plan to search for molecular outflows to test stellar and AGN feedback models. While powerful galactic winds of ionized gas are found to be ubiquitous amongst starforming galaxies at high-redshift (Pettini et al. 2000;Weiner et al. 2009;Genzel et al. 2011;Newman et al. 2012;Förster Schreiber et al. 2014), detecting molecular gas outflows is still challenging and often limited to nearby quasars and ultra-luminous IR galaxies (Feruglio et al. 2010;Sturm et al. 2011;Geach et al. 2014;Cicone et al. 2014). With more than 180 spectra from PHIBSS and PHIBSS2, we will be able to use deep stacking techniques to detect molecular outflows both in the stellar and in the AGN feedback regimes.
6. We plan to determine the molecular gas distribution and kinematics from sub-arcsecond follow-ups of selected targets to establish spatially resolved KS relations, rotation curves, and velocity dispersion maps at different redshifts. In addition to galaxy-averaged measurements, PHIBSS2 indeed includes spatially resolved molecular gas observations of selected targets with NOEMA and ALMA that can be compared to the stellar, SFR and ionized gas distributions from complementary observations. 7. Lasty, we aim to probe the physical state of the gas from the CO line excitation at different M , SFR, and redshifts. Although recent observations (Ivison et al. 2011;Sharon et al. 2016;Dessauges-Zavadsky et al. 2017) indicate that the CO spectral energy distributions (SEDs) of star-forming galaxies Article number, page 3 of 28 A&A proofs: manuscript no. freundlich_phibss2 at high redshift are similar to but slightly more excited than that of the Milky Way, measurements are still scarce. The combined PHIBSS and PHIBSS2 sample will constitute a benchmark to more systematically investigate the gas excitation at high redshift with additional CO transitions. Followups to probe dense gas tracers such as HCN will further help characterise the conditions ruling star formation.
The first three points are addressed in Genzel et al. (2015) and Tacconi et al. (2018), whose scope extends beyond the PHIBSS and PHIBSS2 programs as these articles use a wealth of molecular gas data, combining both CO and dust measurements in order to yield quantitative scaling relations for the molecular gas fraction and the depletion time and to eliminate concerns about the CO to molecular gas mass conversion factor. The PHIBSS2 program comprises approximately 1068 hours of onsource data gathered by the IRAM NOEMA interferometer over four years, and participates in current efforts to better understand star-forming galaxies and their evolution. It is indeed one element among different large interconnected surveys, including KMOS-3D (Wisnioski et al. 2015), Large Binocular Telescope (LBT) LUCI spectroscopic observations , SINS/zC-SINF (Förster Schreiber et al. 2006, 2014Genzel et al. 2006Genzel et al. , 2011, MUSE imaging and kinematics (Contini et al. 2016), Hubble Space Telescope (HST) imaging with CAN-DELS (Grogin et al. 2011;Koekemoer et al. 2011), and 3D-HST grism spectroscopy Momcheva et al. 2016); many of these surveys draw their samples from the same parent population.

Sample selection
The PHIBSS2 sample was drawn from large panchromatic imaging surveys with good spectroscopic redshifts and wellcalibrated stellar masses, SFR, and HST morphologies, namely the North field of the Great Observatories Origins Deep Survey (GOODS-N; R.A. = 12h36m, DEC. = 62 • 14 ; Giavalisco et al. 2004), the Cosmic Evolution Survey (COSMOS; R.A. = 10h00m, DEC. = 02 • 12 ; Scoville et al. 2007;Laigle et al. 2016), and the All-Wavelength Extended Groth Strip International Survey (AEGIS; R.A. = 14h17m, DEC. = 52 • 30 ; Davis et al. 2007;Noeske et al. 2007). These three fields constitute well-understood parent samples with excellent multi-band ancillary data from the X-ray to the radio, which enables us to quantitatively relate the PHIBSS2 sample to a much larger census of typical star-forming galaxies. Selected galaxies in the GOODS-N and AEGIS fields are part of the 3D-HST sample Momcheva et al. 2016) while those in the COSMOS field were taken from the zCOSMOS survey (Lilly et al. 2007(Lilly et al. , 2009). The stellar masses across the different parent samples are determined through SED modelling based on a Chabrier initial mass function (IMF). Such modelling uses standard assumptions on the star formation histories and the dust attenuation within these galaxies (Erb et al. 2006;Förster Schreiber et al. 2009;Wuyts et al. 2011a). The SFRs are estimated following a combination of UV and IR luminosities to account for both unobscured and dust-embedded star formation according to Eq. 1 of Wuyts et al. (2011a), which is based on Kennicutt (1998a) and corrected for a Chabrier IMF. The total IR luminosity is extrapolated from Spitzer 24 µm assuming a single luminosity independent far-infrared (FIR) SED following Wuyts et al. (2008). The typical systematic uncertainties on both the stellar mass and the SFR are conservatively estimated at about 0.2 dex (e.g. Wuyts et al. 2011a;Whitaker et al. 2014;Roediger & Courteau 2015).
The PHIBSS2 targets are chosen to have deep HST imagery, high-quality spectroscopic redshifts, as well as good rest-frame UV and Herschel PACS and/or 24 µm observations for the SFR estimate. We aimed at a homogeneous coverage of the MS and its scatter in the M -SFR plane, with log(M /M ) ≥ 10.1 and SFR ≥ 3.5 M yr −1 to assure a high probability of detection for reasonable on-source integration times. As shown in Fig. 1, this coverage excludes the lower-mass end of the MS but fully covers the MS above the cuts in stellar mass and SFR. We applied no morphological selection and the relatively high masses surveyed ensure that the selected galaxies have metallicities close to solar metallicity, which minimises the metallicity-induced variations of the CO-to-molecular-gas-mass conversion factor. We further selected galaxies with Hα and, when possible, Hβ and [OIII] emission free from atmospheric line contamination for ionized gas kinematics and metallicity determinations. Considering Poisson errors and our past experience with PHIBSS, we required at least ten measurements in any given part of the parameter space, for example below log(M /M ) = 10.4 at z = 0.5−0.8 or above the Schechter mass in each redshift bin, to establish well-determined average gas fraction and depletion time. As shown by Tacconi et al. (2018) in their Appendix, establishing the redshift, MS-offset, and stellar mass dependencies of the gas fraction and depletion time requires at least 40 sources in more than two redshift slices and a coverage of over 1 dex in both stellar mass and MS offset. Such constraints on the sample size further allow us to test the impact of AGNs and environment, as we can split the sample into mass-matched sub-samples with an expected AGN fraction of 25-50% (Mullaney et al. 2012;Juneau et al. 2013) while 20 to 30 % of the targets display interacting satellites.

Implementation with the NOEMA interferometer
The CO observations were carried out between June 2014 and June 2017 with the IRAM Plateau de Bure millimeter interferometer and its NOEMA upgrade (Guilloteau et al. 1992;Cox 2011;Schuster 2014). The interferometer comprised six 15-m antennas at the beginning of the project and was upgraded to seven and eight antennas in September 2014 and April 2016, enabling us to reach higher sensitivities. Table 2 summarises the observations for the z = 0.5 − 0.8 sample, including the interferometer's configurations, the total integration time t int over all configurations included for a given galaxy, and the beam size. At this redshift, we observed the 12 CO(2-1) rotational transition (rest-frame frequency 230.538 GHz), shifted into the 2-mm band, with the interferometer in compact 'C' and 'D' configurations. Given the integration times, these configurations yield beam sizes in the range 1 −5 . Galaxies L14EG008, XA54, and XG55 were also observed in more extended configurations for higher-resolution follow-ups, which will be presented in a future paper. The integration time per target was initially determined from the expected CO flux estimated from the SFR assuming a linear KS relation, requiring a signal-to-noise ratio (S/N) of at least 4, and later adapted in real time, galaxy per galaxy, during the observation campaign to ensure secure detections. One of the main goals of PHIBSS and PHIBSS2 is indeed to provide molecular gas estimates for a sample of star-forming galaxies covering different stellar masses and MS offsets in a way that is as unbiased as possible.
Given the large number of observed hours, the weather conditions varied from excellent to very bad, with system temperatures ranging between 100 and 500 K depending on atmospheric conditions and season. We alternated source observa-Article number, page 4 of 28 tions with bright quasar calibrators every 20 minutes to measure and remove the instrumental and atmospheric phase and amplitude fluctuations with time. The instrument response per frequency was further measured once per observational track on a strong quasar without spectral lines. The absolute flux scale was derived from secondary flux calibrators (MWC349 and LkHα101), whose fluxes are regularly measured using Jupiter satellites or planets. We mostly used receivers of temperature T rec ∼ 35 − 70 K in band 2, but also the latest NOEMA receivers with better T rec ∼ 30 − 50 K in the last 1.5 years. The observations were carried out using dual polarization in the Single Side Band mode and we used the Widex backend correlator with 3.6-GHz coverage per polarization. The source integration times lie around 7 hours to achieve similar S/N under different weather conditions, except for the high-resolution follow-ups to be presented later, for which the integration times can reach about 30 hours. The data were calibrated using the CLIC package of the IRAM GILDAS software and further analysed and mapped in its MAPPING environment. The spectra were analysed with the CLASS package within GILDAS.
As for the PHIBBS survey and the data compilation used in Tacconi et al. (2018), the data from PHIBSS2 are to be made publicly available at the end of the reduction and interpretation procedure 1 .

Results
3.1. The PHIBSS2 sample at z = 0.5 − 0.8 The PHIBSS2 z = 0.5 − 0.8 sample of 61 near-MS star-forming galaxies which is the focus of this article is presented in Table 1 and Figs. 1 and 2. Appendix A further presents HST I-band images of these galaxies, while Sect. 3.4 presents their sizes and bulge-to-total (B/T) luminosity ratios. As can be seen in the HST I-band images and indicated in Table 1, the sample comprises 49 disc-dominated and 12 bulge-dominated galaxies (80% and 20% of the sample, respectively), 36 of them having clear spiral or ring features (59%), which are highlighted in the residual maps. This repartition agrees very well with that found by Tacconi et al. (2013) for the PHIBSS sample and with larger HST imaging surveys (Wuyts et al. 2011b). A visual inspection also shows that 14 galaxies out of 61 (23%) harbour bars despite the intermediate redshift (Table 1). The relatively regular morphologies observed for most galaxies of the sample are compatible with them being isolated and not undergoing major mergers. Indeed, a visual inspection of the HST images indicates that only 4 galaxies out of 61 (7%) have both asymmetries and companions, which is comparable to the fraction of mergers from other MS studies (e.g. Tacconi et al. 2013;Wisnioski et al. 2015). Beyond the sample at z = 0.5−0.8 presented here, higher-redshift PHIBSS2 samples at z = 1 − 1.6 and z = 2 − 3 will be presented in future articles.

CO fluxes
Tables 2 and 3 summarise the PHIBSS2 CO(2-1) line observations at z = 0.5 − 0.8. In Table 3, we display the CO(2-1) line fluxes F(CO), which correspond to the mean value of three different estimates of the line intensity weighted by their respective uncertainties: (i) directly obtained from the spatially integrated spectrum over the velocity window centred on the peak emission that maximizes the flux; (ii) derived from a Gaussian fit to the spatially integrated spectrum, whose peak luminos-ity and FWHM are indicated in Table 2; and (iii) determined from the velocity-integrated line map (using the GO FLUX tool of GILDAS). The spatially averaged spectra and the Gaussian fits are displayed in Appendix A along with the HST I-band images. Amongst them, eight galaxies clearly display doublehorned profiles which are characteristic of thin rotating discs. The flux uncertainty dF(CO) is estimated from the RMS noise integrated over the full line width, leading to an integrated flux S/N of S/N = F(CO)/dF(CO). The dispersion between the three estimates of the line intensity is in most cases well below the quoted uncertainty dF(CO). In the few cases where there were significant discrepancies between the three estimates, we selected the most reliable one. As shown in Table 3, we detected the CO(2-1) line emission in 60 of the 61 galaxies of the z = 0.5 − 0.8 sample, which corresponds to a detection rate of 97%. Amongst these detections, 5 have low S/N and display a slight offset from the HST I-band image or an ambiguous spatially integrated spectrum: they are indicated as marginal in the table.
For the non-detected galaxy XB55 (GN-6666), we evaluate the RMS noise on the integrated line flux at σ F = 0.12 mJy.km.s −1 using where σ 30 is the noise per 30 km.s −1 -wide channel and ∆V the velocity width over which the signal is integrated when searching for the line, and quote F upper = 3σ F as the upper limit, which corresponds to the flux that should have been detected at S/N > 3 with a 50% probability (e.g. Masci 2011).

Molecular gas masses
Although the CO molecule only represents a small fraction of the total molecular gas mass and its lower rotational lines are almost always optically thick, observations of giant molecular clouds (GMCs) in the Milky Way have shown that the integrated line flux of its rotational lines could be used as a quantitative tracer of the molecular gas mass (Dickman et al. 1986;Solomon et al. 1987;Combes 1991;Young & Scoville 1991;Solomon & Barrett 1991;Dame et al. 2001;Bolatto et al. 2013). The intrinsic CO luminosity associated to any region of flux can be expressed as where F(CO) is the velocity integrated flux, ν rest the rest-frame frequency -230.538 GHz in the case of CO(2-1) -, and D L the luminosity distance (Solomon et al. 1997). Considering a certain J → J −1 CO line, the total molecular gas mass including a 36% correction to account for interstellar helium is then estimated as where α CO is the CO(1-0) luminosity-to-molecular-gas-mass conversion factor and r J1 = L CO(J→J−1) /L CO(1−0) the corresponding line ratio. The α CO conversion factor a priori depends on the average cloud density, the Rayleigh-Jeans brightness temperature of the CO transition, and the metallicity (Strong et al. 2004;Leroy et al. 2011;Genzel et al. 2012;Papadopoulos et al. 2012a;Bolatto et al. 2013;Sandstrom et al. 2013). In the Milky Way, its Article number, page 5 of 28 A&A proofs: manuscript no. freundlich_phibss2   Notes. a CO(2-1) integrated line flux and its uncertainty. b S/N = F(CO)/dF(CO). c Integrated CO(2-1) line luminosity as derived from Eq. 2. d Molecular gas mass, corrected by a factor 1.36 for interstellar Helium, using a Galactic CO-H 2 conversion factor α CO = 4.36 M /(K.km.s −1 .pc 2 ) and a CO ( dense star-forming clumps, nearby MS star-forming galaxies, and low-metallicity galaxies, estimates of the conversion factor based on virial masses, optically thin tracers of the column density, and diffuse gamma-ray emission stemming from the interaction between cosmic rays and interstellar medium (ISM) protons seem to converge towards a relatively uniform value α G = 4.36 ± 0.9 M /(K.km.s −1 .pc 2 ) including helium (Strong & Mattox 1996;Dame et al. 2001;Grenier et al. 2005;Bolatto et al. 2008;Abdo et al. 2010;Schinnerer et al. 2010;Leroy et al. 2011;Bolatto et al. 2013). As the CO emission in the z = 0.5−0.8 galaxies studied in this paper is likely to originate from virialized GMCs with mean densities of the same order of magnitude as their lower-redshift counterparts (Daddi et al. 2008(Daddi et al. , 2010aDannerbauer et al. 2009) and similar dust temperatures (Magnelli et al. 2009;Hwang et al. 2010;Elbaz et al. 2011), their conversion factor should be relatively close to the 'Galactic' conversion factor α G . But since the CO conversion factor increases with decreasing metallicity as the CO molecule gets more photo-dissociated (Wolfire et al. 2010;Bolatto et al. 2013), we do account for its metallicity dependence. From the different metallicity corrections proposed in the literature, we adopt the geometric mean of the recipes by Bolatto et al. (2013) and Genzel et al. (2012) as adopted by Genzel et al. (2015) and Tacconi et al. (2018): where log Z = 12 + log(O/H) is the metallicity on the Pettini & Pagel (2004) scale estimated from the mass-metallicity relation with b = 10.4 + 4.46 × log(1 + z) − 1.78 × (log(1 + z)) 2 (Genzel et al. 2015, and references therein). This metallicity correction leads to a mean α CO = 4.0 ± 0.3 M /(K.km.s −1 .pc 2 ) within the z = 0.5 − 0.8 sample.
The r 21 line ratio converts the observed CO(2-1) luminosity into the CO(1-0) luminosity for which the α CO conversion factor is calibrated. While a thermally excited transition in the Rayleigh-Jeans domain with r 21 = 1 has often been assumed to derive molecular gas masses (Combes et al. 2011Bauermeister et al. 2013;Tacconi et al. 2013), the CO(2-1) line could both be sub-thermally excited and require a Planck-correction, leading to r 21 < 1. In particular, Leroy et al. (2009) obtain values of r 21 between 0.6 and 1 within a sample of 18 nearby galaxies, with a typical value r 21 ∼ 0.8, while Dannerbauer et al. (2009) and Aravena et al. (2010) obtain r 21 ∼ 0.85 at z ∼ 1.5, and Papadopoulos et al. (2012b) around r 21 = 0.91 for a large sample of luminous and ultra-luminous IR galaxies in the local universe. Bothwell et al. (2013) further measure r 21 ∼ 0.84 within a sample of 40 luminous sub-millimitre galaxies in the range z = 1 − 4 while Daddi et al. (2015) find an average r 21 = 0.76 from a sample of four galaxies at z = 1.5. In the following we assume r 21 = 0.77, as also assumed by Genzel et al. (2015) and Tacconi et al. (2018).
The resulting values of the intrinsic CO(2-1) luminosity L CO(2−1) and the molecular gas mass M gas as well as the corresponding gas-to-stellar-mass ratio µ gas = M gas /M , gas fraction f gas = M gas /(M gas + M ) = µ gas /(1 + µ gas ), and depletion time t depl = M gas /SFR are displayed in Table 3. The relative uncertainty on the CO(2-1) line flux dF(CO)/F(CO) = 1/(S/N) is 30% on average, and as high as about 50%, which is transferred to the intrinsic CO luminosity L CO (2−1) . Considering the 30% uncertainty on the Galactic conversion factor α G ), the systematic difference up to 20% between the metallicity corrections of Bolatto et al. (2013) and Genzel et al. (2012) in the metallicity range of the z = 0.5 − 0.8 sample that reflects the scatter in the α CO -metallicity relation, and the more negligible 12% uncertainty on the r 21 line ratio from Daddi et al. (2015) leads to a systematic uncertainty of at least 50% on the final molecular gas masses. Figure 3 shows the distributions of µ gas , f gas , and t depl , comparing them with those obtained at z = 0 from the COLDGASS survey (Saintonge et al. 2011a,b) and at z = 1 − 2 with the first PHIBSS program . The gas-to-stellar-mass ratios µ gas range from 0.03, close to the detection limit, to 1.8, with a median of µ gas = 0.28 ± 0.04. The ranges for f gas and t depl are 0.03 − 0.64 and 0.11−3.82 Gyr, with median values of f gas = 0.22±0.02 and t depl = 0.84 ± 0.07 Gyr, respectively. These values are interme-Article number, page 9 of 28 A&A proofs: manuscript no. freundlich_phibss2 The molecular gas-to-stellar ratio µ gas and gas fraction f gas thus approximately probe the total gas fractions.
Noting from Figs. 1 and 2 that the mass distribution of the PHIBSS2 z = 0.5 − 0.8 sample differ from its CANDELS/3D-HST parent distribution, we further derive mass-matched median values for the molecular gas-to-stellar mass ratio, gas fraction, and depletion time. Following Catinella et al. (2010) and Saintonge et al. (2011a), we place galaxies in stellar mass bins of 0.2 dex width as in the central panel of Fig. 2 and assign as weight the ratio between the number of galaxies in the CANDELS/3D-HST parent sample within 1 dex of the MS line and that in the PHIBSS2 sample at z = 0.5 − 0.8 in each of these stellar-mass bins. Limiting ourselves to stellar masses above log(M /M ) ≥ 10.4 to avoid being affected by the sparsely populated bins below this value, the resulting mass-weighted medians are µ gas = 0.30 ± 0.04, f gas = 0.23 ± 0.02 and t depl = 0.84 ± 0.08 Gyr, which correspond well to the values expected from Tacconi et al. (2018) at the median stellar mass and redshift of the CANDELS/3D-HST parent sample with 10.4 < log(M /M ) < 11.8 and | log(δMS)| < 1 (respectively, 0.29, 0.22, and 0.89). However, we leave the detailed study of the influence of mass selection on the Tacconi et al. (2018) scaling relations and in particular on their zero points to future works.

Size and morphology
The radial distribution of the star-forming molecular gas in most nearby galaxies follows an exponential profile reminiscent of the stellar disc (e.g. Young & Scoville 1982;Scoville & Young 1983;Young 2000) while bulges are mostly made of old stars (e.g. Wyse et al. 1997;Zoccali et al. 2003;Freeman 2008). To address the influence of morphology on star formation and to separate the contribution of disc and bulge, we not only determine the total half-light radius of the galaxies of the PHIBSS2 z = 0.5 − 0.8 sample from single Sérsic fits but also decompose them as two-component bulge disc systems with the 2D morphology fitting code galfit (Peng et al. 2002(Peng et al. , 2010a. The fits are carried out on publicly available high-resolution (0.03 arcsec per pixel) HST Advanced Camera for Survey (ACS) images in the F814W I-band. This band is optimal for our study as it is available for all the galaxies of the sample and probes the blue young stellar population at z = 0.5 − 0.8 while avoiding the restframe UV light from very young stars. The disc is described by an exponential profile (Freeman 1970) where I d is the disc central density and R e its scale length, which is proportional to the disc half-light radius R d = 1.67835R e . The bulge is described by a Sersic (1968) profile:  2016) for the influence of the PSF, the weight map and the background subtraction on galfit models. Neighbouring nearby galaxies or satellites are fitted simultaneously with a single Sérsic model to account for their luminosity distribution.
One of the main difficulties when carrying out multicomponent fits with galfit is to avoid being trapped in a local χ 2 minimum depending on the initial guess instead of the global minimum (e.g. Häussler et al. 2007;Peng et al. 2010a;Bruce et al. 2012). Following Lang et al. (2014), we first build ten initial guesses from the least degenerate single Sérsic fits using an empirical analysis of noise-free two-component models: (i) we generate a grid of ideal, noise-free two-component bulge disc models with different B/T and R b /R d ; (ii) we obtain their global Sérsic indices and half-light radii with galfit using no PSF and a weight map corresponding to ideal Poisson noise; (iii) we estimate the B/T associated to a series of ten values of R b /R d for each galaxy from its Sérsic index using the result of the previous step; and (iv) we determine the corresponding bulge and disc to be used in the ten initial guesses for that galaxy. Noting that not all single Sérsic fits yield physical half-light radii, we also build initial guesses from the pure bulge and pure disc fits with different values of B/T and R b /R d (10 values of R b /R d between 0.1 and 1, B/T = 0.1 and 0.5 when using the pure disc model, B/T = 0.5 and 0.9 when using the pure bulge model), leading to a total of 52 galfit runs per galaxy for the bulge disc model, including the pure-bulge and pure-disc models. The best-fit model is that with the lowest reduced χ 2 , casting away models where the bulge is implausibly small (R b < 0.1 pixel) or larger than the disc (R b > R d ); except for L14GN025 (GN4-36596) where we release this latter condition as the low surface brightness of the stellar halo in which the disc is embedded makes all models with R b < R d unsatisfactory. We note that as in Lang et al. (2014), two-component decompositions are preferred over single Sérsic fits for about two thirds of the sample, namely for 37 galaxies out of 61 (61%). The best-fit models are displayed with the I-band images in Appendix A. Table 4 displays the results of both the single Sérsic and the two-component fits, with the half-light radius R Sersic , Sérsic index n Sersic , axis ratio q Sersic resulting from the single Sérsic fits, the disc and bulge half-light radii R d and R b of the two-component fits, as well as the corresponding bulge-to-totalluminosity ratio B/T for the PHIBSS2 sample at z = 0.5 − 0.8. The Sérsic index n Sersic is constrained to be between 0.2 and 4, and we note that n Sersic = 4 often coincides with relatively large values of the half-light radius R Sersic that are usually corrected with the two-component fits. The bulge-to-total-luminosity ratio is estimated from the two-component model as where F b and F d are the total fluxes associated to the bulge and disc components, respectively, and m b , m d are the associated magnitudes. Assuming that the uncertainties on the single-Sérsic fit parameters only depend on the S/N, we transpose the results of van der Wel et al. (2012) to band I and conservatively evaluate the uncertainties on R Sersic , n Sersic and q Sersic at about 20% given the magnitude of the sources. We note that Bruce et al. (2012) find that the background subtraction induces errors of about 5% for n Sersic and 10% for R Sersic , to which we should add the uncertainties introduced by the PSF choice and those intrinsic to galfit such as the choice of the weight matrix. From Lang et al. (2014), we infer a 0.05 uncertainty on B/T. Figure 4 shows the distributions of the I-band R Sersic , R d , R b , and B/T within the sample. The parent CANDELS/3D-HST measurements in the H-band (van der Wel et al. 2012; Lang et al. 2014) are shown for comparison in the case of R Sersic and B/T. As most B/T = 1 cases correspond to galaxies harbouring clear spiral features that are not well accounted for by the cylindrically symmetric models adopted here, we do not show them in the middle and right panels. More generally, asymmetries and structures such as spiral arms, rings, and bars may introduce biases in the B/T measurements. Accounting for such features would require a caseby-case study that is beyond the scope of this article; here we favour a systematic approach to the determination of B/T compatible with large datasets, in line with other surveys (e.g. van der Wel et al. 2012; Lang et al. 2014;Contini et al. 2016). Compared to the H-band measurements, the I-band half-light radii are more spread out with a higher median value while half of the sample are found to be discs with very faint or non-existent bulges (B/T < 0.1). These trends relate to the lower characteristic wavelength of the I-band, which traces younger stars and hence highlights the disc relative to the H-band images.
Article number, page 11 of 28 A&A proofs: manuscript no. freundlich_phibss2 Notes. a Half-light radius, Sérsic index and axis ratio of the single Sérsic fits in the F814W I-band images. Sérsic indices followed by a cross (+) correspond to cases where the single-Sérsic fit is better than the two-component fit (39% of the sample). b Half-light radii of the n = 1 disc and n = 4 bulge components of the two-component fits in the I-band images. c Bulge-to-total luminosity ratios defined from the two-component fits using Eq. 8. Marginal detection; † Non-detection.
Article number, page 12 of 28

Molecular gas fraction and depletion time
The PHIBSS2 legacy program provides the largest sample todate of CO molecular gas measurements at intermediate redshift with its 60 CO(2-1) detections in the range z = 0.5 − 0.8. As shown in Sect. 3.3, the median molecular gas masses, gas-tostellar-mass ratios, gas fractions, and depletion times obtained for the PHIBSS2 z = 0.5 − 0.8 sample are in excellent agreement with the scaling relations established by Genzel et al. (2015) and Tacconi et al. (2018) on a much larger sample of about 1400 sources in the range z = 0 − 4.5 including both CO and dust observations. These relations, which characterise the dependence of the molecular gas-to-stellar-mass ratio and the depletion time on redshift, stellar mass, MS offset, and galaxy size, constitute the main contribution of the PHIBSS2 program aimed at understanding star formation processes on the MS across cosmic time. The molecular gas-to-stellar-mass ratio µ gas and the depletion time t depl are written as power-law functions of redshift, stellar mass, distance from the MS, and galaxy size such that their logarithms yield In particular, while part of the scatter of the MS is due to the stochasticity of the cosmic accretion, the individual histories and environment, morphology, and fundamental physical quantities of star-forming galaxies, such as their molecular gas fraction and depletion time, vary progressively with δMS. This variation has already been highlighted in different studies (e.g. Schiminovich et al. 2007;Wuyts et al. 2011b;Saintonge et al. 2011bSaintonge et al. , 2012Magdis et al. 2012a;Huang & Kauffmann 2014;Genzel et al. 2015;Tacchella et al. 2016a), but Genzel et al. (2015) and Tacconi et al. (2018) quantify it precisely through the coefficient C. Tacconi et al. (2018) further add a non-linearity in the redshift evolution of the molecular gas fraction to follow the observations more closely, namely considering a redshift evolution of the form B log(1 + z) − F β instead of the linear trend of Eq. 9, where F and β are additional constants. We define the residual when the redshift dependence is subtracted from the original quantity log(y). We determine δt depl and δµ gas for the galaxies of the PHIBSS2 z = 0.5 − 0.8 sample, subtracting the redshift dependence obtained by Tacconi et al. (2018), and study their dependence on δMS, δM, and δR. As can be seen in Fig. 5, these dependences are in good agreement with the scaling relations of Tacconi et al. (2018), although with much bigger uncertainties due to our more limited sample. Coefficients C and D were obtained through simultaneous linear fits of the redshift-subtracted quantities log(δy) as a function of log(δMS) and log(δM) while E results from a single linear fit of the residual (log(δy) − C log(δMS) − D log(δM)) as a function of log(δR). The uncertainties are evaluated by assuming a 0.3 dex uncertainty on µ gas and t depl and 0.2 dex uncertainties on δMS, δM, and δR. This illustrates Appendix A of Tacconi et al. (2018), which shows from model data sets driven by the actual data that the MS offset and stellar mass dependences of the molecular-gas-tostellar-mass ratio and depletion time can be recovered from data sets with N 40 sources as long as the coverage in δMS and δM exceeds 1 dex -which is the case here.

Kennicutt-Schmidt relation
In Fig. 6, we plot the KS relation between SFR and molecular gas mass surface densities Σ SFR = 0.5 SFR/πR 2 Sersic and Σ gas = 0.5 M gas /πR 2 Sersic within the z = 0.5 − 0.8 PHIBSS2 sample. A linear least-square fit to the data yields a KS exponent N = 1.02 ± 0.08 assuming 0.3-dex uncertainties in both SFR and molecular gas surface densities. This strikingly linear relation with Pearson correlation coefficient r = 0.94 corresponds to a uniform depletion time of t depl = 0.82 Gyr in line with the Tacconi et al. (2018) scaling relations, the residual scatter being 0.24 dex. We also tested definitions of Σ SFR and Σ gas using the disc radius R d instead of R Sersic , yielding similar results. The main contributor to the 0.24 dex scatter may be the different evolutionary stages of the molecular clouds within galaxies and their dynamical environment (e.g. Lada et al. 2010;Lombardi et al. 2010;Onodera et al. 2010;Schruba et al. 2010;Murray et al. 2010;Murray 2011;Zamora-Avilés et al. 2012;Zamora-Avilés & Vázquez-Semadeni 2014;Meidt et al. 2013;Davies et al. 2014;Kruijssen & Longmore 2014;Utomo et al. 2015;Kruijssen et al. 2018). Alternatively, regions within a single galaxy could have different star-formation efficiencies (e.g. Freundlich et al. 2013;Cibinel et al. 2017) and the conversion factors used to determine the molecular gas mass and the SFR may also vary from region to region or between galaxies (e.g. Israel 1997;Bolatto et al. 2013). Furthermore, observations in the Milky Way and nearby galaxies reveal that the properties of the molecular gas in GMCs vary considerably from the disc to the central region of a galaxy, in particular in the presence of strong bars (e.g. Oka et al. 2001;Regan et al. 2001;Jogee et al. 2005;Shetty et al. 2012;Kruijssen & Longmore 2013;Colombo et al. 2014;Leroy et al. 2015;Freeman et al. 2017). This variety, which is also expected for the galaxies of the PHIBSS2 sample, is likely to contribute to the scatter in the KS relation since Σ gas and Σ SFR do not always probe the same regions within a galaxy.
In the absence of separate size estimates for the SFR and molecular gas distributions, we use the half-light radius obtained from a single Sérsic fit R Sersic to estimate both surface densities, which are consequently not independent from each other. To ensure that the striking correlation between Σ SFR and Σ gas from Fig. 6 does not stem from the dependence between the two variables, we study the KS relation that would be obtained for non-correlated uniform distributions of log(M gas /M ) and log(SFR/M .yr −1 ) between the extrema of the PHIBSS2 z = 0.5 − 0.8 sample. Figure 7 shows that such distributions would yield a much greater scatter of about 0.50 dex and a less linear relation. While the figure shows the result for one such distribution, we confirmed the trend both in slope and scatter by reproducing the experiment 1000 times, obtaining slopes, Pearson correlation coefficients, and scatters of 0.6 ± 0.1, 0.62 ± 0.08, and 0.48 ± 0.04, respectively. We also note that sticking to the molecular gas mass and the SFR, which are independent variables unlike their surface densities, yields a clear correlation with a slope of 0.81±0.14, a Pearson coefficient of 0.77, and a residual standard deviation 0.18 dex: the striking KS relation we obtain in Fig. 6 does not result from an artificial correlation induced by the dependency of both surface densities on galaxy size. We do Article number, page 13 of 28 A&A proofs: manuscript no. freundlich_phibss2 Dependence of the residual molecular depletion time and gas-to-stellar-mass ratio after subtraction of the redshift dependence on the distance from the MS, stellar mass, and disc size within the PHIBSS2 z = 0.5 − 0.8 sample, compared to the dependences derived from the scaling relations obtained by Tacconi et al. (2018). We assume that the different variables can be separated as in Eqs. 9 and 10, and plot each dependency independently. The black solid lines and the values indicated on the plots refer to the best fits for the z = 0.5 − 0.8 subsample, while the green contours and the dashed lines correspond to the comprehensive data set studied by Tacconi et al. (2018) and its fitting formulae (C = −0.44 ± 0.04, D = +0.07 ± 0.05 and E = +0.12 ± 0.12 for t depl and C = +0.54 ± 0.03, D = −0.32 ± 0.03 and E = +0.09 ± 0.09 for µ gas ).
however notice from Fig. 7 that part of the correlation in the KS diagram is due to our selection of MS galaxies excluding starbursts and quenched galaxies and the fact that both surface densities are not independent variables. These issues are relevant for most KS studies and are not specific to the study presented here.

Star formation and morphology
To address how morphology affects star formation within the PHIBSS2 z = 0.5 − 0.8 sample, we investigate how global physical parameters such as the stellar mass M , the molecular gas mass M gas , and the SFR, as well as derived quantities like the sSFR, the molecular gas depletion time t depl , and the gas-tostellar mass ratio µ gas , depend on the bulge-to-total ratio B/T and the total stellar surface density Σ = 0.5M /πR 2 Sersic . Shi et al. (2011) notably show from a large sample of galaxies at different redshifts that the depletion time is a decreasing function of Σ , which can be understood both in terms of the stellar contribution to the gravitational potential in which stars form and in terms of disc hydrostatic pressure acting on star-forming regions. A high disc pressure indeed enhances the production of H 2 molecular gas from HI atomic gas and hence contributes to balance stellar feedback (Blitz & Rosolowsky 2004;Schaye & Dalla Vecchia 2008;Shi et al. 2011). To quantify the correlations between the different parameters with B/T and Σ , we carry out linear least-square fits with errors on both axes, determine the Pearson correlation coefficient r between them, and indicate the scatter σ of the residuals. B/T and Σ are themselves correlated, with a Pearson correlation coefficient of r = 0.67. As mentioned in Sect. 3.4, most fits with B/T = 1 correspond to cases where the inner structure of the galaxy includes spiral arms not well accounted for; we therefore exclude these points from the correlations. As shown in Fig. 8, we find that while the stellar mass increases with B/T and Σ (respectively with r = 0.43 and 0.31), the SFR and the molecular gas mass do not seem to depend on these parameters (with |r| 0.10). Derived quantities are consistent with these trends: the sSFR and µ gas decrease both with B/T and Σ (respectively with r = −0.  (Saintonge et al. 2011a and the grey triangles to PHIBSS ). The black solid line corresponds to a linear least-square fits to the data points; the dashed lines to a uniform depletion time corresponding to the best-fitting value on the KS diagram. The Pearson correlation coefficient is 0.94 while the standard deviation from the linear fit is 0.24 dex.
advocating relatively robust correlations. The decrease of the sSFR with B/T, which was also observed at low-redshift by Saintonge et al. (2012), can be either interpreted as a decreasing sSFR with bulge growth, or as a consequence of the fact that B/T traces the fraction of stars that formed early and are now part of the bulge while the sSFR traces on the contrary the fraction of stars that formed recently. Similarly, the total moleculargas-to-stellar-mass ratio and the corresponding gas fraction decrease with B/T and Σ in accordance to low-and high-redshift measurements where morphology is probed by the concentration parameter and the Sérsic index (Saintonge et al. 2011a;Papovich et al. 2015). Assuming an evolutionary sequence from small to high B/T for the same objects, the fact that the molecular gas mass does not vary with B/T and Σ suggests an ongoing supply of fresh molecular gas while the stellar bulge assembles, which could stem from mergers, infall from the cosmic web through streams of cold gas penetrating inside the hot circumgalactic medium (Dekel et al. 2009a), or from efficient transformation from atomic to molecular gas owing to the pressure increase (Blitz & Rosolowsky 2004). This continuing supply of gas would be reflected on the disc gas-to-stellar-mass ratio µ gas,disc = M gas /M ,disc , which neither correlates with B/T nor Σ (|r|< 0.05). Without invoking an evolutionary sequence, the absence of correlation for the molecular gas mass, the SFR, and Contrarily to morphological quenching scenarios (Martig et al. 2009) and observations in the nearby universe (Saintonge et al. 2011b), we do not observe any variation of the depletion time with B/T or Σ (|r|< 0.05). This variation is expected to be more pronounced when the gas fraction drops below 20% (Martig et al. 2009;Gobat et al. 2018), so we separately searched for it in galaxies with f gas < 20% but did not observe any significant variation of the depletion time with B/T or Σ . Part of this negative result may come from the fact that Gobat et al. (2018) rely on dust observations encompassing both molecular and atomic gas, while we only have access to the molecular gas. When B/T increases, more gas may remain atomic instead of molecular as the bulge stabilises the disc against gravitational collapse and fragmentation. This means that the total depletion time including both molecular and atomic components may increase without any increase of the molecular gas depletion time. More importantly, Gobat et al. (2018) focus on quenched red and dead galaxies well below the MS while PHIBSS2 galaxies are precisely on and around the MS. By selecting star-forming galaxies, we may exclude those with high depletion times. Furthermore, although our sample does include bulge-dominated galaxies, those are still on the MS and are therefore potentially atypical with relatively high SFR. For example, they could have become bulge-dominated from mergers or violent disc instabilities recently, both processes also being able to trigger star formation. Morphological quenching and compaction events take time to settle down (Gobat et al. 2018;Dekel et al. 2019, in prep.) and may therefore not be observed in the recent bulge-dominated galaxies of our sample.

Conclusion
This paper presents the strategy and the z = 0.5 − 0.8 results of the PHIBSS2 survey, a four-year legacy program with the IRAM NOEMA interferometer designed to investigate early galaxy evolution from the perspective of the molecular gas reservoirs. This survey builds upon the successful PHIBSS program , which uncovered high gas fractions near the peak epoch of star formation and showed that the cosmic evolution of the SFR was mainly driven by the molecular gas reservoirs. The PHIBSS and PHIBSS2 surveys probe a representative sample of star-forming MS galaxies drawn from well-studied parent catalogues in the COSMOS, AEGIS, and GOODS-North cosmological deep fields. While PHIBSS focused on galaxies at z = 1.2 and 2.2 on and above the MS, PHIBSS2 significantly enlarges the sample by probing the build-up epoch at z > 2, the winding-down of star formation at z < 0.8, and galaxies below the MS at z = 1−1.6. It aims at homogeneous coverage of the MS in the M -SFR plane without morphological selection (Figs. 1 and 2). With a total of more than 120 sources, PHIBSS2 significantly adds to the number of molecular gas observations above z = 0.5. Together with PHIBSS, it thus provides a benchmark sample of near MS galaxies at different redshifts with molecular gas measurements, which can be used for further CO and dust continuum follow-ups at high resolution with ALMA and NOEMA as well as for other complementary observations.
In this paper we present the CO(2-1) molecular gas observations obtained at z = 0.5 − 0.8 as part of the PHIBSS2 survey, reporting 60 detections from a sample of 61 galaxies (Tables 1 and 2). We determine the molecular gas masses, gas fractions, gas-to-stellar-mass ratios, and depletion times of these galaxies and carry out single Sérsic and two-component bulge disc fits with the 2D morphology fitting code galfit to obtain the half-light radii of the galaxies and their bulge and disc components as well as their bulge-to-total-luminosity ratios and molecular gas mass and SFR surface densities. The molecular gas-to-stellar-mass ratio, gas fraction, and depletion time, respectively, yield values in the ranges 0.03 − 1.79, 0.03 − 0.64, and 0.11 − 3.82 Gyr with medians µ gas = 0.28 ± 0.04, f gas = 0.22 ± 0.02, and t depl = 0.84 ± 0.07 Gyr (Table 3 and Fig. 3). These values are consistent with the observed increase of the gas fraction and slight decrease of the depletion time with redshift Genzel et al. 2015;Tacconi et al. 2018). They are indeed in excellent agreement with the scaling relations of the depletion time and the gas fraction as a function of stellar mass, offset from the MS, and galaxy size established by Tacconi et al. (2018) within a much more comprehensive sample of about 1400 galaxies between z = 0 and z = 4. 6 (Fig. 5). We show that the Kennicutt-Schmidt relation between molecular gas and SFR surface densities within our sample is strikingly linear (Figs. 6 and 7), which argues in favour of uniform star-formation timescales within galaxies at any given epoch. In terms of morphology, we study the dependence of different global parameters including the depletion time and the molecular gas fraction on the bulge-to-total ratio B/T and the stellar surface density Σ (Table 4 and Fig. 8). In particular, the total molecular gas mass, the SFR, the disc stellar mass, and the disc molecular gas fraction do not seem to depend on either B/T or Σ . This either suggests an ongoing supply of fresh gas to the disc while the stellar bulge assembles or that star formation proceeds irrespectively of the past history of star formation traced by B/T. We find no strong evidence for morphological quenching, which we would expect to manifest as a dependence of the molecular gas depletion time on B/T and Σ . Our sample, however, only focuses on star-forming galaxies within the scatter of the MS; probing morphological quenching might require including galaxies well below it. Therefore, the analysis presented here should not be interpreted as evidence against morphological quenching in general.   CO spectrum Article number, page 28 of 28