The Sami Galaxy Survey: stellar populations of passive spiral galaxies in different environment

We investigate the stellar populations of passive spiral galaxies as a function of mass and environment, using integral field spectroscopy data from the Sydney-AAO Multi-object Integral field spectrograph Galaxy Survey. Our sample consists of $52$ cluster passive spirals and $18$ group/field passive spirals, as well as a set of S0s used as a control sample. The age and [Z/H] estimated by measuring Lick absorption line strength indices both at the center and within $1R_{\rm e}$ do not show a significant difference between the cluster and the field/group passive spirals. However, the field/group passive spirals with log(M$_\star$/M$_\odot)\gtrsim10.5$ show decreasing [$\alpha$/Fe] along with stellar mass, which is $\sim0.1$ dex smaller than that of the cluster passive spirals. We also compare the stellar populations of passive spirals with S0s. In the clusters, we find that passive spirals show slightly younger age and lower [$\alpha$/Fe] than the S0s over the whole mass range. In the field/group, stellar populations show a similar trend between passive spirals and S0s. In particular, [$\alpha$/Fe] of the field/group S0s tend to be flattening with increasing mass above log(M$_\star$/M$_\odot)\gtrsim10.5$, similar to the field/group passive spirals. We relate the age and [$\alpha$/Fe] of passive spirals to their mean infall time in phase-space; we find a positive correlation, in agreement with the prediction of numerical simulations. We discuss the environmental processes that can explain the observed trends. The results lead us to conclude that the formation of the passive spirals and their transformation into S0s may significantly depend on their environments.

1. INTRODUCTION Stellar populations of nearby galaxies allow us to better understand the formation histories of galaxies. Red galaxies, which are generally non star-forming, are more likely to be spheroid dominated, whereas blue galaxies, young and star-forming, are more likely to be disk dominated, and to have spiral arms (e.g. Humason 1936;Fioc & Rocca-Volmerange 1999;Bershady et al. 2000;Mignoli et al. 2009). There is however a population of galaxies that bridges both classes: passive spirals are red and quiescent, yet have prominent spiral patterns typical of starforming galaxies (e.g. van den Bergh 1976;Wilkerson 1980;Bothun & Sullivan 1980;Phillipps 1988;Cayatte et al. 1994). After the discovery of 'anemic' spiral galaxies in the Virgo cluster by van den Bergh (1976) and a significant number of passive spirals with apparently no/weak sign of ongoing star formation have been found minapak@kasi.re.kr in all environments, both at low and high redshift. The formation and evolution of these galaxies have received considerable attention observationally and theoretically (e.g. Couch et al. 1998;Dressler et al. 1999;Poggianti et al. 1999;Bekki et al. 2002;Goto et al. 2003;Yamauchi & Goto 2004;Moran et al. 2006;Lee et al. 2008;Mahajan & Raychaudhury 2009;Wolf et al. 2009;Masters et al. 2010;Fraser-McKelvie et al. 2016;Fraser-McKelvie et al. 2018;Pak et al. 2019). Despite this large number of studies, several questions still remain debated, such as (1) the origin(s) of passive spirals, (2) physical processes responsible for shutting down star formation without destroying their spiral structures, and (3) evolutionary connections with S0s.
The existence of passive spirals may be the evidence for the morphological transformation of spirals into S0s. The numerical simulations from Bekki et al. (2002) show how cluster environmental quenching processes can transform spirals into S0s, passing through an intermediate passive spiral phase. The spiral arm structures fade over several Gyrs, after the gas is stripped. However, they also claim that the passive spirals are found anywhere from galaxies in isolation to the centers of clusters, and hence that no single mechanism can completely explain their origin. Goto et al. (2003) suggested that the formation of passive spirals in the intermediate to high-density environments is closely related with cluster environmental effects: ram pressure stripping (Gunn & Gott 1972), harassment (Moore et al. 1999), thermal evaporation (Cowie & Songaila 1977), strangulation (Larson et al. 1980), galaxy-galaxy interactions including major (Toomre & Toomre 1972) and minor (Walker et al. 1996) mergers and tidal interactions. Secular evolution possibly caused by a bar is another possible mechanism for quenching spiral galaxies (Kormendy & Kennicutt 2004;Athanassoula 2013), which may convert them into S0s. Bars are common structures in disk galaxies in the local universe. Recent work on the bars of nearby disk galaxies suggests that the bar fraction is up to ∼ 50% in the optical bands (Marinova & Jogee 2007;Reese et al. 2007; Barazza et al. 2008). The fraction rises to ∼ 70% in near-infrared studies (Knapen et al. 2000;Menéndez-Delmestre et al. 2007). While all of these devoted studies have drawn attention to passive spirals, it is still under debate which is the dominant pathway of evolution from the passive spirals to S0s.
To find the evolutionary connections between passive spirals and S0s in the perspective of stellar populations, Pak et al. (2019) investigated nine passive spirals using the Calar Alto Legacy Integral Field Area (CALIFA) survey (Sánchez et al. 2012;Husemann et al. 2013). When comparing stellar populations (see figures 5 and 7 in Pak et al. 2019), the S0s were found to have a wider range of age, metallicity and α-abundance than the passive spirals at all radii out to 2R e . The stellar populations of passive spirals were fully encompassed within the spread of the S0 stellar populations, although the distributions of the passive spirals appeard skewed toward younger ages, higher metallicities, and lower α-abundances. However, the environmental dependence was weakly constrained because the number of passive spirals was too small. Thus, investigating the environments of passive spirals using a larger sample may provide further constraints on their quenching mechanisms.
Here, we investigate the spatially resolved stellar populations of passive spirals as a function of their environment using the Sydney-Australian Astronomical Observatory Multi-object Integral Field Spectrograph (SAMI; Croom et al. 2012) Galaxy Survey (Bryant et al. 2015) and the Galaxy and Mass Assembly (GAMA; Driver et al. 2011;Hopkins et al. 2013) survey. In this study, we aim to explore the environmental dependence of the formation and evolution of passive spirals and their evolutionary connections with S0s, and to provide further constraints on the quenching mechanisms.
This paper is organized as follows. Section 2 describes the galaxy samples and the analysis methods. The stellar population properties of passive spirals depending on environments and the comparison with S0s are shown in Section 3. The formation and evolution of passive spirals is discussed in Section 4. Finally, in Section 5, we summarize our results and draw conclusions. Throughout the paper we adopt a standard ΛCDM cosmology with Ω m = 0.3, Ω Λ = 0.7, and H 0 = 70 km s −1 Mpc −1 . All broadband data are given in the AB photometric system.

DATA AND SAMPLE
The SAMI Galaxy Survey is a spatially-resolved spectroscopic survey for over 3000 galaxies in the redshift range of 0.004 < z < 0.095. The SAMI instrument (Croom et al. 2012) using 13 fused fiber bundles (Hexabundles, Bland-Hawthorn et al. 2011;Bryant et al. 2014) is mounted at the prime focus on the 3.9m Anglo-Australian Telescope at Siding Spring Observatory in Australia. SAMI fibers are fed to the double-beam AAOmega spectrograph Smith et al. 2004;Sharp et al. 2006). Details of the galaxy sample of SAMI Galaxy Survey are described in Bryant et al. (2015), and additional details of the cluster sample are described in Owers et al. (2017). Besides galaxies from eight clusters, over 2000 galaxies were targeted from the three 4 • × 12 • GAMA regions centered on 9, 12, and 15h right ascension at dec = 0 (G09, G12, and G15 regions; Driver et al. 2011). For all observed galaxies, the SAMI Galaxy Survey measured resolved optical properties such as star formation rate, age, metallicities, and stellar and ionized gas kinematics (van de Sande et al. 2017;Scott et al. 2018).

Sample Selection
Firstly, the passive spirals are classified by visual inspection (MP and JHL) using composite color images from the fourteenth data release of the Sloan Digital Sky Survey (SDSS DR14; Abolfathi et al. 2018) and the Dark Energy Camera Legacy Survey (DECaLS; Dey et al. 2016) for the SAMI sample. We select red spiral galaxies with prominent red arms (e.g. 9016800089 and 288992 in Figure 1). We also select the galaxies in which the light distribution is not smooth and the arms are open (not a ring). In this case, the arms could be less prominent but still exist (e.g. 9011900418 and 107528 in Figure 1). The selected passive spirals are classified as from E to Early-spiral classes by Cortese et al. (2016). We removed the galaxies that are too inclined to tell if they have spiral arms or not, from the sample: 0% in E (294) and E/S0 (254) classes, ∼ 25.6% (91/355) in S0 class, ∼ 30.7% (104/339) in S0/Early-spiral class, and ∼ 4.9%(17/349) in Early-spiral class. The galaxies showing clear dust lanes and star-forming arms are also excluded: ∼ 13.0% (44/339) and ∼ 11.2% (39/349) in S0/Early-spiral and Early-spiral classes, respectively. In addition, we removed the four candidates (out of ∼ 1500 galaxies from E to Early-spiral types) that appear distorted probably due to interactions with neighbors, for which the distinction between spiral arms and tidal features is ambiguous.
Secondly, the galaxies are selected with 4.6−12µm ≤ 2 and 3.4 − 4.6µm ≤ 0.8 using WISE colors (Jarrett et al. 2017), which is a good indicator for distinguishing quiescent galaxies and excluding optically red galaxies due to dust-obscured star formation ( Figure 2). With these criteria, we find 70 passive spirals: 52 from the SAMI clusters and 18 in the SAMI-GAMA regions (group/field environments), respectively. Several examples of the final sample are shown in Figure   and S0s from the SAMI Galaxy Survey. Stars are the passive spirals and dots are the S0s. We use the magnitudes in the WISE catalog extracted using elliptical aperture photometry. When the elliptical-aperture magnitude is not available, we use the instrumental profile-fit photometry magnitude (black open stars for the passive spirals and black dots for the S0s). The dashed line distinguishes the quiescent galaxies (spheroidals) from intermediate disk galaxies (Jarrett et al. 2017).
As a comparison sample, we select S0s by adopting the SAMI visual morphology classification (Cortese et al. 2016). In our analysis, the S0 comparison sample consists of E/S0, S0, and S0/Early-spiral subtypes. Our S0s are also controlled by their WISE colors in the same manner as our passive spirals (Figure 2), in order to strictly exclude star-forming S0s. Therefore, in the S0/Early-spiral subtype, the galaxies without arms and with no/weak star formation are classified as control S0 sample. Among all S0s, 273 and 351 are selected in the cluster and the GAMA regions, respectively. Hereafter, we refer to our sample as the 'cluster passive spirals/S0s' and the 'field/group passive spirals/S0s'. Figure 3 presents the stellar mass and redshift distributions of the final sample. As seen in Figure 4, which presents specific star formation rate as a function of mass and the WISE [4.6]-[12] color, our final sample is mostly well distinguished  Figure 2. We also mark late-type galaxies (blue circles) from the SAMI Galaxy Survey data to infer that our sample selected by the WISE color-color diagram is well distinguished from star-forming late-type galaxies. The threshold of quiescent galaxies adopted from Choi et al. (2014)  from the star-forming late-type galaxies (blue circles). A few passive spirals and S0s above the threshold of quiescent galaxies (dashed line in the top panel of Figure 4) do not change our conclusion.

Measurements of the Stellar Population Properties
The measurements of stellar populations are obtained from Scott et al. (2017). The measured 20 Lick indices include five Balmer indices (Hδ A , Hδ F , Hγ A , Hγ F , Hβ), six iron-dominated indices (Fe4383, Fe4531, Fe5015, Fe5270, Fe5335, Fe5406), four molecular indices (CN1, CN2, Mg1, Mg2) and five more indices in the SAMI blue wavelength range (Ca4227, G4300, Ca4455, C4668, Mgb). Each index was measured from the observed spectrum after correcting for broadening and emission lines. Luminosity-weighted simple stellar populationequivalent age, metallicity and α-abundance ratio were measured by using the χ 2 minimization method (Proctor et al. 2004) fitted to the stellar population models of Schiavon (2007) and Thomas et al. (2011). The full details of the analysis are in section 3 of Scott et al. (2018). We adopt the measurements within a 1.4 arcsec diameter aperture (center) and within an elliptical aperture with a major axis radius of R e . The 1.4 arcsec diameter mostly corresponds to less than ∼half R e for passive spirals.
3. RESULTS 3.1. Passive spiral galaxies: comparison between cluster and field/group environments Figure 5 presents the age, [Z/H] and [α/Fe] within 1.4 arcsec and R e as a function of stellar mass and velocity dispersion (σ ) for the cluster and field/group passive spirals. The σ is measured from the spectrum inside a circular aperture of radius R e , as described in Scott et al. (2018) using the method from van de Sande et al. (2017).
Age shows no correlation with either mass or σ both in the cluster and field/group passive spirals. [Z/H] shows a very marginal difference between the two environments. In the clusters, [Z/H] tends to increase with mass (and σ ) with a large scatter and to be systematically higher in the center (α ∼ 0.22 ± 0.17) than within one R e (α ∼ 0.16 ± 0.16), whereas such a correlation is hardly detected in the field/groups. The environmental dependence also appears to be tight for [α/Fe] (α ∼ 0.17±0.157 in the center and α ∼ 0.19 ± 0.151 within one R e ): the cluster passive spirals have obviously higher [α/Fe] than the field/group passive spirals at the massive/highdispersion end.
We investigate the environment of the field/group passive spirals by using the group catalog from Treyer et al. (2018). Among 18 galaxies, six are in isolation, the rest of them are in the groups with a wide range of halo mass (log M /M ) ∼ 9.8 − 11.65. All isolated passive spirals are young ( 6 Gyr) but are not distinct in [Z/H] or [α/Fe], as shown in Figure 5. 3.2. Passive spirals vs. S0s: comparison between cluster and field/group environments We compare age, [Z/H] and [α/Fe] within R e with stellar mass and σ between passive spirals and S0s in the cluster and field/group. Figure 6 shows that cluster passive spirals tend to be slightly younger, more metalrich and less α-enhanced than S0s as a function of mass (and σ ), which results in the clear differences of the histograms. A two-dimensional Kolmogorov-Smirnov (KS) test of similarity in the cumulative distributions between passive spirals and S0s yields a probability (P KS ) of 0.0009 for age, 0.028 for [Z/H] and 0.0001 for [α/Fe]. These differences are clearer in the lower mass (or σ ) range.
Unlike in the clusters, the distribution of [α/Fe] shows no notable difference (P KS ∼ 0.7 in Figure 7i) between the field/group passive spirals and S0s in Figure 7. Interestingly, the [α/Fe] -mass(σ ) correlation slope in the field/groups appears to be shallower than in the clusters for S0, as well as for passive spirals. The slope in [α/Fe] is nearly constant (α ∼ 0.03 ± 0.20) or even decreasing with stellar mass at the high-mass end for the field/group S0s, similar to the passive spirals (α ∼ 0.03 ± 0.04). In addition, field/group S0s tend to have slightly larger scatter in both [Z/H] and [α/Fe] compared to cluster S0s. This is particularly evident at the high-mass end (see rms values in the top right corner of the Figures 6  and 7). We estimated the spearman's rank coefficient for [α/Fe], to quantitatively compare its mass (σ ) dependence between environments: 0.56 (0.63) for cluster PSp and −0.06 (0.09) for field/group PSp, and 0.36 (0.65) for cluster S0s and 0.04 (0.24) for field/group S0s. Since the comparisons show that massive field/group PSp and S0 galaxies tend to have lower [α/Fe] than cluster ones, we suspect that galaxies in low-density environments may have more extended star-formation histories ( Figure 8 shows the stellar mass versus σ for the passive spirals and S0s. The σ of passive spirals tends to be lower (mean ∆σ in all stellar mass range ∼ 32 km  Note. -The Spearman's rank correlation coefficient (ρ) will be between a value of −1 and +1. ρ = −1 indicates a perfect negative correlation and ρ = +1 indicates a perfect positive correlation. s −1 ) than that of S0s at a given stellar mass. This may imply that some S0s suffer a kind of dynamical heating after star formation stops. Loss of stellar mass in the galaxies could be also playing a role in mass−σ relations Joshi et al. (2020). The environmental dependence of the stellar mass−σ relations at a given galaxy type appears not to be significant.
In Figure 9, in order to compare all together, we show the mean of stellar population parameters with stellar mass (top panels) and σ (bottom panels) bins for all subdivisions as shown by the Figures 5 -7. We present the number of galaxies in case the galaxies less than 5 in each bin for caution. It is clear that [α/Fe] flattens and/or bends over at log (M /M ) 10.5 or σ 100 km s −1 for the field/group passive spirals and S0s.

DISCUSSION
In the previous section we have shown that stellar populations show different trends between cluster and field/group passive spirals, especially for [α/Fe]. Here, we discuss the possible origins of these different trends between environments and between passive spirals and S0s.
From our results, [α/Fe] increases with mass (and σ ) for both passive spirals and S0s, in the clusters. This finding is consistent with previous studies: for earlytype galaxies both metallicity and α-abundance correlate tightly with stellar mass (and σ ; Bernardi et al. 2006;Fig. 7.-The same as Figure 6 but for the field/group passive spirals and S0s. In histogram, the blue and green bins show passive spirals and S0s, respectively. McDermid et al. 2015). In particular, the [α/Fe] -mass correlation (Figures 6g, 6h) is an evidence that the more massive galaxies quenched in a short timescale at earlier epochs. Notably, cluster passive spirals have slightly younger age and, crucially, lower α-abundance compared to cluster S0s ( Figure 6). If passive spirals and S0s commonly originate from star-forming spiral galaxies, this means that passive spirals had undergone star formation for a longer timescale and became quiescent more recently than S0s. The mean age of cluster and field/group passive spirals is ∼ 5 Gyrs. This is coincident with the simulations from Bekki et al. (2002), in which spiral arm structures are found to fade over several Gyrs, after gas is stripped. Bekki & Couch (2011) argued that the progenitors of cluster S0s might be reshaped and quenched even before cluster infall, through mergers and/or tidal interactions in galaxy groups or cluster outskirts (pre-processing;De Lucia et al. 2012, Oh et al. 2018). On the other hand, the fact that passive spirals are younger and less α-enhanced than S0s in the clusters suggests that passive spirals may have reached the clusters without severe interactions with neighbors. After infall, they may have experienced star formation quenching by cluster environmental effects such as thermal evaporation (Cowie & Songaila 1977), ram-pressure stripping (Gunn & Gott 1972), starvation or strangulation (Larson et al. 1980;Bekki et al. 2002). This would naturally explain why passive spirals show younger age and longer star-formation timescale than S0s. As an additional check for the scenario for clusters, we inspect the distribution of stellar ages and [α/Fe] of all the cluster passive spirals in the projected phase-space diagram (Figures 10 and 11). We compare the observed distribution with the analytic curves from Pasquali et al. (2019), which grade the average infall time (= time elapsed since the first infall) of the galaxies. The distribution of the average infall time of the galaxies systematically shifts from high to low value with increasing zone number in their simulations (1 for the earliest infall, while 8 for the latest infall; see figure 4 in Pasquali et al. 2019). The stellar ages and [α/Fe] of passive spirals and S0s show an overall shift from older to younger ages and from more α-enhanced to less α-enhanced along R/R 200 and ∆v/σ 200 : galaxies with smaller R/R 200 and ∆v/σ 200 tend to have suffered quenching earlier. This is clearly seen in Figure 12. Furthermore, cluster S0s show older mean age and more α-enhanced than cluster passive spirals in all zones. This is similar to the results from Pasquali et al. (2019) and Smith et al. (2019) with much larger SDSS sample.
In summary, star-forming spiral galaxies may be quenched through mergers or interactions before falling into a cluster, becoming relatively old and α-enhanced S0s. Otherwise, without significant tidal events, spiral galaxies may arrive in the infall region of a cluster with ongoing star formation. Such spiral galaxies may suffer star formation quenching by cluster environmental effects and eventually evolve into S0s via the transitional phase of passive spirals. Those S0s (or passive spirals) have younger ages and lower α-enhancements than the S0s formed through mergers at an earlier epoch.
As shown in Figure 9, S0s tend to be more α-enhanced (by 0.06 − 0.08 dex at a given mass bin) than passive spirals in the cluster environments, while their metallicities are similar, which indicates that cluster S0s have suffered more rapid chemical enrichment and star formation quenching than cluster passive spirals. However, such a difference in [α/Fe] between passive spirals and S0s in clusters is hardly found in massive field/group passive spirals and S0s, which implies that their formation pro-cesses in low-density environments may be different from those in clusters.
In field/group environments, the trend of [α/Fe] is different from the well-known linear correlation between [α/Fe] and stellar mass: they appear to be flattened or even decreasing with increasing mass at log (M /M ) 10.5, both for passive spirals and S0s (see Figure 7g and h). According to Bernardi et al. (2006), the stars in early-type galaxies formed at slightly earlier times and on a slightly shorter timescale in dense regions than in less dense regions. Our finding shows that the different quenching timescale between high-and low-density environments is due to the difference at the high-mass end. At log (M /M ) 10.5, passive spirals or S0s in low-density environments appear to have longer starformation timescales, unlike those in high-density environments. That is, in low-density environments, starformation quenching mechanisms may be weak or, alternatively, there may be some mechanisms that prolong star formation.
One possible scenario for low-density environments is that those massive galaxies may be constantly rejuvenated by interactions with gas-rich neighbor galaxies, which is known to be more frequent in low-density environments with relatively low velocity-dispersion (Toomre & Toomre 1972, Lavery & Henry 1988, Byrd & Valtonen 1990. Radial transfer of gas to the central region and subsequent triggering of new star formation may influence light-weighted [Z/H] and [α/Fe] in interacting galaxies. Although the change of metallicity by interactions may depend on the properties of the interacting neighbors, [α/Fe] is expected to decrease as star formation is going on. Alternatively, massive passive spirals and S0s in low-density environments may be supplied with fuel for star formation by tidal stirring (Mayer et al. 2001) or gas accretion. Since gas stripping is not strong in lowdensity environments, they can keep forming stars using accreted gas, and consequently become relatively young and α-depressed galaxies. However, the suggested scenarios need to be verified using a much larger sample, because the sample size of our low-density galaxies (18) is not sufficient.

SUMMARY AND CONCLUSIONS
We have investigated the stellar populations of passive spirals with respect to their environment using a large sample from the SAMI Galaxy Survey. We found that star formation timescale of passive spirals appears to be different between clusters and field/groups. In the low-density environments, passive spirals show no [α/Fe]mass correlation, and have low [α/Fe] values even at the highest stellar mass. This indicates that passive spiral galaxies may have different formation histories depending on their environments, which confirms the previous findings that environmental effects play a key role on the star-formation quenching in spiral galaxies (Barsanti et al. 2018;Schaefer et al. 2017;Schaefer et al. 2019).
We discussed possible processes that can result in the observed trends, focusing on the difference between the environments. Like massive galaxies in clusters, those in low-density regions may have experienced burst of star formation making them old, metal-rich and α-enhanced at earlier epochs as well. However, cold gas accretion may occur more easily in low-density environments, which  Figures  5 -7. The error bar is the standard error of the mean. We mark the number of galaxies beside symbol when the galaxies of each bin is < 5. The vertical dotted lines identify the width of the bins.
consequently prolongs star formation -with the effect being most noticeable at the high-mass end. Alternatively, gas fuel by wet minor mergers can also make lower [α/Fe].
In clusters, there may be various and complex mechanisms that accelerate galaxy evolution. However, here we suggest two simplified channels that transform spirals to S0s through the passive spiral phase (Owers et al. 2019): (1) S0s may be formed by late-late or earlylate type merger at early epoch before infall to a cluster halo. The starburst triggered by merger and subsequent mass-quenching may have made them old, metalrich and α-enhanced.
(2) Spirals may be transformed into S0s via the passive spiral phase, by losing gas without morphological distortion. Their gas can be stripped away predominantly in the halo and outer disks by rampressure stripping or other cluster mechanisms, while passing through the cluster. After losing their gas, spirals become quiescent, and evolve secularly holding their spiral structures a few Gyrs -this is the passive spiral phase (Bekki et al. 2002). Our findings provide observational evidence that there are multiple channels to form passive spirals and the formation mechanisms closely depend on their environments. Future studies on the detailed structures and kinematics of passive spirals may be beneficial to verify and elaborate our scenarios.

ACKNOWLEDGMENTS
We gratefully thank the anonymous referee for constructive comments that have significantly improved this manuscript. This work was supported by UST Young Scientist Research Program through the University of Science and Technology (No. 2019YS10). The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney-AAO Multiobject Integral field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the GAMA Survey and the VST AT-LAS Survey. The SAMI Galaxy Survey is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013, the Australian Research Council Centre of Excellence for Allsky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. JvdS acknowledges support of an Australian Research Council Discovery Early Career Research Award (project number DE200100461) funded by the Australian Government. FDE acknowledges funding through the H2020 ERC Consolidator Grant 683184. JBH is supported by an ARC Laureate Fellowship that funds Jesse van de Sande and an ARC Federation Fellowship that funded the SAMI prototype. H.J. is supported by the National Research Foundation of Korea(NRF) grant funded by the Korea government(MSIT) (No. 2019R1F1A1041086). TMB is supported by an Australian Government Research Train- Fig. 10.-Top row: The age distribution of passive spirals (left column) and S0s (right column) in cluster and field/group environments across projected phase-space. Red: older than 9 Gyrs, Orange: 6 ≤ Age < 9 Gyrs, Green: 3 ≤ Age < 6 Gyrs, Blue: younger than 3 Gyrs. The σ 200 , and R 200 of eight clusters are taken from table 1 in Owers et al. (2017). The solid lines show the zones from 1 to 8 defined in Pasquali et al. (2019). Bottom row: the mean age and the number of galaxies in each bin are presented.