MEGADES: MEGARA galaxy disc evolution survey

Astronomy & Astrophysics A&A 670, A117 (2023) https://doi.org/10.1051/0004-6361/202245111 © The Authors 2023 MEGADES: MEGARA galaxy disc evolution survey Data release I: Central fields M. Chamorro-Cazorla1,2, A. Gil de Paz1,2, Á. Castillo-Morales1,2, J. Gallego1,2, E. Carrasco3, J. Iglesias-Páramo4, M. L. García-Vargas5, S. Pascual1,2, N. Cardiel1,2, C. Catalán-Torrecilla1,2, J. Zamorano1,2, P. Sánchez-Blázquez1,2, A. Pérez-Calpena5, P. Gómez-Álvarez5, and J. Jiménez-Vicente6,7 1Departamento de Física de la Tierra y Astrofísica, Fac. CC. Físicas, Universidad Complutense de Madrid, Plaza de las Ciencias, 1, Madrid 28040, Spain 2Instituto de Física de Partículas y del Cosmos, IPARCOS-UCM, Fac. CC. Físicas, Universidad Complutense de Madrid, Plaza de las Ciencias 1, Madrid 28040, Spain e-mail: [email protected] 3Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro No.1, C.P. 72840, Tonantzintla, Puebla, Mexico 4Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain 5FRACTAL S.L.N.E.. C/ Tulipán 2, p13, 1A, 28231, Las Rozas de Madrid, Spain 6Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus de Fuentenueva, 18071 Granada, Spain 7Instituto Carlos I de Física Teórica y Computacional, Universidad de Granada, 18071 Granada, Spain Received 29 September 2022 / Accepted 31 October 2022 ABSTRACT The main interest of the science team for the exploitation of the MEGARA instrument at the 10.4m Gran Telescopio Canarias (GTC) is devoted to the study of nearby galaxies. The focus lies on researching the history of star formation, and the chemical and kinematical properties of disc systems. We refer to this project as MEGADES: the MEGARA galaxy disc evolution survey. The initial goal of MEGADES is to provide a detailed study of the inner regions of nearby disc galaxies in terms of their spectrophotometric and chemical evolution, and to provide a dynamical characterisation by distinguishing the contribution of in situ and ex situ processes to the history of star formation and effective chemical enrichment of these regions. In addition, the dynamical analysis of these inner regions naturally includes the identification and characterisation of galactic winds that might be present in these regions. At a later stage, we will extend this study farther out in galactocentric distance. The first stage of this project encompasses the analysis of the central regions of 43 nearby galaxies observed with the MEGARA integral field unit for ∼114h, including both guaranteed time and open time observations. In this paper we provide a set of all the processed data products available to the community and early results from the analysis of these data regarding stellar continuum and ionised and neutral gas features. Key words. galaxy: bulge – galaxies: ISM – galaxies: evolution – galaxies: stellar content – techniques: imaging spectroscopy 1. Introduction Whereas the fundamental principles of stellar evolution are reasonably well understood since the last century, the fundamental aspects of galaxy evolution continue to be the subject of fierce discussion within the astronomical community. This is due to the fact that the distance between galaxies, relative to their own size, is considerably smaller than in the case of stars, which means that the evolution of the vast majority of galaxies has proceeded under the influence of other galaxies, and did not occur in isolation, especially in early epochs when the universe was much denser than it is at present. Moreover, some processes that take place in galaxies and are considered to be internal secular processes, might be periodic, and can be triggered by the interaction of the galaxies with their environment, such as nuclear activity or intense star formation. However, even if these mechanisms are classified as secular (considering the definition of secularity given by Kormendy & Kennicutt 2004), they leave an evident and clearly distinct imprint on the later evolution of these objects that helps to distinguish the evolution of the different galaxies. Some of the mechanisms capable of affecting the kinematic, chemical, and photometric properties of galaxies are major and minor mergers (Toomre & Toomre 1972), bars, rings, density waves (Lin & Shu 1964), active galactic nuclei (AGN) feedback (Croton et al. 2006;Fabian 2012), stellar diffusion, gas in-fall (Sancisi et al. 2008), and, in the case of galaxies in clusters, also ram-pressure striping (Gunn & Gott 1972) and galaxy harassment (Moore et al. 1996). At the same time, galactic winds (GWs) constitute an important mechanism for redistributing dust and metals both in galaxies and towards the intergalactic medium (IGM) and have been invoked to reproduce the scale relations observed in galaxies, as well as to understand the apparent discrepancies between the theoretical and observed luminosity functions and to understand the evolution of galaxies (especially of high-redshift objects) through the green valley. The contribution of all these mechanisms is rather complex, therefore, determining the evolution of galaxies is in many aspects still a puzzle. In recent years, our knowledge about these questions has progressed significantly, mostly through studies carried out with integral field spectroscopy (IFS) instruments. These instruments are particularly well suited for understanding the role played A117, page 1 of 106 Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. This article is published in open access under the Subscribe to Open model.Subscribe to A&A to support open access publication. A&A 670, A117 (2023) by each of these mechanisms in the evolution of galaxies, as they provide two-dimensional spectroscopic information. This technique has already demonstrated its potential in the study of nearby galaxies such as SAURON1(de Zeeuw et al. 2002), ATLAS3D (Cappellari et al. 2011), CALIFA2(Sánchez et al. 2012), MaNGA3(Bundy et al. 2015), VENGA4(Blanc et al. 2013) and SIGNALS5(Rousseau-Nepton et al. 2019). These surveys have enabled a great advance, especially in studies of galaxies at low redshift, because existing techniques did not allow performing diverse analyses like this before. At higher redshifts, we also count on surveys based on IFS observations such as SINS6(Förster Schreiber et al. 2009), MASSIVE7(Contini et al. 2012), KMOS3D,8(Wisnioski et al. 2015), and MAGIC9(Mercier et al. 2022). The main difference between these studies and those based on observations made on nearby galaxies is that at high redshift, these surveys basically focus on the analysis of the brightest emission lines and do not study the stellar continuum because the sensitivity of the instruments prevents observing them correctly. Studies based on multi-band photometric observations that generate spectral energy distributions (SED), such as J-PAS10 (Benitez et al. 2014) and SHARDS11 (Pérez-González et al. 2013), represent the best alternative to these high-zsurveys when the stellar continuum is to be studied. SED-based surveys have all the spatial information and are very powerful at high redshift in determining a large number of parameters (i.e. mean ages, redshifts, and stellar masses), but they lack the spectral resolution needed to measure individual lines or different kinematic components. However, we are now on the verge of an unprecedented revolution in the study of distant galaxies through the start of the JWST12 (Gardner et al. 2006) observations, in photometry with NIRcam13 (Rieke et al. 2005) and in 2D spectroscopy with NIRSpec14 (Bagnasco et al. 2007). These surveys have also taught us that the amount of information that their data provide and the studies that can be carried out with them must rely on multi-wavelength information from multiple facilities, both ground-based and from space. This necessitates public sharing of the observations with the rest of the community, and with them, the legacy surveys, in order to be able to exploit them in the best possible way. In this paper, we present the first data release within MEGADES (MEGARA galaxy disc evolution survey), the legacy survey of the MEGARA instrument (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía; Gil de Paz et al. 2018;Carrasco et al. 2018). MEGARA is a high-resolution optical spectrograph installed on the 10.4m GTC telescope with two observing modes, the large compact bundle (LCB) mode, an IFU covering a field of view (FoV) of 12.5 ×11.3arcsec2with a 1Spectroscopic Areal Unit for Research on Optical Nebulae. 2The Calar Alto Legacy Integral Field Area survey. 3Mapping Nearby Galaxies at APO. 4The VIRUS-P Exploration of Nearby Galaxies. 5Star-formation, Ionized Gas and Nebular Abundances Legacy Survey. 6Spectroscopic Imaging survey in the Near-infrared with SINFONI. 7Mitchell spectrograph Assembly of Stars and Stuffwith Integral-field spectroscopy in the Visible. 8K-band Multi Object Spectrograph Survey. 9MUSE-gAlaxy Groups In Cosmos Survey. 10 Javalambre Physics of the Accelerating Universe Astrophysical Survey. 11 Survey for High-z Absorption Red & Dead Sources. 12 James Webb Space Telescope. 13 The JWST Near Infrared Camera. 14 The JWST Near Infrared Spectrograph. spatial resolution of 0.62arcsec, and the multi-object spectroscopy (MOS) mode, which allows the simultaneous acquisition of 92 object spectra in an area of 3.5×3.5 arcmin2around the IFU. The observations can cover a spectral interval from 3650 to 9700Å in different ranges with three possible resolutions, R=λ/FWHM ∼6000, 12000, and 20000. The unique characteristics of MEGARA and the large collecting area of GTC mean that the MEGADES survey is another step forward on our way to discovering the mechanisms that shape the evolution of galaxies through the unprecedented combination of depth, spatial, and especially spectral resolutions. MEGADES aims to improve our knowledge of the secular processes that galaxies undergo by studying the kinematic properties of stars and gas in all the phases in which the latter is present, determining the characteristics of stellar populations, analysing diagnostic diagrams of the emission line ratio and discovering the nature of the galaxy bulges in the sample. In this first paper, we present studies of the stellar and gas kinematics and spectral line flux measurements in the central regions of MEGADES galaxies. Together with this paper, we release the processed observations and the analysis products we obtained. In Sect. 2, we describe the scientific goals of the survey together with the sample of observed galaxies. Section 3 describes the observations in detail. In Sect. 4, we explain the process of data reduction and subsequent data refinements. We detail the analysis of the stellar kinematics and the spectral line fitting performed on the data in Sect. 5. In Sect. 6, we detail all the data and products that are released together with this paper. Finally, we summarise in Sect. 8. Throughout this paper, we assume a standard ΛCDM universe, whose cosmological parameters are H0= 70 km s−1Mpc−1,ΩΛ= 0.7, and Ωm=0.3. 2. Survey 2.1. MEGADES goals Since this is introductory paper to MEGADES that includes data from the central regions of the galaxies alone together with the first kinematic analyses of the stellar content and interstellar gas, the bulk of the MEGADES goals will be addressed in future papers. The long-term objective of MEGADES is to understand the impact of secular processes on disc evolution. Our primary goal is to test whether gas infall is one of the main mechanisms in the evolution of galaxies, and whether it drives the inside-out formation of discs. Therefore, we will test the model predictions for this scenario against our MEGADES observations by analysing the secular and external causes of the differences, that is, nuclear activity, stellar migration, minor mergers, intense star formation, and so on. We will use MEGARA high spatial and spectral resolution 2D spectroscopy to analyse the kinematic properties of the stellar component in order to detect different structures such as bars or inner discs in the central regions of MEGADES galaxies. We will also analyse line indices sensitive to age and metallicity (Chamorro-Cazorla et al. 2022), and for the detected HII regions, the gas emission line spectrum, from which we will produce diagnostic diagrams and determine chemical abundances. Finally, we will study the presence and frequency of GWs in the MEGADES sample, both in its warm and cold phases. We will examine the kinematic properties and the shape of the Hαemission line to distinguish different kinematic components to study the warm phase, and we will use the NaI D absorption doublet to analyse the cold phase. A117, page 2 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey A&A proofs: manuscript no. MEGADES_DR1 Fig. 1. RGB images of some of the galaxies in the MEGADES sample from PanSTARRS observations (g, r, and i filters). The white box in the centre of each panel indicates the MEGARA IFU FoV. The images of all the galaxies in the MEGADES sample can be found in the Appendix A, Figure A.1. Fig. 2. Concatenated spectra of the galaxy NGC 0718 observed with the VPH LR-B, LR-V, and LR-R in blue, green, and red, respectively. The spectrum of each VPH is the result of coadding the 567 spectra measured simultaneously in one single exposure with the MEGARA IFU. of the detector. Bad pixels are automatically masked in this step with the file master_bpm.fits, available in the pipeline. The trajectory of each one of our fibre spectra needs to be properly traced on the detector. To do this, we used the TraceMap calibration images obtained by illuminating the focal plane with a halogen lamp providing homogeneous illumination. When performing this step, we were careful with the calibration images we used because the position of the fibres on the detector changes depending on the temperature of the telescope. It is recommended to use calibration images as close as possible to the observation of the scientific target to best minimise the temperature difference between them. The DRP tasks we used for this purpose were MegaraTraceMap and MegaraModelMap. The first task tracks the path of the light projected by the fibres onto the CCD, and the second task makes a more exhaustive model of it in order to perform the extraction, assuming each fibre has a Gaussian light profile across dispersion. In some cases, 11 observations taken with LR-B and 3 with LR-R, we had problems tracing the last fibre box (from fibre 603 to 623) because the instrument was not properly focused. In these cases, the spectra from these fibres were ignored. An example of the impact Fig. 3. Seeing values, provided by the monitors of observatory, and histogram for the nights of the MEGADES sample observations. The dashed black line indicates the size of the hexagonal spaxels that comprise the MEGARA IFU. caused by doing this on our data is shown in Figure B.22. In panels (t) and (v), continuum images taken with LR-B and LR- R, respectively, are shown, and all the spaxels corresponding to the out-of-focus fibres are shown in white. We then calibrated the wavelength. Here we used images that were acquired using ThAr or ThNe lamps, depending generally on the VPH we used for our observation. As a general rule, for LR-B, LR-V, and LR-R observations, we used ThAr lamps. For this task, it is necessary to confirm that the traces obtained in the previous tasks match the path followed by the projection of the fibres on the detector in the images of the arc lamps. If there is a small offset between the two, this can be corrected by indicating it in the recipe we use, MegaraArcCalibration. In this paper, we only calibrated three observations with ThNe lamps: NGC 4189, NGC 2552, and NGC 3104 observed with LR-R, because these calibrations are even more precise, with RMS <0.5km s−1(see Figure 4). The median RMS values in Å for LR-B, LR-V, and LR-R are 0.019, 0.030, and 0.020, respectively, and the value is 0.020 for the whole sample. We find that the RMS represents Article number, page 4 of 106 Fig. 1. RGB images of some of the galaxies in the MEGADES sample from PanSTARRS observations (g,r, and ifilters). The white box in the centre of each panel indicates the MEGARA IFU FoV. The images of all the galaxies in the MEGADES sample can be found in the Appendix A, Fig. A.1. With this first data release, we will be able to perform all these studies in the central regions of the galaxies in the sample and then place them in context with analyses of the outer emission disc when these observations become available. We will study the stellar populations that make up the bulges of the MEGADES galaxies together with their kinematical properties. With this information, we will be able to determine whether classical bulges dominate the galaxies in our sample or if there are more galaxies with pseudo-bulges (Kormendy & Kennicutt 2004). We will also study the possible presence of outflows associated with nuclear starbursts and AGN, considering the existence of different kinematic components in the neutral or warm phase, and the differences that may exist between the two phases. In addition to all of this, we will be able to generate different diagnostic diagrams with the information contained in the different lines we will study. 2.2. MEGADES sample The original MEGADES sample (see Table 1and Figs. 1and A.1) was extracted from the Spitzer survey of stellar structure in galaxies (S4G) sample, Sheth et al. 2010). The S4G was designed as a volume- (d<40 Mpc, |b|>30◦), magnitude- (mB,corr <15.5mag), and diameter-limited (D25 >1′) survey. The use of the MEGARA IFU to carry out all observations makes a diameter-limited sample a reasonable idea, as has been the case for the CALIFA sample (Sánchez et al. 2012) or PHANGS-MUSE (Emsellem et al. 2022). In addition to the limitations of the S4G sample, we imposed further constraints to fit the sample to our scientific goals. We wished to avoid dwarf systems and elliptical galaxies because in most cases, they are not supported by rotation. We also removed galaxies with inclinations higher than 70◦to be able to analyse the metallicity and have the possibility of deriving velocity ellipsoids. Taking into account all the previous considerations, and because it is not practical to observe the entire S4G sample (2331 galaxies) because of the required telescope time, we must consider further selection criteria in our sample: We limited the diameter to a range in which on the lower side, we removed the smallest galaxies, and on the upper side, we limited the diameter to approximately the field of view of the MEGARA MOS (2.5′<D25 <4′)15. We also limited the declination (Dec(J2000) > –20◦). Summarising all the above selection criteria, the galaxies in our sample are selected by distance d<40Mpc (z∼0.0092), galactic latitude |b|>30◦, declination Dec(J2000)>–20◦, apparent magnitude mB,corr <15.5 mag, apparent diameter 2.5′<D25 <4′, and inclination i<70◦. This paper includes a random subsample of 30 out of the 215 galaxies that meet the selection criteria of the MEGADES-S4G sample (see Table 1). However, to enrich our sample, we added 13 galaxies from the CALIFA sample (Calar Alto Legacy Integral Field Area Survey, marked with a dagger in Table 1) that show signs of containing interstellar NaI D and are candidates for hosting galactic winds in their neutral phase because their EWISM≻NaID > 1.5 Å. The CALIFA survey, with SDSS DR716 (Abazajian et al. 2009) as the parent sample, is limited in diameter (45′′ <D25 <80′′), redshift (0.005 <z<0.03), galactic latitude above 20◦, and declination above +7◦. 3. MEGARA observations All MEGADES observations (43 galaxies) of this first release, DR1, were taken with the MEGARA IFU at the GTC. The MEGARA IFU, or LCB, covers a field of view of 12.5×11.3 arcsec2using 567 fibres in a hexagonal tessellation with a spaxel size of 0.62 arcsec. In addition to these fibres, it also uses 56 fibres to simultaneously measure sky-background spectra with the observation of the scientific target in order to subtract them from the observations afterwards. These sky fibres are distributed in eight distinct regions in the outermost parts of the MOS field of view, located between 1.75 and 2arcmin 15 Note that as part of the outer-disc extension of MEGADES we plan to obtain MOS spectra of HII regions over the whole galaxies extension. 16 Sloan Digital Sky Survey Data Release 7. A117, page 3 of 106 A&A 670, A117 (2023) Table 1. Global properties of the galaxy sample. Name Morphology(1) t(2) z(1) RA(1) Dec(1) Scale(3) DL(3) Spectral class(1) (J2000) (J2000) (kpcarcsec−1) (Mpc) IC 1683(†)S? 2.7 0.01624 01h22m39s .000 +34d26m13s .000 0.331 70.4 – NGC 0023(†)SB(s)a 1.2 0.01523 00h09m53s .410 +25d55m25s .600 0.310 66.0 HII LIRG NGC 0600 (R’)SB(rs)d 7.0 0.00614 01h33m05s .300 –07d18m41s .100 0.127 26.4 HII NGC 0716(†)SBa: 1.1 0.01521 01h52m59s .681 +12d42m30s .490 0.310 65.9 HII NGC 0718 SAB(s)a 1.0 0.00578 01h53m13s .300 +04d11m45s .000 0.119 24.9 – NGC 1042 SAB(rs)cd 6.0 0.00457 02h40m23s .967 –08d26m00s .760 0.094 19.6 NLAGN NGC 1087 SAB(rs)c 5.2 0.00508 02h46m25s .164 –00d29m55s .140 0.105 21.8 WR HII NGC 2500 SB(rs)d 7.0 0.00171 08h01m53s .210 +50d44m13s .600 0.035 7.3 HII NGC 2537 SB(s)m pec 8.8 0.00148 08h13m14s .640 +45d59m23s .300 0.031 6.3 HII NGC 2543(†)SB(s)b 3.0 0.00824 08h12m57s .922 +36d15m16s .660 0.169 35.5 – NGC 2552 SA(s)m? 9.0 0.00175 08h19m20s .532 +50d00m34s .660 0.036 7.5 – NGC 2967 SA(s)c 5.2 0.00626 09h42m03s .295 +00d20m11s .180 0.169 26.9 – NGC 3104 IAB(s)m 9.9 0.00201 10h03m57s .350 +40d45m24s .900 0.042 8.6 HII NGC 3485 SB(r)b: 3.2 0.00478 11h00m02s .380 +14d50m29s .700 0.099 20.5 AGN NGC 3507 SB(s)b 3.1 0.00327 11h03m25s .357 +18d08m07s .620 0.068 14.0 LINER NGC 3780 SA(s)c: 5.2 0.00798 11h39m22s .360 +56d16m14s .400 0.164 34.4 – NGC 3893 SAB(rs)c: 5.1 0.00323 11h48m38s .190 +48d42m39s .000 0.067 13.9 HII NGC 3982 SAB(r)b: 3.2 0.00371 11h56m28s .129 +55d07m30s .860 0.077 15.9 HII Sy2 NGC 3998(∗)SA0ˆ0(r)? –2.2 0.00350 11h57m56s .133 +55d27m12s .922 0.072 15.0 Sy1 LINER NGC 4037 SB(rs)b: 3.3 0.00310 12h01m23s .670 +13d24m03s .700 0.064 13.3 – NGC 4041 SA(rs)bc: 4.0 0.00405 12h02m12s .202 +62d08m14s .000 0.084 17.4 HII NGC 4189 SAB(rs)cd? 5.9 0.00700 12h13m47s .270 +13d25m29s .300 0.144 30.1 HII NGC 4278(∗)E1-2 –4.8 0.00207 12h20m06s .824 +29d16m50s .722 0.043 8.9 Sy1 LINER NGC 4593(∗)(R)SB(rs)b 3.0 0.00831 12h39m39s .425 –05d20m39s .340 0.171 35.8 Sy1 NGC 4750(∗)(R)SA(rs)ab 2.4 0.00540 12h50m07s .271 +72d52m28s .720 0.111 23.2 LINER NGC 5218(†)SB(s)b? pec 3.1 0.00949 13h32m10s .379 +62d46m03s .910 0.195 40.9 HII LINER NGC 5394(†)SB(s)b pec 3.1 0.01150 13h58m33s .652 +37d27m12s .550 0.235 49.7 HII LIRG NGC 5616(†)SBc 4.0 0.02810 14h24m20s .699 +36d27m41s .120 0.564 122.9 – NGC 5953(†)SAa: pec 0.1 0.00656 15h34m32s .383 +15d11m37s .590 0.135 28.2 Sy2 LINER NGC 5957(∗)(R’)SAB(r)b 2.9 0.00605 15h35m23s .214 +12d02m51s .360 0.125 26.0 LINER NGC 5963 S pec 4.1 0.00219 15h33m27s .860 +56d33m34s .900 0.045 9.4 – NGC 6027(†)S0 pec –1.5 0.01466 15h59m12s .537 +20d45m48s .090 0.299 63.5 HII NGC 6140 SB(s)cd pec 5.6 0.00303 16h20m58s .160 +65d23m26s .000 0.063 13.0 – NGC 6217 (R)SB(rs)bc 4.0 0.00454 16h32m39s .200 +78d11m53s .400 0.094 19.5 HII Sy2 NGC 6339 SBd 6.3 0.00703 17h17m06s .500 +40d50m41s .900 0.145 30.3 – NGC 6412 SA(s)c 5.2 0.00438 17h29m37s .510 +75d42m15s .900 0.090 18.8 – NGC 7025(†)Sa 1.0 0.01657 21h07m47s .340 +16d20m09s .100 0.350 74.6 – NGC 7437 SAB(rs)d 6.7 0.00707 22h58m10s .060 +14d18m30s .590 0.146 30.4 – NGC 7479(∗)SB(s)c 4.3 0.00792 23h04m56s .650 +12d19m22s .400 0.163 34.1 Sy2 LINER NGC 7591(†)SBbc 3.6 0.01654 23h18m16s .280 +06d35m08s .900 0.337 71.7 Sy LIRG LINER NGC 7738(†)SB(rs)b 3.0 0.02251 23h44m02s .059 +00d30m59s .860 0.455 98.1 – NGC 7787(†)(R’)SB(rs)0/a: 0.4 0.02221 23h56m07s .823 +00d32m58s .140 0.449 96.7 – PGC 066559 SB(s)dm pec 8.1 0.00900 21h19m43s .040 –07d33m12s .500 0.185 38.8 – Notes. (∗)Data products from these galaxies are under temporary embargo as they constitute the core of Hermosa-Muñoz et al. (in prep.). (†) CALIFA survey data. References. (1) NASA/IPAC extragalactic database. (2) Morphological type code from Hyperleda. (3) Wright (2006). from the IFU. The fundamental feature that makes MEGARA ideal for performing the analyses required in MEGADES is its spectral resolution. MEGARA has 18 different volume-phase holographic (VPH) transmission gratings that allow covering a range from 3650 to 9700Å with low (LR), medium (MR), and high (HR) resolutions. We observed the central regions of the MEGADES galaxies using three different VPHs, VPH480-LR (LR-B), VPH570-LR (LR-V), and VPH675-LR (LR-R), whose specifications can be found in Table 2. This produces a combined spectrum covering the spectral range from 4350 to 7288 Å (see Fig. 2for the combined MEGARA spectrum of NGC 0718). This range includes spectral features such as Hβ,[OIII]λ5007, NaI D, and Hα, as well as absorption features needed for the stellar populations analysis (Chamorro-Cazorla et al. 2022). For the 13 CALIFA galaxies, we only have LR-V and LR-R observations. They suffice for A117, page 4 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey Table 2. MEGARA VPH specifications. MEGARA VPH Spectral coverage R.L.D.(*) ∆λFWHM R (Å)(Åpx≻1)(Å) LR-B 4350.6–5250.8 0.23 0.79 6061 LR-V 5165.6–6176.2 0.27 0.94 6078 LR-R 6158.3–7287.7 0.31 1.11 6100 Notes. (∗)Reciprocal linear dispersion. A&A proofs: manuscript no. MEGADES_DR1 Fig. 1. RGB images of some of the galaxies in the MEGADES sample from PanSTARRS observations (g, r, and i filters). The white box in the centre of each panel indicates the MEGARA IFU FoV. The images of all the galaxies in the MEGADES sample can be found in the Appendix A, Figure A.1. Fig. 2. Concatenated spectra of the galaxy NGC 0718 observed with the VPH LR-B, LR-V, and LR-R in blue, green, and red, respectively. The spectrum of each VPH is the result of coadding the 567 spectra measured simultaneously in one single exposure with the MEGARA IFU. of the detector. Bad pixels are automatically masked in this step with the file master_bpm.fits, available in the pipeline. The trajectory of each one of our fibre spectra needs to be properly traced on the detector. To do this, we used the TraceMap calibration images obtained by illuminating the focal plane with a halogen lamp providing homogeneous illumination. When performing this step, we were careful with the calibration images we used because the position of the fibres on the detector changes depending on the temperature of the telescope. It is recommended to use calibration images as close as possible to the observation of the scientific target to best minimise the temperature difference between them. The DRP tasks we used for this purpose were MegaraTraceMap and MegaraModelMap. The first task tracks the path of the light projected by the fibres onto the CCD, and the second task makes a more exhaustive model of it in order to perform the extraction, assuming each fibre has a Gaussian light profile across dispersion. In some cases, 11 observations taken with LR-B and 3 with LR-R, we had problems tracing the last fibre box (from fibre 603 to 623) because the instrument was not properly focused. In these cases, the spectra from these fibres were ignored. An example of the impact Fig. 3. Seeing values, provided by the monitors of observatory, and histogram for the nights of the MEGADES sample observations. The dashed black line indicates the size of the hexagonal spaxels that comprise the MEGARA IFU. caused by doing this on our data is shown in Figure B.22. In panels (t) and (v), continuum images taken with LR-B and LR- R, respectively, are shown, and all the spaxels corresponding to the out-of-focus fibres are shown in white. We then calibrated the wavelength. Here we used images that were acquired using ThAr or ThNe lamps, depending generally on the VPH we used for our observation. As a general rule, for LR-B, LR-V, and LR-R observations, we used ThAr lamps. For this task, it is necessary to confirm that the traces obtained in the previous tasks match the path followed by the projection of the fibres on the detector in the images of the arc lamps. If there is a small offset between the two, this can be corrected by indicating it in the recipe we use, MegaraArcCalibration. In this paper, we only calibrated three observations with ThNe lamps: NGC 4189, NGC 2552, and NGC 3104 observed with LR-R, because these calibrations are even more precise, with RMS <0.5km s−1(see Figure 4). The median RMS values in Å for LR-B, LR-V, and LR-R are 0.019, 0.030, and 0.020, respectively, and the value is 0.020 for the whole sample. We find that the RMS represents Article number, page 4 of 106 Fig. 2. Concatenated spectra of the galaxy NGC 0718 observed with the VPH LR-B, LR-V, and LR-R in blue, green, and red, respectively. The spectrum of each VPH is the result of coadding the 567 spectra measured simultaneously in one single exposure with the MEGARA IFU. A&A proofs: manuscript no. MEGADES_DR1 Fig. 1. RGB images of some of the galaxies in the MEGADES sample from PanSTARRS observations (g, r, and i filters). The white box in the centre of each panel indicates the MEGARA IFU FoV. The images of all the galaxies in the MEGADES sample can be found in the Appendix A, Figure A.1. Fig. 2. Concatenated spectra of the galaxy NGC 0718 observed with the VPH LR-B, LR-V, and LR-R in blue, green, and red, respectively. The spectrum of each VPH is the result of coadding the 567 spectra measured simultaneously in one single exposure with the MEGARA IFU. of the detector. Bad pixels are automatically masked in this step with the file master_bpm.fits, available in the pipeline. The trajectory of each one of our fibre spectra needs to be properly traced on the detector. To do this, we used the TraceMap calibration images obtained by illuminating the focal plane with a halogen lamp providing homogeneous illumination. When performing this step, we were careful with the calibration images we used because the position of the fibres on the detector changes depending on the temperature of the telescope. It is recommended to use calibration images as close as possible to the observation of the scientific target to best minimise the temperature difference between them. The DRP tasks we used for this purpose were MegaraTraceMap and MegaraModelMap. The first task tracks the path of the light projected by the fibres onto the CCD, and the second task makes a more exhaustive model of it in order to perform the extraction, assuming each fibre has a Gaussian light profile across dispersion. In some cases, 11 observations taken with LR-B and 3 with LR-R, we had problems tracing the last fibre box (from fibre 603 to 623) because the instrument was not properly focused. In these cases, the spectra from these fibres were ignored. An example of the impact Fig. 3. Seeing values, provided by the monitors of observatory, and histogram for the nights of the MEGADES sample observations. The dashed black line indicates the size of the hexagonal spaxels that comprise the MEGARA IFU. caused by doing this on our data is shown in Figure B.22. In panels (t) and (v), continuum images taken with LR-B and LR- R, respectively, are shown, and all the spaxels corresponding to the out-of-focus fibres are shown in white. We then calibrated the wavelength. Here we used images that were acquired using ThAr or ThNe lamps, depending generally on the VPH we used for our observation. As a general rule, for LR-B, LR-V, and LR-R observations, we used ThAr lamps. For this task, it is necessary to confirm that the traces obtained in the previous tasks match the path followed by the projection of the fibres on the detector in the images of the arc lamps. If there is a small offset between the two, this can be corrected by indicating it in the recipe we use, MegaraArcCalibration. In this paper, we only calibrated three observations with ThNe lamps: NGC 4189, NGC 2552, and NGC 3104 observed with LR-R, because these calibrations are even more precise, with RMS <0.5km s−1(see Figure 4). The median RMS values in Å for LR-B, LR-V, and LR-R are 0.019, 0.030, and 0.020, respectively, and the value is 0.020 for the whole sample. We find that the RMS represents Article number, page 4 of 106 Fig. 3. Seeing values, provided by the monitors of observatory, and histogram for the nights of the MEGADES sample observations. The dashed black line indicates the size of the hexagonal spaxels that comprise the MEGARA IFU. studying the possible presence of outflows in the neutral (NaI D) and the warm (Hα) components. Table A.1 shows the observing dates, airmass, and exposure times for all the galaxies in the sample. Table A.2 provides the observing conditions for each observing night with information on the seeing and atmospheric transparency. Figure 3shows a histogram with the seeing values provided by the monitors of the observatory during the nights of MEGADES observations. 4. Data processing 4.1. Basic reduction: MEGARA DRP We used the MEGARA data reduction pipeline (DRP) v0.12.0 (Pascual et al. 2022) to process all the data provided by the telescope. This data reduction was performed according to the instructions provided in Castillo-Morales et al. (2020)17.We have followed the same routines as we used to reduce the data for the galaxy NGC 7025 in Chamorro-Cazorla et al. (2022), considering the particularities of each individual observation. We started by removing the level of bias present in the image. This bias is an electronic pedestal that is added to all images taken with MEGARA before the analogue-to-digital converter (ADC) to minimise errors associated with the conversion of voltages that would otherwise be very close to zero. For the purpose of removing this pedestal from the counts in the images, we used the bias calibration images and the task MegaraBiasImage. These images are taken with zero exposure time, and the bias level is slightly different at the top and bottom of the image (∼100 counts) because the MEGARA CCD (a CCD231-84 from E2V) is read through two diagonally opposed amplifiers. The use of two (instead of the four available) amplifiers minimises electronic cross-talk during the read-out process. The images were corrected from overscan and trimmed to match the physical size of the detector. Bad pixels are automatically masked in this step with the file master_bpm.fits, available in the pipeline. The trajectory of each one of our fibre spectra needs to be properly traced on the detector. To do this, we used the TraceMap calibration images obtained by illuminating the focal plane with a halogen lamp providing homogeneous illumination. When performing this step, we were careful with the calibration images we used because the position of the fibres on the detector changes depending on the temperature of the telescope. It is recommended to use calibration images as close as possible to the observation of the scientific target to best minimise the temperature difference between them. The DRP tasks we used for this purpose were MegaraTraceMap and MegaraModelMap. The first task tracks the path of the light projected by the fibres onto the CCD, and the second task makes a more exhaustive model of it in order to perform the extraction, assuming each fibre has a Gaussian light profile across dispersion. In some cases, 11 observations taken with LR-B and 3 with LR-R, we had problems tracing the last fibre box (from fibre 603 to 623) because the instrument was not properly focused. In these cases, the spectra from these fibres were ignored. An example of the impact caused by doing this on our data is shown in Fig. B.22. In panels t and v, continuum images taken with LR-B and LR-R, respectively, are shown, and all the spaxels corresponding to the out-of-focus fibres are shown in white. We then calibrated the wavelength. Here we used images that were acquired using ThAr or ThNe lamps, depending generally on the VPH we used for our observation. As a general rule, for LR-B, LR-V, and LR-R observations, we used ThAr lamps. For this task, it is necessary to confirm that the traces obtained in the previous tasks match the path followed by the projection of the fibres on the detector in the images of the arc lamps. If there is a small offset between the two, this can be corrected by indicating it in the recipe we use, MegaraArcCalibration. In this paper, we only calibrated three observations with ThNe lamps: NGC 4189, NGC 2552, and NGC 3104 observed with LR-R, because these calibrations are even more precise, with RMS<0.5kms≻1(see Fig. 4). The median RMS values in Åfor LR-B, LR-V, and LR-R are 0.019, 0.030, and 0.020, respectively, and the value is 0.020 for the whole sample. We find that the RMS represents only 2.4% (LR-B), 3.2% (LR-V), and 1.8% (LR-R) of the reciprocal linear dispersion of each VPH (see Table 2). In Fig. 4, we show the average of the wavelength calibration RMS (in km s≻1) 17 DOI: 10.5281/zenodo.1974953 A117, page 5 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 Fig. 4. Wavelength calibration RMS of all observations by VPH. Blue, green, and red histograms represent LR-B, LR-V, and LR-R observations, respectively. tion for each VPH in our sample exposures are 0.090, 0.086, and 0.096 for LR-B, LR-V, and LR-R, respectively. The last correction to fully reduce our images is the fl ux calibration. For this purpose, we used spectra of standard stars available in the ESO spectrophotometric standards database (Oke 1990;Hamuy et al. 1992,1994): BD+33 26 42, HD192281, HR153, HR718, HR1544, HR1996, HR3454, HR4468, HR4554, HR4963, HR5501, HR7596, HR7950, and HR8634. The exposures of standard stars were also examined to determine whether the previously computed traces were still valid for these observations. The task MegaraLcbAcquisition determines the region of the MEGARA IFU field of view in which the standard star is located in order to know in which fibres the spectra to be considered are placed when they are compared with those of CALSPEC. To ensure that we do not miss fl ux when measuring in the image of the star, we computed the position of the centroid using the spectra of three concentric rings around the brightest spaxel (37 spaxels in total). In this step, an atmospheric extinction correction is also applied using a reference file provided by the GTC (King 1985). With this information, we ran the MegaraLcbStdStar task, which produces the sensitivity curve needed to fl ux calibrate our data. This curve was saved in the master_sensitivity.fits file. Figure 5 shows the sensitivity curves for the fl ux calibration obtained during the reduction of the whole sample. Absolute fl ux calibration is difficult to guarantee, but relative fl ux calibration is much more reliable. This is very important when measuring and comparing lines that have been observed with the same VPH. The file master_sensitivity.fits includes information in its headers that is very valuable when the MEGARA observations are analysed later. This information provides the spectral coverage after fl ux calibration in pixels and in Angstroms for at least one fibre (PIXLIMR1-2 and WAVLIMR1-2), common to all fibres (PIXLIMM1-2 and WAVLIMM1-2) and with a proper fl ux calibration (PIXLIMF1-2 and WAVLIMF1-2). The WAVLIMM1- 2and WAVELIMF1-2 ranges are shown in Figure 5using cyan and dashed brown lines, respectively. This steps completes the calibration files that an observation of this kind requires. However, before applying all these corrections, we must verify two important details. The first detail is to confirm that the traces we used are correct for the scientific target image or to decide that we need to apply some offset on these traces, as in previous steps. The second detail is to determine whether any diffuse light in these images might spoil the observation because in some exposures, moonlight managed to sneak Fig. 5. Sensitivity curves for the fl ux calibration of all MEGADES observations. Panels (a), (b), and (c) show the sensitivity curves derived from all the standard stars observed with the LR-B, LR-V, and LR-R gratings, respectively. Cyan lines mark the spectral coverage after fl ux calibration in Angstroms for all fibres. Dashed brown lines indicate the spectral coverage after fl ux calibration in Angstroms, with a proper fl ux calibration. into the detector. Fortunately, this light only adds a few counts to the image and can easily be removed with one of the megaratools,megaratools-diffuse_light. This tool makes a model of the diffuse light using information from the regions of the CCD that are not illuminated by the fibres. This model allows us to eliminate all traces of diffuse light from our observations. The obser- Article number, page 6 of 106 Fig. 4. Wavelength calibration RMS of all observations by VPH. Blue, green, and red histograms represent LR-B, LR-V, and LR-R observations, respectively. for each observation, separated by VPH, of the fittings after all observations are calibrated in wavelength. MEGARA transmits the light from the focal plane of the telescope to the spectrograph via optical fibres. This means that each fibre transmits the light in a different way and with different wavelength dependences. The fibre-specific calibration of the variation in transmission as a function of wavelength is done with the MegaraFiberFlatImage task using the same images as were used for the MegaraTraceMap recipe. The median of the standard deviation values of the fiber-to-fiber sensitivity variation for each VPH in our sample exposures are 0.090, 0.086, and 0.096 for LR-B, LR-V, and LR-R, respectively. The last correction to fully reduce our images is the flux calibration. For this purpose, we used spectra of standard stars available in the ESO spectrophotometric standards database (Oke 1990;Hamuy et al. 1992,1994): BD+33 26 42, HD 192281, HR153, HR718, HR1544, HR1996, HR3454, HR4468, HR4554, HR4963, HR5501, HR7596, HR7950, and HR8634. The exposures of standard stars were also examined to determine whether the previously computed traces were still valid for these observations. The task MegaraLcbAcquisition determines the region of the MEGARA IFU field of view in which the standard star is located in order to know in which fibres the spectra to be considered are placed when they are compared with those of CALSPEC. To ensure that we do not miss flux when measuring in the image of the star, we computed the position of the centroid using the spectra of three concentric rings around the brightest spaxel (37 spaxels in total). In this step, an atmospheric extinction correction is also applied using a reference file provided by the GTC (King 1985). With this information, we ran the MegaraLcbStdStar task, which produces the sensitivity curve needed to flux calibrate our data. This curve was saved in the master_sensitivity.fits file. Figure 5shows the sensitivity curves for the flux calibration obtained during the reduction of the whole sample. Absolute flux calibration is difficult to guarantee, but relative flux calibration is much more reliable. This is very important when measuring and comparing lines that have been observed with the same VPH. The file master_sensitivity.fits includes information in its headers that is very valuable when the MEGARA observations are analysed later. This information provides the spectral coverage after flux calibration in pixels and in Angstroms for at least one fibre (PIXLIMR1-2 and WAVLIMR1-2), common to all fibres A&A proofs: manuscript no. MEGADES_DR1 Fig. 4. Wavelength calibration RMS of all observations by VPH. Blue, green, and red histograms represent LR-B, LR-V, and LR-R observations, respectively. tion for each VPH in our sample exposures are 0.090, 0.086, and 0.096 for LR-B, LR-V, and LR-R, respectively. The last correction to fully reduce our images is the fl ux calibration. For this purpose, we used spectra of standard stars available in the ESO spectrophotometric standards database (Oke 1990;Hamuy et al. 1992,1994): BD+33 26 42, HD192281, HR153, HR718, HR1544, HR1996, HR3454, HR4468, HR4554, HR4963, HR5501, HR7596, HR7950, and HR8634. The exposures of standard stars were also examined to determine whether the previously computed traces were still valid for these observations. The task MegaraLcbAcquisition determines the region of the MEGARA IFU field of view in which the standard star is located in order to know in which fibres the spectra to be considered are placed when they are compared with those of CALSPEC. To ensure that we do not miss fl ux when measuring in the image of the star, we computed the position of the centroid using the spectra of three concentric rings around the brightest spaxel (37 spaxels in total). In this step, an atmospheric extinction correction is also applied using a reference file provided by the GTC (King 1985). With this information, we ran the MegaraLcbStdStar task, which produces the sensitivity curve needed to fl ux calibrate our data. This curve was saved in the master_sensitivity.fits file. Figure 5 shows the sensitivity curves for the fl ux calibration obtained during the reduction of the whole sample. Absolute fl ux calibration is difficult to guarantee, but relative fl ux calibration is much more reliable. This is very important when measuring and comparing lines that have been observed with the same VPH. The file master_sensitivity.fits includes information in its headers that is very valuable when the MEGARA observations are analysed later. This information provides the spectral coverage after fl ux calibration in pixels and in Angstroms for at least one fibre (PIXLIMR1-2 and WAVLIMR1-2), common to all fibres (PIXLIMM1-2 and WAVLIMM1-2) and with a proper fl ux calibration (PIXLIMF1-2 and WAVLIMF1-2). The WAVLIMM1- 2and WAVELIMF1-2 ranges are shown in Figure 5using cyan and dashed brown lines, respectively. This steps completes the calibration files that an observation of this kind requires. However, before applying all these corrections, we must verify two important details. The first detail is to confirm that the traces we used are correct for the scientific target image or to decide that we need to apply some offset on these traces, as in previous steps. The second detail is to determine whether any diffuse light in these images might spoil the observation because in some exposures, moonlight managed to sneak Fig. 5. Sensitivity curves for the fl ux calibration of all MEGADES observations. Panels (a), (b), and (c) show the sensitivity curves derived from all the standard stars observed with the LR-B, LR-V, and LR-R gratings, respectively. Cyan lines mark the spectral coverage after fl ux calibration in Angstroms for all fibres. Dashed brown lines indicate the spectral coverage after fl ux calibration in Angstroms, with a proper fl ux calibration. into the detector. Fortunately, this light only adds a few counts to the image and can easily be removed with one of the megaratools,megaratools-diffuse_light. This tool makes a model of the diffuse light using information from the regions of the CCD that are not illuminated by the fibres. This model allows us to eliminate all traces of diffuse light from our observations. The obser- Article number, page 6 of 106 Fig. 5. Sensitivity curves for the flux calibration of all MEGADES observations. Panels a,b, and cshow the sensitivity curves derived from all the standard stars observed with the LR-B, LR-V, and LR-R gratings, respectively. Cyan lines mark the spectral coverage after flux calibration in Angstroms for all fibres. Dashed brown lines indicate the spectral coverage after flux calibration in Angstroms, with a proper flux calibration. (PIXLIMM1-2 and WAVLIMM1-2) and with a proper flux calibration (PIXLIMF1-2 and WAVLIMF1-2). The WAVLIMM1-2 and WAVELIMF1-2 ranges are shown in Fig. 5using cyan and dashed brown lines, respectively. This steps completes the calibration files that an observation of this kind requires. However, before applying all these corrections, we must verify two important details. The first detail is A117, page 6 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey to confirm that the traces we used are correct for the scientific target image or to decide that we need to apply some offset on these traces, as in previous steps. The second detail is to determine whether any diffuse light in these images might spoil the observation because in some exposures, moonlight managed to sneak into the detector. Fortunately, this light only adds a few counts to the image and can easily be removed with one of the megaratools,megaratools-diffuse_light. This tool makes a model of the diffuse light using information from the regions of the CCD that are not illuminated by the fibres. This model allows us to eliminate all traces of diffuse light from our observations. The observations affected by this diffuse light are identified in Table A.1 with the dagger. Finally, we applied all the corrections calculated in the data reduction process, including correction for diffuse light, if necessary. For this purpose, we ran the MegaraLcbImage task with the science images. This task, in addition to applying all the corrections described in this section, also subtracts an average spectrum of the sky background measured simultaneously on the outermost 56 fibres of the MEGARA MOS. As final products, we have several images in row-stacked spectra (RSS) format. This format consists of a 2D image with 623 rows, one for each fibre (567 target and 56 sky background fibres) and 4300 columns of spectral information. The most relevant products we have at the end of the data reduction process with the MEGARA DRP are final_rss.fits, which is the reduced science image with sky subtraction applied, reduced_rss.fits, which is the reduced science image that still includes the sky background, and sky_rss.fits, which contains the sky background information. The images we used for our analysis are the final_rss.fits. There is one final caveat before we start the pertinent analysis. If there is too much contrast between the brightest spaxel and the adjacent fibres in the final_rss.fits, there may be crosstalk in these fibres that the ModelMap could not account for. This usually happens when the galaxy is not well centred in the IFU. We must take this into account to avoid drawing incorrect conclusions when this effect is noticeable. 4.2. Post-processing 4.2.1. Astrometry correction We may wish to compare our observations with observations from other studies, either photometric or spectroscopic. We are therefore interested in keeping the coordinates of our pointings as precise as possible. The GTC website claims that the pointing accuracy of the telescope is around 1–2arcsec. For this reason, we verified whether the coordinates that appear in the headers of our images correspond to the real coordinates of the objects. To do this, we compared our observations with the images available in the Pan-STARRS survey (Chambers et al. 2016) and measured the offsets between the peak of the brightest contours in the Pan-STARRS images and the brightest spaxel in the MEGARA observations. This procedure allowed us to ensure that our pointing is correct with an error ≤1 spaxel (0.62′′). Figure 6 shows the offsets we applied to our observations, both in right ascension and declination, to match the Pan-STARRS pointing. In most cases, the deviation of the targets clearly follows the same trend. The information of the new pointing has been included in the header of the final_rss.fits images by updating the following keywords: RADEG,DECDEG,RA, and Dec from extension 0 and CRVAL1 and CRVAL2 from extension 1 (FIBERS extension). The FIBERS extension is the one used by the cube megaratool. M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey vations affected by this diffuse light are identified in Table A.1 with the dagger. Finally, we applied all the corrections calculated in the data reduction process, including correction for diffuse light, if necessary. For this purpose, we ran the MegaraLcbImage task with the science images. This task, in addition to applying all the corrections described in this section, also subtracts an average spectrum of the sky background measured simultaneously on the outermost 56 fibres of the MEGARA MOS. As final products, we have several images in row-stacked spectra (RSS) format. This format consists of a 2D image with 623 rows, one for each fibre (567 target and 56 sky background fibres) and 4300 columns of spectral information. The most relevant products we have at the end of the data reduction process with the MEGARA DRP are final_rss.fits, which is the reduced science image with sky subtraction applied, reduced_rss.fits, which is the reduced science image that still includes the sky background, and sky_rss.fits, which contains the sky background information. The images we used for our analysis are the final_rss.fits. There is one final caveat before we start the pertinent analysis. If there is too much contrast between the brightest spaxel and the adjacent fibres in the final_rss.fits, there may be crosstalk in these fibres that the ModelMap could not account for. This usually happens when the galaxy is not well centred in the IFU. We must take this into account to avoid drawing incorrect conclusions when this effect is noticeable. 4.2. Post-processing 4.2.1. Astrometry correction We may wish to compare our observations with observations from other studies, either photometric or spectroscopic. We are therefore interested in keeping the coordinates of our pointings as precise as possible. The GTC website claims that the pointing accuracy of the telescope is around 1 to 2arcsec. For this reason, we verified whether the coordinates that appear in the headers of our images correspond to the real coordinates of the objects. To do this, we compared our observations with the images available in the Pan-STARRS survey (Chambers et al. 2016) and measured the offsets between the peak of the brightest contours in the Pan- STARRS images and the brightest spaxel in the MEGARA observations. This procedure allowed us to ensure that our pointing is correct with an error ≤1 spaxel (0.6200). Figure 6shows the offsets we applied to our observations, both in right ascension and declination, to match the Pan-STARRS pointing. In most cases, the deviation of the targets clearly follows the same trend. The information of the new pointing has been included in the header of the final_rss.fits images by updating the following keywords: RADEG,DECDEG,RA, and DEC from extension 0 and CRVAL1 and CRVAL2 from extension 1 (FIBERS extension). The FIBERS extension is the one used by the cube megaratool. 4.2.2. Voronoi binning A systematic procedure was followed to analyse all the MEGADES data, using the final RSS as a departure point. First we separated the stellar signal from the interstellar contribution in our spectra. However, if our data are to be sufficiently robust to make this distinction, we must perform a Voronoi binning first. We used the Voronoi binning method by Cappellari & Copin (2003) to reach a signal-to-noise ratio (S/N) per angstrom of 10 at least. We calculated this signal-to-noise ratio in the continuum near the spectral lines of interest in each spectral range Fig. 6. Offsets applied to all MEGADES sample images for pointing correction. The blue, green, and red dots represent the offsets in the LR-B, LR-V, and LR-R observations, respectively. and took the redshift of each galaxy into account. For LR-B, we measured it between 4800Å and 4850Å, for LR-V between 5920Å and 5970Å,and for LR-R between 6604Å and 6654Å (all rest-frame). We recall that each observation will have a different Voronoi binning independent from the rest of the observations because it only depends on the signal-to-noise ratio we measure in the spaxels of each exposure. Figure 7(bottom panel) shows the S/N as a function of the distance to the brightest spaxel in each observation for all spaxels in the MEGADES sample separated by VPH. The solid lines represent the median S/N value for each distance, and the dashed lines represent the corresponding 5th and 95th percentile bin. The S/N values decrease away from the centre of the galaxies, as expected. Furthermore, the small differences that may exist between the different VPHs become smaller with distance from the brightest spaxel. In the top panel of Figure 7, we show the surface AB magnitude per spaxel as a function of distance to the brightest spaxel, in a similar way as in the S/N figure. In this case, the behaviour of the curves is similar to that of the S/N because the noise level in the whole detector is rather homogeneous. Out of the 65905 spaxels in our sample, 32493 (∼49%) have an S/N below 10. This means that all these spaxels are combined within a Voronoi region in their corresponding observation, and the rest of them are analysed individually. After performing the Voronoi binning of the data, we find that 91.6 % of all Voronoi regions in the sample consist of 3 or fewer spaxels. The median S/N values plotted in Figure 7and their intersection with the horizontal dashed line, which represents the S/N cut we made to create the Voronoi regions, show that we reach in single spaxels a distance of 2 arcsec, 3.5 arcsec, and 4 arcsec for the LR-B, LR-V, and LR-R observations, respectively. The average sample distance is 34.8Mpc; therefore, this means that we can reach 0.33kpc (LR-B), 0.58kpc (LR-V), and 0.66kpc (LR-R) without binning. 5. Analysis For the analysis of the stellar continuum (and its subtraction for the line analysis), the same software as was used for the pilot study of the MEGADES sample performed in Chamorro- Cazorla et al. 2022 was employed; the penalized pixel-fitting (pPXF) by Cappellari & Emsellem 2004 (see also Cappellari 2017). pPXF enables us to determine the kinematic characteristics of the stellar component of galaxies and their stellar popu- Article number, page 7 of 106 Fig. 6. Offsets applied to all MEGADES sample images for pointing correction. The blue, green, and red dots represent the offsets in the LR- B, LR-V, and LR-R observations, respectively. 4.2.2. Voronoi binning A systematic procedure was followed to analyse all the MEGADES data, using the final RSS as a departure point. First we separated the stellar signal from the interstellar contribution in our spectra. However, if our data are to be sufficiently robust to make this distinction, we must perform a Voronoi binning first. We used the Voronoi binning method by Cappellari & Copin (2003) to reach a signal-to-noise ratio (S/N) per angstrom of 10 at least. We calculated this signal-to-noise ratio in the continuum near the spectral lines of interest in each spectral range and took the redshift of each galaxy into account. For LR-B, we measured it between 4800 Åand 4850 Å, for LR-V between 5920 Å and 5970Å,and for LR-R between 6604Åand 6654Å(all restframe). We recall that each observation will have a different Voronoi binning independent from the rest of the observations because it only depends on the signal-to-noise ratio we measure in the spaxels of each exposure. Figure 7(bottom panel) shows the S/N as a function of the distance to the brightest spaxel in each observation for all spaxels in the MEGADES sample separated by VPH. The solid lines represent the median S/N value for each distance, and the dashed lines represent the corresponding 5th and 95th percentile bin. The S/N values decrease away from the centre of the galaxies, as expected. Furthermore, the small differences that may exist between the different VPHs become smaller with distance from the brightest spaxel. In the top panel of Fig. 7, we show the surface AB magnitude per spaxel as a function of distance to the brightest spaxel, in a similar way as in the S/N figure. In this case, the behaviour of the curves is similar to that of the S/N because the noise level in the whole detector is rather homogeneous. Out of the 65905 spaxels in our sample, 32 493 (∼49%) have an S/N below 10. This means that all these spaxels are combined within a Voronoi region in their corresponding observation, and the rest of them are analysed individually. After performing the Voronoi binning of the data, we find that 91.6% of all Voronoi regions in the sample consist of 3 or fewer spaxels. The median S/N values plotted in Fig. 7and their intersection with the horizontal dashed line, which represents the S/N cut we made to create the Voronoi regions, show that we reach in single spaxels a distance of 2 arcsec, 3.5arcsec, and 4 arcsec for the LR-B, LR-V, and LR-R observations, respectively. The average sample distance is 34.8Mpc; therefore, this means that we can reach 0.33 kpc (LR-B), 0.58 kpc (LR-V), and 0.66kpc (LR-R) without binning. A117, page 7 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 Fig. 7. Surface AB magnitude per spaxel and signal-to-noise ratio per Angstrom as a function of distance to the brightest spaxel for all spaxels in the MEGADES sample separated by VPH. Top panel: Surface AB magnitude per spaxel for all the spaxels in the sample as a function of the distance. In both cases, the solid lines represent the median S/N value for each distance and VPH, and the dashed lines encompass the 5th and 95th percentiles for each of them. Blue, green, and red correspond to the measurements for the LR-B, LR-V, and LR-R observations, respectively. Bottom panel: Signal-to-noise ratio per Angstrom of all the spaxels in the sample as a function of the distance. The dashed horizontal line identifies the S/N 10 value. lations (which will be discussed in future papers) in addition to enabling us to discern the features that have a stellar origin and those that do not. In section 5.1 we describe in detail how we applied this software to our data. One of the products we obtain from the pPXF analysis are the residuals that remain after the best fit is subtracted from the original data. This means that all features found in these residual spectra, in emission and absorption, do not have a stellar origin. This information allows us to study the interstellar gas in the ionised and neutral phases present in these galaxies. However, in contrast to the stellar information, the interstellar spectral lines are not analysed from a Voronoi binned region, but are analysed spaxel by spaxel. This means that we have to use the best-fitting spectra of the underlying stellar populations in Voronoi regions to subtract the stellar continuum from individual spaxels. The continuum level differs between the Voronoi regions and the induvidual spaxels that comprise these regions, therefore, we need to normalise each best-fitting Voronoi spectrum to the continuum level of the original spaxel in order to correctly subtract the stellar information. Moreover, since we have the continuum level information in the spectral range in which we have measured the signal, close to the lines of interest, we can add the same continuum level to the residuals as in the original data in order to measure the equivalent widths (EW) of the lines of interest in our spectra. In section 5.2 we discuss in detail which lines we studied and the method we applied for this purpose. 5.1. Stellar continuum fi tting To extract all the information of the stellar continuum present in the spectra, we used, as mentioned above, the full spectral fitting analysis software pPXF. This programme is based on the analysis of the absorption lines in order to estimate the stellar populations present in the spectra. This means that it is essential to avoid the emission lines we may have in the spectra from affecting these fits. For this purpose, we masked the spectral regions in which this type of feature was present, and the regions in which the subtraction of the sky lines was not perfect. These masked regions may be different depending on the galaxy that is analysed, as not all of them have the same spectral features. These characteristics can even change from one spaxel to the next within the same observation. In the case of LR-V observations, it is also important to mask the wavelength range corresponding to the sodium doublet (NaI D) in addition to these areas because pPXF distinguishes based on the remaining absorption lines the part of this absorption that comes from the stars and the part that comes from the interstellar medium. In Figure 8we show some examples of these fittings and the different masked regions depending on the analysed galaxy. The process we followed to perform our analysis with pPXF is similar to the one followed in the study by Kacharov et al. (2018). We first analysed the properties of the stellar kinematics using additive and multiplicative polynomials of degree 10. After this step, we already know the velocity, velocity dispersion, skewness, and kurtosis in our data. This allows us to analyse the stellar populations by fixing their kinematic parameters. In this step, where we analyse the stellar populations, we set the degree of the additive polynomials to 0 and keep the degree of the multiplicative polynomials at 10. These latter fittings are used to separate the stellar signal from the interstellar component. Throughout all of our analyses, we use a first-order regularisation with a low factor (R =5; see Kacharov et al. 2018). It is necessary to use stellar population synthesis models in order to be able to fit our spectra. In the case of this survey, we used the stellar population synthesis model predictions (SSP) by Vazdekis et al. (2010) based on the MILES stellar library and Padova+00 isochrones (Sánchez-Blázquez et al. 2006 and Falcón-Barroso et al. 2011). These models (350 in total) cover a very wide age range, from 0.063 Gyr to 17.78 Gyr, and have seven different levels of metallicity ([M/H]): −2.32, −1.71, −1.31, −0.71, −0.40, and 0.00 y +0.22. Its spectral coverage, ranging from 3525Å to 7500Å, perfectly spans the spectral range of the MEGARA VPHs used in this survey. Although the FWHM of the MILES models (2.5Å) is lower than that of our MEGARA observations (R∼6000), the broadening of the lines along the line of sight in the central galaxy regions allows the use of these models. Of all the possible available initial mass functions (IMF), we used a unimodal IMF with a logarithmic slope of 1.3, that is, Salpeter (Salpeter 1955), and did not take any kind of α-enhancement into account as they are not available in these models. 5.2. Emission and absorption lines We followed different strategies for the analysis of the lines, depending on the VPH used for the observation. For the lines observed with LR-B, Hβ, and [OIII]λ5007, as well as for the lines observed within LR-V, that is, NaI D, we employed the spectra obtained from the residuals of the stellar populations with a constant fl ux bias added to match the level of the original (reduced) spectra for EW measurement purposes. However, for the Article number, page 8 of 106 Fig. 7. Surface AB magnitude per spaxel and signal-to-noise ratio per Angstrom as a function of distance to the brightest spaxel for all spaxels in the MEGADES sample separated by VPH. Top panel: Surface AB magnitude per spaxel for all the spaxels in the sample as a function of the distance. In both cases, the solid lines represent the median S/N value for each distance and VPH, and the dashed lines encompass the 5th and 95th percentiles for each of them. Blue, green, and red correspond to the measurements for the LR-B, LR-V, and LR-R observations, respectively. Bottom panel: Signal-to-noise ratio per Angstrom of all the spaxels in the sample as a function of the distance. The dashed horizontal line identifies the S/N 10 value. 5. Analysis For the analysis of the stellar continuum (and its subtraction for the line analysis), the same software as was used for the pilot study of the MEGADES sample performed in Chamorro- Cazorla et al. 2022 was employed; the penalized pixel-fitting (pPXF) by Cappellari & Emsellem 2004 (see also Cappellari 2017). pPXF enables us to determine the kinematic characteristics of the stellar component of galaxies and their stellar populations (which will be discussed in future papers) in addition to enabling us to discern the features that have a stellar origin and those that do not. In Sect. 5.1, we describe in detail how we applied this software to our data. One of the products we obtain from the pPXF analysis are the residuals that remain after the best fit is subtracted from the original data. This means that all features found in these residual spectra, in emission and absorption, do not have a stellar origin. This information allows us to study the interstellar gas in the ionised and neutral phases present in these galaxies. However, in contrast to the stellar information, the interstellar spectral lines are not analysed from a Voronoi binned region, but are analysed spaxel by spaxel. This means that we have to use the best-fitting spectra of the underlying stellar populations in Voronoi regions to subtract the stellar continuum from individual spaxels. The continuum level differs between the Voronoi regions and the induvidual spaxels that comprise these regions, therefore, we need to normalise each best-fitting Voronoi spectrum to the continuum level of the original spaxel in order to correctly subtract the stellar information. Moreover, since we have the continuum level information in the spectral range in which we have measured the signal, close to the lines of interest, we can add the same continuum level to the residuals as in the original data in order to measure the equivalent widths (EW) of the lines of interest in our spectra. In Sect. 5.2 we discuss in detail which lines we studied and the method we applied for this purpose. 5.1. Stellar continuum fitting To extract all the information of the stellar continuum present in the spectra, we used, as mentioned above, the full spectral fitting analysis software pPXF. This programme is based on the analysis of the absorption lines in order to estimate the stellar populations present in the spectra. This means that it is essential to avoid the emission lines we may have in the spectra from affecting these fits. For this purpose, we masked the spectral regions in which this type of feature was present, and the regions in which the subtraction of the sky lines was not perfect. These masked regions may be different depending on the galaxy that is analysed, as not all of them have the same spectral features. These characteristics can even change from one spaxel to the next within the same observation. In the case of LR-V observations, it is also important to mask the wavelength range corresponding to the sodium doublet (NaI D) in addition to these areas because pPXF distinguishes based on the remaining absorption lines the part of this absorption that comes from the stars and the part that comes from the interstellar medium. In Fig. 8we show some examples of these fittings and the different masked regions depending on the analysed galaxy. The process we followed to perform our analysis with pPXF is similar to the one followed in the study by Kacharov et al. (2018). We first analysed the properties of the stellar kinematics using additive and multiplicative polynomials of degree 10. After this step, we already know the velocity, velocity dispersion, skewness, and kurtosis in our data. This allows us to analyse the stellar populations by fixing their kinematic parameters. In this step, where we analyse the stellar populations, we set the degree of the additive polynomials to 0 and keep the degree of the multiplicative polynomials at 10. These latter fittings are used to separate the stellar signal from the interstellar component. Throughout all of our analyses, we use a first-order regularisation with a low factor (R=5; see Kacharov et al. 2018). It is necessary to use stellar population synthesis models in order to be able to fit our spectra. In the case of this survey, we used the stellar population synthesis model predictions (SSP) by Vazdekis et al. (2010) based on the MILES stellar library and Padova+00 isochrones (Sánchez-Blázquez et al. 2006; Falcón-Barroso et al. 2011). These models (350 in total) cover a very wide age range, from 0.063 Gyr to 17.78 Gyr, and have seven different levels of metallicity ([M/H]): ≻2.32,≻1.71,≻1.31, ≻0.71,≻0.40, and 0.00 and +0.22. Its spectral coverage, ranging from 3525Åto 7500 Å, perfectly spans the spectral range of the MEGARA VPHs used in this survey. Although the FWHM of the MILES models (2.5 Å) is lower than that of our MEGARA observations (R∼6000), the broadening of the lines along the line of sight in the central galaxy regions allows the use of these models. Of all the possible available initial mass functions (IMF), we used a unimodal IMF with a logarithmic slope of 1.3, that is, Salpeter (Salpeter 1955), and did not take any kind of α-enhancement into account as they are not available in these models. 5.2. Emission and absorption lines We followed different strategies for the analysis of the lines, depending on the VPH used for the observation. For the lines A117, page 8 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey Fig. 8. Examples of stellar continuum fitting using pPXF for 2 galaxies of the sample. Top left panel: NGC 0718 spectrum in the LR-B spectral range. Top right panel: NGC 0718 spectrum in the LR-V spectral range. Bottom left panel: NGC 3982 spectrum in the LR-B spectral range. Bottom right panel: NGC 3982 spectrum in the LR-V spectral range. The black lines show the original spectrum observed with MEGARA for these spaxels. The red lines are the best fit performed by pPXF on the data. The green lines are the residuals resulting from subtracting the best model from the original data. The vertical blue regions are areas that were masked during the fitting. lines observed within LR-R, Hα, [NII]λ6584,and the two [SII] lines, [SII]λ6717 and [SII]λ6731, we used a different procedure because in the wavelength range covered by this VPH, not many spectral features are available to fit the stellar populations in a robust way. Therefore, we measured the lines in this spectral range directly on the reduced observations of the galaxy. Only one of the four lines we measured in this setup can be affected by absorption features of variable intensity depending on the different underlying stellar populations present. This is Hα. To solve this problem, we combined the LR-V and LR-R observations so that we could take advantage of the information present in the LR-V spectra to estimate the Hαcomponent in absorption. We then corrected our fl ux and EW measurements for Hαin emission in the following way: EWtotal =EWemission +|EWabsorption| Fluxtotal =EWtotal ×Fluxcontinuum. The pointing of the observations sometimes varies from one VPH to the next in the same galaxy, therefore the spaxel in which we measure the emission may be thought to have a different underlying stellar population as the spaxel in which we measure the absorption. However, since the offsets between observations are rather small (typically 1 spaxel) and the variations in the absorption of the Hαline are not affected at these scales, we find that this correction is not affected by this effect, as will be shown in the MEGADES II paper. All lines with a signal to noise ratio measured at the peak of the line higher than 3 were analysed individually using Gauss- Hermite models, except for NaI D, for which we used an anchored double-Gaussian model. We also fitted the continuum emission around the lines using the information available on both sides of the line. For this task, we made use of one of the tools developed for the analysis of MEGARA observations, the Table 3. Line-fitting window definitions in restframe. Ion λ0Line window Continuum windows [Å] [Å] [Å] Hβ4861.333 4848 - 4877 4828 - 4848 & 4877 - 4892 [OIII]λ5007 5006.843 4997 - 5017 4977 - 4997 & 5017 - 5037 NaI D 5889.950 5883 - 5905 5850 - 5870 & 5910 - 5930 Hα6562.819 6555 - 6573 6513 - 6533 & 6598 - 6618 [NII]λ6584 6583.460 6575 - 6594 6513 - 6533 & 6598 - 6618 [SII]λ6717 6716.440 6707 - 6724 6680 - 6700 & 6751 - 6771 [SII]λ6731 6730.810 6724 - 6741 6680 - 6700 & 6751 - 6771 analyze_rss megaratool. The spectral ranges used for each line are listed in Table 3. 6. Data release MEGADES is a legacy survey, and therefore, we make all data public to the community in order to exploit its full potential. We deliver all our observations reduced and with corrected pointings, ready for science. In addition to the reduced observations, we also deliver the analyses of stellar kinematics performed with pPXF and the measurements of some spectral lines carried out with analyze_rss. The study of the stellar populations was performed on the observations with a Voronoi binning so that all analysed regions reach a signal-to-noise ratio of 10. On the other hand, the study of the spectral lines was performed spaxel by spaxel, without any kind of binning, in order to take full advantage of the spatial resolution of the instrument. In future papers, we will publish our analysis for the stellar populations and diagnostic diagrams using all measured lines. Some of the data included in this data release have already demonstrated their scientific potential in the analysis of stellar kinematics (Dullo et al. 2019) and stellar populations (Chamorro-Cazorla et al. 2022). Other MEGARA observations have also been successfully exploited to study spatially resolved Article number, page 9 of 106 Fig. 8. Examples of stellar continuum fitting using pPXF for 2 galaxies of the sample. Top left panel: NGC 0718 spectrum in the LR-B spectral range. Top right panel: NGC 0718 spectrum in the LR-V spectral range. Bottom left panel: NGC 3982 spectrum in the LR-B spectral range. Bottom right panel: NGC 3982 spectrum in the LR-V spectral range. The black lines show the original spectrum observed with MEGARA for these spaxels. The red lines are the best fit performed by pPXF on the data. The green lines are the residuals resulting from subtracting the best model from the original data. The vertical blue regions are areas that were masked during the fitting. observed with LR-B, Hβ, and [OIII]λ5007, as well as for the lines observed within LR-V, that is, NaI D, we employed the spectra obtained from the residuals of the stellar populations with a constant flux bias added to match the level of the original (reduced) spectra for EW measurement purposes. However, for the lines observed within LR-R, Hα,[NII]λ6584,and the two [SII] lines, [SII]λ6717 and [SII]λ6731, we used a different procedure because in the wavelength range covered by this VPH, not many spectral features are available to fit the stellar populations in a robust way. Therefore, we measured the lines in this spectral range directly on the reduced observations of the galaxy. Only one of the four lines we measured in this setup can be affected by absorption features of variable intensity depending on the different underlying stellar populations present. This is Hα. To solve this problem, we combined the LR-V and LR-R observations so that we could take advantage of the information present in the LR-V spectra to estimate the Hαcomponent in absorption. We then corrected our flux and EW measurements for Hαin emission in the following way: EWtotal =EWemission +|EWabsorption| Fluxtotal =EWtotal ×Fluxcontinuum. The pointing of the observations sometimes varies from one VPH to the next in the same galaxy, therefore the spaxel in which we measure the emission may be thought to have a different underlying stellar population as the spaxel in which we measure the absorption. However, since the offsets between observations are rather small (typically 1 spaxel) and the variations in the absorption of the Hαline are not affected at these scales, we find that this correction is not affected by this effect, as will be shown in the MEGADES II paper. All lines with a signal to noise ratio measured at the peak of the line higher than 3 were analysed individually using Gauss–Hermite models, except for NaI D, for which we used Table 3. Line-fitting window definitions in restframe. Ion λ0Line window Continuum windows (Å) (Å) (Å) Hβ4861.333 4848–4877 4828–4848 & 4877–4892 [OIII]λ5007 5006.843 4997–5017 4977–4997 & 5017–5037 NaI D 5889.950 5883–5905 5850–5870 & 5910–5930 Hα6562.819 6555–6573 6513–6533 & 6598–6618 [NII]λ6584 6583.460 6575–6594 6513–6533 & 6598–6618 [SII]λ6717 6716.440 6707–6724 6680–6700 & 6751–6771 [SII]λ6731 6730.810 6724–6741 6680–6700 & 6751–6771 an anchored double-Gaussian model. We also fitted the continuum emission around the lines using the information available on both sides of the line. For this task, we made use of one of the tools developed for the analysis of MEGARA observations, the analyze_rss megaratool. The spectral ranges used for each line are listed in Table 3. 6. Data release MEGADES is a legacy survey, and therefore, we make all data public to the community in order to exploit its full potential. We deliver all our observations reduced and with corrected pointings, ready for science. In addition to the reduced observations, we also deliver the analyses of stellar kinematics performed with pPXF and the measurements of some spectral lines carried out with analyze_rss. The study of the stellar populations was performed on the observations with a Voronoi binning so that all analysed regions reach a signal-to-noise ratio of 10. On the other hand, the study of the spectral lines was performed spaxel by spaxel, without any kind of binning, in order to take full advantage of the spatial resolution of the instrument. In future A117, page 9 of 106 A&A 670, A117 (2023) Gunn, J. E., & Gott, J. Richard, I. 1972, ApJ, 176, 1 Hamuy, M., Walker, A. R., Suntzeff, N. B., et al. 1992, PASP, 104, 533 Hamuy, M., Suntzeff, N. B., Heathcote, S. R., et al. 1994, PASP, 106, 566 Hernandez, O., Carignan, C., Amram, P., Chemin, L., & Daigle, O. 2005, MNRAS, 360, 1201 Kacharov, N., Neumayer, N., Seth, A. 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M., Wuyts, S., et al. 2015, ApJ, 799, 209 Wright, E. L. 2006, PASP, 118, 1711 A117, page 16 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey Appendix A: Additional material M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey Appendix A: Additional material Fig. A.1. MEGADES sample: RGB images from PanSTARRS observations (g, r, and i filters). The white box in the centre of each panel indicates the MEGARA IFU FoV. Article number, page 17 of 106 Fig. A.1. MEGADES sample: RGB images from PanSTARRS observations (g, r, and i filters). The white box in the centre of each panel indicates the MEGARA IFU FoV. A117, page 17 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 Fig. A.1. (cont.) MEGADES sample: RGB images from PanSTARRS observations (g, r, and i filters). The white box in the centre of each panel indicates the MEGARA IFU FoV. Article number, page 18 of 106 Fig. A.1. (cont.) MEGADES sample: RGB images from PanSTARRS observations (g, r, and i filters). The white box in the centre of each panel indicates the MEGARA IFU FoV. A117, page 18 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey Table A.1. Observing log. LR-B LR-V LR-R Galaxy Date secz* texp Date secz* texp Date secz* texp IC 1683 – – – 19 Sep. 2018 1.2 5×720 19 Sep. 2018 1.01 5×720 NGC 0023 – – – 22 Sep. 2019 1.03 3×1200 22 Sep. 2019 1.14 3×1200 NGC 0600 27 Sep. 2019 1.24 3×1200 27 Sep. 2019 1.34 3×1200 27 Sep. 2019 1.48 3×1200 NGC 0716 – – – 31 Dec. 2018 1.04 5×720 31 Dec. 2018 1.06 5×720 NGC 0718 12 Oct. 2018†1.45 3×1200 02 Oct. 2018†1.1 3×1200 02 Oct. 2018†1.13 3×1200 NGC 1042 24 Oct. 2019 1.34 3×1200 24 Oct. 2019 1.26 3×1200 24 Oct. 2019 1.29 3×1200 NGC 1087 06 Nov. 2018†1.17 3×1200 30 Nov. 2018†1.21 3×1200 06 Nov. 2018 1.36 3×1200 NGC 2500 02 Dec. 2018†1.13 3×1200 02 Dec. 2018†1.09 3×600 02 Dec. 2018†1.08 3×1200 NGC 2537 08 May 2019 1.28 3×1200 04 Dec. 2019 1.31 3×1200 03 Dec. 2018†1.05 3×1200 NGC 2543 – – – 30 Nov. 2018 1.06 5×720 30 Nov. 2018 1.01 5×720 NGC 2552 01 Dec. 2019 1.15 3×1200 01 Dec. 2019 1.08 3×1200 01 Dec. 2019 1.07 3×1200 NGC 2967 30 Jan. 2019†1.26 3×1200 30 Jan. 2019†1.15 3×1200 30 Jan. 2019†1.15 3×1200 NGC 3104 02 Dec. 2019 1.11 3×1200 02 Dec. 2019 1.26 3×1200 02 Dec. 2019 1.33 3×1200 NGC 3485 02 Jan. 2019†1.12 3×1200 02 Jan. 2019†1.12 3×1200 11 Jan. 2019†1.12 3×1200 NGC 3507 03 Jan. 2019†1.02 3×1200 03 Jan. 2019†1.04 3×1200 03 Jan. 2019†1.1 3×1200 NGC 3780 31 Dec. 2019 1.29 3×1200 31 Dec. 2019 1.18 3×1200 01 Feb. 2019†1.24 3×1200 NGC 3893 12 Jan. 2019†1.06 3×1200 11 Jan. 2019†1.06 3×1200 11 Jan. 2019†1.08 3×1200 NGC 3982 20 Mar. 2021 1.14 3×1200 19 Mar. 2021 1.21 3×1200 19 Mar. 2021 1.25 3×1200 NGC 3998 15 Mar. 2021†1.24 3×1200 15 Mar. 2021 1.4 3×1200 – – – NGC 4037 14 Mar. 2021†1.05 3×1200 14 Mar. 2021 1.13 3×1200 15 Mar. 2021 1.07 3×1200 NGC 4041 14 Jan. 2019†1.39 3×1200 14 Jan. 2019†1.26 3×1200 01 Feb. 2019†1.22 3×1200 NGC 4189 07 May 2019 1.07 3×1200 08 May 2019 1.18 3×1200 08 May 2019 1.43 3×1200 NGC 4278 08 May 2019 1.01 3×1200 09 May 2019 1.07 3×1200 – – – NGC 4593 08 Feb. 2019 1.22 3×1200 06 May 2019 1.32 3×1200 08 Feb. 2019 1.25 3×1200 NGC 4750 09 Feb. 2019 1.4 3×1200 07 May 2019 1.4 3×1200 07 May 2019 1.55 3×1200 NGC 5218 – – – 19 Mar. 2021 1.21 3×1200 19 Mar. 2021 1.24 3×1200 NGC 5394 – – – 09 May 2019 1.14 3×1200 09 May 2019 1.44 3×1200 NGC 5616 – – – 08 May 2019 1.49 3×1200 02 Aug. 2019 1.45 3×1200 NGC 5953 – – – 19 Mar. 2021 1.03 3×1200 19 Mar. 2021 1.04 3×1200 NGC 5957 25 May 2019 1.07 3×1200 29 May 2019 1.16 3×1200 29 May 2019 1.67 3×1200 NGC 5963 04 May 2021 1.17 3×1200 10 Jun. 2019 1.29 3×1200 10 Jun. 2019 1.21 3×1200 NGC 6027 – – – 06 May 2019 1.07 3×1200 06 May 2019 1.21 3×1200 NGC 6140 27 May 2019†1.27 3×1200 29 May 2019 1.26 3×1200 30 May 2019 1.27 3×1200 NGC 6217 20 Aug. 2018 1.6 3×1200 20 Aug. 2018 1.7 3×1200 21 Aug. 2018†1.84 3×1200 NGC 6339 10 Jul. 2019 1.02 3×1200 11 Jul. 2019 1.07 3×1200 11 Jul. 2019 1.31 3×1200 NGC 6412 30 May 2019 1.48 3×1200 30 May 2019 1.53 3×1200 11 Jun. 2019 1.6 3×1200 NGC 7025 01 Aug. 2017 1.09 3×900 01 Aug. 2017 1.23 3×900 01 Aug. 2017 1.37 3×600 NGC 7437 28 Jul. 2019 1.2 3×1200 28 Jul. 2019 1.03 3×1200 27 Dec. 2019 1.25 3×1200 NGC 7479 30 Jul. 2019 1.24 3×1200 30 Jul. 2019 1.09 3×1200 30 Jul. 2019 1.08 3×1200 NGC 7591 – – – 29 Sep. 2018 1.48 5×720 29 Sep. 2018 1.2 5×720 NGC 7738 – – – 23 Sep. 2019 1.18 3×1200 23 Oct. 2019 1.13 3×1000 NGC 7787 – – – 31 Jul. 2019 1.2 3×1200 31 Jul. 2019 1.13 3×1200 PGC 066559 11 Jul. 2019 1.25 3×1200 11 Jul. 2019 1.26 3×1200 01 Aug. 2019 1.24 3×1200 (†)Observations affected by diffuse light. *Airmass measured at the beginning of the observation. A117, page 19 of 106 A&A 670, A117 (2023) Table A.2. Observing nights. Date Seeing (”) Atm. Conditions 01 Aug. 2017 0.7 – 02 Aug. 2017 1.1 – 20 Aug. 2018 0.6 - 0.7 Clear 21 Aug. 2018 0.8 Clear 19 Sep. 2018 0.9 Clear 29 Sep. 2018 0.8 Clear 02 Oct. 2018 0.7 Clear 12 Oct. 2018 0.9 Clear 06 Nov. 2018 1.0 Clear 30 Nov. 2018 0.8 Clear 02 Dec. 2018 1.0 - 1.1 Clear 03 Dec. 2018 0.8 Clear 31 Dec. 2018 0.8 - 1.0 Clear 02 Jan. 2019 0.9 Clear 03 Jan. 2019 0.8 Clear 11 Jan. 2019 0.9 Clear 12 Jan. 2019 0.9 Clear 14 Jan. 2019 1.1 - 1.2 Clear 30 Jan. 2019 1.2 Clear 01 Feb. 2019 1.2 Clear 08 Feb. 2019 0.7 Photometric 09 Feb. 2019 0.8 Photometric 06 May 2019 0.7 - 0.8 Photometric 07 May 2019 0.6 - 0.8 Photometric 08 May 2019 0.6 - 0.8 Photometric 09 May 2019 0.5 - 0.6 Photometric 25 May 2019 0.8 Clear 27 May 2019 1.0 Clear 29 May 2019 1.0 - 1.1 Clear 30 May 2019 0.9 Photometric 10 Jun. 2019 1.1 - 1.2 Clear 11 Jun. 2019 1.0 Clear 10 Jul. 2019 1.3 Clear 11 Jul. 2019 1.0 - 1.2 Clear 28 Jul. 2019 1.0 Clear 30 Jul. 2019 1.0 Photometric 31 Jul. 2019 0.9 Photometric 01 Aug. 2019 1.0 Photometric 02 Aug. 2019 0.8 Photometric 22 Sep. 2019 0.6 Clear 23 Sep. 2019 1.1 Clear 27 Sep. 2019 0.9 - 1.0 Photometric 23 Oct. 2019 1.2 Clear 24 Oct. 2019 1.1 - 1.2 Clear 01 Dec. 2019 0.6 - 1.1 Clear 02 Dec. 2019 0.6 - 0.7 Clear 04 Dec. 2019 0.9 Clear 27 Dec. 2019 0.9 Clear 31 Dec. 2019 1.1 - 1.2 Spectroscopic 26 Jan. 2020 1.2 Clear 14 Mar. 2021 1.0 Clear 15 Mar. 2021 1.0 Clear 19 Mar. 2021 0.9 - 1.1 Clear 20 Mar. 2021 1.0 Clear 04 May 2021 1.1 Clear A117, page 20 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey Appendix B: Galaxy cards M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey Appendix B: Galaxy cards 1h22m39.6s39.4s39.2s39.0s38.8s38.6s 34◦2602000 1500 1000 0500 RA (J2000) DEC (J2000) (a) IC 1683 0.00000 0.00002 0.00004 0.00006 0.00008 0.00010 Jy 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (c) Stellar v 4750 4800 4850 4900 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (d) Stellar σ 60 80 100 120 140 160 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (e) Stellar h3 −0.04 −0.02 0.00 0.02 0.04 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (f) Stellar h4 −0.025 0.000 0.025 0.050 0.075 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (o) NaI Flux −4−3−2−1 0 erg s−1cm−2˚A−1×10−16 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (p) NaI EW −4−3−2−1 0 ˚A 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (q) NaI v 4700 4800 4900 5000 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (r) NaI line ratio 0.0 0.5 1.0 1.5 Fig. B.1. IC 1683 card. Article number, page 21 of 106 Fig. B.1. IC 1683 card. A117, page 21 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (s) MEGARA RGB IC 1683 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (v) Continuum LR-R 02468 erg s−1cm−2˚A−1×10−17 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (w) HαFlux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−15 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 80 100 ˚A 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (y) Hαv 4700 4800 4900 5000 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (z) Hα σ 20 40 60 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 5 10 15 20 25 30 ˚A 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 4700 4800 4900 5000 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 20 40 60 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0246 erg s−1cm−2˚A−1×10−16 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 2 4 6 8 10 ˚A 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 4700 4800 4900 5000 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 20 40 60 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−16 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 2 4 6 8 10 ˚A 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 4700 4800 4900 5000 km s−1 1h22m39.4s39.2s39.0s38.8s38.6s 34◦2601800 1500 1200 0900 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 20 40 60 km s−1 Fig. B.1. (cont.) IC 1683 card. Article number, page 22 of 106 Fig. B.1. (cont.) IC 1683 card. A117, page 22 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 0h09m54.0s53.8s53.6s53.4s53.2s53.0s 25◦5503000 2500 2000 RA (J2000) DEC (J2000) (a) NGC 0023 0.00000 0.00005 0.00010 0.00015 0.00020 0.00025 0.00030 Jy 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (c) Stellar v 4400 4500 4600 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (d) Stellar σ 80 100 120 140 160 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (e) Stellar h3 −0.05 0.00 0.05 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (f) Stellar h4 0.00 0.05 0.10 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (o) NaI Flux −6−4−2 erg s−1cm−2˚A−1×10−16 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (p) NaI EW −3−2−1 ˚A 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (q) NaI v 4400 4450 4500 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (r) NaI line ratio 0.2 0.4 0.6 0.8 Fig. B.2. NGC 0023 card. Article number, page 23 of 106 Fig. B.2. NGC 0023 card. A117, page 23 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 0023 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (u) Continuum LR-V 0123 erg s−1cm−2˚A−1×10−16 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (v) Continuum LR-R 0 1 2 3 erg s−1cm−2˚A−1×10−16 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (w) HαFlux 02468 erg s−1cm−2˚A−1×10−15 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (x) HαEW 0 50 100 150 ˚A 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (y) Hαv 4400 4500 4600 4700 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (z) Hα σ 40 60 80 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 01234 erg s−1cm−2˚A−1×10−15 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 20 40 60 ˚A 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 4400 4500 4600 4700 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 40 60 80 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 5 10 15 20 ˚A 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 4400 4500 4600 4700 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 40 60 80 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 5 10 15 ˚A 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 4400 4500 4600 4700 km s−1 0h09m53.8s53.6s53.4s53.2s53.0s 25◦5503300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 40 60 80 km s−1 Fig. B.2. (cont.) NGC 0023 card. Article number, page 24 of 106 Fig. B.2. (cont.) NGC 0023 card. A117, page 24 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 1h33m05.6s05.4s05.2s05.0s04.8s −7◦1803500 4000 4500 RA (J2000) DEC (J2000) (a) NGC 0600 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 Jy ×10−5 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (c) Stellar v 1790 1800 1810 1820 1830 km s−1 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (d) Stellar σ 53 54 55 56 km s−1 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (e) Stellar h3 −0.01 0.00 0.01 km s−1 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 −0.01 0.00 0.01 km s−1 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (g) HβFlux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (h) HβEW 0.0 2.5 5.0 7.5 10.0 12.5 15.0 ˚A 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (i) Hβv 1830 1840 1850 1860 1870 km s−1 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (j) Hβ σ 10 20 30 km s−1 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 01234 erg s−1cm−2˚A−1×10−17 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 02468 ˚A 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 1830 1840 1850 1860 1870 km s−1 1h33m05.6s05.4s05.2s05.0s −7◦1803600 3900 4200 4500 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 10 20 30 km s−1 Fig. B.3. NGC 0600 card. Article number, page 25 of 106 Fig. B.3. NGC 0600 card. A117, page 25 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 1042 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (t) Continuum LR-B 0123 erg s−1cm−2˚A−1×10−17 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (u) Continuum LR-V 012345 erg s−1cm−2˚A−1×10−17 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (v) Continuum LR-R 01234 erg s−1cm−2˚A−1×10−17 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (w) HαFlux 0 2 4 6 erg s−1cm−2˚A−1×10−16 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (x) HαEW 0 10 20 30 40 ˚A 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (y) Hαv 1350 1360 1370 1380 km s−1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (z) Hα σ 0 10 20 30 km s−1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−16 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0.0 2.5 5.0 7.5 10.0 12.5 15.0 ˚A 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 1350 1360 1370 1380 km s−1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 10 20 30 km s−1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 1 2 3 4 5 ˚A 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 1350 1360 1370 1380 km s−1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 10 20 30 km s−1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 01234 ˚A 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 1350 1360 1370 1380 km s−1 2h40m24.4s24.2s24.0s23.8s23.6s −8◦2505400 5700 2600000 0300 0600 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 10 20 30 km s−1 Fig. B.6. (cont.) NGC 1042 card. Article number, page 32 of 106 Fig. B.6. (cont.) NGC 1042 card. A117, page 32 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905000 5500 3000000 RA (J2000) DEC (J2000) (a) NGC 1087 0 1 2 3 4 Jy ×10−5 2h46m25.4s25.2s25.0s24.8s −0◦2904800 5100 5400 5700 3000000 RA (J2000) DEC (J2000) (c) Stellar v 1460 1480 1500 1520 1540 1560 km s−1 2h46m25.4s25.2s25.0s24.8s −0◦2904800 5100 5400 5700 3000000 RA (J2000) DEC (J2000) (d) Stellar σ 60 80 100 120 km s−1 2h46m25.4s25.2s25.0s24.8s −0◦2904800 5100 5400 5700 3000000 RA (J2000) DEC (J2000) (e) Stellar h3 −0.02 0.00 0.02 0.04 km s−1 2h46m25.4s25.2s25.0s24.8s −0◦2904800 5100 5400 5700 3000000 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (g) HβFlux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−15 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (h) HβEW 0 10 20 30 40 ˚A 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (i) Hβv 1480 1500 1520 1540 1560 1580 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (j) Hβ σ 20 25 30 35 40 45 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0123 erg s−1cm−2˚A−1×10−16 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 2 4 6 8 10 ˚A 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 1480 1500 1520 1540 1560 1580 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 20 25 30 35 40 45 km s−1 Fig. B.7. NGC 1087 card. Article number, page 33 of 106 Fig. B.7. NGC 1087 card. A117, page 33 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 1087 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (t) Continuum LR-B 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−17 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (u) Continuum LR-V 01234 erg s−1cm−2˚A−1×10−17 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (v) Continuum LR-R 0 1 2 3 erg s−1cm−2˚A−1×10−17 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (w) HαFlux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−15 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (x) HαEW 0 50 100 150 ˚A 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (y) Hαv 1480 1500 1520 1540 1560 1580 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (z) Hα σ 20 25 30 35 40 45 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 20 40 60 ˚A 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 1480 1500 1520 1540 1560 1580 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 20 25 30 35 40 45 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−16 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 5 10 15 20 25 ˚A 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 1480 1500 1520 1540 1560 1580 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 20 25 30 35 40 45 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−16 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 5 10 15 20 ˚ A 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 1480 1500 1520 1540 1560 1580 km s−1 2h46m25.6s25.4s25.2s25.0s24.8s −0◦2905100 5400 5700 3000000 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 20 25 30 35 40 45 km s−1 Fig. B.7. (cont.) NGC 1087 card. Article number, page 34 of 106 Fig. B.7. (cont.) NGC 1087 card. A117, page 34 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 8h01m53.5s53.0s52.5s 50◦4402000 1500 1000 RA (J2000) DEC (J2000) (a) NGC 2500 0.0 0.5 1.0 1.5 2.0 Jy ×10−5 8h01m53.5s53.0s52.5s 50◦4402100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (c) Stellar v 500 520 540 km s−1 8h01m53.5s53.0s52.5s 50◦4402100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (d) Stellar σ 55 60 65 70 km s−1 8h01m53.5s53.0s52.5s 50◦4402100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (e) Stellar h3 0.00 0.01 0.02 0.03 km s−1 8h01m53.5s53.0s52.5s 50◦4402100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (f) Stellar h4 −0.01 0.00 0.01 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (g) HβFlux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (h) HβEW 0 5 10 15 20 25 ˚A 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (i) Hβv 500 510 520 530 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (j) Hβ σ 0 5 10 15 20 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−16 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 20 40 60 ˚A 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 500 510 520 530 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 5 10 15 20 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (o) NaI Flux −2−1 0 1 erg s−1cm−2˚A−1×10−17 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (p) NaI EW −6−4−2 0 2 ˚A 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (q) NaI v 300 320 340 360 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (r) NaI line ratio 0.0 0.1 0.2 0.3 0.4 Fig. B.8. NGC 2500 card. Article number, page 35 of 106 Fig. B.8. NGC 2500 card. A117, page 35 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 2500 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−17 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−17 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (v) Continuum LR-R 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−17 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (w) HαFlux 0 2 4 6 erg s−1cm−2˚A−1×10−16 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 ˚A 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (y) Hαv 500 510 520 530 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (z) Hα σ 0 5 10 15 20 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 2 4 6 8 erg s−1cm−2˚A−1×10−17 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0.0 2.5 5.0 7.5 10.0 12.5 ˚A 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 500 510 520 530 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 5 10 15 20 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 02468 erg s−1cm−2˚A−1×10−17 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 2 4 6 8 ˚A 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 500 510 520 530 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 5 10 15 20 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−17 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 2 4 6 ˚A 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 500 510 520 530 km s−1 8h01m53.5s53.0s52.5s 50◦4401800 1500 1200 0900 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 5 10 15 20 km s−1 Fig. B.8. (cont.) NGC 2500 card. Article number, page 36 of 106 Fig. B.8. (cont.) NGC 2500 card. A117, page 36 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 8h13m15.0s14.5s14.0s 45◦5903000 2500 2000 RA (J2000) DEC (J2000) (a) NGC 2537 0.00 0.25 0.50 0.75 1.00 1.25 1.50 1.75 Jy ×10−5 8h13m15.0s14.8s14.6s14.4s14.2s14.0s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (c) Stellar v 440 460 480 km s−1 8h13m15.0s14.8s14.6s14.4s14.2s14.0s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (d) Stellar σ 52.5 55.0 57.5 60.0 62.5 65.0 km s−1 8h13m15.0s14.8s14.6s14.4s14.2s14.0s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (e) Stellar h3 −0.01 0.00 0.01 0.02 km s−1 8h13m15.0s14.8s14.6s14.4s14.2s14.0s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 −0.01 0.00 0.01 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (h) HβEW 0246 ˚A 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (i) Hβv 455 460 465 470 475 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (j) Hβ σ 10 15 20 25 30 35 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 5 10 15 ˚A 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 455 460 465 470 475 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 10 15 20 25 30 35 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s14.0s 45◦5902700 2400 2100 1800 RA (J2000) DEC (J2000) (o) NaI Flux −2−1 0 1 erg s−1cm−2˚A−1×10−17 8h13m15.2s15.0s14.8s14.6s14.4s14.2s14.0s 45◦5902700 2400 2100 1800 RA (J2000) DEC (J2000) (p) NaI EW −3−2−1 0 1 ˚A 8h13m15.2s15.0s14.8s14.6s14.4s14.2s14.0s 45◦5902700 2400 2100 1800 RA (J2000) DEC (J2000) (q) NaI v 280 300 320 340 360 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s14.0s 45◦5902700 2400 2100 1800 RA (J2000) DEC (J2000) (r) NaI line ratio 0.000 0.025 0.050 0.075 0.100 0.125 Fig. B.9. NGC 2537 card. Article number, page 37 of 106 Fig. B.9. NGC 2537 card. A117, page 37 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 2537 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−17 8h13m15.2s15.0s14.8s14.6s14.4s14.2s14.0s 45◦5902700 2400 2100 1800 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−17 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (v) Continuum LR-R 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−17 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (w) HαFlux 0123 erg s−1cm−2˚A−1×10−16 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (x) HαEW 0 5 10 15 20 25 30 ˚A 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (y) Hαv 455 460 465 470 475 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (z) Hα σ 10 15 20 25 30 35 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 012345 erg s−1cm−2˚A−1×10−17 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0246 ˚A 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 455 460 465 470 475 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 10 15 20 25 30 35 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 012345 erg s−1cm−2˚A−1×10−17 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 02468 ˚A 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 455 460 465 470 475 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 10 15 20 25 30 35 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0123 erg s−1cm−2˚A−1×10−17 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0246 ˚A 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 455 460 465 470 475 km s−1 8h13m15.2s15.0s14.8s14.6s14.4s14.2s 45◦5903000 2700 2400 2100 1800 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 10 15 20 25 30 35 km s−1 Fig. B.9. (cont.) NGC 2537 card. Article number, page 38 of 106 Fig. B.9. (cont.) NGC 2537 card. A117, page 38 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502000 1500 1000 RA (J2000) DEC (J2000) (a) NGC 2543 0 1 2 3 4 5 6 7 8 Jy ×10−5 8h12m58.2s58.0s57.8s57.6s57.4s 36◦1502400 2100 1800 1500 1200 RA (J2000) DEC (J2000) (c) Stellar v 2400 2450 2500 2550 km s−1 8h12m58.2s58.0s57.8s57.6s57.4s 36◦1502400 2100 1800 1500 1200 RA (J2000) DEC (J2000) (d) Stellar σ 60 80 100 120 140 160 km s−1 8h12m58.2s58.0s57.8s57.6s57.4s 36◦1502400 2100 1800 1500 1200 RA (J2000) DEC (J2000) (e) Stellar h3 −0.025 0.000 0.025 0.050 0.075 km s−1 8h12m58.2s58.0s57.8s57.6s57.4s 36◦1502400 2100 1800 1500 1200 RA (J2000) DEC (J2000) (f) Stellar h4 −0.04 −0.02 0.00 0.02 0.04 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (o) NaI Flux −2.5−2.0−1.5−1.0−0.5 0.0 erg s−1cm−2˚A−1×10−16 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (p) NaI EW −6−4−2 0 ˚A 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (q) NaI v 2460 2480 2500 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (r) NaI line ratio 0.0 0.5 1.0 1.5 Fig. B.10. NGC 2543 card. Article number, page 39 of 106 Fig. B.10. NGC 2543 card. A117, page 39 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 2543 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (u) Continuum LR-V 02468 erg s−1cm−2˚A−1×10−17 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (v) Continuum LR-R 0 2 4 6 8 erg s−1cm−2˚A−1×10−17 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (w) HαFlux 0 1 2 3 erg s−1cm−2˚A−1×10−15 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 ˚A 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (y) Hαv 2350 2400 2450 2500 2550 2600 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (z) Hα σ 0 20 40 60 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−15 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 5 10 15 20 ˚A 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 2350 2400 2450 2500 2550 2600 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 20 40 60 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 01234 erg s−1cm−2˚A−1×10−16 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 2 4 6 ˚A 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 2350 2400 2450 2500 2550 2600 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 20 40 60 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0123 erg s−1cm−2˚A−1×10−16 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 1 2 3 4 5 6 ˚A 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 2350 2400 2450 2500 2550 2600 km s−1 8h12m58.4s58.2s58.0s57.8s57.6s57.4s 36◦1502100 1800 1500 1200 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 20 40 60 km s−1 Fig. B.10. (cont.) NGC 2543 card. Article number, page 40 of 106 Fig. B.10. (cont.) NGC 2543 card. A117, page 40 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 8h19m21.0s20.5s20.0s 50◦0004000 3500 3000 RA (J2000) DEC (J2000) (a) NGC 2552 0.0 0.5 1.0 1.5 2.0 2.5 3.0 Jy ×10−5 8h19m21.0s20.5s20.0s 50◦0004200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (c) Stellar v 500 520 540 560 km s−1 8h19m21.0s20.5s20.0s 50◦0004200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (d) Stellar σ 54 56 58 60 62 km s−1 8h19m21.0s20.5s20.0s 50◦0004200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (e) Stellar h3 0.000 0.005 0.010 0.015 km s−1 8h19m21.0s20.5s20.0s 50◦0004200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (f) Stellar h4 −0.010 −0.005 0.000 0.005 km s−1 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (g) HβFlux 0246 erg s−1cm−2˚A−1×10−17 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (h) HβEW 0 5 10 15 20 25 ˚A 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (i) Hβv 520 530 540 550 km s−1 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (j) Hβ σ 0 10 20 30 km s−1 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0 1 2 3 4 erg s−1cm−2˚A−1×10−17 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 5 10 15 20 ˚A 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 520 530 540 550 km s−1 8h19m21.0s20.5s20.0s 50◦0003900 3600 3300 3000 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 10 20 30 km s−1 Fig. B.11. NGC 2552 card. Article number, page 41 of 106 Fig. B.11. NGC 2552 card. A117, page 41 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 3485 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 2700 RA (J2000) DEC (J2000) (t) Continuum LR-B 0246 erg s−1cm−2˚A−1×10−17 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 2700 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 2 4 6 erg s−1cm−2˚A−1×10−17 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (v) Continuum LR-R 0 2 4 6 erg s−1cm−2˚A−1×10−17 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (x) HαEW 0 10 20 30 40 ˚A 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (y) Hαv 1410 1420 1430 1440 km s−1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (z) Hα σ 0 10 20 30 km s−1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−15 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0.0 2.5 5.0 7.5 10.0 12.5 15.0 ˚A 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 1410 1420 1430 1440 km s−1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 10 20 30 km s−1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−16 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 1 2 3 4 5 6 ˚A 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 1410 1420 1430 1440 km s−1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 10 20 30 km s−1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−16 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 1 2 3 4 5 6 ˚A 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 1410 1420 1430 1440 km s−1 11h00m02.8s02.6s02.4s02.2s02.0s 14◦5003900 3600 3300 3000 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 10 20 30 km s−1 Fig. B.14. (cont.) NGC 3485 card. Article number, page 48 of 106 Fig. B.14. (cont.) NGC 3485 card. A117, page 48 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1000 0500 RA (J2000) DEC (J2000) (a) NGC 3507 0.00000 0.00002 0.00004 0.00006 0.00008 0.00010 Jy 11h03m25.6s25.4s25.2s25.0s 18◦0801500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (c) Stellar v 940 960 980 1000 km s−1 11h03m25.6s25.4s25.2s25.0s 18◦0801500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (d) Stellar σ 60 80 100 120 km s−1 11h03m25.6s25.4s25.2s25.0s 18◦0801500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (e) Stellar h3 −0.025 0.000 0.025 0.050 0.075 km s−1 11h03m25.6s25.4s25.2s25.0s 18◦0801500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 0.04 km s−1 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (h) HβEW 0246810 ˚A 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 012345 ˚A Fig. B.15. NGC 3507 card. Article number, page 49 of 106 Fig. B.15. NGC 3507 card. A117, page 49 of 106 A&A 670, A117 (2023) A & A proofs: manuscript no. MEGADES_DR1 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (w) HαFlux 0123 erg s−1cm−2˚A−1×10−15 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (x) HαEW 0 10 20 30 40 50 ˚A 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (y) Hαv 960 980 1000 km s−1 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (z) Hα σ 0 20 40 60 80 km s−1 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 5 10 15 20 ˚A 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 02468 ˚A 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−15 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 02468 ˚A 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 960 980 1000 km s−1 11h03m25.4s25.2s25.0s24.8s24.6s 18◦0801500 1200 0900 0600 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 20 40 60 80 km s−1 Fig. B.15. (cont.) NGC 3507 card. Article number, page 50 of 106 Fig. B.15. (cont.) NGC 3507 card. A117, page 50 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 11h39m23.0s22.5s22.0s 56◦1602000 1500 1000 RA (J2000) DEC (J2000) (a) NGC 3780 0 1 2 3 4 5 6 Jy ×10−5 11h39m23.0s22.5s22.0s21.5s 56◦1602100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (c) Stellar v 2350 2375 2400 2425 2450 2475 km s−1 11h39m23.0s22.5s22.0s21.5s 56◦1602100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (d) Stellar σ 60 70 80 90 100 km s−1 11h39m23.0s22.5s22.0s21.5s 56◦1602100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (e) Stellar h3 −0.02 0.00 0.02 0.04 0.06 km s−1 11h39m23.0s22.5s22.0s21.5s 56◦1602100 1800 1500 1200 0900 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 km s−1 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (h) HβEW 0 5 10 15 20 ˚A 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (i) Hβv 2350 2400 2450 km s−1 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (j) Hβ σ 0 10 20 30 40 km s−1 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−17 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 2 4 6 8 10 ˚A 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 2350 2400 2450 km s−1 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 10 20 30 40 km s−1 Fig. B.16. NGC 3780 card. Article number, page 51 of 106 Fig. B.16. NGC 3780 card. A117, page 51 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 3780 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (t) Continuum LR-B 01234 erg s−1cm−2˚A−1×10−17 11h39m23.0s22.5s22.0s 56◦1601800 1500 1200 0900 RA (J2000) DEC (J2000) (u) Continuum LR-V 0246 erg s−1cm−2˚A−1×10−17 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (v) Continuum LR-R 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−17 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (x) HαEW 0 5 10 15 ˚A 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (y) Hαv 2350 2400 2450 km s−1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (z) Hα σ 0 10 20 30 40 km s−1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−17 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0.0 0.5 1.0 1.5 2.0 2.5 3.0 ˚A 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 2350 2400 2450 km s−1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 10 20 30 40 km s−1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−17 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0.0 0.5 1.0 1.5 2.0 ˚A 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 2350 2400 2450 km s−1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 10 20 30 40 km s−1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−17 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 0.5 1.0 1.5 2.0 ˚A 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 2350 2400 2450 km s−1 11h39m22.5s22.0s21.5s 56◦1602100 1800 1500 1200 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 10 20 30 40 km s−1 Fig. B.16. (cont.) NGC 3780 card. Article number, page 52 of 106 Fig. B.16. (cont.) NGC 3780 card. A117, page 52 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 11h48m38.5s38.0s37.5s 48◦4205000 4500 4000 RA (J2000) DEC (J2000) (a) NGC 3893 0.00000 0.00002 0.00004 0.00006 0.00008 0.00010 0.00012 Jy 11h48m38.5s38.0s37.5s 48◦4204500 4200 3900 3600 RA (J2000) DEC (J2000) (c) Stellar v 940 960 980 1000 1020 1040 km s−1 11h48m38.5s38.0s37.5s 48◦4204500 4200 3900 3600 RA (J2000) DEC (J2000) (d) Stellar σ 60 80 100 120 km s−1 11h48m38.5s38.0s37.5s 48◦4204500 4200 3900 3600 RA (J2000) DEC (J2000) (e) Stellar h3 −0.04 −0.02 0.00 0.02 0.04 0.06 km s−1 11h48m38.5s38.0s37.5s 48◦4204500 4200 3900 3600 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 0.04 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (h) HβEW 0.0 2.5 5.0 7.5 10.0 12.5 ˚A 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (i) Hβv 925 950 975 1000 1025 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (j) Hβ σ 20 25 30 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0246 erg s−1cm−2˚A−1×10−17 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 1 2 3 4 ˚A 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 925 950 975 1000 1025 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 20 25 30 km s−1 11h48m38.5s38.0s37.5s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (o) NaI Flux −1.25 −1.00 −0.75 −0.50 −0.25 0.00 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s37.5s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (p) NaI EW −1.5−1.0−0.5 0.0 ˚A 11h48m38.5s38.0s37.5s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (q) NaI v 880 900 920 940 960 km s−1 11h48m38.5s38.0s37.5s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (r) NaI line ratio 0.00 0.25 0.50 0.75 1.00 1.25 Fig. B.17. NGC 3893 card. Article number, page 53 of 106 Fig. B.17. NGC 3893 card. A117, page 53 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 3893 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s37.5s 48◦4204800 4500 4200 3900 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.00 0.25 0.50 0.75 1.00 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (v) Continuum LR-R 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 80 100 ˚A 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (y) Hαv 925 950 975 1000 1025 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (z) Hα σ 20 25 30 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 5 10 15 20 25 ˚A 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 925 950 975 1000 1025 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 20 25 30 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 02468 ˚A 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 925 950 975 1000 1025 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 20 25 30 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 2 4 6 ˚A 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 925 950 975 1000 1025 km s−1 11h48m38.5s38.0s 48◦4204800 4500 4200 3900 3600 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 20 25 30 km s−1 Fig. B.17. (cont.) NGC 3893 card. Article number, page 54 of 106 Fig. B.17. (cont.) NGC 3893 card. A117, page 54 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 11h56m29.0s28.5s28.0s27.5s 55◦0703500 3000 2500 RA (J2000) DEC (J2000) (a) NGC 3982 0.00000 0.00002 0.00004 0.00006 0.00008 0.00010 0.00012 0.00014 Jy 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (c) Stellar v 1080 1100 1120 1140 1160 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (d) Stellar σ 60 70 80 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (e) Stellar h3 −0.02 0.00 0.02 0.04 0.06 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (g) HβFlux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−15 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (h) HβEW 0 5 10 15 ˚A 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (i) Hβv 1080 1100 1120 1140 1160 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (j) Hβ σ 20 40 60 80 100 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−14 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 50 100 150 200 ˚A 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 1080 1100 1120 1140 1160 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 20 40 60 80 100 km s−1 Fig. B.18. NGC 3982 card. Article number, page 55 of 106 Fig. B.18. NGC 3982 card. A117, page 55 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 3982 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (v) Continuum LR-R 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (w) HαFlux 0 2 4 6 erg s−1cm−2˚A−1×10−15 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 ˚A 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (y) Hαv 1080 1100 1120 1140 1160 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (z) Hα σ 20 40 60 80 100 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−15 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 10 20 30 40 50 ˚A 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 1080 1100 1120 1140 1160 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 20 40 60 80 100 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0.0 2.5 5.0 7.5 10.0 12.5 ˚A 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 1080 1100 1120 1140 1160 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 20 40 60 80 100 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−15 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 5 10 15 ˚A 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 1080 1100 1120 1140 1160 km s−1 11h56m28.5s28.0s27.5s 55◦0703600 3300 3000 2700 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 20 40 60 80 100 km s−1 Fig. B.18. (cont.) NGC 3982 card. Article number, page 56 of 106 Fig. B.18. (cont.) NGC 3982 card. A117, page 56 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 11h57m57.0s56.5s56.0s55.5s 55◦2702000 1500 1000 RA (J2000) DEC (J2000) (a) NGC 3998 0.0000 0.0002 0.0004 0.0006 0.0008 Jy 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (c) Stellar v 950 1000 1050 1100 1150 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (d) Stellar σ 175 200 225 250 275 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (e) Stellar h3 −0.025 0.000 0.025 0.050 0.075 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (f) Stellar h4 −0.025 0.000 0.025 0.050 0.075 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (h) HβEW 012345 ˚A 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (i) Hβv 900 1000 1100 1200 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (j) Hβ σ 0 50 100 150 200 250 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 1 2 3 ˚A 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 900 1000 1100 1200 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 50 100 150 200 250 km s−1 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (o) NaD Flux −1.5−1.0−0.5 erg s−1cm−2˚A−1×10−15 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (p) NaD EW −2.5−2.0−1.5 ˚A 11h57m56.5s56.0s55.5s 55◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (q) NaD v 900 1000 1100 1200 km s−1 11 h 57 m 56.5 s 56.0 s 55.5 s 55 ◦ 27 0 18 0 0 15 0 0 12 0 0 09 0 0 RA (J2000) DEC (J2000) (r) NaI line ratio 0.5 1.0 1.5 2.0 2.5 11 h 57 m 56:5 s 56:0 s 55:5 s 55 27 0 18 00 15 00 12 00 09 00 RA (J2000) DEC (J2000) (r) NaI line ratio 0:5 1:0 1:5 2:0 2:5 Fig. B.19. NGC 3998 card. Article number, page 57 of 106 Fig. B.19. NGC 3998 card. A117, page 57 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 4189 12h13m47.6s47.4s47.2s47.0s 13◦2503300 3000 2700 2400 RA (J2000) DEC (J2000) (t) Continuum LR-B 0 2 4 6 erg s−1cm−2˚A−1×10−17 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 2 4 6 erg s−1cm−2˚A−1×10−17 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (v) Continuum LR-R 0 2 4 6 erg s−1cm−2˚A−1×10−17 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (w) HαFlux 01234 erg s−1cm−2˚A−1×10−15 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 ˚A 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (y) Hαv 2100 2120 2140 2160 km s−1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (z) Hα σ 0 20 40 60 km s−1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 5 10 15 20 25 ˚A 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 2100 2120 2140 2160 km s−1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 20 40 60 km s−1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 1 2 3 4 erg s−1cm−2˚A−1×10−16 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0.0 2.5 5.0 7.5 10.0 12.5 ˚A 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 2100 2120 2140 2160 km s−1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 20 40 60 km s−1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 01234 erg s−1cm−2˚A−1×10−16 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 2.5 5.0 7.5 10.0 12.5 ˚A 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 2100 2120 2140 2160 km s−1 12h13m47.6s47.4s47.2s47.0s 13◦2503600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 20 40 60 km s−1 Fig. B.22. (cont.) NGC 4189 card. Article number, page 64 of 106 Fig. B.22. (cont.) NGC 4189 card. A117, page 64 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 12h20m07.4s07.2s07.0s06.8s06.6s06.4s 29◦1605500 5000 4500 RA (J2000) DEC (J2000) (a) NGC 4278 0.00000 0.00005 0.00010 0.00015 0.00020 0.00025 0.00030 Jy 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (c) Stellar v 575 600 625 650 675 700 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (d) Stellar σ 180 200 220 240 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (e) Stellar h3 −0.050 −0.025 0.000 0.025 0.050 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (f) Stellar h4 −0.04 −0.02 0.00 0.02 0.04 0.06 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−15 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (h) HβEW 012345 ˚A 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (i) Hβv 500 600 700 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (j) Hβ σ 50 100 150 200 250 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−15 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 01234 ˚A 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 500 600 700 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 50 100 150 200 250 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (o) NaD Flux −6−5−4−3−2−1 erg s−1cm−2˚A−1×10−16 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (p) NaD EW −2.5−2.0−1.5−1.0−0.5 ˚A 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (q) NaD v 500 600 700 km s−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦160570 0 540 0 510 0 480 0 450 0 RA (J2000) DEC (J2000) (r) NaI line ratio 0.0 0.5 1.0 1.5 2.0 2.5 12 h 20 m 07:2 s 07:0 s 06:8 s 06:6 s 06:4 s 29 16 0 57 00 54 00 51 00 48 00 45 00 RA (J2000) DEC (J2000) (r) NaI line ratio 0:0 0:5 1:0 1:5 2:0 2:5 Fig. B.23. NGC 4278 card. Article number, page 65 of 106 Fig. B.23. NGC 4278 card. A117, page 65 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 12 h 20 m 07.2 s 07.0 s 06.8 s 06.6 s 06.4 s 29 ◦ 16 0 57 0 0 54 0 0 51 0 0 48 0 0 45 0 0 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 4278 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (t) Continuum LR-B 0 10 20 30 erg s−1cm−2˚A−1 12h20m07.2s07.0s06.8s06.6s06.4s 29◦1605700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 10 20 30 erg s−1cm−2˚A−1 Fig. B.23. (cont.) NGC 4278 card. Article number, page 66 of 106 Fig. B.23. (cont.) NGC 4278 card. A117, page 66 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003500 4000 4500 RA (J2000) DEC (J2000) (a) NGC 4593 0.00000 0.00002 0.00004 0.00006 0.00008 0.00010 Jy 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (c) Stellar v 2400 2450 2500 2550 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (d) Stellar σ 80 100 120 140 160 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (e) Stellar h3 −0.05 0.00 0.05 0.10 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (f) Stellar h4 0.00 0.05 0.10 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (h) HβEW 02468 ˚A 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (i) Hβv 2400 2500 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (j) Hβ σ 0 25 50 75 100 125 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−16 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 02468 ˚A 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 2400 2500 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 25 50 75 100 125 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (o) NaD Flux −1.5−1.0−0.5 erg s−1cm−2˚A−1×10−16 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (p) NaD EW −1.5−1.0−0.5 ˚A 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (q) NaD v 2400 2500 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦200330 0 360 0 390 0 420 0 450 0 RA (J2000) DEC (J2000) (r) NaI line ratio 0.0 0.5 1.0 1.5 2.0 12 h 39 m 39:8 s 39:6 s 39:4 s 39:2 s 39:0 s 5 20 0 33 00 36 00 39 00 42 00 45 00 RA (J2000) DEC (J2000) (r) NaI line ratio 0:0 0:5 1:0 1:5 2:0 Fig. B.24. NGC 4593 card. Article number, page 67 of 106 Fig. B.24. NGC 4593 card. A117, page 67 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 12 h 39 m 39.8 s 39.6 s 39.4 s 39.2 s 39.0 s −5 ◦ 20 0 30 0 0 33 0 0 36 0 0 39 0 0 42 0 0 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 4593 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 RA (J2000) DEC (J2000) (t) Continuum LR-B 02468 erg s−1cm−2˚A−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003300 3600 3900 4200 4500 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 2 4 6 8 10 erg s−1cm−2˚A−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (v) Continuum LR-R 02468 erg s−1cm−2˚A−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (w) HαFlux 0 25 50 75 100 125 erg s−1cm−2˚A−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (x) HαEW 0 5 10 15 20 25 ˚A 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (y) Hαv 2400 2500 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (z) Hα σ 0 25 50 75 100 125 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 02468 erg s−1cm−2˚A−1×10−16 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 2 4 6 8 10 ˚A 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 2400 2500 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 25 50 75 100 125 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0.0 0.5 1.0 1.5 2.0 2.5 3.0 ˚A 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 2400 2500 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 25 50 75 100 125 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 0.5 1.0 1.5 2.0 2.5 3.0 ˚A 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 2400 2500 2600 km s−1 12h39m39.8s39.6s39.4s39.2s39.0s −5◦2003000 3300 3600 3900 4200 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 25 50 75 100 125 km s−1 Fig. B.24. (cont.) NGC 4593 card. Article number, page 68 of 106 Fig. B.24. (cont.) NGC 4593 card. A117, page 68 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 12h50m09.0s08.0s07.0s06.0s 72◦5203500 3000 2500 RA (J2000) DEC (J2000) (a) NGC 4750 0 2 4 6 8 Jy ×10−5 12h50m08.0s07.0s06.0s 72◦5203600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (c) Stellar v 1600 1650 1700 km s−1 12h50m08.0s07.0s06.0s 72◦5203600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (d) Stellar σ 80 100 120 140 km s−1 12h50m08.0s07.0s06.0s 72◦5203600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (e) Stellar h3 −0.10 −0.05 0.00 0.05 0.10 km s−1 12h50m08.0s07.0s06.0s 72◦5203600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (f) Stellar h4 0.00 0.05 0.10 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (g) HβFlux 0123 erg s−1cm−2˚A−1×10−16 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (h) HβEW 0 1 2 3 4 5 ˚A 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (i) Hβv 1500 1550 1600 1650 1700 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (j) Hβ σ 0 25 50 75 100 125 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 1 2 3 4 ˚A 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 1500 1550 1600 1650 1700 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 25 50 75 100 125 km s−1 Fig. B.25. NGC 4750 card. Article number, page 69 of 106 Fig. B.25. NGC 4750 card. A117, page 69 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 12 h 50 m 08.0 s 07.0 s 06.0 s 72 ◦ 52 0 33 0 0 30 0 0 27 0 0 24 0 0 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 4750 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (t) Continuum LR-B 0246 erg s−1cm−2˚A−1 12h50m08.0s07.0s06.0s 72◦5203600 3300 3000 2700 2400 RA (J2000) DEC (J2000) (u) Continuum LR-V 02468 erg s−1cm−2˚A−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (v) Continuum LR-R 02468 erg s−1cm−2˚A−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (w) HαFlux 0 20 40 60 80 100 erg s−1cm−2˚A−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (x) HαEW 0 5 10 15 20 ˚A 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (y) Hαv 1500 1550 1600 1650 1700 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (z) Hα σ 0 25 50 75 100 125 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−15 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0.0 2.5 5.0 7.5 10.0 12.5 15.0 ˚A 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 1500 1550 1600 1650 1700 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 25 50 75 100 125 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−16 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 012345 ˚A 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 1500 1550 1600 1650 1700 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 25 50 75 100 125 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−16 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 012345 ˚A 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 1500 1550 1600 1650 1700 km s−1 12h50m08.0s07.0s06.0s 72◦5203300 3000 2700 2400 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 25 50 75 100 125 km s−1 Fig. B.25. (cont.) NGC 4750 card. Article number, page 70 of 106 Fig. B.25. (cont.) NGC 4750 card. A117, page 70 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 13h32m11.0s10.5s10.0s09.5s 62◦4601000 0500 0000 RA (J2000) DEC (J2000) (a) NGC 5218 0.0 0.5 1.0 1.5 2.0 2.5 Jy ×10−5 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (c) Stellar v 2800 2850 2900 2950 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (d) Stellar σ 75 100 125 150 175 200 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (e) Stellar h3 −0.050 −0.025 0.000 0.025 0.050 0.075 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (f) Stellar h4 −0.050 −0.025 0.000 0.025 0.050 0.075 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (o) NaI Flux −2.0−1.5−1.0−0.5 erg s−1cm−2˚A−1×10−16 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (p) NaI EW −6−4−2 ˚A 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (q) NaI v 2800 2850 2900 2950 3000 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (r) NaI line ratio 0.2 0.4 0.6 0.8 1.0 Fig. B.26. NGC 5218 card. Article number, page 71 of 106 Fig. B.26. NGC 5218 card. A117, page 71 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 5218 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 1 2 3 erg s−1cm−2˚A−1×10−17 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (v) Continuum LR-R 0123 erg s−1cm−2˚A−1×10−17 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 80 ˚A 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (y) Hαv 2800 2850 2900 2950 3000 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (z) Hα σ 20 40 60 80 100 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 10 20 30 40 50 ˚A 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 2800 2850 2900 2950 3000 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 20 40 60 80 100 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−16 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 2 4 6 8 10 ˚A 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 2800 2850 2900 2950 3000 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 20 40 60 80 100 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 01234 erg s−1cm−2˚A−1×10−16 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 2 4 6 8 10 12 ˚A 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 2800 2850 2900 2950 3000 km s−1 13h32m11.0s10.5s10.0s09.5s 62◦4600900 0600 0300 0000 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 20 40 60 80 100 km s−1 Fig. B.26. (cont.) NGC 5218 card. Article number, page 72 of 106 Fig. B.26. (cont.) NGC 5218 card. A117, page 72 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 13h58m34.0s33.5s 37◦2702000 1500 1000 RA (J2000) DEC (J2000) (a) NGC 5394 0.00000 0.00005 0.00010 0.00015 0.00020 0.00025 0.00030 0.00035 0.00040 Jy 13h58m34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (c) Stellar v 3400 3420 3440 3460 3480 km s−1 13h58m34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (d) Stellar σ 60 80 100 120 km s−1 13h58m34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (e) Stellar h3 −0.02 0.00 0.02 0.04 0.06 km s−1 13h58m34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 0.04 0.06 km s−1 13h58m34.2s34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (o) NaI Flux −2.0−1.5−1.0−0.5 erg s−1cm−2˚A−1×10−15 13h58m34.2s34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (p) NaI EW −6−5−4−3−2−1 ˚A 13h58m34.2s34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (q) NaI v 3000 3100 3200 3300 3400 3500 km s−1 13h58m34.2s34.0s33.8s33.6s33.4s33.2s 37◦2701800 1500 1200 0900 RA (J2000) DEC (J2000) (r) NaI line ratio 0.0 0.5 1.0 1.5 Fig. B.27. NGC 5394 card. Article number, page 73 of 106 Fig. B.27. NGC 5394 card. A117, page 73 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 15 h 35 m 23.6 s 23.4 s 23.2 s 23.0 s 22.8 s 12 ◦ 02 0 57 0 0 54 0 0 51 0 0 48 0 0 45 0 0 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 5957 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 1 2 3 erg s−1cm−2˚A−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (v) Continuum LR-R 0123 erg s−1cm−2˚A−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (w) HαFlux 0 5 10 15 erg s−1cm−2˚A−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (x) HαEW 0 5 10 15 ˚A 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (y) Hαv 1800 1820 1840 1860 km s−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (z) Hα σ 0 5 10 15 20 25 km s−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 2 4 6 8 erg s−1cm−2˚A−1×10−17 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 02468 ˚A 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 1800 1820 1840 1860 km s−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 10 20 30 40 km s−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−17 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0.0 0.5 1.0 1.5 2.0 2.5 ˚A 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 1800 1820 1840 1860 km s−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 10 20 30 40 km s−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−17 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 0.5 1.0 1.5 2.0 ˚A 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 1800 1820 1840 1860 km s−1 15h35m23.6s23.4s23.2s23.0s22.8s 12◦0205700 5400 5100 4800 4500 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 10 20 30 40 km s−1 Fig. B.30. (cont.) NGC 5957 card. Article number, page 80 of 106 Fig. B.30. (cont.) NGC 5957 card. A117, page 80 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 15h33m28.5s28.0s27.5s27.0s 56◦3304000 3500 3000 RA (J2000) DEC (J2000) (a) NGC 5963 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 Jy ×10−5 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (c) Stellar v 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (d) Stellar σ 50.0 52.5 55.0 57.5 60.0 62.5 65.0 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (e) Stellar h3 −0.01 0.00 0.01 0.02 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (f) Stellar h4 −0.03 −0.02 −0.01 0.00 0.01 km s−1 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (g) HβFlux 01234 erg s−1cm−2˚A−1×10−16 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (h) HβEW 0 5 10 15 20 ˚A 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (i) Hβv 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (j) Hβ σ 10 15 20 25 km s−1 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0.0 2.5 5.0 7.5 10.0 12.5 ˚A 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 10 15 20 25 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (o) NaI Flux −1 0 1 erg s−1cm−2˚A−1×10−17 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (p) NaI EW −1.0−0.5 0.0 0.5 1.0 1.5 ˚A 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (q) NaI v 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (r) NaI line ratio 0.00 0.05 0.10 0.15 Fig. B.31. NGC 5963 card. Article number, page 81 of 106 Fig. B.31. NGC 5963 card. A117, page 81 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 5963 15h33m28.5s28.0s27.5s 56◦3303900 3600 3300 3000 RA (J2000) DEC (J2000) (t) Continuum LR-B 01234 erg s−1cm−2˚A−1×10−17 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 1 2 3 erg s−1cm−2˚A−1×10−17 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (v) Continuum LR-R 0123 erg s−1cm−2˚A−1×10−17 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (x) HαEW 0 25 50 75 100 125 ˚A 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (y) Hαv 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (z) Hα σ 10 15 20 25 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−16 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 10 20 30 40 ˚A 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 10 15 20 25 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 5 10 15 ˚A 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 10 15 20 25 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 2.5 5.0 7.5 10.0 12.5 ˚A 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 620 640 660 680 700 km s−1 15h33m28.5s28.0s27.5s27.0s 56◦3304200 3900 3600 3300 3000 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 10 15 20 25 km s−1 Fig. B.31. (cont.) NGC 5963 card. Article number, page 82 of 106 Fig. B.31. (cont.) NGC 5963 card. A117, page 82 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505500 5000 4500 RA (J2000) DEC (J2000) (a) NGC 6027 0.00000 0.00002 0.00004 0.00006 0.00008 0.00010 Jy 15h59m12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 RA (J2000) DEC (J2000) (c) Stellar v 4300 4350 4400 4450 4500 km s−1 15h59m12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 RA (J2000) DEC (J2000) (d) Stellar σ 100 150 200 km s−1 15h59m12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 RA (J2000) DEC (J2000) (e) Stellar h3 −0.050 −0.025 0.000 0.025 0.050 0.075 km s−1 15h59m12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 0.04 0.06 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (o) NaI Flux −3−2−1 erg s−1cm−2˚A−1×10−16 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (p) NaI EW −6−5−4−3−2−1 ˚A 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (q) NaI v 4000 4020 4040 4060 4080 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (r) NaI line ratio 0.25 0.50 0.75 1.00 1.25 Fig. B.32. NGC 6027 card. Article number, page 83 of 106 Fig. B.32. NGC 6027 card. A117, page 83 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 6027 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (v) Continuum LR-R 02468 erg s−1cm−2˚A−1×10−17 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−15 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (x) HαEW 0 10 20 30 ˚A 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (y) Hαv 4300 4350 4400 4450 4500 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (z) Hα σ 0 20 40 60 80 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−16 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 02468 ˚A 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 4300 4350 4400 4450 4500 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 20 40 60 80 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 012345 ˚A 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 4300 4350 4400 4450 4500 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 20 40 60 80 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 1 2 3 4 5 ˚A 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 4300 4350 4400 4450 4500 km s−1 15h59m13.0s12.8s12.6s12.4s12.2s 20◦4505400 5100 4800 4500 4200 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 20 40 60 80 km s−1 Fig. B.32. (cont.) NGC 6027 card. Article number, page 84 of 106 Fig. B.32. (cont.) NGC 6027 card. A117, page 84 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 16h20m59.0s58.5s58.0s57.5s57.0s 65◦2303000 2500 2000 RA (J2000) DEC (J2000) (a) NGC 6140 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Jy ×10−5 16h20m59.0s58.5s58.0s57.5s57.0s 65◦2303300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (c) Stellar v 880 900 920 km s−1 16h20m59.0s58.5s58.0s57.5s57.0s 65◦2303300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (d) Stellar σ 55 60 65 70 75 80 km s−1 16h20m59.0s58.5s58.0s57.5s57.0s 65◦2303300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (e) Stellar h3 −0.01 0.00 0.01 0.02 km s−1 16h20m59.0s58.5s58.0s57.5s57.0s 65◦2303300 3000 2700 2400 2100 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 −0.01 0.00 0.01 0.02 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (g) HβFlux 0 1 2 3 erg s−1cm−2˚A−1×10−16 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (h) HβEW 0 10 20 30 ˚A 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (i) Hβv 890 900 910 920 930 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (j) Hβ σ 5 10 15 20 25 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 01234 erg s−1cm−2˚A−1×10−16 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 20 40 60 ˚A 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 890 900 910 920 930 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 5 10 15 20 25 km s−1 Fig. B.33. NGC 6140 card. Article number, page 85 of 106 Fig. B.33. NGC 6140 card. A117, page 85 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 6140 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−17 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−17 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (v) Continuum LR-R 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−17 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (x) HαEW 0 50 100 150 200 ˚A 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (y) Hαv 890 900 910 920 930 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (z) Hα σ 5 10 15 20 25 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 1 2 3 4 erg s−1cm−2˚A−1×10−16 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 10 20 30 40 ˚A 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 890 900 910 920 930 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 5 10 15 20 25 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 5 10 15 20 25 ˚A 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 890 900 910 920 930 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 5 10 15 20 25 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−16 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 2.5 5.0 7.5 10.0 12.5 15.0 ˚A 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 890 900 910 920 930 km s−1 16h20m59.0s58.5s58.0s57.5s 65◦2303000 2700 2400 2100 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 5 10 15 20 25 km s−1 Fig. B.33. (cont.) NGC 6140 card. Article number, page 86 of 106 Fig. B.33. (cont.) NGC 6140 card. A117, page 86 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1200000 1105500 5000 RA (J2000) DEC (J2000) (a) NGC 6217 0.0000 0.0001 0.0002 0.0003 0.0004 0.0005 0.0006 0.0007 0.0008 Jy 16h32m40.0s39.0s38.0s37.0s 78◦1200000 1105700 5400 5100 4800 RA (J2000) DEC (J2000) (c) Stellar v 1300 1320 1340 1360 1380 1400 km s−1 16h32m40.0s39.0s38.0s37.0s 78◦1200000 1105700 5400 5100 4800 RA (J2000) DEC (J2000) (d) Stellar σ 60 80 100 120 km s−1 16h32m40.0s39.0s38.0s37.0s 78◦1200000 1105700 5400 5100 4800 RA (J2000) DEC (J2000) (e) Stellar h3 −0.04 −0.02 0.00 0.02 0.04 0.06 km s−1 16h32m40.0s39.0s38.0s37.0s 78◦1200000 1105700 5400 5100 4800 RA (J2000) DEC (J2000) (f) Stellar h4 −0.02 0.00 0.02 0.04 km s−1 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (g) HβFlux 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−14 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (h) HβEW 0 10 20 30 ˚A 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (i) Hβv 1300 1320 1340 1360 1380 1400 km s−1 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (j) Hβ σ 40 60 80 100 km s−1 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0123 erg s−1cm−2˚A−1×10−15 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 5 10 15 ˚A 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 1300 1320 1340 1360 1380 1400 km s−1 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 40 60 80 100 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (o) NaI Flux −5−4−3−2−1 0 erg s−1cm−2˚A−1×10−16 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (p) NaI EW −2−1 0 ˚A 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (q) NaI v 1100 1150 1200 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (r) NaI line ratio 0.2 0.4 0.6 0.8 1.0 Fig. B.34. NGC 6217 card. Article number, page 87 of 106 Fig. B.34. NGC 6217 card. A117, page 87 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 6217 16h32m41.0s40.0s39.0s38.0s37.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−15 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (u) Continuum LR-V 0246 erg s−1cm−2˚A−1×10−16 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (v) Continuum LR-R 012345 erg s−1cm−2˚A−1×10−16 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (w) HαFlux 0 1 2 3 erg s−1cm−2˚A−1×10−14 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (x) HαEW 0 50 100 150 ˚A 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (y) Hαv 1300 1320 1340 1360 1380 1400 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (z) Hα σ 40 60 80 100 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−14 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 20 40 60 80 ˚A 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 1300 1320 1340 1360 1380 1400 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 40 60 80 100 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 1 2 3 4 erg s−1cm−2˚A−1×10−15 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 5 10 15 20 25 ˚A 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 1300 1320 1340 1360 1380 1400 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 40 60 80 100 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 01234 erg s−1cm−2˚A−1×10−15 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 5 10 15 20 ˚A 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 1300 1320 1340 1360 1380 1400 km s−1 16h32m41.0s40.0s39.0s38.0s 78◦1105700 5400 5100 4800 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 40 60 80 100 km s−1 Fig. B.34. (cont.) NGC 6217 card. Article number, page 88 of 106 Fig. B.34. (cont.) NGC 6217 card. A117, page 88 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 17h17m07.0s06.5s06.0s 40◦5005000 4500 4000 RA (J2000) DEC (J2000) (a) NGC 6339 0.0 0.5 1.0 1.5 2.0 2.5 Jy ×10−5 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (c) Stellar v 2075 2100 2125 2150 2175 km s−1 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (d) Stellar σ 60 70 80 90 100 110 km s−1 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (e) Stellar h3 −0.02 0.00 0.02 0.04 km s−1 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (f) Stellar h4 −0.04 −0.02 0.00 0.02 km s−1 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (h) HβEW 0 5 10 15 20 ˚A 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (i) Hβv 2075 2100 2125 2150 2175 km s−1 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (j) Hβ σ 20 30 40 km s−1 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 02468 erg s−1cm−2˚A−1×10−17 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 02468 ˚A 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 2075 2100 2125 2150 2175 km s−1 17h17m07.0s06.8s06.6s06.4s06.2s06.0s 40◦5004800 4500 4200 3900 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 20 30 40 km s−1 Fig. B.35. NGC 6339 card. Article number, page 89 of 106 Fig. B.35. NGC 6339 card. A117, page 89 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 7437 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (t) Continuum LR-B 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−17 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (u) Continuum LR-V 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−17 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (v) Continuum LR-R −2.5 0.0 2.5 5.0 7.5 erg s−1cm−2˚A−1×10−18 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−16 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (x) HαEW 0 10 20 30 40 ˚A 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (y) Hαv 2100 2110 2120 2130 km s−1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (z) Hα σ 0 5 10 15 20 km s−1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−17 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 5 10 15 ˚A 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 2100 2110 2120 2130 km s−1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 5 10 15 20 km s−1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−17 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0.0 2.5 5.0 7.5 10.0 ˚A 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 2100 2110 2120 2130 km s−1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 5 10 15 20 km s−1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−17 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 2.5 5.0 7.5 10.0 ˚A 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 2100 2110 2120 2130 km s−1 22h58m10.4s10.2s10.0s09.8s 14◦1803600 3300 3000 2700 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 5 10 15 20 km s−1 Fig. B.38. (cont.) NGC 7437 card. Article number, page 96 of 106 Fig. B.38. (cont.) NGC 7437 card. A117, page 96 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 23h04m57.2s57.0s56.8s56.6s56.4s56.2s 12◦1903000 2500 2000 RA (J2000) DEC (J2000) (a) NGC 7479 0 1 2 3 4 5 6 7 Jy ×10−5 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (c) Stellar v 2325 2350 2375 2400 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (d) Stellar σ 80 100 120 140 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (e) Stellar h3 −0.05 0.00 0.05 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (f) Stellar h4 −0.05 0.00 0.05 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (g) HβFlux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−16 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (h) HβEW 0 2 4 6 8 10 ˚A 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (i) Hβv 2250 2300 2350 2400 2450 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (j) Hβ σ 0 25 50 75 100 125 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 2 4 6 ˚A 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 2250 2300 2350 2400 2450 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 20 40 60 80 100 km s−1 Fig. B.39. NGC 7479 card. Article number, page 97 of 106 Fig. B.39. NGC 7479 card. A117, page 97 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 23 h 04 m 57.0 s 56.8 s 56.6 s 56.4 s 12 ◦ 19 0 27 0 0 24 0 0 21 0 0 18 0 0 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 7479 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (t) Continuum LR-B 0 1 2 3 4 erg s−1cm−2˚A−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 2 4 6 erg s−1cm−2˚A−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (v) Continuum LR-R 012345 erg s−1cm−2˚A−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (w) HαFlux 0 20 40 60 80 erg s−1cm−2˚A−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (x) HαEW 0 10 20 30 ˚A 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (y) Hαv 2250 2300 2350 2400 2450 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (z) Hα σ 0 25 50 75 100 125 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−16 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 5 10 15 ˚A 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 2250 2300 2350 2400 2450 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 25 50 75 100 125 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−16 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 2 4 6 ˚A 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 2250 2300 2350 2400 2450 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 25 50 75 100 125 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 erg s−1cm−2˚A−1×10−16 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 01234 ˚A 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 2250 2300 2350 2400 2450 km s−1 23h04m57.0s56.8s56.6s56.4s 12◦1902700 2400 2100 1800 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 25 50 75 100 125 km s−1 Fig. B.39. (cont.) NGC 7479 card. Article number, page 98 of 106 Fig. B.39. (cont.) NGC 7479 card. A117, page 98 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 23h18m16.8s16.6s16.4s16.2s16.0s15.8s 6◦3501500 1000 0500 RA (J2000) DEC (J2000) (a) NGC 7591 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 Jy ×10−5 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 RA (J2000) DEC (J2000) (c) Stellar v 4800 4900 5000 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 RA (J2000) DEC (J2000) (d) Stellar σ 100 150 200 250 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 RA (J2000) DEC (J2000) (e) Stellar h3 −0.050 −0.025 0.000 0.025 0.050 0.075 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 RA (J2000) DEC (J2000) (f) Stellar h4 −0.025 0.000 0.025 0.050 0.075 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (o) NaI Flux −2.5−2.0−1.5−1.0−0.5 erg s−1cm−2˚A−1×10−16 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (p) NaI EW −6−4−2 ˚A 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (q) NaI v 4800 4900 5000 5100 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (r) NaI line ratio 0 1 2 3 Fig. B.40. NGC 7591 card. Article number, page 99 of 106 Fig. B.40. NGC 7591 card. A117, page 99 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 7591 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (u) Continuum LR-V 01234 erg s−1cm−2˚A−1×10−17 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (v) Continuum LR-R 012345 erg s−1cm−2˚A−1×10−17 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−15 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (x) HαEW 0 20 40 60 ˚A 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (y) Hαv 4800 4900 5000 5100 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (z) Hα σ 50 100 150 200 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0.0 0.5 1.0 1.5 2.0 erg s−1cm−2˚A−1×10−15 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 10 20 30 ˚A 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 4800 4900 5000 5100 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 50 100 150 200 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 012345 erg s−1cm−2˚A−1×10−16 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0 2 4 6 8 10 ˚A 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 4800 4900 5000 5100 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 50 100 150 200 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−16 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 2.5 5.0 7.5 10.0 12.5 ˚ A 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 4800 4900 5000 5100 km s−1 23h18m16.6s16.4s16.2s16.0s 6◦3501500 1200 0900 0600 0300 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 50 100 150 200 km s−1 Fig. B.40. (cont.) NGC 7591 card. Article number, page 100 of 106 Fig. B.40. (cont.) NGC 7591 card. A117, page 100 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100500 0000 3005500 RA (J2000) DEC (J2000) (a) NGC 7738 0 1 2 3 4 5 6 Jy ×10−5 23h44m02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 RA (J2000) DEC (J2000) (c) Stellar v 6550 6600 6650 6700 6750 6800 km s−1 23h44m02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 RA (J2000) DEC (J2000) (d) Stellar σ 100 125 150 175 200 km s−1 23h44m02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 RA (J2000) DEC (J2000) (e) Stellar h3 −0.05 0.00 0.05 0.10 km s−1 23h44m02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 RA (J2000) DEC (J2000) (f) Stellar h4 0.00 0.05 0.10 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (o) NaI Flux −4−3−2−1 erg s−1cm−2˚A−1×10−16 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (p) NaI EW −6−4−2 ˚A 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (q) NaI v 6600 6650 6700 6750 6800 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (r) NaI line ratio 0.25 0.50 0.75 1.00 1.25 Fig. B.41. NGC 7738 card. Article number, page 101 of 106 Fig. B.41. NGC 7738 card. A117, page 101 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 7738 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (u) Continuum LR-V 0246 erg s−1cm−2˚A−1×10−17 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (v) Continuum LR-R 0.00 0.25 0.50 0.75 1.00 1.25 erg s−1cm−2˚A−1×10−17 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (w) HαFlux 0 2 4 6 erg s−1cm−2˚A−1×10−16 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (x) HαEW 0 10 20 30 40 50 ˚A 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (y) Hαv 6600 6700 6800 6900 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (z) Hα σ 0 25 50 75 100 125 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−16 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 10 20 30 40 50 ˚A 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 6600 6700 6800 6900 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 25 50 75 100 125 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−17 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0123456 ˚A 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 6600 6700 6800 6900 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 25 50 75 100 125 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0 2 4 6 erg s−1cm−2˚A−1×10−17 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0 2 4 6 ˚A 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 6600 6700 6800 6900 km s−1 23h44m02.4s02.2s02.0s01.8s01.6s 0◦3100600 0300 0000 3005700 5400 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 25 50 75 100 125 km s−1 Fig. B.41. (cont.) NGC 7738 card. The velocity field of the [SII]λ6717 line (subfigure* η)isaffected by atmospheric telluric absorptions. Article number, page 102 of 106 Fig. B.41. (cont.) NGC 7738 card. The velocity field of the [SII]λ6717 line (subfigure* η) is affected by atmospheric telluric absorptions. A117, page 102 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300500 0000 3205500 RA (J2000) DEC (J2000) (a) NGC 7787 0 1 2 3 4 Jy ×10−5 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (c) Stellar v 6400 6500 6600 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (d) Stellar σ 100 150 200 250 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (e) Stellar h3 −0.05 0.00 0.05 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (f) Stellar h4 0.00 0.05 0.10 0.15 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (o) NaI Flux −2.0−1.5−1.0−0.5 0.0 erg s−1cm−2˚A−1×10−16 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (p) NaI EW −3−2−1 0 1 ˚ A 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (q) NaI v 6500 6600 6700 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (r) NaI line ratio 0.00 0.25 0.50 0.75 1.00 1.25 Fig. B.42. NGC 7787 card. Article number, page 103 of 106 Fig. B.42. NGC 7787 card. A117, page 103 of 106 A&A 670, A117 (2023) A&A proofs: manuscript no. MEGADES_DR1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (s) MEGARA RGB NGC 7787 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (u) Continuum LR-V 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−17 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (v) Continuum LR-R 0 2 4 6 erg s−1cm−2˚A−1×10−17 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (w) HαFlux 0.0 0.2 0.4 0.6 0.8 1.0 erg s−1cm−2˚A−1×10−15 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (x) HαEW 0 5 10 15 20 25 ˚A 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (y) Hαv 6500 6600 6700 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (z) Hα σ 0 20 40 60 80 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (α) [NII]λ6584 Flux 0 1 2 3 erg s−1cm−2˚A−1×10−16 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (β) [NII]λ6584 EW 0 2 4 6 8 10 ˚A 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (γ) [NII]λ6584 v 6500 6600 6700 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (δ) [NII]λ6584 σ 0 20 40 60 80 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (²) [SII]λ6717 Flux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−17 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (ζ) [SII]λ6717 EW 0.0 0.2 0.4 0.6 0.8 1.0 ˚A 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (η) [SII]λ6717 v 6500 6600 6700 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (θ) [SII]λ6717 σ 0 20 40 60 80 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (ι) [SII]λ6731 Flux 0.0 0.5 1.0 1.5 2.0 2.5 erg s−1cm−2˚A−1×10−17 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (κ) [SII]λ6731 EW 0.0 0.2 0.4 0.6 0.8 1.0 ˚A 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (λ) [SII]λ6731 v 6500 6600 6700 km s−1 23h56m08.2s08.0s07.8s07.6s07.4s 0◦3300300 0000 3205700 5400 RA (J2000) DEC (J2000) (µ) [SII]λ6731 σ 0 20 40 60 80 km s−1 Fig. B.42. (cont.) NGC 7787 card.The velocity field of the [SII]λ6717 line (subfigure* η)isaffected by atmospheric telluric absorptions. Article number, page 104 of 106 Fig. B.42. (cont.) NGC 7787 card.The velocity field of the [SII]λ6717 line (subfigure* η) is affected by atmospheric telluric absorptions. A117, page 104 of 106 M. Chamorro-Cazorla et al.:MEGADES: MEGARA galaxy disc evolution survey M. Chamorro-Cazorla et al.: MEGADES: MEGARA galaxy disc evolution survey 21h19m43.4s43.2s43.0s42.8s42.6s −7◦3300500 1000 1500 RA (J2000) DEC (J2000) (a) PGC 066559 0 1 2 3 4 Jy ×10−6 21h19m43.4s43.2s43.0s42.8s42.6s −7◦3300600 0900 1200 1500 RA (J2000) DEC (J2000) (c) Stellar v 2600 2650 2700 2750 2800 km s−1 21h19m43.4s43.2s43.0s42.8s42.6s −7◦3300600 0900 1200 1500 RA (J2000) DEC (J2000) (d) Stellar σ 0 50 100 150 200 250 km s−1 21h19m43.4s43.2s43.0s42.8s42.6s −7◦3300600 0900 1200 1500 RA (J2000) DEC (J2000) (e) Stellar h3 0.00 0.02 0.04 0.06 0.08 0.10 km s−1 21h19m43.4s43.2s43.0s42.8s42. 6s −7◦3300600 0900 1200 1500 RA (J2000) DEC (J2000) (f) Stellar h4 −0.08 −0.06 −0.04 −0.02 0.00 km s−1 21h19m43.4s43.2s43.0s42.8s42. 6s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (g) HβFlux 0 1 2 3 4 5 erg s−1cm−2˚A−1×10−17 21h19m43.4s43.2s43.0s42.8s42.6s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (h) HβEW 0 5 10 15 20 ˚A 21h19m43.4s43.2s43.0s42.8s42.6s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (i) Hβv 2680 2700 2720 2740 km s−1 21h19m43.4s43.2s43.0s42.8s42. 6s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (j) Hβ σ 0 5 10 15 20 25 km s−1 21h19m43.4s43.2s43.0s42.8s42.6 s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (k) [OIII]λ5007 Flux 0123456 erg s−1cm−2˚A−1×10−17 21h19m43.4s43.2s43.0s42.8s42.6s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (l) [OIII]λ5007 EW 0 5 10 15 20 25 ˚A 21h19m43.4s43.2s43.0s42.8s 42.6s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (m) [OIII]λ5007 v 2680 2700 2720 2740 km s−1 21h19m43.4s43.2s43.0s42.8s42.6 s −7◦3300600 0900 1200 1500 1800 RA (J2000) DEC (J2000) (n) [OIII]λ5007 σ 0 5 10 15 20 25 km s−1 Fig. B.43. PGC 066559 card. Article number, page 105 of 106 Fig. B.43. PGC 066559 card. A117, page 105 of 106