Spatial distribution of stellar mass and star formation activity at 0.2¡z¡1.2 across and along the Main Sequence

Spatial distribution of stellar mass and star formation activity at 0.2¡z¡1.2 across and along the Main Sequence

L. Morselli Excellence Cluster Universe, Boltzmannstr. 2, 85748 Garching bei München, Germany    P. Popesso Excellence Cluster Universe, Boltzmannstr. 2, 85748 Garching bei München, Germany    A. Cibinel Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton, BN1 9QH, United Kindom    P. A. Oesch Observatoire de Genéve, 51 Ch. des Maillettes, 1290 Versoix, Switzerland    M. Montes School of Physics, University of New South Wales, NSW 2052, Australia    H. Atek Institut d’astrophysique de Paris, CNRS UMR7095, Sorbonne Universite, 98bis Boulevard Arago, F-75014 Paris, France    G. D. Illingworth UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA    B. Holden UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA
Received 2 November 2018 / Accepted 14 December 2018
Key Words.:
galaxies: evolution - galaxies: star formation - galaxies: structure

High-resolution multi-wavelength photometry is crucial to explore the spatial distribution of star formation in galaxies and understand how these evolve. To this aim, in this paper we exploit the deep, multi-wavelength Hubble Space Telescope (HST) data available in the central parts of the GOODS fields and study the distribution of star formation activity and mass in galaxies located at different positions with respect to the Main Sequence (MS) of star-forming galaxies. Our sample consists of galaxies with stellar mass in the redshift range 0.2 . Exploiting 10-band photometry from the UV to the near-infrared at HST resolution, we derive spatially resolved maps of galaxies properties, such as stellar mass and star formation rate and specific star formation rate, with a resolution of arcsec. We find that the star formation activity is centrally enhanced in galaxies above the MS and centrally suppressed below the MS, with quiescent galaxies (1 dex below the MS) characterised by the highest suppression. The sSFR in the outer region does not show systematic trends of enhancement or suppression above or below the MS. The distribution of mass in MS galaxies indicates that bulges are growing when galaxies are still on the MS relation. Galaxies below the MS are more bulge-dominated with respect to MS counterparts at fixed stellar mass, while galaxies in the upper envelope are more extended and have Sérsic indexes that are always smaller than or comparable to their MS counterparts. The suppression of star formation activity in the central region of galaxies below the MS hints at inside-out quenching, as star formation is still ongoing in the outer regions.

1 Introduction

Star forming (SFGs) and passive galaxies differ not only in their level of star formation activity, but in a large range of properties. SFGs dominate the low mass end of the galaxy mass function, while passive galaxies dominate the high mass end (e.g. Pannella et al. 2006; Pozzetti et al. 2009; Drory et al. 2009; Ilbert et al. 2009). SFGs largely populate low density environments, while passive ones are mostly found in massive galaxy groups and clusters (e.g. Dressler 1980; Balogh et al. 2004; Blanton et al. 2005; Blanton & Moustakas 2009). SFGs are mainly disk-dominated, while bulge-dominated structures are found to efficiently describe objects with little or no ongoing star formation activity (Morgan & Mayall 1957; Robert C Kennicutt 1998; Kauffmann et al. 2003; Wuyts et al. 2011; Cheung et al. 2012).

In the star formation rate (SFR) - stellar mass (M) plane, SFGs and passive galaxies populate very different loci. SFGs occupy a very tight relation called the Main Sequence (MS), characterised by a slope ranging from 0.6 to 1.2 and a very small scatter of dex (e.g. Noeske et al. 2007; Daddi et al. 2007; Elbaz et al. 2007; Pannella et al. 2009; Peng et al. 2010; Rodighiero et al. 2010; Karim et al. 2011; Popesso et al. 2012; Whitaker et al. 2012; Bernhard et al. 2014; Magnelli et al. 2014; Speagle et al. 2014; Renzini & Peng 2015; Steinhardt et al. 2017; Maragkoudakis et al. 2017). Such a relation is already in place at z 4 (e.g. Speagle et al. 2014) and is considered the dominant mode of star formation, leading to 90 of the stellar mass budget in the Universe today (Schreiber et al. 2015). In addition, its relatively small scatter suggests that star formation is regulated by secular evolution more than by stochastic events like mergers.

The MS has been extensively studied to better understand the nature of its scatter, and thus reveal physical processes responsible, at a given galaxy stellar mass, of enhancing or suppressing star formation. Observational studies reveal that galaxy morphology changes across and along the MS. In particular, galaxies in the upper and lower envelop of the relation seem to be more bulge dominated than MS counterparts at fixed stellar mass, and the bulge prominence also increases with increasing stellar mass, when moving along the MS (Wuyts et al. 2011; Bluck et al. 2014; Lang et al. 2014; Guo et al. 2015; Morselli et al. 2017). Morselli et al. (2017) conclude that, at any stellar mass, the MS is located at the minimum of the B/T distribution. Galaxies in the MS upper envelope are characterised by a blue, star forming bulge, while the lower envelope is occupied by compact structures with dead bulges.

From the theoretical point of view, Zolotov et al. (2015) and Tacchella et al. (2016) propose that episodes of compaction and gravitational instabilities could drive gas towards the centre of galaxies. This would lead to the creation of a blue, star forming, central component. After the compaction event, gas consumption would then quench the central star formation region, leaving a quenched, red bulge. Subsequent episodes of compaction and quenching would move galaxies above and below the MS and along it and explain the observed scatter. It is thus clear that in order to understand the evolution of the star formation activity and thereby the migration of galaxies across the MS, it is mandatory to obtain observational data that can spatially resolve galactic structure (Allen et al. 2006; Abramson et al. 2014; Morselli et al. 2017). At low redshift, Spindler et al. (2017) find that galaxies classified as AGN/LI(N)ER typically have centrally-suppressed sSFR profiles, possibly indicating a relation between central quenching and AGN activity. They also find that suppression of sSFR, both central and at outer radii, happens in galaxies that are more bulge-dominated than typical star forming ones, further suggesting that the presence of a central spheroidal component might result in the cessation of star formation activity also in the disk, as suggested by Martig et al. (2009). Lin et al. (2017), exploiting ALMA observations of three nearby MaNGA green valley galaxies, conclude that star formation activity has to be first suppressed in the bulge following the depletion of cold gas, and subsequently in the disk, thus implying that quenching has to be an inside-out mechanism. Using MaNGA data, Ellison et al. (2017) find that galaxies above the MS are characterised by an enhancement in star formation activity that is more pronounced at small radii, while passive galaxies have suppressed star formation activity especially in the central region, thus confirming qualitatively the compaction/depletion scenario. Belfiore et al. (2017) argue that a slow quenching process must result in the suppression of the star formation activity at all radii, and not only in the central regions, as they find that green valley galaxies have typically non star forming bulges and lower star formation in the disk. Other works, instead, find that nearby early type galaxies are characterised by slightly positive age gradients, thus favouring an outside-in evolution of star formation in galaxies (e.g. Goddard et al. 2017)

At higher redshifts, Nelson et al. (2016, hereafter N16) use stacked profiles and find that SFR from above (below) the MS is enhanced (suppressed) at all radii, suggesting a scenario where the physical processes driving the change in star formation activity are independent of the host galaxy mass and act throughout the galactic disk in a coherent manner. Inside-out quenching is instead advocated by Morishita & Ichikawa (2016), Tacchella et al. (2015a), Tacchella et al. (2016), and Tacchella et al. (2017b) to explain trends of sSFR, colours, and dust, observed in real and simulated galaxies.

In this work, we exploit the combination of high-resolution optical-to-NIR photometric data from the GOODS+CANDELS surveys, with the deep UV observations collected with the WFC3/UVIS camera as part of the HDUV survey (Oesch et al. 2018) to derive resolved stellar population maps. This allows us to study the spatial distributions of stellar mass and star formation activity as a function of the offset from the MS. In Sec. 2 we describe the catalogues from which different quantities are taken (Sec. 2.1), the final sample used in this work (Sec. 2.2), and the procedures to obtain the resolved maps of stellar properties (Sec. 2.1), the structural parameters of galaxies (Sec. 2.4), the radial profiles (Sec. 2.5) and the MS for the final sample (Sec. 2.6). In Sec. 3.1 we study the distribution of SFR, stellar mass, and sSFR, while in Sec. 3.2 we check the distribution of dust and UV luminosity. We discuss our results and their implications in Sec. 4.

2 Data

In this work we use galaxies lying in the central part of the GOODS fields (Giavalisco et al. 2004) covered by the Hubble Deep UV survey (HDUV, PI: P. Oesch), representing some of the deepest, high resolution UV data to date 111The HDUV imaging data are available as high-level science products at https://archive.stsci.edu/prepds/hduv/.. The HDUV is a legacy imaging program carried out with the WFC3/UVIS camera onboard HST that with a total of 132 orbits allows to get very deep images (27.5-28 mag) with the F275W and F336W filters, over a wide area of 100 arcmin and with high spatial resolution (0.1”).

Available in the central parts of the GOODS fields are the photometric and spectroscopic observations taken as part of the GOODS, CANDELS, and 3DHST surveys with HST/ACS and WFC3 (Giavalisco et al. 2004; Grogin et al. 2011; Koekemoer et al. 2011; Skelton et al. 2014; Momcheva et al. 2016), as well as the deepest far-IR data to date, obtained combining observations of the GOODS fields taken with PACS (Photodetector Array Camera and Spectrometer) as given by the combination pf the PACS Evolutionary probe survey (Lutz et al. 2011) and of the GOODS-Herschel survey (Elbaz et al. 2011), described in Magnelli et al. (2013, hereafter M13). The IR data allow an accurate determination of IR luminosity (), and thus of the obscured SFR of dusty high redshift star forming galaxies. Together with other available imaging data in the central parts of the GOODS fields, it is thus possible to construct SEDs over a large wavelength range, including the rest-frame UV for galaxies at z 0.2

2.1 Redshifts, Stellar Masses, SFRs and structural parameters

Redshifts and stellar masses are taken from the public releases of 3D-HST data products (Skelton et al. 2014). In particular, redshifts are ranked as spectroscopic, grism, and photometric (Momcheva et al. 2016) and the best available estimate is used for the computation of the stellar masses (Skelton et al. 2014), obtained from fitting the 0.3-8 SED range with the FAST code (Kriek et al. 2009) using the Bruzual & Charlot (2003) stellar population synthesis models, a Chabrier (2003) IMF, solar metallicities, a Calzetti et al. (2000) dust attenuation law and a exponentially declining star formation history.

SFRs are considered as the sum of the UV unobscured and the IR obscured contributions to the star formation activity of galaxies. For sources that are in the GOODS-Herschel catalogue of M13, SFR is computed from using the Kennicutt relation (Robert C Kennicutt 1998). The total , covering the range 8-1000, is estimated by fitting the flux densities at 70, 100 and 160 (when available) with the SED templates of Elbaz et al. (2011). For details on the procedure, see Ziparo et al. (2013). For sources without counterparts in the GOODS-H catalogue (mainly galaxies with low SFRs, located in the lower envelope of the MS, and passive galaxies) SFR comes from the catalogue of Whitaker et al. (2014, hereafter W14). Briefly, W14 derived a photometric catalogue of Spitzer/MIPS 24 sources using the approach described in Skelton et al. (2014). The 24 flux density is used to estimate through a luminosity-independent conversion, demonstrated to recover in good agreement with Herschel-PACS estimates (Wuyts et al. 2011). The UV contribution to the SFRs is also taken from W14, and it is estimated from the 2800 luminosity, following the work of Bell et al. (2005). We underline here that for all the sources with the SFR is given by SFR = SFR + SFR. For galaxies with 1 S/N 3 at 24, W14 provides an upper limit of , and thus of SFR. For sources undetected in 24 the SFR is purely based on the UV contribution, and thus it is a lower limit.

2.2 Galaxy Sample

The sample is mass selected and it has been built by selecting galaxies in the 3D-HST catalogue located within the HDUV footprints and satisfying the criteria: LogM 9.5 M and . This is done in order to reach the high completeness level of 95 up to z1, as shown in W14, Muzzin et al. (2013) and Tal et al. (2013). As the aim of this work is to study the spatial distribution of star formation activity in galaxies, AGN contribution to the UV emission of a galaxy might represent a source of contamination. For this reason, we removed X-ray selected AGN by cross matching our sample with the X-ray selected AGN catalogue of (Shao et al. 2010, for GOODS-N) and (Brusa et al. 2010, for GOODS-S). This results in the omission of of the sources. In addition, visual inspection was carried out on the stellar mass maps of galaxies to avoid sources with corrupted stellar properties maps and merging systems. Following visual inspection, The final sample is made of 712 galaxies, of which have spectroscopic redshifts and have grism redshifts. In addition, 56 have a counterpart in M13, thus an estimate of from Herschel/PACS. Of the remaining galaxies, 71 has S/N 1 at 24, 18 has S/N 1 at 24, and 11 has S/N 0 at 24. In the following analysis, we split the sample in two redshift bins: [0.2:0.7] (low-z sample) and [0.7:1.2] (high-z sample).

2.3 Resolved Stellar Population Maps

In this paper, we exploit the multi-wavelength, high-resolution HST imaging data to obtain a resolved picture of galaxy evolution through stellar population maps. To build resolved maps, we follow the method described in Cibinel et al. (2015). First, we match all the images in the different bands to the same resolution of the H-band, that with is the filter with the worst PSF among the available ones. We then extract the pixel-by-pixel fluxes within an elliptical aperture equal to 1.5 times the Kron radius of each galaxy, and fit them with stellar population models. To overcome the problem of relatively low flux in individual pixels, we apply the ADAPTSMOOTH code of Zibetti (2009) to the galaxy images in all the available filters. When, for a given pixel, the S/N is lower than a given threshold, the code replaces that value with an average of the values over a lager circular area. As explained in Cibinel et al. (2015), an advantage of using ADAPTSMOOTH is the facility to smooth images in different filters on the same scale length, which is a necessary step to obtain self-consistent SEDs. We run the code on stacked images of all ACS and WCF3 stamps (to ensure that smoothing is applied on those pixels where the majority of the bands reach a low S/N while preserving the structural variations in the different filters) by requiring a minimum S/N = 5 and stop the algorithm when the averaging area reaches the maximum radius of 5 pixels. The smoothing pattern obtained as output is then applied to all available bands.

Figure 1: Comparison between the stellar mass obtained from SED fitting in the work of W14, and the stellar mass computed as sum of the value in each pixel of the stellar mass maps created for this work, from the F160W images as explained in Sec.3.2 . The red line is the 1-to-1 relation. The total stellar mass derived from our resolved stellar mass maps is in very good agreement with the estimate obtained from the integrated photometry (scatter of 0.15dex).

The pixel-by-pixel SED maps are then fitted with LEPHARE (Arnouts et al. 1999; Ilbert et al. 2006) using the Bruzual & Charlot (2003) synthetic spectral library with a Chabrier (2003) IMF and a delayed exponential star formation history (). We apply the following constrains to the fits: 1) the typical timescale can vary between 0.01 and 10 Gyr in 22 steps, and 2) the template ages are selected between 100 Myr and the age of the Universe at the redshift of the source. We apply a Calzetti et al. (2000) extinction law, with E(B-V) varying between 0 and 0.9 mag and allowing for three values of metallicity Z (Z = Z, Z = 0.2 Z, Z = 0.4 Z). As result of the fitting procedure, we obtain median maps, where the value of each pixel is given by the median of the full probability distribution function from all the templates, and a best-fit map (i.e., minimum ). In the following analysis, we make use of the median maps. Fig. 2 shows a comparison between the SFR obtained as sum over all pixels of the SED-based SFR maps and the SFR by UV + IR tracers (see Sec. 2.1). Despite a large scatter, there is good agreement between the two estimates of SFR.

Figure 2: Comparison between the SED-based integrated SFR, computed by summing the pixel-by-pixel values of SFR maps, and the UV+IR SFRs described in Sec. 2.1.

While for the SFR and E(B-V) we use the resolved maps as directly obtained from the SED-fitting, the derivation of the stellar mass maps requires a slightly different approach, motivated by the fact that we will use these maps to derive mass-based structural parameters with GALFIT. In fact, as the maps obtained from SED fitting are defined within an aperture equal to the Kron radius and have zero values outside such radius, they do not include a sky component. This could lead to artifacts or unstable fitting with GALFIT. Therefore, we use the best-fit M/L maps obtained from SED fitting where we replace the zero values with the mean of the closest 15 pixels that have non-zero values. We then multiply these M/L maps with the -band maps to get stellar mass maps that include the sky-noise contribution. To check the reliability of this procedure, in Fig. 1 we show a comparison between the total stellar mass computed as sum of the values in each pixel of the mass map obtained from the -band image, and the stellar mass in the 3D-HST catalogue. The two estimates are in good agreement, with a scatter of 0.15 dex.

Finally, the UV luminosity maps are constructed from interpolation to the observed photometry, and they can be non-dust corrected, or corrected for dust using the UV beta slope - A relation (Meurer et al. 1999; Overzier et al. 2011), where the UV beta slope is obtained from a linear fit to the best-fit SED model.

Figure 3: Comparison between the mass-weighted structural parameters obtained from a single Sérsic component GALFIT 2D fitting technique in this work and the light-weighted estimates of van der Wel et al. (2012). Top row: position angle (left) and axis ratio (right). Bottom row: effective radii (left) and Sérsic index (right). In all four panels, the black symbols indicate galaxies with reliable fits in vdW12, while green ones mark galaxies with trustable fits in this work, but not in vdW12. The blue line is the 1-to-1 relation. For clarity, few points with extremely large errorbars have been omitted in this plot. The mass-weighted structural parameters obtained in this work are in good agreement with the light-weighted estimated of vdW12, especially for the axis ratio and the position angle. The majority of galaxies in the sample has mass-weighted effective radius smaller than the light-weighted value, and Sérsic index larger than estimate of vdW12.

2.4 Mass-weighted structural parameters from GALFIT

Light-weighted structural properties of galaxies in GOODS-S and GOODS-N have already been studied as part of the work of van der Wel et al. (2012, vdW12 hereafter). The authors use GALFIT (Peng 2010) to derive structural parameters by fitting the cutouts of each galaxy in different filters (F160W, F125W and, when available, F105W) with a single Sérsic profile. of the galaxies in our sample have, in vdW12, a flag corresponding to suspicious, bad, or non-existent fitting results. In this work, we compute mass-weighted structural parameters of galaxies, by fitting with GALFIT our 2D stellar mass maps using a single Sérsic model. Our fits are reliable for the of the sample, while only of fits retrieve unreliable estimates of the parameters (not within the input ranges) or non-existing fitting results. This difference most likely arises from the different input images that GALFIT needs to model. Here, in fact, GALFIT is run on the stellar mass maps obtained from pixel-by-pixel SED fitting of 10-bands photometric images that have been previously smoothed using ADAPSMOOTH (see Sec. 2.3 for the details on the creation of maps). Fig. 3 shows a comparison of the mass-weighted structural parameters obtained in this work and the light-weighted ones obtained by vdW12 for the galaxies with reliable fitting results in our work. The panels show: the position angle (, top-left panel), the axis ratio (, top-right panel), the effective radii (R, bottom-left panel) and the Sérsic index (, bottom-right panel), respectively. Galaxies that have reliable fits both in this work and in vdW12 are marked in black; for these sources, light-weighted and mass-weighted structural parameters show a very good agreement. The green symbols mark galaxies with reliable fits in this work but not in vdW12. While the mass-weighted and light weighted estimates of the position angle and of the axis ratio of these galaxies show again a very good agreement, the scatter in the relation increases for the effective radius and the Sérsic index. For these galaxies, the mass-weighted effective radius is often smaller than the light-weighted estimate, especially towards larger light-weighted R, in agreement with Szomoru et al. (2013). The relation between the mass-weighted Sérsic index and the light-weighted one is characterised by a large scatter, with the majority of galaxies having mass-weighted larger than the light-weighted estimate. Table 2 is released with this paper222Table 1 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/, and contains the ID of the galaxy, its RA, DEC and redshift, and the mass-weighted structural parameters obtained from GALFIT: effective radius (in arcsec), Sersic index, axis ratio, and position angle.

Figure 4: Distribution of galaxies in the - LogM plane. Blue stars mark galaxies in the final sample with a counterpart the Herschel catalogue of M13. Grey stars indicate galaxies with no counterpart in M13, but detected with MIPS. Galaxies that are not detected in MIPS are shown with arrows: pink when the 24 is given as an upper limit, and maroon when the SFR comes from UV only. The triangles show the average distance from the MS of galaxies undetected in MIPS, for which the SFR from SED fitting was used to compute . The percentages represent the completeness of the final sample (after removal of AGNs and corrupted data from visual inspection) with respect to the total HDUV sample in the same redshift bin. The shaded regions mark the bins defined according to the distance from the MS, and will be used from now on in this work.
ID RA DEC z Re err Re n err n q err q PA err PA
3138 189.217644 62.150245 0.97 0.19 0.11 2.85 0.19 0.78 0.02 47.47 3.66
3164 189.262815 62.150191 0.49 0.12 0.01 1.73 0.02 0.29 0.00 -62.52 0.14
3359 189.273982 62.151396 1.16 0.71 0.25 2.43 0.06 0.41 0.00 66.43 0.41
3456 189.287288 62.152743 0.87 0.19 0.06 4.03 0.16 0.65 0.01 -2.76 1.3
3630 189.232313 62.154862 0.47 0.38 0.04 2.66 0.02 0.54 0.0 -78.1 0.26
Table 1: Example of the table released with this paper, containing the ID of the galaxy, its RA, DEC and redshift, and the mass-weighted structural parameters obtained from GALFIT: effective radius (in arcsec), Sersic index, axis ratio, and position angle.

2.5 Radial profiles

The 1D azimuthally averaged profiles of stellar mass, SFR, and sSFR of each galaxy are created from the 2D maps using the structural parameters obtained with GALFIT. First, a gaussian kernel is applied to the mass map to find the position of the peak, that we take as centre of the galaxy. Then, concentric ellipses are drawn on the 2D map of the analysed quantity (e.g. SFR or sSFR), where the major axis inclination depends on the galaxy position angle, together with the axis ratio used to define the ellipses. We build two types of radial profile: 1) the one normalised for the effective radii of each galaxy, where R comes from the GALFIT fitting procedures; and 2) the physical one, where the radius is given in kpc. While the first method allows us to take care of the intrinsic distribution of R with redshift (as galaxies at larger redshifts are more compact), it suffers from the large uncertainties in the estimate of R. On the other hand the second approach applied on a large redshift range, inevitably suffers from physical variation in the size of galaxies at different redshifts.

The median profile for a given mass and redshift bin is just the arithmetic median of all the regions between the same adjacent ellipses at a certain distance from the centre. We truncate the median profile at the radius that contains 50 of the galaxies of the given subsample.This is done to have a very high completeness in each region, in particular in the galaxy outskirts, that could be otherwise dominated by few particularly extended sources. In the specific case of the stellar mass, before computing the median each individual profile has been normalised to enhance possible differences in the mass profile shape. The observed trends do not vary when considering the average profiles instead of the median ones. We checked the consistency of the profile procedure by comparing the mass obtained as sum of the values in each pixels of the map, and the total mass obtained from the integration of the radial profiles. As the two show very good agreement, we consider our method robust.

2.6 Main Sequence definition

The aim of this work is to understand how the distribution of star formation activity and stellar mass change as a function of the location of a galaxy around the MS. To this aim, we use the MS of Karim et al. (2011, K11 hereafter), where SFRs are computed from 1.4GHz emission, considering a Chabrier (2003) IMF, Bruzual & Charlot (2003) models, and Calzetti et al. (2000) extinction curve. The K11 MS was chosen as it covers the redshift range in small redshift steps of 0.2 and has been computed using a relatively wide range in stellar masses (2dex) that also includes low mass galaxies. While the former point is key in getting the right normalisation of the MS at each redshift, the latter is important to avoid possible biases due to the flattening of the MS. The MS flattening, still highly debated in literature (e.g. Whitaker et al. 2014; Erfanianfar et al. 2016), if present would induce a bias in a selection of galaxies based on a MS computed only with massive sources.

Figure 5: Median SFR (first row), stellar mass (second row), and sSFR (third row) surface densities as a function of distance from the centre (in kpc) for galaxies in the redshift range [0.2:0.7]. The three columns indicate galaxies with different stellar masses: 9.5Log(M/M)10.0 in the first, 10.0Log(M/M)10.5 in the second, and 10.5Log(M/M)11.0 in the third column, respectively. The thickness of the profiles in a given bin of distance from the centre is given by the standard deviation of the values in that bin, dived by the square root of the number of points in that bin. Different colours mark different bins of distance from the MS, as defined in Fig. 4. The SSFR profiles of galaxies below the MS are characterised by a central suppression that becomes more significant with increasing distance from the MS.

Using the K11 definition of the MS at each redshift bin, we compute the distance of each galaxy from the relation at the galaxy’s redshift. Fig. 4 shows the distribution of galaxies in the final sample on the - LogM plane, where = LogSFR - LogSFR. The colours indicate different SFRs used to compute , as explained in Sec. 2.1. Herschel detected galaxies (blue) mainly populate the upper envelope of the MS. MIPS-only detected galaxies (grey) mainly populate the lower envelope of the MS, especially at low stellar masses. MIPS upper limits with 1 S/N 3 (orange) populate the valley and quiescent region 1 dex below the MS. Galaxies undetected in MIPS (maroon), that only have the UV contribution to the SFR and thus are lower limits, are mainly found at distances larger that 1 dex below the MS. As a sanity check, we compute the average value of distance from the MS for galaxies that are undetected in MIPS, by summing the values in each pixel of the SED SFR maps. These values are marked in Fig. 4 with filled triangles. As expected, galaxies that are undetected in MIPS for which only the UV contribution to the SFR is considered are found closer to the MS when SFR from SED is used, but still well below the relation.

We define six subsamples of galaxies based on their distance from the MS, chosen to have enough statistics and, at the same time, to take into account the average scatter of the MS (0.2 - 0.3 dex). All galaxies with constitute the starburst (SB) sample, indicated with the blue shaded region. Galaxies in the upper envelope of the MS, with , make up the SUP1 sample (light blue area in Fig. 4). The MS sample is comprised of galaxies that have (gray area in Fig. 4). The lower envelope on the MS is divided in the SUB1 and SUB 2 samples, that include galaxies with (light pink area in Fig. 4), and (orange area in Fig. 4), respectively. Finally, all galaxies with form the quiescent (QUIE) sample marked by the shaded red colour. We note that due to the limited area covered by the HDUV survey, the number of real starbursts (usually defined in literature as galaxies with ) is relatively small. Tab. 2 shows the number of galaxies in each bin of mass, redshift, and distance from the MS. The completeness of our final sample in each stellar mass and distance from the MS bin is always larger than , as indicated by the numbers in Fig. 4.

Log(M/M) Log(M/M) Log(M/M)
Sample 9.5:10.0 10.0:10.5 10.5:11.0
high-z   low-z high-z   low-z high-z   low-z
QUIE 21  8 29  20 34  9
SUB2 15  6 17  8 24  7
SUB1 49  16 10  5 12  4
MS 102  28 31  14 17  7
SUP1 50  40 43  22 11  6
SB 5  12 10  7 -   2
Table 2: Number of galaxies in each bin of distance from the MS, stellar mass, and redshift.

3 Results

3.1 Sfr, M, and sSFR profiles

In Fig. 5, we show the median SFR (first row), M (second row), and sSFR (third row) profiles in the different bins of distance from the MS and stellar mass for the low-z subsample. The profiles are computed as a function of the physical distance from the centre in kpc. The thickness of the profiles in a given bin of distance from the centre is given by the standard deviation of the values in that bin, dived by the square root of the number of points in that bin.The three columns of Fig. 5 represent three stellar mass bins: 9.5 Log(M/M) 10.0, 10.0 Log(M/M) 10.5, and 10.5 Log(M/M) 11.0, respectively. In all panels, the colours correspond to galaxies at different distances from the MS: from passive (red) to MS galaxies (grey) and upper MS galaxies (blue), as defined in Fig. 4. For galaxies with Log(M/M) , the SFR profile of galaxies well below the MS (QUIE and SUB2) is almost flat at every radii, while the SFR profiles of galaxies around the MS or above it increases towards the inner radii. For larger stellar masses, the increase of SFR in the central part is more enhanced for galaxies at higher SFR, with SB showing the largest SFR surface density in the inner 5 kpc. At R 5 kpc, the difference between the SFR profiles of QUIE and SB galaxies with Log(M/M) 10 reaches 3 orders of magnitudes. At larger radii (r 5 kpc) the SFR surface density decreases significantly in galaxies above and on the MS, reaching values comparable with the ones of galaxies well below the relation, that on contrary are characterised by a dip in the SFR distribution at small radii.

Figure 6: Same as Fig.5, but for galaxies in the redshift range [0.7:1.2]. Also in the high-z sample we observe that the sSFR of galaxies below the MS is significantly lower in the central regions with respect to MS counterparts.

The second row of Fig. 5 shows the stellar mass profiles of galaxies. We recall here that each single profile has been normalised for the total stellar mass obtained integrating the profile, to account for differences in M within the 0.5 dex bin, before the computation of the median profile. As expected, passive galaxies are always less extended and more concentrated with respect to MS galaxies. MS galaxies become more extended with increasing stellar mass and their mass distribution seems to become more centrally concentrated, consistent with the idea of the build-up of the bulge component. Galaxies located above the MS are more extended than MS counterparts, and show no central enhancement of their stellar mass distribution.

The third row of Fig. 5 shows the sSFR profiles of galaxies. At large radii, r 5 kpc, the median sSFR profile does not show significant differences for the subsamples of galaxies located at various distances from the MS; galaxies with the largest SFRs and passive ones have the same sSFR surface density, or they differ of 0.5 dex. At small radii, r 5 kpc, the sSFR profiles depend dramatically on the distance from the MS. The sSFR profiles of galaxies below the MS are characterised by a decrease which is proportional to the distance from the relation, with quiescent galaxies showing the largest decline. MS and SUP1 galaxies are characterised by a small decline of sSFR in the inner radii, while SB galaxies have flat or enhanced sSFR profile in the innermost 5 kpc.

Figures 6 shows the median SFR, stellar mass, and sSFR profiles of galaxies in the high-z sample, computed as a function of the physical distance from the centre in kpc. No significant evolution within the two redshift bin is observed, as the trends in the high-z sample are very similar to the low-z one. The only difference concerns the SFR profile of SB galaxies (notice that we do not have SB galaxies in the most massive bin). While in the low-z sample the SB SFR profile is the one characterised by the largest SFR surface density at small radii, in the high-z one the SFR profile of SB galaxies is consistent with the one of SUB1 and MS galaxies. The trends observed in Fig. 5 and Fig. 6, in which the surface densities are shown as a function of the physical distance from the centre in kpc, are also observed when the surface densities are computed as a function of the distance normalised by the galaxies’ effective radii (see Appendix A).

As explained in Section 3.2, the images in the different bands are PSF-matched to the F160W image prior to the pixel-by-pixel SED fitting routine. To investigate possible contamination due to PSF effects in the trends observed in the radial profiles, we selected the most extended galaxies in the low redshift range, for which PSF-related effects should be minimised. In Fig. 7 we show the radial profiles of galaxies that have an effective radii larger than 3 times the PSF FWHM in the H band, thus . The sample inevitably suffers of small statistics, thus we consider all galaxies in the stellar mass range 10 Log(M/M) 11.0. The trends observed in Figures  5 and  6 characterise also the SFR and SSFR profiles of the most extended galaxies in our lower redshift sample, thus proving that our analysis is robust against PSF-related effects.

Figure 7: Median SFR (first row) and sSFR (second row) surface densities as a function of distance from the centre (in kpc) for all the galaxies in the redshift range [0.2:0.7] and stellar mass range 10.0Log(M/M)11.0 that have an effective radius larger than 0.45 arcsec. The observed trends are similar to the ones of the whole galaxy sample, independent on the galaxy size.

To further study the mass distribution in galaxies above/below the MS, both in the low and high redshift sample, we show in Fig.8 the distribution of the average Sérsic index as a function of the distance from the MS, . The Sérsic index used here is obtained as output of the GALFIT fitting procedure, as explained in Sec. 2.4. The errorbars in this analysis are computed via bootstrapping. We observe, as discussed qualitatively when analysing the stellar mass profiles, a quasi-monotonic decrease of with increasing in each stellar mass and redshift bin: galaxies below the MS are more concentrated than galaxies located on the MS or above it. Galaxies on the MS become more concentrated with increasing stellar mass, transforming from pure disks structures to bulge+disk ones. Also for galaxies below the MS the increases with increasing stellar mass. No increase in is observed in galaxies above the MS with respect to MS counterparts at fixed stellar mass, as found for the local counterparts in Morselli et al. (2017).

Figure 8: Mass-weighted Sérsic index, obtained from GALFIT, as a function of distance from the MS, , for the low and high redshift samples (left and right panels, respectively). The three stellar mass bins are represented with different colours. At all stellar masses, galaxies below the MS are more compact than MS counterparts, while galaxies above the MS have similar or lower Sérsic index than MS sources. An increase of the Sérsic index is visible on the MS relation, with increasing stellar mass.
Figure 9: From top to bottom: stacked maps of SFR, stellar mass, sSFR, uncorrected L, dust corrected L, and E(B-V) of galaxies with axis ratio , , , and Log(M/M). The six columns are the six bins of distance from the MS. On the right side of the figure, the median radial profiles of galaxies in each bin are showed using the same color code of Fig. 4 and Fig. 5. The trends shown in this figure hint towards inside-out quenching below the MS and enhanced SF activity above the MS.

3.2 Stacked maps

From what has been discussed thus far, the star formation activity in the central part of a galaxy seems to strongly correlate with the location of the galaxy in the LogSFR-LogM plane. Nevertheless, the sSFR and SFR surface density profiles from which these conclusions are drawn come from SED fitting, which is very sensitive to dust and, in general is the least stable method to derive SFRs. For this reason, we decided to further investigate the distribution of dust and UV luminosity (corrected and not-corrected for dust). Fig. 9 shows the mean stacked maps of SFR, stellar mass, sSFR, not-corrected UV luminosity, dust-corrected UV luminosity and E(B-V). The stacked maps have been built by excluding galaxies with axis ratio (obtained with GALFIT) and . These cuts avoid biases due to highly inclined galaxies, or to extremely compact/extended galaxies that are not representative of the galaxy population in the bins. We focus on the range and Log(M/M) so as to ensure the best statistics while trying to limit the width of the redshift range, as intrinsic differences in the shape of galaxies at different cosmic times can bias the results, as the individual maps are not normalised to the effective radii before stacking. In addition, the radial profiles computed as explained in Sec. 2.5 are also shown in Fig. 9 to better visualise trends (with the same color-coding used in Fig. 4 and Fig. 5).

The SFR maps show a monotonic increase of the SFR in the centre of galaxies when moving towards larger integrated SFRs. We underline here that even if the star formation activity is taking place in clumps in individual galaxies, the stacking procedure produces a ”smooth” distribution of SFR in the disk. In the SB bin, the distribution of SFR (as well as other properties) looks more disturbed, as the number of galaxies in this bin is small. Nevertheless, the increase of SFR in the central part is visible. The mass distribution shows that galaxies below the MS, in the quiescent region of the LogSFR-LogM plane, are less extended and more concentrated than MS and upper MS galaxies, reflecting the trends in Sérsic index observed both in the low-z and high-z sample (Fig.8). As discussed above, galaxies above the MS are more extended than MS counterparts. sSFR maps enhance the trends visible in the SFR maps. Below the MS we can clearly see that star formation activity is taking place only in the outskirts of galaxies. The position of the clumps of star formation obtained as a result of stacking analysis are irrelevant to this study. However, note that the ”hole” (or the lack of star formation) seen in the central part is a common feature of all the galaxies below the MS. The sSFR progressively increases in the central part of galaxies from the quiescent bins towards the MS and above it, but it is interesting to observe that also on the MS the sSFR in the outskirts is larger than in the inner region of galaxies. Above the MS, the distribution is smoother in the SUP1 sample. In the SB sample, the distribution reveals an increase of sSFR in the central part of the galaxy, as well as other clumps of SF in the outskirts. The UV luminosity maps also show a trend of increasing L in the centre with increasing integrated SFR, even without dust correction. The distribution is ”flat” for QUIE galaxies and progressively peaks in the central part of galaxies when moving towards larger integrated SFRs. Correcting for dust reveals a clumpy distribution of UV luminosity in the outskirts of galaxies in the QUIE and SUB2 samples, and further unveils the presence of a central depression of UV luminosity not visible when dust correction is not taken into account. When dust correction is applied, the UV luminosity in the central part of SB galaxies becomes more peaked than for SUP1 and MS galaxies. Finally, the trends seen in dust distribution are analogous to the ones seen for the SFR. A central hole in is visible in the stacked maps of QUIE and SUB2 galaxies, while for the remaining bins the distribution peaks at the centre, and the peak value increases with increasing integrated SFR. We underline here that the average trends visible in the stacked maps of Fig. 9 are not biased by our stacking procedure, or by selection effects caused by limiting the sample to nearly face-on galaxies. The visual inspection of all maps confirms that, while the extension of the central region might vary from system to system, the central ”hole” in sSFR in galaxies below the MS and the central SF enhancement in galaxies above it are visible in all systems of the two categories, respectively.

The analysis of the stacked maps of galaxy properties presented in Fig. 9 shows that the radial trends observed in SFR and sSFR are reliable against dust correction and thus underline the importance of the central region of galaxies in determining the scatter of the MS and in understanding the quenching mechanism. We will discuss the possible scenarios arising from such trends in the next section.

4 Discussion

We discuss here how our results compare with others in literature, as well as the emerging picture on how galaxies move in the LogSFR-LogM plane.

4.1 SFR and sSFR profiles

The SFR and sSFR profiles of galaxies suggest a fundamental role of the star formation activity in the central region in determining the location of a source around the MS and, thus, in the LogSFR-LogM plane.

At fixed stellar mass, galaxies with the highest (lowest) SFR exhibit also the highest (lowest) SFR surface density within the inner 5 kpc. This leads to a clear trend as a function of the distance from the MS, with centrally active galaxies populating the region of the sequence and its upper envelope, and centrally suppresses galaxies located below the relation. We do observe a difference in the SFR level of the outskirts. However, this variation, in particular in the sSFR profile, is much lower (0.5-0.7dex) with respect to the variation in the central region (2-3 dex).

Figure 10: SFR from H as obtained by integrating the SFR profiles of N16 in different bins of distance from the MS and stellar mass, compared to the SFR from SED fitting.The two are in agreement within the large errors associated to SFR from SED fitting.

Most of previous studies relate the enhancement and suppression of the galaxy central region to the stellar mass. Spindler et al. (2017) analyse the distribution of star formation activity in MaNGA galaxies and its dependence on integrated mass, structure, and environment. They propose the existence of two classes of galaxies, namely Centrally Suppressed and Unsuppressed, defined as galaxies that have sSFR in their disk at least 10 times larger than the core, and galaxies with flat sSFR profiles respectively. They find that there is a strong dependence of the classification of galaxies as Centrally Suppressed and Unsuppressed on stellar mass. This is consistent with our finding of more pronounced decrease of sSFR in the inner part of galaxies with increasing stellar mass. Centrally Suppressed galaxies have up to 0.5 dex suppression in their sSFR at larger radii compared to Unsuppressed galaxies, which is also the maximum difference seen in our data in the sSFR values at r 5 kpc for star-forming and quiescent galaxies. Finally, when studying the dependence of central suppression of star formation on galaxy morphology, Splinder et al. (2017) conclude that it is strongly related to the presence of a bulge, in agreement with our findings of increased Sérsic index in galaxies with the deepest central depression in their sSFR profiles.

Belfiore et al. (2017) analyze the H equivalent width profiles of MaNGA galaxies, and find that the typical sSFR profile of MS galaxies is flat at LogM 10.5 M, while the sSFR of more massive MS galaxies shows a decrease in the central region. This result is partially in disagreement with our findings for the low-z sample, as we observe that the sSFR profiles of MS galaxies is always smaller in the central 5 kpc than at larger radii even if the difference is only up to 0.5 dex. This discrepancy is most likely due to different selection criteria for MS galaxies in the two works. In fact, in Belfiore et al. (2017) MS galaxies are not distinguishable from upper MS and SB galaxies, which might exhibit a centrally enhanced SFR profile. As a consequence, the median profile is flat and shows a decrease at inner radii only at larger stellar masses, when the depression in the SFR profile of MS galaxies becomes more significant. Our median SFR profiles as a function of galaxy distance from the MS are in qualitative agreement with the ones reported by Ellison et al. (2017). In both studies, galaxies above the MS are characterized by a considerable enhancement of SFR surface density in the central regions, while passive galaxies show a depression in the inner part. The result of centrally-suppressed SFR profiles in passive galaxies is also in agreement with the study of Delgado et al. (2013), which analyze CALIFA galaxies to study the dependence of the SFR profile on morphological classification. They find that SFR profiles of disk-like galaxies increase towards the centre, while galaxies and ellipticals have centrally suppressed profiles. This is compatible with our observations as galaxies whose SFR profile is suppressed at the centre also exhibit Sérsic indexes comparable to bulge+disk systems, or pure spheroidal morphologies below the MS (see Fig. 8).

As we discussed above, no evolution is seen between the low-z and high-z samples. The only marginal difference between the two samples is related to SB galaxies. In fact, we do not find many of them in the high redshift bin. Those few tend to exhibit a less significant central enhancement in the SFR profile with respect to the MS galaxies, as clearly visible, instead, in the low redshift bin. However, this could also be due to the low number statistics in the highest redshift bin, in which the SB region is not much populated in our dataset. This would suggest that the distribution of the SF activity in galaxies is driving the scatter of the MS in the same way at least up to z1.2.

Nelson et al. (2016) present the average surface SFR and sSFR profiles based on H luminosity in the 3D-HST sample. The subsample is, in particular, H flux-selected in the redshift range [0.7:1.5]. The authors find evidence of a ”coherent” SFR distribution, whereas above the MS the SFR profile is on average enhanced at all radii, while below the MS, it is suppressed at all radii, but with a very similar shape. They also observe an enhancement of the SF activity in the central region towards the upper envelope of the MS, although less significant than in our results and limited to a small stellar mass range. The spatial region investigated by N16 is limited to the inner 6-8 kpc, while SED fitting gives us the possibility to explore a wider area, up to 15-20 kpc. In addition, their below MS subsample includes galaxies down to -0.8 dex from the MS and it does not sample sources in the quiescence region, as our SUB2 and QUIE subsamples. The two sets of SFR profiles are in agreement within the inner kpc when galaxies are selected in a consistent way as a function of the distance from the MS. We find that the mean integrated H-based SFR and the SED fitting-based SFR for the same class of galaxies agree well (see Fig. 10) and are consistent within the errors. Those are obtained by integrating the H-based SFR profiles of N16 and the HDUV profiles of this work for the same class of galaxies in the same redshift range. We notice instead a disagreement with the stellar mass distribution. While in N16 the stellar mass profiles of galaxies above, on, and below the MS are remarkably similar, in this work we find that the stellar mass distribution of galaxies well below the MS is always more compact and centrally peaked than MS counterparts, as also revealed by the study of the Sersic index and in agreement with previous studies (e.g. Whitaker et al. 2014 and references therein). As a consequence we obtain a sSFR profile more centrally suppressed than in N16 for galaxies below the MS. Furthermore, due to the H selection, in N16 the region below the MS is highly incomplete and potentially biased towards H bright sources of the subsample. This could lead to SFR profiles more similar to those of MS galaxies and less flat as observed in our work, where the completeness is much higher in the quiescence region.

Other recent works investigating the spatial distribution of SFR in galaxies are based on small samples for which high spatial resolution data is available. Tacchella et al. (2015b) studied H derived SFR profiles in 22 galaxies at z 2 (resolution 1 kpc) and observed that the average profiles do not change with stellar mass (and are consistent with a disk-like profile). We also do not observe significant changes in the SFR profiles of MS galaxies at different stellar masses. More recently, Tacchella et al. (2017a) show dust, UV, and H dust-corrected profiles for 10 galaxies at z 2 and found centrally suppressed sSFR profiles only in the most massive bin (MM), while a flat sSFR profile is observed at MM. In our sample, central suppression is always visible in the sSFR profiles of galaxies in the high-z sample, but the suppression becomes more significant at increasing stellar masses. In the same work, the authors also argue that galaxies above the MS have sSFR characterised by a central enhancement, in agreement with what is suggested by the trends in our profiles.

4.2 Stellar mass distribution across - along the MS

While our work on the sSFR and SFR profiles is in clear agreement with previous results, the trends in stellar mass distribution across the MS and for galaxies with the largest SFRs present a challenge. In Morselli et al. (2017) we study the the structure of z 0 SDSS galaxies using the B/T decomposition of Simard et al. (2011) and find that the MS of star-forming galaxies corresponds to the minimum of the B/T distribution at each stellar mass; in other words, galaxies in the upper envelope of the MS are characterised by a larger B/T with respect to MS counterparts. The result, while in agreement with the original work of Wuyts et al. (2011), does not comply with the findings of this work where an opposite trend of decreasing Sérsic index is observed when moving from the MS towards its upper envelope. This discrepancy could be ascribed to the fact that, since we employ the small inner region of the GOODS sample, we are missing real starburst galaxies located more than one dex above the MS.These galaxies that we miss in our current sample could be pure spheroidals (Almaini et al. 2017), the inclusion of which would increase the average Sérsic index of galaxies above the MS.

On the other hand, the morphological trend of increasing Sérsic index along the MS is confirmed by different works in recent literature, both at low (Bluck et al. 2014; Morselli et al. 2017) and high (Lang et al. 2014) redshift. Such trends, together with the more pronounced decrease of the sSFR of MS galaxies with increasing stellar mass, indicate that galaxies grow their bulge component while moving along the MS, and that star formation in massive MS galaxies takes place only in the disk, while the bulges remain passive, as argued in Tacchella et al. (2015a)

4.3 Migration of galaxies across the MS and implications on quenching mechanism

The shapes of the observed SFR and sSFR profiles are compatible with the compaction-depletion scenario of Tacchella et al. (2015b), based on the VELA simulations (Ceverino et al., 2014). These studies propose a scenario where star forming galaxies migrate across the MS due to the successive episodes of gas inflow and star formation ongoing in the central part. Here, cold gas flowing to the inner region of galaxies causes an overall compaction of the system, which in turn leads to a phase of high star formation activity. Following this, central depletion of gas due to star formation forces a galaxy below the MS. As a result, sSFR profiles of galaxies are expected to be centrally enhanced (suppressed) above (below) the MS, which is in good agreement with our findings.

The shape of the SFR and sSFR profiles is also a powerful tool to obtain information on the nature of the quenching mechanism. The coherent star formation picture presented in Nelson et al. (2016) was used to conclude that the suppression of star formation at all radii, observed for galaxies below the MS, must be related to a quenching mechanism that acts not only in the central part of galaxies but also troughout the disk. The central suppression observed in the sSFR profiles of galaxies below the MS is compatible with the so-called quenching mechanism, where the star formation halts first in the innermost radii and then in the outer regions of the disk, implying that disks are still forming stars when the central part of a galaxy is dominated by a passive bulge. Such a quenching mechanism has been advocated frequently in recent studies. Morishita & Ichikawa (2016) used HST/WFC3 and ACS observations to study UV rest frame colours of Milky Way progenitors in . Despite the uncertainties in using UV colours as SFR tracers, they find that quenching must first occur in the central region, followed by the outskirts. Tacchella et al. (2015a) employ the centrally-suppressed sSFR profiles of massive MS galaxies to conclude that quenching must proceed in an fashion, with timescales ranging from few hundred million years in the central regions to a few billion years at larger radii. In Tacchella et al. (2016) the authors used cosmological simulations to extract a sample of 26 galaxies at and found that the onset of gas depletion occurs in the central 1 kpc and follows a phase of wet compaction and SFR peaked in the centre. The quenching hence also proceeds , implying that when the central region is passive star formation is still ongoing in an outer ring. A small sample of 10 star forming galaxies at z 2, observed as part of a SINS/zC-SINF AO program, is used in Tacchella et al. (2017a) to study dust and UV profiles. They find that only massive galaxies (MM) show sSFR profiles that are suppressed in the centre with respect to the outskirts and hence must be experiencing quenching. More work needs to be done in order to understand the main driver behind the suppression of the central star formation, f.e. by SFHs of quiescent galaxies.

4.4 Summary

In this work, we exploit multi-wavelength, high-resolution HST imaging to study the spatially resolved properties of galaxies located in the central parts of the GOODS fields. We summarise our main findings as follows:

  • the sSFR profiles of galaxies in the redshift range is centrally enhanced above the MS and centrally suppressed below the MS, with quiescent galaxies characterised by the deepest suppression. The sSFR in the outer region does not show systematic trends of enhancement or suppression above or below the MS.

  • the Sérsic index of MS galaxies increases with increasing stellar mass, indicating that bulges are growing when galaxies are still on the relation. Galaxies are also more bulge-dominated in the lower envelope of the MS, while galaxies in the upper envelope are more extended and have Sérsic indexes that are always smaller than or comparable to their MS counterparts.

These findings suggest that galaxies above the MS could be in a evolutionary phase where cold gas is available in the central region, possibly due to minor mergers or disk instabilities, but no compaction has still taken place. Furthermore, our work indicates that inside-out quenching is indeed taking place, as star formation is centrally-suppressed in galaxies below the MS, but still occurs in the outer regions. Follow up studies are warranted in order to: 1) increase the statistics, especially above the MS so as to cover the area at 1 dex from the relation, and 2) investigate the spatial distribution of cold gas so as to understand the reasons behind the growth of the bulge observed below the MS, e.g. the stabilisation of the disk against further collapse vs. removal of cold gas due to AGN activity.

Aknowledgements

LM thanks Erica Nelson and Pieter van Dokkum for comments that greatly improved the analysis, and Sandro Tacchella for giving useful feedback on the manuscript. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. Support for this work was provided by NASA through grant HST-GO-13872 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. LM thanks Bhaskar Agarwal and Matias Blana for useful and stimulating discussion.

References

  • Abramson et al. (2014) Abramson L. E., Kelson D. D., Dressler A., Poggianti B., Gladders M. D., Oemler A. J., Vulcani B., 2014, The Astrophysical Journal Letters, 785, L36
  • Allen et al. (2006) Allen P. D., Driver S. P., Graham A. W., Cameron E., Liske J., De Propris R., 2006, arXiv.org, pp 2–18
  • Almaini et al. (2017) Almaini O., et al., 2017, Monthly Notices of the Royal Astronomical Society, 472, 1401
  • Arnouts et al. (1999) Arnouts S., Cristiani S., Moscardini L., Matarrese S., Lucchin F., Fontana A., Giallongo E., 1999, Monthly Notices, 310, 540
  • Balogh et al. (2004) Balogh M. L., Baldry I. K., Nichol R., Miller C., Bower R., Glazebrook K., 2004, The Astrophysical Journal, 615, L101
  • Belfiore et al. (2017) Belfiore F., et al., 2017, arXiv.org, p. arXiv:1710.05034
  • Bell et al. (2005) Bell E. F., et al., 2005, The Astrophysical Journal, 625, 23
  • Bernhard et al. (2014) Bernhard E., Bethermin M., Sargent M., Buat V., Mullaney J. R., Pannella M., Heinis S., Daddi E., 2014, Monthly Notices of the Royal Astronomical Society, 442, 509
  • Blanton & Moustakas (2009) Blanton M. R., Moustakas J., 2009, Annual Review of Astronomy and Astrophysics, 47, 159
  • Blanton et al. (2005) Blanton M. R., Eisenstein D., Hogg D. W., Schlegel D. J., Brinkmann J., 2005, The Astrophysical Journal, 629, 143
  • Bluck et al. (2014) Bluck A. F. L., Mendel J. T., Ellison S. L., Moreno J., Simard L., Patton D. R., Starkenburg E., 2014, Monthly Notices of the Royal Astronomical Society, 441, 599
  • Brusa et al. (2010) Brusa M., et al., 2010, The Astrophysical Journal, 716, 348
  • Bruzual & Charlot (2003) Bruzual G., Charlot S., 2003, Monthly Notices of the Royal Astronomical Society, 344, 1000
  • Calzetti et al. (2000) Calzetti D., Armus L., Bohlin R. C., Kinney A. L., Koornneef J., Storchi-Bergmann T., 2000, The Astrophysical Journal, 533, 682
  • Chabrier (2003) Chabrier G., 2003, The Publications of the Astronomical Society of the Pacific, 115, 763
  • Cheung et al. (2012) Cheung E., et al., 2012, The Astrophysical Journal, 760, 131
  • Cibinel et al. (2015) Cibinel A., et al., 2015, The Astrophysical Journal, 805, 181
  • Daddi et al. (2007) Daddi E., et al., 2007, The Astrophysical Journal, 670, 156
  • Delgado et al. (2013) Delgado R. G., et al., 2013, The Intriguing Life of Massive Galaxies, 295, 300
  • Dressler (1980) Dressler A., 1980, Astrophysical Journal, 236, 351
  • Drory et al. (2009) Drory N., et al., 2009, arXiv.org, pp 1595–1609
  • Elbaz et al. (2007) Elbaz D., et al., 2007, Astronomy & Astrophysics, 468, 33
  • Elbaz et al. (2011) Elbaz D., et al., 2011, Astronomy & Astrophysics, 533, A119
  • Ellison et al. (2017) Ellison S. L., Sanchez S. F., Ibarra-Medel H., Antonio B., Mendel J. T., Barrera-Ballesteros J., 2017, arXiv.org, p. arXiv:1711.00915
  • Erfanianfar et al. (2016) Erfanianfar G., et al., 2016, Monthly Notices of the Royal Astronomical Society, 455, 2839
  • Giavalisco et al. (2004) Giavalisco M., et al., 2004, The Astrophysical Journal, 600, L93
  • Goddard et al. (2017) Goddard D., et al., 2017, Monthly Notices of the Royal Astronomical Society, 465, 688
  • Grogin et al. (2011) Grogin N. A., et al., 2011, The Astrophysical Journal Supplement, 197, 35
  • Guo et al. (2015) Guo K., Zheng X. Z., Wang T., Fu H., 2015, arXiv.org, p. L49
  • Ilbert et al. (2006) Ilbert O., et al., 2006, Astronomy & Astrophysics, 457, 841
  • Ilbert et al. (2009) Ilbert O., et al., 2009, arXiv.org, pp 644–663
  • Karim et al. (2011) Karim A., et al., 2011, The Astrophysical Journal, 730, 61
  • Kauffmann et al. (2003) Kauffmann G., et al., 2003, Monthly Notice of the Royal Astronomical Society, 341, 54
  • Koekemoer et al. (2011) Koekemoer A. M., et al., 2011, The Astrophysical Journal Supplement, 197, 36
  • Kriek et al. (2009) Kriek M., van Dokkum P. G., Franx M., Illingworth G. D., Magee D. K., 2009, The Astrophysical Journal Letters, 705, L71
  • Lang et al. (2014) Lang P., et al., 2014, The Astrophysical Journal, 788, 11
  • Lin et al. (2017) Lin L., et al., 2017, arXiv.org, p. arXiv:1710.08610
  • Lutz et al. (2011) Lutz D., et al., 2011, Astronomy & Astrophysics, 532, A90
  • Magnelli et al. (2013) Magnelli B., et al., 2013, Astronomy & Astrophysics, 553, A132
  • Magnelli et al. (2014) Magnelli B., et al., 2014, Astronomy & Astrophysics, 561, A86
  • Maragkoudakis et al. (2017) Maragkoudakis A., Zezas A., Ashby M. L. N., Willner S. P., 2017, Monthly Notices of the Royal Astronomical Society, 466, 1192
  • Martig et al. (2009) Martig M., Bournaud F., Teyssier R., Dekel A., 2009, The Astrophysical Journal, 707, 250
  • Meurer et al. (1999) Meurer G. R., Heckman T. M., Calzetti D., 1999, The Astrophysical Journal, 521, 64
  • Momcheva et al. (2016) Momcheva I. G., et al., 2016, The Astrophysical Journal Supplement Series, 225, 27
  • Morgan & Mayall (1957) Morgan W. W., Mayall N. U., 1957, Publications of the Astronomical Society of the Pacific, 69, 291
  • Morishita & Ichikawa (2016) Morishita T., Ichikawa T., 2016, The Astrophysical Journal, 816, 87
  • Morselli et al. (2017) Morselli L., Popesso P., Erfanianfar G., Concas A., 2017, Astronomy & Astrophysics, 597, A97
  • Muzzin et al. (2013) Muzzin A., et al., 2013, The Astrophysical Journal, 777, 18
  • Nelson et al. (2016) Nelson E. J., et al., 2016, The Astrophysical Journal, 828, 27
  • Noeske et al. (2007) Noeske K. G., et al., 2007, The Astrophysical Journal, 660, L47
  • Oesch et al. (2018) Oesch P. A., et al., 2018, arXiv.org, p. arXiv:1806.01853
  • Overzier et al. (2011) Overzier R. A., et al., 2011, The Astrophysical Journal Letters, 726, L7
  • Pannella et al. (2006) Pannella M., Hopp U., Saglia R. P., Bender R., Drory N., Salvato M., Gabasch A., Feulner G., 2006, arXiv.org, pp L1–L4
  • Pannella et al. (2009) Pannella M., et al., 2009, arXiv.org, pp L116–L120
  • Peng (2010) Peng C., 2010, American Astronomical Society, 215, 229.09
  • Peng et al. (2010) Peng Y.-j., et al., 2010, The Astrophysical Journal, 721, 193
  • Popesso et al. (2012) Popesso P., et al., 2012, Astronomy & Astrophysics, 537, A58
  • Pozzetti et al. (2009) Pozzetti L., et al., 2009, arXiv.org, p. A13
  • Renzini & Peng (2015) Renzini A., Peng Y.-j., 2015, The Astrophysical Journal Letters, 801, L29
  • Robert C Kennicutt (1998) Robert C Kennicutt J., 1998, arXiv.org, pp 189–232
  • Rodighiero et al. (2010) Rodighiero G., et al., 2010, Astronomy & Astrophysics, 518, L25
  • Schreiber et al. (2015) Schreiber C., et al., 2015, Astronomy & Astrophysics, 575, A74
  • Shao et al. (2010) Shao L., et al., 2010, Astronomy & Astrophysics, 518, L26
  • Simard et al. (2011) Simard L., Mendel J. T., Patton D. R., Ellison S. L., McConnachie A. W., 2011, The Astrophysical Journal Supplement, 196, 11
  • Skelton et al. (2014) Skelton R. E., et al., 2014, The Astrophysical Journal Supplement Series, 214, 24
  • Speagle et al. (2014) Speagle J. S., Steinhardt C. L., Capak P. L., Silverman J. D., 2014, arXiv.org, p. 15
  • Spindler et al. (2017) Spindler A., et al., 2017, arXiv.org, p. arXiv:1710.05049
  • Steinhardt et al. (2017) Steinhardt C. L., Yurk D., Capak P., 2017, Monthly Notices of the Royal Astronomical Society, 468, 849
  • Szomoru et al. (2013) Szomoru D., Franx M., van Dokkum P. G., Trenti M., Illingworth G. D., Labbé I., Oesch P., 2013, The Astrophysical Journal, 763, 73
  • Tacchella et al. (2015a) Tacchella S., et al., 2015a, Science, 348, 314
  • Tacchella et al. (2015b) Tacchella S., et al., 2015b, The Astrophysical Journal, 802, 101
  • Tacchella et al. (2016) Tacchella S., Dekel A., Carollo C. M., Ceverino D., DeGraf C., Lapiner S., Mandelker N., Primack J. R., 2016, Monthly Notices of the Royal Astronomical Society, 458, 242
  • Tacchella et al. (2017a) Tacchella S., et al., 2017a, arXiv.org, p. arXiv:1704.00733
  • Tacchella et al. (2017b) Tacchella S., et al., 2017b, arXiv.org, p. 56
  • Tal et al. (2013) Tal T., van Dokkum P. G., Franx M., Leja J., Wake D. A., Whitaker K. E., 2013, The Astrophysical Journal, 769, 31
  • Whitaker et al. (2012) Whitaker K. E., van Dokkum P. G., Brammer G., Franx M., 2012, The Astrophysical Journal Letters, 754, L29
  • Whitaker et al. (2014) Whitaker K. E., et al., 2014, The Astrophysical Journal, 795, 104
  • Wuyts et al. (2011) Wuyts S., et al., 2011, The Astrophysical Journal, 742, 96
  • Zibetti (2009) Zibetti S., 2009, arXiv.org, p. arXiv:0911.4956
  • Ziparo et al. (2013) Ziparo F., et al., 2013, Monthly Notices of the Royal Astronomical Society, 434, 3089
  • Zolotov et al. (2015) Zolotov A., et al., 2015, Monthly Notices of the Royal Astronomical Society, 450, 2327
  • van der Wel et al. (2012) van der Wel A., et al., 2012, The Astrophysical Journal Supplement, 203, 24

Appendix A Radial profiles normalised for effective radii

Here we show the SFR and sSFR surface densities median profiles, where the distance from the centre of each galaxy has been normalised to the mass-weighted effective radius. Fig. 11 shows the result for the low-z sample, and Fig. 12 for the high-z one, respectively. The trends in the SFR and sSFR surface density, computed as a function of the physical distance from the galaxy centre and analysed in Sec. 3.1, are still observed now that the distance is normalised for the mass-weighted effective radii. Galaxies above the MS and galaxies below it have SFR surface densities that differ of up to 2.5 order of magnitudes within 1 R, while in the outer regions the SFR surface densities of galaxies are comparable and independent on their distance from the relation. Analogously, differences up to 2.5 orders of magnitude are observed within one R between the sSFR surface density of galaxies in the QUIE and SUP1/SB samples, and such a difference become less significant at larger radii. As discussed in Sec. 4 we consider such trends to be evidence of inside-out quenching.

Figure 11: Median SFR (first row), stellar mass (second row), and sSFR (third row) surface densities as a function of distance from the centre (in R/R) for galaxies in the redshift range [0.2:0.7]. The three columns indicate galaxies with different stellar masses: 9.5Log(M/M)10.0 in the first, 10.0Log(M/M)10.5 in the second, and 10.5Log(M/M)11.0 in the third column, respectively. Different colours mark different bins of distance from the MS, as defined in Fig. 4. In the second row, the average Sérsic indexes of galaxies in the 6 bins are written at the top of the panel, with colours corresponding to the bins. We observe than the trend of decreasing sSFR surface density in the central region of galaxies with increasing distance below the MS is also visible when considering the distance from the centre normalised by the mass-weighted effective radii.
Figure 12: Same as Fig.11, but for galaxies in the redshift range [0.7:1.2]. Also in this redshift bin the sSFR surface density in the central region of galaxies decreases significantly when moving from the MS towards lower SFRs.
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
326884
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description