El Gordo (ACT-CL J0102-4915) is a massive galaxy cluster with two major mass components at redshift z = 0.87. Using spectral energy distribution fitting results from JWST/NIRCam photometry, the fraction of quenched galaxies in this cluster was measured in two bins of stellar mass: 9 <= log(M-* /M-circle dot ) < 10 and 10 log(M /M ) < 12. While there is no correlation between the quenched fraction and angular separation from the cluster's overall center of mass, there is a correlation between the quenched fraction and angular separation from the center of the nearest of the two mass components for the less-massive galaxies. This suggests that environmental quenching processes are in place at z similar to 1, and that dwarf galaxies are more affected by those processes than massive galaxies.

Although the James Webb Space Telescope has received much attention for its ability to search deeper into the cosmos than ever before, it also enhances our capability to study objects closer to us in the Universe. We apply a methodology of subtracting intracluster light from the PLCK G165.7+67.0 (G165; z = 0.35) cluster, revealing a population of unresolved pointlike sources including globular clusters (GCs). By applying a fitting algorithm in color space used to select galaxy cluster members, we uncover over 900 GC candidates from our point-source sample. We also identify candidates by estimating the contribution of interlopers to the point-source sample, yielding an estimate of 793 +/- 83 GC candidates. We find the color-selected sources to be approximately spatially correlated with the intracluster light and lensing mass of the cluster. The observed luminosity function of the sources shows a turnover point fainter than the completeness limit, so we use fixed-parameter curve-fitting models to predict a k-corrected turnover point in the range -9.4 mag <= M-F200W <= -10.7 mag, although we predict the expected k-corrected turnover point should be closer to -7.7 mag <= M-F200W <= -8.4 mag. We discuss the dynamical state of this disturbed galaxy cluster with a bimodal mass distribution using the spatial distribution of GC candidates and find that the radial profiles of our color-selected GC candidates are very consistent with the lensing-derived surface mass density at >50 kpc.

As part of the SKYSURF Hubble Space Telescope (HST) Legacy Archival programme we present galaxy number counts which yield measurements of the extragalactic background light (EBL) at 15 different wavelengths. We have processed 82,752 HST images across 23 filters into 16 686 mosaics using the same software and processing pipeline throughout. Using 17/23 filters that give reliable galaxy counts, we constrain the integrated galaxy light (IGL) with a 1.4-9 per cent error between 0.3 and 1.6 mu m in combination with 8 bands from WAVES (Wide Area VISTA Extragalactic Survey) and DEVILS (Deep Extragalactic Visible Legacy Survey). While HST was never intended to undertake large area surveys, through extensive quality control and filtering, we were able to extract a reliable and representative sample of fields distributed across the sky. Our final catalogues cover a combined approximate to 19.6 deg2 , with individual filters covering areas ranging from approximate to 0.16-7.0 deg2 . The combination of numerousindependentsight-lines and area coverage allows usto reduce cosmic variance uncertainties in deep number counts to 0.21-1.8 per cent. For the first time we are able to establish a measurement of the IGL, 8.85 +/- 0.30 nW m-2 sr-1, at 0.59 mu m using HST data. We obtain a cosmic optical background value of 25.36 +/- 0.52 nW m-2 sr-1. Different techniques used to measure the COB, both directly and indirectly, have recently converged indicating that the COB arises almost exclusively from processes within galaxies. This in combination with the recent values reported from New Horizons and very high energy (VHE) constraints leaves very little room for any diffuse emission coming from outside the Milky Way

Galaxy mergers are a central driver of galaxy evolution across cosmic time, and thus, quantifying their frequency is critical for constraining hierarchical models of galaxy formation. Motivated by the need to robustly quantify these fractions and their evolution, we build on our previous close-pair analysis by exploring morphological identification techniques within the Deep Extragalactic VIsible Legacy Survey, using the D10 (COSMOS) field, which covers an area of 1.47 deg(2). While close-pairs trace the early stages of galaxy interactions, morphological methods probe more advanced phases of the merging process, including systems with disturbed structures and post-merger remnants. We present galaxy merger fractions over the redshift range 0.2

The internal structure of galaxies encodes the complex baryon cycle driven by gas accretion, star formation, and feedback, together with secular evolution and environmentally driven processes such as mergers and tidal interactions. We present a population-level census of massive nearby galaxies (log(M_⋆/M_⊙) > 10) by comparing Hyper Suprime-Cam Subaru Strategic Program observations with matched mock images from IllustrisTNG, EAGLE, and SIMBA. Using a consistent, like-for-like imaging pipeline, we construct structural abundance functions (SAFs) for key morphological parameters, revealing a structural abundance crisis. Across Sérsic index, concentration, size, and ellipticity, all simulations exhibit large, systematic discrepancies (>5σ; RMSE ∼ 0.2–1.8 dex), typically corresponding to abundance differences of factors of several. While individual simulations display diverse failures—underproducing or overproducing compact spheroids, extended or round galaxies —all underproduce highly flattened disks. Although TNG shows the closest agreement and SIMBA the largest offsets, this shared failure indicates that current models—despite matching global demographics such as the stellar mass function—do not uniquely constrain internal galaxy structure. Our results demonstrate that agreement in integrated observables can mask fundamental shortcomings in the modelling of mass and angular momentum redistribution. We therefore establish SAFs as a stringent, multidimensional, and observationally accessible benchmark for testing and calibrating next-generation galaxy formation models in the era of upcoming deep, wide-field surveys.

We compute the cosmic stellar, dust, and neutral gas mass history at 0 < z less than or similar to 3 using PROSPECT spectral energy distribution modelling of approximate to 800 000 galaxies in the Galaxy and Mass Assembly survey and the Deep Extragalactic VIsible Legacy Survey. The cosmic dust mass history broadly follows the shape of the cosmic star formation history; however, the decline is slower, suggestive of a slowing rate of dust growth and destruction as the star formation declines past its peak at z approximate to 2 . Neutral gas masses were estimated by scaling the dust masses by the metallicity-dependent dust-to-gas ratio. The neutral gas mass density as traced by the dust is an average of approximate to 0 . 7 dex lower than that measured from 21 cm experiments, most likely due to differences in the spatial scales inhabited by dust and HI. Folding in measurements of the supermassive black hole (SMBH) mass density obtained previously with similar data and methods, we present a self-consistent census of the baryons confined to galaxies. Stars, neutral gas, SMBHs, and dust contained within the optical radii of galaxies account for ti 5 per cent of the baryons. Most of the remaining ti 95 per cent of baryons must be ionized and dispersed throughout the interstellar, circumgalactic, and intergalactic media within, around, and between galaxies.

We present SM-Net, a machine-learning model that learns a continuous spectral manifold from multiple high-resolution stellar libraries. SM-Net generates stellar spectra directly from the fundamental stellar parameters effective temperature (Teff), surface gravity (log g), and metallicity (log Z). It is trained on a combined grid derived from the PHOENIX-Husser, C3K-Conroy, OB-PoWR, and TMAP-Werner libraries. By combining their parameter spaces, we construct a composite dataset that spans a broader and more continuous region of stellar parameter space than any individual library. The unified grid covers Teff = 2,000-190,000 K, log g = -1 to 9, and log Z = -4 to 1, with spectra spanning 3,000-100,000 Angstrom. Within this domain, SM-Net provides smooth interpolation across heterogeneous library boundaries. Outside the sampled region, it can produce numerically smooth exploratory predictions, although these extrapolations are not directly validated against reference models. Zero or masked flux values are treated as unknowns rather than physical zeros, allowing the network to infer missing regions using correlations learned from neighbouring grid points. Across 3,538 training and 11,530 test spectra, SM-Net achieves mean squared errors of 1.47 x 10^-5 on the training set and 2.34 x 10^-5 on the test set in the transformed log1p-scaled flux representation. Inference throughput exceeds 14,000 spectra per second on a single GPU. We also release the model together with an interactive web dashboard for real-time spectral generation and visualisation. SM-Net provides a fast, robust, and flexible data-driven complement to traditional stellar population synthesis libraries.

Galaxy mergers are key drivers of galaxy formation and evolution, including triggering active galactic nucleus (AGN) and star formation to a still unknown degree. We thus investigate the impact of galaxy mergers on star formation and AGN activity using 3330 galaxies at z = 4.5-8.5 from eight James Webb Space Telescope fields (CEERS, JADES GOODS-S, NEP-TDF, NGDEEP, GLASS, El-Gordo, SMACS-0723, and MACS-0416), covering an unmasked area of 189 arcmin(2). We focus on star formation rate (SFR) enhancement, AGN fraction, and AGN excess in close pairs defined by Delta z < 0.3 and projected separations r(p) < 100 kpc, relative to non-merger samples. Close pairs with mass ratios greater than 1:4 are used for the SFR-enhancement analysis, whereas no mass-ratio constraint is applied for the AGN fraction and AGN excess measurements. We find SFR enhancement occurs only at r(p) < 20 kpc, with values 0.25 +/- 0 .10 dex and 0 .26 +/- 0 .11 dex above non-merger medians for z = [4.5 , 6.5] and z = [6.5 , 8.5] , respectively. No other statistically significant enhancements in galaxy sSFR or stellar mass are observed at any projected separation or redshift. We also compare observational results with predictions from the SC-SAM simulation, finding no evidence of star formation enhancement in simulations at any separation. Lastly, we examine the fraction and excess of AGNs identified through photometric spectral energy distributions (SED) fitting (Type-I) and BPT diagnostics (Type-II). We find 48(-7)(+33) % of Type-I and 44(-20)(+26)% of Type-II AGNs have a close companion within r(p) < 50 kpc and Delta z < 0.3.Furthermore, 73(-32)( +27)% of AGNs have companions within 100 kpc. Relative to isolated galaxies, we measure an AGN excess factor of 1.26(-0.04)(+0.15 )for Type-I and 1.34(-0.11 )(+0.23)for Type-II AGNs in close pairs, suggesting notable AGN enhancement in galaxy pairs at these higher redshifts.

We describe the drizzling pipeline and contents of the drizzled database for Hubble Space Telescope Cycle 27–29 Archival Legacy project “SKYSURF,” the largest archival project ever approved for Hubble. SKYSURF aims to investigate the extragalactic background light using all 143,914 ACSWFC, WFC3UVIS, and WFC3IR images that have been taken by Hubble since its launch in 2002. SKYSURF has produced 38,027 single-visit mosaics and 7893 multivisit mosaics across 28 ACSWFC, WFC3UVIS, and WFC3IR filters using nonstandard drizzling methods, which include preserving the lowest sky-level of each visit/group in the drizzled products, applying wider apertures for cosmic-ray rejection, correcting effects caused by charge transfer efficiency degradation, and removing potential light gradients from input images via sky-map subtraction. We generate source catalogs for all drizzled products with SExtractor and provide updated star–galaxy separation parameters and integrated galaxy light (IGL) estimates for 25 of the 28 SKYSURF filters (wavelength range 0.2–1.7 μ m) using a novel IGL fitting method made possible by the vast SKYSURF dataset. We discuss the data processing and data analysis challenges encountered, detail our solutions, and offer suggestions that may facilitate future large-scale IGL investigations with Webb, SPHEREx, and Roman.

We present 21 transients from our three-epoch, four-band NIRCam observations covering 14.16 arcmin ^2 in the Spitzer IRAC Dark Field (IDF), taken by the JWST Prime Extragalactic Areas for Reionization and Lensing Science program with a time cadence of ∼6 months. A separate Hubble Space Telescope program provided Advanced Camera for Surveys optical imaging contemporaneous with the second and third epochs of the NIRCam observations. The NIRSpec spectroscopy on three transients confirmed a Type Ia supernova at z = 1.63 and the host galaxies of the other two at z = 2.64 and 1.90, respectively. Combining these with the photometric redshifts ( z _ph ) of the host galaxies in the rest of the sample, we find that the transients are in either a “mid- z ” group at z > 1.6 with M _V ≲ − 16.0 mag or a “low- z ” group at z < 0.4 with M _H ≳ − 14.0 mag. The mid- z transients are consistent with supernovae. In contrast, the low- z transients’ luminosities fall in the range of the so-called “gap transients” between supernovae and novae. However, this latter conclusion is only tentative due to possible catastrophic failures in z _ph that could bias them to low- z . Conversely, if they are indeed at z < 0.4, it would be worth studying similar transients in the future. Our work further demonstrates the power of NIRCam in transient science and also shows that it would be more fruitful to carry out a long-term monitoring program with more passbands, a higher cadence, and prompt follow-up spectroscopy. Being in the continuous viewing zone of the JWST, the IDF is an ideal field for this purpose.

Determining how galaxies accumulate stellar mass is paramount to understanding the Universe. Two primary mechanisms drive this process: star-formation (SF) mergers. Our understanding of star formation, and to some degree the processes that influence the baryon cycle (environment, gas supply, feedback, etc), are either relatively well constrained or will develop significantly over the coming decades via upcoming facilities (i.e. through their imprint on galaxy properties measured with deep multi-wavelength and spectroscopic data). However, the same can not be said for mergers. It is telling that we indirectly know hierarchical assembly through mergers is one of the most crucial processes that shape our Universe, but the robust observational measurement of mergers is almost non-existent outside of the local Universe - let alone how these mergers impact galaxy properties. This is not likely to significantly change in the coming decades as existing or approved facilities/surveys are inadequate in charactering mergers in the distant Universe. Motivated by this, we discuss an ambitious study to first explore mergers, and then the co-dependent astrophysical process that govern the accumulation of stellar mass over the last 10billion years, and highlight the essential need for a 10m+ class multi-object spectroscopic facility.

The James Webb Space Telescope (JWST) has unveiled the existence of numerous z>10 bright ultraviolet (UV) galaxies, potentially challenging galaxy formation models in a Lambda Cold Dark Matter (LCDM) universe. Modifications to star formation and stellar feedback models have been suggested to alleviate the tension. However, the fundamental challenge is to design a galaxy formation model that simultaneously reproduces observations from z=0 to those at the highest redshifts. Here, we present predictions from the Shark semi-analytic model of galaxy formation, which is tuned to reproduce the z=0 universe. We show that the same model is capable of reproducing the current UV luminosity function constraints even up to z=17 without the need to invoke variations in the baryon physics model. This model is also capable of reproducing reasonably well the stellar mass function evolution from z=0 to z=10 and the cosmic star formation rate (SFR) density at 010. We demonstrate that without this mechanism, galaxies are not bursty enough in the model to reproduce the observations at z>10.

Internal gas inflows driven by galaxy mergers are considered to enhance star formation rates (SFR), fuel supermassive black hole growth and stimulate active galactic nuclei (AGN). However, quantifying these phenomena remains a challenge, due to difficulties both in classifying mergers and in quantifying galaxy and AGN properties. We quantitatively examine the merger-SFR-AGN connection using Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) galaxies using novel methods for both galaxy classification and property measurements.} {Mergers in HSC-SSP observational images are identified through fine-tuning Zoobot, a pretrained deep representation learning model, using images and labels based on the Galaxy Cruise project. We use galaxy and AGN properties that were produced by fitting Galaxy and Mass Assembly (GAMA) spectra using the SED fitting code ProSpect, which fits panchromatically across the far-UV through far-infrared wavelengths and obtains galaxy and AGN properties simultaneously.} \textbf{{Little differences are seen in SFR and AGN activity between mergers and controls, with $\Delta \mathrm{SFR}=-0.009\pm 0.003$ dex, $\Delta f_{\mathrm{AGN}}=-0.010\pm0.033$ dex and $\Delta L_{\mathrm{AGN}}=0.002\pm0.025$ dex. After further visual purification of the merger sample, we find $\Delta \mathrm{SFR}=-0.033\pm0.014$ dex, $\Delta f_{\mathrm{AGN}}=-0.024\pm0.170$ dex, and $\Delta L_{\mathrm{AGN}}=0.019\pm0.129$ dex for pairs, and $\Delta \mathrm{SFR}=-0.057\pm0.024$ dex, $\Delta f_{\mathrm{AGN}}=0.286\pm0.270$ dex, and $\Delta L_{\mathrm{AGN}}=0.329\pm0.195$ dex for postmergers. These numbers suggest secular processes being an important driver for SF and AGN activity, and present a cautionary tale when using longer timescale tracers.

The cosmic star formation history (CSFH) and cosmic active galactic nuclei (AGN) luminosity history (CAGNH) are self consistently measured at z = 5.5-13.5. This is achieved by analyzing galaxies detected by the James Webb Space Telescope from approximate to 400arcmin2 fields from the Prime Extragalactic Areas of Reionization and Lensing Science, Cosmic Evolution Early Release Science, Next Generation Deep Extragalactic Exploratory Public, JWST Advanced Deep Extragalactic Survey, and Public Release IMaging for Extragalactic Research surveys. In particular, the combination of spectral energy distribution fitting codes, EAZY and ProSpect, is employed to estimate the photometric redshifts and astrophysical quantities of 3751 distant galaxies, from which we compute the stellar mass, star formation rate, and AGN luminosity distribution functions in four redshift bins. Integrating the distribution functions, we find that the CSFH rises by approximate to 1 dex over z = 13.5-5.5, and the CAGNH rises by approximate to 1 dex over z = 10.5-5.5. We connect our results of the CSFH and CAGNH at z = 13.5-5.5 to that from z = 5-0 to determine the summary of greater than or similar to 13 Gyr of star formation and AGN activity, from the very onset of galaxy formation to the present day.

Internal gas inflows driven by galaxy mergers are considered to enhance star formation rates (SFRs), fuel supermassive black hole growth, and stimulate active galactic nuclei (AGNs). However, quantifying these phenomena remains a challenge, due to difficulties both in classifying mergers and in quantifying galaxy and AGN properties. We quantitatively examine the merger–SFR–AGN connection using Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) galaxies using novel methods for both galaxy classification and property measurements. Mergers in HSC-SSP observational images are identified through fine-tuning Zoobot, a pretrained deep representation learning model, using images and labels based on the Galaxy Cruise project. We use galaxy and AGN properties that were produced by fitting Galaxy and Mass Assembly spectra using the spectral energy distribution fitting code P ro S pect , which fits panchromatically across the far-ultraviolet through far-infrared wavelengths and obtains galaxy and AGN properties simultaneously. Small differences are seen in SFR and AGN activity between mergers and controls, with ΔSFR = −0.009 ± 0.003 dex, Δ f _AGN = −0.010 ± 0.033 dex, and Δ L _AGN = 0.002 ± 0.025 dex. After further visual purification of the merger sample, we find ΔSFR = −0.033 ± 0.014 dex, Δ f _AGN = −0.024 ± 0.170 dex, and Δ L _AGN = 0.019 ± 0.129 dex for pairs, and ΔSFR = −0.057 ± 0.024 dex, Δ f _AGN = 0.286 ± 0.270 dex, and Δ L _AGN = 0.329 ± 0.195 dex for postmergers. These numbers suggest secular processes being an important driver for star formation and AGN activity, and present a cautionary tale when using longer-timescale tracers.

We present JWST NIRSpec integral field spectroscopy observations of the z = 5.89 quasar NDWFS J1425+3254 from 0.6-5.3 mu m, covering the rest-frame ultraviolet and optical at a spectral resolution of R similar to 100. The quasar has a black hole mass of M-BH = (1.4(-1.0)(+3.1)) x 10(9) M-circle dot and an Eddington ratio of L-Bol/L-Edd = 0.3(-0.2)(+0.6), as implied from the broad Balmer H alpha and H beta lines. The quasar host has significant ongoing obscured star formation, as well as a quasar-driven outflow with velocity 6050(-630)(+460) km s(-1) and ionised outflow rate of 1650(-1230)(+130) M-circle dot yr(-1). This is possibly one of the most extreme outflows in the early Universe. The data also reveal that two companion galaxies are merging with the quasar host. The north-eastern companion galaxy is relatively old and very massive, with a luminosity-weighted stellar age of 65(-4)(+9) Myr, stellar mass of (3.6(-0.3)(+0.6))x10(11) M circle dot , and star-formation rate (SFR) of similar to 15-30 M-circle dot yr(-1). A bridge of gas connects this companion galaxy and the host, confirming their ongoing interaction. A second merger is occurring between the quasar host and a much younger companion galaxy to the south, with a stellar age of 6.7 +/- 1.8 Myr, stellar mass of (1.9 +/- 0.4)x10(10) M-circle dot, and SFR of similar to 40-65 M-circle dot yr(-1). There is also another galaxy in the field, likely in the foreground at z = 1.135, which could be gravitationally lensing the quasar with a magnification of 1 < mu < 2 and, thus, < 0.75 mag. Overall, the system is a 'train-wreck' merger of three galaxies, with star formation and extreme quasar activity that were likely triggered by these ongoing interactions.

Large-scale galaxy redshift surveys conducted over the last couple of decades have proven crucial in deepening our understanding of structure growth in the Universe and galaxy evolution. While there have been several such surveys, until now those that achieve the high completeness and precision necessary to probe the low-mass end of galaxy groups have been limited to relatively low redshifts (z≲0.3), with surveys exploring the more distant Universe being constrained by small sample sizes and/or low redshift completeness. The recent Deep Extragalactic VIsible Legacy Survey (DEVILS) aims to explore galaxy environment over the last ∼6 Gyr with a completeness level comparable to the most complete local Universe surveys (>85%). In this work, we present the galaxy group catalogue for the D10-COSMOS field from DEVILS, which achieves a redshift completeness of 90% for galaxies with Y<21.2 mag. We showcase the science potential by exploring the impact of environment on the fraction and power of active galactic nuclei (AGN), finding that satellites in galaxy groups show no evidence of altered AGN properties, while satellites in clusters exhibit increased AGN fractions but decreased AGN luminosities.

The combination of the z = 0–13.5 cosmic star formation history and active galactic nuclei (AGN) luminosity history, as inferred by the James Webb Space Telescope, is connected to the cosmic spectral energy distribution (SED) to explore the sources of reionization. We compute the redshift evolution of the corresponding cosmic ionizing photon emissivity, the neutral fraction, and the cosmic microwave background optical depth. We use the generative SED modelling code P ro S pect to bracket the ionizing emissivity between escape fractions of f esc = 1%–100% for both the stars and AGN. Stars alone could have achieved reionization by z ≈ 6 with f esc ≳ 30% for solar metallicity ( Z = 0.02) stars or f esc ≳ 10% for metal-poor ( Z = 10 −4 ) stars. On the other hand, AGN by themselves would have struggled to produce sufficiently many ionizing photons even with f esc = 100%. A hybrid model containing both stars and AGN is explored, where we find the best fit (median±1 σ ) f esc = 12% ( 1 4 − 7 + 9 % ) for the stars and f esc = 63% ( 6 0 − 32 + 28 % ) for the AGN, maintained at all redshifts. In essence, the joint growth of stellar mass and supermassive black holes produces neither more nor fewer ionizing photons than needed to reionize ≳99% of the intergalactic medium by z ≈ 6.

We present a full analysis of galaxy major merger pair fractions, merger rates, and mass accretion rates, thus uncovering the role of mergers in galaxy formation at the earliest previously unexplored epoch of 4.5 < z < 11.5. We target galaxies with masses log10 (M-*/M-circle dot) = 8.0-10.0, utilizing data from eight JWST Cycle-1 fields [CEERS (Cosmic Evolution Early Release Science Survey), JADES (JWST Advanced Deep Extragalactic Survey) GOODS-S, NEP-TDF (North Ecliptic Pole Time-Domain Field), NGDEEP (Next-Generation Deep Extragalactic Exploratory Public Survey), GLASS (Grism Lens Amplified Survey from Space), El-Gordo, SMACS-0723, MACS-0416], covering an unmasked area of 189.36 arcmin2. We develop a new probabilistic pair-counting methodology that integrates full photometric redshift posteriors and corrects for detection incompleteness to quantify close pairs with physical projected separations between 20 and 50 kpc. Our analysis reveals an increase in pair fractions up to z=8, reaching 0.211 +/- 0.065, followed by a statistically flat evolution to z=11.5. We find that the galaxy merger rate increases from the local Universe up to z=6 and then stabilizes at a value of similar to 6 Gyr(-1) up to z=11.5. The redshift evolution of both pair fractions and merger rates is well described by a power-law plus exponential model. In addition, we measure that the average galaxy increases its stellar mass due to mergers by a factor of 2.77 +/- 0.99 from redshift z=10.5 to z=5.0. Lastly, we investigate the impact of mergers on galaxy stellar mass growth, revealing that mergers contribute as much as 71 +/- 25 per cent to galaxy stellar mass growth. This indicates that mergers drive about half of galaxy assembly at high redshift.

We present the evolution of the size-mass relation since z = 1 in the COSMOS region of the Deep Extragalactic VIsible Legacy Survey (DEVILS). We combine structural decomposition measurements with stellar mass estimates from fitting spectral energy distributions to multiwavelength photometry. We implement a novel technique to fit 2D light profiles to repeated observations, removing the requirement to co-add images, which maximises the effective signal-to-noise ratio and avoids issues arising when averaging point spread functions. The sample is then separated into distinct morphological classifications, which reveals that the size-mass relation of disc-dominated galaxies shows an overall flattened slope with very little redshift evolution over 0 . 3 < z < 1 . 0. In contrast, spheroid-dominated morphologies show a much steeper relation and are generally more compact at a given stellar mass. The size-mass relations of bulge and disc components are also examined revealing that diffuse bulges occupy a similar region to disc structures, in stark contrast to the size-mass relation of compact bulges. Furthermore, the size-mass relation of discs becomes steeper in the presence of a compact bulge, whereas the relation for discs hosting a diffuse bulge is identical to that of pure-discs. The lack of evolution in disc-dominated galaxies (i.e. R-eff proportional to (1 + z)(-0 . 13 +/- 0 . 02) ) is inherent to their self-similar assembly. In contrast, the size-mass relation of spheroid-dominated morphologies is rapidly evolving despite minimal growth in the individual compact bulge components, with average sizes increasing at a pace of R-eff proportional to (1 + z)(-3.0 +/- 0 . 2) and a slope that flattens with time as dlog(10)(R-eff) /dlog(10)(M-star) proportional to (1 + z) (2 . 8 +/- 0 . 2) .