Coincidence between morphology and star formation activity through cosmic time: the impact of the bulge growth

Dimauro, Paola; Daddi, E.; Shankar, Francesco; Cattaneo, Andrea; Huertas-Company, M.; Bernardi, Mariangela; Caro, Fernando; Dupke, Renato A.; Häußler, Boris; Evelyn, Johnston; Cortesi, A.; Mei, S.; Peletier, R. F.

doi:10.1093/mnras/stac884

Cited by 33 publications

(23 citation statements)

References 160 publications

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“…For almost a century, starting with Hubble in (1926), astronomers have linked the morphology of galaxies to the physics of galaxy formation and evolution. Morphology has been shown to be related to many fundamental properties of the galaxy and its environment, including galaxy mass, star formation rate, stellar kinematics, merger history, cosmic environment, and the influence of supermassive black holes (e.g., Bender et al 1992;Tremaine et al 2002;Pozzetti et al 2010;Wuyts et al 2011;Schawinski et al 2014;Huertas-Company et al 2016;Powell et al 2017;Shimakawa et al 2021;Dimauro et al 2022). Studying the morphology of large samples of galaxies at different redshifts is crucial in order to understand the physics of galaxy formation and evolution.…”

Section: Introductionmentioning

confidence: 99%

GaMPEN: A Machine-learning Framework for Estimating Bayesian Posteriors of Galaxy Morphological Parameters

Ghosh

Urry

Rau

et al. 2022

ApJ

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We introduce a novel machine-learning framework for estimating the Bayesian posteriors of morphological parameters for arbitrarily large numbers of galaxies. The Galaxy Morphology Posterior Estimation Network (GaMPEN) estimates values and uncertainties for a galaxy’s bulge-to-total-light ratio (L B /L T ), effective radius (R e ), and flux (F). To estimate posteriors, GaMPEN uses the Monte Carlo Dropout technique and incorporates the full covariance matrix between the output parameters in its loss function. GaMPEN also uses a spatial transformer network (STN) to automatically crop input galaxy frames to an optimal size before determining their morphology. This will allow it to be applied to new data without prior knowledge of galaxy size. Training and testing GaMPEN on galaxies simulated to match z < 0.25 galaxies in Hyper Suprime-Cam Wide g-band images, we demonstrate that GaMPEN achieves typical errors of 0.1 in L B /L T , 0.″17 (∼7%) in R e , and 6.3 × 104 nJy (∼1%) in F. GaMPEN's predicted uncertainties are well calibrated and accurate (<5% deviation)—for regions of the parameter space with high residuals, GaMPEN correctly predicts correspondingly large uncertainties. We also demonstrate that we can apply categorical labels (i.e., classifications such as highly bulge dominated) to predictions in regions with high residuals and verify that those labels are ≳97% accurate. To the best of our knowledge, GaMPEN is the first machine-learning framework for determining joint posterior distributions of multiple morphological parameters and is also the first application of an STN to optical imaging in astronomy.

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Section: Introductionmentioning

confidence: 99%

GaMPEN: A Machine-learning Framework for Estimating Bayesian Posteriors of Galaxy Morphological Parameters

Ghosh

Urry

Rau

et al. 2022

ApJ

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“…It has often been remarked that galaxies more massive than the MS bending host increasingly more massive bulges, to the extent that considering only the disk-like components and ascribing to them the SFR, one gets closer to a rising trend in the MS (Abramson et al 2014;Mancini et al 2019;Dimauro et al 2022). It is worth reconsidering this matter here, in light of our systematic discussion of the evolution of M 0 .…”

Section: Discussionmentioning

confidence: 92%

“…It is worth reconsidering this matter here, in light of our systematic discussion of the evolution of M 0 . We use the results of Dimauro et al (2018Dimauro et al ( , 2019Dimauro et al ( , 2022, who performed bulge-disk decomposition in 0 < z < 2 galaxies in CANDELS using a machine learning approach to identify bulge+disk systems. Limiting the results to colour-selected SF galaxies as in this letter, we can derive the stellar masses along the MS at which the average bulge/total (B/T ) mass fraction in galaxies exceeds 0.2 and 0.4 (Fig.…”

Section: Discussionmentioning

confidence: 99%

“…(2), dashed blue line; based on Mandelker et al 2020a,b, dotted blue line), and stellar mass function (SMF) M * values(Ilbert et al 2013; linear fit to their redshift trends; solid for the total, dotted for those of quiescent and SF galaxies that are decreasing and increasing with redshift, respectively). The masses at which the average bulge/total (B/T ) ratio in MS galaxies rises above 0.2 and 0.4 are based onDimauro et al (2022; green long-dashed). Measurements and relations are converted from stellar to halo masses (and vice versa) using the SHMRs fromBehroozi et al (2013).…”

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confidence: 99%

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The bending of the star-forming main sequence traces the cold- to hot-accretion transition mass over 0 < z < 4

Daddi

Delvecchio

Dimauro

et al. 2022

A&A

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We analyse measurements of the evolving stellar mass (ℳ0 ) at which the bending of the star-forming main sequence (MS) occurs over 0 < z < 4. We find ℳ0 ≈ 1010 M⊙ over 0 < z < 1 before ℳ0 rises up to ∼1011 M⊙ at z = 2 and then stays flat or slowly increases towards higher redshifts. When converting ℳ0 values into hosting dark matter halo masses, we show that this behaviour is remarkably consistent with the evolving cold- to hot-accretion transition mass, as predicted by theory and defined by the redshift-independent Mshock at z < 1.4 and by the rising Mstream at z ≳ 1.4 (for which we propose a revision in agreement with the latest simulations). We therefore argue that the MS bending is primarily due to a drop in cold accretion, causing a reduction in available cold gas in galaxies, which supports predictions of gas feeding theory. In particular, the rapidly rising ℳ0 with redshift at z > 1 is evidence in favour of the cold-streams scenario. In this picture, a progressive fuelling reduction rather than its sudden suppression in halos more massive than Mshock/Mstream produces a nearly constant star-formation rate in galaxies with stellar masses larger than ℳ0, and not their quenching, which therefore requires other physical processes. Compared to the knee M* in the stellar mass function of galaxies, ℳ0 is significantly lower at z < 1.5, and higher at z > 2, suggesting that the imprint of gas deprivation on the distribution of galaxy masses happened at early times (z > 1.5–2). The typical mass at which galaxies inside the MS become bulge-dominated evolves differently from ℳ0, which is consistent with the idea that bulge formation is a distinct process from the phasing out of cold accretion.

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“…The ICLf M of RXJ1007 peaks roughly (given the F606W width) at ∼5400 Å (4300 Å-6500 Å) encompassing the peak emission of G-main-sequence stars. Once the late-type stars in the member galaxy outskirts are removed, it is plausible that tidal stripping would start to remove earlier-type populations closer to the central regions of the galaxies, which differ from those stars responsible for the BIE in that they would be redder and have significantly longer lifespans, assuming that processes of galaxy rejuvenation (e.g., Fang et al 2013;Mancini et al 2019;Dimauro 2022) are not significant.…”

Section: Discussionmentioning

confidence: 99%

Independent Evidence for Earlier Formation Epochs of Fossil Groups of Galaxies through the Intracluster Light: The Case for RX J100742.53+380046.6

Dupke

Jiménez-Teja

et al. 2022

ApJ

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Fossil groups (FG) of galaxies still present a puzzle to theories of structure formation. Despite the low number of bright galaxies, they have relatively high velocity dispersions and ICM temperatures often corresponding to cluster-like potential wells. Their measured concentrations are typically high, indicating early formation epochs as expected from the originally proposed scenario for their origin as being older undisturbed systems. This is, however, in contradiction with the typical lack of expected well developed cool cores. Here, we apply a cluster dynamical indicator recently discovered in the intracluster light fraction (ICLf) to a classic FG, RX J1000742.53+380046.6, to assess its dynamical state. We also refine that indicator to use as an independent age estimator. We find negative radial temperature and metal abundance gradients, the abundance achieving supersolar values at the hot core. The X-ray flux concentration is consistent with that of cool core systems. The ICLf analysis provides an independent probe of the system’s dynamical state and shows that the system is very relaxed, more than all clusters, where the same analysis has been performed. The specific ICLf is about 6 times higher, than any of the clusters previously analyzed, which is consistent with an older noninteractive galaxy system that had its last merging event within the last ∼5 Gyr. The specific ICLf is predicted to be an important new tool to identify fossil systems and to constrain the relative age of clusters.

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Coincidence between morphology and star formation activity through cosmic time: the impact of the bulge growth

Cited by 33 publications

References 160 publications

GaMPEN: A Machine-learning Framework for Estimating Bayesian Posteriors of Galaxy Morphological Parameters

GaMPEN: A Machine-learning Framework for Estimating Bayesian Posteriors of Galaxy Morphological Parameters

The bending of the star-forming main sequence traces the cold- to hot-accretion transition mass over 0 < z < 4

Independent Evidence for Earlier Formation Epochs of Fossil Groups of Galaxies through the Intracluster Light: The Case for RX J100742.53+380046.6

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