The UV window on counter rotating ETGs: insight from SPH simulations with chemo-photometric implementation

Bettoni, D.; Mazzei, P.; Rampazzo, R.; Marino, A. D.; Galletta, G.; Buson, L. M.

doi:10.1007/s10509-014-1973-0

Cited by 10 publications

(10 citation statements)

References 43 publications

(39 reference statements)

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“…disk vs. bulge) and kinematical (gas vs. stars) properties, showing that a major merger (1:1) accounts for the structural and photometric transformations expected in these systems (Querejeta et al 2015). Furtheremore, our approach allowed us to fit the current global properties of i) several other ETGs (Spavone et al 2009(Spavone et al , 2012Trinchieri et al 2012;Bettoni et al 2011Bettoni et al , 2012Bettoni et al , 2014, ii) the blue dwarf galaxy UGC 7639 (Buson et al 2015), iii) a few late-type galaxies of different luminosity classes (Bettoni et al 2011(Bettoni et al , 2014, iv) a pre-merger case, NGC 454 (Plana et al 2017), and v) the false pair NGC 3447/3447A (Mazzei et al 2018), showing that this a powerful tool to investigate galaxy evolution.…”

Section: Introductionmentioning

confidence: 93%

Investigating Early-type Galaxy Evolution with a Multiwavelength Approach. III. Insights from SPH Simulations with Chemophotometric Implementation

Mazzei¹,

Rampazzo²,

Marino³

et al. 2019

ApJ

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We are exploring galaxy evolution in low density environments exploiting smooth particle hydrodynamic simulations including chemo-photometric implementation. From a large grid of simulations of galaxy encounters and mergers starting from triaxial halos of gas e dark matter, we single out the simulations matching the global properties of our targets. These simulations are used to give insights into their evolution. We focus on 11 early-type galaxies selected because of their nearly passive stage of evolution in the nuclear region. However, a variety of UV features are detected in more than half of these galaxies. We find no significant differences in the formation mechanisms between galaxies with or without UV features. Major and minor mergers are able to reproduce their peculiar UV morphologies, galaxy encounters are more suitable for 'normal' early-type galaxies. Their star formation rate self-quenches several Gyr later the merger/encounter occurred, via gas exhaustion and stellar feedback, moving the galaxy from blue to red colors, driving the galaxy transformation. The length of the quenching is mass dependent and lasts from 1 to 5 Gyr or more in the less massive systems. All our targets are gas rich at redshift 1. Three of them assembled at most 40% of their current stellar mass at z>1, and seven assembled more than 50% between redshift 0.5 and 1. Their stellar mass grows with 4% by crossing the Green Valley before reaching their current position on the NUV−r vs. M r diagram.

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Section: Introductionmentioning

confidence: 93%

Investigating Early-type Galaxy Evolution with a Multiwavelength Approach. III. Insights from SPH Simulations with Chemophotometric Implementation

Mazzei¹,

Rampazzo²,

Marino³

et al. 2019

ApJ

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“…Later studies have shown that not only these objects can have some residual star formation activity (e.g. Yi et al 2005;Pipino et al 2009;Salim & Rich 2010;Bettoni et al 2014;Davis et al 2015;Haines et al 2015;Stasińska et al 2015;Sheen et al 2016;Vazdekis et al 2016;López-Corredoira & Vazdekis 2018), but also that some post-main-sequence stellar evolutionary phases are also efficient UV emitters (e.g. post-asymptotic giant branch -post-AGB -, blue horizontal branch -HB -stars, binary systems in interaction, and so on, Greggio & Renzini 1990;Brown 1999;O'Connell 1999;Greggio & Renzini 1999;Deharveng et al 2002;Brown 2004;Yoon et al 2004;Maraston 2005;Han et al 2007;Coelho et al 2009;Donahue et al 2010;Loubser & Sánchez-Blázquez 2011;Hernández-Pérez & Bruzual 2014, and references therein).…”

Section: Introductionmentioning

confidence: 99%

UV bright red-sequence galaxies: how do UV upturn systems evolve in redshift and stellar mass?

Dantas

Coelho

Gonçalves

2019

Monthly Notices of the Royal Astronomical Society

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The so-called ultraviolet (UV) upturn of elliptical galaxies is a phenomenon characterised by the up-rise of their fluxes in bluer wavelengths, typically in the 1,200-2,500 A range. This work aims at estimating the rate of occurrence of the UV upturn over the entire red-sequence population of galaxies that show significant UV emission. This assessment is made considering it as function of three parameters: redshift, stellar mass, and -what may seem counter-intuitive at first -emission-line classification. We built a multiwavelength spectro-photometric catalogue from the Galaxy Mass Assembly survey, together with aperture-matched data from Galaxy Evolution Explorer and Sloan Digital Sky Survey, covering the redshift range between 0.06 and 0.40. From this sample, we analyse the UV emission among UV bright galaxies, by selecting those that occupy the red-sequence locus in the (NUV-r) × (FUV-NUV) chart; then, we stratify the sample by their emission-line classes. To that end, we make use of emission-line diagnostic diagrams, focusing the analysis in retired/passive lineless galaxies. Then, a Bayesian logistic model was built to simultaneously deal with the effects of all galaxy properties (including emission-line classification or lack thereof). The main results show that retired/passive systems host an up-rise in the fraction of UV upturn for redshifts between 0.06 and 0.25, followed by an in-fall up to 0.35. Additionally, we show that the fraction of UV upturn hosts rises with increasing stellar mass.

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“…Stasińska et al 2015;Evans et al 2018;López-Corredoira & Vazdekis 2018) started to be considered as potential explanations (e.g. Yi et al 2005;Kaviraj et al 2007a,b;Pipino et al 2009;Salim & Rich 2010;Bettoni et al 2014;Davis et al 2015;Haines et al 2015;Sheen et al 2016;Vazdekis et al 2016, and references therein). Also, with the better understanding of stellar evolution, other rare stellar evolutionary phases started to be acknowledged as potential culprits for the UV upturn.…”

Section: Introductionmentioning

confidence: 99%

UV upturn versus UV weak galaxies: differences and similarities of their stellar populations unveiled by a de-biased sample

Dantas,

Coelho,

Sánchez-Blázquez

2020

Preprint

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The ultraviolet (UV) upturn is characterised by an unexpected up-rise of the UV flux in quiescent galaxies between the Lyman limit and 2500 Å. By making use of colour-colour diagrams, one can subdivide UV bright red-sequence galaxies in two groups: UV weak and upturn. With these two groups, we propose a comparison between their stellar population properties with the goal of establishing differences and similarities between them. We make use of propensity score matching (PSM) to mitigate potential biases between the two samples, by selecting similar objects in terms of redshift and stellar mass. Also, we take advantage of spectral energy distribution (SED) fitting results from magphys made available by the GAMA collaboration. The analyses are made by comparing the distributions from the SED fitting directly, as well as investigating the differences in correlations between their parameters, and finally by using principal component analysis (PCA). We explore important differences and similarities between UV weak and upturn galaxies in terms of several parameters, such as: metallicity, age, specific star formation rate, time of last burst of star-formation, to mention a few. Notable differences are those concerning (g − r) colour, metallicity, and time since last burst of star-formation: UV upturn are redder in the optical, more metallic, and their last burst of star-formation happened earlier in time. These differences suggest that UV upturn systems have shorter star-formation histories (i.e. have been evolving more passively) when compared to UV weak galaxies. Consequently, these last seem to have a higher diversity of stellar populations.

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The UV window on counter rotating ETGs: insight from SPH simulations with chemo-photometric implementation

Cited by 10 publications

References 43 publications

Investigating Early-type Galaxy Evolution with a Multiwavelength Approach. III. Insights from SPH Simulations with Chemophotometric Implementation

Investigating Early-type Galaxy Evolution with a Multiwavelength Approach. III. Insights from SPH Simulations with Chemophotometric Implementation

UV bright red-sequence galaxies: how do UV upturn systems evolve in redshift and stellar mass?

UV upturn versus UV weak galaxies: differences and similarities of their stellar populations unveiled by a de-biased sample

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