Facundo A. Gómez

University of La Serena

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Robert J. J. Grand

Instituto de Astrofísica de Canarias

Federico Marinacci

University of Bologna

Rüdiger Pakmor

Max Planck Institute for Astrophysics

Volker Springel

Max Planck Institute for Astrophysics

Carlos S. Frenk

Durham University

Christine M. Simpson

Argonne National Laboratory

Francesca Fragkoudi

Durham University

Antonela Monachesi

University of La Serena

Simon D. M. White

Max Planck Institute for Astrophysics

Azadeh Fattahi

Durham University

Cooperative Institutions

Max Planck Society

Max Planck Institute for Astronomy

Centre National de la Recherche Scientifique

Durham University

Max Planck Institute for Astrophysics

Istituto Nazionale di Fisica Nucleare

University of Turin

University of Bologna

Consejo Nacional de Investigaciones Científicas y Técnicas

Istituto Nazionale di Fisica Nucleare, Sezione di Torino

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Galaxy evolution in compact groups II. Witnessing the influence of major structures in their evolution

arXiv (Cornell University) (2024)

Gissel P. Montaguth Antonela Monachesi S. Torres-Flores Facundo A. Gómez Círia Lima-Dias

Compact groups (CGs) of galaxies are extreme environments for morphological transformations and the cessation of star formation. Our objective is to understand the dynamics of CGs and how their surrounding environment impacts galaxy properties. We selected a sample of 340 CGs in the Stripe 82 region, totaling 1083 galaxies, and a control sample of 2281 field galaxies. We find that at least 27\% of our sample of CGs are part of major structures, i.e. non-isolated CGs. We find a bimodality in the effective radius ($R_e$)-S\'ersic index ($n$) plane for all transition galaxies (those with $(u-r) > 2.3$ and $n<2.5$) in CGs. Additionally, transition galaxies in isolated CGs populate more densely the $R_e-n$ plane for $n < 1.75$. In contrast, transition galaxies in non-isolated CGs have smoothly increasing $n$ values, suggesting these galaxies have already suffered morphological transformation, and primarily contribute to the distribution of more compact galaxies in the $R_e-n$ plane for all transition galaxies in CGs. We also find significant differences in the specific star-formation rate (sSFR) distribution between the late-type galaxies (LTGs) ($(u-r)<2.3$ and $n< 2.5$) in non-isolated CGs and the same type of galaxies in the control sample, suggesting that the evolution of LTGs differs in non-isolated CGs. Early-type galaxies ($(u-r)>2.3$ and $n>2.5$) and transition galaxies in non-isolated CGs have lower sSFR values and a higher fraction of quenched galaxies, compared to those in isolated CGs. Based on our results, we propose an evolutionary scenario where the major structures in which the CGs are embedded accelerate the morphological transformations of their members. Our findings highlight the importance of considering the larger structures in which CGs may be located, when analysing the properties of their galaxy, as this can significantly affect the evolution of CGs and their galaxies.

10.48550/arxiv.2406.14671

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Cosmological evolution of metallicity correlation functions from the Auriga simulations

arXiv (Cornell University) (2024)

Zefeng Li Robert J. J. Grand Emily Wisnioski J. Trevor Mendel Mark R. Krumholz

We study the cosmological evolution of the two-point correlation functions of galactic gas-phase metal distributions using the 28 simulated galaxies from the Auriga Project. Using mock observations of the $z = 0$ snapshots to mimic our past work, we show that the correlation functions of the simulated mock observations are well matched to the correlation functions measured from local galaxy surveys. This comparison suggests that the simulations capture the processes important for determining metal correlation lengths, the key parameter in metallicity correlation functions. We investigate the evolution of metallicity correlations over cosmic time using the true simulation data, showing that individual galaxies undergo no significant systematic evolution in their metal correlation functions from $z\sim 3$ to today. In addition, the fluctuations in metal correlation length are correlated with but lag ahead fluctuations in star formation rate. This suggests that re-arrangement of metals within galaxies occurs at a higher cadence than star formation activity, and is more sensitive to the changes of environment, such as galaxy mergers, gas inflows / outflows, and fly-bys.

10.48550/arxiv.2402.08632

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On the correlation between the local dark matter and stellar velocities

Journal of Cosmology and Astroparticle Physics (2019)

Nassim Bozorgnia Azadeh Fattahi D. G. Cerdeño Carlos S. Frenk Facundo A. Gómez

The dark matter velocity distribution in the Solar neighbourhood is an important astrophysical input which enters in the predicted event rate of dark matter direct detection experiments. It has been recently suggested that the local dark matter velocity distribution can be inferred from that of old or metal-poor stars in the Milky Way. We investigate this potential relation using six high resolution magneto-hydrodynamical simulations of Milky Way-like galaxies of the Auriga project. We do not find any correlation between the velocity distributions of dark matter and old stars in the Solar neighbourhood. Likewise, there are no strong correlations between the local velocity distributions of dark matter and metal-poor stars selected by applying reasonable cuts on metallicity. In some simulated galaxies, extremely metal-poor stars have a velocity distribution that is statistically consistent with that of the dark matter, but the sample of such stars is so small that we cannot draw any strong conclusions.

10.1088/1475-7516/2019/06/045

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Exploring the outskirts of the EAGLE disc galaxies

Monthly Notices of the Royal Astronomical Society (2022)

S. Varela P. B. Tissera Facundo A. Gómez Lucas Bignone Claudia del P. Lagos

ABSTRACT Observations show that the surface brightness of disc galaxies can be well-described by a single exponential (TI), up-bending (TIII), or down-bending (TII) profiles in the outskirts. Here we characterize the mass surface densities of simulated late-type galaxies from the eagle project according to their distribution of mono-age stellar populations, the star formation activity, and angular momentum content. We find a clear correlation between the inner scale lengths and the stellar spin parameter, λ, for all three disc types with λ > 0.35. The outer scale lengths of TII and TIII discs show a positive trend with λ, albeit weaker for the latter. TII discs prefer fast rotating galaxies. With regards to the stellar age distribution, negative and U-shape age profiles are the most common for all disc types. Positive age profiles are determined by a more significant contribution of young stars in the central regions, which decrease rapidly in the outer parts. TII discs prefer relative higher contributions of old stars compared to other mono-age populations across the discs whereas TIII discs become progressively more dominated by intermediate age (2–6 Gyr) stars for increasing radius. The change in slope of the age profiles is located after the break of the mass surface density. We find evidence of larger flaring for the old stellar populations in TIII systems compared to TI and TII, which could indicate the action of other processes. Overall, the relative distributions of mono-age stellar populations and the dependence of the star formation activity on radius are found to shape the different disc types and age profiles.

Stellar mass

10.1093/mnras/stac1536

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10 Years Search for Neutrino Bursts with LVD

International Cosmic Ray Conference (2003)

M. Aglietta E. D. Alyea P. Antonioli G. Badino G. Bari

1. AbstractThe Large Volume Detector LVD (Gran Sasso National Laboratory, Italy),is a neutrino telescope mainly designed to search for low energy neutrino burstsfrom Gravitational Stellar Collapses (GSC) in the Galaxy. The experiment hasbeen monitoring the Milky Way since June 1992 under increasing larger conﬁg-urations, reaching in January 2001 the ﬁnal active mass of 1000 t. No burstcandidate has been detected over all the ten years of observation: we present herethe obtained limit to the rate of SuperNova (SN) event in the galaxy.

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Vertical density waves in the Milky Way disc induced by the Sagittarius Dwarf Galaxy

Boletin de la Asociacion Argentina de Astronomia La Plata Argentina (2012)

Facundo A. Gómez Ivan Minchev Brian W. O’Shea Timothy C. Beers James S. Bullock

Recently, Widrow and collaborators announced the discovery of vertical density waves in the Milky Way disk. Here we investigate a scenario where these waves were induced by the Sagittarius dwarf galaxy as it plunged through the Galaxy. Using numerical simulations, we find that the Sagittarius impact produces North-South asymmetries and vertical wave-like behavior that qualitatively agrees with what is observed. The extent to which vertical modes can radially penetrate into the disc, as well as their amplitudes, depend on the mass of the perturbing satellite. We show that the mean height of the disc is expected to vary more rapidly in the radial than in the azimuthal direction. If the observed vertical density asymmetry is indeed caused by vertical oscillations, we predict radial and azimuthal variations of the mean vertical velocity, correlating with the spatial structure. These variations can have amplitudes as large as 8 km/s.

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The star formation histories of dwarf galaxies in Local Group cosmological simulations

Monthly Notices of the Royal Astronomical Society (2019)

Ruth A. R. Digby Julio F. Navarro Azadeh Fattahi Christine M. Simpson Kyle A. Oman

We use the apostle and Auriga cosmological simulations to study the star formation histories (SFHs) of field and satellite dwarf galaxies. Despite sizeable galaxy-to-galaxy scatter, the SFHs of apostle and Auriga dwarfs exhibit robust average trends with galaxy stellar mass: faint field dwarfs (105 < Mstar/M⊙ < 106) have, on average, steadily declining SFHs, whereas brighter dwarfs (107 < Mstar/M⊙ < 109) show the opposite trend. Intermediate-mass dwarfs have roughly constant SFHs. Satellites exhibit similar average trends, but with substantially suppressed star formation in the most recent ∼5 Gyr, likely as a result of gas loss due to tidal and ram-pressure stripping after entering the haloes of their primaries. These simple mass and environmental trends are in good agreement with the derived SFHs of Local Group (LG) dwarfs whose photometry reaches the oldest main-sequence turn-off. SFHs of galaxies with less deep data show deviations from these trends, but this may be explained, at least in part, by the large galaxy-to-galaxy scatter, the limited sample size, and the large uncertainties of the inferred SFHs. Confirming the predicted mass and environmental trends will require deeper photometric data than currently available, especially for isolated dwarfs.

Local Group

10.1093/mnras/stz745

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Citations (36)

Analysis of the Events Recorded by the LVD Neutrino De- tector From Large Solar Flares During High Solar Activity

International Cosmic Ray Conference (2003)

M. Aglietta E. D. Alyea P. Antonioli G. Badino G. Bari

The results of the analysis of events recorded by the LVD neutrino detector at Gran Sasso Laboratory during the maximum peak of the high solar activity (including the very intense Bastille solar flare) are reported. The analysis of

Solar flare

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Solar energetic particles

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The Origin of r-process Enhanced Metal-poor Halo Stars In Now-destroyed Ultra-faint Dwarf Galaxies

The Astrophysical Journal (2019)

Kaley Brauer Alexander P. Ji Anna Frebel Gregory A. Dooley Facundo A. Gómez

The highly r-process enhanced (r-II) metal-poor halo stars we observe today could play a key role in understanding early ultra-faint dwarf galaxies, the smallest building blocks of the Milky Way. If a significant fraction of metal-poor r-II halo stars originated in the ultra-faint dwarf galaxies that merged to help form the Milky Way, observations of r-II stars could help us study these now-destroyed systems and probe the formation history of our Galaxy. To conduct our initial investigation into this possible connection, we use high-resolution cosmological simulations of Milky-Way-mass galaxies from the Caterpillar suite in combination with a simple, empirically motivated treatment of r-process enrichment. We determine the fraction of metal-poor halo stars that could have formed from highly r-process enhanced gas in now-destroyed low-mass ultra-faint dwarf galaxies, the simulated r-II fraction, and compare it to the "as observed" r-II fraction. We find that the simulated fraction, f_{r-II,sim} ~ 1-2%, can account for around half of the "as observed" fraction, f_{r-II,obs} ~ 2-4%. The "as observed" fraction likely overrepresents the fraction of r-II stars due to incomplete sampling, though, meaning f_{r-II,sim} likely accounts for more than half of the true f_{r-II,obs}. Further considering some parameter variations and scatter between individual simulations, the simulated fraction can account for around 20-80% of the "as observed" fraction.

Dwarf spheroidal galaxy

Mass fraction

10.3847/1538-4357/aafafb

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Clash of Titans: A MUSE dynamical study of the extreme cluster merger SPT-CL J0307-6225

Monthly Notices of the Royal Astronomical Society (2022)

D. Hernández-Lang A. Zenteno A. Diaz-Ocampo H. Cuevas John Clancy

ABSTRACT We present MUSE spectroscopy, Megacam imaging, and Chandra X-ray emission for SPT-CL J0307-6225, a $z = 0.58$ major merging galaxy cluster with a large BCG-SZ centroid separation and a highly disturbed X-ray morphology. The galaxy density distribution shows two main overdensities with separations of 0.144 and 0.017 arcmin to their respective BCGs. We characterize the central regions of the two colliding structures, namely 0307-6225N and 0307-6225S, finding velocity derived masses of M200, N = 2.44 ± 1.41 × 1014M⊙ and M200, S = 3.16 ± 1.88 × 1014M⊙, with a line-of-sight velocity difference of |Δv| = 342 km s−1. The total dynamically derived mass is consistent with the SZ derived mass of 7.63 h$_{70}^{-1}$ ± 1.36 × 1014M⊙. We model the merger using the Monte Carlo Merger Analysis Code, estimating a merging angle of 36$^{+14}_{-12}$ ° with respect to the plane of the sky. Comparing with simulations of a merging system with a mass ratio of 1:3, we find that the best scenario is that of an ongoing merger that began 0.96$^{+0.31}_{-0.18}$ Gyr ago. We also characterize the galaxy population using Hδ and [O ii] λ3727 Å lines. We find that most of the emission-line galaxies belong to 0307-6225S, close to the X-ray peak position with a third of them corresponding to red-cluster sequence galaxies, and the rest to blue galaxies with velocities consistent with recent periods of accretion. Moreover, we suggest that 0307-6225S suffered a previous merger, evidenced through the two equally bright BCGs at the centre with a velocity difference of ∼674 km s−1.

Line (geometry)

10.1093/mnras/stac2480

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