arXiv subjects

Maria Emilia De Rossi

Publications and source records attributed to Maria Emilia De Rossi.

17 recordsLinked to original sources

arXiv2026

Co-evolution of Supermassive Black Holes and their Host L* galaxies: implications for Milky Way and M31

We investigate the origin of the scatter in supermassive black hole (BH) masses among L* galaxies, using the ARTEMIS and EAGLE simulations. We classify galaxies by their central BH-to-stellar mass ratios and track systems with the lowest and highest ratios (LBH and HBH, respectively). Although these populations have similar properties at z~ 2, they diverge significantly towards lower redshifts. LBH galaxies maintain higher gas fractions and sustain star formation, while HBHs form stars earlier, experience faster BH growth, more efficient feedback, and subsequent quenching. The simulations broadly match the observed scatter in the BH masses and galaxy morphologies in the L* regime, linking it to differences in merger histories. Galaxies with more active merger histories host more massive BHs at present and are predominantly elliptical, whereas those with quieter histories host lower-mass BHs and tend to be disc-like. Mergers induce BH growth through enhanced gas accretion and direct BH-BH coalescences. However, these channels operate differently: in HBH galaxies, BHs grow primarily (~90%) through gas accretion, whereas in LBHs they grow through both gas accretion and BH--BH mergers, in comparable fractions. These results suggest that the contrasting BH masses in the Milky Way and M31 may arise from differences in their merger histories. We also investigate the role of feedback from supernovae (SN) versus active galactic nuclei (AGN) on these scales. AGN feedback appears to be the primary mechanism responsible for quenching MW-mass systems, although SN feedback remains the dominant regulator of their overall evolution.

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arXiv2026

Determining Total Infrared Luminosities from Submm Measurements of High Redshift Galaxies

Determining total infrared luminosities for very high redshift galaxies is important to estimate the rate of star formation in heavily dust-embedded environments. It is also challenging because the most sensitive far infrared observatory, Herschel, was limited in sensitivity and its deepest measurements are subject to confusion noise. Thus, these determinations largely depend on ALMA, observing in the mm- and/or submm-wavelengths, which sample only the long-wavelength part of the spectral energy distributions (SEDs). Luminosities are conventionally estimated with modified blackbody fits to these measurements, but do not include the emission in the mid-infrared by warmer dust; there is evidence that this mid-IR component may be relatively strong in very high-redshift galaxies compared with local ones. A correction factor must be applied to the modified black body luminosities to derive the total infrared luminosity. We study infrared SEDs using simulations tuned to galactic conditions typical of high-z galaxies. We find that the different behaviors of infrared SEDs are dominated by a single key physical parameter, the luminosity density. This allows us to estimate the corrections for the missing mid-infrared luminosity in a general way. We find that a factor of ~ 1.6 - 1.7 (0.2 dex) is appropriate in most circumstances, with a larger factor of ~ 1.75 - 1.85 (~ 0.25 dex) up to 2 (0.3 dex) necessary for high redshift (z > 4) galaxies at the highest luminosities, > 10^{12} Lsun. These corrections are needed to estimate star formation rates based on total infrared luminosity.

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arXiv2026

Characterizing the Formation and Evolution of S0-galaxies (CaFES-0): Revealing the origin of the mass-size relation for S0 galaxies

We investigate the structural evolution and formation pathways of lenticular (S0) galaxies using the Hydrangea suite of cosmological hydrodynamical simulations. Simulated galaxies reproduce the observed mass-size relation from the SAMI and MaNGA surveys, enabling a direct comparison between morphology, angular momentum, and size growth. We show that the S0 population occupies a characteristic V-shaped locus in the mass-size plane, which arises from the superposition of two physically distinct channels. Low-mass S0s are predominantly faded-formed S0s, quenched after infall into their present-day host halo and retaining the disk sizes of their star-forming progenitors. In contrast, high-mass S0s formed through mergers exhibit structural properties and size evolution similar to ellipticals, and typically quench before infall, consistent with pre-processing in group environments. By tracing their histories back to $z=1$, we find that faded-formed S0s experience minimal structural evolution after quenching, whereas merger-formed S0s grow significantly in size through dissipationless interactions. These divergent evolutionary pathways explain both the slope break and the overall scatter of the S0 mass-size relation, demonstrating that lenticular galaxies arise from multiple formation mechanisms that leave distinct structural imprints.

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arXiv2026

Characterizing the Formation and Evolution of S0-galaxies (CaFES-0): Their formation pathways around Galaxy Clusters

The formation pathways of lenticular galaxies (S0s), which lie morphologically between elliptical and spiral galaxies, remain a topic of active research. Environmental effects, merging histories, and pre-processing mechanisms are often proposed as key factors influencing their transformation. However, the relative importance of these processes remains unclear, particularly when compared with other galaxy types. We use the Hydrangea cosmological zoom-in simulation suite to analyse the environmental histories of S0 galaxies, defined here as central and satellite quenched disk galaxies. We find that the vast majority (>85\%) of our sample of S0s are satellites in massive haloes (log$_{10}$M$_{200}/$M$_\odot$ > 13), while only $\sim10\%$ are centrals in low-mass haloes. Satellite S0s exhibit a highly quiescent merging history, with $\sim60\%$ experiencing no significant mergers since $z=2$. Centrals show more varied merging histories, although our results may be affected by limited sample size. Contrary to expectations, no clear trends in merger ratios with morphology are observed. However, mergers involving lenticular and spiral galaxies tend to occur in low-density environments and are likely gas-rich, enabling disk reformation. Pre-processing effects in groups are critical, influencing both quenching and morphological transformation.} Our results strongly suggest that S0 galaxies predominantly form from faded/stripped spirals in clusters, with a minority forming via mergers in smaller haloes. These results are in agreement with previous observations of lenticular galaxies around galaxy clusters.

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arXiv2025

Unveiling the properties of the first galaxies with JWST and ALMA

The James Webb Space Telescope (JWST) is challenging our understanding of the nature of the very first galaxies in the Universe, having discovered a surprising abundance of very massive galaxies in early cosmic epochs. By applying a model of primeval dust, we estimate the far-infrared (FIR)-continuum luminosities for galaxies of different masses at redshifts $z\gtrsim7$. In particular, we predict observed fluxes for different available bands (3-10) of the Atacama Large Millimeter/sub-mm Array (ALMA), considering typical conservative values expected for the properties of first galaxies (e.g., gas-phase metallicities, dust-to-metal ratio, star formation efficiency). As expected, FIR fluxes increase with stellar mass for all ALMA bands, but with a steeper slope for bands 9 and 10. Encouragingly, first galaxies are affected by a strong negative-K correction, in such a way that sources with similar properties are brighter in bands 3-8 at higher redshifts. Such behavior is stronger for bands 6-7. Although the trends for bands 9-10 are not clear, the highest fluxes for such bands are reached towards extreme $z\gtrsim 15$. Counterintuitively, our results suggest that JWST sources with similar masses and dust properties would be more easily detectable with ALMA if they are located at higher $z$.

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arXiv2023

Probing the Nature of the First Galaxies with JWST and ALMA

By implementing a model of primordial dust emission, we predict dust-continuum fluxes for massive galaxy sources similar to those recently detected by JWST at $z \gtrsim 7$. Current upper flux limits, obtained with ALMA for some of these sources, can constrain gas metallicity and dust fraction of the first galaxies. Encouragingly, if assuming expected properties for typical first galaxies (i.e., dust-to-metal mass ratio: $D/M = 5 \times 10^{-3}$, gas metallicity: $Z_{\rm g} = 5 \times 10^{-3}~Z_{\odot}$, star formation efficiency: $η= 0.01$), model far-infrared (FIR) fluxes are consistent with current upper flux limits inferred from ALMA bands 6 and 7 ($\lesssim 10^4$ nJy). Such low $D/M$ values and metallicities are in agreement with some scenarios proposed in the literature to explain the non-detection of the FIR dust continuum for high-$z$ JWST galaxy candidates. On the other hand, higher values of model parameters $D/M$ ($\gtrsim 0.06$) and $Z_{\rm g}$ ($\gtrsim 5 \times 10^{-2}~Z_{\odot}$) are ruled out by observational data, unless a higher $η$ is assumed. According to our findings, ALMA multi-band observations could constrain the dust chemistry and dust grain size distribution in the early universe. In this context, future observational challenges would involve not only reaching higher FIR sensitivities, but also increasing the wavelength coverage by exploring distinct ALMA bands.

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arXiv2020

Metal-THINGS: On the metallicity and ionization of ULX sources in NGC 925

We present an analysis of the optical properties of three Ultra Luminous X-ray (ULX) sources identified in NGC 925. We use Integral field unit data from the George Mitchel spectrograph in the context of the Metal-THINGS survey. The optical properties for ULX-1 and ULX-3 are presented, while the spaxel associated with ULX-2 had a low S/N, which prevented its analysis. We also report the kinematics and dimensions of the optical nebula associated with each ULX using ancillary data from the PUMA Fabry-Perot spectrograph. A BPT analysis demonstrates that most spaxels in NGC 925 are dominated by star-forming regions, including those associated with ULX-1 and ULX-3. Using the resolved gas-phase metallicities, a negative metallicity gradient is found, consistent with previous results for spiral galaxies, while the ionization parameter tends to increase radially throughout the galaxy. Interestingly, ULX-1 shows a very low gas metallicity for its galactocentric distance, identified by two independent methods, while exhibiting a typical ionization. We find that such low gas metallicity is best explained in the context of the high-mass X-ray binary population, where the low-metallicity environment favours active Roche lobe overflows that can drive much higher accretion rates. An alternative scenario invoking accretion of a low-mass galaxy is not supported by the data in this region. Finally, ULX-3 shows both a high metallicity and ionization parameter, which is consistent with the progenitor being a highly-accreting neutron star within an evolved stellar population region.

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arXiv2020

Redshift Horizon for the Origins Space Telescope from Primordial Dust Emission

We explore the possibility of detecting the first galaxies with the next generation Origins Space Telescope (OST) by applying an analytical model of primordial dust emission. By analysing source densities as a function of redshift (z), and considering deep-field exposures with the Origins Survey Spectrometer, we estimate that the redshift horizon for detecting one individual source would be above z~7 for systems with dust-to-metal ratios higher than those expected for typical primeval galaxies. On the other hand, if confusion limits could be overcome, the Far-infrared Imager and Polarimeter would enable the detection of more typical fainter systems at z>7. Given the dependence of the obtained results with the properties of primeval dust, we conclude that the OST could provide important clues to the nature of the interestellar medium in the early Universe.

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arXiv2020

Dust emission from the first massive galaxies

We compare observed far-infrared (FIR) galaxy spectral energy distributions (SEDs) at $z\sim6$ and theoretical predictions for first massive population II (Pop II) galaxies. Observed FIR SEDs at $z\gtrsim5$ are broad and shifted to bluer wavelengths when compared to galaxies at $z\sim3$. By implementing an analytical model for dust emission from Pop II massive galaxies,we were able to reproduce the observed behaviour as a consequence of the high energy densities and silicate-rich dust composition of high-$z$ model galaxies. As noted in a previous work, the non-blackbody nature of galaxy SEDs at $z \sim 6$ should be taken into account when interpreting measurements of FIR luminosities to avoid underestimating star formation rates.

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arXiv2020

Signatures of first galaxies at FIR/sub-mm wavelengths

We explore the possibility of detecting first galaxies with a generic far-infrared/sub-millimeter telescope by applying an analytical model of primordial dust emission. As shown in previous works, galaxies at redshifts $z>7$ experience a strong negative K-correction in such a way that systems of similar masses are brighter at higher $z$. In addition, at a given mass and $z$, our model predicts that luminosity fluxes increase proportionally to the dust-to-metal ratios ($D/M$) of primeval sources. We evaluate the observability of model sources at different $z>7$ as a function of the observed survey area ($ΔΩ$) and sensitivity ($S$) of a generic instrument. Assuming $ΔΩ\sim 10~{\rm deg}^2$ and a plausible $S \sim 1~μ{\rm Jy}$ for a near future survey, we could assure the detection of at least one typical source with $D/M \sim 5\times10^{-3}$ at $z>7$. For $S\gtrsim 1~μ{\rm Jy}$ and $ΔΩ\lesssim 10~{\rm deg}^2$, higher than typical $D/M$ are required to detect at least one individual source at $z>7$. The observability of model galaxies is also affected by the size distribution of dust grains, specially towards higher $z$.

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arXiv2019

Oxygen yields as a constraint on feedback processes in galaxies

We study the interplay between several properties determined from Optical and a combination of Optical/Radio measurements, such as the effective Oxygen yield (y_eff), the star formation efficiency, gas metallicity, depletion time, gas fraction, and baryonic mass(M_bar), among others. We use spectroscopic data from the SDSS survey, and HI information from the ALFALFA survey to build a statistically significant sample of more than 5,000 galaxies. Furthermore, we complement our analysis with data from the GASS and COLD GASS surveys, and with a sample of star-forming galaxies from the Virgo cluster. Additionally, we have compared our results with predictions from the EAGLE simulations, finding a very good agreement when using the high-resolution run. We explore in detail the M_bar-y_eff relation, finding a bimodal trend that can be separated when the stellar age of galaxies is considered. On one hand, y_eff increases with M_bar for young galaxies(log(t_r) < 9.2 yr), while y_eff shows an anti-correlation with M_bar for older galaxies (log(t_r) > 9.4 yr). While a correlation between M_bar and y_eff has been observed and studied before, mainly for samples of dwarfs and irregular galaxies, their anti-correlated counterpart for massive galaxies has not been previously reported. The EAGLE simulations indicate that AGN feedback must have played an important role in their history by quenching their star formation rate, whereas low mass galaxies would have been affected by a combination of outflows and infall of gas.

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arXiv2019

Redshift Horizon for Detecting the First Galaxies in Far-Infared Surveys

We explore the possibility of detecting the first galaxies with the next generation of space-based far infrared (FIR) telescopes by applying an analytical model of primordial dust emission. Our results indicate that FIR/sub-mm sources at $z \gtrsim 7$ will experience a strong negative K-correction. Systems of a given virial mass would exhibit larger dust luminosities at higher $z$, as a consequence of the increase in dust temperature driven by the higher temperature floor set by the cosmic microwave background. In addition, high-$z$ systems are more concentrated, which enhances the heating efficiency associated with stellar radiation. By analysing source densities as a function of $z$, and considering survey areas of 0.1 ${\rm deg}^2$ and 10 ${\rm deg}^2$, we find that the redshift horizon for detecting at least one source would be above $z\sim 7$ for instrument sensitivities $\lesssim 0.1-0.5 \ μ{\rm Jy}$ and $\lesssim 0.5-3.0 \ μ{\rm Jy}$, respectively, with the exact values depending on the nature of primordial dust. However, galaxy populations with higher than typical metallicities, star formation efficiencies and/or dust-to-metal ratios could relax such sensitivity requirements. In addition, the redshift horizon shows a significant dependence on the nature of primordial dust. We conclude that future FIR campaigns could play a crucial role in exploring the nature of dust and star formation in the early universe.

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arXiv2018

The Far Infrared Emission of the First Massive Galaxies

Massive Population II galaxies undergoing the first phase of vigorous star formation after the initial Population III stage should have high energy densities and silicate-rich interstellar dust. We have modeled the resulting far-infrared spectral energy distributions (SEDs), demonstrating that they are shifted substantially to bluer (`warmer') wavelengths relative to the best fitting ones at z ~ 3, and with strong outputs in the 10 - 40 micron range. When combined with a low level of emission by carbon dust, their SEDs match that of Haro 11, a local moderately-low-metallicity galaxy undergoing a very young and vigorous starburst that is likely to approximate the relevant conditions in young Population II galaxies. We expect to see similar SEDs at high redshifts (z >= 5) given the youth of galaxies at this epoch. In fact, we find a progression with redshift in observed galaxy SEDs, from those resembling local ones at 2 < z < 4 to a closer resemblance with Haro 11 at 5 < z < 7. In addition to the insight on conditions in high redshift galaxies, this result implies that estimates of the total infrared luminosities at z ~ 6 based on measurements near lambda ~ 1 mm can vary by factors of 2 - 4, depending on the SED template used. Currently popular modified blackbodies or local templates can result in significant underestimates compared with the preferred template based on the SED of Haro 11.

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arXiv2016

Contribution of the first galaxies to the cosmic far-infrared/sub-millimeter background - I. Mean background level

We study the contribution of the first galaxies to the far-infrared/sub-millimeter (FIR/sub-mm) extragalactic background light (EBL) by implementing an analytical model for dust emission. We explore different dust models, assuming different grain size distributions and chemical compositions. According to our findings, observed re-radiated emission from dust in dwarf-size galaxies at $z \sim 10$ would peak at a wavelength of $\sim 500 μ{\rm m}$ with observed fluxes of $\sim 10^{-3} - 10^{-2}$ nJy, which is below the capabilities of current observatories. In order to be detectable, model sources at these high redshifts should exhibit luminosities of $\gtrsim 10^{12} L_{\odot}$, comparable to that of local ultra-luminous systems. The FIR/sub-mm EBL generated by primeval galaxies peaks at $\sim 500 μ{\rm m}$, with an intensity ranging from $\sim 10^{-4}$ to $10^{-3} {\rm nW \ m^{-2} \ sr^{-1}}$, depending on dust properties. These values are $\sim 3 - 4$ orders of magnitude below the absolute measured cosmic background level, suggesting that the first galaxies would not contribute significantly to the observed FIR/sub-mm EBL. Our model EBL exhibits a strong correlation with the dust-to-metal ratio, where we assume a fiducial value of $D = 0.005$, increasing almost proportionally to it. Thus, measurements of the FIR/sub-mm EBL could provide constraints on the amount of dust in the early Universe. Even if the absolute signal from primeval dust emission may be undetectable, it might still be possible to obtain information about it by exploring angular fluctuations at $\sim 500 μ{\rm m}$, close to the peak of dust emission from the first galaxies.

astro-ph.CO↗

arXiv2006

Study of the Origin of the Luminosity-Metallicity and the Stellar Mass-Metallicity Relations in Hierarchical Universes

In this work, we study the Luminosity-Metallicity relation (LMR) and the Stellar Mass -Metallicity relation (MMR) of galactic systems in a hierarhical clustering scenario. We performed numerical hydrodynamical simulations with the chemical GADGET-2 of Scannapieco et al.(2005) in a LCDM universe. We found that our simulated galactic systems reproduce the observed local LMR and its evolution in zero point and slope. The simulated MMR is also in agreement with recent observational results. From the analysis of the evolution of the MMR, we found a characteristic mass at ~10^(10.2) M_sun / h which separates two galactic populations with different astrophysical properties. More massive systems tend to have their stars formed at z > 2 and show less evolution than smaller systems. Hence, this characteristic mass is determined by the formation of the structure in a hierarchical scenario. Our results also suggest the need for important supernova feedback.

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arXiv2006

Analysis of the Luminosity-Stellar Mass-Metallicity Relation in cosmological simulations

We study the Luminosity-Metallicity Relation and the Stellar Mass-Metallicity Relation by performing chemo-dynamical simulations in a cosmological scenario. Our results predict a tight linear correlation between oxygen chemical abundance and luminosity for galactic systems up to z=3. The Luminosity-Metallicity Relation evolves with redshift in such a way that systems at a given oxygen abundance were ~3 dex brighter at z=3 compared to local ones, in good agreement with observations. We determin also a characteristic stellar mass M_c~10^(10.2) M_sun/h above which the Stellar Mass-Metallicity Relation starts to flatten. We encounter that this mass arises as a consequence of the hierarchical aggregation of structure in a LCDM universe and segregates two galactic populations with different astophysical properties.

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arXiv2006

Evolution of the Luminosity-Metallicity-Stellar Mass correlation in a hierarchical scenario

We study the evolution of the Stellar Mass-Metallicity Relation and the Luminosity-Metallicity Relation by performing numerical simulations in a cosmological framework. We find that the slope and the zero point of the Luminosity-Metallicity Relation evolve in such a way that, at a given metallicity, systems were ~3 mag brighter at z=3 compared to galaxies in the local universe, which is consistent with the observational trend. The local Stellar Mass-Metallicity Relation shows also a good agreement with recent observations. We identify a characteristic stellar mass M_c ~ 10^(10.2) M_sun/h at which the slope of the Stellar Mass-Metallicity Relation decreases for larger stellar masses. Our results indicate that M_c arises naturally as a consequence of the hierarchical building up of the structure.

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