SFR estimations from <i>z</i> = 0 to <i>z</i> = 0.9

Figueira, M.; Pollo, A.; Małek, K.; Buat, V.; Boquien, M.; Pistis, F.; Cassarà, L. P.; Vergani, D.; Hamed, M.; Salim, Samir

doi:10.1051/0004-6361/202141701

Cited by 9 publications

(4 citation statements)

References 187 publications

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“…For this new catalog of spectroscopic measurements, we adopted the same flag system used in the VIPERS catalogs (Garilli et al 2010;Figueira et al 2022;Pistis et al 2022) in the form of a four-digit number, xyzt. The x-value is equal to 1 if the difference between the centroid of the fit and the centroid of the observed data is less than or equal to 7 Å (equivalent to 1 pixel on the VIMOS spectrograph); otherwise, its value is 0.…”

Section: Vipers Samplementioning

confidence: 99%

A comparative study of the fundamental metallicity relation

Pistis,

Pollo,

Figueira

et al. 2024

A&A

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We aim to investigate the influences on the evolution of the fundamental metallicity relation of different selection criteria. We used $5\,487$ star-forming galaxies at a median redshift of $z 0.63$ extracted from the VIMOS Public Extragalactic Redshift Survey (VIPERS) and $143\,774$ comparison galaxies in the local Universe from the GALEX-SDSS-WISE Legacy Catalog. We employed two families of methods: parametric and nonparametric. In the parametric approaches, we compared the fundamental metallicity relation projections plagued by observational biases on differently constructed control samples at various redshifts. Then, we compare the metallicity difference between different redshifts in stellar mass-star formation rate bins. In the nonparametric approach, we related the metallicity and the normalized specific star formation rate (sSFR). To compare galaxies with the same physical properties, we normalized the sSFR of our samples according to the median value at median redshift $z 0.09$. Then, the galaxies with the same distance from the star-forming main sequence at their respective redshifts were compared when the sSFR is normalized according to the expected values from their respective star-forming main sequences. The methodologies implemented to construct fair, complete samples for studying the mass-metallicity relation and the fundamental metallicity relation produced consistent results showing a small but still statistically significant evolution of both relations up to $z 0.63$. In particular, we observed a systematic trend where the median metallicity of the sample at $z=0.63$ is lower than that of the local sample at the same stellar mass and star formation rate. The average difference in the metallicity of the low and intermediate redshifts is approximately $1.8$ times the metallicity standard deviation of the median of the intermediate redshift sample in stellar mass-star formation rate bins. We confirmed this result using the Kolmogorov-Smirnov test. When we applied the stellar mass-completeness criterion to catalogs, the metallicity difference in redshifts decreased to approximately $0.96$ times the metallicity standard deviation of the median, and thus it was not statistically significant. The limited area of the FMR surface explored once the stellar mass-completeness criterion is applied might dominate this difference reduction, leaving out the area where the difference between the two samples is the highest. A careful reading of the results and their underlying selection criteria is crucial in studies of the mass-metallicity and fundamental metallicity relations. When studying the mass-metallicity and fundamental metallicity relations, we recommend using the nonparametric approach, which provides similar results compared to parametric prescriptions, is easier to use, and is clear to interpret. The nonparametric methodology provides a convenient way to compare physical properties, with a smaller impact on observational selection biases.

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Section: Vipers Samplementioning

confidence: 99%

A comparative study of the fundamental metallicity relation

Pistis,

Pollo,

Figueira

et al. 2024

A&A

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“…This tool is based on the principle of the energy balance between dust-absorbed stellar emission in the ultraviolet and optical bands and its re-emission in the infrared. CIGALE has been thoroughly tested on VIPERS photometry to estimate the physical properties of star-forming galaxies (Figueira et al 2022 ;Pistis et al 2022 ), galaxies hosting active galactic nuclei (Vietri et al 2022 ;Mezcua et al 2023 ;Siudek et al 2023 ), passive galaxies ( L22 ), or the whole population (Turner et al 2021 ). In this work, following the methodology introduced in L22 , we used a delayed SFH model and Bruzual & Charlot ( 2003 ) single stellar population models assuming a Chabrier ( 2003 ) initial mass function and solar metallicity to build a grid of models.…”

Section: Physical Propertiesmentioning

confidence: 99%

Environments of red nuggets at z ∼ 0.7 from the VIPERS survey

Siudek

Lisiecki

Krywult

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Red ultra-compact massive galaxies, called red nuggets were formed at high redshifts (z ∼ 2 − 3). Survivors of red nuggets, known as relics, observed at lower redshifts (z < 2) are believed to remain almost unchanged since their formation. For the first time, we verify the environmental properties of red nuggets at intermediate redshift (0.5 < z < 0.9 ) using 42 red, massive (log(Mstar/M⊙) ≥ 10.9) and ultra-compact (Re < 1.5 kpc) from the VIMOS Public Extragalactic Redshift Survey (VIPERS). We found that the increasing fraction of red galaxies, when moving to denser environments, is driven by the red massive normal-size galaxies. Red nuggets, similarly to red intermediate-mass (10.4 ≲ log (Mstar/M⊙) < 10.9) ultra-compact galaxies, are found in various types of environments, with consistent (within 1σ) fractions across all local densities. Analysis of red nugget stellar ages suggests that relics are preferably found in high-density regions while quiescent red nuggets are overabundant in low-density environments. We speculate that red nuggets have survived to lower redshifts via two channels: i) in low-density environments where the fraction of red nuggets decreases as time passes due to (very) limited merger activity, ii) in high-density environments, where the number of red nuggets drops at higher redshift due to merger activity and is preserved at lower redshift as the high velocities of clusters prevent them from being cannibalised. Even more, the fraction of red nuggets in clusters may increase due to the addition of red massive normal-size galaxies deprived of their envelopes with cosmic time.

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“…3, we cannot tell if this correlation is physical. Galaxies that are preferring CF00 double-component attenuation law and its shallower version LF17, by construction, result in a significantly higher older stellar population, therefore increasing the stellar mass (e.g., Małek et al 2018;Buat et al 2019;Hamed et al 2021;Figueira et al 2022). We also checked the preference of attenuation laws used with SFR for our galaxies.…”

Section: Galaxy Properties and Dust Attenuationmentioning

confidence: 99%

The slippery slope of dust attenuation curves

M.¹,

Małek²,

V.³

et al. 2023

A&A

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Aims. We investigate dust attenuation of 122 heavily dust-obscured galaxies detected with the Atacama Large Millimeter Array (ALMA) and Herschel in the COSMOS field. We search for correlations between dust attenuation recipes and the variation of physical parameters, mainly the effective radii of galaxies, their star formation rates, and stellar masses, and aim to understand which of the commonly used laws best describes dust attenuation in dusty star-forming galaxies (DSFGs) at high redshift. Methods. We make use of the extensive photometric coverage of the COSMOS data combined with highly-resolved dust continuum maps from ALMA. We use CIGALE to estimate various physical properties of these dusty objects, mainly their star formation rates (SFR), their stellar masses and their attenuation in the short wavelengths. We infer galaxy effective radii (Re) using GALFIT in the Y band of HSC and ALMA continuum maps. We use these radii to investigate the relative compactness of the dust continuum and the extension of the rest-frame UV/optical Re(y)/Re(ALMA). Results. We find that the physical parameters calculated from our models strongly depend on the assumption of dust attenuation curve. As expected, the most impacted parameter is the stellar mass, which leads to a change in the "starburstiness" of the objects. We find that taking into account the relative compactness of star-to-dust emission prior to SED fitting is crucial, especially when studying dust attenuation of dusty star-forming galaxies. Shallower attenuation curves did not show a clear preference of compactness with attenuation, while the Calzetti attenuation curve preferred comparable spatial extent of unattenuated stellar light and dust emission. The evolution of the R e (UV)/R e (ALMA) ratio with redshift peeks around the cosmic noon in our sample of DSFGs, showing that this compactness is correlated with the cosmic SFR density of these dusty sources.

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SFR estimations from z = 0 to z = 0.9

Cited by 9 publications

References 187 publications

A comparative study of the fundamental metallicity relation

A comparative study of the fundamental metallicity relation

Environments of red nuggets at z ∼ 0.7 from the VIPERS survey

The slippery slope of dust attenuation curves

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