25 research outputs found
JWST CEERS probes the role of stellar mass and morphology in obscuring galaxies
A population of massive galaxies invisible or very faint in deep
optical/near-infrared surveys, but brighter at longer wavelengths has been
uncovered in the past years. However, the nature of these optically dark/faint
galaxies (OFGs, among other nomenclatures) is highly uncertain. In this work,
we investigate the drivers of dust attenuation in the JWST era. Particularly,
we study the role of stellar mass, size, and orientation in obscuring
star-forming galaxies (SFGs) at , focusing on understanding why
galaxies like OFGs are so faint at optical/near-infrared wavelengths. We find
that stellar mass is the primary proxy of dust attenuation among those studied.
Effective radius and axis ratio do not show a clear link with dust attenuation,
with the effect of orientation close to random. However, there is a subset of
highly dust attenuated (, typically) SFGs, of which OFGs are a
specific case. For this subset, we find that the key distinctive feature is
their compact size (for massive systems with ),
exhibiting 30% smaller effective radius than the average SFGs at the same
stellar mass and redshift. On the contrary, they do not exhibit a preference
for low axis ratios (i.e., edge-on disks). The results in this work show
stellar mass as a primary proxy of dust attenuation and compact stellar light
profiles behind thick dust columns obscuring typical massive SFGs.Comment: Submitted to A&A. 13 pages, 9 figure
Unveiling the distant Universe: Characterizing Galaxies in the first epoch of COSMOS-Web
We report the identification of 15 galaxy candidates at using the
initial COSMOS-Web JWST observations over 77 arcmin through four NIRCam
filters (F115W, F150W, F277W, F444W) with an overlap with MIRI (F770W) of 8.7
arcmin. We fit the sample using several publicly-available SED fitting and
photometric redshift codes and determine their redshifts between and
(), UV-magnitudes between M =
21.2 and 19.5 (with M) and rest-frame
UV slopes (). These galaxies are, on average, more
luminous than most candidates discovered by JWST so far in the
literature, while exhibiting similar blue colors in their rest-frame UV. The
rest-frame UV slopes derived from SED-fitting are blue ([2.0,
2.7]) without reaching extremely blue values as reported in other recent
studies at these redshifts. The blue color is consistent with models that
suggest the underlying stellar population is not yet fully enriched in metals
like similarly luminous galaxies in the lower redshift Universe. The derived
stellar masses with MM are not in tension with the standard
CDM model and our measurement of the volume density of such UV
luminous galaxies aligns well with previously measured values presented in the
literature at . Our sample of galaxies, although compact, are
significantly resolved.Comment: Submitted to Ap
PATIENTS WITH DOWN’S SYNDROME (DS) ARE INSULIN RESISTANT INDEPENDENTLY OF BODY MASS INDEX (BMI)
FEMALE PATIENTS WITH DOWN SYNDROME (DS) SHOW A GREATER INSULIN RESISTANCE IN COMPARISON WITH NORMAL FEMALES (NF)
Marco para desarrollar nuevas unidades de proyectos e incorporar docentes y alumnos en actividades de investigación
El presente proyecto, que es la continuación de una primera experiencia realizada desde el 2020 al 2022, propone la formación de investigadores como objetivo primordial y a la vez define un marco globalizador que permita la coexistencia de diversas unidades de proyectos que de otra manera no tendrían la posibilidad de llegar a la instancia de conformar un proyecto independiente.
Dicho Marco constituirá un espacio de promoción de ideas e iniciativas para la iniciación en la investigación, tanto para estudiantes de grado como para docentes.
Ofrece la posibilidad de realizar prácticas de investigación específicas como un primer peldaño que permita acceder a distintos elementos (categorización, recursos económicos, acompañamiento de los directores del proyecto y miembros con más experiencia, posibilidad de obtención de becas y, fundamentalmente, un contexto que guíe y enmarque la experiencia para favorecer su concreción). Es importante remarcar que normalmente no todo docente (menos aún los estudiantes) logra involucrarse y participar formalmente dentro de un proyecto de investigación dado que los requisitos para la conformación de grupos, la solicitud de financiamiento, y/o su incorporación a actividades de investigación suelen convertirse en un obstáculo. Por ende, permitir la incorporación de los mismos, guiar su trayecto formativo y posibilitar los medios económicos mínimos para desarrollar y dar a conocer sus propuestas, es el objetivo final del presente proyecto.Red de Universidades con Carreras en Informátic
JWST CEERS probes the role of stellar mass and morphology in obscuring galaxies
In recent years, observations have uncovered a population of massive galaxies that are invisible or very faint in deep optical/near-infrared (near-IR) surveys but brighter at longer wavelengths. However, the nature of these optically dark or faint galaxies (OFGs; one of several names given to these objects) is highly uncertain. In this work, we investigate the drivers of dust attenuation in the JWST era. In particular, we study the role of stellar mass, size, and orientation in obscuring star-forming galaxies (SFGs) at 3'., <'., z'., <'., 7.5, focusing on the question of why OFGs and similar galaxies are so faint at optical/near-IR wavelengths. We find that stellar mass is the primary proxy for dust attenuation, among the properties studied. Effective radius and axis ratio do not show a clear link with dust attenuation, with the effect of orientation being close to random. However, there is a subset of highly dust attenuated (AV'., >'., 1, typically) SFGs, of which OFGs are a specific case. For this subset, we find that the key distinctive feature is their compact size (for massive systems with log(M∗/M™ ) > 10); OFGs exhibit a 30% smaller effective radius than the average SFG at the same stellar mass and redshift. On the contrary, OFGs do not exhibit a preference for low axis ratios (i.e., edge-on disks). The results in this work show that stellar mass is the primary proxy for dust attenuation and compact stellar light profiles behind the thick dust columns obscuring typical massive SFGs.</p
Sirius watch 2018:role of non-formal education in migrant children inclusion : links with schools : synthesis report
JWST CEERS probes the role of stellar mass and morphology in obscuring galaxies
International audienceA population of massive galaxies invisible or very faint in deep optical/near-infrared surveys, but brighter at longer wavelengths has been uncovered in the past years. However, the nature of these optically dark/faint galaxies (OFGs, among other nomenclatures) is highly uncertain. In this work, we investigate the drivers of dust attenuation in the JWST era. Particularly, we study the role of stellar mass, size, and orientation in obscuring star-forming galaxies (SFGs) at , typically) SFGs, of which OFGs are a specific case. For this subset, we find that the key distinctive feature is their compact size (for massive systems with ), exhibiting 30% smaller effective radius than the average SFGs at the same stellar mass and redshift. On the contrary, they do not exhibit a preference for low axis ratios (i.e., edge-on disks). The results in this work show stellar mass as a primary proxy of dust attenuation and compact stellar light profiles behind thick dust columns obscuring typical massive SFGs