Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>We investigate the star-forming main sequence of the host galaxies of a large, well-defined sample of 453 redshift ∼0.3 quasars with previously available star formation rates by deriving stellar masses from modeling their broadband (<jats:italic>grizy</jats:italic>) spectral energy distribution. We perform two-dimensional, simultaneous, multi-filter decomposition of Pan-STARRS1 3<jats:italic>π</jats:italic> Steradian Survey images to disentangle the active galactic nucleus (AGN) from its host galaxy, by explicitly considering, for the first time, the wavelength variation of galaxy structures. We quantify the Sérsic profiles and sizes of the host galaxies from mock AGNs generated from both real and idealized galaxies. Detailed morphological classifications of the calibration galaxy sample using Hubble Space Telescope images enable us to estimate crude morphological types of the quasars. Although the majority (∼60%) of the quasars are hosted by bulge-dominated, early-type galaxies, a substantial fraction (∼40%) reside in disk-dominated, late-type galaxies, suggesting that at least in these systems major mergers have not played a significant role in regulating their AGN activity, in agreement with recent simulations and observations of nearby quasars. The vast majority (∼90%) of the quasars have star formation rates that place them on or above the galaxy star-forming main sequence, with more rapidly accreting AGNs displaced further above the main sequence. Quasar host galaxies generally follow the stellar mass–size relation defined by inactive galaxies, both for late-type and early-type systems, but roughly 1/3 of the population has smaller sizes at a given stellar mass, reminiscent of compact star-forming galaxies at higher redshift.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present theoretical expectations for infall toward supercluster-scale cosmological filaments, motivated by the Arecibo Pisces–Perseus Supercluster Survey (APPSS) to map the velocity field around the Pisces–Perseus Supercluster (PPS) filament. We use a minimum spanning tree applied to dark matter halos the size of galaxy clusters to identify 236 large filaments within the Millennium simulation. Stacking the filaments along their principal axes, we determine a well-defined, sharp-peaked velocity profile function that can be expressed in terms of the maximum infall rate <jats:italic>V</jats:italic> <jats:sub>max</jats:sub> and the distance <jats:italic>ρ</jats:italic> <jats:sub>max</jats:sub> between the location of maximum infall and the principal axis of the filament. This simple, two-parameter functional form is surprisingly universal across a wide range of linear mass densities. <jats:italic>V</jats:italic> <jats:sub>max</jats:sub> is positively correlated with the halo mass per length along the filament, and <jats:italic>ρ</jats:italic> <jats:sub>max</jats:sub> is negatively correlated with the degree to which the halos are concentrated along the principal axis. We also assess an alternative, single-parameter method using <jats:italic>V</jats:italic> <jats:sub>25</jats:sub>, the infall rate at a distance of 25 Mpc from the axis of the filament. Filaments similar to the PPS have <jats:inline-formula> <jats:tex-math> <?CDATA ${V}_{\max }=612\ \pm $?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>V</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>max</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>612</mml:mn> <mml:mspace width="0.33em" /> <mml:mo>±</mml:mo> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac815bieqn1.gif" xlink:type="simple" /> </jats:inline-formula> 116 km s<jats:sup>−1</jats:sup>, <jats:inline-formula> <jats:tex-math> <?CDATA ${\rho }_{\max }=8.9\pm 2.1$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>ρ</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>max</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>8.9</mml:mn> <mml:mo>±</mml:mo> <mml:mn>2.1</mml:mn> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac815bieqn2.gif" xlink:type="simple" /> </jats:inline-formula> Mpc, and <jats:italic>V</jats:italic> <jats:sub>25</jats:sub> = 329 ± 68 km s<jats:sup>−1</jats:sup>. We create mock observations to model uncertainties associated with viewing angle, lack of three-dimensional velocity information, limited sample size, and distance uncertainties. Our results suggest that it would be especially useful to measure infall for a larger sample of filaments to test our predictions for the shape of the infall profile and the relationships among infall rates and filament properties.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present spatially resolved observations of Betelgeuse (<jats:italic>α</jats:italic> Orionis) obtained with the Karl G. Jansky Very Large Array at <jats:italic>λ</jats:italic> ∼ 7 mm (44 GHz) and <jats:italic>λ</jats:italic> ∼ 1.3 cm (22 GHz) on 2019 August 2, just prior to the onset of the historical optical dimming that occurred between late 2019 and early 2020. Our measurements suggest recent changes in the temperature and density structure of the atmosphere between radii <jats:italic>r</jats:italic> ∼ 2<jats:italic>R</jats:italic>⋆ and 3<jats:italic>R</jats:italic>⋆. At <jats:italic>λ</jats:italic>7 mm the star is ∼20% dimmer than in previously published observing epochs between 1996 and 2004. We measure a mean gas temperature of <jats:italic>T</jats:italic> <jats:sub> <jats:italic>B</jats:italic> </jats:sub> = 2270 ± 260 K at <jats:italic>r</jats:italic> ∼ 2.1<jats:italic>R</jats:italic>⋆, where <jats:italic>R</jats:italic> <jats:sub>⋆</jats:sub> is the canonical photospheric radius. This is ∼2<jats:italic>σ</jats:italic> lower than previously reported temperatures at comparable radii and &gt;1200 K lower than predicted by previous semiempirical models of the atmosphere. The measured brightness temperature at <jats:italic>r</jats:italic> ∼ 2.6<jats:italic>R</jats:italic> <jats:sub>⋆</jats:sub> (<jats:italic>T</jats:italic> <jats:sub> <jats:italic>B</jats:italic> </jats:sub> = 2580 ± 260 K) is also cooler than expected based on trends in past measurements. The stellar brightness profile in our current measurements appears relatively smooth and symmetric, with no obvious signatures of giant convective cells or other surface features. However, the azimuthally averaged brightness profile is found to be more complex than a uniform elliptical disk. Our observations were obtained approximately 6 weeks before spectroscopic measurements in the ultraviolet revealed evidence of increases in the chromospheric electron density in the southern hemisphere of Betelgeuse, coupled with a large-scale outflow. We discuss possible scenarios linking these events with the observed radio properties of the star, including the passage of a strong shock wave.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We study the long-term evolution of the global structure of axisymmetric accretion flows onto a black hole (BH) at rates substantially higher than the Eddington value (<jats:inline-formula> <jats:tex-math> <?CDATA ${\dot{M}}_{\mathrm{Edd}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> </mml:mrow> <mml:mrow> <mml:mi>Edd</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac75d8ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>), performing 2D hydrodynamical simulations with and without radiative diffusion. In the high-accretion optically thick limit, where the radiation energy is efficiently trapped within the inflow, the accretion flow becomes adiabatic and comprises turbulent gas in the equatorial region and strong bipolar outflows. As a result, the mass inflow rate decreases toward the center as <jats:inline-formula> <jats:tex-math> <?CDATA ${\dot{M}}_{\mathrm{in}}\propto {r}^{p}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> </mml:mrow> <mml:mrow> <mml:mi>in</mml:mi> </mml:mrow> </mml:msub> <mml:mo>∝</mml:mo> <mml:msup> <mml:mrow> <mml:mi>r</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>p</mml:mi> </mml:mrow> </mml:msup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac75d8ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> with <jats:italic>p</jats:italic> ∼ 0.5–0.7 and a small fraction of the inflowing gas feeds the nuclear BH. Thus, super-Eddington accretion is sustained only when a larger amount of gas is supplied from larger radii at ≳100–1000 <jats:inline-formula> <jats:tex-math> <?CDATA $\,{\dot{M}}_{\mathrm{Edd}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mspace width="0.50em" /> <mml:msub> <mml:mrow> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> </mml:mrow> <mml:mrow> <mml:mi>Edd</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac75d8ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>. The global structure of the flow settles down to a quasi-steady state in millions of the orbital timescale at the BH event horizon, which is ≳10–100 times longer than that addressed in previous (magneto-)RHD simulation studies. Energy transport via radiative diffusion accelerates the outflow near the poles in the inner region but does not change the overall properties of the accretion flow compared to the cases without diffusion. Based on our simulation results, we provide a mechanical feedback model for super-Eddington accreting BHs. This can be applied as a subgrid model in large-scale cosmological simulations that do not sufficiently resolve galactic nuclei, and to the formation of the heaviest gravitational-wave sources via accretion in dense environments.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present the Ly<jats:italic>α</jats:italic> emission line luminosity function (LF) of the active galactic nuclei (AGN) in the first release of the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) AGN catalog. The AGN are selected either by emission line pairs characteristic of AGN or by a single broad emission line, free of any photometric preselections (magnitude/color/morphology). The sample consists of 2346 AGN spanning 1.88 &lt; <jats:italic>z</jats:italic> &lt; 3.53, covering an effective area of 30.61 deg<jats:sup>2</jats:sup>. Approximately 2.6% of the HETDEX AGN are not detected at &gt;5<jats:italic>σ</jats:italic> confidence at <jats:italic>r</jats:italic> ∼ 26 in the deepest <jats:italic>r</jats:italic>-band images we have searched. The Ly<jats:italic>α</jats:italic> line luminosity ranges from ∼10<jats:sup>42.3</jats:sup> to 10<jats:sup>45.9</jats:sup> erg s<jats:sup>−1</jats:sup>. Our Ly<jats:italic>α</jats:italic> LF shows a turnover luminosity with opposite slopes on the bright end and the faint end: The space density is highest at <jats:inline-formula> <jats:tex-math> <?CDATA ${L}_{\text{Ly}{\text{\unicode{x003B1}}}}^{\ast }={10}^{43.4}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mi>L</mml:mi> <mml:mrow> <mml:mtext>Ly</mml:mtext> <mml:mtext mathvariant="italic">α</mml:mtext> </mml:mrow> <mml:mo>∗</mml:mo> </mml:msubsup> <mml:mo>=</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>43.4</mml:mn> </mml:msup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac8054ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> erg s<jats:sup>−1</jats:sup>. We explore the evolution of the AGN LF over a broader redshift range (0.8 &lt; <jats:italic>z</jats:italic> &lt; 3); constructing the rest-frame ultraviolet (UV) LF with the 1450 Å monochromatic luminosity of the power-law component of the continuum (M<jats:sub>1450</jats:sub>) from <jats:italic>M</jats:italic> <jats:sub>1450</jats:sub> ∼ −18 to −27.5. We divide the sample into three redshift bins (<jats:italic>z</jats:italic> ∼ 1.5, 2.1, and 2.6). In all three redshift bins, our UV LFs indicate that the space density of AGN is highest at the turnover luminosity <jats:inline-formula> <jats:tex-math> <?CDATA ${M}_{1450}^{* }$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>1450</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac8054ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> with opposite slopes on the bright end and the faint end. The <jats:italic>M</jats:italic> <jats:sub>1450</jats:sub> LFs in the three redshift bins can be well fit with a luminosity evolution and density evolution model: the turnover luminosity (<jats:inline-formula> <jats:tex-math> <?CDATA ${M}_{1450}^{* }$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>1450</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac8054ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>) increases, and the turnover density (Φ*) decreases with increasing redshift.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We demonstrate that changes in the incident radiation in Mg <jats:sc>ii</jats:sc> h and k lines have a significant impact on the results of radiative transfer modeling of prominence-like plasmas. To uncover the extent of this impact and allow easy comparison, here we study two cases, one representing the minimum of the solar activity and the other corresponding to the typical conditions during solar maxima. To represent well the properties of the prominence plasma, we use the 2D non-LTE (i.e., departures from local thermodynamic equilibrium) model of prominence fine structures in both the single-thread configuration and the multithread configuration incorporating prominence dynamics. We show that in the modeled environment of prominence fine structures, the change in the central, integrated, and peak intensities of the synthetic Mg <jats:sc>ii</jats:sc> h and k profiles can be as large as the change in the incident radiation itself. This means that the Mg <jats:sc>ii</jats:sc> h and k spectra of observed prominences can be affected by tens of percent because the illumination from the solar disk can change by such a degree over the solar cycle. That makes the knowledge and use of event-specific incident radiation data very important for the diagnostics of prominences and other chromospheric and coronal structures when using Mg <jats:sc>ii</jats:sc> h and k spectral observations. In addition, the observed Mg <jats:sc>ii</jats:sc> h and k spectra are strongly influenced by the line-of-sight dynamics, as the multithread configuration of the 2D model allows us to reveal. The effect of dynamics is, unsurprisingly, most pronounced in the line widths and integrated intensities.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Chemical models and experiments indicate that interstellar dust grains and their ice mantles play an important role in the production of complex organic molecules (COMs). To date, the most complex solid-phase molecule detected with certainty in the interstellar medium is methanol, but the James Webb Space Telescope (JWST) may be able to identify still larger organic species. In this study, we use a coupled chemodynamical model to predict new candidate species for JWST detection toward the young star-forming core Cha-MMS1, combining the gas–grain chemical kinetic code <jats:italic>MAGICKAL</jats:italic> with a 1D radiative hydrodynamics simulation using <jats:italic>Athena++</jats:italic>. With this model, the relative abundances of the main ice constituents with respect to water toward the core center match well with typical observational values, providing a firm basis to explore the ice chemistry. Six oxygen-bearing COMs (ethanol, dimethyl ether, acetaldehyde, methyl formate, methoxy methanol, and acetic acid), as well as formic acid, show abundances as high as, or exceeding, 0.01% with respect to water ice. Based on the modeled ice composition, the infrared spectrum is synthesized to diagnose the detectability of the new ice species. The contribution of COMs to IR absorption bands is minor compared to the main ice constituents, and the identification of COM ice toward the core center of Cha-MMS1 with the JWST NIRCAM/Wide Field Slitless Spectroscopy (2.4–5.0 <jats:italic>μ</jats:italic>m) may be unlikely. However, MIRI observations (5–28 <jats:italic>μ</jats:italic>m) toward COM-rich environments where solid-phase COM abundances exceed 1% with respect to the column density of water ice might reveal the distinctive ice features of COMs.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present three epochs of early-time ultraviolet (UV) and optical HST/STIS spectroscopy of the young, nearby Type IIP supernova (SN) 2021yja. We complement the HST data with two earlier epochs of Swift UVOT spectroscopy. The HST and Swift UVOT spectra are consistent with those of other well-studied Type IIP SNe. The UV spectra exhibit rapid cooling at early times, while less dramatic changes are seen in the optical. We also present Lick/KAIT optical photometry up to the late-time tail phase, showing a very long plateau and shallow decline compared with other SNe IIP. Our modeling of the UV spectrum with the <jats:monospace>TARDIS</jats:monospace> radiative transfer code produces a good fit for a high-velocity explosion, a low total extinction <jats:italic>E</jats:italic>(<jats:italic>B</jats:italic> − <jats:italic>V</jats:italic>) = 0.07 mag, and a subsolar metallicity. We do not find a significant contribution to the UV flux from an additional heating source, such as interaction with the circumstellar medium, consistent with the observed flat plateau. Furthermore, the velocity width of the Mg <jats:sc>ii</jats:sc> <jats:italic>λ</jats:italic>2798 line is comparable to that of the hydrogen Balmer lines, suggesting that the UV emission is confined to a region close to the photosphere.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>This paper is intended to study the density and the refractive index of the solid carbon monoxide in the interval 13–28 K to improve our understanding of the dynamics in the astrophysical environments where they are present. A series of deposition experiments have been performed under high vacuum conditions to study the properties of this ice under astrophysical conditions. Ice density has been experimentally calculated at different deposition temperatures of astrophysical interest, which complement the scarce values present in the literature. The refractive index has also been experimentally determined. The data have been used to obtain an experimental relationship between refractive index and density. Values of density are necessary to interpret observations of astrophysical objects or to design irradiation experiments to understand how irradiation affects ices present in these objects. The experimental relationship found between density and refractive index allows us to estimate density from a known refractive index, even for temperatures not reached using our experimental setup.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Observations suggest that coronal loops should not be completely transparent. The transparency of coronal loops is rarely investigated in spite of its key role in coronal diagnostics. Here, we present an original investigation of Atmospheric Imaging Assembly 171 coronal loop transparency directly from the radiation of visually intersecting coronal loops, which strongly indicates that the coronal loops may have significant opaqueness on the 171 Å radiation, and therefore should not be optical thin structures at least for some coronal lines. We suggest that this result may not only be helpful for explaining some basic observational features of coronal loops, but also in bringing new clues to the radiation-based diagnostics.</jats:p>