Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>We present the <jats:sc>DustFilaments</jats:sc> code, a full-sky model for the millimeter Galactic emission of thermal dust. Our model, composed of millions of filaments that are imperfectly aligned with the magnetic field, is able to reproduce the main features of the dust angular power spectra at 353 GHz as measured by the Planck mission. Our model is made up of a population of filaments with sizes following a Pareto distribution <jats:inline-formula> <jats:tex-math> <?CDATA $\propto {L}_{a}^{-2.445}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∝</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>a</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2.445</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac54b2ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>, with an axis ratio between short and long semiaxes <jats:italic>ϵ</jats:italic> ∼ 0.16 and an angle of magnetic field misalignment with a dispersion rms(<jats:italic>θ</jats:italic> <jats:sub>LH</jats:sub>) = 10°. On large scales, our model follows a Planck-based template. On small scales, our model produces spectra that behave like power laws up to <jats:italic>ℓ</jats:italic> ∼ 4000 or smaller scales by considering even smaller filaments, limited only by computing power. We can produce any number of Monte Carlo realizations of small-scale Galactic dust. Our model will allow tests of how the small-scale non-Gaussianity affects CMB weak lensing and the consequences for the measurement of primordial gravitational waves or relativistic light relic species. Our model also can generate frequency decorrelation on the modified blackbody spectrum of dust and is freely adjustable to different levels of decorrelation. This can be used to test the performance of component separation methods and the impact of frequency spectrum residuals on primordial <jats:italic>B</jats:italic>-mode surveys. The filament density we paint in the sky is also able to reproduce the general level of non-Gaussianities measured by Minkowski functionals in the Planck 353 GHz channel map.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present an Atacama Large Millimeter/submillimeter Array (ALMA) survey of CO(4–3) line emitting galaxies in 17 quasar fields at <jats:italic>z</jats:italic> ∼ 4 aimed at performing the first systematic search of dusty galaxies in high-<jats:italic>z</jats:italic> quasar environments. Our blind search of galaxies around the quasars results in five CO emitters with S/N ≥ 5.6 within a projected radius of <jats:italic>R</jats:italic> ≲ 1.5 <jats:italic>h</jats:italic> <jats:sup>−1</jats:sup> cMpc and a velocity range of <jats:italic>δv</jats:italic> = ±1000 km s<jats:sup>−1</jats:sup> around the quasar. In blank fields, we expect to detect only 0.28 CO emitters within the same volume, implying a total overdensity of <jats:inline-formula> <jats:tex-math> <?CDATA ${17.6}_{-7.6}^{+11.9}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>17.6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>7.6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>11.9</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac469dieqn1.gif" xlink:type="simple" /> </jats:inline-formula> in our fields, and indicating that quasars trace massive structures in the early universe. We quantify this overdensity by measuring the small-scale clustering of CO emitters around quasars, resulting in a cross-correlation length of <jats:inline-formula> <jats:tex-math> <?CDATA ${r}_{0,\mathrm{QG}}={8.37}_{-2.04}^{+2.42}\,{h}^{-1}\,$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>r</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>0</mml:mn> <mml:mo>,</mml:mo> <mml:mi>QG</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>8.37</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2.04</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>2.42</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em" /> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em" /> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac469dieqn2.gif" xlink:type="simple" /> </jats:inline-formula> cMpc, assuming a fixed slope <jats:italic>γ</jats:italic> = 1.8. This contradicts the reported mild overdensities (x1.4) of Ly<jats:italic>α</jats:italic> emitters (LAEs) in the same fields at scales of <jats:italic>R</jats:italic> ≲ 7 <jats:italic>h</jats:italic> <jats:sup>−1</jats:sup> cMpc, which are well described by a cross-correlation length <jats:inline-formula> <jats:tex-math> <?CDATA ${3.0}_{-1.4}^{+1.5}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>3.0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.5</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac469dieqn3.gif" xlink:type="simple" /> </jats:inline-formula> times lower than that measured for CO emitters. We discuss some possibilities to explain this discrepancy, including low star formation efficiency, and excess of dust in galaxies around quasars. Finally, we constrain, for the first time, the clustering of CO emitters at <jats:italic>z</jats:italic> ∼ 4, finding an autocorrelation length of <jats:italic>r</jats:italic> <jats:sub>0,CO</jats:sub> = 3.14 ±1.71 <jats:italic>h</jats:italic> <jats:sup>−1</jats:sup> cMpc (with <jats:italic>γ</jats:italic> = 1.8). Our work, together with the previous study of LAEs around quasars, traces simultaneously the clustering properties of both optical and dusty galaxy populations in quasars fields, stressing the importance of multiwavelength studies, and highlighting important questions about galaxy properties in high-<jats:italic>z</jats:italic> dense environments.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The acceleration of charged particles by interplanetary shocks (IPs) can drain a nonnegligible fraction of the plasma pressure. In this study, we have selected 17 IPs observed in situ at 1 au by the Advanced Composition Explorer and the Wind spacecraft, and 1 shock at 0.8 au observed by Parker Solar Probe. We have calculated the time-dependent partial pressure of suprathermal and energetic particles (smaller and greater than 50 keV for protons and 30 keV for electrons, respectively) in both the upstream and downstream regions. The particle fluxes were averaged for 1 hr before and 1 hr after the shock time to remove short timescale effects. Using the MHD Rankine–Hugoniot jump conditions, we find that the fraction of the total upstream energy flux transferred to suprathermal and energetic downstream particles is typically ≲16%, in agreement with previous observations and simulations. Notably, by accounting for errors on all measured shock parameters, we have found that for any given fast magnetosonic Mach number, <jats:italic>M</jats:italic> <jats:sub> <jats:italic>f</jats:italic> </jats:sub> &lt; 7, the angle between the shock normal and average upstream magnetic field, <jats:italic>θ</jats:italic> <jats:sub>Bn</jats:sub>, is not correlated with the energetic particle pressure; in particular, the partial pressure of energized particles does not decrease for <jats:italic>θ</jats:italic> <jats:sub>Bn</jats:sub> ≳ 45°. The downstream electron-to-proton energy ratio in the range ≳ 140 eV for electrons and ≳ 70 keV for protons exceeds the expected ∼1% and nears equipartition (&gt;0.1) for the Wind events.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We study the tidal interaction of galaxies in the Eridanus supergroup, using H <jats:sc>i</jats:sc> data from the pre-pilot survey of the Widefield ASKAP <jats:italic>L</jats:italic>-band Legacy All-sky Blind surveY. We obtain optical photometric measurements and quantify the strength of tidal perturbation using a tidal parameter <jats:italic>S</jats:italic> <jats:sub>sum</jats:sub>. For low-mass galaxies of <jats:italic>M</jats:italic> <jats:sub>*</jats:sub> ≲ 10<jats:sup>9</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>, we find a dependence of decreasing H <jats:sc>i </jats:sc>to optical disk size ratio with increasing <jats:italic>S</jats:italic> <jats:sub>sum</jats:sub>, but no dependence of H <jats:sc>i</jats:sc> spectral line asymmetry with <jats:italic>S</jats:italic> <jats:sub>sum</jats:sub>. This is consistent with the behavior expected under tidal stripping. We confirm that the color profile shape and color gradient depend on the stellar mass, but there is an additional correlation of low-mass galaxies having their color gradients within 2<jats:italic>R</jats:italic> <jats:sub>50</jats:sub> increasing with higher <jats:italic>S</jats:italic> <jats:sub>sum</jats:sub>. For these low-mass galaxies, the dependence of color gradients on <jats:italic>S</jats:italic> <jats:sub>sum</jats:sub> is driven by the color becoming progressively redder in the inner disk when tidal perturbations are stronger. For high-mass galaxies, there is no dependence of color gradients on <jats:italic>S</jats:italic> <jats:sub>sum</jats:sub>, and we find a marginal reddening throughout the disks with increasing <jats:italic>S</jats:italic> <jats:sub>sum</jats:sub>. Our result highlights tidal interaction as an important environmental effect in producing the faint end of the star formation suppressed sequence in galaxy groups.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We have used X-ray data from the Neutron Star Interior Composition Explorer (NICER) to search for long-timescale temporal correlations (“red noise”) in the pulse times of arrival (TOAs) from the millisecond pulsars PSR J1824−2452A and PSR B1937+21. These data more closely track intrinsic noise because X-rays are unaffected by the radio-frequency-dependent propagation effects of the interstellar medium. Our search yields strong evidence (natural log Bayes factor of 9.634 ± 0.016) for red noise in PSR J1824−2452A, but the search is inconclusive for PSR B1937+21. In the interest of future X-ray missions, we devise and implement a method to simulate longer and higher-precision X-ray data sets to determine the timing baseline necessary to detect red noise. We find that the red noise in PSR B1937+21 can be reliably detected in a 5 yr mission with a TOA error of 2 <jats:italic>μ</jats:italic>s and an observing cadence of 20 observations per month compared to the 5 <jats:italic>μ</jats:italic>s TOA error and 11 observations per month that NICER currently achieves in PSR B1937+21. We investigate detecting red noise in PSR B1937+21 with other combinations of observing cadences and TOA errors. We also find that time-correlated red noise commensurate with an injected stochastic gravitational-wave background having an amplitude of <jats:italic>A</jats:italic> <jats:sub>GWB</jats:sub> = 2 × 10<jats:sup>−15</jats:sup> and spectral index of timing residuals of <jats:italic>γ</jats:italic> <jats:sub>GWB</jats:sub> = 13/3 can be detected in a pulsar with similar TOA precision to PSR B1937+21. This is with no additional red noise in a 10 yr mission that observes the pulsar 15 times per month and has an average TOA error of 1 <jats:italic>μ</jats:italic>s.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>This paper is the fourth in a series presenting (galaxy morphology, and thus galaxy formation)-dependent black hole (BH) mass, <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub>, scaling relations. We have used a sample of 119 galaxies with directly measured <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub> and host spheroid parameters obtained from multicomponent decomposition of, primarily, 3.6 <jats:italic>μ</jats:italic>m Spitzer images. Here, we investigate the correlations between <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub> and the projected (apparent) luminosity density <jats:italic>μ</jats:italic>, the projected stellar mass density Σ, and the de-projected (internal) stellar mass density <jats:italic>ρ</jats:italic>, for various spheroid radii. We discover the predicted <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub>–<jats:italic>μ</jats:italic> <jats:sub>0,sph</jats:sub> relation and present the first <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub>–<jats:italic>μ</jats:italic> <jats:sub> <jats:italic>e</jats:italic>,sph</jats:sub> and <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub>–<jats:italic>ρ</jats:italic> <jats:sub>e,int,sph</jats:sub> diagrams displaying slightly different (possibly curved) trends for early- and late-type galaxies (ETGs and LTGs, respectively) and an offset between ETGs with (fast-rotators, ES/S0) and without (slow-rotators, E) a disk. The scatter about various <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub>–〈Σ〉<jats:sub>R,sph</jats:sub> (and 〈<jats:italic>ρ</jats:italic>〉<jats:sub> <jats:italic>r</jats:italic>,sph</jats:sub>) relations is shown to systematically decrease as the enclosing aperture (and volume) increases, dropping from 0.69 dex when using the spheroid “compactness,” 〈Σ〉<jats:sub>1kpc,sph</jats:sub>, to 0.59 dex when using 〈Σ〉<jats:sub>5kpc,sph</jats:sub>. We also reveal that <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub> correlates with the internal density, <jats:italic>ρ</jats:italic> <jats:sub>soi,sph</jats:sub>, at the BH’s sphere-of-influence radius, such that core-Sérsic (high Sérsic index, <jats:italic>n</jats:italic>) and (low-<jats:italic>n</jats:italic>) Sérsic galaxies define different relations with total rms scatters 0.21 dex and 0.77 dex, respectively. The <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub>–〈<jats:italic>ρ</jats:italic>〉<jats:sub>soi,sph</jats:sub> relations will help with direct estimation of tidal disruption event rates, binary BH lifetimes, and together with other BH scaling relations, improve the characteristic strain estimates for long-wavelength gravitational waves pursued with pulsar timing arrays and space-based interferometers.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present results from Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm continuum observations of a sample of 27 star-forming galaxies at <jats:italic>z</jats:italic> = 2.1–2.5 from the MOSFIRE Deep Evolution Field survey with metallicity and star formation rate measurements from optical emission lines. Using stacks of Spitzer, Herschel, and ALMA photometry (rest frame ∼8–400 <jats:italic>μ</jats:italic>m), we examine the infrared (IR) spectral energy distributions (SED) of <jats:italic>z </jats:italic>∼ 2.3 subsolar-metallicity (∼0.5 <jats:italic>Z</jats:italic> <jats:sub>⊙</jats:sub>) luminous infrared galaxies (LIRGs). We find that the data agree well with an average template of higher-luminosity local low-metallicity dwarf galaxies (reduced <jats:italic>χ</jats:italic> <jats:sup>2</jats:sup> = 1.8). When compared with the commonly used templates for solar-metallicity local galaxies or high-redshift LIRGs and ultraluminous IR galaxies, even in the most favorable case (with reduced <jats:italic>χ</jats:italic> <jats:sup>2</jats:sup> = 2.8), the templates are rejected at &gt;98% confidence. The broader and hotter IR SED of both the local dwarfs and high-redshift subsolar-metallicity galaxies may result from different grain properties or a harder/more intense ionizing radiation field that increases the dust temperature. The obscured star formation rate (SFR) indicated by the far-IR emission of the subsolar-metallicity galaxies is only ∼60% of the total SFR, considerably lower than that of the local LIRGs with ∼96%–97% obscured fractions. Due to the evolving IR SED shape, the local LIRG templates fit to mid-IR data overestimate the Rayleigh–Jeans tail measurements by a factor of 2–20. These templates underestimate IR luminosities if fit to the observed ALMA fluxes by &gt;0.4 dex. At a given stellar mass or metallicity, dust masses at <jats:italic>z</jats:italic> ∼ 2.3 are an order of magnitude higher than <jats:italic>z</jats:italic> ∼ 0. Given the predicted molecular gas fractions, the observed <jats:italic>z</jats:italic> ∼ 2.3 dust-to-stellar mass ratios suggest lower dust-to-molecular gas masses than in local galaxies with similar metallicities.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The solar wind, when measured close to 1 au, is found to flow mostly radially outward. There are, however, periods when the flow makes angles up to 15° away from the radial direction, both in the east–west and north–south directions. Stream interaction regions (SIRs) are a common cause of east–west flow deflections. Coronal mass ejections (CMEs) may be associated with nonradial flows in at least two different ways: (1) the deflection of the solar wind in the sheath region, especially close to the magnetic ejecta front boundary, may result in large nonradial flows; and (2) the expansion of the magnetic ejecta may include a nonradial component, which should be easily measured when the ejecta is crossed away from its central axis. In this work, we first present general statistics of nonradial solar wind flows as measured by STEREO/PLASTIC throughout the first 13 yr of the mission, focusing on solar cycle variation. We then focus on the larger deflection flow angles and determine that most of these are associated with SIRs near solar minimum and with CMEs near solar maximum. However, we find no clear evidence of strongly deflected flows, as would be expected if large deflections around the magnetic ejecta or ejecta with elliptical cross sections with large eccentricities were common. We use these results to develop a better understanding of CME expansion and the nature of magnetic ejecta, and point to shortcomings in our understanding of CMEs.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Metal cyanides and isocyanides play a relevant role in the metal chemistry of the carbon-rich circumstellar envelope IRC+10216. It is thought that hydrometal cyanides/isocyanides could also be present in these environments; in fact, HMgNC has been detected in the same source that MgCN, MgNC, and AlNC. The aim of this work is to provide information about hydroaluminum cyanide/isocyanide. For this goal, a comprehensive analysis of the doublet and quartet potential energy surfaces of the [Al, C, H, N] system has been carried out. Different quantum chemistry methodologies from density functional theory to ab initio have been employed. For the [Al, C, H, N] isomers, the stability against dissociation and their interconversion processes have been analyzed. Our results show that the most relevant isomers from an experimental point of view are HAlCN and HAlNC. HAlNC has been found to be the most stable isomer followed by HAlCN, which is located at 1.59 kcal mol<jats:sup>−1</jats:sup> (0.0689 eV) at the composite level. The interconversion process between HAlCN and HAlNC presents an energy barrier of 10.0 kcal mol<jats:sup>−1</jats:sup> (5032 K) that makes this process not viable in the interstellar medium. We provide a complete set of relevant spectroscopic parameters for rotational spectroscopy for both HAlCN and HAlNC isomers using state-of-the-art quantum chemical computations, mandatory to guide an eventual laboratory or interstellar detection. Moreover, both isomers present sizable <jats:italic>μ</jats:italic> <jats:sub> <jats:italic>a</jats:italic> </jats:sub> dipole moment components (3.7 and 3.3 D, respectively), which are large enough to enable a characterization by means of rotational spectroscopy, further increasing their interest as interstellar candidates.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present the results of a time-coincident event search for low-energy electron antineutrinos in the KamLAND detector with gamma-ray bursts (GRBs) from the Gamma-ray Coordinates Network and Fermi Gamma-ray Burst Monitor. Using a variable coincidence time window of ±500 s plus the duration of each GRB, no statistically significant excess above the background is observed. We place the world’s most stringent 90% confidence level upper limit on the electron antineutrino fluence below 17.5 MeV. Assuming a Fermi–Dirac neutrino energy spectrum from the GRB source, we use the available redshift data to constrain the electron antineutrino luminosity and effective temperature.</jats:p>