Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>We forecast constraints on the amplitude of matter clustering <jats:italic>σ</jats:italic> <jats:sub>8</jats:sub>(<jats:italic>z</jats:italic>) achievable with the combination of cluster weak lensing and number counts, in current and next-generation weak lensing surveys. We advocate for an approach, analogous to galaxy–galaxy lensing, in which the observables in each redshift bin are the mean number counts and the mean weak lensing profile of clusters above a mass proxy threshold. The primary astrophysical nuisance parameter is the logarithmic scatter <jats:inline-formula> <jats:tex-math> <?CDATA ${\sigma }_{\mathrm{ln}M}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabdc23ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> between the mass proxy and true mass near the threshold. For surveys similar to the Dark Energy Survey (DES), the Roman Space Telescope High Latitude Survey (HLS), and the Rubin Observatory Legacy Survey of Space and Time (LSST), we forecast aggregate precision on <jats:italic>σ</jats:italic> <jats:sub>8</jats:sub> of 0.26%, 0.24%, and 0.10%, respectively, <jats:italic>if</jats:italic> the mass–observable scatter is known externally to <jats:inline-formula> <jats:tex-math> <?CDATA ${\rm{\Delta }}{\sigma }_{\mathrm{ln}M}\leqslant 0.01$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabdc23ieqn2.gif" xlink:type="simple" /> </jats:inline-formula>. These constraints would be degraded by about 20% for <jats:inline-formula> <jats:tex-math> <?CDATA ${\rm{\Delta }}{\sigma }_{\mathrm{ln}M}=0.05$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabdc23ieqn3.gif" xlink:type="simple" /> </jats:inline-formula> in the case of DES or HLS and for <jats:inline-formula> <jats:tex-math> <?CDATA ${\rm{\Delta }}{\sigma }_{\mathrm{ln}M}=0.016$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabdc23ieqn4.gif" xlink:type="simple" /> </jats:inline-formula> for LSST. A 1 month observing program with Roman Space Telescope targeting ∼2500 massive clusters could achieve a ∼ 0.5% constraint on <jats:italic>σ</jats:italic> <jats:sub>8</jats:sub>(<jats:italic>z</jats:italic> = 0.7) on its own, or a ∼ 0.33% constraint in combination with the HLS. Realizing the constraining power of clusters Requires accurate knowledge of the mass–observable relation and stringent control of systematics. We provide analytic approximations to our numerical results that allow for easy scaling to other survey assumptions or other methods of cluster mass estimation.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Type Ia supernovae (SNe Ia) are standardizable candles, but for over a decade there has been a debate on how to properly account for their correlations with host galaxy properties. Using the Bayesian hierarchical model UNITY, we simultaneously fit for the SN Ia light curve and host galaxy standardization parameters on a set of 103 Sloan Digital Sky Survey II SNe Ia. We investigate the influences of host stellar mass, along with both localized (<jats:italic>r</jats:italic> &lt;3 kpc) and host-integrated average stellar ages, derived from stellar population synthesis modeling. We find that the standardization for the light-curve shape (<jats:italic>α</jats:italic>) is correlated with host galaxy standardization terms (<jats:italic>γ</jats:italic> <jats:sub> <jats:italic>i</jats:italic> </jats:sub>) requiring simultaneous fitting. In addition, we find that these correlations themselves are dependent on host galaxy stellar mass that includes a shift in the color term (<jats:italic>β</jats:italic>) of 0.8 mag, only significant at 1.2<jats:italic>σ</jats:italic> due to the small sample. We find a linear host mass standardization term at the 3.7<jats:italic>σ</jats:italic> level, that by itself does not significantly improve the precision of an individual SN Ia distance. However, a standardization that uses both stellar mass and average local stellar age is found to be significant at &gt;3<jats:italic>σ</jats:italic> in the two-dimensional posterior space. In addition, the unexplained scatter of SNe Ia absolute magnitude post standardization, is reduced from <jats:inline-formula> <jats:tex-math> <?CDATA ${0.122}_{-0.018}^{+0.019}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabd550ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> to 0.109 ± 0.017 mag, or ∼10%. We do not see similar improvements when using global ages. This combination is consistent with either metallicity or line-of-sight dust affecting the observed luminosity of SNe Ia.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>State-of-the-art cosmological simulations on classical computers are limited by time, energy, and memory usage. Quantum computers can perform some calculations exponentially faster than classical computers, using exponentially less energy and memory, and may enable extremely large simulations that accurately capture the whole dynamic range of structure in the universe within statistically representative cosmic volumes. However, not all computational tasks exhibit a “quantum advantage.” Quantum circuits act linearly on quantum states, so nonlinearities (e.g., self-gravity in cosmological simulations) pose a significant challenge. Here we outline one potential approach to overcome this challenge and solve the (nonlinear) Schrödinger–Poisson equations for the evolution of self-gravitating dark matter, based on a hybrid quantum–classical variational algorithm framework (Lubasch et al.). We demonstrate the method with a proof-of-concept mock quantum simulation, envisioning a future where quantum computers will one day lead simulations of dark matter.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The Maunder Minimum (MM; 1645–1715) is currently considered the only grand minimum within telescopic sunspot observations since 1610. During this epoch, the Sun was extremely quiet and unusually free from sunspots. However, despite a reduced frequency, candidate aurorae were reported in the mid-European sector during this period and have been associated with occurrences of interplanetary coronal mass ejections (ICMEs), although some of them have been identified as misinterpretations. Here, we have analyzed reports of candidate aurorae on 1680 June 1 with simultaneous observations in central Europe, and compared their descriptions with visual accounts of early modern aurorae. Contemporary sunspot drawings on 1680 May 22, 24, and 27 have shown a sunspot. This sunspot may have been a source of ICMEs, which caused the reported candidate aurorae. On the other hand, its intensity estimate shows that the geomagnetic storm during this candidate aurora was probably within the capability of the storms derived from the corotating interaction region (CIR). Therefore, we accommodate both ICMEs and CIRs as its possible origin. This interpretation is probably applicable to a number of candidate aurorae in the oft-cited Hungarian catalog, on the basis of the reconstructed margin of their equatorward auroral boundary. Moreover, this catalog itself has clarified that the considerable candidates during the MM were probably misinterpretations. Therefore, the frequency of the auroral visibility in Hungary was probably lower than previously considered and agrees more with the generally slow solar wind in the existing reconstructions, whereas sporadic occurrences of sunspots and coronal holes still caused occasional geomagnetic storms.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present the merger rate density of Population III binary black holes (BHs) by means of a widely used binary population synthesis code <jats:monospace>BSE</jats:monospace> with extensions to very massive and extreme metal-poor stars. We consider not only low-mass BHs (lBHs: 5–50<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>) but also high-mass BHs (hBHs: 130–200<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>), where lBHs and hBHs are below and above the pair-instability mass gap (50–130<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>), respectively. Population III BH–BHs can be categorized into three subpopulations: BH–BHs without hBHs (hBH0s: <jats:italic>m</jats:italic> <jats:sub>tot</jats:sub> ≲ 100<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>), with one hBH (hBH1s: <jats:italic>m</jats:italic> <jats:sub>tot</jats:sub> ∼ 130–260<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>), and with two hBHs (hBH2s: <jats:italic>m</jats:italic> <jats:sub>tot</jats:sub> ∼ 270–400<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>), where <jats:italic>m</jats:italic> <jats:sub>tot</jats:sub> is the total mass of a BH–BH. Their merger rate densities at the current universe are ∼0.1 yr<jats:sup>−1</jats:sup> Gpc<jats:sup>−3</jats:sup> for hBH0s, and ∼0.01 yr<jats:sup>−1</jats:sup> Gpc<jats:sup>−3</jats:sup> for the sum of hBH1s and hBH2s, provided that the mass density of Population III stars is ∼10<jats:sup>13</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> Gpc<jats:sup>−3</jats:sup>. These rates are modestly insensitive to initial conditions and single star models. The hBH1 and hBH2 mergers can dominate BH–BHs with hBHs discovered in the near future. They have low effective spins ≲0.2 in the current universe. The number ratio of hBH2s to hBH1s is high, ≳0.1. We also find that BHs in the mass gap (up to ∼85<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>) merge. These merger rates can be reduced to nearly zero if Population III binaries are always wide (≳100<jats:italic>R</jats:italic> <jats:sub>⊙</jats:sub>), and if Population III stars always enter into chemically homogeneous evolution. The presence of close Population III binaries (∼10<jats:italic>R</jats:italic> <jats:sub>⊙</jats:sub>) is crucial for avoiding the worst scenario.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present <jats:monospace>StrayCats</jats:monospace>, a catalog of NuSTAR stray light observations of X-ray sources. Stray light observations arise for sources 1°–4° away from the telescope pointing direction. At this off-axis angle, X-rays pass through a gap between the optics and aperture stop and so do not interact with the X-ray optics; instead, they directly illuminate the NuSTAR focal plane. We have systematically identified and examined over 1400 potential observations resulting in a catalog of 436 telescope fields and 78 stray light sources that have been identified. The sources identified include historically known persistently bright X-ray sources, X-ray binaries in outburst, pulsars, and type I X-ray bursters. In this paper, we present an overview of the catalog, how we identified the <jats:monospace>StrayCats</jats:monospace> sources, and the analysis techniques required to produce high-level science products. Finally, we present a few brief examples of the science quality of these unique data.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Planets form in young circumstellar disks called protoplanetary disks. However, it is still difficult to catch planet formation in situ. Nevertheless, from recent ALMA/SPHERE data, encouraging evidence of the direct and indirect presence of embedded planets has been identified in disks around young stars: co-moving point sources, gravitational perturbations, rings, cavities, and emission dips or shadows cast on disks. The interpretation of these observations needs a robust physical framework to deduce the complex disk geometry. In particular, protoplanetary disk models usually assume the gas pressure scale height given by the ratio of the sound speed over the azimuthal velocity <jats:italic>H</jats:italic>/<jats:italic>r</jats:italic> = <jats:italic>c</jats:italic> <jats:sub> <jats:italic>s</jats:italic> </jats:sub>/<jats:italic>v</jats:italic> <jats:sub>k</jats:sub>. By doing so, <jats:italic>radiative</jats:italic> pressure fields are often ignored, which could lead to a misinterpretation of the real vertical structure of such disks. We follow the evolution of a gaseous disk with an embedded Jupiter-mass planet through hydrodynamical simulations, computing the disk scale height including radiative pressure, which was derived from a generalization of the stellar atmosphere theory. We focus on the vertical impact of the radiative pressure in the vicinity of circumplanetary disks, where temperatures can reach ≳1000 K for an accreting planet and radiative forces can overcome gravitational forces from the planet. The radiation pressure effects create a vertical, optically thick column of gas and dust at the protoplanet location, casting a shadow in scattered light. This mechanism could explain the peculiar illumination patterns observed in some disks around young stars such as HD 169142 where a moving shadow has been detected or the extremely high aspect ratio <jats:italic>H</jats:italic>/<jats:italic>r</jats:italic> ∼ 0.2 observed in systems like AB Aur and CT Cha.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>A protoplanetary disk (PPD) typically forms a dead zone near its midplane at a distance of a few astronomical units from the central protostar. Accretion through such a magnetically layered disk can be intrinsically unstable and has been associated with episodic outbursts in young stellar objects. We present the first investigation into the effects of a low-metallicity environment on the structure of the dead zone, as well as the resulting outbursting behavior of the PPD. We conducted global numerical hydrodynamic simulations of PPD formation and evolution in the thin-disk limit. The consequences of metallicity were considered via its effects on the gas and dust opacity of the disk, the thickness of the magnetically active surface layer, and the temperature of the prestellar cloud core. We show that the metal-poor disks accumulate much more mass in the innermost regions as compared to the solar-metallicity counterparts. The duration of the outbursting phase also varies with metallicity; the low-metallicity disks showed more powerful luminosity eruptions with a shorter burst phase, which was confined mostly to the early, embedded stages of the disk evolution. The lowest-metallicity disks with the higher cloud core temperature showed the most significant differences. The occurrence of outbursts was relatively rare in the disks around low-mass stars, and this was especially true at the lowest metallicities. We conclude that the metal content of the disk environment can have profound effects on both the disk structure and evolution in terms of episodic accretion.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>As cosmic structures form, matter density fluctuations collapse gravitationally and baryonic matter is shock-heated and thermalized. We therefore expect a connection between the mean gravitational potential energy density of collapsed halos, <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Omega }}}_{W}^{\mathrm{halo}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabe387ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>, and the mean thermal energy density of baryons, Ω<jats:sub>th</jats:sub>. These quantities can be obtained using two fundamentally different estimates: we compute <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Omega }}}_{W}^{\mathrm{halo}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabe387ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> using the theoretical framework of the halo model, which is driven by dark matter statistics, and measure Ω<jats:sub>th</jats:sub> using the Sunyaev–Zeldovich (SZ) effect, which probes the mean thermal pressure of baryons. First, we derive that, at the present time, about 90% of <jats:inline-formula> <jats:tex-math> <?CDATA ${{\rm{\Omega }}}_{W}^{\mathrm{halo}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabe387ieqn3.gif" xlink:type="simple" /> </jats:inline-formula> originates from massive halos with <jats:italic>M</jats:italic> &gt; 10<jats:sup>13</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>. Then, using our measurements of the SZ background, we find that Ω<jats:sub>th</jats:sub> accounts for about 80% of the kinetic energy of the baryons available for pressure in halos at <jats:italic>z</jats:italic> ≲ 0.5. This constrains the amount of nonthermal pressure, e.g., due to bulk and turbulent gas motion sourced by mass accretion, to be about Ω<jats:sub>non‐th</jats:sub> ≃ 0.4 × 10<jats:sup>−8</jats:sup> at <jats:italic>z</jats:italic> = 0.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Solar filaments often erupt partially. Although how they split remains elusive, the splitting process has the potential of revealing the filament structure and eruption mechanism. Here we investigate the pre-eruption splitting of an apparently single filament and its subsequent partial eruption on 2012 September 27. The evolution is characterized by three stages with distinct dynamics. During the quasi-static stage, the splitting proceeds gradually for about 1.5 hr, with the upper branch rising at a few kilometers per second and displaying swirling motions about its axis. During the precursor stage that lasts for about 10 minutes, the upper branch rises at tens of kilometers per second, with a pair of conjugated dimming regions starting to develop at its footpoints; with the swirling motions turning chaotic, the axis of the upper branch whips southward, which drives an arc-shaped extreme-ultraviolet front propagating in a similar direction. During the eruption stage, the upper branch erupts with the onset of a C3.7-class two-ribbon flare, while the lower branch remains stable. Judging from the well-separated footpoints of the upper branch from those of the lower one, we suggest that the pre-eruption filament processes a double-decker structure composed of two distinct flux bundles, whose formation is associated with gradual magnetic flux cancellations and converging photospheric flows around the polarity inversion line.</jats:p>