Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>Standard halo occupation distribution (HOD) models predict how galaxies occupy halos based on a single property, the virial mass, <jats:italic>M</jats:italic> <jats:sub>vir</jats:sub>. To incorporate galaxy assembly bias, we consider alternative halo mass proxies to use in the HOD. A promising replacement is maximum circular velocity, <jats:inline-formula> <jats:tex-math> <?CDATA ${V}_{\max }$?> </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:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="rnaasac67f3ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>, which measures the halo’s potential well, and successfully predicts galaxy clustering in subhalo abundance matching models. We fit galaxy clustering measurements from SDSS DR7 with two modified HODs besides the standard <jats:italic>M</jats:italic> <jats:sub>vir</jats:sub>-based model: one where <jats:inline-formula> <jats:tex-math> <?CDATA ${V}_{\max }$?> </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:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="rnaasac67f3ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> is used as the halo property that determines galaxy occupation, and the other adopting an adjustable combination of <jats:italic>M</jats:italic> <jats:sub>vir</jats:sub> and <jats:inline-formula> <jats:tex-math> <?CDATA ${V}_{\max }$?> </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:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="rnaasac67f3ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>. Except for the reduced volume <jats:italic>M</jats:italic> <jats:sub> <jats:italic>r</jats:italic> </jats:sub> &lt; − 20 threshold sample fit with <jats:inline-formula> <jats:tex-math> <?CDATA ${V}_{\max }$?> </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:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="rnaasac67f3ieqn4.gif" xlink:type="simple" /> </jats:inline-formula> alone, neither change improves the model performance in predicting the projected two-point correlation function, <jats:italic>w</jats:italic> <jats:sub>p</jats:sub>. We conclude that switching the primary variable to <jats:inline-formula> <jats:tex-math> <?CDATA ${V}_{\max }$?> </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:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="rnaasac67f3ieqn5.gif" xlink:type="simple" /> </jats:inline-formula> does not significantly improve the HOD model’s ability to fit galaxy clustering.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We study the newly released light curve from the fireball of the first interstellar meteor CNEOS 2014-01-08. The measured velocity and three observed flares down to an altitude of 18.7 km imply ambient ram pressure in the range of 113–194 MPa when the meteor disintegrated. The required yield strength is ≳20 times higher than stony meteorites and ≳2 times larger than iron meteorites. The implied slowdown in the atmosphere suggests an initial speed of about 66.5 km s<jats:sup>−1</jats:sup>, strengthening the case for an interstellar origin of this meteor and making it an outlier relative to the velocity dispersion of local stars.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The relatively new and expansive Apache Point Observatory Catalog of Optical Diffuse Interstellar Bands was analyzed to identify novel correlations between diffuse interstellar bands (DIBs) and optical reddening <jats:italic>E</jats:italic>(<jats:italic>B</jats:italic> − <jats:italic>V</jats:italic>), with a principal aim being to facilitate future identifications of the host molecular carriers. The following lines exhibit the highest Pearson <jats:italic>r</jats:italic> correlations in descending order (0.930 ≥ <jats:italic>r</jats:italic> ≥ 0.885), and are tied to DIBs featuring <jats:italic>n</jats:italic> ≥ 10 sightlines and possessing equivalent width uncertainties: <jats:italic>λ</jats:italic> (Å) ≃ 5236.27, 5793.24, 5797.18, 6449.27, 6795.26, 5948.87, 6113.22, 6860.02, 6059.34, 6520.74. Independent observations to confirm the preliminary trends are desirable, and extinction estimates could be subsequently inferred for targets by relying on longer-wavelength (NIR) photometric calibrations linked to a weighted subset of numerous DIBs. Lastly, several DIBs appear unassociated with <jats:italic>E</jats:italic>(<jats:italic>B</jats:italic> − <jats:italic>V</jats:italic>), thereby reaffirming that diverse carriers exist.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Rotational suppression of convection can occur on length scales which are larger than a critical length. Featherstone &amp; Hindman suggest that this can account for a second preferred length-scale in solar convection on supergranule scales. Here, I explore if rotational suppression of convection also occurs in the atmospheres of Earth and Venus.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present the SuperWASP light curve of a 10th magnitude A7V star containing a single, well-defined U-shaped transit-like event lasting around 11 days with a depth of 1.1%. The star is otherwise non-variable throughout the 8 yr duration of the observations. If the event is modeled as an exoplanet transit, it is compatible with a 1.8 <jats:italic>R</jats:italic> <jats:sub>J</jats:sub> exoplanet in a ∼205 au orbit with a period of ∼2200 yr.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Recently, we reported the discovery of a kpc-scale CO structure in the inner Galaxy which we named the Gangotri wave. The structure is at least 2 kpc in extent and its vertical distribution is wave-like in morphology. The analysis of the velocity data suggests Gangotri wave being a spur of the Milky Way or a sub-branch of the Norma arm. Following the discovery, there is a rebuttal published, expressing concerns on identifying the inner Galaxy CO emission features as a single coherent structure. In this article, we aim to address the concerns of the rebuttal article, hoping to clarify some of the criticisms.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The analysis of nine high resolution SWP spectra of the HgMn star <jats:italic>χ</jats:italic> Lupi obtained through the large aperture recorded by the International Ultraviolet Explorer reveals that the far-ultraviolet flux of <jats:italic>χ</jats:italic> Lupi remained probably constant over a timescale of about 24 hr, i.e., about 25% of the recently determined rotational period. <jats:italic>Whereas eight spectra have levels consistent with the average spectrum</jats:italic>, one spectrum shows a lower flux by about 15%. This probably reflects an instrumental effect, possibly a loss of the flux (the star may have slipped outside the aperture for a fraction of the exposure). <jats:italic>The available</jats:italic> IUE <jats:italic>data do not rule out variations in the FUV flux</jats:italic>.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Studies suggest that fracture systems are the driving mechanism for the formation of polygonal impact craters (PICs) on planetary bodies including the Moon and Vesta. We used the Java Mission-planning and Analysis for Remote Sensing crater application to investigate PICs on regional scales for both the Moon and Vesta to further understand how surface and subsurface fracture systems play a role in PIC formation. We measured the number of straight rim segments (sides) for each PIC, measured the angle between each of the straight rim segments and calculated the mean angle for each crater and the mean angle for the body to conduct a further analysis with other planetary bodies. The comparison with other planetary bodies helps to identify how PIC formation may vary based on a body's surface composition. From this study, it appears that surface fractures are not the main driving mechanism for PIC formation within our study regions and instead subsurface fractures may be the more dominant factor.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The analysis of 8 high resolution SWP spectra of the HgMn star <jats:italic>μ</jats:italic> Leporis obtained through the large aperture recorded by the International Ultraviolet Explorer reveals that the far ultraviolet flux of <jats:italic>μ</jats:italic> Leporis remained probably constant over a timescale of about 29 hr, ie. about 40% of the recently determined rotational period. One spectrum taken 10 yr before also has the same level than the average spectrum of the run. Whereas seven spectra of the 29 hr run have levels consistent with the average spectrum, one spectrum shows a lower flux by about 7% probably caused by a loss of the flux. The spectra taken with the LWP camera consistently show that the mid-UV flux remained stable over the 29 hr run. Hence the available IUE data do not show evidence of real flux variations in the ultraviolet range for <jats:italic>μ</jats:italic> Leporis.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>How much one has learned from an experiment is quantifiable by the information gain, also known as the Kullback–Leibler divergence. The narrowing of the posterior parameter distribution <jats:italic>P</jats:italic>(<jats:italic>θ</jats:italic>∣<jats:italic>D</jats:italic>) compared with the prior parameter distribution <jats:italic>π</jats:italic>(<jats:italic>θ</jats:italic>), is quantified in units of bits, as: <jats:inline-formula> <jats:tex-math> <?CDATA ${D}_{\mathrm{KL}}(P| \pi )=\int {\mathrm{log}}_{2}\left(\displaystyle \frac{P(\theta | D)}{\pi (\theta )}\right)\,P(\theta | D)d\theta \mathrm{bits}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>D</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>KL</mml:mi> </mml:mrow> </mml:msub> <mml:mo stretchy="true">(</mml:mo> <mml:mi>P</mml:mi> <mml:mo stretchy="true">∣</mml:mo> <mml:mi>π</mml:mi> <mml:mo stretchy="true">)</mml:mo> <mml:mo>=</mml:mo> <mml:mo>∫</mml:mo> <mml:msub> <mml:mrow> <mml:mi>log</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msub> <mml:mfenced close=")" open="("> <mml:mrow> <mml:mstyle displaystyle="true"> <mml:mfrac> <mml:mrow> <mml:mi>P</mml:mi> <mml:mo stretchy="true">(</mml:mo> <mml:mi>θ</mml:mi> <mml:mo stretchy="true">∣</mml:mo> <mml:mi>D</mml:mi> <mml:mo stretchy="true">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mi>π</mml:mi> <mml:mo stretchy="true">(</mml:mo> <mml:mi>θ</mml:mi> <mml:mo stretchy="true">)</mml:mo> </mml:mrow> </mml:mfrac> </mml:mstyle> </mml:mrow> </mml:mfenced> <mml:mspace width="0.25em" /> <mml:mi>P</mml:mi> <mml:mo stretchy="true">(</mml:mo> <mml:mi>θ</mml:mi> <mml:mo stretchy="true">∣</mml:mo> <mml:mi>D</mml:mi> <mml:mo stretchy="true">)</mml:mo> <mml:mi>d</mml:mi> <mml:mi>θ</mml:mi> <mml:mi>bits</mml:mi> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="rnaasac6b40ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> This research note gives an intuition what one bit of information gain means. It corresponds to a Gaussian shrinking its standard deviation by a factor of three.</jats:p>