Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>The Gemini Near-infrared Integral Field Spectrograph (NIFS) reduction pipeline is widely used to reduce NIFS data. However, there are critical known limitations. A new NIFS reduction pipeline has recently been developed and solves several of these problems. We present a comparison of stellar kinematics derived from the new and old data reduction pipelines, as well as recommendations for optimal NIFS data reduction.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We describe calibrated TESS images that serve as the input to the MIT Quick Look Pipeline, which we are releasing as a High Level Science Product (HLSP). We also outline the python package <jats:monospace>tica</jats:monospace>, which we use to fully calibrate the raw pixels and apply astrometric registration in the form of World Coordinate Solutions. This HLSP could serve as a means for delivering calibrated Full Frame Images to the public promptly after downlink from the spacecraft, which occurs every two weeks. This capability would potentially enable new science investigations with TESS data such as fast follow-up of transient sources and determination of new solar system object ephemerides.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We investigate how measurements of differential chromatic refraction might influence choices for survey strategy in the Legacy Survey of Space and Time.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The cometary globule CG 12 and its associated young cluster NGC 5367 is located at a Galactic latitude of <jats:italic>b</jats:italic> = 21°, and the origin of this high-latitude star formation event has been unclear. Getman et al. identified a nearby group of B stars and suggested they could be the remnant of a group of massive stars of which one exploded as a supernova. We here use Gaia EDR3 data to measure the accurate distance of NGC 5367 and the B-stars. We find a mean distance of 670 pc for NGC 5367 and 675 pc for the B-stars, strongly supporting the suggestion of Getman et al.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The black hole in the quasar SDSS J140821.67+025733.2 has been reported to have a mass of 1.96 × 10<jats:sup>11</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> based on measurements from the SDSS DR12 Quasar Catalog. As a result, references to this object as the most massive known black hole in the universe have recently appeared in scientific articles and in popular media including Wikipedia. We show that this extremely high mass estimate is incorrect, resulting from a faulty measurement of the C <jats:sc>iv</jats:sc> line width. From a new measurement of the Mg <jats:sc>ii</jats:sc> line width, we derive an estimate of <jats:italic>M</jats:italic> <jats:sub>BH</jats:sub> ≈ 8 × 10<jats:sup>9</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We report the discovery of a one magnitude increase in the optical brightness of the 59.63 minutes orbital period AM CVn binary SDSS J113732.32+405458.3. Public <jats:italic>g</jats:italic>, <jats:italic>r</jats:italic>, and <jats:italic>i</jats:italic> band data from the Zwicky Transient Facility exhibit a subsequent decline over a 300 days period, while a few data points from commissioning show that the peak was likely seen. Such an outburst is likely due to a change in the state of the accretion disk, making this the longest period AM CVn binary to reveal an unstable accretion disk. The object is now back to its previously observed (by SDSS and PS-1) quiescent brightness that is likely set by the accreting white dwarf. Prior observations of this object also imply that the recurrence times for such outbursts are likely more than 12 yr.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We combine different measurements of the polytropic index of the proton plasma in the heliosphere: (i) near-adiabatic index in the inner heliosphere ∼1 au, (ii) subadiabatic indices in the outer heliosphere ∼20–40 au, and (iii) near-zero indices in the inner heliosheath. These observations are unified by a single theoretical model of the polytropic index throughout its radial extent in the heliosphere; the corresponding fitting reveals the decreasing trend of the polytropic index with increasing heliocentric distance <jats:italic>R</jats:italic>. We anticipate that with increasing <jats:italic>R</jats:italic>, (i) the Debye length and mean-free-path decreases; (ii) the Landau damping is less effective, transferring thus less wave energy to particles; and (iii) the collisionality degree increases, indicating that the proton plasma in the inner heliosheath might be collisionless.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>I report the detection of linear X-ray features associated with PSR B2224+65, based on a new Chandra observation, plus two obtained ∼6 and 12 yr earlier. This mid-aged pulsar is known for its extreme proper motion and its associated guitar-shaped optical nebula in the opposite direction. The main jet-like feature with the same proper motion is <jats:inline-formula> <jats:tex-math> <?CDATA $\sim 2\buildrel{\,\prime}\over{.} 4$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∼</mml:mo> <mml:mn>2</mml:mn> <mml:mo>.′</mml:mo> <mml:mn>4</mml:mn> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="rnaasabd854ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> long and directed 62° away from the nebula, which is associated with a faint X-ray tail detected for the first time. Also now clearly revealed are the sharp forward edge and epoch-dependent substructures of the feature and its curvature near the pulsar, as well as a much fainter/shorter counter-jet. Magnetic field appears to play a central role in the formation of the features, which represent the synchrotron radiation of energetic particles leaked out from the bow shock nebula through small holes, produced probably by localized magnetic reconnection, and streaming along interstellar magnetic field lines.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>A research project on the activities of solar-type stars based on the LAMOST sky survey was initiated recently. We describe the data processing workflow of the project and perspective on scientific yields.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Stellar models often use relations between the temperature <jats:italic>T</jats:italic> and optical depth <jats:italic>τ</jats:italic> to evaluate the structure of their optically thin outer layers. We fit a novel analytic function to the Hopf function <jats:italic>q</jats:italic>(<jats:italic>τ</jats:italic>) of a radiation-coupled hydrodynamics simulation of near-surface convection with solar parameters by Trampedach et al. The fit is accurate to within 0.82% for the solar simulation and to within 13% for all the simulations that are not on either the low-temperature or low-gravity edges of the grid of simulations.</jats:p>