adsabs/AstroCLIMB huggingface dataset:
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Resonance locations in the K2-381 system. The orbital period is shown on the y-axis and eccentricity is on the x-axis; note that the y-axes of the two subplots are discontinuous and not to scale. The locations of planets b and c are shown with green and blue circles, respectively, and the solid horizontal lines extend to the eccentricity at which each planet would cross the next planet’s orbit. The shaded regions show, as a function of eccentricity, the location and analytically estimated widths of the 2:1 mean motion resonance for planets b and c, and the 5:3 mean motion resonance for planets c and d; the label “5:3-d” indicates, for instance, that a test particle at that location would complete three orbits in the same amount of time that planet c takes to complete five orbits. The shaded regions surrounding each resonance line are the resonance widths corresponding to the lower (dark shading) and upper (light shading) planet mass limits, as propagated from the uncertainty on the planets’ radii.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: The location and analytically estimated widths of the low-order mean motion resonances in the K2-384 system. See Figure 10 for a description.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Validated planet centroid plots. The contours show the 1σ, 2σ, and 3σ contours for the centroid locations for out-of-transit cadences; the gray points show the remaining out-of-transit centroid locations that fall outside those contours. The blue points are the centroid locations of the in-transit cadences.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Validated planet folded light curves. The solid green line is the best-fit transit model; the large blue points are binned observations.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Validated planet folded light curves. Description as for Figure 3.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Validated planet centroid plots. Description as for Figure 7.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Left: gas density, n(H2), as a function of the H2 column density in a 3D model of the H-MM1 core (see text). The shaded regions show the densities between the 5th and 95th percentile (pale blue) and between the 16th and 84th percentile (turquoise) within a certain column density bin. The red line shows a linear fit to the weighted mean densities, ﹩\bar{n}({{\rm{H}}}_{2})﹩, where each LOS is weighted according to standard deviation of the density (﹩1/{\sigma }_{n}^{2}﹩) along that LOS. The error bars correspond to the weighted sigmas of the sample densities. The median density in each N(H2) bin is shown with small horizontal bars. Right: fractional NH3 abundance as a function of gas density in H-MM1. The relationship is derived by fitting a broken line to mean NH3 column densities below and above the turning point N(H2) = 2.6 × 1022 cm−2 (see Section 3.4), and using a linear fit to ﹩\bar{n}({{\rm{H}}}_{2})﹩ vs. N(H2) on the left. Also shown are predictions from our chemistry model including chemical desorption (CD; diamonds) and CD turned off (plus signs; see text).
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: (a) Spline fit through local N(H2) peaks along the ridge of H-MM1. (b) Horizontal cut through the N(H2) maximum of the core, together with a Plummer-type fit to the profile. (c) Density model of H-MM1 constructed from Plummer fits. The isodensity surfaces shown are n(H2) = 104 cm−3 (green), 105 cm−3 (purple), 5 × 105 cm−3 (red), and 106 cm−3 (blue). The numbers indicate angular separations in arcseconds. The distance to the object is 138.4 pc, so a separation of 100″ corresponds to 13,840 au.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Probability density function estimated with KDEs of the fractional NH3 abundance toward H-MM1, [NH3]/[H2]. The value estimated from single-dish observations (Harju et al. 2017) is shown by the vertical brown line, ﹩{[{\mathrm{NH}}_{3}]/[{{\rm{H}}}_{2}]}_{\mathrm{SD}}=7.6\,\times \,{10}^{-9}﹩. The mean value of the column density ratio is marked with a vertical blue line, ﹩{[{\mathrm{NH}}_{3}]/[{{\rm{H}}}_{2}]}_{\mathrm{int}}=2.7\,\times \,{10}^{-8}﹩, and the slope of the linear fit is marked with a red line, ﹩{[{\mathrm{NH}}_{3}]/[{{\rm{H}}}_{2}]}_{\mathrm{fit}}=(1.975\pm 0.005)\times {10}^{-8}﹩ ( ±10% systematic).
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Corner plot of the marginalized posterior distributions for each parameter. The 16th, 50th, and 84th percentiles of each marginalized posterior distributions are shown by the vertical dashed lines. The results are summarized in Table 1, where a and b are the [NH3]/[H2] abundance (in units of 10−8) and the H2 column density offset (in units of 1014 cm2) of the linear relation in the lower column density region, respectively; x 0 is the H2 column density (in units of 1022 cm2) beyond which the depletion region is identified; and c is the [NH3]/[H2] abundance (in units of 10−8) in the depletion region.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Physical model of H-MM1 adopted in chemical simulation: H2 number density (green), as well as the gas (blue) and dust (red) temperatures, as functions of the radial distance from the center.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Modeled fractional abundances of selected species as functions of the volume density at the time 3 × 105 yr after the beginning of the simulation. Left: a model without CD. Right: a model with CD turned on, assuming that 1% of exothermic surface reactions will lead to the evaporation of the product.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: NH3 emission in LTE in the center of H-MM1. KDE comparison between the ratios of the excitation to kinetic temperature derived from NH3 and H2 column densities. In the case of perfect LTE the temperature ratio is 1. The data, for which at higher N(H2) values the temperature ratio is nearly constant ≈0.9, display a behavior very close to LTE. The black horizontal segments show the mean values within the N(H2) bins.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Velocity dispersion of NH3 lines (color map) and the distribution of bright 96.7 GHz methanol emission (contours) in H-MM1. The contour levels go from 0.8 to 4.0 K km s−1 by steps of 0.8 K km s−1 and alternating between blue and purple.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Simulated p NH3 column density (left) and integrated intensity ((1, 1) and (2, 2); middle and right panels, respectively) maps. The white circle in each panel indicates a region of 2000 au diameter.
Paper: Hubble Space Telescope STIS Spectroscopy of Nova T Aurigae 1891
Authors: Conor Larsen, Patrick Godon, Edward M. Sion
Figure caption: The spectrum of T Aur (in red) is fitted with an accretion disk model (in black) with a WD mass M wd = 0.80M ⊙, an accretion rate ﹩\dot{M}={10}^{-8}\,{M}_{\odot }﹩ yr−1, and an inclination i = 41°, giving a distance of 858 pc and a ﹩{\chi }_{\nu }^{2}﹩ value of 12.7. All the disk models with M wd = 0.55, 0.80, & 1.03M ⊙, with an accretion rate of the order of 10−8 M ⊙ and inclination i = 41 & 60°, give about the same results (large ﹩{\chi }_{\nu }^{2}﹩ and same distance) as the Lyα region cannot properly be fitted with such disk models. The regions in blue have been masked before the fitting.
Paper: Hubble Space Telescope STIS Spectroscopy of Nova T Aurigae 1891
Authors: Conor Larsen, Patrick Godon, Edward M. Sion
Figure caption: The spectrum of T Aur (in red) is fitted with an accretion disk with absorbing slabs and ISM absorption model (solid black line). The addition of three absorbing slabs generates a spectrum with some absorption lines (dashed black line); and the addition of the ISM models creates a Lyα profile (solid black) that matches the observed spectrum (red). A best fit is obtained for a WD mass of 1.03M ⊙ accreting at a rate of 7.6 × 10−9 M ⊙ yr−1, with an inclination of 41°, giving a distance of 839 pc and bringing the ﹩{\chi }_{\nu }^{2}﹩ value down to 2.30.
Paper: Hubble Space Telescope STIS Spectroscopy of Nova T Aurigae 1891
Authors: Conor Larsen, Patrick Godon, Edward M. Sion
Figure caption: The HST/STIS spectrum of the Nova T Aurigae 1891 is shown with line identification. The spectrum has been dereddened assuming E(B − V) = 0.42.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: The MUSE + GNIRS spectrum of PSO J083+11 (black line) and its associated shot noise (gray line). The median composite spectrum of the low-redshift quasar analogs is shown as a cyan line with the 1σ dispersion around the median as a light blue region. The composite spectrum gives a decent fit to the main features observed in the PSO J083+11 spectrum redward of the Lyα emission. On the other hand, the PCA model to better predict the blue side of the quasar spectrum and its 1σ dispersion are denoted with the red line and shaded region, respectively. The wavelength range and spectrum used in the PCA fit to predict Lyα is shown with the red dashed line. The inset figure shows the zoom-in to the region around Lyα. The Mg II λλ2796,2803 doublet and Mg I λ2853 absorptions at z = 2.2305 are marked with blue dotted lines. The wavelength ranges highlighted with magenta (λ obs = 8850–8997 Å) and green (λ obs = 9100–9200 Å) colors are the region of interest for creating the Lyα pseudo-narrowband and continuum images, respectively.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: Velocity stack of the sub-DLA metal absorption lines at z = 6.314 observed in the continuum-normalized combined MUSE + FIRE spectrum. The data are shown as black lines with fitted models superposed in red. Note that the width of the red lines corresponds to the model uncertainty (see Section 3.1). Blue curves show a 1σ shot noise spectrum. We use gray lines to show the data in regions with high noise due to skylines. The absorptions from Mg II λλ2796,2803 doublet and C II λ1334are clearly seen while there is only a marginal detection of O I λ1302. Finally, the other associated metals like Si II, Al II, and Fe II, which one would expect specifically for a strong absorber, are not apparent in the spectrum.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption:  Left panel: MUSE image centered around PSO J083+11, created by collapsing the λ obs = 8000–9000 Å layers. An overlay of [C II] emission from ALMA data is shown with a black contour. We then extract the spectrum at the region of interest using an aperture of 0.″5 radius (dotted circles). Right panel: MUSE spectrum of J083.8372+11.8474 (black line)—i.e., a z = 6.3309 companion galaxy near PSO J083+11–and its associated shot noise (red line). We do not find any prominent emission lines in the wavelength region where the Lyα emission from the companion galaxy is expected (blue area). A faint continuum emission is seen, which originates from the adjacent bright galaxy at z ≈ 0.29 in the southeast direction.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: SED slope (α) vs. Hα equivalent width for Taurus and Upper Sco/ρ Oph. These quantities are measures of infrared excess and accretion strength, respectively. We use colors to denote different variability types and search for correlations between flux behavior and inner disk properties. The most prominent patterns identified include consistently low gas emission for the dippers and periodic stars, as well as very weak disks (i.e., low infrared excess) for the latter. As in previous figures, points are scaled in size according to amplitude to the 1/3 power.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: Available inclination measurements vs. Q value, and colored by variability class. Points are scaled in size according to variability amplitude to the 1/3 power. Those circled in black denote blends (e.g., multiple-star systems). These data, particularly for Upper Scorpius and ρ Oph (bottom panel), suggest that single (nonbinary) periodic and quasiperiodic sources are associated with disk inclinations of at least 30°–40°.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: Infrared excess slope as a function of spectral type (a proxy for mass) and variability type. We use this diagram to assess correlations in variability type as a function of stellar mass and disk evolutionary status, but do not detect appreciable trends apart from periodic sources appearing almost exclusively in the class III set.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: Light curves of candidate disk-bearing stars in Taurus observed with K2, in order of EPIC identifier. Figure labels include the variability type from Table 2, namely “P” = strictly periodic behavior, “MP” = multiple distinct periods, “QPD” = quasiperiodic dippers, “QPS” = quasiperiodic symmetric, “APD” = aperiodic dippers, “B” = bursters, “S” = stochastic stars, and “L” = long-timescale behavior that does not fall into the other categories. Values of flux symmetry metric M and the quasiperiodicity metric Q from Table 2 are also provided.
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: Comparison of various labeling schemes for multiresolution maps. The figures are cylindrical projections of Figure 3(c). A single base pixel is highlighted. (a) The MOL scheme labels each pixel by their equivalent order and pixel index in single-resolution NESTED maps. (b) The RS scheme uses the beginning (inclusive) and end (exclusive) indices of a equivalent NESTED map with the highest resolution level. (c) The NUNIQ encodes the equivalent order and nested pixel index into a single unambiguous number (explained in text). (d) The TREE scheme stores the corresponding base pixel and the node indices in a quadtree.
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: Example of the result of taking the product between two maps, (a) and (b), depending on various conditions. A single base pixel is shown. Figures (c) and (d) assume both maps are density-like, resulting also in a density-like map. Figures (e) and (f) consider m 0 to be density-like and m 1 histogram-like, the output therefore being histogram-like. Standard operations, with no information loss, are shown in (c) and (e), while in-place operations that keep the m 0 mesh unchanged result in (d) and (f).
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: A multiresolution map representing the localization of SSS17a/AT 2017gfo by the Swope Telescope, both all-sky (a) and zoomed in around the source (b). The underlying mesh is overlaid. Sky maps for such well-localized sources are impractical or unfeasible using standard single-resolution maps.