adsabs/AstroCLIMB huggingface dataset:
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Our VLA B-configuration 20 cm radio continuum emission from disk galaxy NGC 5595 in contours superposed on the reproduction of the 103aO blue optical emission from NGC 5595 (Diaz-Hernández et al. 2009) in gray scale. Contours are at 3, 4, 5, 6, 8, 10, 11, 12, 14, 15, and 15.6 × 1σ, where 1σ ∼ 167 μJy beam−1. The brightest 20 cm radio continuum source coincides with the optical nucleus. Two other sources at a distance of ∼10″ from the center toward the E and W might be part of a circumnuclear structure. There is weak emission from almost all over the optical disk but no 20 cm radio continuum emission from either the NE or the SW H I 21 cm extended structures (see Figure 11).
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Our low-resolution VLA B-configuration H I 21 cm moment 0 image in gray scale and contours, obtained using a u v range restricted between zero and 5 kλ to search for any H I 21 cm intergalactic extended emission or bridges associated with the disks of NGC 5595 and NGC 5597. Here NGC 5597 is at the SE, and NGC 5595 is at the NW. The gray-scale stretch is 250–450 mJy beam−1 km s−1. The moment 0 contours are at 15, 17, 21, 25, 30, 35, 40, 45, 50, 52, 55, 60, 70, 80, 90, 95, 100, and 108 × 1σ, where 1σ ∼ 19.45 mJy beam−1 km s−1. No intergalactic H I 21 cm structure or filaments exist between the two galaxies. The synthesized beam at FWHM, which is ∼30.″7  ×  28.″8 at P.A. ∼ +50° E of N, is shown in the bottom left corner.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Reproduction of the 103aO blue optical emission of NGC 5595 (Diaz-Hernández et al. 2009) in contours superposed on the H I 21 cm moment 0 image in gray scale. Optical emission is not flux calibrated; its contours are at 4.7, 9, 13, 20, 25, 30, 40, 46, 53, 60, 75, and 92 × 1σ, where 1σ ∼ 90 in arbitrary units proportional to intensity. The gray-scale stretch is from 6.6 to 37 mJy beam−1 km s−1. Notice that the H I 21 cm NE and SW elongated structures do not have optical continuum emission counterparts.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Median composites of the Redrock-identified QSOs from the deep-field VI (blue) and QSOs missed by Redrock but identified from the afterburner approaches in the sparse-field VI (red). The composite spectra are normalized over rest-frame 3800–3900 Å for visualization purposes. The inset plot is focused around 3700–4000 Å to highlight the prominent stellar absorption features in the missed QSO sample. The vertical lines indicate several key emission and absorption features.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption:  r-band magnitude vs. redshift for (left) high-quality Redrock-identified QSOs from the deep-field VI (blue squares) and the missed QSOs in the sparse-field VI (red squares) and (right) high-quality missed QSOs from the sparse VI, split between those with reliable redshifts (dz < 0.01: pink squares) and those with large catastrophic redshift failures (dz > 0.1: maroon squares); we note that missed QSOs with dz = 0.01–0.1 are not plotted in the right-hand panel. The black dashed curve shows the expected track for an M I = −23 mag QSO to provide a basic discrimination between classical QSOs and lower-luminosity Seyfert-type galaxies. The top panels show the redshift distributions for the (left) high-quality Redrock QSOs (blue) and missed QSOs (red) and (right) high-quality missed QSOs with reliable redshifts (pink) and redshift failures (maroon).
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption:  r-band fiber magnitude vs. redshift for (left) the deep-field VI (see Section 2.3.1) and (right) the missed QSOs from the sparse VI (see Section 2.3.2); the redshift is taken from the VI for the high-quality spectra and from Redrock for the low-quality spectra. The target classifications are based on the visually inspected optical spectral type for the high-quality spectra (VI ≥2.5): QSO (blue circle), galaxy (green square), and star (orange star). The low-quality (VI <2.5) identifications are plotted as black triangles. The top panels show the redshift distributions for the high-quality QSOs (blue) and the galaxies (green).
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Pipeline redshift vs. VI redshift for the high-quality missed QSOs from the sparse VI. The plotted pipeline redshifts from (top) the standard Redrock pipeline (blue) and modified pipeline (red) and (bottom) the QuasarNet (magenta) and SQUEzE (yellow) afterburners. We note that all missed QSOs are plotted for the standard and modified pipelines while, for QuasarNet and SQUEzE, only the missed QSOs identified by that afterburner are plotted.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Good-redshift purity vs. r-band magnitude for main-selection targets identified as QSOs by either the standard Redrock pipeline (blue) or the modified pipeline (red) for two dz thresholds in dark-time exposures of ≈1000 s for (left) tracer QSOs and (right) Lyα QSOs. The cumulative fractions are plotted for dz_thresh = 0.0033 and dz_thresh = 0.010; the shaded regions indicate the 1σ uncertainty for a binomial distribution. The dotted horizontal line indicates the DESI scientific requirement.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Median absolute deviation (MAD) of the velocity offsets (Δv) between redshift pairs vs. r-band magnitude for main-selection targets identified as QSOs by either the standard Redrock pipeline (blue) or the modified pipeline (red) in dark-time exposures of ≈1000 s for (left) tracer QSOs and (right) Lyα QSOs. The shaded regions indicate the 1σ uncertainty calculated via bootstrapping the sample 500 times.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Assessment of redshift accuracy (expressed as the velocity offset, dv, in kilometers per second) for main-selection targets with dark-time exposures of ≈1000 s matched to the SDSS DR16 quasar catalog for the standard Redrock pipeline (blue) and the modified pipeline (red). The dotted vertical line indicates the median velocity offset.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Compilation of DESI spectra to illustrate some of the diversity in systems identified in the QSO survey (left) and thumbnail images (18″ × 18″) centered on each target (right). Salient information for each target is plotted at the top of each spectrum including a description of the QSO subtype. For each target, both an unsmoothed (gray) and smoothed (black) spectrum are plotted along with the associated error spectrum (orange). Some of the most prominent emission lines (blue vertical dashed lines) and absorption lines (green vertical dashed lines) are highlighted.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Redshift distributions for high-quality QSOs from the missed QSOs in the sparse VI for (top) Mg II afterburner selected systems, (middle) QN selected systems, and (bottom) SQ selected systems.
Paper: Warm Jupiters Beyond the Tidal Synchronization Limit may Exhibit a Wide Range of Secondary Eclipse Depths
Authors: Emily Rauscher, Nicolas B. Cowan, Rodrigo Luger
Figure caption: To assess the feasibility of measuring seasonal effects on gaseous exoplanets, we compare the parameter space over which tidal forces from the star should have or have not synchronized and aligned a planet’s rotation vector to the regime where a planet’s atmospheric response to a seasonal cycle may be minimal and to expected planet-to-star flux ratios and two different wavelengths. The middle black dashed line marks the boundary where the tidal timescale for a Jupiter analog equals an assumed system age of 4.14 Gyr, so planets to the left of this should be in synchronous and aligned rotation states, while the lines to the left and right of that are for factor of 10 differences in the assumed system age, tidal Q parameter, or initial rotation rate (Equation (1)). The gray region with stellar masses ≲0.6M ⊙ is where Tan (2022) identified weak atmospheric responses to seasonal cycles. The filled color contours show predicted planet-to-star flux ratios (in parts per million) at 10 μm. The white dots represent known gaseous exoplanets within this parameter space, with labels given to those particularly bright planets (K ≤ 8.131) whose estimated tidal timescales are comparable to their system ages (0.25 < age/τ tidal < 2). The best targets to search for seasonal effects are likely planets at or below a solar mass.
Paper: Warm Jupiters Beyond the Tidal Synchronization Limit may Exhibit a Wide Range of Secondary Eclipse Depths
Authors: Emily Rauscher, Nicolas B. Cowan, Rodrigo Luger
Figure caption: Eclipse depths for our hypothetical warm Jupiter, from models with different combinations of rotation rate and obliquity. For each model the eclipse depth depends on the timing of the eclipse relative to the planet’s seasonal cycle. The median value for each model is marked as a line, with the distribution of possible values indicated by the violin plots. Marked as a dashed line is the eclipse depth this planet would have if it had a uniform temperature equal to its zero-albedo equilibrium temperature, from which we can also estimate the depth relative to the stellar flux (in ppm: parts per million) at 10 μm and an early evaluation of the precision of the MIRI instrument on the JWST (from Bouwman et al. 2023) with the error bars. For most rotation rates a nonzero obliquity can cause deviations from the zero-obliquity expectation, ranging from insignificant differences for ψ ≤ 10°, to a 5% effect at ψ = 30° (potentially differentiated by the JWST), to a 15%–20% effect at ψ ≥ 60° (easily differentiated by the JWST). The eclipse depth alone cannot constrain a planet’s rotation rate and obliquity, but if those parameters are otherwise unconstrained, they can induce uncertainty in the interpretation of a measured eclipse depth.
Paper: Warm Jupiters Beyond the Tidal Synchronization Limit may Exhibit a Wide Range of Secondary Eclipse Depths
Authors: Emily Rauscher, Nicolas B. Cowan, Rodrigo Luger
Figure caption: Plots of the coefficients for the uniform disk and second eigencurve components, found from fitting to the 90 simulated secondary eclipse observations for each of the 25 rotation rate/obliquity models. The colors of the points indicate the rotation rate (left) or obliquity (right) of the model. The coefficients indicate the strength of that signal in the observation; on the axes for the histograms we translate this into an rms signal in parts per million, as described in the text. The spatial brightness structure of the planet’s dayside, if it could be measured by eclipse mapping, would constrain the planet’s rotation state.
Paper: Warm Jupiters Beyond the Tidal Synchronization Limit may Exhibit a Wide Range of Secondary Eclipse Depths
Authors: Emily Rauscher, Nicolas B. Cowan, Rodrigo Luger
Figure caption: Estimated timescales for tidal synchronization and alignment (from Equation (1)) vs. orbital period and system age for gaseous exoplanets (R  p  > 0.4R J) with measured masses. No errors are shown, but generally the orbital periods are very well known while the system ages are not (and here are set to 4.14 Gyr if not listed). Particularly bright planets that are near the boundary where tidal timescales equal system ages (0.25 < age/τ tidal < 2) are labeled.
Paper: The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
Authors: David M. Alexander, Tamara M. Davis, E. Chaussidon, V. A. Fawcett, Alma X. Gonzalez-Morales, Ting-Wen Lan, Christophe Yèche, S. Ahlen, J. N. Aguilar, E. Armengaud, S. Bailey, D. Brooks, Z. Cai, R. Canning, A. Carr, S. Chabanier, Marie-Claude Cousinou, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, A. C. Edge, S. Eftekharzadeh, K. Fanning, James Farr, A. Font-Ribera, J. Garcia-Bellido, Lehman Garrison, E. Gaztañaga, Satya Gontcho A Gontcho, C. Gordon, Stefany Guadalupe Medellin Gonzalez, J. Guy, Hiram K. Herrera-Alcantar, L. Jiang, S. Juneau, N. G. Karaçaylı, R. Kehoe, T. Kisner, A. Kovács, M. Landriau, Michael E. Levi, C. Magneville, P. Martini, Aaron M. Meisner, M. Mezcua, R. Miquel, P. Montero Camacho, J. Moustakas, Andrea Muñoz-Gutiérrez, Adam D. Myers, S. Nadathur, L. Napolitano, J. D. Nie, N. Palanque-Delabrouille, Z. Pan, W. J. Percival, I. Pérez-Ràfols, C. Poppett, F. Prada, César Ramírez-Pérez, C. Ravoux, D. J. Rosario, M. Schubnell, Gregory Tarlé, M. Walther, B. Weiner, S. Youles, Zhimin Zhou, H. Zou, Siwei Zou
Figure caption: Examples of systems where two objects are contributing to the DESI optical spectrum (left) and thumbnail images (18″ × 18″) centered on each target (right). Salient information for each target is plotted at the top of each spectrum including a description of the two contributing objects. For each target, both an unsmoothed (gray) and smoothed (black) spectrum are plotted along with the associated error spectrum (orange). All of the plotted spectra are high quality with VI quality flags of 4. Some of the most prominent emission and absorption lines are highlighted using vertical dashed lines and plotted in green (stellar absorption features), blue (QSO emission lines), and orange (galaxy emission lines).