adsabs/AstroCLIMB huggingface dataset:
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: A demonstration of our rescaling of the synthetic solar system catalog S3M to match MPCORB observations at bright magnitudes. All panels compare known objects (from MPCORB) with synthetic objects (from S3M). The left column shows the distribution of apparent magnitude of observations of asteroids for a single representative night of LSST. The top row shows the original S3M distributions and the bottom row shows the distribution after applying our rescaling.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: An example of asteroids detected in a single night of LSST observations. This example has ∼350,000 observed asteroids, of which ∼1000 are NEOs. Gray curve indicates the ecliptic plane.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: A demonstration of the prediction algorithm described in Section 3.2 using 1 yr of simulated observations for both NEOs (top) and MBAs (bottom). Left: probability that an object will be detected within 15 nights, split into a population of objects that are actually detected within 15 nights in the simulated observations and a population that are not. The black dashed line indicates our threshold of 0.8 for submission to the NEOCP. Right: a contingency matrix representing the algorithm’s ability to predict the detectability of an object. The truth columns correspond to whether an object would be successfully followed up by Rubin and the prediction columns correspond to whether the probability predicted by our algorithm surpassed a threshold of 0.8. Lower right quadrants are labeled as “excess NEOCP” given that the objects would be unnecessarily prioritized for external follow-up. Upper right quadrants are labeled “lost objects” since they would be deprioritized for external follow-up, and also not receive adequate follow-up from Rubin. Small annotated values indicate the number of objects that would be followed up by Rubin by the end of the first year of LSST, but after the initial 15 night window.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Traffic (number of objects sent) and purity (fraction of objects sent that are NEOs) of the NEOCP during the first year of LSST if every observation that qualifies for submission and with an apparent magnitude of m < 22 is submitted. Each line is plotted using a rolling window of 10 days to smooth stochastic effects (such that the nightly rate is averaged over all values within 10 nights, excluding nights where no observations took place). Different colors correspond to different constraints on the number of observations for a tracklet to be submitted. In the top panel, solid lines indicate traffic for any magnitude, while dashed lines are limited to mV < 22. Nights on which no observations were taken are highlighted with gray areas.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: The blue curve shows the average nightly traffic of objects with digest2 ≥ 65 and apparent magnitude <​​​​​​22 (left axis) and the purple curve shows the average purity (right axis) for a given latitude cut. Dotted gray lines at particular latitudes are annotated with y-axis values and average apparent magnitudes. Interactive version.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: The digest2 score cannot adequately distinguish NEOs in the presence of a large MBA background. digest2 scores for all NEOs and MBAs observed in the first year of our simulated LSST observations. (a) Normalized histograms of digest2 scores, (b) the same histograms unnormalized, and (c) NEO histogram divided by the sum of the histograms in (b). Note that the latter two panels are on a logarithmic scale.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Nightly NEOCP submission rate as a function of lunation averaged over 2019–2023. Histogram shows 30 equally spaced bins over a full lunation, weighted such that each bin height corresponds approximately to an average nightly submission rate. Illustrations of the moon as a function of lunation are shown along the top axis.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Variant orbits computed for an example NEO in our sample based on a single night of mock LSST observations. The white arrow indicates the initial sight-line for the observation. The blue dotted line indicates the orbit of the Earth. Background stars are for illustrative purposes only.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Apparent magnitude of LSST NEO observations in year 1, split up by whether they are trailed sources.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Total number of submissions to the NEOCP per year since 2002. Annotated lines show the start of operations of significant contributors to the NEOCP.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Apparent magnitude of NEOs and MBAs with a digest2 score ≥ 65 observed in the first year of LSST.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Color–magnitude diagram (left), initial mass–magnitude relation (center), and initial mass–magnitude diagram zoomed-in on the post-AGB phase (right) for an isochrone at a grid point metallicity and halfway between grid points in age. The green line shows an isochrone using the MIST Web interpolator, and the red line is the resulting isochrone from our standard interpolation scheme. For stars beyond the main sequence, this can produce spurious magnitudes and parameters. The blue line shows the isochrone resulting from the CHARONINTERPOLATOR method described in Appendix B. This minimizes spurious output, with a smaller effect only in the post-AGB phase. In the center panel, the dashed, black lines show the isochrones for the assigned metallicity and adjacent age grid points. In the right panel, the dashed, black line marks the end of the AGB for the CHARONINTERPOLATOR isochrone, and the dotted, black lines mark the isochrones for the adjacent grid points following the mass-modification scheme used by the CHARONINTERPOLATOR.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Comparison between the Galactocentric coordinates (black) and Galactic longitude and latitude systems (green). Left: Top view of the Milky Way with Cartesian coordinates. The z-axis points out of the page. Middle: Side view of the Milky Way with Cartesian coordinates. The y-axis points into the page (x0, z0 not to scale). Right: Top view of the Milky Way with cylindrical coordinates. The ﹩\tilde{z}﹩-axis points out of the page. Underlying artist’s concept of Milky Way from NASA / JPL-Caltech / R. Hurt (SSC-Caltech).
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Runtime comparison of SYNTHPOP and GALAXIA. The left panel shows total runtime for a range of field sizes, and the right panel shows number of stars generated per second. In the left panel, the SYNTHPOP values for the star generation process along are shown in orange, with initialization time shown in blue; in the right panel, these colors likewise indicate whether initialization was included in the total runtime. GALAXIA has no separable initialization process and is shown in green.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Distance distribution for the bulge, thin disk, thick disk, and halo stellar populations. The density of all stars generated by the SYNTHPOP model we adopt is shown in gray, reflecting the underlying total stellar density distribution for stars with m > 0.1 M⊙. The green and blue lines indicate the density for all SYNTHPOP stars brighter than 20 mag in the Gaia G-band, with and without renormalization, respectively. The density estimated from the Gaia Universe Model catalog is shown in red.
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Luminosity function for the outer (left) and inner (right) Galactic fields. In green, the stars generated by SYNTHPOP are shown. The back line shows the number of stars in Gaia DR3, and red shows the number of stars in the Gaia Universe Model catalog. The bottom panels give the ratio between the number of stars in SYNTHPOP and the Gaia DR3 (black) and the Gaia Universe Model (red).
Paper: SYNTHPOP: A New Framework for Synthetic Milky Way Population Generation
Authors: Jonas Klüter, Macy J. Huston, Abigail Aronica, Samson A. Johnson, Matthew T. Penny, Marz Newman, Farzaneh Zohrabi, Alison L. Crisp, Allison Chevis
Figure caption: Color–magnitude diagrams for SYNTHPOP, Gaia Universe Model, and Gaia DR3. The top row is in observed magnitudes, and the bottom row is in absolute magnitudes.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Example spectra for eight quiescent galaxies organized by increasing redshift, ranging from z = 1.53 to 1.88, displayed across four rows. Each row is dedicated to galaxies at a specific redshift and features two examples: one with a high S/N and the other with a low S/N. Upper panels: redshift probability distribution, log[P(z)], obtained from initial coarse redshift fitting phase for each target. Middle panels: optimally extracted 1D spectra (gray) derived by combining all exposures of each target and corresponding Grizli best-fit templates (red). Positions of key absorption spectral features, including Ca II HK, Hδ, Hγ, Hβ, Mgb, and NaD, are marked at the best-fit Grizli redshift. The flux unit is in 10−19 erg s−1 cm−2 Å−1. The S/N, true redshift and best-fit redshift are presented in the lower right legend. Lower panels: corresponding direct images and simulated 2D G150 spectra (PA = 0∘).
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Efficiency of redshift recovery by galaxy magnitude in F158 across 36 simulated grism images with different exposure times. These simulations assume that objects are observed in all eight exposures. The left axis indicates redshift completeness, representing the percentage of galaxies in each magnitude bin meeting specific criteria: (1) redshift accuracy with ﹩{\sigma }_{z}=\left|{\rm{\Delta }}z/(1+z)\right|\,\leqslant \,0.01﹩; (2) S/N ≥ 5; and (3) presence of a singular peak in the redshift PDF. The histogram in the background illustrates the distribution of galaxy magnitudes among the simulated sample, with the number of galaxies displayed on the right axis. Data points reflect the observed redshift completeness, with various colors denoting different exposure times as detailed in the legend. Solid lines represent logistic regression models, ﹩f(x)=\frac{1}{1+\exp (-k* (x-{x}_{0}))}﹩, fitted to the observed redshift completeness data.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Top panel: redshift completeness, defined as the fraction of quiescent galaxies with reliable redshift estimates (single dominant peak in P(z)) and small residuals (σz ≤ 0.02) vs. S/N for quiescent sources in the simulation. The red dashed line indicates the S/N threshold of 5, beyond which 90% completeness is achieved. Bottom panel: F158-band magnitude as a function of S/N for the quiescent galaxy sample in the simulation.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Comparison of true redshifts vs. measured redshifts using Grizli (left panel) and Bagpipes (right panel) for all quiescent galaxies with a S/N greater than 5 in the simulation. The bottom panels show the residuals, defined as (zfit − ztrue)/(1 + ztrue) as a function of true redshift. Note that the plotting range for the residual plots has been adjusted to better highlight the residuals, resulting in the exclusion of outliers from the upper panels.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: A single 2D cutout region of the source in one position angle (PA = 0°). The target galaxy is shown in the upper left. Top panel: cutout region of the simulated Roman grism images centered on the source. Middle panel: contamination model obtained by iteratively fitting polynomial spectral templates to the grism spectra of all objects in the field. Bottom panel: cleaned science image, on which the redshift fitting is performed, after subtracting the contamination model.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Residuals (z-ztrue)/(1+ztrue) vs. S/N (upper panel) and true redshift (lower panel) based on standard exposure time in HLSS, assuming objects are covered in all eight exposures. The orange shaded region shows the ±1σ region of the redisduals. All galaxies satisfying selection threshold are shown.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Same plot as Figure 7 but for different number of available exposures.
Paper: Search for the True Parent Body of the Phoenicid Meteor Shower
Authors: Martina Kováčová, Luboš Neslušan, Dušan Tomko
Figure caption: The evolution of the perihelion distance, q (panels (a), (c), and (e)), and inclination, i ((b), (d), and (f)), of 100 cloned orbits of each of comets 46P/Wirtanen ((a), (b)), 104P/Kowal 2 ((c), (d)), and 289P/Blanpain ((e), (f)) during the last millennium. The density of the cloned orbits in the given q- or i-space is shown in the color scale. The behavior of given element of nominal orbit is shown with the black curve. Notice the different vertical scale.
Paper: Search for the True Parent Body of the Phoenicid Meteor Shower
Authors: Martina Kováčová, Luboš Neslušan, Dušan Tomko
Figure caption: The dependence of the Southworth–Hawkins D discriminant, calculated between the predicted southern filaments of three studied comets and mean orbit of Phoenicid and M2023-Y1 showers, on the serial number of filaments, when these are arranged in order of increasing DSH. The dependence for the Phoenicid shower with AdNo = 0 (AdNo = 1) is shown in panels (a) and (b) and that for M2023-Y1 in panel (c).
Paper: Search for the True Parent Body of the Phoenicid Meteor Shower
Authors: Martina Kováčová, Luboš Neslušan, Dušan Tomko
Figure caption: The evolution of the perihelion distance (panels (a), (c), and (e)) and inclination ((b), (d), and (f)) of the nominal orbits of comets 46P/Wirtanen (a, b), 104P/Kowal 2 ((c), (d)), and 289P/Blanpain ((e), (f)). The numerical integration was performed by using the Runge–Kutta integration method (thick red curve), Leap-Frog integrator (LF, thin green curve), and Gauss–Radau or RA15 integrator (RA15, purple curve). Notice the different vertical scale.
Paper: Search for the True Parent Body of the Phoenicid Meteor Shower
Authors: Martina Kováčová, Luboš Neslušan, Dušan Tomko
Figure caption: The positions of the mean radiant of two solutions of shower #254 (red asterisks) and shower M2023-Y1 (purple asterisk) on sky.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Integrated spectrum of the central 5′ × 6′ region of the Orion Nebula (black solid line), together with the best-fitted stellar model (red solid line), the model of the strongest emission lines fitted with Gaussian functions (blue solid line), the residual after subtraction of the stellar model (cyan solid line), and the combination of both models, including a final correction to the shape of the residual (yellow solid line). The first three panels from top to bottom present the wavelength ranges covered by the blue (first row), green (second row), and infrared (third row) arms that comprise the LVM spectrograph. Shaded regions correspond to the overlapping regimes between them. Like in the case of Figures 5 and 6, the insets in the two bottom rows show a set of zoom-in views at certain particular wavelength ranges. The panels in the fourth row illustrate the quality of the modeling of the strongest emission lines, including the same lines already shown in Figures 5 and 6. Finally, the last row of panels includes three wavelength ranges (3651–3726 Å, 4801–4999 Å, and 8151–8299 Å) that illustrate certain particularities of the spectrum discussed in the text. Three additional panels present a zoom-in look around the three auroral lines most frequently used to determine the electron temperature in ionized nebulae: [O III] λ4363, [N II] λ5755, and [S III] λ6312. The flux ranges in these three last insets are the same to facilitate the comparison between the lines. In the particular case of this very deep spectrum, all three are clearly detected.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Spatial distribution of fluxes recovered by the DAP of the [O III] λ5007 (blue), Hα (green), and [N II] λ6583 (red) emission lines for the combination of unsaturated pointings covering the central region of the Orion Nebula described in the text, using an arbitrary scale to enhance the contrast. The approximate location of the slit spectroscopy data presented by O92 and B00, and the IFS data presented by S07 are indicated with a red and blue line and a cyan polygon, respectively. The black circle corresponds to the location from which we have extracted the integrated spectrum discussed in the text.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Comparison between the simulated (blue contours) and recovered (red contours) PDF of the physical properties of stars (Teff, log(g), [Fe/H], and [α/Fe]) derived for one of the 1700 simulations generated by mixing randomly the spectra of 5 stars within the RSP template comprising 1253 stars with an average S/N ∼ 20. The black contours in each panel, the meaning of each contour, and the distribution of panels are similar to those shown in Figure 9.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Comparison between the recovered and simulated stellar physical parameters (Teff: top left; log(g): top right; [Fe/H]: bottom left; and [α/Fe]: bottom right) using LVM-DAP for a set of 1700 realistic simulations in which a number of stars between 5 and 125 was assumed. Contours, symbols, and lines in each panel have the same meaning as those in Figure 7.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Example of the analysis performed by LVM-DAP to recover the properties of the ionized gas emission lines. Each panel shows the distribution across the FOV of the LVM IFU of the flux intensity estimated by the weighted-moment procedure for the 20 brightest emission lines in the integrated spectrum (Figure 15), extracted from the combined frame centered in the core of the Orion Nebula discussed in the text. The emission lines are ordered from the brightest (top left) to the faintest (bottom right). The legend in each panel indicates the represented emission line.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Normalized histograms of the distribution of S/N ratios (top panels) and cumulative distributions (bottom panels) for three representative emission lines (Hα: black; [O III] λ5007: blue; and [N II] λ5755: cyan) and the stellar continuum around ∼5000 Å (red) for ∼seven million individual LVM fiber spectra (left panels) and ∼4000 spectra integrating each LVM pointing (right panels). The x-axis is shown on a logarithmic scale for a better visualization of the distributions.