adsabs/AstroCLIMB huggingface dataset:
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: PV diagram generated using 13CO emission, along the path (red vectors) overlaid in Figure 8 for the southern molecular structure. In the direction of location S2 (see Figure 8), at least two velocity peaks are seen, which are highlighted by straight orange lines.
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: m-0, m-1, and line-width maps (column-wise) for 12CO (J = 1 − 0) and 13CO (J = 1 − 0) emission, respectively, in the velocity range [−4, 6] km s−1 for IRAS 05331+3115. The emission is depicted above the 5σ value (σ being the rms noise for respective spectral cubes).
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Upper left panel: Color-composite image (red: WISE 12 μm; green: Spitzer 3.6 μm, and Blue: 2MASS K-band 2.17 μm) of the region overlaid with the locations of identified YSOs (Class I (yellow asterisk) and Class II (green asterisk)). Upper right panel: Representation of MST connections in the cluster (orange) and core (purple) along with the locations of identified YSOs (orange asterisks for the YSOs in the cores and purple asterisks for the locations of YSOs in clusters). The extracted clusters/cores are also enclosed by the Convex hulls using yellow and purple line segments, respectively. Black asterisks also mark the locations of all the identified YSOs. Lower left panel: Surface density map of all stellar sources. Lower right panel: Extinction map overlaid with the locations of identified YSOs (Class I (yellow asterisk) and Class II (green asterisk)). The lowest contour level for the generation of the surface density map is 1 YSO arcmin−2 with a step size of 29.5 stars arcmin−2, whereas for the extinction map, it is 2.7 mag with a step size of 1.92 mag.
Paper: Investigating the Star-forming Sites in the Outer Galactic Arm
Authors: Aayushi Verma, Saurabh Sharma, Lokesh K. Dewangan, Devendra K. Ojha, Kshitiz Mallick, Ram Kesh Yadav, Harmeen Kaur, Tarak Chand, Mamta, Archana Gupta
Figure caption: Panel (a): J vs. (J − H) CMD generated using the NIR catalog for the stars within the AFGL 5157 region. The red solid curve defines the ZAMS isochrone by Pecaut & Mamajek (2013), corrected for the distance of 1.6 kpc and A  V  = 2.24 mag. Panel (b): J vs. (J − H) CMD for the stars within the FSR0807 cluster. The red solid curve defines the ZAMS isochrone by Pecaut & Mamajek (2013), corrected for the distance of 1.6 kpc and zero-reddening. Panel (c): J vs. (J − H) CMD for the stars within the KPS0620 cluster. The red solid curve defines the ZAMS isochrone by Pecaut & Mamajek (2013), corrected for the distance of 3.26 kpc and A  V  = 2.56 mag. Panel (d): J vs. (J − H) CMD for the stars within the IRAS 05331+3115 cluster. The red solid curve defines the ZAMS isochrone by Pecaut & Mamajek (2013), corrected for the distance of 3.26 kpc and A  V  = 3.20 mag. The YSOs and Gaia DR3 members are marked in all the panels with magenta asterisks and green circles, respectively. Due to less detection of optical clustering, the Gaia members are not marked for KPS0620 and IRAS 05331+3115.
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption: Phase-folded Gaia G, G RP, and G BP photometry of Gaia DR3 4042390512917208960. The smooth sinusoidal modulation is evident in all colors.
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption: Phase-folded OGLE I-band photometry. The same shape can be seen as in Figure 1.
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption: Comparison of PHOENIX template (T eff = 6700 K, ﹩\mathrm{log}g=4.0﹩) spectrum with the shifted and averaged spectrum of all observations of Gaia DR3 4042390512917208960. The left, middle, and right panels are cutouts around Hγ, Hβ, and Hα, respectively. Broadly, there is good agreement between the synthetic PHOENIX spectrum and the averaged observed spectrum. Note that the depth of the Hα line is much shallower in the observed spectrum.
Paper: A Contact Binary Misclassified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches
Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader
Figure caption: Comparison of PHOENIX template (T eff = 6700 K, ﹩\mathrm{log}g=4.0﹩) spectrum with the shifted and averaged spectrum of all observations of Gaia DR3 4042390512917208960 in the regions used with FXCOR. The shaded regions indicate sections of the spectra that were excluded from the cross-correlation. Note that while we exclude Hγ and Hβ, the region includes prominent lines from many atomic species (e.g., Fe, Ca, Na, and Mg).
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: NSC stellar mass vs. host galaxy halo mass in the same format as in Figure 12. We find ﹩{M}_{\mathrm{NSC}}/{M}_{\odot }={10}^{6.11\pm 0.05}{({M}_{h,\mathrm{gal}}/{10}^{10}{M}_{\odot })}^{0.92\pm 0.05}﹩ with 0.32 dex scatter.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: The deviation from the M NSC–M  h,gal relation (Figure 13) and the stellar mass fraction. Galaxies above the best-fit line in Figure 13 tend to have a higher stellar mass fraction. The p-value from the Spearman rank correlation test is 3.28 × 10–10.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: The correlation matrix displays the parameters analyzed for the NSC occupation fraction. The values within each cell represent the p-values obtained from the Spearman rank correlation test. We display only the cells where the p-value is less than 0.01.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: NSC color vs. galaxy magnitude diagram in the same format as Figure 4. Markers with a black edge show the NSC color as a function of the absolute magnitude of the host galaxy. For a comparison, we plot the ordinary color–magnitude diagram with small circles.
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: (a) The period distribution of the 92 LMRs from CSS and the 98 LMRs from ASAS-3. (b–d) Dependence of T 1 on q, M 1, and M tot respectively, for the sample of 317 LMRs (cyan) and the 253 well-studied EWs (Latković & Čeki 2021; purple). The upper panel in each plot represents the corresponding distributions of T 1 for the two samples whereas the right-hand histograms in (c) and (d) represent the distribution of M 1 and M tot, respectively, for the two samples.
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: Contour plots of ﹩\mathrm{log}{\chi }^{2}﹩ (color coded according to the scale on the right) on the (q, ﹩\sin i﹩) plane as resulted from the q − i scan using the CSS LC. The white crosses represent the solutions of the systems with the error bars derived from the MC and heuristic scanning, respectively. The size of the error bars is drawn according to the errors.
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: (a) The mass distribution of the progenitors of the initial massive component (M 2i) and (b) the distribution of the initial mass ratio (1/q i) of the progenitors of LMRs from CSS and Yildiz & Doğan (2013) and EWs with q > 0.25 from the latter.
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: (a) The mean density of the primary component ρ 1(ρ ☉) as a function of period and fill-out factor f. (b) The mass ratio q as a function of fill-out factor f and the ratio of densities ρ 2/ρ 1. (c) The ratio of densities ρ 2/ρ 1 of the components as a function of mass ratio q and fill-out factor f. Color coded according to the scale on the right.
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: The observed LCs (black points) from CSS and the best-fitted models (red lines) for the nine LMR systems.
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: Same as Figure 3 but for J210228 (upper panel) and J231513 (lower panel) using CSS (left) and new BVRI observations (right).
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: The distributions of (a) q, (b) f, (c) M 1, and (d) T 1 of the 92 CSS LMRs.
Paper: A Study of Nine Extremely Low Mass Ratio-contact Binary Systems
Authors: Eleni Lalounta, Panagiota-Eleftheria Christopoulou, Athanasios Papageorgiou, C. E. Ferreira Lopes, Márcio Catelan
Figure caption: Phase-folded BVRI (left) and VRI (right) observations for J210228 and J231513, respectively, with their models (black line).
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: CMD for the star cluster population around NGC 1275. No correction has been made for foreground reddening. The relatively sharp cutoff of the data at the faint end represents SNR = 4. The second and third panels show the CMD for inner and outer radial zones: in the inner zone, the bluer clusters with (F485W-F814W) ≲1.2 are relatively more prominent, and the limiting magnitude of the photometry is brighter.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption:  Upper panel: Comparison of completeness fraction plotted vs. either the measured magnitudes (black line) or the input magnitudes (red line). See the text for the exact definitions of each fraction. The dashed red line shows the best-fit sigmoid function fit to the binned f vs. the input magnitude. Lower panel: Fractional excess of recovered stars for each bin, gained at the expense of other bins: see text for explanation.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Completeness as a function of magnitude for the artificial stars in four radial zones around NGC 1275, for the AST data binned in 0.2 mag steps. Solid lines show the results for the exponentially rising input LF, while the dashed lines show the results for the flat input LF. Black lines are for radial zone 1 (r < 20″), blue for zone 2 (20″ − 40″), green for zone 3 (40″ − 60″), and red for zone 4 (r > 60″). Zone 1 is heavily affected by background sky noise in the central bulge of the galaxy, reducing the completeness fraction even for relatively bright objects. Note that at brighter magnitudes, the curves for the rising LF are statistically noisier because the numbers of input stars are smaller than for the flat LF.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Dependence of local crowding level on galactocentric radius R  gc  (arcmin), for all measured stars in the NGC 3377 field. The crowding density parameter x 4 is defined as the local mean surface brightness in the image around each object after background subtraction, as described in the text. The trend follows a simple power-law form x 4 ∼ R −2.38 shown by the magenta line and is equivalent to the surface brightness profile of the galaxy. The “spikes” of points extending upward from the main locus represent objects near small satellites or background galaxies, or bright stars, where the local background light is enhanced. The sparse dusting of points below the main locus shows objects near the CCD detector edges.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: CMDs for the NGC 3377 halo, in four different zones of projected galactocentric radius R  gc . The innermost edge of the ACS field is at ﹩1.6^{\prime} ﹩ from the galaxy center.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Standard deviation of local sky noise plotted vs. galactocentric radius, for the measured objects around NGC 1275. Here σ  sky  in adu is measured on the F814W reference image within an annulus of 4 to 9 px around each object. Note the “spikes” of higher noise at large radii where satellite galaxies are located.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Portion of the field in the halo of NGC 3377, imaged with HST/ACS. The field shown is 55″ across (about one-quarter of the width of the ACS field of view), corresponding to a linear distance of 3 kpc. Large numbers of halo red-giant stars are scattered across the image; the galaxy center is off the field to the lower right. See also Figures 1 and 2 of Harris et al. (2007).
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: LFs for the two sets of ASTs run on the NGC 1275 images. The first set (blue) assumes a flat LF while the second set (magenta) assumes an exponentially rising LF toward fainter magnitudes. The vertical dashed line indicates the magnitude level at which the recovery fraction is approximately 50% depending on radial zone and color (see text for additional details).
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: CMD in F814W vs. F475W−F814W for artificial stars following the exponentially rising LF. Left panel: Input magnitudes and colors of the artificial stars. Right panel: Measured values for stars that were successfully recovered (i.e., were detected and passed the culling tests).
Paper: Discovery of the Remarkably Red L/T Transition Object VHS J183135.58-551355.9
Authors: Thomas P. Bickle, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Austin Rothermich, Johanna M. Vos, Genaro Suárez, J. Davy Kirkpatrick, Aaron M. Meisner, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, Sarah L. Casewell, Dan Caselden, Daniella C. Bardalez Gagliuffi
Figure caption: Left: smoothed Magellan/FIRE spectrum of VHS J1831−5513 (black) compared to the spectral standards (red, labeled) 2MASS J08251968+2115521 (L7) from Cruz et al. (2018), 2MASS J16322911+1904407 (L8) and 2MASS J02550357−4700509 (L9) from Kirkpatrick et al. (2010), and SDSS J120747.17+024424.8 (T0) and SDSS J083717.21−000018.0 (T1) from Burgasser et al. (2006). Right: VHS J1831−5513 compared to the young, planetary-mass objects WISEA J1147−2040 (Schneider et al. 2016), PSO J318.5−22 (Liu et al. 2013), and CWISE J0506+0738 (Schneider et al. 2023a). All spectra are normalized between 1.27 and 1.29 μm.
Paper: Discovery of the Remarkably Red L/T Transition Object VHS J183135.58-551355.9
Authors: Thomas P. Bickle, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Austin Rothermich, Johanna M. Vos, Genaro Suárez, J. Davy Kirkpatrick, Aaron M. Meisner, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, Sarah L. Casewell, Dan Caselden, Daniella C. Bardalez Gagliuffi
Figure caption: Color–color diagrams comparing VHS J1831−5513 (blue square) to L and T dwarfs with photometry from Schneider et al. (2023b; yellow to red circles) and CWISE J0506+0738 (green diamond; Schneider et al. 2023a). VHS J1831−5513 is plotted using its VHS and CatWISE photometry, and represents a significant outlier from even the reddest known objects. The blue lines in the left and right plots indicate the synthetic J − K S color calculated from the Magellan/FIRE spectrum of VHS J1831−5513, which is still an outlier from the bulk of the brown dwarf population, but is similar to that of CWISE J0506+0738, the reddest known L/T transition dwarf.
Paper: Discovery of the Remarkably Red L/T Transition Object VHS J183135.58-551355.9
Authors: Thomas P. Bickle, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Austin Rothermich, Johanna M. Vos, Genaro Suárez, J. Davy Kirkpatrick, Aaron M. Meisner, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, Sarah L. Casewell, Dan Caselden, Daniella C. Bardalez Gagliuffi
Figure caption: Left: comparison between the H (top) and K (bottom) bands of VHS J1831−5513 (black, smoothed; gray, original resolution) and the young, planetary-mass companion VHS 1256–1257 b (red; Miles et al. 2023). CH4 absorption features that appear in both objects are marked by blue bands. Right: Sonora Bobcat (Marley et al. 2021) models at solar metallicity and log(g) = 3.5, with a range of effective temperatures. The blue bands represent the locations of the absorption features in the corresponding band of the left column.
Paper: Discovery of the Remarkably Red L/T Transition Object VHS J183135.58-551355.9
Authors: Thomas P. Bickle, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Austin Rothermich, Johanna M. Vos, Genaro Suárez, J. Davy Kirkpatrick, Aaron M. Meisner, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, Sarah L. Casewell, Dan Caselden, Daniella C. Bardalez Gagliuffi
Figure caption: Magellan/FIRE spectrum of VHS J1831−5513 (black), Gaussian smoothed using a width of 15 pixels. Key molecular absorption features are labeled. Original resolution data are plotted in gray and flux uncertainty is shown in blue.(The data used to create this figure are available in the                    .)
Paper: The Solar System Notification Alert Processing System (SNAPS): Asteroid Population Outlier Detection
Authors: Michael Gowanlock, David E. Trilling, Daniel Kramer, Maria Chernyavskaya, Andrew McNeill
Figure caption: The distribution of ϵ select values for the number of neighbors metric across all 32,752 feature spaces (Section 3.3). Because the ϵ values can vary significantly between feature spaces, where ϵ tends to increase with dimensionality, we show the index j of the selected value of ϵ  j  ∈ G, denoted as arg(ϵ select).
Paper: The Solar System Notification Alert Processing System (SNAPS): Asteroid Population Outlier Detection
Authors: Michael Gowanlock, David E. Trilling, Daniel Kramer, Maria Chernyavskaya, Andrew McNeill
Figure caption: Illustrative example of a d = 2 feature space comparing outlier detection approaches for (a) DSSJ with ϵ = 0.67 and (b) a graphic representation of k NNSJ with k = 3. (a) The points are shown as black dots, where a fixed radius is drawn around each point. (b) The k NN graph is shown where a directed edge between two nodes denotes the k = 3 neighbors for each point. Since k = 3 and there are 10 points, there are a total of 30 directed edges. Colors are used to improve readability in both subfigures. The DSSJ and k NNSJ approaches will be described in greater detail in Sections 3.5–3.7.
Paper: The Solar System Notification Alert Processing System (SNAPS): Asteroid Population Outlier Detection
Authors: Michael Gowanlock, David E. Trilling, Daniel Kramer, Maria Chernyavskaya, Andrew McNeill
Figure caption: Example plots showing computing the best value of ϵ on an example d = 5 feature space, which are the first five features in Table 1. U min (U max) refers to the fraction (f) of the top-n objects that are in both ranked lists for ϵ = 0.0360 (ϵ = 0.1707) and the ϵ values on the horizontal axis. The value of ϵ select is shown as the vertical dotted line for (a) the number of neighbors metric (distance-oblivious), and (b) the mean distance metric (distance-aware).
Paper: The Solar System Notification Alert Processing System (SNAPS): Asteroid Population Outlier Detection
Authors: Michael Gowanlock, David E. Trilling, Daniel Kramer, Maria Chernyavskaya, Andrew McNeill
Figure caption: Illustration of several result sets for query point q in a d = 2 feature space, where data points are shown as black dots and q is shown as the red dot. Three evenly spaced search distances are shown (ϵ 1, ϵ 2, and ϵ 3), which are illustrated as circles centered on query point q. The result sets (A) are as follows: A(ϵ 1) = {2, 3, 6}; A(ϵ 2) = {1, 4, 5} ∪ A(ϵ 1); and A(ϵ 3) = {7, 8} ∪ A(ϵ 1) ∪ A(ϵ 2). Points 9 and 10 are not within any of the result sets. Thus, the result sets for ϵ 1 and ϵ 2 can be directly derived from that of ϵ 3.
Paper: The Solar System Notification Alert Processing System (SNAPS): Asteroid Population Outlier Detection
Authors: Michael Gowanlock, David E. Trilling, Daniel Kramer, Maria Chernyavskaya, Andrew McNeill
Figure caption: Example plots showing the computation of the best value of k using ﹩{k}_{{\rm{\min }}}=2﹩ and ﹩{k}_{{\rm{\max }}}=4096﹩ on the same feature space shown in Figure 2. U min (U max) refers to the fraction (f) of the top-n objects that are in both ranked lists for k = 2 (k = 4096) and the k values on the horizontal axis. The value of k select is shown as the vertical dotted line for (a) the in-degree metric (distance-oblivious), and (b) the mean distance to each point’s k neighbors (distance-aware).