adsabs/AstroCLIMB huggingface dataset:
Paper: Lux: A Generative, Multioutput, Latent-variable Model for Astronomical Data with Noisy Labels
Authors: Danny Horta, Adrian M. Price-Whelan, David W. Hogg, Melissa K. Ness, Andrew R. Casey
Figure caption: The Lux model label precision as a function of SNR for effective temperature (left), surface gravity (middle), and element abundance ratios (right). The median (solid) and (16th and 84th) interquartile range (shaded) are computed by imputing 10 realizations of each stellar label for 2000 randomly selected stars from the high-SNR field RGB-test and low-SNR field RGB-test sets; this is accomplished by sampling 10 realizations of the spectrum of these 2000 stars and using these stellar fluxes to infer 10 realizations of the latent representations for each star (see text in Section 4.6 for further details). Overall, the precision on the Lux model is quite remarkable for all stellar labels examined, even at low SNR. This test illustrates how precisely Lux is able to infer stellar labels for APOGEE stars across SNR. In each panel we also show as vertical dotted lines the average SNR expected for some large-scale stellar surveys of interest.
Paper: Lux: A Generative, Multioutput, Latent-variable Model for Astronomical Data with Noisy Labels
Authors: Danny Horta, Adrian M. Price-Whelan, David W. Hogg, Melissa K. Ness, Andrew R. Casey
Figure caption: Replica of Figure 9 but for high-SNR RGB (triangles), dwarf (squares), and other (star symbol) stars from the high-SNR field all-test sample. The Lux model used to infer these labels was trained on the high-SNR field all-train sample. The Lux labels shown are determined by optimizing the test set latent representations using each star’s spectral fluxes. Overall, the RMSE values obtained are reasonably low and the bias values are smaller than the average ASPCAP uncertainty, indicating that the Lux model is able to infer stellar labels accurately for samples including all stellar types. See text in Section 4.8 for further details.
Paper: Lux: A Generative, Multioutput, Latent-variable Model for Astronomical Data with Noisy Labels
Authors: Danny Horta, Adrian M. Price-Whelan, David W. Hogg, Melissa K. Ness, Andrew R. Casey
Figure caption: Replica of Figure 9 but for OC stars in the high-SNR OC RGB-test set. The Lux labels are determined by optimizing the test set latent representations using each star’s spectral fluxes. Overall, the RMSE values obtained are low and the bias values are smaller than the average ASPCAP uncertainty, indicating that the Lux model is able to infer stellar labels accurately for benchmark stars in OCs. See text in Section 4.7 for further details.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Planet mass and density. The color of the points represent the planets’ equilibrium temperatures, with darker colors representing higher temperatures. Small points indicate the known population, with errorbars omitted for visual clarity. The large stars show the nine planets from this work. The “puffy” exoplanets discussed in Section 5 are circled for reference.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Global fit for WASP 188 b. Photometric lightcurves have been offset, and the TESS-SPOC lightcurves for Sectors 40, 53, and 54 are combined in the final plot for visual clarity. The KeplerCam and MuSCAT2 data shown here are binned to a 2 minute cadence, which was used when fitting the model.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Final joint transit model fit for WASP-195 b. TESS Sectors 50 and 52 are shown together, and all lightcurves are offset for clarity.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Planet period and radius. Gray points show the known planet population, while red stars show the nine new planets presented here.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Final joint transit model fit for WASP-194 b. Photometric observations have been offset, and the eight TESS sectors of observations are combined for clarity.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Final joint transit model fit for WASP-197 b. WASP and TESS lightcurves are offset for clarity.
Paper: Detection of an Explosive Outflow in G34.26+0.15
Authors: Namitha Issac, Xing Lu, Tie Liu, Luis A. Zapata, Hong-Li Liu, Anandmayee Tej, Yan-Kun Zhang, Wenyu Jiao, Suinan Zhang
Figure caption: (a) The 1.3 mm continuum map of G34 is depicted in the color scale. The peak position of HMC is marked with a “×.” The contours of the 3.6 cm emission is overlaid in black with contour levels 5, 50, 100, 200, 400, 800, 1200 times σ (σ = 0.2 mJy beam−1). The two HC H II regions, A and B, and the UC H II region, C are indicated by “+.” The arrow indicates the direction toward the shell-like H II region, D. The beams of the 1.3 mm and 3.6 cm continuum are shown at the bottom-right and bottom-left corners, respectively. (b) SiO(5–4) moment-one map of G34 within the velocity range 0 to 120 km s−1 overlaid with the receding (red curves) and approaching (blue curves) CO(2–1) outflow streamers identified. The contours of the 1.3 mm emission is also overlaid in gray with contour levels 10, 80, 160, 320, and 640 times σ (σ = 0.5 mJy beam−1). The positions of the HMC and the UC H II region are marked with “×” and “+,” respectively. A portion of the H II region, D is depicted by the dashed ellipse. The beam of the SiO(5–4) cube is shown at the bottom-left corner. The green box denotes the field-of-view of (a). (c) Two-color-composite moment-zero maps of CO(2–1) integrated over the velocity ranges 0–48 km s−1 (blue) and 68–120 km s−1 (red). The redshifted and blueshifted outflow streamers are show in pink and cyan, respectively.
Paper: Detection of an Explosive Outflow in G34.26+0.15
Authors: Namitha Issac, Xing Lu, Tie Liu, Luis A. Zapata, Hong-Li Liu, Anandmayee Tej, Yan-Kun Zhang, Wenyu Jiao, Suinan Zhang
Figure caption: (a) Color-composite image of G34 from IRAC 3.6 μm (blue), 4.5 μm (green), and 8.0 μm bands. (b) IRAC [4.5]/[3.6] flux ratio map with contour levels 1.5, 2.0, and 2.5. The image is smoothed to 3 pixels to improve the contrast against the background. The H2 jets identified from both these images are depicted by the dashed lines. The redshifted and blueshifted CO outflow streamers are also overlaid. The hollow star and triangle mark the positions of the UC H II region and the possible origin of the outflow, respectively.
Paper: Detection of an Explosive Outflow in G34.26+0.15
Authors: Namitha Issac, Xing Lu, Tie Liu, Luis A. Zapata, Hong-Li Liu, Anandmayee Tej, Yan-Kun Zhang, Wenyu Jiao, Suinan Zhang
Figure caption: Position–velocity diagram of the outflow streamers identified toward G34. Each streamer identified is designated a different color and labeled as RF1-RF9 and BF1-BF9 for the red and blueshifted streamers, respectively. The gray lines indicate the linear trend between the projected distance and radial velocity starting from the projected distance of 0″ corresponding to the origin of the outflow and 58 km s−1, the systemic velocity G34. The shaded portion indicates the region where the emission is contaminated by the ambient cloud.
Paper: Detection of an Explosive Outflow in G34.26+0.15
Authors: Namitha Issac, Xing Lu, Tie Liu, Luis A. Zapata, Hong-Li Liu, Anandmayee Tej, Yan-Kun Zhang, Wenyu Jiao, Suinan Zhang
Figure caption: The 850 μm Stokes I map of the region surrounding G34 from JCMT SCUBA-2/POL-2 with contour levels 5, 10, 25, 65, 100, 200, and 500 σ (σ = 0.04 Jy beam−1). The purple line segments represent the magnetic-field direction as inferred from the polarization data. The redshifted and blueshifted CO outflow streamers (red and blue curves) and the H2 jets identified from Figure 3 (dashed lines) are also overlaid. The hollow star and triangle mark the positions of the UC H II region and the possible origin of the outflow, respectively. The beam is shown on the bottom-left corner.
Paper: Detection of an Explosive Outflow in G34.26+0.15
Authors: Namitha Issac, Xing Lu, Tie Liu, Luis A. Zapata, Hong-Li Liu, Anandmayee Tej, Yan-Kun Zhang, Wenyu Jiao, Suinan Zhang
Figure caption: Redshifted (a) and blueshifted (b) CO(2–1) condensations detected in each CO(2–1) velocity channel toward G34. The velocity of the redshifted emission ranges from 68 to 120 km s−1 and of the blueshifted emission from 0 to 48 km s−1. The median position of the intersection points of the outflows which is the possible origin of the outflow is indicated by the brown triangle. The position of the UC H II region is denoted by the black star. The red and blue dotted lines in (a) and (b), respectively show the different orientations of the streamers with respect to the origin of the outflow.
Paper: Detection of an Explosive Outflow in G34.26+0.15
Authors: Namitha Issac, Xing Lu, Tie Liu, Luis A. Zapata, Hong-Li Liu, Anandmayee Tej, Yan-Kun Zhang, Wenyu Jiao, Suinan Zhang
Figure caption: The ALMA 12CO(2–1) channel maps from in the velocity range 0–50 km s−1 (left) and 70–120 km s−1 (right) toward G34. The CO condensations in each channel having a nearly linear structure with velocity increment are identified as the outflow streamers.
Paper: Detection of an Explosive Outflow in G34.26+0.15
Authors: Namitha Issac, Xing Lu, Tie Liu, Luis A. Zapata, Hong-Li Liu, Anandmayee Tej, Yan-Kun Zhang, Wenyu Jiao, Suinan Zhang
Figure caption: The angle difference between of the magnetic-field lines (θB) and the H2 jet direction (θjet) along each H2 jet identified in G34.
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: Results of the simultaneous MCMC on the white transit-only light curves of the NRS1 (left panels) and NRS2 (right panels) detectors. The shaded blue regions indicate the times of ingress and egress calculated according to J. N. Winn (2010). Top panels: the black circles show the data and the orange lines show the model light curves applying the ML set of parameters. The faint yellow lines show models calculated using 100 random draws from the final parameter samples. Bottom panels: the relative residuals between the data and the ML model are shown as black circles with the error bars of the data propagated onto the relative residuals. The residuals binned to a lower resolution in time are plotted using red solid lines.
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: Posterior probabilities for the fit parameters of the simultaneous fit to both detectors’ white light curves. For a description of each parameter, see Table 1.
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: Models of the ejection velocity of dust from 289P as a function of particle radius. The SSA model (blue curve) and the Whipple model (red curve) are compared. The blue circle marks the particle radius ad = 1 mm and the velocity vd = 0.5 m s−1 determined by the 1956 Phoenicids studies (Section 3.2). The black symbol indicates ad = 2.3 μm and vd < 48 m s−1 limited by the FWHM of 289P in the W2 band (Section 3.1).
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: The left panel shows W1-band photometry of 289P in Visit A (MJD 58786: UT 2019 October 30, inbound), phased to the two-peaked period Prot = 14.8224 ± 2.9899 hr ≈ 15 ± 3 hr. The blue curve displays the fitting result has an amplitude ~ 1.3 mag. The right panel shows spectral analysis curves for the data. The maxima at Prot = 0.6176 days (=14.8224 hr) is taken as the best solution. The significance level is ~45%.
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: Phoenicid stream mass is plotted as a function of the differential power-law index, γ, as a blue solid line (γ ≠ 3.0 and 4.0 in Equation (13)). The possible stream mass range (Ms), based on the nucleus mass (Mn; D. Jewitt 2006) and the estimated stream mass (~1011 kg; P. Jenniskens & E. Lyytinen 2005), is shown as a reddish horizontal band. The Phoenicid stream mass is determined at γ = 3.3 (blue circle), which lies closest to the possible stream mass range, within the plausible index range 3.3 ≤ γ ≤ 4.4 (double-headed arrow) derived from the observed comet-sourced meteoroids (R. C. Blaauw et al. 2011; A. Egal et al. 2022a, 2022b; P. Koten et al. 2023; A. V. Moorhead et al. 2025).
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: Precursor spin-up timescale is plotted as a function of the radius of the ice sublimating area (patch), rps, from Equation (15). Solid and dashed curves (black) show kT = 0.05 and 0.007 (D. Jewitt 1997, 2021), respectively. A horizontal band (yellow) indicates the range of spin-up timescales constrained both by orbital period and empirical observations. The two curves within the band highlight the parameter space where rotational destruction can occur.
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: Same as Figure 6 but from the W2 band, presenting the Prot = 13.2168 ± 2.3551 hr ≈ 13 ± 2 hr with an amplitude ~ 2.0 mag in the left panel and the maxima Prot = 0.5507 days (=13.2168 hr) in the right panel. The significance level is ~45%.
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: Calculated spectral energy distribution and measured flux densities from the 289P composite image in Visit A (MJD 58786: UT 2019 October 30, inbound). The flux densities at W1 (3.4 μm) and W2 (4.6 μm) are shown as points. The uncertainties are within the point size. The reflected sunlight model (blue line), thermal model (red line), and combined signal (black line) are overplotted. The geometric parameters Rh = 1.20 au, Δ = 0.40 au, and α = ﹩49\mathop{.}\limits^{\circ }8﹩, are used for the models.
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: Same as Figure 6 but from the weighted mean of the W1 and W2 magnitudes (Wwm), presenting the Prot = 8.8536 ± 0.3860 hr with an amplitude ~ 1.6 mag in the left panel and the maxima Prot = 0.3689 days (=8.8536 hr) with a significance level of 30.5% in the right panel. Another candidate Prot ~ 15.6 hr (~0.65 days) has a significance level of 30.4%.
Paper: Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids
Authors: Toshihiro Kasuga
Figure caption: Same as Figure 9 but in Visit B (MJD 58860: UT 2020 January 11–12, outbound). Rh = 1.01 au, Δ=0.09 au, and α = ﹩70\mathop{.}\limits^{\circ }2﹩ are used for the models.
Paper: Deep Learning-based Identification of CP1 and CP2 Stars from LAMOST DR11
Authors: ZhiWei Lu, Xiaoming Kong, YaTao Zhang, ZhenPing Yi, Meng Liu
Figure caption: Original LAMOST low-resolution spectrum (top panel) and its normalized spectrum (bottom panel).