adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Study of Five Intermediate-age Pismis (2, 3, 7, 12, 15) Clusters Using Photometric and Astrometric Data from Gaia EDR3
Authors: D. Bisht, Qingfeng Zhu, W. H. Elsanhoury, R. K. S. Yadav, Geeta Rangwal, Devesh P. Sariya, Alok Durgapal, Ing-Guey Jiang
Figure caption: Same as Figure 16, but for clusters Pi 12 and Pi 15.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Abundances of individual elements as a function of metallicity. From top to bottom, left to right: α-elements (Mg, Si, O), odd-Z element (Al), and Fe-peak elements (Mn, Ni). Markers and colors are the same as in Figure 1, except for the red markers that correspond to the stars that might have an origin close to the Galactic center, from the kinematic point of view. The gray region represents the density distribution obtained from all the available APOGEE DR17 data. The solid and dashed lines in the top-left panel separate the halo stars from the disk stars, and the thin disk from the thick disk stars, respectively (Lane et al. 2022). The typical uncertainty in the abundances is ∼0.05 dex (Jönsson et al. 2020).
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Halo stars in the [α/Fe] vs. [Fe/H] space (left), and the [Mg/Fe] vs. [Fe/H] space (right). Markers and colors for the HiVel sample are the same as in Figure 1. Gray dots are all the halo stars from APOGEE DR17. The black dashed lines separate the high-α or high-Mg (in situ) population from the low-α or low-Mg (accreted) population, as defined by Nissen & Schuster (2010; left) and Hayes et al. (2018; right). The gray dashed line in the right panel is the corrected limit accounting for the systematic differences in Mg abundances between APOGEE DR13 and DR17. Typical uncertainties in [Mg/Fe] are below 0.05 dex (Jönsson et al. 2020).
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Distance from the Galactic center to the last intersection of the orbit with the Galactic plane (R dc), as a function of the orbital energy. The vertical defines the limit between bounded (negative energy) and unbounded (positive energy) orbits. The horizontal line corresponds to a Galactocentric distance of 1 kpc, for reference. Markers and colors are the same as in Figure 1. Left: without the LMC. Right: including the LMC.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Maximum height over the Galactic plane (Z max) reached during orbit integration as a function of orbital eccentricity (e). Markers and colors are the same as in Figure 1. Left, without the LMC. Right, including the LMC.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: The H-R diagrams of the HiVel sample. The left panel shows the Gaia G absolute magnitude as a function of the Gaia BP–RP color. The right panel shows the surface gravity (﹩\mathrm{log}g﹩) as a function of the effective temperature (T eff). Markers and colors are the same as in Figure 1. Green lines indicate the stellar isochrones obtained from PARSEC.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Comparison between the photogeometric distances of Bailer-Jones et al. (2021) used in this work (vertical axis) and other distance estimates for the HiVel stars: Gaia parallaxes (top panel), StarHorse2 (middle panel), and AstroNN (bottom panel). Markers and colors are the same as in Figure 1.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Distribution of the HiVel sample in the action diamond space. Markers and colors are the same as in Figure 1. The green box represents the locations of the Gaia-Sausage remnant.
Paper: DELIGHT: Deep Learning Identification of Galaxy Hosts of Transients using Multiresolution Images
Authors: Francisco Förster, Alejandra M. Muñoz Arancibia, Ignacio Reyes-Jainaga, Alexander Gagliano, Dylan Britt, Sara Cuellar-Carrillo, Felipe Figueroa-Tapia, Ava Polzin, Yara Yousef, Javier Arredondo, Diego Rodríguez-Mancini, Javier Correa-Orellana, Amelia Bayo, Franz E. Bauer, Márcio Catelan, Guillermo Cabrera-Vives, Raya Dastidar, Pablo A. Estévez, Giuliano Pignata, Lorena Hernández-García, Pablo Huijse, Esteban Reyes, Paula Sánchez-Sáez, Mauricio Ramírez, Daniela Grandón, Jonathan Pineda-García, Francisca Chabour-Barra, Javier Silva-Farfán
Figure caption: Same as Figure B1, but for the 10 examples with the largest errors normalized by angular separation among galaxies with an angular separation larger than 2.″5. Note that large normalized errors are seen in cases where there is a degeneracy between two or more galaxies as potential hosts, such as in SN2008bf, SN20011ft, ZTF21aaawhkf, and SN2012fk; when SExtractor masks H II regions in a given galaxy as different extended sources, such as in SN2006C and ZTF20actogyl; and when there are bright stars close to or in the line of sight of the real host, such as in ZTF20abaslyx, ZTF20acitlbp, ZTF19achtehz, and SN2009bw.
Paper: DELIGHT: Deep Learning Identification of Galaxy Hosts of Transients using Multiresolution Images
Authors: Francisco Förster, Alejandra M. Muñoz Arancibia, Ignacio Reyes-Jainaga, Alexander Gagliano, Dylan Britt, Sara Cuellar-Carrillo, Felipe Figueroa-Tapia, Ava Polzin, Yara Yousef, Javier Arredondo, Diego Rodríguez-Mancini, Javier Correa-Orellana, Amelia Bayo, Franz E. Bauer, Márcio Catelan, Guillermo Cabrera-Vives, Raya Dastidar, Pablo A. Estévez, Giuliano Pignata, Lorena Hernández-García, Pablo Huijse, Esteban Reyes, Paula Sánchez-Sáez, Mauricio Ramírez, Daniela Grandón, Jonathan Pineda-García, Francisca Chabour-Barra, Javier Silva-Farfán
Figure caption: Same as Figure B1, but for the 10 examples with the largest standard deviation of the DELIGHT predictions normalized by angular separation, among galaxies with an angular separation larger than 2.″5. They tend to be similar cases to those found in Figure B3, with four of these largest normalized standard deviations also being among the top 10 worst cases in terms of normalized errors.
Paper: DELIGHT: Deep Learning Identification of Galaxy Hosts of Transients using Multiresolution Images
Authors: Francisco Förster, Alejandra M. Muñoz Arancibia, Ignacio Reyes-Jainaga, Alexander Gagliano, Dylan Britt, Sara Cuellar-Carrillo, Felipe Figueroa-Tapia, Ava Polzin, Yara Yousef, Javier Arredondo, Diego Rodríguez-Mancini, Javier Correa-Orellana, Amelia Bayo, Franz E. Bauer, Márcio Catelan, Guillermo Cabrera-Vives, Raya Dastidar, Pablo A. Estévez, Giuliano Pignata, Lorena Hernández-García, Pablo Huijse, Esteban Reyes, Paula Sánchez-Sáez, Mauricio Ramírez, Daniela Grandón, Jonathan Pineda-García, Francisca Chabour-Barra, Javier Silva-Farfán
Figure caption: Same as Figure B1, but for 10 random examples from the nearby sample.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: Left: posterior distributions of parameters of KIC 3127873 (nol 3) and KIC 5022908 (l 3) are obtained by NN models and MCMC algorithm. Right: fitting results of KIC 3127873 and KIC 5022908. The blue dots are the original light curves. The red lines are the light curves generated by NN models. The x points are the light curves generated by Phoebe. This two targets have higher orbital inclination and lower mass ratio.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: Left: posterior distributions of parameters of KIC 9392682 (nol 3) and KIC 7339123 (l 3) are obtained by NN models and MCMC algorithm. Right: fitting results of KIC 9392682 and KIC 7339123. The blue dots are the original light curves. The red lines are the light curves generated by NN models. The x points are the light curves generated by Phoebe. The two targets have lower orbital inclination and lower mass ratio.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: Left: posterior distributions of parameters of KIC 6431545 (nol 3) and KIC 9519590 (l 3) are obtained by NN models and MCMC algorithm. Right: fitting results of KIC 6431545 and KIC 9519590. The blue dots are the original light curves. The red lines are the light curves generated by NN models. The x points are the light curves generated by Phoebe. The two target have lower orbital inclination and higher mass ratio.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: Left: posterior distributions of parameters of KIC 6671698 (nol 3) and KIC 4909422 (l 3) are obtained by NN models and MCMC algorithm. Right: fitting results of KIC 6671698 and KIC 4909422. The blue dots are the original light curves. The red lines are the light curves generated by NN models. The x points are the light curves generated by Phoebe. The two targets have higher orbital inclination and higher mass ratio.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: Left: the distribution of the standard deviation of the residuals of the predicted light curves and synthetic light curves, which have l 3 influence. Right: the blue light curve is generated by Phoebe. The yellow light curve is generated by model with l 3 influence. The two light curves are generated from the same input parameters.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: Left: the distribution of the standard deviation of the residuals of the predicted light curves and the synthetic light curves, which have no l 3 influence. Right: the blue light curve is generated by Phoebe. The yellow light curve is generated by model without l 3 influence. The two light curves are generated from the same input parameters.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: The distribution of the difference between the parameters obtained by MCMC and the model without l 3 influence and the true values is shown in the figure.
Paper: Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Authors: Xu Ding, KaiFan Ji, XuZhi Li, JianPing Xiong, QiYuan Cheng, JinLiang Wang, Hui Liu
Figure caption: The distribution of the difference between the parameters obtained by MCMC and the model with l 3 influence and the true values is shown in the figure.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Raw contrast (left panels) and speckle noise floor after subtracting a PSF reference star (right panels) of the LUVOIR-A apodized pupil Lyot coronagraph (APLC; top panels) and the LUVOIR-B vector vortex charge six coronagraphs (VC6; bottom panels) used in this work to simulate coronagraphic observations of exoplanetary systems. The different shadings represent different stellar angular diameters given in units of λ/D. In the top panels, the blue curves correspond to a model assuming a wave front error of 10 pm rms and the orange curves correspond to a model assuming a wave front error of 90 pm rms.
Paper: Simulating Reflected Light Coronagraphy of Earth-like Exoplanets with a Large IR/O/UV Space Telescope: Impact and Calibration of Smooth Exozodiacal Dust
Authors: Jens Kammerer, Christopher C. Stark, Kevin J. Ludwick, Roser Juanola-Parramon, Bijan Nemati
Figure caption: Same as Figure 1 but showing the full 2D speckle fields instead of the azimuthally averaged 5σ contrast curves. Here, the baseline (10 pm rms WFE) case is shown for the APLC in the top panels. The images are evaluated for observations of a Solar analog at a distance of 10 pc and an observing wavelength of 500 nm.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the Wilson diagram, adding details from top to bottom. The top panel presents the velocity splitting as a function of ionization energy from all forbidden nebular lines and all permitted lines, except those of O0, C+, N+, O+, and Ne+. These lines establish a well-defined relation between velocity splitting and ionization potential. In the second panel, we add the auroral forbidden lines of N+, O+, O2+, S+, S2+, Ar2+, and Ar3+ (open squares). For N+, O+, O2+, and Ar3+, these transitions have smaller velocity splitting than the nebular transitions. In the bottom panel, we add the permitted lines of O0, C+, N+, O+, and Ne+. Although these lines span a wide range of ionization potentials, they share a common velocity splitting. The permitted lines of H0 and He0 and the forbidden lines of O2+ and Ne2+ are shown in larger symbols since these lines sample the majority of the nebular volume. The small symbols for Mn4+, Ne3+ (forbidden), and C3+ (permitted) indicate that they are difficult measurements. The tick marks and labels indicate the ionization energies.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We compare an image (left; Hubble Space Telescope proposal ID 8594) and PV diagram (right; CD#2) of NGC 6153 in the light of Hα. The spectrograph slit is shown on the left. The position of the central star, whose continuum is subtracted from the PV diagram, would appear at the position of the horizontal line (right panel; y-coordinate of zero). The main structure of NGC 6153 is its main shell, which is the origin of the “ ∩ ”-shaped structure in the PV diagram (dashed line). The Doppler effect separates the emission from the approaching and receding sides, except at the top where the expansion is perpendicular to the line of sight. The rectangle (right panel) indicates the three rows used to compute the velocity separation between the approaching and receding sides of the nebula (Section 3.1). The systemic velocity is the average radial velocity for the object.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We present the PV diagrams for lines spanning the full range of ionization energies in NGC 6153: C IV λλ5801,5811, He II λ4686, [Ar IV] λ4740, [O III] λ4959, [Ar III] λ7135, [N II] λ6583, and [O I] λ6300 (top to bottom). The intensity in each panel is normalized to its maximum value, indicated at the upper left in each panel, below the line identification. The color bar at top is common to all panels (−5%–100% of the maximum value; linear scale). We identify several morphological features that we refer to in the text. There are clear, continuous, and systematic changes in the shape of the emission line profile as a function of the ionization energy. Likewise, the difference in velocity between the approaching and receding sides varies with ionization energy.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams in the lines of C II λ6578, O II λ4649, N II λ5680 , and Ne II λ3694. Although the PV diagram for Ne II λ3694 is of lower S/N, all of the lines share the same morphology, indicating that they arise from the same volume of plasma. Note that the morphology of these PV diagrams is quite different from the morphology of the PV diagrams for [O III] λλ4959,5007 and [Ne III] λ3869 (Figures 4, 47, and 48). They are more similar to the PV diagrams in Figure 46, but their overall shape is even more circular because of their larger velocity splitting.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We plot the reddening, E(B − V), from Tables 3 and 4 as a function of wavelength for H I and He I lines. For the lines indicated as “H I, CD#X,” the line ratio is Hn/Hβ or Pn/Hβ and plotted at the wavelength of Hn or Pn, respectively, the Balmer and Paschen lines originating at upper level n. For the reddening computed from the ratio of Paschen to Balmer lines, Pn/Bn, the reddening is plotted at the wavelength of the Paschen line. The horizontal dashed line represents the mean value of E(B − V) for the H I lines in the CD2 wavelength interval (reference value). For the He I lines, the squares represent ratios using He I λ4922 as the reference line while the crosses use He I λ5876 as the reference line. The reddening computed from the He I λλ5015/4922 and He I λλ7281/5876 line ratios falls at negative values (these reddening values are not shown). Both lines are apparently much too weak.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: This image from the (red) slit camera shows the slit superposed upon NGC 6153. The arrows indicate the image orientation. The slit size is 15.″75 × 2″ and its position angle is 118° (N through E). The decker limits the slit length to 10″ (CD1 and CD2) or 13″ (CD3 and CD4).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: The top panel presents the PV diagram of the difference between the [O III] and [Ar III] temperatures. The contours are of the intensity of [Ar III] λ7135. The rectangle indicates the columns and rows considered for the statistics. In the bottom panel, we plot the mean [O III] and [Ar III] temperatures as a function of the limiting relative intensity of the [Ar III] λ7135 line, i.e., both temperatures are averaged over the same PV coordinates. (The dotted line shows the effect of correcting for the contamination in the [O III] λ4363 line.) As in Figure 37, the [O III] temperature is systematically higher. We also plot the T 0 and t 2 parameters for the temperature fluctuation formalism of Peimbert (1967) for the same limiting relative intensities of the [Ar III] λ7135 line, as well as the predicted temperature for the Balmer jump following Peimbert (2019). When large volumes are considered, T 0 is similar to the kinematic temperature (Section 3.2.1).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These PV diagrams present the variation of the ADF for O2+ as a function of position and velocity within our slit. The top panel presents the ADF computed using all of the permitted O II λ4649 emission, while the bottom panel uses only the emission due to the additional plasma component. The scale is common to the two panels, but the contours are not. At the top, the contours are of the intensity of the observed O II λ4649 intensity. At bottom, they are of the intensity of this line due to the additional plasma component only. In the top panel, the ADF for the diffuse emission beyond the receding side of the nebula is near 1.0, implying that this emission is due to the normal nebular plasma, i.e., there is no abundance discrepancy when considering this volume of the normal nebular plasma. In both panels, the apparently high values at the largest velocities are due to the C III λ4650 line in the PV diagram of O II λ4649.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: The left panel presents mean and median values of the [O III] temperature as a function of the limiting intensities of [O III] λ4363 or [O III] λ4959 with respect to the maximum value for each line. The error bars represent the extent of the distributions from the 5th–95th percentiles. The right panels present the same information for the [Ar III] temperatures as a function of the line intensity limit for the [Ar III] λλ5191,7135 lines. In both cases, there is a systematic difference depending upon whether they are weighted by the intensity of the nebular or auroral line, with the values weighted using the auroral line being systematically higher.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We present the ratio of the PV diagram of the Hβ line and the model of this line based upon the [O III] λ4959 line broadened for a temperature of 8000 K. The top panel considers the observed PV diagram of Hβ (Figure 9). The next four panels consider the observed PV diagram of Hβ after subtracting a contribution due to the additional plasma component, which we model using the O II λ4649 line broadened for a temperature of 2000 K, equivalent to 5%, 10%, 15%, and 40% of the total Hβ emission. Contributions below 5% are not noticeable. For contributions of 5% and 10% (second and third panels), the result is a flatter ratio, presumably indicating that removing the emission due to the additional plasma component improves the agreement for the normal nebular plasma. For contributions of 15% or more (fourth and fifth panels), there is a deficit of Hβ emission at the positions and velocities expected for the additional plasma component.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These PV diagrams present the fraction of the mass in the additional plasma component for N2+ (left) and O2+ (right) computed assuming (T  e , N  e ) = (2000 K, 10, 000 cm−3) for the additional plasma component and (T  e , N  e ) = (8000 K, 5000 cm−3) for the normal nebular plasma. The contours are of the intensity of the [O III] λ4959 line. Locally, the additional plasma component represents up to 50%–60% of the total mass of N2+ and O2+ and is concentrated in the inner part of the main shell. The region of apparently high fractional mass at the right side of the PV diagram for O2+ is due to contamination from the C III λ4650 line adjacent to the O II λ4649 line.