adsabs/AstroCLIMB huggingface dataset:
Paper: The Giant Low Surface Brightness Galaxy Malin 1: New Constraints for Its Molecular Gas Mass from GBT/ARGUS Observations
Authors: Gaspar Galaz, David T. Frayer, Matías Blaña, J. Christopher Howk, Thomas Puzia, Evelyn J. Johnston, Yasna Ordenes-Briceño, Sarah Church, Santiago Gil, Katerine Joachimi, Marcelo Mora
Figure caption: Same as Figure 3, but correcting from disk peculiar velocity induced by disk rotation. The correction is made using the projection of the rotation curve from Lelli et al. (2010), which is derived using the H I data of Pickering et al. (1997) and assuming that the molecular gas has the same rotation profile.
Paper: Laboratory and Astronomical Discovery of Magnesium Dicarbide, MgC2 
Authors: P. B. Changala, H. Gupta, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Rotational temperature diagram of 24MgC2 in IRC+10216, fitted with the two-temperature model described in Appendix B. The slope of the parallel lines through each K ladder yields the rotational temperature (T rot), and the slope of the line through points across the K ladders yields the kinetic temperature (T kin). The flux of the K = 4 transition is assumed to be one-half the total flux of the unresolved 542 − 441/541 − 440 doublet. The error bar on each data point is twice the error shown in Table 2. Error bars on the parameters are twice the standard error of the fit.
Paper: Laboratory and Astronomical Discovery of Magnesium Dicarbide, MgC2 
Authors: P. B. Changala, H. Gupta, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Spectra of 25MgC2 and 26MgC2 toward IRC+10216. The simulated profile of the 202 − 101 transition of 26MgC2 (shown in blue in the top left panel) accounts for contamination from overlapping CH2CN transitions (shown in red); the total emission is shown in magenta. The profile for 25MgC2 (top right) includes quadrupole hyperfine splittings calculated from the laboratory constants. “U” indicates unidentified lines.
Paper: Laboratory and Astronomical Discovery of Magnesium Dicarbide, MgC2 
Authors: P. B. Changala, H. Gupta, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Spectra of 24MgC2 toward IRC+10216. The fitted profiles are plotted in red. “U” indicates unidentified lines.
Paper: The Dark Matter Tidal Stripping History of the Sagittarius Core with N-body Simulations
Authors: Hai-Feng Wang, Francois Hammer, Yan-Bin Yang, Jian-Ling Wang
Figure caption:                         Left column: Sgr core density and kinematics of the model projected on the Galactocentric x–z, x–y, and z–y planes. Stellar density is shown by black contours and colored from yellow to blue. The projected tangential velocities after subtraction of the COM velocity are shown by the black arrows and the orange arrows indicate the projected bulk velocity of the COM region. The blue arrow shows the projection of the internal angular momentum. The direction toward the MW center is indicated by the white dashed line. All arrows are scaled in order to be clearly shown for physical discussion. Right column: the observational results from Pino et al. (2021) (see their Figure 10) that are shown for comparison. A more detailed view of the stellar motions is shown in the Appendix in Figure 5.
Paper: The Dark Matter Tidal Stripping History of the Sagittarius Core with N-body Simulations
Authors: Hai-Feng Wang, Francois Hammer, Yan-Bin Yang, Jian-Ling Wang
Figure caption: It shows the dark matter and stellar mass evolution history during our simulation over a 4.7 Gyr duration (top panels: within a radius of 5 kpc; bottom panels: within a 2 kpc radius). The left, middle, and right panels show the ratio of dark matter to the stellar mass, the stellar stripping history of the core, and that of the dark matter.
Paper: The Dark Matter Tidal Stripping History of the Sagittarius Core with N-body Simulations
Authors: Hai-Feng Wang, Francois Hammer, Yan-Bin Yang, Jian-Ling Wang
Figure caption: It compares our full-particle simulation presented in the Letter and this simulation with the analytical MW (see the blue and red dots, respectively). The latter is assumed without numerical heating, since it does not possess massive particles. From top to bottom: the velocity dispersion perpendicular to the orbital plane, as it is a quantity that could be only affected by the Sgr disk particle motions; the distance of a dwarf galaxy from the MW center; the number of massive MW particles within the Sgr core (with a radius of 2 kpc). For a double check, we ran a new simulation by increasing the resolution of the MW by a factor of 10; see the green dots. It shows a very smooth evolution in the velocity dispersion perpendicular to the orbital plane of a dwarf galaxy, which verifies the concern that using less massive MW particles reduces the artificial kicking. These tests confirm that the artificial kicking happens only for short durations near the pericenter passage, and has a marginal impact to the results and conclusions of the Letter.
Paper: The Dark Matter Tidal Stripping History of the Sagittarius Core with N-body Simulations
Authors: Hai-Feng Wang, Francois Hammer, Yan-Bin Yang, Jian-Ling Wang
Figure caption: Similar to Figure 1, but with more arrows and points to make the rotation and expansion in the outskirts clearer. Left column: Sgr core density and kinematics of the model projected on the Galactic centric x–z, x–y, and z–y planes. Right column: the observational results from del Pino et al. (2021) (see their Figure 10) that are shown for more comparison.
Paper: The Dark Matter Tidal Stripping History of the Sagittarius Core with N-body Simulations
Authors: Hai-Feng Wang, Francois Hammer, Yan-Bin Yang, Jian-Ling Wang
Figure caption: It shows stellar and dark matter tracks at the present time after 4.7 Gyr evolution. The top panel shows the stellar leading, trailing arm, core, north and south bifurcation. The bottom panel indicates how the dark matter may distribute differently than stars.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: Comparison of the GC (all, blue, and red GCs) number density contour maps with the ICL map (pseudocolor map) of the F277W image of the central field that was derived from a median boxcar (51 × 51 pixels) smoothing filter. Red triangles and blue circles represent the known cluster member galaxies and the gravitational lens sources (Mahler et al. 2022), respectively. Black circles denote the bright stars with F200W0 <22 mag, the sizes of which are scaled according to relative magnitudes. The yellow star is the center of the BCG. The color-scale bars represent the ICL surface brightness.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: (a) and (b) F200W vs. (F150W – F200W) CMDs of the point sources in the BCG and intracluster GC regions in the central field of SMACS 0723, as marked in Figure 1. The yellow dashed lines mark the 50% completeness limit. (c) Color histograms of the BCG (black line) and intracluster GC (blue line) regions after subtracting the contribution of the background based on the parallel field. Note that the color distribution of the intracluster GC region shows a strong peak at (F150W – F200W)0 = 0.05, while that of the BCG region shows a strong peak at 0.1 redder color, (F150W – F200W)0 = 0.15. Note also that both regions show a broad color distribution across the peak. Cyan boxes represent the boundary for selecting GC candidates, and green dashed lines mark the boundary for separating blue and red GCs.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: (a) Spatial distribution of the GCs (green squares) in the gray-scale map of the F200W image for the central field of SMACS 0723. Red triangles represent the confirmed cluster member galaxies, and dark red diamonds denote the selected bright red-sequence galaxies (with −0.65 < (F277W – F356W)0 < −0.45 and F277W0 < 22.5 mag). Blue open circles represent the gravitational lens image sources (Mahler et al. 2022). Yellow and cyan stars denote the BCG and other bright galaxies. Two large circles mark the BCG and intracluster GC regions. (b) Contour map and color gradient map of the GC number density in the gray-scale map of the F200W image. The contours were plotted from the 2σ bg level with 4σ bg steps. The color-scale bar represents the GC number density per square kiloparsec, and GCC 1 and GCC 2 denote GC clumps.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: Radial number density profiles of the GCs (all GCs, black circles; blue GCs, blue circles; red GCs, red circles). Solid lines represent the two-component Sérsic-law fitting results for the central plus intracluster GC components (dashed lines for individual components). The black, blue, and red lines denote, respectively, fitting results for all, blue, and red GCs. Thick dotted–dashed lines denote the power-law fitting results for the outer region (158 kpc <R <631 kpc).
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: Comparison of radial number density profiles of the GCs in SMACS 0723 (black circles for the data and the thick black line for the fitting result of the intracluster component) and the dark matter mass density profiles from four strong lensing models given in Mahler et al. (2022; their Figure 6): RELICS-lenstool (Coe et al. 2019; light green line), RELICS-GLAFIC (Coe et al. 2019; yellow line), LTM (Golubchik et al. 2022; blue line), and Mahler et al. (2022; red line). The lensing model profiles were arbitrarily shifted to match the GC data for 50 kpc < R < 200  kpc.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: Comparison of the GC number density contour maps for the central field of SMACS 0723 with the dark matter surface mass density map (convergence map) from strong lensing models given by Mahler et al. (2022; pseudocolor map). Red triangles and blue circles represent the known cluster member galaxies and the gravitational lens sources (Mahler et al. 2022), respectively. The color-scale bars denote the convergence (the dark matter surface mass density normalized to the critical surface mass density).
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: Same as Figure 7(b) but for blue (−0.2 < (F150W − F200W)0 < 0.2) and red (0.2 < (F150W–F200W)0 < 0.6) GCs.
Paper: The Giant Low Surface Brightness Galaxy Malin 1: New Constraints for Its Molecular Gas Mass from GBT/ARGUS Observations
Authors: Gaspar Galaz, David T. Frayer, Matías Blaña, J. Christopher Howk, Thomas Puzia, Evelyn J. Johnston, Yasna Ordenes-Briceño, Sarah Church, Santiago Gil, Katerine Joachimi, Marcelo Mora
Figure caption: Left: ARGUS field superimposed to an optical image of Malin 1 from Galaz et al. (2015). We observed especially the center of Malin 1 and some regions also observed by Braine et al. (2000). The true orientation of the beams will depend on the hour angle of the observations, but we probed the spiral arms of the galaxy too (Galaz et al. 2015; Boissier et al. 2016). Malin 1 is ∼3′ diameter, and the ARGUS footprint is 1.′52 × 1.′52, with 30.″4 spacing between individual elements, each with 7″ FOV. Right: figure by Braine et al. (2000) at the same scale of the left panel, showing the regions where they pointed the IRAM 30 m telescope to find 12CO(1-0) and 12CO(2-1). In Braine et al. (2000) the resolution of the 12CO(1-0) observations was 22″, and in our case was 7″. The lack of a precise picture of the structure of Malin 1, as revealed by this figure, prevented these authors pointing the beam to regions where the molecular gas is more likely present, except the center of the galaxy, clearly visible in the optical image at that time. Compare this right image with the left one, where we have in full view the optical spiral structure of Malin 1. In spite of the better spatial resolution in our observations, we also failed to detect 12CO(1-0), in the same regions depicted by this figure, as well as others shown in the left panel.
Paper: Diverse Properties of Molecular Gas in the Host Galaxies of Fast Radio Bursts
Authors: Bunyo Hatsukade, Tetsuya Hashimoto, Yuu Niino, Tzu-Yin Hsu
Figure caption: CO spectrum (left column), CO velocity-integrated intensity map (middle column), and continuum map (right column) of the host galaxies of FRB 20180924B (top row), FRB 20190102C (middle row), and FRB 20190711A (bottom row). The velocity resolution of the spectrum is 50 km s−1, and the line flux is measured with a 1″-radius aperture centered at the host-galaxy position. The velocity from −200 to +200 km s−1 is integrated for the velocity-integrated intensity maps of the hosts of FRBs 20180924B and 20190102C, while the range from +200 to +400 km s−1 is integrated for the FRB 20190711A host. The contours are ±2σ, ±3σ, and a 1σ step subsequently. The maximum contour level for the velocity-integrated intensity map of the FRB20180924A host is 11σ. The green circle shows the 90% confidence region of the FRB position (Macquart et al. 2020). The green cross represents the host position (Heintz et al. 2020). The synthesized beam size is shown in the lower-left corner of the maps.
Paper: The Giant Low Surface Brightness Galaxy Malin 1: New Constraints for Its Molecular Gas Mass from GBT/ARGUS Observations
Authors: Gaspar Galaz, David T. Frayer, Matías Blaña, J. Christopher Howk, Thomas Puzia, Evelyn J. Johnston, Yasna Ordenes-Briceño, Sarah Church, Santiago Gil, Katerine Joachimi, Marcelo Mora
Figure caption: Spectrum with the 12CO(1-0) signal over the 1.′52 square FOV of the ARGUS instrument, where all 16 beams of ARGUS were combined. There is no significant emission up to a threshold of 0.15 mK (T* A , 1σ). The velocity resolution was smoothed to 50 km s−1, and the temperature scale shown is ﹩{T}_{A}^{* }﹩ (see text for details).
Paper: Diverse Properties of Molecular Gas in the Host Galaxies of Fast Radio Bursts
Authors: Bunyo Hatsukade, Tetsuya Hashimoto, Yuu Niino, Tzu-Yin Hsu
Figure caption: Molecular gas fraction (left) and gas depletion time (right) as a function of the offset from the reference MS line after removal of redshift dependence. For comparison, star-forming galaxies (Cicone et al. 2017; Tacconi et al. 2018) and the hosts of SNe (Galbany et al. 2017), SLSNe (Arabsalmani et al. 2019; Hatsukade et al. 2020a), LGRBs (Hatsukade et al. 2020b), and AT2018cow (Morokuma-Matsui et al. 2019) are presented. We restricted the redshift of the galaxies in the comparison to z < 1 to match the redshift range of the FRB hosts. The dashed line shows the best-fit line for the MS galaxies derived in Tacconi et al. (2018).
Paper: The Giant Low Surface Brightness Galaxy Malin 1: New Constraints for Its Molecular Gas Mass from GBT/ARGUS Observations
Authors: Gaspar Galaz, David T. Frayer, Matías Blaña, J. Christopher Howk, Thomas Puzia, Evelyn J. Johnston, Yasna Ordenes-Briceño, Sarah Church, Santiago Gil, Katerine Joachimi, Marcelo Mora
Figure caption: Spectrum with the 12CO(1-0) signal at the central position of Malin 1 with the GBT 7.″0 beam. There is no significant emission up to a threshold of 0.23 mK (T* A , 1σ). The velocity resolution was smoothed to 50 km s−1, and the temperature scale shown is ﹩{T}_{A}^{* }﹩ (see text for details).
Paper: Diverse Properties of Molecular Gas in the Host Galaxies of Fast Radio Bursts
Authors: Bunyo Hatsukade, Tetsuya Hashimoto, Yuu Niino, Tzu-Yin Hsu
Figure caption: Comparison of molecular gas mass and SFR of the FRB hosts. For comparison, we plot local star-forming galaxies from the samples of ALLSMOG (Cicone et al. 2017) and xCOLDGASS (Saintonge et al. 2017), starbursts (Kennicutt & Reyes 2021), the hosts of SNe (Galbany et al. 2017), SLSNe (Arabsalmani et al. 2019; Hatsukade et al. 2020a), LGRBs (Hatsukade et al. 2020b), and AT2018cow (Morokuma-Matsui et al. 2019). The dotted, dashed, and dotted–dashed lines represent gas depletion times of 0.1, 1, and 10 Gyr, respectively.
Paper: Large Ion-neutral Drift Velocities and Plasma Heating in Partially Ionized Coronal Rain Blobs
Authors: David Martínez-Gómez, Ramón Oliver, Elena Khomenko, Manuel Collados
Figure caption: Comparison between adiabatic and frictional heatings. panels (a) and (b) represent the adiabatic variation of internal energy of the charged and the neutral fluids, Q ad,c  and Q ad,n , respectively. Panel (c) shows the frictional heating due to collisions. panels (d) and (e) represent the ratios between the frictional heating and the absolute values of Q ad,c  and Q ad,n , respectively.
Paper: Large Ion-neutral Drift Velocities and Plasma Heating in Partially Ionized Coronal Rain Blobs
Authors: David Martínez-Gómez, Ramón Oliver, Elena Khomenko, Manuel Collados
Figure caption: Top and bottom panels show horizontal and vertical cuts, respectively, of the absolute value of the drift velocity (left) and the heating term (right). Each line color corresponds to a different time of the simulation. Vertical dotted lines in the bottom panels mark the position of the density peak at each time.
Paper: Large Ion-neutral Drift Velocities and Plasma Heating in Partially Ionized Coronal Rain Blobs
Authors: David Martínez-Gómez, Ramón Oliver, Elena Khomenko, Manuel Collados
Figure caption: Top panel shows the spatially averaged value of the heating term, 〈Q  V 〉, as a function of time. The solid orange line and the blue crosses in the middle panel show the falling speed of the density peak of the charged and the neutral fluid, respectively, as a function of time. The bottom panel shows the maximum of the drift velocity (green solid lines) and the spatially averaged drift velocity (black dotted line) as a function of time.
Paper: Large Ion-neutral Drift Velocities and Plasma Heating in Partially Ionized Coronal Rain Blobs
Authors: David Martínez-Gómez, Ramón Oliver, Elena Khomenko, Manuel Collados
Figure caption: Horizontal cuts of the temperature variations caused by charged-neutral collision (top panels), densities (middle panels) and relative abundances, χ c and χ n (bottom panels). Left panels show the results for the charged fluid and right panels show the results for the neutral fluid. Each line color corresponds to a different time of the simulation.
Paper: Large Ion-neutral Drift Velocities and Plasma Heating in Partially Ionized Coronal Rain Blobs
Authors: David Martínez-Gómez, Ramón Oliver, Elena Khomenko, Manuel Collados
Figure caption: Sketch of the initial time of the simulation. Top and middle panels show the densities, ρ s, and the relative abundances, χ s, of the charged and neutral fluids, represented by orange solid lines and blue dashed-dotted lines, respectively. Bottom panel shows the coupling degree between the two fluids, given by the term α ρ c ρ n.
Paper: Large Ion-neutral Drift Velocities and Plasma Heating in Partially Ionized Coronal Rain Blobs
Authors: David Martínez-Gómez, Ramón Oliver, Elena Khomenko, Manuel Collados
Figure caption: Maximum values of the heating terms as functions of time. Orange and blue solid lines correspond to the maximum values of the adiabatic heating of the charged and the neutral fluid, respectively. The dotted-dashed line represent the results for the frictional heating due to charged-neutral collisions. The vertical dotted line shows the time of the simulation represented in Figure A1.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: (a) Gray scale maps of the F200W images of the central (left) and parallel (right) fields of SMACS 0723 (see also Figure 1 of Pontoppidan et al. 2022). Two large circles with radius of 15″ represent the BCG region and intracluster GC region, and the brightest galaxies including the BCG are labeled. Burgundy color denotes the edge regions with low signal to noise ratios in the combined images, which were not used for analysis. (b) A zoomed-in view of the BCG region in the central field of SMACS 0723: the Sparkler galaxy (z = 1.38, with a red linear shape embedding several red point sources) is at 15″ east of the BCG. (c, d, and e) Zoomed-in views of the original F200W image of the red box region in (b), the same image smoothed with a ring median filter, and the background-subtracted image. Red circles represent the point sources (thin dotted line) and GC candidates (thick solid line) found in this study, which are visible more clearly in the background-subtracted image.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: The F200W vs. (F150W – F200W) CMDs of the point sources in the central (a) and parallel (b) fields of SMACS 0723. Magenta and orange circles, respectively, represent the GCs and other compact sources of the Sparkler galaxy (z = 1.38) in Mowla et al. (2022). Magenta and orange boxes are the point sources selected in this study. The sources inside the cyan box of the central field are mostly GCs belonging to SMACS 0723. Cyan boxes represent the boundary for selecting the GC candidates in this study. The yellow dashed lines mark the 50% completeness limit. In panel (c), the thick red line denotes the net color histogram of the point sources with 27.5 mag < F2000 < 29.5 mag in the central field (thin red line) after subtracting the contribution of the background based on the parallel field (black line).
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: Effective radius r  h  vs. F277W (AUTO) magnitudes of the sources detected with SExtractor. Red squares represent the sources with stellarity <0.4, and blue squares denote the sources with stellarity > 0.8. The narrow slanted line dominated by the blue squares represents the point sources. Note that some bright sources (F277W0 < 22.5 mag) with stellarity >0.8 have large effective radii, r  h  >1.8 pixels. In this study, we select extended sources using the effective radius criterion, r  h  >1.8 pixels in the F277W image, as marked by the vertical black line.
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: The LW (F277W vs. (F277W – F356W)) and SW (F200W vs. (F150W – F200W)) CMDs of the extended sources with AUTO magnitudes in the central field of SMACS 0723. Red circles denote the spectroscopically confirmed cluster member galaxies, and blue circles represent the gravitational lens image sources (Mahler et al. 2022). The yellow star is the BCG, and cyan stars represent the bright galaxies (G2, G3, G4, and G5) marked in Figure 1. The red box in the left panel represents the selection criteria for the optically red sequence galaxies, which are mostly early-type members of the cluster. Note that the blue member galaxies in (F277W – F356W) colors are optically red galaxies, so they are plotted with red circles.