adsabs/AstroCLIMB huggingface dataset:
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: (a) Peak 12CO(2–1) temperature of the 1.4 × 5.7 kpc2 (deprojected) field along each line-of-sight pixel, with a spatial resolution of ∼7 pc. The peak locations of dendrogram leaves are plotted as red points. Where leaf footprints overlap, we show only the brightest. The 6″ border is shown in white. In the upper right, an ACA map shows the full-galaxy context in grayscale. (b) Integrated intensity (zeroth moment) of the field. Five major trunks of the dendrogram, those containing eight or more hierarchical levels, are highlighted as contours in projection using the same colors as in Figure 2. (c) Intensity-weighted velocity (first moment) of the field using a high-sensitivity “strict” mask. (d) Effective linewidth of the field using the strict mask.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Recovery of 1005 test sources injected into signal-free regions of the 12CO(2–1) cube. We plot the injected Σmol, αvir, and MCO against each other and indicate whether or not the corresponding source is detected. In each panel, the solid blue line shows a logistic regression to determine where structures would be detected with 50% completeness, while the neighboring dashed lines show analogous boundaries of 10% and 90%.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Density distribution of the double derivative of the structure function ∂2Ξ/∂z ∂δθ. The three different panels correspond to the different reionization histories considered. The different colored filled contours here represent various percentages of the area encompassed by the ∂2Ξ/∂z ∂δθ surface, as shown in the labels. The horizontal dashed lines mark zmid. The dashed lines represent the angular size of bubbles varying with z.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Left: ﹩{\sigma }_{{\rm{DM}}}/{\overline{{\rm{DM}}}}_{{\rm{EoR}}}﹩ as a function of z. The three different line styles correspond to the different bubble sizes chosen here with radii R = 5, 10 and 20 (in grid units). Right: derivative of the ratio shown in the left panel with respect to z. The three different green lines correspond to the fluctuating estimates from the toy model simulations, whereas the orange lines are after a Gaussian smoothing. The vertical gray line shows the redshift corresponding to zmid.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: A similar plot of ∂2Ξ/∂z ∂δθ as in Figure 4. Three different panels correspond to the models with different bubble sizes but the same reionization history. The horizontal lines mark zmid, and the dashed line represents how the bubble size varies with redshift in terms of the angular size, θR.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Light-cone slices of the ionization field. The three different panels correspond to the LC slices obtained from the realistic GRIZZLY simulations for Slower, Fiducial, and Faster reionization histories, as labeled.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Sky-averaged DM and the corresponding cosmic variance during EoR. The solid lines represent the ﹩{\overline{{\rm{DM}}}}_{{\rm{EoR}}}﹩ estimates computed from realistic GRIZZLY LC simulations. Shaded regions around them are the corresponding 1σ cosmic variance. The cyan, green, and orange colors, respectively, represent Slower, Fiducial, and Faster reionization histories. The three dashed lines represent the ﹩{\overline{{\rm{DM}}}}_{{\rm{EoR}}}﹩ computed using the globally averaged ionization fractions ﹩{\bar{x}}_{{\rm{H}}\,\mathrm{II}}﹩ shown in Figure 9.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Derivative of ﹩{\overline{{\rm{DM}}}}_{{\rm{EoR}}}(z)﹩ with respect to redshift z. The three lines show the derivatives obtained from realistic simulations shown in Figure 10.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: The distribution shown in Figure 4 marginalized along δθ. The three solid lines represent ∫(∂2Ξ/∂z ∂δθ)dδθ for the three reionization histories. The dashed vertical lines correspond to the respective zmid values.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: The distribution shown in Figure 7 but marginalized along z. Vertical lines denote, 〈θR〉 which is θR(z) marginalized over the z range of interest.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Global averaged ionization fraction of the IGM during reionization. The three different lines represent different reionization histories obtained from realistic GRIZZLY simulations of EoR.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: The left column presents the normalized flux distribution for the H2 0–0 S(1), S(3), and S(5) emission lines normalized by the maximum flux value for NGC 3081. The black contours overlaid on the H2 0–0 S(1) line map present the ALMA CO(2–1) intensity distribution (D. Rosario et al. 2018); contours range from 10−1.35 to 10−0.3 Jy (0.35 dex steps). The solid black line overlaid on the H2 0–0 S(3) line map indicates the orientation of the disk (PA = 90°), and the dotted black lines indicate the edges of the ionization bicone (PA = 165°, ΩOut = 30°). The associated velocity fields for both the primary and secondary fit components are presented in the right two panels. The tan contours overlaid on the H2 0–0 S(5) normalized flux distribution represent the [Fe II]5.34μm intensity distribution; contours range between 10−7.25 and 10−6.25 Jy (0.5 dex steps). The center column presents the rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Low-frequency Probes of the Persistent Radio Sources Associated with Repeating Fast Radio Bursts
Authors: Yash Bhusare, Yogesh Maan, Ajay Kumar
Figure caption: Left: A logarithmic plot of the luminosity vs. absolute RM adapted from G. Bruni et al. (2024a), with the addition of FRB 20240114A. The PRS luminosity at 650 MHz is plotted after subtracting the expected contribution from the host galaxy. At low RM values (the shaded region; nominally for RM < 100 rad m−2), it is difficult to estimate the host contribution unambiguously. We have also included potential PRS candidates associated with FRB 20190417A and FRB 20181030A (A. L. Ibik et al. 2024) denoted by stars. Right: The radio spectrum of the candidate PRS associated with FRB 20240114A, using measurements from this work at 650 MHz, from X. Zhang & W. Yu (2024) at 1.3 GHz and from G. Bruni et al. (2024b) at 5 GHz. The spectral index is derived from the flux density measurements corrected for the host galaxy emission (dark, filled circles). The fainter points (almost overlapping with the dark points) represent observed values without this correction, while more faded points show the sub-banded measurements, wherever available.
Paper: Low-frequency Probes of the Persistent Radio Sources Associated with Repeating Fast Radio Bursts
Authors: Yash Bhusare, Yogesh Maan, Ajay Kumar
Figure caption: The uGMRT Band 4 radio images showing the fields around FRB 20220912A (left) and FRB 20240619D (right). The image of the FRB 20240619D field is limited by dynamic range due to the presence of a nearby bright active galactic nucleus. Circles indicate the locations of the respective FRBs.
Paper: Low-frequency Probes of the Persistent Radio Sources Associated with Repeating Fast Radio Bursts
Authors: Yash Bhusare, Yogesh Maan, Ajay Kumar
Figure caption: The allowed parameter space for the off-axis GRB afterglow models consistent with the measured 650 MHz flux density of the PRS associated with FRB 20240114A. Shaded regions show the combinations of circumburst density, n, and isotropic energy, Eiso, that reproduce our measurement within 3σ uncertainties, for viewing angles of θobs = 30°, 60°,  and 90°. The colors indicate the time at which the model light curve intersects the observed flux density. The dotted vertical lines show the typical range of observed Eiso.
Paper: Low-frequency Probes of the Persistent Radio Sources Associated with Repeating Fast Radio Bursts
Authors: Yash Bhusare, Yogesh Maan, Ajay Kumar
Figure caption: The allowed regions in the energy injection rate and the ejecta-density (﹩{\dot{E}}_{{\rm{mag}}}-\zeta ﹩) parameter space for an assumed minimum nebula age of 28 days. The shaded rectangular bands indicate the parameter ranges for different formation channels (SLSNe, LGRBs, AIC, and BNS), as shown in Figure 4 of B. Margalit et al. (2019). The gray region is the excluded parameter space from radio detection at 650 MHz by considering a minimum age of 28 days.
Paper: Low-frequency Probes of the Persistent Radio Sources Associated with Repeating Fast Radio Bursts
Authors: Yash Bhusare, Yogesh Maan, Ajay Kumar
Figure caption: Left: A uGMRT Band 4 image of the field around FRB 20240114A, showing a detection of a PRS at the FRB location. Right: Band 3 image of the same field with no detection, limited by relatively large noise. White circles are centered at location of the FRB with a 4″ radius.
Paper: Low-frequency Probes of the Persistent Radio Sources Associated with Repeating Fast Radio Bursts
Authors: Yash Bhusare, Yogesh Maan, Ajay Kumar
Figure caption: SED modeling of the host galaxy of FRB 20240114A using CIGALE. The observed photometric data points (purple dots) from SDSS and WISE are fitted with the model (solid black line) to estimate properties such as the SFR and the stellar mass.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Comparison of cavity precession and inner disk light curve for (a) model R22.5 and (b) model R45. Top panels show the cavity’s eccentricity (ecav, blue) and major-axis orientation (θcav, red) as a function of time during its precession. Pronounced oscillations occur from ∼100 to 160 days in model R22.5 and from ∼65 to 83 days in model R45, characterized by the rotation of the cavity’s major axis and quasi-periodic variations in its eccentricity, temporally aligned with the oscillation signals in EUV and Soft X-ray light curves shown in the middle and bottom panels.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: A sketch map that shows the definitions of the parameters to describe the configuration of the perturbed AGN disk. The blue region represents the initial disk with unit vector ﹩{\hat{{\boldsymbol{n}}}}_{{\rm{init}}}﹩. The inner disk inside Rc is tilted by an angle θin relative to the initial orientation after the fallback of debris stream in a misaligned orbit. Its unit vector is ﹩{\hat{{\boldsymbol{n}}}}_{{\rm{inner}}}﹩. The unit vector of the line of sight of the observer is ﹩{\hat{{\boldsymbol{n}}}}_{{\rm{LoS}}}﹩, marked by a green arrow.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Face-on surface density maps from the resolution test at t = 75.8 days are shown for two cases: (a) orbital inclination θinc = 45°, and (b) θinc = 90°. The number of particles for both the disk (Ndisk) and the star (Nstar) is indicated in each panel. The left column provides a zoom-in view of the inner disk region. The right column displays the global structure, including the debris stream and the perturbed disk.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: The left panel shows the radial profile of the blackbody effective temperature (Teff) of the initial disk, where gray circles represent the numerical results from Equation (B5), and the black solid line is a power-law fit given by T = 4 × 106 K﹩\cdot {(R/{R}_{g})}^{-3/4}﹩. The right panel shows the corresponding multitemperature blackbody spectrum (νLν) of the initial disk.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: The top of each panel shows the surface number density profiles of targets and spectroscopically observed member stars along the major axis, ﹩{x}^{{\prime} }﹩, for each dSph. The black squares and triangles are mean surface number densities in elliptical isophotal radial bins of targets and spectroscopically observed member stars. The colored dashed curves represent different MGE components, and the black solid curves are the summations of these MGE components, which match well with the black squares. The bottom of each panel shows the completeness fraction of spectroscopically observed member stars vs. targets, as a function of the projected distance along the major axis. The left, middle, and right panels are for Draco, Sextans, and UMi, respectively.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Best recovered dark matter density profiles of three dSphs: (a) Draco, (b) Sextans, and (c) UMi. The black and orange solid curves represent median values obtained through our single-population and chemodynamical models, respectively, with the shaded regions denoting the 1σ confidence regions. The black, red, and blue dashed vertical lines correspond to the half-number radii of the total, metal-rich, and metal-poor populations in each galaxy, with the shaded regions denoting the 1σ uncertainties. Note that the half-number radii for the metal-rich and metal-poor populations are based on the joint posterior probability of the best model.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Surface number density profiles of the two template maps along the major axis, ﹩{x}^{{\prime} }﹩, for each dSph. The two template maps are obtained for the metal-rich (red) and metal-poor (blue) subpopulations after a hard cut in metallicity for the division, and the hard cut is chosen to maximize the difference in the half-number radii of the two populations. Red and blue dots are surface number densities directly calculated from corresponding template maps. Solid curves with the same colors as dots denote the reconstructed profiles from different MGEs. The left, middle, and right panels are for Draco, Sextans, and UMi, respectively.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Best-fit model parameters for the single-population (magenta) and chemodynamical (green) models, with the three rows referring to Draco, Sextans, and UMi. The left and right green arrows in the first two columns for parameters λ and κ represent results for the metal-poor and metal-rich populations separated by the chemodynamical model. The y-axis ranges for different parameters are not the same. The meanings of the different model parameters can be found in Section 3.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Top: the comparison between the Draco member star LOSV measurements by DESI MWS (y-axis) and M. G. Walker et al. (2023; x-axis). The red line is the best fit with a slope of 1, and its y-intercept is the offset between the two observations (see the legend). Bottom: the histogram of the differences between the Draco member star LOSV measurements by DESI MWS and M. G. Walker et al. (2023). The red dashed vertical line represents the offset between the two observations determined from the fit in the top panel.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: The likelihood contours of six model parameters for Draco. The meanings of the different model parameters can be found in Section 3. The yellow, light-blue, and two dark-blue contours represent the 10%, 1σ, 2σ, and 3σ regions of the MCMC post-burn distributions, respectively.