adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: The H-R diagram for DG Leo displays the positions of all three stellar components. The inner binary components are represented by a green dot (Aa) and a red dot (Ab), respectively. Component B’s location is indicated by a pink dot, with all positions derived from the light-curve modeling. Additionally, a blue dot denotes the current evolutionary state of component B according to the best-fitting stellar model (Model A3), while the accompanying curve traces its predicted evolutionary track.
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: The five nonradial pulsation amplitudes and phases, modulated over the orbital period of the inner binary. The time zero-point is set to t0 = BJD 2458871.77213, chosen such that the phases of the first two orbital sidelobes are equal.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Reconstruction of the whitened deviation strain δs for deviation from the GR parameterized by the δβ2 phase coefficient. The blue curve is the whitened strain in each detector. The orange curve is the true injected δs. The black curve is the median estimate of δs using Gaussian process regression, and the gray shaded region is the 90% credible interval on δs.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Cumulative distribution function (CDF) of the log-signal-to-noise Bayes factor ﹩{\mathrm{ln}}{ \mathcal B }﹩ for 174 segments of realistic noise, ﹩\pi ({ \mathcal B })﹩ (blue curve). Also indicated is the value of ﹩{\mathrm{ln}}{ \mathcal B }﹩ for GW150914 residual data (black dotted line) and for GW190916_200658 residual data (red dotted line), the event with the highest ﹩{\mathrm{ln}}{ \mathcal B }﹩, though still typical of the distribution of ﹩{\mathrm{ln}}{ \mathcal B }﹩ for noise segments.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution of the Gaussian process hyperparameters for a simulated gravitational-wave signal with a parameterized deviation from GR in the form of a δβ2 ≠ 0 phase coefficient. The contours are the 1σ, 2σ, and 3σ intervals.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Reconstruction of the whitened deviation strain δs for a simulated signal that includes a deviation from GR drawn from our kernel. The blue curve is the whitened strain in each detector. The orange curve is the true injected δs. The black curve is the median estimate of δs using Gaussian process regression, and the gray shaded region is the 90% credible interval on δs.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution of the Gaussian process hyperparameters for a simulated signal with a deviation from GR drawn from our kernel. The contours are the 1σ, 2σ, and 3σ intervals. The true values are plotted as orange crosshairs and are included within at least the 3σ interval for all hyperparameters.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Example deviations from GR drawn from our kernel (Equation (5)), with scale factor k0 = 10−45, characteristic frequency f0 = [100] Hz, width w = 2.0, and length l = 2.5.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Example of a Gaussian wing classification: J012910+145935 in [O III] λ5007. In the top row, we compare the Gaussian core + Gaussian wing vs. Gaussian core + power-law wing models. In the second row, we subtract each core model from the flux and overlay the best-fit wing model. In the third row, we compare Gaussian and power-law models for each set of wings in log–log space. The maximum wing velocity ﹩{V}_{{\rm{Max}}}﹩, the minimum velocity VMin in the power-law model, and the continuum fit are shown with lines as indicated in the legends. Gray regions in the power-law models represent the transition regions between the Gaussian core and power-law wings, which are not accounted for in our models. The noise spike at V  ∼ −110 km s−1 is masked prior to fitting.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Example of a power-law wing classification: J124835+123403 in [O III] λ5007. The panels are analogous to those in Figure 1. The feature around 500 km s−1 is emission from Fe II λ5018, which is masked from the fits.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Gray points show the full sample, while colored points (coded by redshift) denote the selected subsample (Section 4.3). The red and blue arrows indicate the expected size–mass evolution for galaxies undergoing minor and major mergers, respectively. The dotted and dashed lines represent the results from previous studies by A. van der Wel et al. (2014) and K. Ito et al. (2024), respectively.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: LyC escape fraction ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩ vs. maximum broad-wing velocity ﹩{V}_{{\rm{Max}}}﹩ in [O III]λ5007, color-coded by wing morphology. The triangles represent upper limits on ﹩{f}_{{\rm{esc}}}^{{\rm{LyC}}}﹩.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Example of an ambiguous wing classification: J144010+461937 in [O III] λ5007. The panels are analogous to those in Figure 1.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Comparison of ﹩{V}_{{\rm{Max}}}﹩ and L≥300 between LyC leakers (blue) and non-leakers (orange).
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Measured broad-wing parameters from [O III] λ5007: maximum broad-wing velocity ﹩{V}_{{\rm{Max}}}﹩ vs. luminosity L≥300, color-coded by 5007 Å median continuum luminosity.
Paper: Dynamical Environment and Stability around Centaur (2060) Chiron
Authors: G. Madeira, B. E. Morgado, C. L. Pereira, G. Ramon, R. Sfair, F. Braga-Ribas
Figure caption: Lifetime of particles in the vicinity of Chiron, assuming the object’s nominal parameters. Each colored pixel corresponds to a particle with a given initial semimajor axis (x-axis) and eccentricity (y-axis), with color indicating its lifetime. Filled black squares mark the maximum eccentricity recorded for particles that begin on Keplerian circular orbits and survive until the end of the simulation, whereas open black squares indicate the last values of the eccentricities registered by the N-body code for particles that are lost through ejection or collision with Chiron. Vertical red lines mark the theoretical locations of spin-orbit resonances, colored curves the resonance centers extracted from Poincaré maps, and shaded regions their widths. The observed ring locations are shown by vertical black lines.
Paper: Dynamical Environment and Stability around Centaur (2060) Chiron
Authors: G. Madeira, B. E. Morgado, C. L. Pereira, G. Ramon, R. Sfair, F. Braga-Ribas
Figure caption: Theoretical locations of spin-orbit resonances (dashed lines) and stable region boundaries (black curves) for different C22 values, as a function of Chiron’s mass. The gray area marks the extent of the detected disk, and the narrow, dark gray bands indicate the rings.
Paper: Dynamical Environment and Stability around Centaur (2060) Chiron
Authors: G. Madeira, B. E. Morgado, C. L. Pereira, G. Ramon, R. Sfair, F. Braga-Ribas
Figure caption: Selected Poincaré maps showing the stability islands of spin-orbit resonances closest to each ring. The top panel highlights, in blue, the three islands of the 2:5 SOR, near Chi1R; the middle panel, in shades of green, highlights the double islands of the 1:3 SOR, near Chi2R; and the bottom panel, in shades of purple, highlights the double islands of the 1:5 SOR, near Chi3R. The Jacobi constant associated with each map is indicated in the upper right corner of the panels.
Paper: Dynamical Environment and Stability around Centaur (2060) Chiron
Authors: G. Madeira, B. E. Morgado, C. L. Pereira, G. Ramon, R. Sfair, F. Braga-Ribas
Figure caption: Stable region boundary around Chiron as a function of its mass and C22, shown by the colormap. Black curves mark the parameter combinations where the boundary coincides with the inner edge of the disk, Chi1R, and Chi2R. The white “X” indicates Chiron’s nominal parameters.
Paper: Converging on the Cepheid Metallicity Dependence: Implications of Nonstandard Gaia Parallax Recalibration on Distance Measures
Authors: Louise Breuval, Gagandeep S. Anand, Richard I. Anderson, Rachael Beaton, Anupam Bhardwaj, Stefano Casertano, Gisella Clementini, Mauricio Cruz Reyes, Giulia De Somma, Martin A. T. Groenewegen, Caroline D. Huang, Pierre Kervella, Saniya Khan, Lucas M. Macri, Marcella Marconi, Javier H. Minniti, Adam G. Riess, Vincenzo Ripepi, Martino Romaniello, Daniel Scolnic, Erasmo Trentin, Piotr Wielgórski, Wenlong Yuan
Figure caption: Recent empirical and theoretical estimates of the Cepheid metallicity dependence γ from the literature in the ﹩{m}_{H}^{W}﹩ and ﹩{m}_{VI}^{W}﹩ Wesenheit indices. A few analyses were excluded from this plot (e.g., W. L. Freedman & B. F. Madore 2011; P. Wielgórski et al. 2017; K. A. Owens et al. 2022) due to issues that were identified and discussed in L. Breuval et al. (2022). The blue band shows broad agreement between γ ∼ −0.15 and −0.30 mag dex−1. The methods labeled with different shapes include comparison between P–L relations in different galaxies, metallicity gradients, Milky Way Cepheids with Gaia EDR3 parallaxes, Baade–Wesselink distances, and theoretical predictions. The red point indicates the γ ∼ 0 multiwavelength result by MF25, based on a variety of methods. The metallicity dependence γ in the ﹩{m}_{H}^{W}﹩ Wesenheit magnitude and the Hubble constant H0 are related as follows: γ shifts the luminosity of Cepheids which show the largest metallicity difference with respect to Cepheids in SNIa hosts (i.e., in the SH0ES distance ladder, the metal-poor LMC, and SMC). This luminosity difference directly translates into a shift in H0. We note that the H0 values represented on the top x-axis are not actually measured in the quoted references but are derived from H0DN Collaboration et al. (2025).
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Phase trajectory maps of grain alignment for the RAT model of ﹩{q}^{{\rm{\max }}}=1﹩ and SPM grains of δmag = 103 in the RD regime with different U/(n1T2) (panels (a)–(c)). Some grains are driven rapidly to be aligned at the high-J attractor, and the rest of the grains are driven to low-J rotation and trapped by the RAT trapping.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 17 but for temporal evolution of the alignment degrees. Alignment degree increases with time due to the random transport of grains to high-J attractors and achieves perfect alignment at TPA ∼ 10–20τdamp.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 19 but for temporal evolution of the alignment degrees. Alignment degree increases with time due to slow transport of grains to high-J attractors by collisional and magnetic excitations, and grains achieve perfect alignment at TPA ∼ 20–100τdamp.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Phase trajectory maps for grain alignment in the CNM, WIM, and PDR, assuming the RAT model with ﹩{q}^{{\rm{\max }}}=1﹩ and SPM grains of δmag = 103. All grains align at the high-J attractor due to slow transport by gas collisions. Grains with low tensile strength can be disrupted in WIM and PDR.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Phase trajectory maps of grain alignment for the RAT model of ﹩{q}^{{\rm{\max }}}=1﹩ and SPM grains with δmag = 103 in the CD regime and different U/(n1T2) (panels (a)–(c)). Some grains rapidly spin up to the high-J attractor, and the rest of the grains are slowly transported to high-J attractors due to gas collisions and magnetic fluctuations.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Phase trajectory maps of grain alignment for the RAT model of ﹩{q}^{{\rm{\max }}}=3﹩ and SPM grains of δmag = 103 in the CD regime of different U/(n1T2) (panels (a)–(c)). Some grains are rapidly spun up to the high-J attractor, but the rest of the grains are driven to the low-J rotation, followed by slow transport to high-J attractors by collisional and magnetic excitations.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Phase trajectory maps of grain alignment for the RAT model of ﹩{q}^{{\rm{\max }}}=3﹩ and SPM grains of δmag = 103 in the RD regime of different U/(n1T2) (panels (a)–(c)). Some grains are driven rapidly to be aligned at the high-J attractor, and the rest of the grains are driven to low-J rotation and trapped by the RAT trapping.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Time-dependent alignment degrees of grains in the CNM, WIM, and PDR. The alignment degrees increase with time due to slow transport by collisional excitations, and achieve perfect alignment after 10τdamp.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 21 but for temporal evolution of the alignment degrees. Alignment degree increases rapidly within 0.01τdamp and becomes saturated at R ∼ 0.4 for intense radiation due to RAT trapping.
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: The metallicity gradient measured by two different methods of our high-probability Draco members as a function of elliptical radial distance in units of half-light radius (top labels) and arcminutes (bottom labels) from the center. Left panel: the metallicity gradient measured by running the GMM in four elliptical bins, fixing the PM. The best-fit line of the radial distributions of [Fe/H] in this paper is labeled in dark dashed line. The slope of the metallicity distribution measured by E. N. Kirby et al. (2011) in the inner radius is labeled by the red dashed line. Right panel: the metallicity gradient as measured by computing the mean metallicity of just our high-probability Draco members in elliptical bins as a function of the distance in units of half-light radius (top labels) and arcminutes (bottom labels) from the center. The slope of the metallicity distribution measured by E. N. Kirby et al. (2011) in the inner radius is labeled in red. The slope of the metallicity measured by our high-probability Draco members beyond 12′ is −0.0006 ± 0.0014 dex ﹩{{\rm{arcmin}}}^{-1}﹩, consistent with being flat. The slope measured by E. N. Kirby et al. (2011) is a good fit within the half-light radius, and the metallicity gradient flattens at larger radii.
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: [Fe/H] vs. heliocentric radial velocity distribution and the PM distribution of high-probability members in our work plotted with the high-probability members from Y. Qi et al. (2022) and high-probability members we found using data from M. G. Walker et al. (2023). Top left panel: the [Fe/H] vs. heliocentric velocity for the high-probability members from our sample. Top right panel: the [Fe/H] vs. heliocentric velocity for the high-probability members from our sample and M. G. Walker et al. (2023). Lower left panel: the PM distribution in this study. Lower right panel: the PM distribution of our sample (in red circles) and high-probability members in M. G. Walker et al. (2023, blue circles). Two high-probability members outside the tidal radius matched in all three studies (this work, M. G. Walker et al. 2023, and Y. Qi et al. 2022) are labeled in yellow circles. The yellow triangles show the two additional matched extratidal stars in our sample and in M. G. Walker et al. (2023) with the DESI errors for those two stars plotted in red cross.
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: Top panel: the surface number density for stars with a membership probability greater than 0.9, corrected for sample incompleteness (blue data points with error bars). A Plummer model is shown in black, a King surface density profile (I. King 1962) with a green dashed line, and an exponential model in yellow solid. The red data points are the original measured surface density. The gray dash line is the King tidal radius = 48﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩1, as measured in R. R. Muñoz et al. (2018). Bottom panel: the completeness profile as a function of distance from center of Draco. The cyan line shows the ratio of the completeness.