adsabs/AstroCLIMB huggingface dataset:
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Collapsed LRS2 data cubes of the BCG in A1982. The top row shows the target pointings, and the bottom row shows the parallel sky pointings. The channel names are given by the text labels. All images have different flux scaling to visualize structures. The manually chosen galaxy center is marked by the red circle in each panel. It also corresponds to the aperture with 1.″5 radius, in which the spectra are averaged. Each image has a size of 6″ × 12″.
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Three-dimensional views of the FPs for BCGs (red) and normal Es (black).
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Same as Figure 1, but we compare our nonparametric measurements of 54 normal Es based on deep WWFI (x-axis) and shallower SDSS (y-axis) imaging data.
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Same as Figure 1, but the SDSS de Vaucouleurs models are replaced by parametric MaNGA Sérsic models. The sample consists of 245 normal Es.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Example spectra of YSOs in CMa-ℓ224. Source names from Table 2 (No.) are provided on the left side of the respective spectra. All spectra are normalized to the continuum peak flux density in the wavelength range from 1.97 to 2.47 μm. The red horizontal lines show spectral ranges most affected by telluric lines; the wavelength range around 2.0 μm has been removed for clarity of the plot.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Three-color composite images of YSO candidates with the ≥ 3σ detection in the H2 line at 2.12 μm (in blue), Brγ line at 2.17 μm (in green), and the K-band continuum (in red). In each image, white contours correspond to the K-band continuum emission with contour levels of 25%, 50%, and 75% of the continuum peak marked with the red “×” symbol. Source IDs are indicated in the upper right corners.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: The H2 1-0 S(1) velocity centroid maps for all YSOs associated with the H2 emission; the velocities are calculated with respect to the radial velocity of the corresponding source. Only pixels with H2 detections above 3σ are shown. The contours show the K-band continuum emission, and the red crosses the positions of the YSO candidates (the peak of the K-band continuum emission). The source names are indicated in the upper right corners. Radial velocities of the gas associated with sources No. 78 and 88 cannot be estimated, and here only the apparent radial velocities are shown. The KMOS spectral sampling at 2.12 μm corresponds to 39.67 km s−1.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Herschel/SPIRE 250 μm image of the main filament in the CMa-ℓ224 star-forming region. Gray circles show the positions of YSO candidates observed with VLT/KMOS, while light gray dashed ellipses indicate regions hosting clusters of sources with the extended 4.5 μm emission (most likely tracing outflows) defined in Sewiło et al. (2019), Clusters A, B, and C. North is up, and east is to the left.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: KMOS K-band continuum maps of YSO candidates with possible stellar companions. Only spaxels with the continuum flux above 3σ are shown. White contours correspond to 25%, 50%, and 75% of the K-band continuum peak. The position of the brighter source in each map is indicated with a red “×” symbol (the “A” component in Table 2), and the fainter one with a gray “+” symbol (the “B” component). The size of the pixel (0.″2) corresponds to 184 au.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: The H2 1-0 S(1) channel maps for source No. 47. The velocities relative to the rest velocity of the H2 line are shown in the upper right corners. The green “×” symbol shows the position of the K-band continuum peak.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Total particle kinetic energy in the neutron star crust and core for (a) a decoupled fluid crust and a fluid core, (b) a solid crust and fluid core, and (c) a solid crust on top of a frozen core. The kinetic energy of the latter is not shown as it is zero.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Comparison of oscillation patterns for the NST crust after imposing a m = 0, l = 2 toroidal mode, with M = 3.8 × 105 cm s−1. The oscillations are tracked via the crust’s kinetic energy. Different reduction factors κ are shown as well as a case where the crust is modeled as fluid.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Toroidal oscillation sequence of the neutron star crust with N = 2.8 × 104 particles, M = 3.8 × 105 cm s−1, and a frozen core.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Top: initial shear velocity distribution in the φ-direction in rad per second, corresponding to M ∼ 4 × 107 cm s−1. Bottom: the velocity distribution after about 1250 iterations, or approximately 0.8 ms. It can be seen that the entire star, i.e., crust and core, is now in motion due to the toroidal velocity having propagated into the fluid core.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Kinetic energy oscillations for an NST crust initialized as in Figure 22 with numerical viscosities using α = 0.1, vs. α = 1.0.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: von-Mises stress for N = 2.8 × 104 particles, M = 3.8 × 105 cm s−1, and κ = 104.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Oscillations of a fluid crust with a fluid core, showing the φ-velocity in the crust using the Hammer projection at 0.067, 0.074, and 0.082 s.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Fast Fourier transform analysis of crust energy oscillations seen in Figure 18.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption:  φ-velocity in the fluid crust and core at 0.035 s showing the core velocities being much smaller than the velocities in the crust.
Paper: Interplanetary Coronal Mass Ejections and Stream Interaction Regions Observed by Tianwen-1 and MAVEN at Mars
Authors: Yutian Chi, Chenglong Shen, Long Cheng, Bingkun Yu, Bin Miao, Yuming Wang, Tielong Zhang, Zhuxuan Zou, Mengjiao Xu, Zonghao Pan, Zhenpeng Su, Jingnan Guo, Dongwei Mao, Zhihui Zhong, Zhiyong Zhang, Junyan Liu, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yang Du
Figure caption: Tianwen-1 and MAVEN spacecraft in situ observations of a 4 day time interval starting from 00:05 UT on 2021 December 9. From top to bottom, these panels show the magnetic field strength (B), the elevation (θ), and azimuthal (ϕ) angles of the magnetic field in the MSO coordinate system; three components of the magnetic field in the MSO coordinate system (B  x , B  y , and B  z ) from MAVEN/MAG (black asterisks) and Tianwen-1/MOMAG (red asterisks). Panels (g)–(l) show the solar wind speed (V sw), proton density (N  p ), dynamic pressure (P dp), proton temperature (T  p ), total pressure (P  t ), and proton beta (β) from MAVEN/SWIA. The lavender-colored band indicates the interval corresponding to the ICME inferred from the data in this figure. The two vertical black lines represent the interval in which we only use three out of four criteria (neglecting the criterion of ﹩\sqrt{(}T/| v| )\lt ﹩ 0.012) to select the MAVEN undisturbed solar wind periods.
Paper: Interplanetary Coronal Mass Ejections and Stream Interaction Regions Observed by Tianwen-1 and MAVEN at Mars
Authors: Yutian Chi, Chenglong Shen, Long Cheng, Bingkun Yu, Bin Miao, Yuming Wang, Tielong Zhang, Zhuxuan Zou, Mengjiao Xu, Zonghao Pan, Zhenpeng Su, Jingnan Guo, Dongwei Mao, Zhihui Zhong, Zhiyong Zhang, Junyan Liu, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yang Du
Figure caption: Orbits of Tianwen-1 (red line) and MAVEN (blue line) for the time interval from 06:00 UT on 2021 November 16 to 00:00 UT on 2021 November 18. (a) Tianwen-1’s and MAVEN’s trajectories in a cylindrical coordinate system. The inner dashed black line indicates the average location of the magnetic pileup boundary, and the outer black line marks the average location of the bow shock (Trotignon et al. 2006). (b) The orbits of the two spacecraft in the X–Y plane along the Z = 0 plane. (c) The orbits of the two spacecraft in the X–Z plane along the y = 0 plane. The Sun is to the right. (d) The orbits of the two spacecraft as viewed from the Sun. The panels are presented in the MSO coordinate system.
Paper: Interplanetary Coronal Mass Ejections and Stream Interaction Regions Observed by Tianwen-1 and MAVEN at Mars
Authors: Yutian Chi, Chenglong Shen, Long Cheng, Bingkun Yu, Bin Miao, Yuming Wang, Tielong Zhang, Zhuxuan Zou, Mengjiao Xu, Zonghao Pan, Zhenpeng Su, Jingnan Guo, Dongwei Mao, Zhihui Zhong, Zhiyong Zhang, Junyan Liu, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yang Du
Figure caption: The orbits of Mars, Venus, Mercury, and Earth in Heliocentric Earth Ecliptic (HEE) coordinates from 2021 November 16 to 2021 December 31, color coded by time. The black dot, red dots, purple dots, and green dots show the position of Earth, Venus, Mercury, and Mars, respectively.
Paper: Interplanetary Coronal Mass Ejections and Stream Interaction Regions Observed by Tianwen-1 and MAVEN at Mars
Authors: Yutian Chi, Chenglong Shen, Long Cheng, Bingkun Yu, Bin Miao, Yuming Wang, Tielong Zhang, Zhuxuan Zou, Mengjiao Xu, Zonghao Pan, Zhenpeng Su, Jingnan Guo, Dongwei Mao, Zhihui Zhong, Zhiyong Zhang, Junyan Liu, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yang Du
Figure caption: Tianwen-1 and MAVEN spacecraft in situ observations of a 4 day time interval starting from 00:01 UT on 2021 December 28. The lavender-colored band indicates the interval of an ICME inferred from the data in this figure. The plot setup is the same as in Figure 3.
Paper: Interplanetary Coronal Mass Ejections and Stream Interaction Regions Observed by Tianwen-1 and MAVEN at Mars
Authors: Yutian Chi, Chenglong Shen, Long Cheng, Bingkun Yu, Bin Miao, Yuming Wang, Tielong Zhang, Zhuxuan Zou, Mengjiao Xu, Zonghao Pan, Zhenpeng Su, Jingnan Guo, Dongwei Mao, Zhihui Zhong, Zhiyong Zhang, Junyan Liu, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yang Du
Figure caption: Tianwen-1 and MAVEN spacecraft in situ observations of a 3 day time interval starting from 12:04 UT on 2021 December 15. The lavender-colored band indicates the SIR interval inferred from the data in this figure. The plot setup is the same as in Figure 3.
Paper: Interplanetary Coronal Mass Ejections and Stream Interaction Regions Observed by Tianwen-1 and MAVEN at Mars
Authors: Yutian Chi, Chenglong Shen, Long Cheng, Bingkun Yu, Bin Miao, Yuming Wang, Tielong Zhang, Zhuxuan Zou, Mengjiao Xu, Zonghao Pan, Zhenpeng Su, Jingnan Guo, Dongwei Mao, Zhihui Zhong, Zhiyong Zhang, Junyan Liu, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yang Du
Figure caption: Tianwen-1 and MAVEN in situ observations of a 3 day time interval starting from 15:05 UT on 2021 November 17. The lavender-colored band indicates the SIR interval from the data in this figure. The blue vertical line indicates the stream interface of the SIR. The plot setup is the same as in Figure 3.
Paper: Interplanetary Coronal Mass Ejections and Stream Interaction Regions Observed by Tianwen-1 and MAVEN at Mars
Authors: Yutian Chi, Chenglong Shen, Long Cheng, Bingkun Yu, Bin Miao, Yuming Wang, Tielong Zhang, Zhuxuan Zou, Mengjiao Xu, Zonghao Pan, Zhenpeng Su, Jingnan Guo, Dongwei Mao, Zhihui Zhong, Zhiyong Zhang, Junyan Liu, Can Wang, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yang Du
Figure caption: Tianwen-1 and MAVEN spacecraft in situ observations of a 4 day time interval starting from 12:05 UT on 2021 December 1. The lavender-colored band indicates the interval of an SIR inferred from the data in this figure. The plot setup is the same as in Figure 3.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: Galactic Plane Figures of Merit used to compare baseline_v1.5 (dark purple, diamonds) and _v2.0 (salmon pink, stars). Left: summed science priorities of the HEALpix within a given science region to receive adequate sampling in the τ obs = 11 days (τ obs = 5 days) category (bars), compared with the number of HEALpix sampled (symbols). Right: the product of the number of visits to a HEALpix and its priority, summed over the survey regions of interest and presented as a percentage of the fiducial value expected from an ideal survey.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: Top: number of visits per sky pointing over all years and filters, derived from the simulated v1.5 (left) and v2.0 (right) survey strategies. Bottom: sky maps with a normalized color gradient (values 0–1) indicating the log10 (density of stars) based on TRILEGAL models, overlaid with the two sets of Galactic Plane pencil-beam fields represented in yellow (values 1+; see Section 2.1.1). Set 1 is plotted on the left, set 2 on the right.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: Sky maps where each HEALpix is weighted according to a priority metric for a broad combination of Galactic Plane science, presented for each filter, and including the field set 1 pencil beams.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: Maps of the combined science priority of each HEALpix region to receive at least 1309 visits during LSST (the average cadence adequate to detect variability on intermediate timescales of ∼11 days). The dark areas indicate which scientifically desirable regions are insufficiently observed. Left: baseline_v1.5. Right: baseline_v2.0.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: The percentages of the desired survey regions to receive the indicated number of visits over the 10 yr survey lifetime in the baseline_v2.0 simulation, plotted for the four categories of variability timescale.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: The percentages of the desired survey regions to receive the indicated number of visits over the 10 yr survey lifetime in the baseline_v1.5 simulation (%ofPriority metric), plotted for the four categories of variability timescale.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: Survey cadence metrics evaluated for the baseline_v2.0 strategy. Left: survey visit interval metric (VIM). Right: season visit gap metric (SVGM).
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: Percentages of desired survey regions to have ﹩{R}_{\exp }\geqslant 1.0﹩, comparing the time spent dedicated in different passbands for the baseline_v2.0 (left) and baseline_v2.1 (right) strategies.
Paper: LSST Survey Strategy in the Galactic Plane and Magellanic Clouds
Authors: R. A. Street, X. Li, S. Khakpash, E. Bellm, L. Girardi, L. Jones, N. S. Abrams, Y. Tsapras, M. P. G. Hundertmark, E. Bachelet, P. Gandhi, P. Szkody, W. I. Clarkson, R. Szabó, L. Prisinzano, R. Bonito, D. A. H. Buckley, J. P. Marais, R. Di Stefano
Figure caption: Merit function representing how the scientific value of sequential observations of time-variable objects decreases as the interval between observations exceeds the timescale characteristic of the object’s variability.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). V. The Complete SMUDGes Catalog and the Nature of Ultradiffuse Galaxies
Authors: Dennis Zaritsky, Richard Donnerstein, Arjun Dey, Ananthan Karunakaran, Jennifer Kadowaki, Donghyeon J. Khim, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: Footprint of the sky covered in all three bands by the DR9 release of the Legacy Survey (Dey et al. 2019). Observations used in this study from the northern part of the Legacy Survey are shown in tan (MzLS and BASS, jointly referred to as MB). Footprints of our previous work in Coma (Paper I), Sloan Digital Sky Survey Stripe 82 (Paper II), and the full southern region of the Survey (DECaLS and DES; Paper III) are displayed in green, red, and blue, respectively. The Galactic plane is traced by the orange curve.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). V. The Complete SMUDGes Catalog and the Nature of Ultradiffuse Galaxies
Authors: Dennis Zaritsky, Richard Donnerstein, Arjun Dey, Ananthan Karunakaran, Jennifer Kadowaki, Donghyeon J. Khim, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: Fractional redshift error vs. physical size. We plot the difference between the estimated and spectroscopically measured redshifts, divided by the redshift, as a function of inferred candidate size. The darker points represent candidates for which the estimate was within 3σ of the measured value, while those in the lighter symbols represent those for which it was not. The left panel contains results for SMUDGes candidates with spectroscopic redshifts from the Kadowaki et al. (2021) compilation and the right panel for HI-selected ultradiffuse galaxies (HUDs) from Leisman et al. (2017). The shaded area highlights the region where the candidates are no longer classified as UDGs due to their small physical size.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). V. The Complete SMUDGes Catalog and the Nature of Ultradiffuse Galaxies
Authors: Dennis Zaritsky, Richard Donnerstein, Arjun Dey, Ananthan Karunakaran, Jennifer Kadowaki, Donghyeon J. Khim, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: The distribution of candidate UDGs across the sky in R.A. and decl. The right panel is the same as the left except that we have decreased the opacity of each point to help highlight the higher density regions. We label some well-known local overdensities for reference.