adsabs/AstroCLIMB huggingface dataset:
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Top: heliocentric-corrected velocities (cz) and projected distances of galaxies in the proximity of SAGA host galaxies. The velocity and distance plotted for each galaxy are calculated with respect to their individual hosts. The gray error bars in the upper left corner show the typical velocity errors. We define satellites (green-filled squares) as galaxies that lie in the SAGA footprint (within 300 kpc in projection) and within ±275 km s−1 of their host galaxies; these criteria are indicated by dotted lines. Galaxies in the SAGA footprint that do not meet the velocity criterion are considered to be background galaxies (purple-filled triangles). In this plot, we also show galaxies that are beyond 300 kpc in projection (i.e., outside the SAGA footprint, yellow-filled circles). The red solid lines show the circular velocity of an NFW profile with M vir = 2 × 1012 M ⊙ and c = 10. Note that our satellite definition does not guarantee the satellites are gravitationally bound to the host. The survey did not attempt to obtain any redshifts within 10 kpc of the host galaxy (indicated as the gray vertical band on the left). Bottom: the velocity dispersion of objects within the satellite velocity selection window, in bins of projected distance.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Left: the average satellite SMF of the 101 SAGA systems, shown in the differential form (﹩d\,\langle {N}_{\mathrm{sat}}\rangle /d\,\mathrm{log}{M}_{\star }﹩). The darker solid curves show the SMF when survey incompleteness is taken into account, while the fainter dashed curves show only confirmed satellites. The curves with black-filled triangles, blue-filled circles, and red-filled squares show all satellites, only star-forming satellites, and only quenched satellites, respectively. The gold-dotted and silver-dotted–dashed vertical lines show the corresponding stellar mass limits of the Gold and Silver samples. These SMF data points are provided in Table C5. Right: same as the left panel, but comparing the SAGA satellite SMF (black-filled triangles) with the ELVES survey (orange crosses; Carlsten et al. 2022) and a constant slope of −0.43 (green dotted line; typically quoted as α = −1.43, see Nadler et al. 2020). Both SAGA and ELVES SMFs are corrected for survey incompleteness; the uncorrected SMFs are shown as gray and faint orange-dashed lines, respectively. The error bars near the right border of both panels show the Poisson error on the SAGA SMF.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Left: the effective surface brightness–mass distribution of confirmed SAGA satellites; the large blue-filled circles and large red-filled squares show star-forming and quenched satellites, respectively. The small and fainter markers show a random realization of satellites that we may have missed in the Gold and Silver samples, according to our incompleteness model; the color of the small markers indicates whether the missed satellites are star forming (blue) or quenched (red). The gold and silver vertical lines show the corresponding stellar mass limit of the Gold and Silver samples. Right: stacked histograms, in bins of effective surface brightness, of the confirmed (dark) and potentially missed (faint) satellites in the Gold and Silver samples, separated by whether the satellites are star forming (blue) or quenched (red).
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Distribution of the K-band absolute magnitudes (x-axis; Jarrett et al. 2000), stellar masses (y-axis), and g − r colors (color of the markers) of 101 SAGA host galaxies. The filled circles and square markers indicate regular and Local Group–like hosts, respectively (here Local Group–like means having exactly one MW-mass companion within 1 Mpc). Filled square markers that are connected by a thin dotted line are Local Group–like pairs. The black star and plus sign show the luminosities and stellar masses of the MW and M31, respectively.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Top: a stacked histogram of confirmed redshifts of galaxies in the SAGA footprint (defined in Section 2.2). The olive and pink colors in the stacked histogram show the number of spectra collected by the SAGA team and from the literature, respectively. The inset shows the same data, but zoomed in on the z < 0.04 region. Bottom: the percentage of galaxy redshifts first obtained by the SAGA Survey, in bins of redshift (x-axis) and r-band magnitude (y-axis), represented by the color of the cell (darker olive indicates more SAGA-obtained redshifts, darker pink indicates more literature redshifts). The size of each cell represents the total number of redshifts in the corresponding bin.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Images of 378 satellites, sorted by M  r,o  within each of the 101 complete systems that have satellites. Four of the 101 systems have the same level of survey completeness but do not have any confirmed satellites. The images of host galaxies are not included. The colors of the frames are assigned by the number of satellites. Images are taken from DESI Imaging DR9 (Dey et al. 2019). The width and height of each image correspond to 40″.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Distribution of stellar masses (x-axis; shown as ﹩\mathrm{log}[{{M}}_{\star }/{{M}}_{\odot }]﹩) and spectroscopic redshifts (y-axis) of galaxies in the SAGA footprint and within z < 0.05. The satellites (as defined in Section 4.3) are shown in green and all other galaxies (background) are shown in purple. The main panel shows the joint distribution with contours indicating density and points indicating individual galaxies in low-density regions. The two side panels show the stacked histograms of stellar masses (top panel) and redshifts (right panel).
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Sky distribution of 203 SAGA MW analog systems as defined in Section 2.2. Orange-filled squares show the 101 systems that have been surveyed and are presented in this work. Empty circles show systems that match our host selection (i.e., from the Grand List with criteria Equations (1a)–(1g) applied) but have not been surveyed.
Paper: Radio Morphology of Gamma-Ray Sources: Double-lobed Radio Sources
Authors: Vaidehi S. Paliya, D. J. Saikia, Alberto Domínguez, C. S. Stalin
Figure caption: The histograms of the core dominance (panel (a)), radio power (panel (b)), and redshift (panel (c)) for the 149 misaligned AGN found in this work. In the top left panel, the blue-dotted and red-hatched histograms refer to objects whose optical spectra exhibit broad emission lines and host galaxy absorption features or narrow emission lines, respectively. In the top middle and right panels, these correspond to objects showing FR I and II morphologies, respectively, as found in this work. Panel (d) shows the γ-ray luminosity vs. photon index plot for Fermi-LAT detected jetted sources. The panels (e) and (f) correspond to the WISE color–color diagram and total radio power versus projected jet length plot, respectively. In all the panels, the γ-ray detected misaligned AGN are highlighted with filled cyan stars. The filled triangles shown in panel (e) refer to the upper limit in the W3-band magnitude. The gray data points belong to the Fermi-LAT blazars (panel (d)) and LOFAR-detected sources (panels (e) and (f)).
Paper: Radio Morphology of Gamma-Ray Sources: Double-lobed Radio Sources
Authors: Vaidehi S. Paliya, D. J. Saikia, Alberto Domínguez, C. S. Stalin
Figure caption: The VLASS contours overplotted on PanSTARRS i-band images of one of the γ-ray emitting AGN exhibiting double-lobed radio structure (top panel). Along with the 4FGL name, we also mention the classification reported in the 4FGL-DR4 catalog (S. Abdollahi et al. 2022). The radio morphologies observed by other surveys, when available, are plotted in the middle panel. In all plots, the contour levels start at 3 × rms × (−2, ﹩-\sqrt{2}﹩, −1, 1) and increase in multiple of ﹩\sqrt{2}﹩. The bottom panel shows the optical spectrum of the source when available. By default, the north is up and east to the left. For DECAM optical images, we have added a compass to guide the eye. The references for the shown optical spectra are provided in Table 1. The complete figure set is available on ZENODO (doi:10.5281/zenodo.13908693).
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Left panel (a): relationship between metallicity and stellar surface mass density (Σ*–Z gas). The solid red circles represent spaxels belonging to the ALM region, satisfying the criterion of ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})\lt -5{\sigma }_{Z}﹩ (σ  Z  = 0.037 from Y. Luo et al. 2021), which corresponds to the red vertical dashed line in the right panel (b). The open red and gray circles show the spaxels with ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})\gt -3{\sigma }_{Z}﹩ and ﹩-3{\sigma }_{Z}\lt {\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})\lt -5{\sigma }_{Z}﹩, respectively. The gray dots and curves are from Y. Luo et al. (2021) in two low-mass bins. Right panel (b): distribution of the metallicity deviation ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩ in star-forming spaxels. The gray dashed curve represents the distribution in galaxies with M * > 109  M ⊙, which is compiled from Y. Luo et al. (2021). The gray solid curve shows the distribution in dwarf (M * < 109  M ⊙) galaxies, assuming that ∼2% of dwarf galaxies in the SDSS-IV MaNGA survey behave like PGC 44685. The blue histogram is the total distribution of both. We fit only the positive side of the blue histogram to derive the symmetric negative side using a Gaussian profile. The orange line shows the best-fit Gaussian profile, with a standard deviation of ﹩{\sigma }_{Z}^{{\prime} }=0.037﹩, which is the same value (σ  Z  = 0.037) obtained in Y. Luo et al. (2021). The shaded region shows the ﹩\pm {\sigma }_{Z}^{{\prime} }﹩ coverage around the center of the Gaussian distribution. The vertical dashed lines mark the locations where ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})=-5{\sigma }_{Z}﹩ (red) and where ﹩{\rm{\Delta }}{\rm{log}}({\rm{O}}/{\rm{H}})=-3{\sigma }_{Z}^{{\rm{{\prime} }}}=3{\sigma }_{Z}﹩ (orange), respectively. We refer to those spaxels that deviate from a lower metallicity by more than the former value as ALM spaxels.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Distributions of the physical parameters color-coded by the BPT diagram (panel (a)), Hα flux (panel (b)), the ratio of Hα to Hβ (panel (c)), and gas-phase metallicity based on the RS32 method (panel (d)), respectively. All spaxels satisfy the criteria of SNR > 5 for both stellar and emission components. The black plus marks the galaxy center. The black polygons mark the found W-R region (see Section 3.1). Three dotted circles in panels (b) and (d) represent triple star-forming regions with labels A, B, and C, identified by the Hα distribution in Section 3.3. The W-R region is located within region C. White dots in panel (d) illustrate the ALM region with ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})\lt -0.185﹩ (see Section 3.2 and Figure 5 for details).
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: The stacked W-R spectrum (in a black curve) summing all 20 spectra with W-R features. Panel (a) shows the spectrum in a large range of wavelengths. The shaded blue and red regions represent the W-R blue and red bump regions, respectively. The zoom-in spectra are shown in panels (b) and (c), separately. Orange curves are windows used to fit the continuum. The best linear fitting indicates the best-fit continuum, shown by the black line. Broad Gaussian components in solid blue curves and narrow Gaussian components in solid green curves are overlaid on the best-fitting continuum. The red lines imply the final best-fit profiles, i.e., all Gaussian components plus the linear-fit continuum. Colored vertical dashed lines illustrate the wavelength centers of emission lines within the bump ranges, and corresponding legends are printed in the top right corner of each panel. Panels (d) and (e) show their residual spectra after subtracting the continua and Gaussian components. The clear residuals imply that the fitting is appropriate.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Optical grz image of PGC 44685 with triple star-forming regions from DESI Legacy Imaging Surveys (A. Dey et al. 2019). White contours show the corresponding Ks -band image observed by VISTA/VIRCAM. The closed black polygonal region represents the strongest star-forming region with W-R features (see Section 3.1). The white plus sign marks the center of the galaxy. Three dotted circles represent three star-forming regions (labeled A, B, and C, respectively), identified by the Hα distribution in Section 3.3.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Left: distribution of ﹩{\gamma }_{\max }﹩ and particle age for jet simulation Std90 at time t = 50. The colors indicate the location of the respective particle in the 3D jet MHD structure. (i) Red indicates the recollimation shock (RS) from z = 6.4–10, (ii) sky blue indicates the strong, steady shock (SS) from z = 10.8–16, (iii) dark green indicates the Mach shock (MS) from z = 26.8–28, (iv) orange indicates the region from the base of the jet up to the recollimation shock from z = 0–6.4, (v) brown indicates the region beyond the recollimation shock up to the strong steady shock from z = 10–10.8, (vi) light green indicates the region beyond the strong steady shock up to the Mach shock from z = 16–26.8, (vii) pink indicates the region beyond the Mach shock to the jet termination for z > 28, and (viii) yellow indicates the particles in the cocoon and the backflow for radii R > 2. Right: the SEDs for the different particle populations, as shown on the left. The color of the SEDs here indicates the same particle populations as shown left. The black dotted line represents the cumulative SED, considering all the particles in the domain, and thus the “core” SED.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption:  GALFIT-fitting results in the R band. The left to right panels present the original R-band image observed at the Palomar Observatory 60 inch telescope (A. Gil de Paz et al. 2003), the best-fit model by adopting a Sérsic profile, and the residual after subtracting the best-fit model from the original image, respectively. The center in the best fit is shown in the red cross, which is aligned with the galaxy center in the white plus sign, derived from the Ks -band isophote in Figure 2.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Left: histogram showing ﹩{\gamma }_{\max }﹩ and the age of injected particles for simulations Std90 (top), Var90 (center), and Prc90 (bottom) at time t = 50. The color bars (in log scale) indicates the number of particles with a particular value of ﹩{\gamma }_{\max }﹩ and age. The boxes with colored boundaries therein enclose different populations of particles. Right: the SEDs for different populations of particles for simulations Std90 (top), Var90 (center), and Prc90 (bottom) at time t = 50. The color of the SEDs here indicates the population of those particles enclosed within the boxes of corresponding colors, as shown in the left panel. The black dotted line represents the “core” SED, considering all the particles in the domain.
Paper: PGC 44685: A Dwarf Star-forming Lenticular Galaxy with a Wolf–Rayet Population
Authors: Shiying Lu, Qiusheng Gu, Yulong Gao, Yong Shi, Luwenjia Zhou, Rubén García-Benito, Xiangdong Li, Jiantong Cui, Xin Li, Liuze Long, Zhengyi Chen
Figure caption: Stacked ALM spectra in three star-forming regions. The panels from top to bottom show the summed ALM spectra in regions A, B, and C, respectively. These star-forming regions are classified in Section 3.3. The continuum and emission are fitted using the same method as in Section 3.1.
Paper: Why Do Semianalytic Models Predict Higher Scatter in the Stellar Mass–Halo Mass Relation Than Cosmological Hydrodynamic Simulations?
Authors: Antonio J. Porras-Valverde, John C. Forbes, Rachel S. Somerville, Adam R. H. Stevens, Kelly Holley-Bockelmann, Andreas A. Berlind, Shy Genel
Figure caption: The stellar mass scatter—computed as half the 16th–84th interpercentile range—at fixed halo mass ﹩(\sigma ({\mathrm{log}}_{10}({M}_{* }| {M}_{h})))﹩ as a function of halo mass for central galaxies. The top panel shows literature results from: (a) observations of X-ray measurements shown in dark slate blue octagons (A. V. Kravtsov et al. 2018), satellite kinematics shown in gray pentagons (J. U. Lange et al. 2019), and black squares (S. More et al. 2011); (b) empirical models from A. P. Hearin & D. F. Watson (2013), R. M. Reddick et al. (2013), M. R. Becker (2015), Y. Zu & R. Mandelbaum (2015), J. L. Tinker et al. (2017), P. Behroozi et al. (2019), J.-z. Cao et al. (2020), and C. H. To et al. (2020) are shown as dashed lines using varying light colors; (c) SAMs from R. S. Somerville et al. (2012). (Note that this version of the SANTA CRUZ SAM uses the extended Press–Schechter formalism for the dark matter merging histories. Therefore, this is not included in Table 1.) Y. Lu et al. (2014), B. M. B. Henriques et al. (2015), and D. J. Croton et al. (2016) are shown as solid lines with varying green shades, and (d) cosmological hydrodynamical simulations from N. Khandai et al. (2015), S. McAlpine et al. (2016), and A. Pillepich et al. (2018) are shown as dotted lines with different blue shades. Several lines are taken from both R. H. Wechsler & J. L. Tinker (2018) and J.-z. Cao et al. (2020). Note that, for R. M. Reddick et al. (2013), J. L. Tinker et al. (2017), J. U. Lange et al. (2019), J.-z. Cao et al. (2020), and C. H. To et al. (2020), the extent displayed in the x-error bar is the range of halo masses estimated to be probed with each study. Both top and bottom panels include the same DARK SAGE fiducial line in purple. The bottom panel shows the experimental modifications to DARK SAGE when we turn off disk instabilities (orange), quasar (green), and radio (pink) mode feedback. Below the quenching mass, the stellar mass scatter is significantly larger in DARK SAGE fiducial compared to TNG and most models. We find that, when we turn off radio mode feedback, the scatter in stellar mass at fixed halo mass reduces significantly at all halo masses.
Paper: Why Do Semianalytic Models Predict Higher Scatter in the Stellar Mass–Halo Mass Relation Than Cosmological Hydrodynamic Simulations?
Authors: Antonio J. Porras-Valverde, John C. Forbes, Rachel S. Somerville, Adam R. H. Stevens, Kelly Holley-Bockelmann, Andreas A. Berlind, Shy Genel
Figure caption: Stellar mass as a function of halo mass for central galaxies using: DARK SAGE fiducial (purple), TNG (blue; left panel), and DARK SAGE when we turn off disk instabilities, radio, and quasar mode feedback (red, violet, and green, respectively on the right panel). For all our models, we use a bin size of 0.1 dex to show the median SMHMR and scatter. The black line on the right panel shows Y. Zu & R. Mandelbaum (2015)'s SMHM empirical relation taken from observational constraints from galaxy–galaxy lensing and galaxy clustering. All solid lines connecting the dots show the median value binned by halo mass. The shaded regions enclose 68% of the data. Above the quenching mass, DARK SAGE fiducial galaxies trace TNG's SMHMR. Below that mass, DARK SAGE overproduces stellar mass galaxies. Surprisingly, when we turn off radio mode feedback and instabilities, the scatter in stellar mass at fixed halo mass reduces significantly at all halo masses. Additionally, all models predict different slopes.