adsabs/AstroCLIMB huggingface dataset:
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Left panels: LS periodograms performed on the g′- and r′-band light curves of J2117-B acquired with ZTF. Right panels: ZTF optical light curves of J2117-B folded at the photometric period P ZTF = 0.2209805 days and reference epoch T 0 = 58745.308 MJD.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Left panels: PDM periodograms performed on the g′- and r′-band light curves of J2117-A acquired with ZTF. Right panels: ZTF optical light curves of J2117-A folded at the photometric period P ZTF = 0.12664 days and reference epoch T 0 = 59025.415 MJD.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: 3FGL J0737.2−3233 field of view observed with LCO/Sinistro. 3FGL and 4FGL 95% error ellipses are shown in yellow and cyan, respectively, while the spider candidate is highlighted in green.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: 3FGL J2117.6+3725 field of view observed with INT/WFC. 3FGL and 4FGL 95% error ellipses are shown in yellow and cyan, respectively, while the two spider candidates are highlighted in green.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: 3FGL J2221.6+6507 field of view observed with STELLA/WiFSIP. The 3FGL 95% error ellipse is shown in yellow, while the spider candidate is highlighted in green and the two other periodic variables are reported in orange.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Top panel: ZTF g′- and r′-band light curves of J2117-B folded with the assumed orbital period P orb = 0.441961 days and reference epoch T 0 = 58745.308 MJD, where two cycles are shown for display purposes. Bottom panel: observed ﹩(g^{\prime} -r^{\prime} )﹩ color curve of J2117-B.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Top panel: ZTF g′- and r′-band light curves of J2117-A folded with the assumed orbital period P orb = 0.25328 days and reference epoch T 0 = 59025.415 MJD, where two cycles are shown for display purposes. Bottom panel: observed ﹩(g^{\prime} -r^{\prime} )﹩ color curve of J2117-A.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Fermi-3FGL/4FGL fields of view observed with STELLA/WiFSIP (1.2 m).
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: (continued).
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Fermi-3FGL/4FGL fields of view observed with LCO/Sinistro (1 m) and LCO/SBIG (0.4 m).
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Fermi-3FGL/4FGL fields of view observed with INT/WFC (2.5 m).
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption:  σ vs. Δm plots for each of the 33 COBIPULSE fields of view.
Paper: COBIPULSE: A Systematic Search for Compact Binary Millisecond Pulsars
Authors: Marco Turchetta, Manuel Linares, Karri Koljonen, Jorge Casares, Paulo A. Miles-Páez, Pablo Rodríguez-Gil, Tariq Shahbaz, Jordan A. Simpson
Figure caption: Phase-folded optical light curves for each of the 17 COBIPULSE periodic variables.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Stellar irradiation received by TRAPPIST-1e in our model. The black dot represents the substellar point, which is fixed at 180° longitude and 0° latitude over the Pacific Ocean. The black outlines represent the land masses.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Cross section of O x  production rate on the meridional plane passing through the substellar point for our TRAPPIST-1e model. The white region on the plot indicates zero production rate.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Horizontal slices of the O3 number density for our TRAPPIST-1e model at a pressure (altitude) of (a) 103 hPa (∼15 km) and (b) 609 hPa (∼5 km). The substellar point is at 180° longitude and 0° latitude. N represents the north pole and S represents the south pole. Lower panels show the polar projections.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Catalytic species concentration on the meridional plane passing through the substellar point for (a) OH, (b) HO2, (c) NO, (d) NO2, (e) Cl, and (f) Br for our TRAPPIST-1e model. The catalytic species are roughly symmetrically distributed, and their concentrations are lower than the O3 concentrations.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Stellar irradiance at top of the atmosphere of TRAPPIST-1e (orange) and Earth (blue). The orange shaded region represents the range of UV wavelengths.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Time taken by the catalytic species to destroy O3 on the meridional plane passing through the substellar point for our TRAPPIST-1e model.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Zonal-mean latitudinal variation of TOC density for our TRAPPIST-1e model (blue) and Earth (orange).
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Cross section of the O3 number density on the meridional plane passing through the (a) substellar point and (b) antistellar point for our TRAPPIST-1e model.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: High-resolution (8.″5) uGMRT images at 400 (left) and 675 MHz (right) overlaid with contours. The image properties are listed in Table 1; see labels IM2 and IM5. The contours are drawn at levels [−1, 1, 2, 4, 8, …] × 3σ rms. Negative contours are shown with dashed lines.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: 400 MHz high-resolution uGMRT image of the Sausage cluster. The image properties are listed in Table 1; see label IM1. The source labels are adopted from G. Di Gennaro et al. (2018).
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: uGMRT 400 MHz image, same as Figure 2 (left panel), with regions indicating individual diffuse radio sources over which integrated flux densities are estimated.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: High-resolution (8.″5) spectral index map between 400 and 675 MHz of the RN, R5, and R3 relics. The images used to make this map are IM2 and IM5 in Table 1. The contours overlaid on the map correspond to the 400 MHz image (IM2) and are drawn at levels [−1, 1, 4, 16, …] × 4σ rms.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Helmholtz rotational eddy winds at pressures (a) 20, (b) 103, and (c) 800 hPa. Arrows represent wind velocity vectors and point in the direction of flow, with the length of the arrows representing the magnitude of the wind speed (with the mean wind speed shown in the top right corner of each plot).
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Meridional mass streamfunction on the meridional plane passing through the (a) substellar point and the (b) antistellar point for our TRAPPIST-1e model. The positive values (red) indicate clockwise circulation and the negative values (blue) indicate counterclockwise circulation. The values are in log scale.
Paper: Asymmetries in the Simulated Ozone Distribution on TRAPPIST-1e due to Orography
Authors: Anand Bhongade, Daniel R Marsh, Felix Sainsbury-Martinez, Gregory Cooke
Figure caption: Helmholtz divergent winds at pressures (a) 20, (b) 103, and (c) 800 hPa. Arrows represent wind velocity vectors and point in the direction of flow, with the length of the arrows representing the magnitude of the wind speed (with the mean wind speed shown in the top right corner of each plot).
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Zoomed-in high-resolution 400 MHz image (IM1), shown in Figure 1, focusing on the southern relic. The arrows trace the component relic extents. The black “X” marks the location of the optical counterpart of a cluster member galaxy [DJS2015] J224231.818+525622.413 (W. A. Dawson et al. 2015).
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: (Left) Zoomed-in 400 MHz image (Figure 2 left panel) in linear scale, showing the different features of the R1 and R4 relics. (Right) High-resolution (8.″5) spectral index map between 400 and 675 MHz of the R1 and R4 relics. The images used to make this map are IM2 and IM5 in Table 1. The contours overlaid on the map correspond to the 400 MHz image (IM2), and are drawn at levels [−1, 1, 2, 4, 8, …] × 3σ rms. The circular regions of beamwidth are used to extract the spectral index and brightness profiles of the R1 (red) and R4 (magenta) relics. These profiles are presented in Figure 9.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: (Top) East–west spectral index profile of the RN relic, extracted from the spectral index map in Figure 4 within circular regions of the beam size, i.e., width = 8.″5. (Bottom) Zoomed-in 400 MHz image, shown in Figure 2 (left panel), focusing on the northern relic. The red circular regions are used for the spectral index profile shown in the top panel. The black sectors show the regions where we extracted spectral index profile across the RN relic width, whereas the blue and magenta sectors show the same for the R3 relic. These profiles are shown in Figure 6.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Spectral index profiles across the width of the RN and R3 relics. The regions within which these profiles are extracted are shown in Figure 5, with the width of the rectangular boxes being 8.″5.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: (Left) Zoomed-in 400 MHz image, shown in Figure 2 (left panel), focusing on relic R3. (Right) Low-resolution (15″) spectral index map of the R3 relic between 400 and 675 MHz. The images used to make this map are IM3 and IM6 in Table 1. The contours overlaid on the map correspond to the 400 MHz image (IM3), and are drawn at levels [−1, 1, 2, 4, 8, …] × 3σ rms.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Schematic representation of the shock components possibly associated with the different relics in the “Sausage” cluster. The different possible shock pairs are indicated with different colors.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Zoomed-in 400 MHz image in Figure 2 (compact sources unsubtracted), focusing on source I. The white “X” marks the location of a cluster member galaxy [DJS2015] J224248.254+530849.495 (W. A. Dawson et al. 2015).
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: North–south spectral index and brightness profiles of the R1 (left) and R4 (right) relics, corresponding to the regions shown in Figure 8.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Zoomed-in 400 MHz image in Figure 2 (compact sources unsubtracted), focusing on relic R5.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Low-resolution (15″) uGMRT image at 400 MHz overlaid with contours. The image properties are listed in Table 1; see label IM3. The contours are drawn at levels [−1, 1, 2, 4, 8, …] × 3σ rms. Negative contours are shown with dashed lines. The circular regions with beamwidth are used to extract spectral index profiles of the RS1 (red), RS3 (blue), and RS4 (black) relics. The RS5 relic profile is extracted with circles of width 30″, indicated in magenta color. These profiles are presented in Figure 18.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Low-resolution (15″) uGMRT image at 675 MHz overlaid with contours. The image properties are listed in Table 1; see label IM6. The contours are drawn at levels [−1, 1, 2, 4, 8, …] × 3σ rms. Negative contours are shown with dashed lines.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: (Left) Low-resolution (15″) spectral index map of the southern relic RS between 400 and 675 MHz. The images used to make this map are IM3 and IM6 in Table 1. The contours overlaid on the map correspond to the 400 MHz image (IM3), and are drawn at levels [−1, 1, 2, 4, 8, …] × 3σ rms. (Right) Spectral index profile of the RS relic, combining the RS1, RS3, and RS4 regions shown in Figure 15.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Spectral index profiles of the RS1 (top left), RS3 (top right), RS4 (bottom left), and RS5 (bottom right) relic, corresponding to the regions shown in Figure 15.
Paper: uGMRT Sub-GHz View of the Sausage Cluster Diffuse Radio Sources
Authors: Ramij Raja, Oleg M. Smirnov, Tiziana Venturi, Majidul Rahaman, H.-Y. Karen Yang
Figure caption: Spectral index uncertainty maps corresponding to Figure 4 in (top left) panel, Figure 8 in (top right) panel, Figure 11 in (bottom left) panel, and Figure 14 in (bottom right) panel.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Completeness of dwarf galaxy detection based on the injection of >3000 artificial dwarfs (>40 per bin in the figure). For comparison, we show the positions of known Milky Way (circles) and M31 (triangles) dwarfs from the Local Volume Database. NGC 2403's satellite MADCASH-1 is shown as a large star with black outline; DDO 44 is much brighter than the upper limit we explored with artificial dwarfs and thus outside the boundaries of this figure. Diagonal lines represent constant surface brightness values, ranging from 24 to 32 mag arcsec−2. The gray dotted line is the interpolated M  V –r half relation from C. M. Brasseur et al. (2011), which we use to extract the LF corrections applied to Figure 9. Our data set and search sensitivity should recover most typical dwarfs brighter than M  V  < −7.0 and ﹩{\mu }_{{\rm{V}}}\lesssim 30\,\mathrm{mag}\,{\mathrm{arcsec}}^{-2}﹩ and some fraction at even fainter absolute magnitudes.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Example images of synthetic dwarfs that were injected into the images to measure our recovery rate. Images are 1′ on a side, corresponding to a projected physical width of ∼870 pc at a distance of 3 Mpc. Each row shows dwarfs with fixed values of surface brightness, with μ  =  26.0, 27.5, 29.0 mag arcsec−2 in the top, middle, and bottom rows. From left to right, injected dwarfs have M  V  = −6.5, −7.5, −8.5 in each row. However, the middle panel has been replaced with an image of the MADCASH-1 dwarf, which has μ  =  26.7 mag arcsec−2 and M  V  = −7.8. All of the dwarfs shown in this figure were recovered by our search. Our injected dwarf recovery fractions for similar dwarfs were 23%, 34%, and 63% for the top panels; 26% and 67% for the left- and right-hand panels in the middle row; and 26%, 57%, and 72% for the dwarfs in the bottom row. The bin in Figure 8 corresponding to MADCASH-1 had a recovery rate of 74%.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Satellite LF of NGC 2403. The filled bands represent predicted satellite populations for LMC-mass hosts from I. M. E. Santos-Santos et al. (2022, blue) and G. A. Dooley et al. (2017, orange). The shaded regions for both comparisons represent the 1σ variation in the number of satellites over the model realizations. The predicted LFs have been corrected for dwarf detection completeness as well as a volume correction to account for the observational incomplete coverage of the virial volume (see Section 5 for details).
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: The final 10σ point-source depths as a function of position from our Subaru/HSC data set. The upper panel shows the g-band depth, and the lower panel depicts i-band depth. There is as much as ∼1 mag of variation in depth over the footprint, which is mostly due to different observing conditions (e.g., seeing; see Table 3) at the time the images were obtained.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Map of selected RGB star candidates, shown here as the RGB number density “signal-to-noise” above the local background, ﹩(N-{N}_{\mathrm{bg}})/\sqrt{{N}_{\mathrm{bg}}}﹩. DDO 44 and its tidal stream (J. L. Carlin et al. 2019) are prominent in the northern region of this panel. The faint satellite MADCASH-1 (J. L. Carlin et al. 2021) is visible (and circled in white) as a small overdensity to the east (and slightly south) of the main body of NGC 2403. The black cross (×) to the SE of NGC 2403 is MCG+11-10-022, and the one slightly SW is UGC-3894. The outskirts of NGC 2403are otherwise fairly featureless, with no obvious stellar streams or tidal debris structures visible. A rough estimate based on the background density and mean flux of RGB candidates suggests that these data should be sensitive to streams with surface brightnesses as faint as μ V ∼ 32 mag arcsec−2.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Absolute K-band luminosity (M K) vs. distance for Local Volume galaxies from the catalog of I. D. Karachentsev et al. (2013). MC analog host galaxies (i.e., galaxies with stellar masses ﹩\tfrac{1}{3}{M}_{* ,\ \mathrm{SMC}}\lt {M}_{* }\lt 3{M}_{* ,\ \mathrm{LMC}}﹩) targeted by the MADCASH and DELVE-DEEP surveys are highlighted, with the subject of this work (NGC 2403) shown as a blue star.