adsabs/AstroCLIMB huggingface dataset:
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: VLA 3 GHz flux densities of 89 radio sources matched to the 68 SCUBA-2 source positions, as a function of corrected Poissonian probability, p (left), and as a function of the angular separation between the radio sources and the SCUBA-2 sources (right). SCUBA-2 sources with S/N > 4 are marked with blue filled circles. There are 37 multiple radio counterpart matches to 16 SCUBA-2 sources, and these are indicated with red diamond marks. After the probability cut p = 0.065 is applied, 33 multiple matches to 14 SCUBA-2 sources remain. The red vertical line is the probability cut adopted from the analysis of ALMA identifications of SMGs by An et al. (2019). With that criterion, four radio sources are removed from the radio-identified sample. Hence, in total 85 radio sources are matched to 66 SCUBA-2 sources.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: The photometric redshift distribution of radio-identified SMGs in the JWST-TDF. The red hatched histogram shows the distribution of samples at S/N > 4.0, yielding a median redshift of z = 2.22 ± 0.12 and a 16th–84th percentile range of z = 1.50−3.11. If we include the sample with 850 μm S/N = 3.5–4 (pink shaded histogram), then we derive a median redshift of z = 1.96 ± 0.08 and a 16th–84th percentile range of z = 1.44−2.70. The redshift distributions from the submm flux-limited survey (AS2UDS, blue histogram), the AS2UDS sample with radio detection and K < 22.5 mag limits applied to mimic the selection of our sample (green histogram), and finally the radio-identified SMG sample (yellow histogram) from Chapman et al. (2005) are also shown for comparison.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: Cumulative and differential number counts of the 850 μm 114 sources (S 850µm = 2–20 mJy, S/N > 3.5) in the JWST-TDF area. For comparison, we show results from previous submm surveys (Chen et al. 2013; Karim et al. 2013; Hsu et al. 2016; Geach et al. 2017; Stach et al. 2018; Simpson et al. 2019, 2020). The best-fitting results from Simpson et al. (2019, 2020), Shim et al. (2020), and Geach et al. (2017) are also presented. In general, our number counts are in reasonable agreement with those from the other surveys, although there is a slight excess at the bright end, S 850µm > 10 mJy, arising from a small number of bright sources in the field.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: A 28″ × 28″ zoomed-in image of the stacked SCUBA-2 850 μm image at the positions of the radio counterparts matched to 67 SCUBA-2 sources. The red cross is the center from the two-dimensional Gaussian fitting of each stacked image. This shows a small mean coordinate shift of 0.″83 ± 0.″22 and −0.″34 ± 0.″03 in R.A. and decl., respectively, which we corrected for in our SCUBA-2 catalog positions.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: The deboosted 850 μm flux density distribution of the 114 detected SCUBA-2 sources. SNR is the S/N from the observation. Eighty-two and thirty-two sources have S/N > 4.0 (red histogram) and S/N = 3.5–4.0 (pink histogram), respectively, and every source having a deboosted flux of >2.3 mJy is in this regime.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: The 32″ × 32″ images of the main 83 SCUBA-2 sources (S/N > 4) detected in the JWST-TDF. If the source has a radio counterpart, the label is black; otherwise, it is red. The positions of the radio counterparts are shown with blue crosses on the JCMT image and square marks on the HSC G and MMIRS Y and K images. If there is more than one counterpart lighter blue marks are also added to the figure in orders of distances. The matching radius of 7.″5 is indicated with four yellow marks. The complete set of postage stamps (14 images) is available online. The first 10 images are of the main sources; the last four are of the supplementary sources. 1 of 14 images
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: Two-dimensional density plots showing the results of 1000 jackknife simulations performed for our survey. (Left) A plot of injected sources as a function of input flux density and instrumental noise. (Middle) A density plot of completeness, the ratio of the number of recovered sources to that of injected sources, as a function of input flux density and instrumental noise. The contours are labeled with the completeness fraction. (Right) The plot shows the average boosting factor of the output flux density with the given instrumental noise. The dashed line shows the S/N = 3.5 limit. The contour labels indicate the flux boost factor.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: The best-fit MAGPHYS model SEDs for the 85 SMGs in this work that have 3 GHz radio counterparts, including the 61 sources for which we have sufficient optical and/or NIR photometry data to derive useful constraints on their SED properties. The bold frame represents the main targets at S/N > 4. We list the desired photometric redshifts and if available any spectroscopic values. The sources range within z = 0.8–3.8 and all sources show a strong FIR peak in their SEDs traced by the SCUBA-2 850 μm emission.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: Flux density distribution of observed flux (black curve) and deboosted flux (red curve) for example sources derived from the empirical recovery method. Labels with red and black colors show the median value of the corrected flux and observed flux, respectively. All results assume Gaussian uncertainties of σ inst = 1.0 mJy, which is the median instrumental noise of the final map of the TDF. For bright sources, the effect of flux boosting is minimal. But, at the limit of our catalog, it can be considerable (≃30%−50%).
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: (a) Light-curve amplitude (Δm) vs. the V-band absolute magnitude (H  V ). Green and orange symbols are TNOs and Centaurs from the LCDB (using the maximum amplitude value), blue symbols correspond to TNOs with detected periods from our K2 survey (this paper), red symbols are amplitude upper limits of TNOs without detected periods from our K2 survey (this paper, represented by 3σ  f  at f = 1 c/d), and purple symbols are K2 measurements of Gonggong (2007 OR10), 2002 GV31, and 2007 JJ43 (Pál et al. 2015, 2016). (b) Δm vs. H V relationship of K2 TNOs with a linear fit. The purple dashed–dotted and blue dashed–triple-dotted lines correspond to fits with and without Gonggong, respectively. (c) Same as panel (b) but using ﹩{H}_{\min }^{R}={m}_{110}^{R}-{\rm{\Delta }}m/2﹩ instead of H  V . The linear fits to the data with and without Gonggong are so close to each other that they are represented by a single solid line. (d) Distance modulus vs. V-band absolute magnitude.
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: Light-curve amplitude vs. estimated size of the targets in our sample. Symbols/colors are the same as in Figure 3; blue symbols with dark blue “cores” mark those targets for which the actual rotation period would indicate a density ρ ≤ 0.5 g cm−3 assuming a Jacobi ellipsoid. The region between the vertical dashed lines marks the irregular-to-spherical transition size range in the main belt. Black symbols represent the “deformed shape” light-curve amplitudes of main belt asteroids studied by Vernazza et al. (2021), and the solid black curve is the “mean” light-curve amplitude curve obtained from this sample (see the main text for a detailed explanation). The blue curves are the mean K2 TNO amplitudes considering the detections only (dashed–dotted) and also considering nondetections (solid). Orange symbols correspond to the Centaurs and TNOs whose shape and size are obtained from the combination of occultation and light-curve measurements; the dwarf planet Haumea is marked. Brown symbols represent the Centaurs from Marton et al. (2020). The solid red curve is the mean amplitude curve from Showalter et al. (2021).
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: Cumulative amplitude distribution of the K2 TNOs. The brown dashed, black solid, and purple dashed–dotted curves represent our TNO sample assuming different distributions for the nondetections, as discussed in Section 3.4 (cases 1, 2, and 3, respectively). The blue, green, and red curves correspond to the “Combined,” “Centaur,” and “OSSOS” curves in Figure 11 in Showalter et al. (2021). The pale gray and pink curves in the background show the cumulative amplitude distribution of contact binaries assuming spherical shapes, size ratios from 0.5 to 1.0, Lambert (gray) or Lommel–Seeliger (pink) scattering, and either uniform aspect angle (solid curves) or isotropic pole orientation (dashed curves) distributions for a set of simulated objects (see a more detailed discussion in Showalter et al. 2021). The yellow curve is the cumulative amplitude distribution in the main belt as derived in Masiero et al. (2009).
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: (a) Light-curve amplitude as a function of mean brightness. Blue filled circles represent the K2 TNOs with detected periods. The data of three previous K2 TNO light-curve detections (purple circles; Gonggong, 2007 JJ43, and 2002 GV31; Pál et al. 2015, 2016) are also included. Open circles show the TNOs without a detected period; in these cases, the amplitude upper limit is obtained as Δm = 3﹩{\sigma }_{f}^{1}﹩. The blue and red dashed lines represent linear fits to the light-curve amplitudes of the detections and the ﹩3{\sigma }_{f}^{1}﹩ upper limits of period nondetections, respectively. The black dashed–dotted curve corresponds to a constant flux density detection limit fitted to the nondetection upper limits with Δm = 0.0133 mag at 〈m〉 = 20 mag. (b) Distance modulus of our K2 targets vs. their mean apparent brightness.
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: Left panel: light-curve amplitude as a function of light-curve (rotational) frequency. Color coding is the same as in the previous figures; brown filled circles show the Centaurs from Marton et al. (2020). Each dashed curve represents a specific density (indicated by the numbers in units of g cm−3) that corresponds to the rotation of a strengthless body with the shape of a Jacobi ellipsoid. Right panel: same data as in the left panel, but instead of the constant density Jacobi ellipsoid curves, we show the critical density curves calculated as ﹩{\rm{\Delta }}m={({\rho }_{c}/[1\,{\rm{g}}\,{\mathrm{cm}}^{-3}])(f/[7.27\,{\rm{c}}/{\rm{d}}])}^{-2}-1﹩ (Pravec & Harris 2000).
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: Top panel: frequency distribution of asteroids. Cyan, magenta, green, and blue represent the TNOs in the LCDB and Jovian Trojans, Hildas, and TNOs from K2, respectively. Bottom panel: cumulative distribution of the same data sets as in the top panel. The gray region between the vertical black lines shows where TNOs overcome Hilda asteroids.
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: Frequency as a function of absolute magnitude. Big circles with error bars mark the median values with standard deviations for the different samples. The actual values are listed in Table 3. The boundaries of fast, slow, and very slow rotators are also shown in the figure (black dotted lines).
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: Duty cycle vs. the full length of the observations. Histograms of duty cycle and observation length are shown on the right and top of the figure, respectively.
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: For each target (one target per row), we present the phase dispersion vs. frequency in the left column. Red arrows mark the light-curve frequencies detected by our analysis. In the right panels, we show the light curves folded with the periods/frequencies identified, as listed in Table 1. The name of the target and the folding periods/frequencies are indicated.                    1 of 6 images
Paper: Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope
Authors: Viktória Kecskeméthy, Csaba Kiss, Róbert Szakáts, András Pál, Gyula M. Szabó, László Molnár, Krisztián Sárneczky, József Vinkó, Róbert Szabó, Gábor Marton, Anikó Farkas-Takács, Csilla E. Kalup, László L. Kiss
Figure caption: We present the Fourier spectrum (amplitude vs. frequency) of the light curves of targets for which no peaks in the Fourier/residual spectra matched the detection criteria, as described in Section 2.1. The blue curve represents the 1σ rms of the frequency spectrum. The name of the target is indicated in each figure.
Paper: A Spectral Solver for Solar Inertial Waves
Authors: Jishnu Bhattacharya, Shravan M. Hanasoge
Figure caption: Top left: spectrum of Rossby waves in a uniformly rotating Sun, for modes where the toroidal stream function V( x ) is symmetric about the equator. Bottom left: the same as the top left, but for modes for which V( x ) is antisymmetric about the equator. The error bars indicate the high-frequency Rossby modes detected by Hanson et al. (2022; ring-diagram spectrum). Top right: the line widths of sectoral, symmetric Rossby modes ﹩(\omega \approx \tfrac{2{\rm{\Omega }}}{m+1})﹩, as measured by Proxauf et al. (2020), compared with our results. Bottom right: the line widths of high-frequency Rossby modes from observations (Hanson et al. 2022; error bars) and our work (circles).
Paper: A Spectral Solver for Solar Inertial Waves
Authors: Jishnu Bhattacharya, Shravan M. Hanasoge
Figure caption: Left: inverse scale heights for the density (ρ) and temperature (T), multiplied by the solar radius. Right: the deviation from the adiabatic temperature gradient δ(r).
Paper: A Spectral Solver for Solar Inertial Waves
Authors: Jishnu Bhattacharya, Shravan M. Hanasoge
Figure caption: Left: the smoothed radial profile of differential rotation at the solar equator that we use in our analysis. Right: the Doppler-shifted dispersion relation of the sectoral modes (circles), and a least-squares fit assuming a uniform rotation rate Ω0 + ΔΩ0, where Ω0 is the angular velocity of the tracking frame. The horizontal dotted line in the left panel indicates ΔΩ0/2π, which is the best-fit uniform rotation rate obtained from this fit.
Paper: A Spectral Solver for Solar Inertial Waves
Authors: Jishnu Bhattacharya, Shravan M. Hanasoge
Figure caption: Left: profile of the normalized toroidal stream function V( x ) for the sectoral mode for m = 14, assuming that the Sun is rotating uniformly. The top left panel shows the angular profile at the surface, while the bottom left panel shows the depth profile at the equator. Right: the angular profiles of the various toroidal stream functions V  m (r, θ) for m = 14 at r = r out. The index n indicates the number of radial nodes.
Paper: A Spectral Solver for Solar Inertial Waves
Authors: Jishnu Bhattacharya, Shravan M. Hanasoge
Figure caption: Antisymmetric high-frequency eigenfunctions for m = 10, having a peak frequency of 175 nHz (nearest the frequency of the high-frequency ridge, as measured by Hanson et al. 2022). The fields are all in units of velocity, although within an arbitrary overall normalization factor.
Paper: A Spectral Solver for Solar Inertial Waves
Authors: Jishnu Bhattacharya, Shravan M. Hanasoge
Figure caption: The first few basis functions chosen to satisfy the boundary conditions on V  ℓ (r) (left), W  ℓ (r) (middle), and ﹩{S}_{{\ell }}^{{\prime} }(r)﹩ (right).
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: DECaPS2 source-density map (using a HEALPix grid at NSide = 512) in r band (top) and z band (bottom) using a common, logarithmic color scale. This figure employs a cut requiring sources be brighter than 19th magnitude in the reported band and be detected in at least one of the two immediately adjacent bands.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Histogram (2D) for injected source tests as a function of the true injected S/N (s 0) and fractional error in recovered flux using either flux (left) or cflux (right). Color scale is logarithmic density (light, white, low; dark, blue, high density) with gray indicating 0 density. All panels include a cut selecting for unblended sources (see text). The green line shows the binned trimmed (excluding the highest and lowest 10%) mean as a function of S/N, and the white-dashed line provides the zero-error reference.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Mollweide projection in Galactic coordinates of large survey footprints with spatial or photometric coverage overlapping DECaPS2. The boundaries of each footprint are shown with shading on the side the survey covers. Gaia, 2MASS, and WISE are not shown because they are all sky surveys.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Comparison of DECaPS2 and DECaPS1 catalogs on three representative fields: in a low-reddening calibration field, (ℓ, b, Δθ) = (236°, −14°, 3°); in the Galactic plane, (ℓ, b, Δθ) = (−65°, 0°, 0.°5); and in the Galactic bulge, (ℓ, b, Δθ) = (−5°, 2°, 0.°5). Δθ is the angular radius of the circular field. The color scale is in log-density, and each panel has its own normalization (light, white, low; dark, blue, high density). Lines indicate quartiles in the y-axis per x-axis bin with 25% and 75% in black and 50% (the median) in green. Outlier robust center (median) and scatter (σ IQR) metrics are shown for stars between 15th and 17th mag.