adsabs/AstroCLIMB huggingface dataset:
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: ALMA 1.2 mm views of z ≳ 9 galaxies in UNCOVER. RGB NIRCam color cutouts (3″ × 3″) for spec-z confirmed galaxies presented in S. Fujimoto et al. (2024b; hereafter F24) and photometric galaxies presented in H. Atek et al. (2023a; hereafter A23) at z ≳ 9. The white bars mark the z ≳ 9 galaxies, and the inset labels present their IDs and their zspec or zphot estimates in F24 or A23. The green (white) contours denote 2.0σ, 2.5σ, and 3.0σ (−2.0σ, −2.5σ, and −3.0σ) significance levels of the ALMA 1.2 mm continuum in the natural map. F24-26185 has been reported to be an X-ray AGN at z ∼ 10 (A. Bogdan et al. 2024) and confirmed at z = 10.07 (see also A. D. Goulding et al. 2023). Interestingly, the marginal ALMA detection (∼2.6σ) coinciding with the source position is identified only in F24-26185, implying an early active coevolution of the central black hole and its host at z > 10.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: [C II] line emitter at z = 6.33 serendipitously detected (SNR = 7.0 with an aperture) in the ALMA data cube of DUALZ. Left panel: RGB NIRCam color cutout (5″ × 5″) centered on the [C II] emitter. The green (red) contours indicate the 2σ, 3σ, 4σ, 5σ, and 6σ (2σ, 2.5σ, 3σ, and 3.5σ) significance levels of the velocity-integrated [C II] (dust continuum) intensity. The white ellipse denotes the ALMA synthesized beam. In the NIRCam map, three components are detected within a ﹩0\mathop{.}\limits^{^{\prime\prime} }5﹩ radius, with zphot values for all three components within z ∼ 5.9–6.6. The inset labels show the properties of the nearest NIRCam counterpart. Right panel: ALMA Band6 spectrum for the [C II] emitter with the Deep-natural cube. The red dashed curve presents the best-fit Gaussian for the line emission, and the inset label denotes the best-fit line properties. The inset panel shows the comparison between z[CII] and P(z) obtained from the Prospector fit for the nearest NIRCam counterpart.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Cumulative [C II] luminosity function from recent [C II] line studies at z ∼ 5–6. The red circle shows the volume density of the [C II] line emitter, based on our single successful detection in DUALZ (Section 4.3). The lower limit is estimated from the Poisson uncertainty at the single-sided confidence level of 84.13%, as presented in N. Gehrels (1986). Recent ALMA blind line survey results are indicated by the blue triangle (243 archival data cubes; Matsuda et al. 2015), blue inverse triangle (four lensing clusters; Y. Yamaguchi et al. 2017), blue square (ASPECS; R. Decarli et al. 2020; B. D. Uzgil et al. 2021), and blue cross (SSA22; N. H. Hayatsu et al. 2017, 2019), respectively. The green circle denotes the ALPINE results (F. Loiacono et al. 2021). The magenta square and pentagon show the serendipitous [C II] line detection from bright SMGs at z ∼ 5 reported in A. M. Swinbank et al. (2012) and E. A. Cooke et al. (2018), respectively. The red shaded regions indicate the current constraints based on both our results and those previously obtained. For comparison, we also present the semianalytical model results (G. Popping et al. 2016; G. Lagache et al. 2018) and the SFR function (SFRF; R. Smit et al. 2018), including the dust correction, whose SFR value is converted into L[C II] using the local empirical relation (I. De Looze et al. 2014).
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: The 2D (top) and 1D (bottom) JWST/NIRSpec prism spectra taken for the [C II] line emitter at z = 6.33. The inset panel shows the NIRCam RBG 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 × 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 cutout, where the three shutter positions are overlaid. The inset label shows its MSA ID and our best-fit redshift estimate from the prism spectrum. The red horizontal dashed lines in the top panel indicate the extraction aperture for the 1D spectrum. The black and red curves in the bottom panel denote the extracted 1D spectra and the best-fit EAZY template (see the text). The green vertical lines represent wavelengths of the emission lines detected at SNR ≥ 4.0.
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: NIRCam F277W+F356W+F444W detection image cutout (5″ × 5″) around the JWST-dark (F444W > 30 mag) ALMA galaxy candidates. The red solid (dashed) contours represent the 3.0σ, 3.5σ, 4.0σ, and 4.5σ (−3.0σ and −3.5σ) significance levels of the ALMA 1.2 mm continuum in the Wide-natural and Deep-tapered maps for AID60 and AID66, respectively, where the map showing the higher SNR is adopted. The blue cross denotes the potential NIRCam counterpart, with that of AID66 estimated to have zphot ∼ 9 by our SED fits (B. Wang et al. 2025), but that of AID60 is not included in the NIRCam catalog (J. R. Weaver et al. 2024), placing a 2σ upper limit of 29.4 mag in F444W. While the ALMA SNR close to the detection limit indicates these could be just spurious, the probability of chance projection of z > 9 NIRCam candidates is estimated to be ∼0.04% (see the text).
Paper: DUALZ—Deep UNCOVER-ALMA Legacy High-Z Survey
Authors: Seiji Fujimoto, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Sedona H. Price, Bingjie Wang, John R. Weaver, Yoshinobu Fudamoto, Pascal A. Oesch, Christina C. Williams, Pratika Dayal, Robert Feldmann, Jenny E. Greene, Joel Leja, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Lukas J. Furtak, Richard Pan, Iryna Chemerynska, Vasily Kokorev, Tim B. Miller, Hakim Atek, Pieter van Dokkum, Stéphanie Juneau, Susan Kassin, Gourav Khullar, Danilo Marchesini, Michael Maseda, Erica J. Nelson, David J. Setton, Renske Smit
Figure caption: Stacked ALMA 1.2 mm continuum map constructed using the Wide-natural images of 16 galaxies with zspec or zphot ≳ 9 presented in Figure 15. Solid (positive) and dashed (negative) contours start at ±2σ and increase in steps of 1σ, where 1σ = 11.8 μJy beam−1 after primary beam correction. The synthesized beam is shown as the white ellipse at the bottom left. A marginal detection (∼2.3σ) is visible at the central stacked position, implying an intrinsic (lens-corrected) flux density of 14.0 ± 6.2 μJy when adopting a median magnification factor of 1.9 for the stacked sources.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Top: CMD for galaxies in the weak-lensing map. Gray triangles, green squares, blue crosses, and red circles represent galaxies without a spectroscopic redshift, galaxies with a spectroscopic redshift but not members of the Coma cluster, blue members, and red members, respectively. For clarity, only 50% of the gray triangles and green squares are shown. Bottom: differential spectroscopic completeness for galaxies in the weak-lensing map of the Coma cluster. The black dashed, purple dotted–dashed, and orange solid lines represent spectroscopic completeness of redshift data from SDSS and NED, those combined with the redshifts measured with our MMT/Hectospec observations, and all data available, respectively. The vertical dotted lines indicate the magnitude limits at which the spectroscopic completeness drops below 50%.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Relation between M2D and Nbkg, the number of nonmember galaxies in the redshift range 0.01 < z < 0.45 and within rt of each subhalo center. Only nonmember galaxies with mr,Petro,0 < 20.2 are counted. The black solid line represents the best-fit power law to the observed data, while the blue dashed line shows the power-law relation of random sky pointings using the same aperture set. Note that the error on βrand is the 68% interval for 1000 random realizations, not the uncertainties of individual realizations.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Distribution of galaxies in redshift space and along apparent magnitude (mr,Petro,0). Red filled circles, blue crosses, and black open circles represent red members, blue members, and nonmembers, respectively (middle left and bottom left panels). Red and blue hatched histograms show the marginalized histograms of red and blue galaxies along the cluster-centric distance (top left), line-of-sight velocity (middle right), and mr,Petro,0 (bottom right). Black histograms show distribution of all galaxies for the middle left and bottom right panels.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Background galaxy distributions along the line of sight of Subhalo ID 32. The color image represents the κ map from N. Okabe et al. (2014). The blue and green contours show the number density of galaxies at redshift ranges of 0.160 < z < 0.175 and 0.180 < z < 0.200, respectively. The contour levels start from 1σ above the mean number density with a step size of 1σ. The black, blue, and green crosses indicate the center of the Subhalo ID 32, RM J130142.6+290438.5, and GMBCG J195.34791+29.07201, respectively. The black dashed circle show the truncation radius rt of the Subhalo ID 32.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: MMT/Hectospec survey region (cyan box) with the fields of view (black dashed circles). Left: weak-lensing κ map, in units of signal-to-noise ratio adopted from N. Okabe et al. (2014). Right: X-ray surface brightness observed by ROSAT.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Physical parameters of galaxies in the weak-lensing map as a function of redshift. Top: extinction-corrected apparent r-band magnitude. Black, purple, and orange dots are galaxies with measured redshifts from SDSS and NED, this study, and DESI EDR, respectively. We show 50% of the data points for clarity. Bottom: redshift histogram. The purple and orange histograms represent data obtained with our MMT/Hectospec observations and retrieved from DESI EDR, respectively. The black histogram shows the redshift distribution of all galaxies.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: 2D spectroscopic completeness in the field of the Coma cluster weak-lensing map as a function of R.A. and of decl. Marginal spectroscopic completeness as a function of R.A. (top left) and decl. (bottom right) are also shown.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Mass scaling relation of weak-lensing subhalos. Left: relation between weak-lensing mass M2D and number of subhalo members Nsub,mem. Center: relation between M2D and the line-of-sight velocity dispersion of galaxies within the subhalo σp. Right: M2D vs. dynamical mass ﹩{r}_{t}{\sigma }_{p}^{2}{G}^{-1}﹩. The red circles represent the “clean” subhalos flagged for the GMM. We also show Subhalo ID 32 for reference. The red dashed lines show the best-fitting power laws only for the “clean” subhalos.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Bottom left: line-of-sight velocity as a function of cluster-centric radius. Black open circles and red filled circles indicate cluster member galaxies and subhalos, respectively. The size of the circle is proportional to the subhalo mass. Top left and bottom right: histograms of galaxies (black) and subhalos (red).
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Redshift space distribution of galaxies and subhalos within the clusters Halo ID 1 (a) and Halo ID 2 (b) from the TNG300 simulation. This figure is analogous to Figure 10. Bottom left: black open circles and red filled circles represent galaxies and groups with three or more members. Top left and bottom right: histograms of data points corresponding to the same colors in the bottom left panel.
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Comparison of the M–σ relation from the literature and this work. The red circles and red dashed line represent the M2D–σp relation from this work. The dotted line and squares show the M200–σp relation of clusters from K. J. Rines et al. (2016), and the dotted–dashed line and triangles show the relation from D. Rana et al. (2022). The gray solid line and dashed lines show the relation and its 68% confidence interval for elliptical galaxies (H. J. Zahid et al. 2016).
Paper: A Redshift Survey of the Coma Cluster (A1656): Understanding the Nature of Subhalos in the Weak-lensing Map
Authors: Wooseok Kang, Ho Seong Hwang, Nobuhiro Okabe, Changbom Park
Figure caption: Mass scaling relations of subhalos in two galaxy clusters in the TNG300 simulation. The black crosses represent galaxy groups with three or more members and Mgroup > 1012 h−1 M⊙. The black dashed lines show the best-fit power law.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: The difference in Cepheid distances calculated with different methods, plotted against Galactic longitude, where dGaia is from Gaia Collaboration et al. (2023) and dS19 is from S19. The Galactic center is at l = 0°, while the anticenter is at l = ±180°. The mean general offset of about 200 pc is calculated in the range l >120° and l < −120°. The distance difference for −100° < l < 100° has a mean absolute value of about 930 pc and a dispersion of 1400 pc.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Distribution of the differences in the astrometric and photometric distances for bright (W1A < 8.25 mag) Cepheids with good parallaxes using W1 (top panel) and W2 (bottom panel). The red and blue histograms show differences derived from the unWISE magnitudes and the AllWISE magnitudes, respectively. An offset of 0.024 mag has been applied to the unWISE magnitudes, while the differences between the astrometric and photometric distances derived from AllWISE W1A magnitudes are shown both with (solid line) and without (dashed line) a 0.142 offset applied to the AllWISE magnitudes for stars brighter than W1 < 8.25.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: The completeness of the classical Cepheid sample in Galactic coordinates. The OGLE footprint is shown with orange. The ZTF sky coverage extends north of the equator (green line). The Gaia, ASAS-SN, and ATLAS surveys observe the entire sky. The gray background shows the distribution of 5.5 million Gaia DR3 variable stars (excluding AGN and planetary transits) with num_selected_g_fov  > 40 at HEALPix level 5. The cyan points show the location of our entire Milky Way Cepheid catalog (3659 sources), and in red we overplot only those that are exclusively detected outside of Gaia (605 sources), using the flag in_vari_cepheid = False.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Completeness estimate of Gaia Cepheids across Galactic longitude (l) in 10°-wide bins. Panel (a) shows the distribution of l as a function of G magnitude. In cyan are all Cepheids detected with the Gaia survey, while in red are all Cepheids exclusively discovered outside of Gaia. The black dotted line indicates the magnitude limit (84th percentile) of Gaia Cepheids (G < 16.7 mag). Panel (b) shows the contribution of Cepheids from Gaia (NGaia) to the entire catalog (Nall) as a function of l, restricting the sample to within the magnitude limit of Gaia, where this metric provides a measure for the completeness of Cepheids observed by Gaia. The two green dashed lines indicate completeness of 0.95 and 1.0.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: The difference between the WISE W1 (averaged) and Spitzer [3.6] μm magnitudes for the Cepheids in this study, shown as a function of source density per square degree (blue points). The running median and the 16th and 84th percentiles are shown as red solid and dashed lines, respectively.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Standard deviation of the difference in W1 photometry between unWISE and CatWISE shown in black, as a function of W1 from unWISE, for a field far away from the Galactic plane (205° < l < 225° and 10° < b < 20°) and G < 17 mag. The green curve is the nominal uncertainty in CatWISE W1, while in blue we boost this value by adding in quadrature additional uncertainty σW1 from Equation (1), in order to scale up to the observed curve in black.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Difference in W1 magnitudes between AllWISE and unWISE as a function of W1 from AllWISE. The dashed horizontal line shows the mean offset between the two catalogs for W1 > 8.25 mag (0.024 mag), while the red horizontal line is the mean offset for magnitudes brighter than 8.25 mag (0.166 mag).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Corner plot of the distribution of possible model parameters (ϖ0, σ0, σμ) based on the MCMC samples after maximizing the likelihood of the Δμ distribution with respect to the modeled distribution.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Extinction in W1 as a function of G − W1 color, shown for the Cepheids from this study as black (−90° < l < 90°) and blue (90° < l < −90°) points. The orange line shows the prediction for RV = 3.1 assuming the extinction curve from K. D. Gordon et al. (2023), where we adopt a Cepheid intrinsic mean color of (G − W1)0 = 1.5 mag. Cyan and red lines show the predictions for RV = 2.6 and RV = 3.6, respectively.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Distribution of the difference in the W1-based photometric and astrometric distance moduli (Δμ) as seen in the subset of 910 Cepheids with good parallaxes (histogram), and the pdf (renormalized to the binned counts) of such a sample modeled with the parameters estimated via maximum likelihood (orange line). See text for details.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: The distribution of differences in distance (left) and extinction (right) between this study and S19, for Cepheids with W1 > 8.25 mag. In blue we plot the distance/extinction difference when using the 0.470 conversion factor and G. M. Green et al. (2019) maps, and in black we plot that when using the 0.591 conversion factor and G. M. Green et al. (2015) maps. Mean offsets are marked on the plots with corresponding colors.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Difference in the W1-based photometric and parallax-based astrometric distance moduli (Δμ) with respect to the unWISE W1 magnitudes for the subset of Cepheids with σϖ/ϖ < 0.1. Dashed horizontal lines show the Δμ = ±2 mag limits, and the red circles mark 20 Cepheids falling outside these limits.