adsabs/AstroCLIMB huggingface dataset:
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The CO(1–0) multiline emission of Finger 4 (left) and Finger 1 (right). In the two panels, the 12CO emission contours (blue; integrated between −1 and +7 km s−1) start at 5σ and increase in steps of 3σ (1σ ∼ 0.8 K km s−1). The 13CO emission contours (green; integrated between 0.5 and 6.5 km s−1) start at 4σ and increase in steps of 2σ (1σ ∼ 0.37 K km s−1). The C18O emission is integrated between 4.5 and 6.5 km s−1, and the contours (red) start at 3σ and increase in steps of 1σ (1σ ∼ 0.21 K km s−1).
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The velocity-integrated intensity channel maps of the 12CO(1–0) emission toward the west of the Cassiopeia Filament. The integrated velocity range is written in the bottom right corner of each panel (in km s−1). The blue dashed-line rectangle in the panels shows the extent of the arc-like shell found in the velocity range from roughly −1 to +7 km s−1.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: Top panel: the 12CO(1–0) velocity-integrated intensity image of the shell region. The unit of the scale bar is K km s−1. The 12CO emission is integrated between −1 and +7 km s−1 (1σ ∼ 0.8 K km s−1). Bottom panel: the enlarged view of the shell and finger-like structures.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The velocity-integrated intensity channel maps of the 12CO(1–0) emission toward the Galactic Cassiopeia region. The integrated velocity range is written in the bottom right corner of each panel (in km s−1). The unit of the scale bar is K km s−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward W Hya (white cross), imaged with GALEX. (a) The FUV emission in the near vicinity of W Hya (white cross); white dashed vector shows the star’s proper motion of 45.4 mas yr−1 at PA = 194°, magnified by a factor of 104. (b) The FUV emission around W Hya over a large field of view, with major structural features marked. Dashed white circles show partial ringlike structures of radii 65″, 160″, and 220″. Several radial (compact as well as extended) features, likely corresponding to outflows, are labeled as A, B, ... G. Outflows A, B, and C show diametrically opposed pairs (denoted with subscripts 1 and 2, e.g., A1 and A2). Outflow G is inferred from the presence of diffuse emission regions (encircled with green ellipses) located roughly north of the star. Four large azimuthal structures are labeled T 1–T 4. Bright compact bright sources (labeled “g”) are likely background galaxies. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward R Hya, imaged with GALEX. The white dashed circle, with radius of 120″, delineates the radial extent of the termination shock in the astrosphere, west of R Hya (black cross); white solid circle delineates a termination-shock radius of 93″ estimated from far-IR imaging by Cox et al. (2012). Black vector shows the star’s proper motion of 36.7 mas yr−1 at PA = 310°, magnified by a factor of 104; white vector shows symmetry axis of the fan-shaped astrosphere. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward RX Boo, imaged with GALEX. The white dashed circle (radius 325″), delineates the radial extent of the termination shock in the astrosphere, south-southeast of RX Boo (black cross). The white dashed vectors labeled SymAx 1 and SymAx2 represent two possible symmetry axes of the astrosphere. Black vector shows the star’s proper motion of 58.8 mas yr−1 at PA = 132°, magnified by a factor 104. “A” shows where a bright point source could not be removed; “B” shows a related ghost artifact. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward RW Boo, imaged with GALEX. The dashed white circle (radius 260″), delineates the radial extent of the termination shock in the astrosphere, seen to the west of RW Boo. Black vector shows the star’s proper motion of 12.4 mas yr−1 at PA = 356°, magnified by a factor 104; white vector shows symmetry axis of the astrosphere. Region A (black ellipse) shows local environment around a bright point source that could not be adequately removed. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cuts of the FUV emission around RX Boo, averaged over azimuthal wedges with their apexes centered on the star, and spanning the range from PA = 150° to 190° (green curve), PA = 120° to 160° (red curve), and an average of the two (black curve). The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around W Hya; intensity has been averaged over an azimuthal wedge with its apex centered on the star and covering the angular range PA = 95° to 235°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around RT Vir, averaged over an azimuthal wedge with its apex centered on the star and spanning the range from PA = 65° to 145°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around R Hya, averaged over an azimuthal wedge with its apex centered on the star and spanning the range from PA = −123° to −43°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around RW Boo; intensity has been averaged over an azimuthal wedge with its apex centered on the star, covering the angular range PA = −75° to 5°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: A model FUV-band spectrum due to electron impact excitation of H2, scaled to fit the FUV emission flux observed in an elliptical patch of size 210″ × 110″ covering the brightest part of the leading edge of the astrosphere of IRC+10216. Top panel shows the full spectrum of Lyman–Werner band lines, whereas the bottom panel shows an expanded view of the spectrum indicating the centers of two wavelength windows that would be optimum for observations with AMUSS.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward VX Eri, imaged with GALEX. The dashed white circle (radius 290″), delineates the radial extent of the termination shock in the astrosphere, southeast of VX Eri. Black vector shows the star’s proper motion of 14.4 mas yr−1 at PA = 213°, magnified by a factor of 104. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around VX Eri; intensity has been averaged over an azimuthal wedge with its apex centered on the star and covering the angular range PA = 100° to 180°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward CIT 6, imaged with GALEX (adapted from Sahai & Mack-Crane 2014). Red vector shows the star’s proper motion of 16.6 mas yr−1 at PA = 300°, magnified by a factor of 104; red cross shows the star’s location. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: Eccentricities for all transiting exoplanets with >3σ mass measurements. We show Jupiter-sized exoplanets (R > 8R ⊕) in blue and smaller planets in gray. TOI-4127 b (red) has an eccentricity higher than all but five exoplanets in this class. We also show the constant angular momentum tidal circularization track for this planet. TOI-4127 b is not expected to tidally circularize during the main-sequence lifetime of its host star, although we note that the circularization timescale is highly sensitive to our choice of Q  p , which is not well constrained. Known planet parameters were taken from the NASA Exoplanet Archive on 2023 January 12.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: TESS PDCSAP photometry for TOI-4127. From top to bottom, we show long-cadence (30 minutes) TESS-SPOC data for Sectors 20 and 26, and short-cadence (2 minutes) SPOC data for Sectors 40, 47, and 53. We report the transit time in the lower right-hand corner of each panel for the sectors in which high-quality transits were detected (Sectors 20, 26, and 53), and we show the SAP data for the low-quality Sector 47 transit in gray.
Paper: A High-Eccentricity Warm Jupiter Orbiting TOI-4127
Authors: Arvind F. Gupta, Jonathan M. Jackson, Guillaume Hébrard, Andrea S. J. Lin, Keivan G. Stassun, Jiayin Dong, Steven Villanueva, Diana Dragomir, Suvrath Mahadevan, Jason T. Wright, Jose M. Almenara, Cullen H. Blake, Isabelle Boisse, Pía Cortés-Zuleta, Paul A. Dalba, Rodrigo F. Díaz, Eric B. Ford, Thierry Forveille, Robert Gagliano, Samuel Halverson, Neda Heidari, Shubham Kanodia, Flavien Kiefer, David w. Latham, Michael W. McElwain, Ismael Mireles, Claire Moutou, Joshua Pepper, George R. Ricker, Paul Robertson, Arpita Roy, Martin Schlecker, Christian Schwab, S. Seager, Avi Shporer, Guđmundur Stefánsson, Ryan C. Terrien, Eric B. Ting, Joshua N. Winn, Allison Youngblood
Figure caption: Spectral energy distribution of TOI-4127. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black).
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: 4U 0142+61 data fitted with XSPEC before (left) and after (right) the background rejection; the considered spectral model is TBABS*(BBODY+POWERLAW). At the bottom, residuals with respect to the best-fit model are shown. On the right panel, the backgrounds before and after rejection are compared, and it is possible to appreciate its reduction after the rejection procedure.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Polarization degree (top) and angle (bottom) obtained for 4U 0142+61 data fitted with XSPEC in different energy bins before (light blue) and after (orange) the background rejection. It is possible to observe that in the last energy bin, where the background dominates, the rejection strategy produces a more significant polarization degree because the dilution effect is partially washed out, while the polarization angle is well compatible in the two cases.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Energy spectrum from Cal D in the three detectors of IXPE, from left to right: DU1, DU2 and DU3. In each plot, the spectrum without rejection (blue line) with label all is compared with the one of events tagged as source (src) after rejection (orange line) and the rejected events tagged background (bkg, green line).
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Percentage residuals of the energy spectrum from Cal C (left) and Cal D (right) in one of the three detectors (DU1), as a case study, but results in the other DUs are comparable. It is possible to observe that the residuals deviate at maximum at 0.05% from zero.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Cas A data images from the original data (left), after the background rejection (center), and for the rejected events (right). The same color scale was applied.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Contours enclosing regions at the confidence level of 68.3% (solid lines) and 99.7% (dotted lines) in case of original unrejected data (light blue), after the rejection of Section 4.2.4 (orange) and for the events rejected because identified as background (green).
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Energy spectrum from Cal C in the three detectors of IXPE, from left to right: DU1, DU2, DU3. In each plot, the spectrum without rejection (blue line) with label all is compared with the one of events tagged as source (src) after rejection (orange line) and the rejected events tagged background (bkg, green line).
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: Logarithmic luminosity functions of CVs. The lower panel shows the luminosity functions for all CVs and the mCVs. Upper panel demonstrates the logarithmic luminosity function for all CVs in the sample. The red line represent 500 times the luminosity function of all CVs and the blue line logarithmic luminosity function of white dwarfs taken from Gaia Collaboration et al. (2021b).
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: The z-histograms for all CVs in the sample in terms of the orbital period. The orbital period (P orb(h)) intervals are shown in brackets. The best fits to the z-histograms are also presented. The blue dashed line represents the ﹩{{\rm{sech}} }^{2}﹩ function and the red solid line the exponential function.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: The logarithmic density functions of all CVs (panel a) and mCVs (panel b) in the sample. The dashed lines represent the exponential fits applied to the data.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: The number of stars for z = 0 pc (n 0) vs. scale height (H), estimated with 15,000 trials in MC simulations. The simulations were performed for all CVs in the sample, keeping magnetic systems in the sample as they are and assuming 22% of the remaining sample to be magnetic by arbitrary selection. The left and right panels are plotted for exponential and ﹩{{\rm{sech}} }^{2}﹩ scale heights, respectively. The red straight lines show the most probable values. 1σ values are indicated with blue straight lines.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: The absolute magnitudes M G of the CVs in the preliminary sample against their distances d BJ obtained from Bailer-Jones et al. (2021). The red dashed lines show the distances estimated from the bright (G = 9 mag) and faint (G = 18.5 mag) limiting apparent magnitudes for absolute magnitude intervals of 1 mag. The blue solid lines correspond to the bright and faint apparent magnitude limits.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: The spatial distribution of CVs in the final sample with respect to the Sun. X, Y, and Z are Sun-centered rectangular Galactic coordinates. Magnetic systems (mCVs) are shown with blue symbols. Number histograms created according to coordinates are shown to the right and top of the figure.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: The distribution of CVs according to equatorial (α, δ) and Galactic (l, b) coordinates. The distributions of the magnetic and nonmagnetic systems are shown with different colors, blue and black, respectively. The red dashed lines represent the Galactic plane (upper panel) and the celestial equator (lower panel). The green star in the upper panel indicates the location of the Galactic center in the plot.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: Gaia DR3 H-R diagram of CVs for which the orbital periods P orb are known in the final sample. The separating point of the orbital period gap is accepted as 2.6 hr (Ak et al. 2010). White dwarf and the main-sequence and giant star regions are shaded in blue and gray, respectively (Abril et al. 2020).
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: The z-histograms for CVs. The upper panel shows the z-histogram for all CVs in the sample and the lower panel magnetic systems (mCVs). The blue dashed line represents the ﹩{{\rm{sech}} }^{2}﹩ function and the red solid line the exponential function. The 2D posterior probability distributions of the model parameters sampled by MCMC are demonstrated to the right of the z-histograms.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: Location of nine CVs with different apparent G-band magnitudes selected from the Gaia DR3 catalog are shown with Pan-STARRS g-band images using Aladin. Target objects are located at the centers of the images.