adsabs/AstroCLIMB huggingface dataset:
Paper: PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release
Authors: Thomas G. Williams, Janice C. Lee, Kirsten L. Larson, Adam K. Leroy, Karin Sandstrom, Eva Schinnerer, David A. Thilker, Francesco Belfiore, Oleg V. Egorov, Erik Rosolowsky, Jessica Sutter, Joseph DePasquale, Alyssa Pagan, Travis A. Berger, Gagandeep S. Anand, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jonathan D. Henshaw, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Eric W. Koch, Jing Li, Daizhong Liu, Sharon E. Meidt, J. Eduardo Méndez-Delgado, Eric J. Murphy, Justus Neumann, Lukas Neumann, Nadine Neumayer, Elias K. Oakes, Debosmita Pathak, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Lise Ramambason, Andrea Romanelli, Mattia C. Sormani, Sophia K. Stuber, Jiayi Sun, Yu-Hsuan Teng, Antonio Usero, Elizabeth J. Watkins, Tony D. Weinbeck
Figure caption: Multitile destriping for one F200W observation of NGC 628. Left: uncorrected data. Middle: noise model. Right: corrected data. This step successfully removes the majority of the remaining large-scale striping in the data, leaving a mostly flat background.
Paper: PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release
Authors: Thomas G. Williams, Janice C. Lee, Kirsten L. Larson, Adam K. Leroy, Karin Sandstrom, Eva Schinnerer, David A. Thilker, Francesco Belfiore, Oleg V. Egorov, Erik Rosolowsky, Jessica Sutter, Joseph DePasquale, Alyssa Pagan, Travis A. Berger, Gagandeep S. Anand, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jonathan D. Henshaw, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Eric W. Koch, Jing Li, Daizhong Liu, Sharon E. Meidt, J. Eduardo Méndez-Delgado, Eric J. Murphy, Justus Neumann, Lukas Neumann, Nadine Neumayer, Elias K. Oakes, Debosmita Pathak, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Lise Ramambason, Andrea Romanelli, Mattia C. Sormani, Sophia K. Stuber, Jiayi Sun, Yu-Hsuan Teng, Antonio Usero, Elizabeth J. Watkins, Tony D. Weinbeck
Figure caption: Schematic overview of our data reduction. While most stages are instrument-agnostic, there are some specific to either NIRCam or MIRI. Steps that are present in the official JWST pipeline are highlighted as blue-outlined hexagons.
Paper: PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release
Authors: Thomas G. Williams, Janice C. Lee, Kirsten L. Larson, Adam K. Leroy, Karin Sandstrom, Eva Schinnerer, David A. Thilker, Francesco Belfiore, Oleg V. Egorov, Erik Rosolowsky, Jessica Sutter, Joseph DePasquale, Alyssa Pagan, Travis A. Berger, Gagandeep S. Anand, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jonathan D. Henshaw, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Eric W. Koch, Jing Li, Daizhong Liu, Sharon E. Meidt, J. Eduardo Méndez-Delgado, Eric J. Murphy, Justus Neumann, Lukas Neumann, Nadine Neumayer, Elias K. Oakes, Debosmita Pathak, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Lise Ramambason, Andrea Romanelli, Mattia C. Sormani, Sophia K. Stuber, Jiayi Sun, Yu-Hsuan Teng, Antonio Usero, Elizabeth J. Watkins, Tony D. Weinbeck
Figure caption: Diagnostic diagrams showing the NIRCam-to-HST astrometric alignment quality for example galaxy NGC 1566. Each of the panels displays the resulting R.A./decl. “scatterball” for a different NIRCam band using our final NIRCam-measured sky coordinate minus HST R.A./decl. The points are plotted with transparency in order to allow assessment of peak location and distribution shape for each scatterball. The FWHM extent of the NIRCam PSF in each band is drawn as a red dotted circle with a black dashed cross, and the pixel size on either the short (F200W) or long (F300M, F335M, F360M) NIRCam detectors is marked as a thick gray square. With text in each panel, we provide the sigma-clipped mean residual R.A./decl. offset from HST in arcseconds. This galaxy is typical in quality of NIRCam alignment, though it does not show evidence for tile-to-tile intramosaic alignment residuals as some galaxies do.
Paper: PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release
Authors: Thomas G. Williams, Janice C. Lee, Kirsten L. Larson, Adam K. Leroy, Karin Sandstrom, Eva Schinnerer, David A. Thilker, Francesco Belfiore, Oleg V. Egorov, Erik Rosolowsky, Jessica Sutter, Joseph DePasquale, Alyssa Pagan, Travis A. Berger, Gagandeep S. Anand, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jonathan D. Henshaw, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Eric W. Koch, Jing Li, Daizhong Liu, Sharon E. Meidt, J. Eduardo Méndez-Delgado, Eric J. Murphy, Justus Neumann, Lukas Neumann, Nadine Neumayer, Elias K. Oakes, Debosmita Pathak, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Lise Ramambason, Andrea Romanelli, Mattia C. Sormani, Sophia K. Stuber, Jiayi Sun, Yu-Hsuan Teng, Antonio Usero, Elizabeth J. Watkins, Tony D. Weinbeck
Figure caption: Diagnostic diagrams showing the MIRI-to-NIRCam relative astrometric alignment quality for example galaxy NGC 1566. Each of the panels displays the resulting R.A./decl. “scatterball” for a different MIRI band using our final MIRI-measured sky coordinate minus NIRCam F300M R.A./decl. The plotted points are plotted with transparency in order to allow assessment of peak location and distribution shape for each scatterball. The FWHM extent of the MIRI PSF in each band is drawn with a red dotted circle with a black dashed cross, and the pixel size on the MIRI detector is marked as a thick gray square. With text in each panel, we provide the sigma-clipped mean residual R.A./decl. offset from NIRCam F300M in arcseconds. This galaxy is in the top third of galaxies in ranked quality of MIRI-to-NIRCam alignment.
Paper: PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release
Authors: Thomas G. Williams, Janice C. Lee, Kirsten L. Larson, Adam K. Leroy, Karin Sandstrom, Eva Schinnerer, David A. Thilker, Francesco Belfiore, Oleg V. Egorov, Erik Rosolowsky, Jessica Sutter, Joseph DePasquale, Alyssa Pagan, Travis A. Berger, Gagandeep S. Anand, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jonathan D. Henshaw, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Eric W. Koch, Jing Li, Daizhong Liu, Sharon E. Meidt, J. Eduardo Méndez-Delgado, Eric J. Murphy, Justus Neumann, Lukas Neumann, Nadine Neumayer, Elias K. Oakes, Debosmita Pathak, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Lise Ramambason, Andrea Romanelli, Mattia C. Sormani, Sophia K. Stuber, Jiayi Sun, Yu-Hsuan Teng, Antonio Usero, Elizabeth J. Watkins, Tony D. Weinbeck
Figure caption: Variations in the standard deviation of an empty sky region after convolving the F2100W maps with a 2D Gaussian with the FWHM value displayed on the lower x-axis. The approximate final resolution is listed on the upper x-axis. Green lines show the measured standard deviations. Vertical red lines represent the Gaussian kernel that will approximately produce our chosen 0.″90 final resolution, a kernel FWHM of 0.″60. Horizontal blue dash-dot lines represent the background 1σ of the regions at the native resolution, before any convolution. The gray dashed line represents the theoretical prediction for uncorrelated noise, normalized to the measured curve at our chosen final resolution. Each panel represents a different map that includes an empty sky region in all of the MIRI bands.
Paper: PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release
Authors: Thomas G. Williams, Janice C. Lee, Kirsten L. Larson, Adam K. Leroy, Karin Sandstrom, Eva Schinnerer, David A. Thilker, Francesco Belfiore, Oleg V. Egorov, Erik Rosolowsky, Jessica Sutter, Joseph DePasquale, Alyssa Pagan, Travis A. Berger, Gagandeep S. Anand, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jonathan D. Henshaw, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Eric W. Koch, Jing Li, Daizhong Liu, Sharon E. Meidt, J. Eduardo Méndez-Delgado, Eric J. Murphy, Justus Neumann, Lukas Neumann, Nadine Neumayer, Elias K. Oakes, Debosmita Pathak, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Lise Ramambason, Andrea Romanelli, Mattia C. Sormani, Sophia K. Stuber, Jiayi Sun, Yu-Hsuan Teng, Antonio Usero, Elizabeth J. Watkins, Tony D. Weinbeck
Figure caption: External anchoring for NGC 628 at F300M to IRAC1 (both convolved to 4″ resolution). The gray dots indicate individual pixels, and the red dots are binned medians for the region over which we fit to anchor. The best-fit line is shown in dashed gray, with the fit parameters given in the top left.
Paper: PHANGS-JWST: Data-processing Pipeline and First Full Public Data Release
Authors: Thomas G. Williams, Janice C. Lee, Kirsten L. Larson, Adam K. Leroy, Karin Sandstrom, Eva Schinnerer, David A. Thilker, Francesco Belfiore, Oleg V. Egorov, Erik Rosolowsky, Jessica Sutter, Joseph DePasquale, Alyssa Pagan, Travis A. Berger, Gagandeep S. Anand, Ashley T. Barnes, Frank Bigiel, Médéric Boquien, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Eric Emsellem, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Jonathan D. Henshaw, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Eric W. Koch, Jing Li, Daizhong Liu, Sharon E. Meidt, J. Eduardo Méndez-Delgado, Eric J. Murphy, Justus Neumann, Lukas Neumann, Nadine Neumayer, Elias K. Oakes, Debosmita Pathak, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Lise Ramambason, Andrea Romanelli, Mattia C. Sormani, Sophia K. Stuber, Jiayi Sun, Yu-Hsuan Teng, Antonio Usero, Elizabeth J. Watkins, Tony D. Weinbeck
Figure caption: Comparison of the scatter measured within background regions of MIRI data to the mean of the pipeline-generated error map value within the same region (one region per galaxy).
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: The HMI cutout image of an AR (NOAA AR 2989) recorded at 23:59 on 2022 April 13 (left panel) and the magnetogram taken 3 minutes later (right panel). The selected window size is 75 × 75 pixels. The complex network is constructed considering a threshold of 18 G. Patch borders and labels are indicated in red and blue, respectively. According to the introduced tracking and labeling system, patches such as O-6, O-3, and O-7 are one-to-one matches, while patches like 10 and 11 merge and are relabeled as M-11. Patches E-26 and E-35 appear and patches 5 and 26 disappear in the right panel. Patch 8 fragments and is assigned with a new label as F1-37. To avoid a cluttered presentation, labels of the small patches are not indicated.
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: (a) The HMI cutout image of an AR recorded by the SDO at 23:58 on 2022 January 17 (NOAA AR 2929). The selected window size is 75 × 75 pixels. The complex network is constructed considering a threshold of about 20 G. (b) The node-degree image. (c) The identified regions of the node-degree image correspond to magnetic patches. (d) The PageRank image. In the PageRank image, bright pixels indicate high PageRank values. The PageRank image is the same size as the original cutout HMI magnetogram.
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: (a) An artificial magnetogram of 100 × 100 pixels, featuring randomly generated background levels with the absolute values of the background less than 17 G. (b) The original node-degree image. Panels (c) and (d) represent the node-degree image after masking the largest patch (i.e., patch No. 55) and the patch with the highest degree (i.e., patch No. 4), respectively.
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: Frequency–size distribution of magnetic patches identified by the conventional downhill technique (blue line) and features of a node-degree image (red line) for an AR (a) and a quiet Sun (b).
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: The identified magnetic patches ranked by numbers according to (a) the total degree of the nodes, (b) the average degree of the nodes for pixels (divided by patch size), (c) the total magnetic field, and (d) the average magnetic field for pixels (divided by patch size).
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: Feature sizes for various choices of threshold applying the downhill algorithm: (a) in a node-degree image corresponding to an AR; (b) in a node-degree image related to a quiet Sun.
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: Consecutive HMI magnetograms with the cadence of 45 s (top panels) together with the identified features from the node-degree images constructed with the network approach (bottom panels). The patches with green arrows correspond to the small-scale events of the corner panels that were not detected in the middle frame.
Paper: Complex Network View of the Sun’s Magnetic Patches. I. Identification
Authors: Zahra Tajik, Nastaran Farhang, Hossein Safari, Michael S. Wheatland
Figure caption: (a) The HMI cutout image of a quiet region recorded by the SDO at 23:59 on 2022 July 12. The selected window size is 113 × 101 pixels. The complex network is constructed considering a threshold of about 18 G. (b) The node-degree image. (c) The identified node-degree regions corresponding to magnetic patches. (d) The PageRank image.
Paper: The Plane Quasar Survey: First Data Release
Authors: Jessica Werk, Kirill Tchernyshyov, Hannah Bish, Yong Zheng, Mary Putman, Joshua Peek, David Schiminovich
Figure caption: UV-bright QSO all-sky distribution: An all-sky Aitoff projection in Galactic coordinates, centered at b = 0°, l = 180°, showing the distribution of different UV-bright QSO samples, including the plane QSO candidates (dark- and light-purple shapes). For orientation within this frame of reference, the underlying gray map shows high-velocity (∣v LSR∣ > 80 km s−1) H I detected in 21 cm emission from the HI4PI Survey (HI4PI Collaboration et al. 2016; Westmeier 2018), generally with N H I  > 1018 cm−2. The black circles show the 401 archival QSO sight lines with high-resolution HST/COS spectra from the COS Quasar Database for Galactic Absorption Lines (Zheng et al. 2019) , and the gray pluses show all the confirmed AGN from the UVQS (Monroe et al. 2016), including those that were previously identified by the Milliquas Survey (Flesch 2023). Purple diamonds highlight the spectroscopically confirmed low-latitude QSOs, which fill a gap in the existing data sets. The 12 stars show objects in our candidate list that were confirmed stellar sources, and the light-purple crosses are targets from our candidate list that have not yet been observed.
Paper: The Plane Quasar Survey: First Data Release
Authors: Jessica Werk, Kirill Tchernyshyov, Hannah Bish, Yong Zheng, Mary Putman, Joshua Peek, David Schiminovich
Figure caption: UV-bright QSO photometric selection: A WISE-GALEX color–magnitude diagram showing the distribution of different UV-bright QSO samples in GALEX NUV magnitude vs. W1–W2 color, including the our plane QSO candidates from both selection methods (dark- and light-purple shapes). The gray plus signs show the confirmed AGN from the UVQS Survey (Monroe et al. 2016), including those that were previously identified by the Milliquas Survey (Flesch 2023). Purple diamonds highlight the spectroscopically confirmed low-latitude QSOs, which fill a gap in the existing data sets. The 12 maroon stars show objects in our candidate list that are spectroscopically confirmed as stellar sources, and the light-purple crosses are targets from our candidate list that have not yet been observed.
Paper: The Plane Quasar Survey: First Data Release
Authors: Jessica Werk, Kirill Tchernyshyov, Hannah Bish, Yong Zheng, Mary Putman, Joshua Peek, David Schiminovich
Figure caption: Top: We compare our redshifts derived from narrow-line fits (generally to [O III] λ λ 4960, 5008) with those available in the literature, from different sources, determined with a variety of methods based on data of highly variable quality. Bottom: We compare our MARZ-template-fitted QSO redshifts with those same literature QSO redshift estimates. On both panels, we have labeled the mean velocity offsets between the PQS redshifts and archival estimates with ±1σ spreads. We have eliminated from this analysis the eight cases discussed in the text with >1000 km s−1 differences.
Paper: The Plane Quasar Survey: First Data Release
Authors: Jessica Werk, Kirill Tchernyshyov, Hannah Bish, Yong Zheng, Mary Putman, Joshua Peek, David Schiminovich
Figure caption: Example PQS spectra: We show six flux- and wavelength-calibrated 1D spectra from the three different telescopes used during our PQS observing runs. On the upper right of each panel, we provide the MARZ redshift determined using the template QSO spectrum fits. Some of the strong emission lines identified in each spectrum are labeled, and the telescope and PQS target name are given in the lower-right-hand corner of the spectra. All of the spectra are available to download on MAST.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: Likelihood contours in the (π E,N, π E,E) plane. The red, orange, yellow, lime, green, cyan, blue, and dark blue colors mark Δχ 2 = 1, 4, 9, 16, 25, 36, 49, 64, respectively. The arrows mark the directions of positive π E,∥ and π E,⊥, that is, directions parallel and perpendicular to the projected acceleration of the Sun in the adopted geocentric frames.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: Detection efficiency to microlensing events as a function of the Einstein timescale for field LMC501 (averaged for sources brighter than I = 22 mag). The purple line marks the detection efficiency for stars observed during OGLE-III and OGLE-IV phases of the project, and the orange line—for stars observed during OGLE-IV only.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: Surface density of source stars brighter than I = 22 in the analyzed OGLE-IV fields. The black polygon marks the region observed during the OGLE-III phase.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: Ratio between the mean surface density of stars brighter than I = 21 detected in the HST and OGLE images (correction factor) as a function of density of stars observed by OGLE.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: (a) Activity–rotation relation of single stars. The gray, green, blue, cyan, and coral dots are from Wright et al. (2011, 2018), Pizzocaro et al. (2019), Wang et al. (2020), and this study, respectively. Ro that were empirically estimated are shifted by a factor of Ro/3. The magenta lines are our best-fit results. (b) Comparisons of activity–rotation relations from different studies. The shaded region shows 100 models extracted randomly from the posterior probability distribution.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Activity–rotation relations of F-, G-, K-, and M-type single stars, respectively. Stars with T eff lower than 4000 K are classified as M-type stars. K-type stars are those with T eff between 4000 K and 5300 K. G-type stars have T eff ranging from 5300 K to 6000 K. The T eff range of F-type stars is set to be from 6000 K to 7500 K. The magenta dashed lines are the best-fit activity–rotation relations shown in Figure 3.
Paper: Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Authors: Henggeng Han, Song Wang, Chuanjie Zheng, Xue Li, Kai Xiao, Jifeng Liu
Figure caption: Left panel: Histograms of L  X  of dwarfs, giants, YSOs and binaries. The shaded area represents the region in which X-ray luminosity is higher than 1031 erg s−1. Right panel: histograms of R  X  of dwarfs, giants, binaries, and ultraluminous sources.
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: All-sky distribution of 1O/F double-mode δ Sct stars in Galactic coordinates. The top panel shows the sample with P 1 > P 2, while the bottom panel shows the sample with P 1 < P 2. The colors indicate the logarithm of the longer period P  L .
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: Statistical properties of the 1O/F double-mode δ Sct stars. (a) Histograms of the F-mode period and 1O-mode period. (b) Histograms of the amplitude corresponding to the F and 1O modes; the two solid lines are the Gaussian fits. (c) Histograms of the period ratio. (d) Distribution of amplitude vs. period.