adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Contours of Δχ 2 = 1, 4, 9 (black, red, yellow) relative to the minimum of the C-ML-1 source’s g − r color and g-band brightness from MCMC realizations are shown with the HST color–magnitude diagram (density map) from the PHAT survey. The HST magnitudes are transformed into the CFHT bands. The color and magnitude of C-ML-1's source is consistent with being a star in M31.
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Distribution of different types of variable sources in the color–magnitude diagram.
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Examples of light curves for pulsating variable stars (left panels) and eclipsing binary stars (right panels). To the left side of the light curves, some related information is labeled, including period, CFHT g-band magnitude, light variation amplitude, g − r color, or binary type.
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Upper: Light curves of microlensing candidate C-ML-1 observed in g (green) and r (red) shown with the best-fit point-source-point-lens microlensing model (black). The magnitudes are normalized to the g band. Lower: the residuals for the microlensing model.
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Normalized light curves of the 19 flares. The legend on the left shows the color, flare amplitude, and magnitude of the stars. The green and red dots represent CFHT g and r magnitudes, respectively. Note the CFHT r magnitudes have been shifted to a position close to the CFHT g magnitudes by adding the average g − r color.
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Sinusoidal-like light curves of the 42 variables. The curved are sorted by their periods. The period, CFHT g-band magnitude, light variation amplitude, and g − r color are labeled.
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Trajectories of the 24 asteroids. The thick red, green, and blue lines represent the paths of the asteroids on three different days. The thin red dotted lines indicate new asteroid candidates we discovered, and the thin black dotted lines indicate known asteroids.
Paper: Searching for Short-period Variables in M31: Method and Catalogs
Authors: Hongrui Gu, 弘睿 顾, Haibo Yuan, 海波 苑, Subo Dong, 苏勃 东, Chenfa Zheng, 晨发 郑, Shenzhe Cui, 深哲 崔, Yi Ren, 逸 任, Haozhu Fu, 皓竹 付, Yang Huang, 样 黄, Zhou Fan, 舟 范
Figure caption: Top panels: error distributions of the original WCS. Bottom panels: error distributions after the correction.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Mollweide projection of the positions for 5.86 million stars selected from the Southern Hemisphere (SMSS) and Northern Hemisphere (SAGES) photometric surveys, in equatorial (left panel) and Galactic (right panel) coordinates. The metallicity of this final sample is based on calibrated v − G BP colors and a combination of the u/v bands from SMSS/SAGES (Huang et al. 2022, 2023). See the Appendix for a discussion of the cuts that are applied to the sample prior to assigning the final metallicities. The gray filled circles indicate the stars with derived metallicities in the range −2 < [Fe/H] ≤ +0.5, the light-blue filled circles are stars with −3 < [Fe/H] ≤ −2, and the black filled circles represent stars with −4 < [Fe/H] ≤ −3. The stars shown all have available RVs and astrometric information. For the purpose of our analysis, we exclude stars identified as likely binaries by Huang et al. (2022, 2023), cool dwarfs (T eff < 4500 K), metal-rich stars masquerading as VMP/EMP stars (see text), and likely members of recognized globular clusters. For stars in common between the two surveys, we have used the average value of the photometric-metallicity estimates.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Top panel: rotational velocity distribution (v  ϕ ) of the SMSS/SAGES sample as a function of photometric metallicity ([Fe/H]). The number density is color-coded on a logarithmic scale. The MWTD, the SD, and the GSE substructure are marked with black dashed ellipses. The highly prograde VMP/EMP candidates are shown by white circles. Middle panel: same as the top panel, but for dwarfs. Bottom panel: same as the top panel, but for giants. The number of VMP/EMP stars with v  ϕ  > 150 km s−1 is about 2150, including 650 dwarfs and 1500 giants.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Left panel: cumulative number distribution of the MP ([Fe/H] ≤ −1) stars as a function of [Fe/H], for stars with ﹩{Z}_{\max }﹩ >3 kpc (black line), ﹩{Z}_{\max }﹩ ≤3 kpc (red line), and ﹩{Z}_{\max }﹩ ≤1 kpc (blue line). Middle panel: cumulative distribution functions of [Fe/H] for these subsamples. Each population is normalized on the basis of the number of stars at [Fe/H] = −1. Right panel: eccentricity distribution for these subsamples with [Fe/H] ≤ −1.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Histogram of the errors in photometric-metallicity estimates (δ [Fe/H]) for the final SMSS/SAGES sample. From left to right, the panels correspond to MP ([Fe/H] ≤ −1), VMP ([Fe/H] ≤ −2), and EMP ([Fe/H] ≤ −3) subsamples, respectively. The black, blue, and red histograms represent the total, dwarf, and giant stars in each metallicity range, respectively. The number of stars and the median values of δ [Fe/H] are indicated in the legend of each panel.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Left column: comparison of the combined SMSS/SAGES photometric-metallicity estimates and spectroscopic metallicities for VMP/EMP stars, based on cross-matches to medium/high-resolution spectroscopic samples with available [Fe/H] and [C/Fe]. The stars from Yoon et al. (2016), Li et al. (2022a), Placco et al. (2022), Zepeda et al. (2023), and Viswanathan et al. (2024) are shown as red triangles, blue squares, green diamonds, purple pentagons, and gray stars, respectively. The black circles indicate carbon-enhanced metal-poor (CEMP) stars that satisfy [C/Fe]  > +0.7. Note that for our present purpose we employ the “as-observed” [C/Fe], without applying evolutionary corrections (e.g., from Placco et al. 2014). The black solid line is a linear regression line for all metallicity regions except for the range [Fe/H]﹩{}_{\mathrm{Literature}}\leqslant -3﹩, a light-blue shaded region, and the dashed line represents a one-to-one line. The legends in each panel indicate the number of matching stars (N), the p-value, and the r 2 value in the Pearson correlation analysis, as well as the biweight location (μ) and scale (σ) of the metallicity residuals. Right column: comparison with the same spectroscopic catalogs, but excluding (recognized) CEMP stars. From top to bottom, the panels indicate matches for stars with metallicities based on the calibrated u − G BP colors, the v − G BP colors, and, when available, an average of both of these colors (Huang et al. 2022, 2023).
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Top panels: number distributions of VMP/EMP stars on both retrograde and prograde orbits as a function of eccentricity, from the left to right panels, for [Fe/H] ≤ −2, −2.5, and −3, respectively. The black, red, and blue solid lines indicate the stars with ﹩{Z}_{\max }﹩ > 3 kpc, 1 kpc < ﹩{Z}_{\max }﹩ ≤3 kpc, and ﹩{Z}_{\max }﹩ ≤ 1 kpc, respectively. The number of stars in each region is indicated in the legend in the upper right corner of the panels. The dashed and dotted–dashed lines are shown at ecc = 0.2 and 0.4, respectively. Bottom panels: same as the top panels, but for the highly prograde stars with v  ϕ  > 150 km s−1.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Number distribution of VMP/EMP stars as a function of IA, for [Fe/H] ≤ −2, −2.5, and −3, from left to right, respectively. The total, prograde, and retrograde orbiting stars are shown with black, purple, and orange lines, respectively. The prograde stars with v  ϕ  > 150 km s−1 are shaded in blue. The number of stars in each region is indicated in the legend on the top of the panels. The dashed and dotted–dashed lines indicate IA = 0.25 and 0.65 rad, respectively.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Top panels: number distributions of VMP/EMP stars as a function of eccentricity, from left to right, for [Fe/H] ≤2, 2.5, and 3, respectively. The black, red, and blue solid lines indicate the stars with IA > 0.65 rad, 0.25 rad < IA ≤ 0.65 rad, and IA ≤ 0.25 rad, respectively. The dashed and dotted–dashed lines are shown at ecc = 0.2 and 0.4, respectively. The number of stars in each region is indicated in the legend in the upper right corner of the panels. Bottom panels: same as in the top panels, but for the highly prograde stars with v  ϕ  > 150 km s−1.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Number distributions of VMP/EMP stars with prograde orbits as a function of rotational velocity (v  ϕ ), for the stars with [Fe/H] ≤ −2 (left panel), −2.5 (middle panel), and −3 (right panel), respectively. The vertical dashed line is at v  ϕ  = 150  km s−1, which is used to select disklike stars on highly prograde orbits. Note that the bins on v  ϕ  used for the stars with [Fe/H] ≤ −3 are twice the size for the more metal-rich stars, due to their lower numbers.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Fraction of prograde stars as a function of [Fe/H]. The black line shows the combined SMSS/SAGES sample. The blue line shows the simulation results of Hirai et al. (2022). The Galactocentric distance of the data considered is confined to between 3 and 20 kpc, roughly corresponding to the combined SMSS/SAGES sample. The error bars shown are calculated using the normal approximation for the binomial proportions; they are quite small owing to the large number of stars in our data set.
Paper: Candidate Members of the VMP/EMP Disk System of the Galaxy from the SkyMapper and SAGES Surveys
Authors: Jihye Hong, Timothy C. Beers, Young Sun Lee, Yang Huang, Yutaka Hirai, Jonathan Cabrera Garcia, Derek Shank, Shuai Xu, Haibo Yuan, Mohammad K. Mardini, Thomas Catapano, Gang Zhao, Zhou Fan, Jie Zheng, Wei Wang, Kefeng Tan, Jingkun Zhao, Chun Li
Figure caption: Top panels: the ﹩{Z}_{\max }﹩ distribution as a function of ﹩{R}_{\max }﹩ for the full sample of prograde stars. Dashed and dotted–dashed lines represent IA = 0.25 and 0.65 rad, respectively. The number of stars is shown in the legend at the top right of each panel. Bottom panels: same as the top panels, but for the stars with v  ϕ  > 150 km s−1.
Paper: Lagrangian Perspectives on the Small-scale Structure of Alfvénic Turbulence and Stochastic Models for the Dispersion of Fluid Particles and Magnetic Field Lines in the Solar Wind
Authors: N. H. Bian, Gang Li
Figure caption: A particular realization of the stationary Uhlenbeck & Ornstein (1930) process, extensively reviewed by Chandrasekhar (1943), representing here one component of the Lagrangian velocity as a function of time t. The function is Hölder continuous with H-exponent H = 1/2. In this work, the Ornstein–Uhlenbeck process is used to model the velocity and magnetic field fluctuations evaluated along fluid particle trajectories and along magnetic field lines in Alfvénic turbulence.
Paper: Lagrangian Perspectives on the Small-scale Structure of Alfvénic Turbulence and Stochastic Models for the Dispersion of Fluid Particles and Magnetic Field Lines in the Solar Wind
Authors: N. H. Bian, Gang Li
Figure caption: One-hundred realizations of stochastic magnetic field lines modeled by the integrated Ornstein–Uhlenbeck process that is not Markov. The magnetic field lines are smooth differentiable curves. Tending ﹩{L}_{\parallel }^{B}\to 0﹩ while keeping the magnetic field line diffusivity ﹩{D}_{{\rm{m}}}={L}_{\parallel }^{B}\langle \delta {B}_{\perp }^{2}\rangle /{B}_{0}^{2}﹩ finite in the model, the magnetic field lines tend to the Wiener process whose realizations have neither definite path length nor local direction. The path length L at the distance z is a random variable.
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: Color mosaics showing the JWST images for our full 19 galaxy sample developed to support a 2024 January press release, https://webbtelescope.org/contents/news-releases/2024/news-2024-105. Red is a combination of the MIRI filters (F770W, F1000W, F1130W, and F2100W), green is a combination of NIRCam and MIRI (F360M and F770W), and blue is purely NIRCam (F300M and F335M). F200W imaging has also been obtained but is not included in the color composites. Note that in many cases, these mosaics are zoomed, and so do not show the full extent of coverage of the galaxy. For the full coverage of each observation, see Figure 9.
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: Illustration of how the temporal variability of MIRI backgrounds affects the final science images, using F2100W IC 5332 observations. Left: MIRI background using later NIRCam parallel observation, as the initial observation failed. This background is therefore taken close in position to IC 5332, but not close in time. Middle: combination of IC 5332 background (close in position) and NGC 7496 background (close in time) observations. Right: using only the NGC 7496 (close in time) background observation. Clearly, using backgrounds taken closer in time leads to a better, and overall flatter 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: Multitile destriping for one F200W observation of NGC 628, having smoothed the stacked image perpendicular to the stripe axis. Left: uncorrected data. Middle: noise model. Right: corrected data. This step successfully removes the remaining striping, so having completed this step our backgrounds are flattened.
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: Single-tile destriped model for one F200W observation of NGC 628. The left panel shows the original data, the middle panel is our stripe model, and the right panel shows the destriped data. Although effective at removing much of the striping, some low-level, large-scale stripes remain.
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: Applying the single-tile destriping to Spitzer observations of M33. The left and middle panels show the original and destriped data, respectively, and are locked at the same color scale. The right panel shows the difference image, on the order of 0.001 MJy sr−1, essentially below the noise level of the original image. The white pixels in the difference image are due to pixels with no data; these are not present in the JWST noise models but are present here due to differences in the specifics of the data between JWST and Spitzer.