adsabs/AstroCLIMB huggingface dataset:
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Panel (a): elliptical annuli overlaid on the gas-phase abundance map of 12+log(O/H), identical to Figure 10(c). Panel (b): radial metallicity profiles of AGC 102004 (red dots) and AGC 111629 (blue dots), derived using the [N2] index (M. Pettini & B. E. J. Pagel 2004). The profile of AGC 111629 is obtained from Panel (a), while that of AGC 102004 is adopted from Figure 8(c) in T.-W. Cao et al. (2024b). In both cases, low-signal spaxels are included, and the Hα morphology parameters from GALFIT are used to compute the mean 12+log(O/H) values within elliptical annuli.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Color image of AGC 111629 and its satellite galaxy AGC 748815, based on smoothed Legacy Survey DR9 data (https://www.legacysurvey.org/viewer). Both galaxies are marked. The HI spectra from ALFALFA show that the two galaxies share the same velocity. A diffuse structure is clearly visible between AGC 111629 and AGC 748815. 1″ corresponds to 0.43 kpc.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Power-law fit to the correlation between tcond and t2 for both LMC and Galactic novae. The black solid line represents the best-fit relation, ﹩{t}_{{{\rm{cond}}}}=5.34\times {t}_{2}^{0.67}﹩, while the shaded region indicates the 1σ confidence interval. The lower panel displays the residuals of the fit. The red solid line represents the fit for LMC novae only, ﹩{t}_{{{\rm{cond}}}}=5.49\times {t}_{2}^{0.65}﹩. The dashed green and blue lines show the derived fits from S. Williams et al. (2013) for graphite and ACH2 grains, respectively.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Correlation between the dust tcond and t2 for novae in the LMC. The observed trend is consistent with previous studies of Galactic (A. Shafter et al. 2011; S. Williams et al. 2013).
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: The SED shows a best-fit blackbody to the WISE data taken on day 395, with a temperature of about 700 K.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Detection probability maps in mass and semimajor axis space for each survey target, demonstrating sensitivity to Saturn-mass exoplanets around all targets, and specifically to Saturn-mass exoplanets with a Saturn-like semimajor axis (9.5 au) around at least six of the nine targets. We show the mass sensitivity achieved in the F444W filter, as the Ames-Cond, ATMO-CEQ, and BEX-petitCODE cooling curves predict substellar objects to be the brightest in this filter as compared to F356W. The solid white lines show detection probability contours of 50%, 80%, and 95%, and the hatched region shows where our observations are sensitive to masses below the lower limit of the available model grids for a given target’s age, and thus we have extrapolated the cooling curves to lower masses (lower temperatures) for visualization purposes. The mass sensitivity of the GTO 1184 survey surpasses the low-mass limit of available planet evolution and atmosphere grids for every target, regardless of age or intrinsic brightness.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: SNRE maps of all targets in GTO 1184, in the F444W filter. All observations were reduced with RDI using the full library of reference PSFs. Point-like and extended sources are labeled in the images (with names beginning with “P” and “E,” respectively), and the point-like sources are magnified in the image insets. Extended background sources are abundant in the survey, and the edge-on disk of AU Mic is clearly detected.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Results of data reduction steps for GTO 1184 target G 7-34 (roll 1 in the F444W filter), using the JWST Calibration Pipeline wrapped by spaceKLIP (J. Kammerer et al. 2022; H. Bushouse et al. 2023). We also include additional custom processing steps for flagging cosmic-ray (CR) persistence. Panel (a) shows the raw data as downloaded from the MAST archive. Panel (b) shows the output of the first stage of the pipeline, which flags and corrects for detector-level errors. Panel (c) shows the output of the second stage, which corrects instrument-specific errors, smooths over unreliable pixels, and converts the image to physical fluxes. Significant residual starlight is still present in the center of the frame, which needs to be removed with PSF-subtraction techniques.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: 5σ contrast sensitivity curves for different PSF-subtraction techniques and reference PSF choices applied to the G 7-34 observation in F444W, as a function of angular separation from the target star. The teal, blue, and purple lines show the results for ADI, RDI, and ADI + RDI, respectively. Reductions using the full library of PSF references are shown with a solid line, those using only HIP 17695 as a reference are shown with a dashed line, and those using no references (ADI only) are shown with a dotted line. The 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 coronagraph IWA is shown as a vertical gray dashed line. We can see that RDI and ADI + RDI outperform ADI alone at nearly all separations, regardless of the number of references used.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: SNRE maps of all targets in GTO 1184, in the F356W filter. All observations were reduced with RDI using the full library of reference PSFs. Point-like and extended sources are labeled in the images (with names beginning with “P” and “E,” respectively), and the point-like sources are magnified in the image insets. In cases where the candidate source is not detected in the F356W filter, we still label it and provide an inset image to demonstrate its nondetection. Extended background sources are abundant in the survey, and the edge-on disk of AU Mic is clearly detected.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Results of PSF subtraction via ADI, RDI, and ADI + RDI using spaceKLIP, for G 7-34 in the F444W filter. The positive signal is shown in red, and the negative signal (due to subtraction artifacts) is shown in blue. Panel (a) shows the ADI result, where each off-axis source has clear negative residuals due to the 10∘ roll angle difference. Panel (b) shows the RDI result using only HIP 17695 (the target star with the cleanest FOV) as a reference, and panel (c) shows the ADI + RDI result, which is performed just like the RDI method but including the second roll of the science target as an element in the reference PSF library (J. Kammerer et al. 2022).
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Examples of the two different approaches used for forward-model PSF fitting, showing source P1 near TYC 5899 as an example. The left column shows the image data, the center column shows the best-fit PSF model, and the right column shows the residuals. The result from the LSQ PSF fitting routine are shown in the top row, while the default spaceKLIP fitting routine is shown in the bottom row and produces a similar result.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: The 5σ mass sensitivity curves for the G 7-34 observations, as a function of angular separation from the target star, demonstrate extremely deep mass sensitivity with the F444W filter (in red) as compared to the F356W filter (in blue). Due to this difference in sensitivity, we expect significantly sub-Jupiter-mass companions to appear as “F356W dropouts,” e.g., being detectable at F444W, but not at F356W. The masses are derived from the BEX-petitCODE cooling curve models, and the hatched region shows where we have extrapolated the model grid to temperatures below the lower limit of 150 K.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: The median 5σ sensitivity curves for the entire survey in the F444W filter (red lines) and F356W filter (blue lines). The sensitivity is given in units of planet–star flux contrast in the upper panel, and apparent magnitude in the lower panel. The coronagraph IWA is shown in the gray dashed line. The separations where only partial coverage exists due to square framed observations at multiple roll angles are shown by the gray shaded region. We demonstrate deep limits in absolute flux at close angular separations.
Paper: Modeling the Optical Impact of the Second-generation Starlink Satellite Constellation
Authors: Ian J. Muirhead, Nicholas H. Crisp, Ciara N. McGrath, Peter C. E. Roberts
Figure caption: Example illumination analysis extract centered on a latitude of λ = +30° in the showing the Starlink Gen2 visibility by altitude grouping on the northern hemisphere winter solstice. Figure 3(a) shows a constellation LOS illumination extract as night falls and is separated by VLEO (top) and traditional LEO (bottom) groupings. Figure 3(b) contains skyplots showing the modeled LOS constellation illumination at λ = +30° and terrestrial height 2500 m ASL at astronomical dusk (top) and +30 minutes later (bottom). A gray mask has been applied for elevations below ﹩{\epsilon }_{{\rm{\min }}}=30^\circ ﹩ and the direction of the Sun below the horizon is indicated.
Paper: Modeling the Optical Impact of the Second-generation Starlink Satellite Constellation
Authors: Ian J. Muirhead, Nicholas H. Crisp, Ciara N. McGrath, Peter C. E. Roberts
Figure caption: The changing LOS illumination of the Starlink Gen2 constellation by latitude (λ) for a 24 hr period (midday to midday) on the December solstice above the (a) visible and (b) astronomical horizons. Plots are separated into all constellation layers A to I (top), VLEO layers A to D <450 km (middle), and traditional LEO layers E to I >450 km (bottom) and the local dawn/dusk points are superimposed and identified by the associated Sun angle key. Note the differing scale of (a) and (b) as shown by the respective colourbars.
Paper: Modeling the Optical Impact of the Second-generation Starlink Satellite Constellation
Authors: Ian J. Muirhead, Nicholas H. Crisp, Ciara N. McGrath, Peter C. E. Roberts
Figure caption: 24 hr mean Starlink Gen2 satellites visible by latitude in line-of-sight (but not necessarily illuminated) above the horizon (1(a)) and ﹩A\left(z\right)\approx 2.0﹩ (1(b)). The plots show the full constellation, layers A–D <450 km, and layers E–I >450 km. Irregularities in the curves are caused by the motion of the constellation as modeled over the time period.
Paper: An Early Look at the Performance of IGRINS-2 at Gemini-North with Application to the Ultrahot Jupiter, WASP-33 b
Authors: Yeon-Ho Choi, Ueejeong Jeong, Jae-Joon Lee, Hyun-Jeong Kim, Heeyoung Oh, Chan Park, Changwoo Kye, Luke Finnerty, Micheal R. Line, Krishna Kanumalla, Jorge A. Sanchez, Peter C. B. Smith, Sanghyuk Kim, Hye-In Lee, Woojin Park, Youngsam Yu, Yunjong Kim, Moo-Young Chun, Jae Sok Oh, Sungho Lee, Jeong-Gyun Jang, Bi-Ho Jang, Hyeon Cheol Seong, Cynthia B. Brooks, Gregory N. Mace, Hanshin Lee, John M. Good, Daniel T. Jaffe, Kang-Min Kim, In-Soo Yuk, Narae Hwang, Byeong-Gon Park, Hwihyun Kim, Brian Chinn, Francisco Ramos, Pablo Prado, Ruben Diaz, John White, Eduardo Tapia, Andres Olivares, Valentina Oyarzun, Emma Kurz, Hawi Stecher, Carlos Quiroz, Ignacio Arriagada, Thomas L. Hayward, Hyewon Suh, Jen Miller, Siyi Xu, Emanuele Paolo Farina, Charlie Figura, Teo Mocnik, Zachary Hartman, Mark Rawlings, Andrew Stephens, Bryan Miller, Kathleen Labrie, Paul Hirst, Byeong-Cheol Lee
Figure caption: Atmospheric model spectra for WASP-33 b’s dayside, showing contributions from individual molecular species (CO, H2O, and OH). The gray-shaded boxes represent the spectral orders used for CO detection. The right panel shows the corresponding P-T profile and emission contribution functions. The models were generated with petitRADTRANS using a Guillot P-T profile.
Paper: An Early Look at the Performance of IGRINS-2 at Gemini-North with Application to the Ultrahot Jupiter, WASP-33 b
Authors: Yeon-Ho Choi, Ueejeong Jeong, Jae-Joon Lee, Hyun-Jeong Kim, Heeyoung Oh, Chan Park, Changwoo Kye, Luke Finnerty, Micheal R. Line, Krishna Kanumalla, Jorge A. Sanchez, Peter C. B. Smith, Sanghyuk Kim, Hye-In Lee, Woojin Park, Youngsam Yu, Yunjong Kim, Moo-Young Chun, Jae Sok Oh, Sungho Lee, Jeong-Gyun Jang, Bi-Ho Jang, Hyeon Cheol Seong, Cynthia B. Brooks, Gregory N. Mace, Hanshin Lee, John M. Good, Daniel T. Jaffe, Kang-Min Kim, In-Soo Yuk, Narae Hwang, Byeong-Gon Park, Hwihyun Kim, Brian Chinn, Francisco Ramos, Pablo Prado, Ruben Diaz, John White, Eduardo Tapia, Andres Olivares, Valentina Oyarzun, Emma Kurz, Hawi Stecher, Carlos Quiroz, Ignacio Arriagada, Thomas L. Hayward, Hyewon Suh, Jen Miller, Siyi Xu, Emanuele Paolo Farina, Charlie Figura, Teo Mocnik, Zachary Hartman, Mark Rawlings, Andrew Stephens, Bryan Miller, Kathleen Labrie, Paul Hirst, Byeong-Cheol Lee
Figure caption: Detection of molecules (CO+H2O+OH) in WASP-33 b’s dayside atmosphere. Top panel: trail plot showing cross-correlation coefficients calculated from the post-SVD residual data using the composite atmospheric model of WASP-33 b. The dashed red line indicates the expected radial velocity of the planet (Kp = 226.0 km s−1), while the white horizontal dashed line indicates the ingress phase (ϕ = 0.451) of WASP-33 b. Bottom panel: Kp–ΔVsys map of SNR detection with a peak value of 7.4. The peak position (black cross) is well consistent with the expected planetary radial velocity and system velocity (Vsys = −9.2 km s−1 from G. A. Gontcharov 2006), indicated by the dashed white lines.
Paper: An Early Look at the Performance of IGRINS-2 at Gemini-North with Application to the Ultrahot Jupiter, WASP-33 b
Authors: Yeon-Ho Choi, Ueejeong Jeong, Jae-Joon Lee, Hyun-Jeong Kim, Heeyoung Oh, Chan Park, Changwoo Kye, Luke Finnerty, Micheal R. Line, Krishna Kanumalla, Jorge A. Sanchez, Peter C. B. Smith, Sanghyuk Kim, Hye-In Lee, Woojin Park, Youngsam Yu, Yunjong Kim, Moo-Young Chun, Jae Sok Oh, Sungho Lee, Jeong-Gyun Jang, Bi-Ho Jang, Hyeon Cheol Seong, Cynthia B. Brooks, Gregory N. Mace, Hanshin Lee, John M. Good, Daniel T. Jaffe, Kang-Min Kim, In-Soo Yuk, Narae Hwang, Byeong-Gon Park, Hwihyun Kim, Brian Chinn, Francisco Ramos, Pablo Prado, Ruben Diaz, John White, Eduardo Tapia, Andres Olivares, Valentina Oyarzun, Emma Kurz, Hawi Stecher, Carlos Quiroz, Ignacio Arriagada, Thomas L. Hayward, Hyewon Suh, Jen Miller, Siyi Xu, Emanuele Paolo Farina, Charlie Figura, Teo Mocnik, Zachary Hartman, Mark Rawlings, Andrew Stephens, Bryan Miller, Kathleen Labrie, Paul Hirst, Byeong-Cheol Lee
Figure caption: Cross-correlation results for CO, H2O, and OH in WASP-33 b’s atmosphere. The detection significance reaches SNR values of 6.3 for CO, 4.7 for H2O, and 4.2 for OH. The dashed white lines indicate the expected values for the planet’s radial velocity and the system velocity from the literature, and the black cross marks the peak value of the SNR.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The different bandpasses used by (a) TESS (image credit: G. R. Ricker et al. 2015) and (b) the Sony-α 7R II (ILCE-7RM2) DSLR camera (image credit: K. Sato et al. 2016) (a). Here, we show the “TESS spectral response function (black line), defined as the product of the long-pass filter transmission curve and the detector quantum efficiency curve. Also plotted, for comparison, are the Johnson-Cousins V, RC, and IC filter curves and the Sloan Digital Sky Survey z filter curve. Each of the functions has been scaled to have a maximum value of unity” (G. R. Ricker et al. 2015). (b) The Sony-α 7R II uses an Exmor R CMOS sensor, and here its spectral response function for each image band is shown, where each function has been scaled to a maximum value of unity as well.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The image processing pipeline steps and their products. The arrows indicate the products of each step and where they will be used.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: Arrangement of pixels sensitive to different colors in superpixels (highlighted area) in a DSLR detector.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The source extraction vs. catalog projections of our astrometry step placed on top of the corresponding FITS image, where blue squares are the catalogs projected sources and red squares are the extracted sources from our astrometry.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The change in magnitude vs. phase plot of TX Ursae Majoris (TX UMa, GDR3 829685534384441344, Gaia G magnitude 6.9229). We determined its period to be 3.0633368 days from combining TESS and our data. (a.) Our light curve points (corresponding to each color channel (i.e., red, green, and blue)) are binned (each corresponding color channel (i.e., red, green, and blue) circle points) and folded by the period. The corresponding TESS light curves (sectors 21 and 48, black points) are included. (b.) The zoomed-in plot shows the clear changes in the light curves per color channel and changes in each TESS light curve.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The change in magnitude vs. phase plot of GQ Dra (GDR3 1415133175038821888). We determined its period to be 0.765901 days from combining TESS and our data. (a.) Our combined light curve points (teal) are binned (circle teal points) and folded by the period. The corresponding TESS light curves (sectors 74, 78, 80, and 84, black points) are included. (b.) The binary system showed no color dependence (no obvious variance in red, blue, or green data points).
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The scatter (median absolute deviation from the median (MAD)) of the combined channel completely processed (i.e., after performing magnitude fitting, EPD, and TFA steps) light curves vs. GAIA G magnitude (black points) for fields G262 (a), (b), G111 (c), (d), and G139 (e), (f) for dither patterns D25 (left) and D26 (right). For comparison, the red channel scatter is also shown (red points)
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The change in magnitude vs. phase plot of V0551 Dra (GDR3 1431129011933593088, Gaia G magnitude 11.5235). We determined its period to be 0.329331 days from combining TESS and our data. (a.) Our light curve points (teal) are binned (circle teal points) and folded by the period. The corresponding TESS light curves (sectors 15, 16, 19, 22, 23, 24, 25, 49, 50, 51, 52, 56, 59, 76, 77, 78, 79, 83, and 86; black points) are included. (b.) The binary system showed no color dependence (no obvious variance in red, blue, or green data points).