adsabs/AstroCLIMB huggingface dataset:
Paper: MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
Authors: E. Bachelet, Y. Tsapras, Andrew Gould, R. A. Street, David P. Bennett, M. P. G. Hundertmark, V. Bozza, D. M. Bramich, A. Cassan, M. Dominik, K. Horne, S. Mao, A. Saha, J. Wambsganss, Weicheng Zang, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Stela Ishitani Silva, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Andrzej Udalski, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: The new color–radius relation based on the (g − i) o  (left) and (r − i) o  (right) colors. For both figures, the best fit is indicated by the blue line and the 1σ uncertainty interval is displayed in light blue.
Paper: MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
Authors: E. Bachelet, Y. Tsapras, Andrew Gould, R. A. Street, David P. Bennett, M. P. G. Hundertmark, V. Bozza, D. M. Bramich, A. Cassan, M. Dominik, K. Horne, S. Mao, A. Saha, J. Wambsganss, Weicheng Zang, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Stela Ishitani Silva, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Andrzej Udalski, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: CMDs from the ROME/REA survey. The blue circles represents all stars within 2′ around the event location from the VPHAS catalog (Drew et al. 2016), while the aligned ROME/REA stars are in orange. The source and blend are represented in magenta and blue, respectively. The dashed square in the left panel represents the stars that have been used to estimate the RGC centroid for both CMDs.
Paper: MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
Authors: E. Bachelet, Y. Tsapras, Andrew Gould, R. A. Street, David P. Bennett, M. P. G. Hundertmark, V. Bozza, D. M. Bramich, A. Cassan, M. Dominik, K. Horne, S. Mao, A. Saha, J. Wambsganss, Weicheng Zang, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Stela Ishitani Silva, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Andrzej Udalski, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: (Normalized) distribution of the derived parameters for the 2L1S+POM model. The first line represents the mass, distance, and proper-motion distributions of stars from the Besançon (blue) and GalMod (orange) models. The last two lines represent the posterior distribution of the event parameters from the MCMC exploration.
Paper: MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
Authors: E. Bachelet, Y. Tsapras, Andrew Gould, R. A. Street, David P. Bennett, M. P. G. Hundertmark, V. Bozza, D. M. Bramich, A. Cassan, M. Dominik, K. Horne, S. Mao, A. Saha, J. Wambsganss, Weicheng Zang, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Stela Ishitani Silva, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Andrzej Udalski, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: CMD from the MOA survey, calibrated to the OGLE-III system, for stars located in the square 2′ × 2′ around the event. We also display the position of the source and the blend using the I measurements from the OGLE light curve.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: Results for i = 75° and i = 15°. Top panels: results for i = 75°. From left to right shows the polarization fraction, the angle difference with the spherical case, and the histogram of angle differences. Bottom panels: results for i = 15° in the same order.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The same as Figure A6 but for MRN-distributed dust grains with ﹩{a}_{\max }=1\mu {\rm{m}}﹩.
Paper: Analytic Light Curve for Mutual Transits of Two Bodies Across a Limb-darkened Star
Authors: Tyler A. Gordon, Eric Agol
Figure caption: Subdivision of the region of overlap between three circles. The total area of overlap is found by adding the areas of each of these subregions. The expressions for each area are given in the text.
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: Image magnifications for asymptotically circular image configurations, relative to the image magnifications for a source at the center of the diamond caustic. Two cases are shown, one with the source close to an axis of the diamond caustic (ϕ  s  = 2°), and a second far from either axis (ϕ  s  = 30°). The two closest images (those on the secondary branch of Witt’s hyperbola) increase in brightness inversely as their separation. By contrast, the relative magnifications of the images at θ 1 and θ 4 on the primary branch of Witt’s hyperbola vary only by factors of order unity and quickly reach limiting values, even in the cusp-like case of ϕ  s  = 2°. The convention is that of Section 4.1.
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: Outer circle: images for two different source positions for a single point-mass lens with asymptotically vanishing shear and lens strength b = 1.25. Inner circle: images formed by an SIS lens with vanishing shear (γ → 0) and b = 1. The source positions have the same causticity and astroidal angle for both circles, but the symmetry axes of the two configurations have been rotated to avoid confusion. Keeton’s lensmodel (Keeton 2010) has been used to verify the configurations.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Flagging percentages for various values of M compared to the data rate of the RFI signal. (a) BPSK modulation with a 1/W FIR cutoff. (b) BPSK modulation with a 4/W FIR cutoff. (c) 2-bit ASK modulation with a 1/W FIR cutoff. (d) 4-bit ASK modulation with a 1/W FIR cutoff.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Flagged RFI and ﹩\widehat{{SK}}\,﹩ vs. log power for a 1 ksps and 200 ksps BPSK signal. As the data rate rises, the sidelobes of the signal become much more powerful but fail to be detected by ﹩\widehat{{SK}}﹩. In panels (c) and (d), the red lines denote the acceptable ﹩\widehat{{SK}}\,﹩ thresholds. Any points that do not lie between these thresholds are flagged as RFI.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: False positive rates of ﹩\widehat{{SK}}\,﹩ on signal-free noise, depending on M.
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: Top panel: period–metallicity distribution for the 252 WD binaries in our sample with well-defined orbital solutions fit to the APOGEE RVs. The vast majority of these binaries have an orbital period of a few days but span a wide metallicity range (−0.7 < [M/H] < +0.3). A number of metal-poor ([M/H] < −1) systems are found covering a broad range of periods. Bottom panel: the CDF of the metallicity for three samples selected according to the orbital period. The solid black line represents systems with P < 100 days and the red solid line systems with P < 5 days, while the dashed line shows binaries where P > 100 days. Systems with shorter orbital periods tend to have higher metallicity.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for Type II Cepheids
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Jing-Yi Henderson, Matthew J. Graham, Russ R. Laher, Michael S. Medford, Josiah Purdum, Ben Rusholme
Figure caption: Left panel: comparison of the slopes (top panel), zero-points (ZPs; middle panel), and the dispersions (bottom panel) for PL relations derived in Bhardwaj (2022, for BVIJHK band, in open symbols) and the preliminary gri-band PL relations using TIICs listed in Table 1 (in filled symbols). Right panel: same as the left panel, but for the updated PL relations as described in Section 4.2.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for Type II Cepheids
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Jing-Yi Henderson, Matthew J. Graham, Russ R. Laher, Michael S. Medford, Josiah Purdum, Ben Rusholme
Figure caption: ZTF light curves for V6 in M2 folded with the period determined from LombScargleMultiband (left panel) and twice that of the determined period (right panel). Alternate minima can be seen when the determined period is doubled. The black curves are the fitted low-order Fourier expansion given in Equation (1). Crosses are rejected outliers based on the two-step fitting process (see the text for details).
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for Type II Cepheids
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Jing-Yi Henderson, Matthew J. Graham, Russ R. Laher, Michael S. Medford, Josiah Purdum, Ben Rusholme
Figure caption: Examples of ZTF light curves for TIICs in three different period ranges roughly represent the three subtypes (BL Herculis, W Virginis, and RV Tauri) of TIICs. The black curves are the fitted low-order Fourier expansion given in Equation (1). Crosses are rejected outliers based on the two-step fitting process (see the text for details).
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: The S/N distribution with frequency of clock oscillator harmonics. The statistics here involve 298 clock oscillator harmonics in Beam 1. Some of them are not detected by turboSETI, but are visible on the waterfall plots. If a signal is totally absent from the waterfall plots in one polarization (but present in the other polarization), then the S/N of the signal in that polarization is determined as 1. (a) The S/N distribution in XX and YY. (b) The ratios of S/N of YY to XX in logarithm. The signals above the horizontal dashed line are stronger in YY than in XX; otherwise stronger in XX than in YY.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: Waterfall plots of the neutral hydrogen line in the observation toward Kepler-438 (top panels) and NBS 210629 (bottom panels). The left panels show XX, and the right panels show YY. The strengths of XX and YY of neutral hydrogen line are similar, while NBS 210629 appears obviously stronger in YY than in XX.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: Waterfall plots around 1140.604 MHz of the observations toward Kepler-438 and other 8 sources. The left panels show XX, and the right panels show YY. The 8 weak signals we find for comparison with NBS 210629 are the drifting ones visible on the right panels. They are only present in Beam 1 and YY, consistent with NBS 210629.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Surfaces of sections in the g 1 = 0 plane, with different masses of γ Cep Ab, by varying the perturbation Hamiltonian ﹩{ \mathcal H }({\rm{\Delta }}h\to \pi )﹩. Panels (a), (c), and (e): dynamical maps for m 1 = 11 M Jup. Panels (b), (d), and (f): dynamical maps for m 1 = 15 M Jup.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Distributions of the maximum i mut for S-type planetary systems with various initial SMA a 1 and eccentricities e 1, e 2. Each diagram has specific initial parameters a 1 and a 2. The color bar on the right represents the maximum value of i mut over 100 Myr, while the regions in dark red represent orbits with i mut excited up to 180°.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Distribution of the maximum i mut for S-type planets, with a 1 = 2 au and a 2 = 20 au. Panel (a): m 1 = 11 M Jup. Panel (b): m 1 = 15 M Jup. The color bar on the right represents the maximum value of i mut over 100 Myr.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Two examples of Hamiltonian level curves with m 1 = 11 M Jup and 15 M Jup in the (e 1, g 1) plane, where e 2 and G tot are fixed. The blue circles and green curves are resonant and oscillating orbits with equilibrium points of 90° and 180°, respectively.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: (a): spatial distribution for the cluster members and 88 variable stars, (α  J2000 δ  J2000). (b): proper motion distribution for them. (c): histogram of parallax (ω) for cluster members (black line) and variable stars located in the area of 3σ  ω  boundary (gray dashed lines). The histogram of members’ parallax is fitted with a single Gaussian profile(red dashed line). (d): spatial distribution for the cluster members and circled variable stars in (c) with their tangential velocities. Arrows point out the direction of tangential velocities for each star and arrow length is in proportion to the tangential speed. In the top panels, light gray dots mean the complete samples of observation, and black dots represent 328 cluster members. Red, blue, green, and orange circles represent eclipsing binaries, pulsators, rotating variables, and unclear variables, respectively. Solid and hollow refer to whether they are matched members of NGC 2355.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: CMD of open cluster NGC 2355 with isochrone and the instability strip of δ Scuti stars. Gray dots represent the 328 member stars of open cluster NGC 2355 by Cantat-Gaudin et al. (2018). The PARSEC isochrones of 700, 800, and 900 Myr with metallicity [Fe/H]=-0.07 and extinction A  V  = 0.744 are indicated by the blue dashed, green dashed, and red solid lines, respectively. The approximate range of theoretical pulsation instability strip on the isochronous line is pointed by two black dashed lines. Different types of member variable stars are plotted with different symbols in the diagram the same as described in Figure 9.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: The (U − B) vs. (B − V) color–color diagram of the open cluster NGC 2355. The black solid curve line represents the locus of Turner (1976, 1979) ZAMS for solar metallicity. The red solid curve line is fitted to the black hollow circle by translating over the ZAMS with the condition given in the text.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: Observed HST F850LP sky surface brightness from observations in the GOODS North fields against various telescope attitude angles. In order to assess the sensitivity of the parameters to stray light, we selected a field with high ecliptic latitudes and minimal time-variable zodiacal light contribution. Top-left panel: Sun altitude shows a strong correlation with the sky surface brightness. This indicates observations taken at nighttime (i.e., Sun altitude <0°) lead to a lower measured sky, presumably due to minimal stray light from earthshine. Observations over the daytime (i.e., Sun altitude >0°) portion of Earth show a higher sky surface brightness likely from increased earthshine stay light contributions. Top-right panel: sky surface brightness as a function of limb angle. Observations over a daytime Earth show a correlation with limb angle, indicating the angular distance between a target field and Earth impacts the amount of earthshine stray light entering the telescope. For nighttime observations taken in Earth’s shadow, there appears to be little correlation until very low limb angles of <20°) are reached. Lower panels: Sun angles below ∼80° and Moon angles below ∼70° also show correlations as sky surface brightness increases as HST points closer to the Sun and Moon, respectively. The variation in the minimum observed sky is likely due to the variations in the zodiacal light intensity with time.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: In this study, four key angles are used to describe the relationship between the orientation of the telescope and potential sources of stray light. The four angles and the vectors that define them are illustrated in this figure. The primary scattering area is from a circular region defined by the visible horizon from a given orbital altitude. For this work, angles are defined from the midpoint of a given exposure with respect to the surface of Earth, the Moon, or the Sun.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: The observed sky surface brightness in the GOODS North fields and the COSMOS fields in F850LP and F814W filters, respectively. Observations are colored by the mean Sun altitude at which the observation was taken. The predicted zodiacal light is shown in gray. For the GOODS North field on the left panel, which is high off the ecliptic plane, data points scatter upward from the baseline zodiacal models by as much as 34% of the total observed sky surface brightness. These data points correspond to observations with high Sun altitudes, which are consistent with the idea that increased earthshine is able to get into the telescope at higher Sun altitudes (see Figure 2). For the COSMOS field on the right panel, we see the data approximately follows the predicted zodiacal light variation with time. Scatter to higher sky surface brightness reflects various observed Sun altitudes on approximately the same date.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: Sky surface brightness vs. total irradiance from the space-based CERES weather data. Sky surface brightness data are from the F850LP filter in the GOODS North field. CERES irradiance is the sum of CERES flux from observations in the estimated region on Earth directly below HST during an exposure. The data generally show a correlation, indicating that the specific weather or region on Earth below Hubble at least partially determines the sky surface brightness levels. We note this is direct evidence that stray light from earthshine can significantly impact HST sky surface brightness estimates. The data show significant scatter, especially at higher CERES fluxes. Colors show three different limb angle bins with lines fit to each to highlight an underlying correlation. Higher limb angles result in a shallower relationship, likely because HST is pointing farther away from Earth and hence will receive less stray light from earthshine.