adsabs/AstroCLIMB huggingface dataset:
Paper: New Ultracool Companions to Nearby White Dwarfs
Authors: Alexia Bravo, Adam C. Schneider, Sarah Casewell, Austin Rothermich, Jacqueline K. Faherty, Jenni R. French, Thomas P. Bickle, Aaron M. Meisner, J. Davy Kirkpatrick, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, John H. Debes, Arttu Sainio, Léopold Gramaize, Frank Kiwy, Peter A. Jałowiczor, Awab Abdullahi
Figure caption: GBP −GRP vs. G −W2 colors for Gaia white dwarfs within 100 pc from N. P. Gentile Fusillo et al. (2021). Objects on the normal white dwarf color sequence are displayed as orange dots. Objects showing signs of infrared excess were selected as having redder G − W2 colors than the dashed line. The color positions of previously known excess sources and newly discovered excess candidates selected via Method I are shown as blue squares and red diamonds, respectively. Rejected excess candidates are shown with gray x symbols.
Paper: New Ultracool Companions to Nearby White Dwarfs
Authors: Alexia Bravo, Adam C. Schneider, Sarah Casewell, Austin Rothermich, Jacqueline K. Faherty, Jenni R. French, Thomas P. Bickle, Aaron M. Meisner, J. Davy Kirkpatrick, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, John H. Debes, Arttu Sainio, Léopold Gramaize, Frank Kiwy, Peter A. Jałowiczor, Awab Abdullahi
Figure caption: Three color RGB optical and WISE images of all new unresolved candidates. Optical images either come from Pan-STARRS (PS1; K. C. Chambers et al. 2016) or DECam images obtained through the Astro Data Lab image cutout service (M. J. Fitzpatrick et al. 2014; R. Nikutta et al. 2020). WD identifiers are listed for each object.
Paper: New Ultracool Companions to Nearby White Dwarfs
Authors: Alexia Bravo, Adam C. Schneider, Sarah Casewell, Austin Rothermich, Jacqueline K. Faherty, Jenni R. French, Thomas P. Bickle, Aaron M. Meisner, J. Davy Kirkpatrick, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, John H. Debes, Arttu Sainio, Léopold Gramaize, Frank Kiwy, Peter A. Jałowiczor, Awab Abdullahi
Figure caption: IRTF/SpeX spectra of four newly discovered companions. All spectra are normalized between 1.27 and 1.29 μm. WD J0806+2215B is best matched to the the L3 spectral standard (2MASSW J1506544+132106; A. J. Burgasser 2007), while WD J2025+3515B, WD J2119+4206B, and WD J2355+5131B are best matched to the M8 spectral standard (VB 10; A. J. Burgasser et al. 2004).
Paper: New Ultracool Companions to Nearby White Dwarfs
Authors: Alexia Bravo, Adam C. Schneider, Sarah Casewell, Austin Rothermich, Jacqueline K. Faherty, Jenni R. French, Thomas P. Bickle, Aaron M. Meisner, J. Davy Kirkpatrick, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, John H. Debes, Arttu Sainio, Léopold Gramaize, Frank Kiwy, Peter A. Jałowiczor, Awab Abdullahi
Figure caption: Spectral binary fits to the Gaia spectra of WD J1125−1631, WD J1657−1256, and WD J2339+2552. White dwarf spectra are shown in cyan, M dwarf spectra are shown in red, and the combined white dwarf + M dwarf templates are shown in purple. The observed Gaia spectra for these three unresolved candidates are shown in black.
Paper: New Ultracool Companions to Nearby White Dwarfs
Authors: Alexia Bravo, Adam C. Schneider, Sarah Casewell, Austin Rothermich, Jacqueline K. Faherty, Jenni R. French, Thomas P. Bickle, Aaron M. Meisner, J. Davy Kirkpatrick, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, John H. Debes, Arttu Sainio, Léopold Gramaize, Frank Kiwy, Peter A. Jałowiczor, Awab Abdullahi
Figure caption: Three color RGB images of all new resolved candidates. White dwarf primaries are marked with yellow lines while candidate ultracool companions are marked with red lines. The WD 0807−5350 system has only r- and g-band DECam images, and thus the candidate companion is difficult to see in the image (though is resolved in Gaia). Note that the “unreliable” candidates are not included in this figure.
Paper: A Small Brown Dwarf in an Aligned Orbit Around a Young, Fully Convective M Star
Authors: Madison Brady, Jacob L. Bean, Gumundur Stefánsson, Nina Brown, Andreas Seifahrt, Ritvik Basant, Tanya Das, Rafael Luque, Julian Stürmer
Figure caption: The field around LP 261-75 in TESS sector 21, with the pipeline aperture outlined in red. Red circles indicate other stars known from Gaia DR3, with their size indicating their flux relative to LP 261-75. The results from sector 48 are similar and thus not included. This figure was generated using tpfplotter.
Paper: New Ultracool Companions to Nearby White Dwarfs
Authors: Alexia Bravo, Adam C. Schneider, Sarah Casewell, Austin Rothermich, Jacqueline K. Faherty, Jenni R. French, Thomas P. Bickle, Aaron M. Meisner, J. Davy Kirkpatrick, Marc J. Kuchner, Adam J. Burgasser, Federico Marocco, John H. Debes, Arttu Sainio, Léopold Gramaize, Frank Kiwy, Peter A. Jałowiczor, Awab Abdullahi
Figure caption: Gemini/GMOS-N spectrum of WD J0400−2611 showing clear Hα absorption and a lack of He lines.
Paper: Earth Detecting Earth: At What Distance Could Earth’s Constellation of Technosignatures Be Detected with Present-day Technology?
Authors: Sofia Z. Sheikh, Macy J. Huston, Pinchen Fan, Jason T. Wright, Thomas Beatty, Connor Martini, Ravi Kopparapu, Adam Frank
Figure caption: The maximum distances that each of Earth’s modern-day technosignatures could be detected at using modern-day receiving technology, in visual form. Also marked are various astronomical objects of interest.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: Phase-folded light curves of 10 targets from TMTS. The L band is the TMTS Luminous filter.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred center displacements of the planet’s shadow disk: Δci,xi, Δci,yi, Δce,xe, and Δce,ye. The dots represent the median values from MCMC sampling, and the error bars represent the 68% credible intervals. The colored dots indicate the case using α(λ) estimated from (Ttot + Tfull)/2, while the small gray dots indicate the case using α(λ) = 1. The bottom panels show the distribution of displacement values converted from MCMC sampling at selected wavelengths, which are indicated by open dots in the top and middle panels. The dotted lines represent the X-axis and Y-axis, and the dashed lines represent the xi-axis and yi-axis for the left-side four panels and the xe-axis and ye-axis for the right-side four panels. The edge of the host star is plotted as black solid lines, which are nearly aligned with the yi-axis or ye-axis. The distribution along the host star’s edge is clearly visible.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of k = Rp/Rs, the timing of ingress ti, the timing of egress te, the duration of ingress τi, and the duration of egress τe for an asymmetric planet, based on the MCMC analysis of simulated data. The dots represent the median values from the MCMC sampling, while the error bars indicate the 68% credible intervals. Results are shown for both noiseless data and data with added Gaussian noise (mean = 0, standard deviation = 250 ppm), along with the true values (colored lines). The values for a symmetric planet are also plotted (gray lines). The inferred τi and τe are identical because a circular orbit model was used in the analysis. In the panel for τi and τe, the true values of both are plotted but are difficult to distinguish as the lines are very close and nearly overlap.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩, and ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩ for an asymmetric planet, based on the MCMC analysis of simulated data. The values were converted using the estimated orbital parameters. The dots represent the median values from the MCMC sampling, while the error bars indicate the 68% credible intervals. Results are shown for both noiseless data and data with added Gaussian noise (mean = 0, standard deviation = 250 ppm), along with the true values. The arrangement of the panels reflects the positional relationship between the regions on the planet contributing to each spectrum, as viewed from the night side. The central panel shows the planet viewed from the night side, along with the xi-axis, yi-axis, xe-axis, and ye-axis.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of the timing of ingress ti, the timing of egress te, and the duration of ingress and egress τ. The dots with error bars represent the median values from the MCMC sampling with 68% credible intervals. The solid blue lines (using α(λ) estimated from (Ttot + Tfull)/2) and the dashed gray lines (using α(λ) = 1) represent these values in the case of a completely symmetrical atmosphere, derived from the orbital parameters of the planet’s center of mass and the inferred planetary radii.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Partial derivatives of Δci,xi (left) and Δce,xe (right) with respect to each orbital parameter. The functions used to estimate the partial derivatives were Δci,xi and Δce,xe, which were derived by converting the median values of k, tI, tII, tIII, and tIV obtained from the MCMC analysis using the orbital parameters estimated from the same analysis. Δci,xi and Δce,xe are also shown in the top panels, along with the true values.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of all the parameters in the light-curve model obtained from the MCMC sampling. For the limb-darkening coefficients, the inferred values at the minimum and maximum wavelengths, along with the wavelength dependence for each sampling, are shown. u1 and u2, converted from q1 and q2, are also displayed. The dots represent the median values of the MCMC sampling, and the error bars indicate the 68% credible intervals. The open dots indicate the wavelengths that exhibit radii smaller than the 10th percentile and are used to determine the orbit of the planet’s center of mass.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of Δci,xi, Δce,xe, and ΔcY during ingress and egress for an asymmetric planet, based on the MCMC analysis of simulated data. The values were converted using the estimated orbital parameters. The dots represent the median values from the MCMC sampling, and the error bars indicate the 68% credible intervals. Results are shown for noiseless data (left) and data with added Gaussian noise (mean = 0, standard deviation = 250 ppm) (right), along with the true values.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Result of light-curve fitting at 4080 nm. The black dots represent the data. The orange line shows the median of the MCMC sampling, and the blue region represents the 68% credible interval. The residuals are the differences between the data and the median of the MCMC sampling. The gray vertical line indicates the median of the inferred central transit time, t0. The dark gray region represents the median of the inferred total duration, Ttot. The light gray region represents the median of the inferred full duration, Tfull.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred value of (Ttot + Tfull)/2 and its linear regression line (blue solid line). The dots with error bars represent the median values of the MCMC sampling and the 68% credible intervals.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: Light variations of OGLE-BLAP-006. (Left) Top panel displays the KMTNet I-band data, spanning eight years from 2016, with distinct colors for each year. The phase diagram in the middle reveals notable annual changes in the phase of maximum brightness, indicating pulsation timing variations. The pulsation phases were computed using the primary frequency f1 from the Fourier amplitude spectrum in the bottom panel. The inset offers a close-up view of prewhitening results around the frequency f1, marked by a vertical red line, highlighting prominent side peaks due to the timing variations. −nf1 represents the prewhitening process that subtracts light variations linked to f1 and its harmonics. (Right) Phase diagrams corrected for timing variations using the O − C values from Figure 4 are shown for three data sets: from the top, the KMTNet I, V, and OGLE I bands. Red lines represent synthetic fitting curves, with fitting error bars in the bottom right of each panel.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: O − C diagram for the pulsation period of OGLE-BLAP-006. The OGLE and KMTNet data were divided into 1.0 yr and 0.5 yr segments, respectively, to derive the observed times of maximum light. The red curve in the top panel represents a model parabola with a period change rate of (1/P)(dP/dt) =  −4.51  ×  10−7 yr−1. The black curve is of the model that combines the parabola with two LTT terms; the residuals of the model fit are shown in the bottom panel. The middle panel displays the two LTT terms: a blue dashed curve for the inner companion, a red dashed curve for the outer companion, and a thick black curve for their combined model. The error bars in the O − C values, derived from phase errors (σϕ1), were doubled, as recommended by G. Handler et al. (2000).
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: Fourier amplitude spectra of OGLE-BLAP-006 after correcting for timing variations. (Left) Upper panel displays the KMTNet I-band spectrum, showing higher amplitudes than those obtained before the timing correction in Figure 1. The prewhitening process in the lower panel reveals four new frequencies, f2 to f5. Frequencies with amplitudes above the horizontal blue dashed line of S/N = 4.0 are 1.0 day−1 aliasing sidelobes and close frequencies. (Right) Upper and lower panels show prewhitening results for the KMTNet V and OGLE I bands, respectively. The vertical red lines indicate frequencies f2 to f5 identified in the KMTNet I-band data. The OGLE spectrum exhibits 1.0 day−1 aliasing sidelobes with significantly higher amplitudes than those in the KMTNet.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: Fourier spectra of OGLE-BLAP-006 from KMTNet I-band data separated by year, with an arbitrary offset on the y-axis. These zoomed-in views focus on six frequencies: f1, 2f1, and f2 to f5. Notable frequency changes appear in f2, f3, and f4.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Moment 0 maps (top), moment 1 maps (middle), and spectra (bottom) for the Particle SPH (left), Scanline Tracing SPH (middle), and MFM (right) constructed from noiseless mock H I cubes of Galaxy 467 of the SIMBA 50 Mpc simulation taken at a distance of 20 Mpc with WALLABY observation parameters. The ring in the bottom left corner of the first moment 0 map shows the beam FWHM. For the moment 1 maps, the cube is masked at a threshold of 1.6 mJy beam−1 (approximately the WALLABY noise rms) and we use the CosmosCanvas (J. English et al. 2024) color map. The galaxy is composed of  ~1600 collisional particles and has an H I mass of  ~1.8 × 1010 M⊙.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Same as Figure 1, but for a noiseless, WALLABY-like mock of Galaxy 1531. The galaxy is composed of  ~1100 collisional particles and has an H I mass of  ~1.5 × 109 M⊙.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: SLICERASTRO view of noiseless mocks of the H I cube of Galaxy 467 presented in Figure 1 for the particle SPH (top), scanline SPH (middle), and scanline MFM (bottom). The E–N–Z axes show the R.A.–decl.–velocity axes, respectively, with +Z indicating the approaching velocity. The values of A3D for each mock, computed around the minimum of the potential, are given in the top left corner of each panel.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Comparison of 1D and 2D asymmetries of noiseless, WALLABY-like, Scanline MFM mocks of SIMBA galaxies. The dashed black line shows the 1:1 relation. The points are colored by H I mass, which correlates to resolution by virtue of the size–mass relation (J. Wang et al. 2016).
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Same as in Figure 3, but for Galaxy 153 presented in Figure 2.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Plot of the difference of 3D asymmetry between the Particle SPH and MFM Scanline Tracing realizations of SIMBA mock cubes described in Section 2.2 as a function of the cube H I mass.
Paper: WALLABY Pilot Survey and ASymba: Comparing H I Detection Asymmetries to the SIMBA Simulation
Authors: Mathieu Perron-Cormier, Nathan Deg, Kristine Spekkens, Mark L. A. Richardson, Marcin Glowacki, Kyle A. Oman, Marc A. W. Verheijen, Nadine A. N. Hank, Sarah Blyth, Helga Dénes, Jonghwan Rhee, Ahmed Elagali, Austin Xiaofan Shen, Wasim Raja, Karen Lee-Waddell, Luca Cortese, Barbara Catinella, Tobias Westmeier
Figure caption: Same as in Figure 6, except for the combination of 1D and 2D asymmetries plotted against 3D asymmetry. Ten H I sources fall outside the 0, 1 range for the combined A1D + A2D.
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: The results of the precisions derived via a conventional weighted fourth-order polynomial in blue and the refined approach in red, respectively. The modes are shown as colored numbers. The bin size is 0.3 mas. Note that, the residuals in R.A. direction have multiplied with cos(decl.).
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: Diagram of the refined approach procedure.
Paper: A Candidate High-velocity Exoplanet System in the Galactic Bulge
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Aparna Bhattacharya, Jon Hulberg, Macy J. Huston, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Jessica R. Lu, Clément Ranc, Natalia E. Rektsini, Aikaterini Vandorou
Figure caption: Left: a zoom-in view of the stacked K-band image of MB11262, with the brighter source star near center and the faint lens star candidate indicated with the crosshair. Middle: zoomed-in frame with a single-PSF model fit to the source star and subtracted from the frame; the remaining flux comes primarily from the lens and is indicated with the crosshair. The other bright nearby stars are also subtracted with the same PSF model. Right: zoomed-in frame with the PSF model fit and subtracted from the source and lens stars. North is up, east is left in all frames. Note there are several faint ambient field stars that are at or below the default detection threshold in DAOPHOT.
Paper: A Candidate High-velocity Exoplanet System in the Galactic Bulge
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Aparna Bhattacharya, Jon Hulberg, Macy J. Huston, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Jessica R. Lu, Clément Ranc, Natalia E. Rektsini, Aikaterini Vandorou
Figure caption: Confirmed planetary systems with measured transverse velocities from the NASA Exoplanet Archive (accessed 2024 June 25). MB11262L (in red with error bars) is the highest-velocity planetary system and the most distant planetary system with a measured transverse velocity. For reference, the previous highest-velocity system (BD+20 2457; A. Niedzielski et al. 2009), lowest-velocity system (Kepler-1166; T. D. Morton et al. 2016), and TRAPPIST-1 (M. Gillon et al. 2016) are labeled.