adsabs/AstroCLIMB huggingface dataset:
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Overlay of all 152 individual HPF exposures of HAT-P-67, spanning 2020–2022. Variability is seen in the He I 10833 Å triplet near the vertical orange shaded band but not in the adjacent Si line. These snapshot spectra were barycentric corrected and continuum flattened with a linear fit to the regions in the blue vertical bands. Sharp telluric absorption lines have been masked in regions near 10835 and 10837.5 Å.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Equivalent width lightcurve of helium absorption in HAT-P-67b. The system exhibits a characteristic absorption leading up to transit, followed by a sharp decline after transit passage. The EWs were computed in the orange shaded band (10832.3−10834.2 Å) in Figure 7.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Overview of all available TESS Sectors showing 24 full or partial transits with 34 visits with HPF (vertical gray bars), 7 of which coincide with transits. The rest of the visits sample out-of-transit phases. The 8 HPF visits between days 2050 and 2690 are not shown. It is worth noting the large time breaks between some consecutive panels, which correspond roughly to the duration of a TESS sector.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Mass–radius trends for inflated hot sub-Saturns and hot Jupiters, with layout following Figure 2 of Thorngren & Fortney (2018) and updated with NASA Exoplanet Archive confirmed planets. The trend lines show the mass–radius relationship for equilibrium temperatures of 500, 1000, 1250, 1500, and 2000 K, assuming the mean composition and mean heating efficiency from the original figure. HAT-P-67 b (⋆ symbol) stands alone in a region defined by the lack of inflated sub-Saturns and explained by short lifetimes from runaway inflation and mass loss.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: RV orbit fit including both HPF and Keck HIRES data points. The RV information content in HPF is much less than in Keck HIRES for this F5 spectral type, and so the joint fit constrains the mass to roughly a Saturn mass.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: MIST evolutionary model tracks for HAT-P-67. The T eff and luminosity of HAT-P-67 (gray circle) are consistent with either the late main sequence or a recently evolved subgiant. The labeled numbers indicate age in Gyr.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Four observing campaigns centered on an in-transit epoch with before-and-after visits typically separated by one night. The after-transit spectra tend to show negligible absorption. Line-of-sight velocity substructure can be seen in the epochs before and during transit.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Best-fit orbit overlaid on the composite TESS lightcurve. Revised planet properties are consistent with Zhou et al. (2017), with a systematic shift from a revised Gaia DR3 distance.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Overview of exoplanet demographics. The pixel bins reflect the observed density of over 5000 planets accessed from the NASA Exoplanet Archive. Detections of atmospheric escape are common among large planets with strong insolation. HAT-P-67 b is among the most inflated planets known.
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: The Hα contamination fraction as a function of veto band 5σ depth for a Lyα Roman grism survey spanning a redshift range of z Lyα  = 7.25–8.75. Our CUBGRISM reduction produces a line-flux-limited sample, and we show three contamination curves that encompass the average survey flux limits, f line, listed in Table 1 in units of erg s−1 cm−2. As the veto band depth increases, we can efficiently distinguish between high-redshift LAEs, which have a strong spectral break at λ obs ∼ 1 μm, and foreground Hα emitters, which even at the highest observed EWs will have detectable continuum flux. The red vertical line shows the expected Roman r-band 5σ depth in 128 s, demonstrating Roman's ability to efficiently obtain deep wide-field veto band imaging.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption: Integrated intensity distribution of the original 12CO(3 − 2) cube and the reconstructed cube. (a), (b) and (c) Integrated intensity distribution of the full reconstructed cube, reconstructed blue cloud, and reconstructed red cloud, respectively. (d), (e) and (f) Integrated intensity map of original 12CO(3 − 2) cube over velocity ranges corresponding to W5-NW complex, W5-NWa and W5-NWb, respectively. The velocity ranges used to obtain the maps are mentioned in the top left of panels (d)–(f). Panels (e) and (f) are the same as Figures 2 (a) and (c). Pixels where Gaussian fitting is not possible are not considered in the analysis and are excluded from this plot.
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: A 20″ × 20″ region of our simulated Roman direct image and three selected wavelength slices from our data cube constructed from 25 Roman grism images. From left to right, we show the Roman direct image, a 1.155 μm data-cube slice containing one simulated z = 8.5 LAE, a 1.277 μm data-cube slice containing two simulated z = 9.5 LAEs, and a 1.398 μm data-cube slice containing two simulated z = 10.5 LAEs. The simulated LAEs are circled in red. The number associated with each LAE indicates the line flux of the source, where the Lyα flux is in units of 10−17 erg s−1 cm−2. By design continuum sources are not recovered in our data cube due to our background-subtraction procedure (see Section 3 for details).
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: We show a small 40″ × 40″ region of our simulated ﹩{t}_{\exp }=10﹩ ks grism image before and after continuum subtraction. We have highlighted a foreground emission-line galaxy (blue circle) and an artifact caused by the 0–0 order of a bright star (underlined in blue). See Section 3.1 for additional discussion of our continuum-subtraction method. We demonstrate that our emission-line search technique, CUBGRISM, can effectively remove contamination from 0–0 spectra and recover a clean sample of emission-line sources.
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: Left: observed HST F160W image. Middle: our simulated F160W image. Right: our simulated Roman grism image with a position angle (PA) aligned with the x-axis. For our deep-field simulations, we consider up to 25 independent PAs and up to 69.4 hr of total integration time. We use a noise level of 0.8 e− pix−1 s−1, which is the expected near-infrared background for the High Latitude Survey.
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: Roman WFI grism response functions for the in-focus spectral orders. For display purposes, we increased the 2–2 and 0–0 grism response functions by a factor of 10. All three in-focus spectral orders are included in our grism simulations.
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: Construction of the noiseless simulated grism images. All the in-focus spectral orders 0–0, 1–1, and 2–2 are simulated independently and then coadded to form our combined grism image. Finally, we add in the Poisson noise appropriate to our desired exposure time (see Figure 4). For the four panels above, we show a ﹩3\buildrel{\,\prime}\over{.} 75\times 3\buildrel{\,\prime}\over{.} 75﹩ FOV.
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: Four examples of modeled Lyα spectra, illustrating some of the redshifts, f Lyα  line fluxes (×10−18 erg s−1 cm−2), and continuum levels that we sample.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: (V − I, I) Color–magnitude diagram of stars in the OGLE-I I I catalog (Szymański et al. 2011) and the Hubble Space Telescope catalog (Holtzman et al. 1998). The black dots are the OGLE-I I I catalog stars located within 2′ of the event OGLE-2014-BLG-0221, and the green dots are the Hubble Space Telescope catalog stars in a field of Baade’s window, whose colors and magnitudes are shifted to match the red clump giant centroid of the OGLE-I I I catalog. The red spot indicates the position of the red clump giant centroid, and the orange, blue, purple, cyan, and magenta spots are source positions of Model-A, Model-B P ±, and Model-B P+LOM ±, respectively.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Posterior probability density distributions of Model-A. The distributions are classified into main-sequence stars, WDs, neutron stars, and BHs and are separated by colors accordingly. In the last plot, the lens brightness of the main-sequence samples is shown, where the vertical blue line is the median value and the cyan and purple regions represent 68.3% and 95.4% credible intervals of the distribution. The apparent source brightness is also plotted by the median magenta line with the magenta dashed line indicating the 68.3% interval.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Model light curves of the two degenerate models around the anomaly. Model-A, Model-A P±, Model-B, Model-B P±, and Model-B P+LOM± are plotted. As different sources and blending fluxes between Model-A and Model-B make different magnifications, the magnification of Model-B is scaled by the source and blending fluxes of Model-A for comparison. The lower residual panel shows the data points binned in 1 day intervals.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Light curve of OGLE-2014-BLG-0221. The black, red, and light-blue data points are the reduced photometric data from the MOA-Red and OGLE I- and V-band observations, respectively. The blue and green lines represent the best-fit binary-lens single-source model and best-fit single-lens single-source model. The lower panel shows the residuals from the best-fit binary-lens model. (The data used to create this figure are available.)
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Probability density functions of the normalized angular source radius ρ from our MCMC chains for (a) Model-A, (b) Model-B P+, and (c) Model-B P+LOM+. The bimodal distribution of each model except Model-B P+LOM+ is approximated by the Gaussian mixture model, and the two components of the best fit are plotted in orange and green lines.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Caustic geometry corresponding to Model-B for versions with nonparallax, parallax (P±), and parallax plus lens orbital motion (P+LOM±). The caustics at ﹩\mathrm{HJD}^{\prime} =6728.6﹩, 6738, 6746, and 6760 are plotted for P+LOM± with the instantaneous source positions in the red open circles whose sizes are not in scale.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Posterior distribution sampled by the MCMC sampler. Colors represent Δχ 2 from the lowest χ 2 parallax plus LOM model.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Caustic geometry corresponding to Model-A for versions with nonparallax and parallax (P±). The caustic is shown in the red curved line. The blue line is the source trajectory.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Current source–lens relative position. The distributions of Model-A P±, Model-B P±, and Model-B P+LOM± are plotted. The contour from dark to light shows 39.3, 86.5, and 98.9% of the highest-density regions.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Same as Figure 8 for Model-B P+LOM+. The plot of the lens brightness is not shown as no main-sequence sample has been generated in the simulation.
Paper: OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Authors: Rintaro Kirikawa, Takahiro Sumi, David P. Bennett, Daisuke Suzuki, Naoki Koshimoto, Shota Miyazaki, Ian A. Bond, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Yutaka Matsubara, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki K. Satoh, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Przemek Mróz, Radosław Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Mateusz J. Mróz
Figure caption: Same as Figure 8 for Model-B P+.