adsabs/AstroCLIMB huggingface dataset:
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Example subsection of the December light curve from 2022 December 9, which we reported back to UCSN observers. This represents data from four citizen astronomer observers from one of four days during the 2022 December campaign. Colored points are fluxes measured from images totaling 2 minutes of integration each. Blue squares are weighted averages of 50 individual flux points. The dashed line is the predicted depth of TIC 139270665 b’s transit. This light curve was chosen to present here as it had the most observers and data for the 4 day December campaign. We note the photometric stability and precision, which allows sensitivity to <1% transit depths and improved where we had overlapping data sets from multiple telescopes. The other individual December light curves were similarly flat, with no transit detection, or there was not enough coverage or data to make substantial conclusions.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Maximum-likelihood model from the MCMC plotted over the UCSN light curve on UTC 2022 December 9. The UCSN data in the light exhibit relatively large scatter compared to the expected transit depth, likely due to a combination of variable atmospheric conditions, systematic instrumental noise, and the inherent complexities of ground-based observations. Thus, drawing definitive conclusions from these data is challenging. The blue squares in the plot represent the weighted averages of fluxes and residuals, respectively, within each time bin of 0.01 days. On average, each blue square is derived from approximately six individual data points.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: MCMC walker trace plot for the period (in days) after trimming the initial 3250 steps (iterations) as burn-in. The bottom group of walkers, clustered between P = 23.620 days and P = 23.621 days, was investigated as a possible second set of solutions.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Normalized and phase-folded light curve from seven of our Unistellar citizen scientist data sets with the MCMC maximum-likelihood model fit (top) and residuals from the best-fit model (bottom). Unistellar data are labeled with observation date and abbreviated serial number, e.g., “YYYYMMDD_abc,” where “abc” represents serial number. The max-likelihood period value was P = 23.627 days. The blue squares represent the weighted means of the individual relative fluxes within each phase bin. On average, each blue square represents about 28.3 data points.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: APF RVs of TIC 139270665. The top panel is the entire time series, while the bottom two panels are planet b's and c’s Keplerian signals separated and phase-folded on the best-fit T  C  values.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Transit light curve for the second night of our February campaign on 2023 February 17 shared with UCSN. The red line is the fitted transit model to the data. A model was fitted to this data because the moving average dropped below the expected transit depth threshold. This represents close to 19 hr of continuous data. The 1 hr integrations show an achieved precision better than 0.1%, and the standard deviation of the fluxes from 2 minutes integrations is only 0.67%. Our light-curve model-fitting routine identified an egress at the beginning of the sequence, which we subsequently rejected as unreliable. The original prediction times are based on our best estimate of the orbital period at the time of observation.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Mass vs. radius for confirmed exoplanets including TIC 139270665 b. TOIs noted in the legend represent other dense warm sub-Saturns. Solar system planets (magenta outline) have P ≫ 100 days. This demonstrates TIC 139270665 b’s discovery and high density to be a valuable addition to our taxonomy of planets to help us further understand the evolutionary history of such bodies. 1σ error bars for TIC 139270665 b are displayed in black.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Maximum-likelihood model from the MCMC plotted over the UCSN light curve on UTC 2023 February 18. Due to data gaps at critical transit stages, transit detection remains uncertain, though there is a possible ingress signal. The blue squares in the plot represent the weighted averages of fluxes and residuals, respectively, within each time bin of 0.01 days. On average, each blue square is derived from approximately 14.6 individual data points.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Transit light curve for 2023 April 5 from our April campaign, shared with UCSN. The red line the fitted transit model to the data. A model was fitted to this data because the moving average dropped below the expected transit depth threshold. Although an ingress-like feature is seen here, we do not declare transit detection as we were unable to confirm this with a follow-up detection later in the month.
Paper: Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
Authors: Lauren I. Biddle, Brendan P. Bowler, Yifan Zhou, Kyle Franson, Zhoujian Zhang
Figure caption: Left: the PSF-subtracted image of AB Aur produced with optimized pyKLIP processing parameters (Section 3.1). Right: the S/N map of the PSF-subtracted image where the S/N of each pixel is computed as the flux divided by the standard deviation of the background in a narrow annulus at that pixel’s separation. The inset frame in the upper right portion of both panels provides an enlarged perspective of the region outlined by the white box at the expected location of the companion. Within the inset views, the white “×” indicates the most recent location reported by Currie et al. (2022; sep = 0.″60, PA = 184.°2), and the black “+” gives the location reported by Zhou et al. (2022; sep = 0.″60, PA = 182.°5). The S/N within an aperture radius of 3 × FWHM at the position of the white “×” is 1.4, and the S/N at the position of the black “+” is 0.8, both of which are below our threshold of 5σ that we use to establish a reliable detection.
Paper: Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
Authors: Lauren I. Biddle, Brendan P. Bowler, Yifan Zhou, Kyle Franson, Zhoujian Zhang
Figure caption: Upper panel: a mapping of the location of emission lines in the NIR IRTF spectrum of AB Aur A. Lower left: the entire flux-calibrated IRTF/SpeX SXD spectrum of AB Aur A (Section 2.2). The spectral ranges ≈1.3–1.5 μm and ≈1.7–1.9 μm fall in telluric regions and have reduced signal to noise. The gray dotted box indicates the spectral region containing the Paβ line and the NIRC2 filter bandpasses utilized in this work. Lower right: a zoomed-in perspective of the region within the dotted box in the left panel. The light-green emission component of the Paβ line indicates the region that was masked during our calculation of the host star’s synthetic J cont magnitude (J cont,syn). The transmission profiles of the relevant NIRC2 filters are displayed below (J filter is shown in teal, the J cont filter is shown in blue, and the Paβ filter is shown in red). The vertical dashed line traces Paβ emission line location.
Paper: Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
Authors: Lauren I. Biddle, Brendan P. Bowler, Yifan Zhou, Kyle Franson, Zhoujian Zhang
Figure caption: Left six panels: normalized quality maps based on injection-recovery tests for the movement and annuli parameters of the KLIP processing using 20 principle components. From the upper left to lower right, the metrics presented are: mean S/N, maximum S/N, average contrast, mean S/N nearest neighbor, max S/N nearest neighbor, and false-positive fraction. See Section 3.1 for details. Individual maps are normalized and colored according to the respective quality rating (0 = worst quality, 1 = best quality). These quality metric maps are used to compute the aggregate quality map from which the optimal parameter combinations are chosen. Right panel: the aggregate quality map constructed from the equally weighted summation of all 6 quality metric maps. The cell with the highest rating from the aggregate map is outlined in black in every panel. Cells containing no quality rating have a combination of movement and annuli parameters that leave no reference images for PSF subtraction as a result of the aggressiveness of the rotational mask.
Paper: Deep Paβ Imaging of the Candidate Accreting Protoplanet AB Aur b
Authors: Lauren I. Biddle, Brendan P. Bowler, Yifan Zhou, Kyle Franson, Zhoujian Zhang
Figure caption: The 5σ contrast curve of the PSF-subtracted image of AB Aur in the NIRC2 narrowband Paβ filter computed for an unresolved source (pink) and a resolved source (maroon). Although the expected ΔJ contrast is ≈9.2 (Currie et al. 2022), the relative Paβ emission line strength between the accreting host star and the candidate companion will impact the contrast of the companion in the Paβ filter.
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: Limits on putative host stars. Assuming that the analyzed objects are wide-orbit planets, the 2D histograms present the expected H-band brightness and lens-source separation of putative host stars during Keck observations. The black solid and dashed lines present the sensitivity of our observations (corresponding to ﹩{\rm{\Delta }}{\chi }_{\mathrm{thresh}}^{2}=250﹩ and ﹩{\rm{\Delta }}{\chi }_{\mathrm{thresh}}^{2}=500﹩, respectively). The black points mark the detected stars.
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: Images for BLG512.18.22725. Upper panels: 30″ × 30″ OGLE I-band image (left-hand), 30″ × 30″ Keck NIRC2 wide camera H-band image (middle), and 5″ × 5″ Keck NIRC2 narrow-camera H-band image (right-hand). Lower panels present a 1″ × 1″ zoom on the narrow-camera image. The lower middle panel presents the residuals after subtracting the microlensing source star, whereas the lower right-hand panel presents the residuals after subtracting all detected stars. The scale bar shows the flux renormalized to the peak of the target.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: Summary of injection-recovery tests for TiO. The horizontal red dashed line indicates S/N = 5. The three vertical lines represent the VMR of TiO at 1 bar from the equilibrium chemical calculations for different metallicities. We assume that 1 bar is the quenching point, and the VMR of TiO is constant above this point. The y-axis indicates the S/N at the expected values in the K  p  map.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: Cross-correlation functions of the remaining searched species (Fe II, Ca I, Mg I, Cr I, Y I, VO, AlO, and FeH).
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: The host mass–distance relations for a putative main-sequence host star of different apparent magnitude for the event OGLE-2015-BLG-1044.
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: Same as Figure A1, but for event OGLE-2015-BLG-1044.
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: Same as Figure A1, but for event OGLE-2012-BLG-1073.
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: Same as Figure A1, but for event OGLE-2012-BLG-1396.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: SED fits of eight example RSGs, the first, second, and third row show the good SED fits for optically thin, C-rich, and O-rich stars, respectively (sflag = 0). The bottom row shows anomalous SED fits of two example stars, due to bad W3/W4 observation (left, sflag = 3), and binarity (right, sflag = 2)).
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: The result of direct fitting without restriction at long wavelengths (blue dotted–dashed line) and the result of refitting after the restriction (black solid line) for an example RSG in the S1 sample. The observations are marked with different symbols of different colors. The black solid curves are the best-fitted models. The black dashed and dotted–dashed lines are the spectra contributed by the center star and the circumstellar dust, respectively. The blue dashed line represents the minimum χ 2 model of another chemical component.