adsabs/AstroCLIMB huggingface dataset:
Paper: OASIS Survey Direct Imaging and Astrometric Discovery of HIP 71618 B: A Substellar Companion Suitable for the Roman Coronagraph Technology Demonstration 
Authors: Mona El Morsy, Thayne Currie, Brianna Lacy, Taylor L. Tobin, Qier An, Yiting Li, Ziying Gu, Masayuki Kuzuhara, Danielle Bovie, Dillon Peng, Jeffrey Chilcote, Olivier Guyon, Miles Lucas, Timothy D. Brandt, Robert de Rosa, Tyler D. Groff, Markus Janson, N. J. Kasdin, Julien Lozi, Christian Marois, Bertrand Mennesson, Naoshi Murakami, Eric Nielsen, Sabina Sagynbayeva, Nour Skaf, William Thompson, Motohide Tamura, Taichi Uyama, Alice Zurlo, Vincent Deo, Sebastien Vievard
Figure caption: The Gaia color–magnitude diagram for the Pleiades (gray) and Hyades (dark red) compared to PARSEC isochrones for 112 Myr and 750 Myr, young stars with interferometrically measured ages ≲150 Myr, stars in the 400 Myr old Ursa Majoris moving group, and other young stars with imaged substellar companions (J. Jones et al. 2015, 2016; J. W. Jones 2016; T. Currie et al. 2023b; T. L. Tobin et al. 2024).
Paper: OASIS Survey Direct Imaging and Astrometric Discovery of HIP 71618 B: A Substellar Companion Suitable for the Roman Coronagraph Technology Demonstration 
Authors: Mona El Morsy, Thayne Currie, Brianna Lacy, Taylor L. Tobin, Qier An, Yiting Li, Ziying Gu, Masayuki Kuzuhara, Danielle Bovie, Dillon Peng, Jeffrey Chilcote, Olivier Guyon, Miles Lucas, Timothy D. Brandt, Robert de Rosa, Tyler D. Groff, Markus Janson, N. J. Kasdin, Julien Lozi, Christian Marois, Bertrand Mennesson, Naoshi Murakami, Eric Nielsen, Sabina Sagynbayeva, Nour Skaf, William Thompson, Motohide Tamura, Taichi Uyama, Alice Zurlo, Vincent Deo, Sebastien Vievard
Figure caption: Top: predicted contrast for HIP 71618 B in the coronagraph’s passbands for different atmosphere models from the updated B. Lacy & A. Burrows (2020) grid distribution. Bottom: predicted contrasts for HIP 71618 B drawn from flux-normalized optical spectra from the young low-gravity spectral standards presented in K. L. Luhman et al. (2017) and K. L. Luhman (2023, 2024). The black data points show contrasts for HD 1160 B—a substellar companion with NIR colors, mass, and age similar to HIP 71618 B—if it orbited HIP 71618.
Paper: OASIS Survey Direct Imaging and Astrometric Discovery of HIP 71618 B: A Substellar Companion Suitable for the Roman Coronagraph Technology Demonstration 
Authors: Mona El Morsy, Thayne Currie, Brianna Lacy, Taylor L. Tobin, Qier An, Yiting Li, Ziying Gu, Masayuki Kuzuhara, Danielle Bovie, Dillon Peng, Jeffrey Chilcote, Olivier Guyon, Miles Lucas, Timothy D. Brandt, Robert de Rosa, Tyler D. Groff, Markus Janson, N. J. Kasdin, Julien Lozi, Christian Marois, Bertrand Mennesson, Naoshi Murakami, Eric Nielsen, Sabina Sagynbayeva, Nour Skaf, William Thompson, Motohide Tamura, Taichi Uyama, Alice Zurlo, Vincent Deo, Sebastien Vievard
Figure caption: Corner plot showing posterior distributions of selected orbital parameters from jointly modeling direct imaging and astrometric data assuming a Gaussian companion mass prior centered on 65 MJup. The contour lines delineate the regions encompassing 68%, 95%, and 99% of the posteriors. The corner plot for the simulation adopting a flat-companion-mass prior is very similar, except that its long tail of higher-mass solutions results in a slightly larger range of masses within the 68% confidence interval.
Paper: OASIS Survey Direct Imaging and Astrometric Discovery of HIP 71618 B: A Substellar Companion Suitable for the Roman Coronagraph Technology Demonstration 
Authors: Mona El Morsy, Thayne Currie, Brianna Lacy, Taylor L. Tobin, Qier An, Yiting Li, Ziying Gu, Masayuki Kuzuhara, Danielle Bovie, Dillon Peng, Jeffrey Chilcote, Olivier Guyon, Miles Lucas, Timothy D. Brandt, Robert de Rosa, Tyler D. Groff, Markus Janson, N. J. Kasdin, Julien Lozi, Christian Marois, Bertrand Mennesson, Naoshi Murakami, Eric Nielsen, Sabina Sagynbayeva, Nour Skaf, William Thompson, Motohide Tamura, Taichi Uyama, Alice Zurlo, Vincent Deo, Sebastien Vievard
Figure caption: Top: HIP 71818 b data compared to the best-fit model from the BT-Settl grids in the NIR spectrum and NIRC2 data point. Bottom: contour plot showing the confidence intervals for the BT-Settl model grid. The red star indicates the best fit.
Paper: OASIS Survey Direct Imaging and Astrometric Discovery of HIP 71618 B: A Substellar Companion Suitable for the Roman Coronagraph Technology Demonstration 
Authors: Mona El Morsy, Thayne Currie, Brianna Lacy, Taylor L. Tobin, Qier An, Yiting Li, Ziying Gu, Masayuki Kuzuhara, Danielle Bovie, Dillon Peng, Jeffrey Chilcote, Olivier Guyon, Miles Lucas, Timothy D. Brandt, Robert de Rosa, Tyler D. Groff, Markus Janson, N. J. Kasdin, Julien Lozi, Christian Marois, Bertrand Mennesson, Naoshi Murakami, Eric Nielsen, Sabina Sagynbayeva, Nour Skaf, William Thompson, Motohide Tamura, Taichi Uyama, Alice Zurlo, Vincent Deo, Sebastien Vievard
Figure caption: Wavelength-collapsed images of HIP 71618 B with SCExAO/CHARIS in broadband NIR light (1.15–2.37 μm) and with Keck/NIRC2 in the Lp filter (3.78 μm). The white arrow denotes the position of HIP 71618 B in each panel.
Paper: A XRISM View of Relativistic Reflection in Cygnus X-1
Authors: Paul A. Draghis, Jon M. Miller, Erin Kara, Elisa Costantini, Oluwashina Adegoke, Javier A. García
Figure caption: Ratio of spectra from the first half of the XRISM observation of Cygnus X-1 to a power-law model (black line), showing the shape of the relativistically broadened Fe line. The red line in both panels shows the best-fit model, obtained with a BH spin of a = 0.975 and an inclination of θ = 62∘. The different colored dashed lines represent the models with different BH spins (left) and different viewing inclinations (right), when the other parameter is held at the best-fit value. The models were shifted to match the flux at the peak of the line, around 7 keV, and do not represent the results of spectral fits. Lower BH spins underpredict the red wing of the Fe line in the left panel, whereas higher spins overpredict both the blue and red wings of the line. Similarly, different inclinations (right panel) fail to capture the profile of the line.
Paper: A XRISM View of Relativistic Reflection in Cygnus X-1
Authors: Paul A. Draghis, Jon M. Miller, Erin Kara, Elisa Costantini, Oluwashina Adegoke, Javier A. García
Figure caption: Complete corner plot obtained based on the MCMC runs on the fits to the two halves of the XRISM Resolve observation of Cygnus X-1. The red contours indicate the measurements obtained from the first half of the observation, while the blue contours indicate the measurements obtained from the second half.
Paper: Evolution of the ZTF SLRN-2020 Star-Planet Merger
Authors: Ricardo Yarza, Morgan MacLeod, Benjamin Idini, Ruth Murray-Clay, Enrico Ramirez-Ruiz
Figure caption: Tidal evolution tracks for a Sun-like star with a 10MJ companion. The abscissa shows the ratio of the orbital decay time to the thermal time at the location of energy deposition (see Equations (15) and (16)); the ratio must be greater than unity for the deposited energy to be observable before the merger. The ordinate shows the ratio of the tidal luminosity to the intrinsic stellar luminosity (see Equation (8)); the ratio must be greater than unity for the tidal energy deposition to be significant. Each line corresponds to a different tidal quality factor. The squares mark the −12 yr epoch at which the archival images of the progenitor were taken. When computing the thermal time, we assume that energy is deposited in the outermost 2 × 10−2M⊙ of the star. None of these tidal quality factors yield observable tidal heating before the merger (upper right region of the figure), suggesting that the archival image was unaffected by the star-planet interaction.
Paper: Characterization of the Host Binary of the Directly Imaged Exoplanet HD 143811 AB b
Authors: Anne E. Peck, William Roberson, Eric L. Nielsen, Robert J. De Rosa, Nathalie Jones, Jason Wang, Bruce A. Macintosh, Briley L. Lewis, Gaspard Duchêne, Stanimir Metchev, Asif Abbas, Jerry W. Xuan, Aniket Sanghi, Jennifer Patience, Travis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Hannah Gallamore, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: We are generally able to accurately recover effective temperature and metallicity when applying our method to well-characterized F and G stars from C. C. Worley et al. (2012). However, the results for stars hotter than ≳6000 K show a systematic offset in temperature and a larger scatter in metallicity compared to G stars. The solid black line is the 1–1 line, representing identical results.
Paper: Characterization of the Host Binary of the Directly Imaged Exoplanet HD 143811 AB b
Authors: Anne E. Peck, William Roberson, Eric L. Nielsen, Robert J. De Rosa, Nathalie Jones, Jason Wang, Bruce A. Macintosh, Briley L. Lewis, Gaspard Duchêne, Stanimir Metchev, Asif Abbas, Jerry W. Xuan, Aniket Sanghi, Jennifer Patience, Travis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Hannah Gallamore, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: The results of a two-star fit to the unresolved optical and near-infrared photometry of the system from Gaia and 2MASS. Plotted are the SED of the blended system (black) and the two components (blue, yellow) drawn from the posterior distributions estimated using MCMC. Also shown are the synthetic photometry of the blended system derived from the median SED (black squares) and the observed photometry (circles).
Paper: Characterization of the Host Binary of the Directly Imaged Exoplanet HD 143811 AB b
Authors: Anne E. Peck, William Roberson, Eric L. Nielsen, Robert J. De Rosa, Nathalie Jones, Jason Wang, Bruce A. Macintosh, Briley L. Lewis, Gaspard Duchêne, Stanimir Metchev, Asif Abbas, Jerry W. Xuan, Aniket Sanghi, Jennifer Patience, Travis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Hannah Gallamore, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: A single-wavelength region used for the spectral fitting for the first 12 epochs. Black points with error bars are the data. Red tracks are random draws from the posterior for the two-star model fit. Blue and yellow tracks are random draws from the posterior for single-star models for the primary and secondary, respectively. Our method finds reliable RVs for both epochs with widely separated lines and epochs with blended lines.
Paper: Characterization of the Host Binary of the Directly Imaged Exoplanet HD 143811 AB b
Authors: Anne E. Peck, William Roberson, Eric L. Nielsen, Robert J. De Rosa, Nathalie Jones, Jason Wang, Bruce A. Macintosh, Briley L. Lewis, Gaspard Duchêne, Stanimir Metchev, Asif Abbas, Jerry W. Xuan, Aniket Sanghi, Jennifer Patience, Travis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Hannah Gallamore, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: The posterior distribution for the two-star fit to the unresolved photometric measurements, giving the six fitted parameters and their covariances. The effective temperature, a derived parameter, of both components is also shown.
Paper: Characterization of the Host Binary of the Directly Imaged Exoplanet HD 143811 AB b
Authors: Anne E. Peck, William Roberson, Eric L. Nielsen, Robert J. De Rosa, Nathalie Jones, Jason Wang, Bruce A. Macintosh, Briley L. Lewis, Gaspard Duchêne, Stanimir Metchev, Asif Abbas, Jerry W. Xuan, Aniket Sanghi, Jennifer Patience, Travis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Hannah Gallamore, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: Continued from Figure 7. A single-wavelength region used for the spectral fitting for the last 10 epochs. Black points with error bars are the data.
Paper: Characterization of the Host Binary of the Directly Imaged Exoplanet HD 143811 AB b
Authors: Anne E. Peck, William Roberson, Eric L. Nielsen, Robert J. De Rosa, Nathalie Jones, Jason Wang, Bruce A. Macintosh, Briley L. Lewis, Gaspard Duchêne, Stanimir Metchev, Asif Abbas, Jerry W. Xuan, Aniket Sanghi, Jennifer Patience, Travis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Hannah Gallamore, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: The posterior distribution for the binary fit to the 2018 April 18 FEROS spectrum, fitting for stellar parameters and RVs of both components of the binary.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Overview of the absorption cross sections for HCs, DMS, and DMDS, taken from PNNL (S. W. Sharpe et al. 2004) and included in HITRAN2024 database (R. J. Hargreaves et al. 2026, in preparation). Each measurement is at 25∘C, 1.0 atm, and has been convolved to a 1.0 cm−1 resolution. The y-axis provides the logarithm of intensity, and each molecule has been offset for display purposes. A minimum intensity of 1.0 × 10−21 cm2 molecule−1 has been applied for each molecule for the purpose of visual clarity. The full spectral range of the underlying PNNL data is presented, showing the degeneracy below 5 μm (also shown in Figure 3). This degeneracy is partially lifted above 5 μm, in the mid- to far-IR, due to the differences in the low-frequency vibrational modes of the C–C and C–H bonds.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Spectra of different molecules may have many similarities, partially due to the presence of spectrally active shared functional groups (C. Sousa-Silva et al. 2019; Z. Zhan et al. 2021). Overview of the absorption cross sections for HCs at 25∘C and 1.0 atm taken from PNNL (S. W. Sharpe et al. 2004) and included in the cross-sections part of the HITRAN2024 database (R. J. Hargreaves et al. 2026, in preparation). The y-axis provides the logarithm of intensity, with each absorption cross section offset for display purposes. A minimum intensity of 1.0 × 10−21 cm2 molecule−1 has been applied for each molecule.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Atmospheric inferences are sensitive to the molecules retrieved for. Posterior distribution of the base atmospheric parameters for an ensemble of 25 “sets,” associated with different selections of molecules retrieved (see Table 3). The “truths” reported in Table 2 are shown in the black dotted lines. Except for acetylene and carbon dioxide, the retrieved molecular values are generally consistent within 2σ of previously reported values. Given the precision of the data, some extreme cases are highly unlikely. This is in particular the case for sets 3, 4, 5, and 6, which do not select a molecule with a sharp absorption feature at the center of the 3.3 μm band, forcing large compensations on the abundance of methane and other parameters while still leading exceedingly large structures (∼50 km versus ∼5 km otherwise) in the residuals (see Figure 6). All other models lead to consistent fits and reveal a scatter of ∼0.5 dex among the mean retrieved abundances for absorbers such as methane.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Not all choices of molecule sets yield equally good fits. Fits of four different combinations of models with the corresponding residuals (left) and posterior distribution of methane’s mixing ratio (right). Colors indicate the sets of molecules used for each retrieval (see Table 3). Sets of molecules without ethane and/or propane lead to substantially worse fits. All other sets lead to comparable fits, yet a range of methane mixing ratios spreading over 0.5–0.75 dex is associated with such preretrieval selections.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Background gas identification via constraints on the scale height from transmission spectroscopy. Left: posterior probability distribution of Titan’s atmospheric scale height yielded by its transmission spectrum (consistent with the stratospheric value). Right: framework to yield robust abundances for terrestrial planets using iterative retrievals through identification of background gas.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Weak absorption features muted during hazy epochs. Left: Titan’s transmission spectrum corresponding to two different visits (T10 and T53, see Table 1). T53 is affected by hazes to such an extent that weak absorption features such as CO2 at 4.3 μm are mostly muted. Right: retrieved CO2 mixing ratios for T10 and T53 showing that in the latter case, the detection of CO2 is less significant due to hazes muting its 4.3 μm band.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Corner plot showing correlation among different parameters for visit T10 for combination set of 7. A number of parameters, including retrieved abundance of methane and retrieved abundance of propane, show a strong correlation.
Paper: The Detection-versus-retrieval Challenge: Titan as an Exoplanet
Authors: Prajwal Niraula, Julien de Wit, Robert J. Hargreaves, Iouli E. Gordon, Clara Sousa-Silva
Figure caption: Posterior distribution of different molecules observed for Titan in our retrievals for molecular set 17. The “truths” reported in Table 2 are shown in the black lines. Except for acetylene and carbon dioxide, the retrieved molecular values are generally consistent within 2σ of previously reported values.
Paper: A XRISM View of Relativistic Reflection in Cygnus X-1
Authors: Paul A. Draghis, Jon M. Miller, Erin Kara, Elisa Costantini, Oluwashina Adegoke, Javier A. García
Figure caption: Focused look in the 6.25–7.15 keV (top) and 6.3–6.5 keV (bottom) at the XRISM Resolve observation of Cygnus X-1, during the first (left) and second (right) halves of the observation. The solid red lines represent our best-fit models. The dashed blue lines show the unblurred MYTorus component, illustrating that the Fe Kα complex is resolved in the data. The spectra were not rebinned for visual purposes and display the spectral bins produced by the “optimal” binning scheme used in the analysis.
Paper: A XRISM View of Relativistic Reflection in Cygnus X-1
Authors: Paul A. Draghis, Jon M. Miller, Erin Kara, Elisa Costantini, Oluwashina Adegoke, Javier A. García
Figure caption: Spectra (top panels) and residuals produced when fitting the spectra from the first half (left) and second half (right) of the XRISM Resolve observation of Cygnus X-1 with a power-law model (middle panels) and with our best-fit model (lower panels). The solid line represents our best-fit model, while the dashed line shows the underlying power-law component. The spectra in the figure were rebinned for visual clarity to have a minimum significance of 50σ per bin, or to combine a maximum number of 20 spectral bins.
Paper: A XRISM View of Relativistic Reflection in Cygnus X-1
Authors: Paul A. Draghis, Jon M. Miller, Erin Kara, Elisa Costantini, Oluwashina Adegoke, Javier A. García
Figure caption: Top: light curve of Cygnus X-1 as seen by XRISM Resolve during ObsID 300049010. The black, blue, and red indicate the light curves in the 2–10, 5–10, and 2–5 keV bands, respectively. The bottom axis shows the MJD of the observation, while the top axis shows the orbital phase of Cygnus X-1. The light curve was binned so that each point corresponds to a 300 s interval. The vertical magenta and cyan lines indicate orbital phases 0.9 and 1, respectively. The vertical black lines indicate the duration of the NuSTAR observation used in this analysis. Bottom: hardness ratio computed by dividing the 5–10 keV light curve in the top panel by the 2–5 keV light curve.