adsabs/AstroCLIMB huggingface dataset:
Paper: Metallicity Regulates Planet Formation across All Masses
Authors: Max Nguyen, Vardan Adibekyan
Figure caption: Summed mass fraction of heavy elements as a function of planetary mass. Left: Z versus the mass of individual planets in the system. Center: Z versus the mass of the most massive planet in each system. Right: Z versus the total planetary mass in the system. The solid black line shows the best-fit OLS regression to the full sample. Green dashed lines show separate OLS fits to the Jupiter-mass and super-Jupiter-mass regimes. The horizontal dotted blue line indicates the mean Z of stars without detected planets, with the shaded region showing the ±1σ interval.
Paper: Metallicity Regulates Planet Formation across All Masses
Authors: Max Nguyen, Vardan Adibekyan
Figure caption: Relationship between Z and planetary mass across system architectures. Left: sub-Neptune- and Neptune-mass planets. Center: Jupiter-mass planets. Right: super-Jupiter-mass planets. Black points correspond to multiplanetary systems, while orange points indicate single-planet systems. Smoothed marginal distributions via kernel density estimates of Z and Mp are shown for both populations.
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption:  ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})﹩ as a function of APOKASC3 log (age) (top) and [C/N]-based log (age) (bottom). The gray gradient shaded regions represent bins of field stars; darker bins imply more stars. The green circles, blue triangles, and red diamonds represent cluster member stars common to samples NGC 6791, NGC 6819, and NGC 6811, respectively. The vertical dashed lines are the T. Cantat-Gaudin et al. (2020)–determined ages for each cluster, and the respective shaded regions show the error in cluster age. The horizontal gray dashed line is where ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})=0﹩ with the surrounding gray region representing a delta of −0.1 and + 0.1. The vertical gray dotted line shows the currently accepted age of the Universe (13.8 ± 0.05 Gyr; Planck Collaboration et al. 2020; DESI Collaboration et al. 2024a; DESI Collaboration et al. 2024b). Median representative error bars are shown in each panel. Cluster members older than the Universe, highlighted with an orange diamond, were found to be rapidly rotating (R. A. Patton et al. 2024), and those highlighted with a purple square were found to be in a binary system (A. M. Price-Whelan et al. 2020).
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption: The [C/N] versus ﹩\mathrm{log}\,(\mathrm{Age}[\mathrm{yr}])﹩ distribution for the final sample, composed of T. Spoo et al. (2022) open cluster sample and globular clusters 47 TUC, M 71, M 4, and M 5. Clusters represented by blue circles are from the final calibration sample of T. Spoo et al. (2022). Globular clusters 47 TUC, M 71, M 4, and M 5 are represented with an indigo square, an orange thin diamond, a cyan left triangle, and a red right triangle, respectively. Our new linear fit is shown as a solid black line, and the fit’s error envelope is shown with the gray region. The accepted age of the Universe is shown as a vertical gray dashed line. The open clusters used in our asteroseismic age comparison are NGC 2682 (M 67), NGC 6791, and NGC 6819 and are shown by a black-outlined red square, green circle, and blue triangle, respectively.
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption: The [C/N] versus ﹩\mathrm{log}\,(\mathrm{Age}[\mathrm{yr}])﹩ distribution for the final sample, composed of the T. Spoo et al. (2022) open cluster sample and globular clusters 47 TUC, M 71, M 4, and M 5. Clusters represented by blue circles are from the final calibration sample of T. Spoo et al. (2022). Globular clusters 47 TUC, M 71, M 4, and M 5 are represented with an indigo square, an orange thin diamond, a cyan left triangle, and a red right triangle, respectively. Our new fit is shown as a solid black line, and the maximum possible calculated age envelope is shown with the gray region. The accepted age of the Universe (13.8 ± 0.05 Gyr; Planck Collaboration et al. 2020; DESI Collaboration et al. 2024a; DESI Collaboration et al. 2024b) is shown as a vertical gray dashed line. The open clusters used in our asteroseismic age comparison are NGC 2682 (M 67), NGC 6791, and NGC 6819 and are shown in a black-outlined red square, green circle, and blue triangle, respectively. Note: uncertainties on the ages for the globular clusters are assumed by this work to be ±0.1, thus conservative, and are likely smaller.
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption:  ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})﹩ as a function of APO-K2 log (age) (top) and [C/N]-based log (age) (bottom). The gray gradient shaded regions represent bins of field stars; darker bins imply more stars. The red squares, green circles, and blue triangles represent cluster member stars common to samples NGC 2682 (M 67), NGC 6791, and NGC 6819, respectively. The vertical dashed lines are the T. Cantat-Gaudin et al. (2020)–determined ages for each cluster, and the respective shaded regions show the error in cluster age. The horizontal gray dashed line is where ﹩{\rm{\Delta }}\mathrm{log}\,(\mathrm{Age})=0﹩, with the surrounding gray region representing a delta of −0.1 and +0.1. The vertical gray dotted line shows the accepted age of the Universe. Median representative error bars are shown in each panel. Clusters member older than the Universe, highlighted with a purple square, were found to be in a binary system (A. M. Price-Whelan et al. 2020).
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption: [C/N] versus [C+N/Fe] plots for globular clusters 47 TUC, M 71, M 4, and M 5. Light-gray dots are APOGEE halo field stars with similar Mg and Fe abundances to the cluster. Stars outlined in black are members of the respective cluster, where those colored in red are considered peculiar enriched stars within the cluster, while those colored in cyan are those that are not peculiar and are similar to the field stars. The black dashed line represents the cut we did to remove the peculiar stars from the calibration sample. A representative error bar is shown in the bottom-left corner of each panel for each cluster.
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption: Log(g) versus [C/N] plot of first population of stars without peculiar enrichment. These are the same stars from Figure 4 shown in cyan. Stars used in our calibration are shown in green. The gray vertical dashed line and vertical red dashed line represent the FDU log(g) cut and extramixing (EM), respectively, from Table 2 of M. Shetrone et al. (2019).
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption: Gaia color–magnitude diagram for globular clusters 47 TUC, M 71, M 4, and M 5 colored by [Fe/H]. Black dashed lines represent the polynomial functions used to separate RGB from red clump and AGB members of each cluster. Note the magnitude errors are smaller than the markers.
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption: [Al/Fe]–[Mg/Fe], [O/Fe]–[Na/Fe], and [Al/Fe]–[Si/Fe] (anti)correlation plots for globular clusters M 4 (top set) and M 5 (bottom set) colored by [Fe/H]. Black dashed lines represent functions to isolate the two populations of stars within the RGB sample.
Paper: Extending the [C/N]–Age Calibration: Using Globular Clusters to Explore Older and Metal-poor Populations
Authors: Taylor Spoo, Katelyn Thomas, Ellie Kaleo Toguchi-Tani, Jonah Otto, Natalie Myers, Jamie Tayar, Jessica S. Schonhut-Stasik, Matthew Shetrone, Alessa Ibrahim Wiggins, John Donor, Peter M. Frinchaboy
Figure caption: [Al/Fe]–[Mg/Fe] and [O/Fe]–[Na/Fe] (anti)correlation plots for globular clusters 47 TUC (top set) and M 71 (bottom set) colored by [Fe/H]. Black dashed lines represent functions to isolate the two populations of stars within the RGB sample.
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Contours of 50% search completeness for the 120 stars with at least 20 nights of RVs (black lines). Top: from left to right, each panel shows the same CL50 lines as a function of ﹩{M}_{{\rm{p}}}\,\sin \,i﹩ and semimajor axis, maximum projected separation (assuming circular orbits), and stellar insolation flux. The median CL50 in each panel is shown by the solid colored line in either orange, red, or blue. The middle 68% of CL50 lines are between the dashed colored lines. The conservative and optimistic HZs for a solar twin (J. F. Kasting et al. 1993; R. K. Kopparapu et al. 2013) are indicated by the green shaded regions in the rightmost panel. Bottom: same as the top row, only with RV semiamplitude K shown on the vertical axis. Earth, Neptune, Saturn, and Jupiter values are indicated by black diamonds in each panel, assuming e = 0, i = 90°, and d = 10 pc for a solar twin.
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Flowchart summarizing the steps followed to compile the public RV data sets identified by the SPORES-HWO R. Hunters volunteers. The arrows in this example trace the data compilation progress for the second target star in target group 2 (T2,2), from being assigned to volunteers to being completed as a final merged and vetted data set. Each volunteer is randomly assigned three target groups, with each target group containing four target stars from the SPORES-HWO Catalog. Multiple volunteers are assigned to the same target star for redundancy. The volunteers then collect and merge data from various databases, catalog papers, and ADS, as described in Section 3.2. Then, the merged data files from each volunteer are vetted and combined once more to create a final data set for each target star.
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Histogram of the number of RV epochs obtained for each target star. Each histogram bin has a width of 0.1 dex. Interestingly, the stars appear to be clustered in roughly three groups based on how many times they have been observed, which we quantified using a best-fit three-Gaussian model (shown in black). The least-observed stars with fewer than 20 RVs were excluded from the analysis in this work. A 2D version of this histogram including the observational time span and the derived HZ sensitivity limits (Section 6.2) is shown in Figure 15 in Appendix A.
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: H-R diagrams of the 164 target stars, where color indicates the number of RV epochs (left) or the lower mass sensitivity limit in the MHZ (right). Stars with fewer than 20 epochs of RV observations are marked with a red “⨂” in both panels. Solar values are shown by the thin dashed lines, and the approximate effective temperature corresponding to the Kraft Break (∼6250 K; R. P. Kraft 1967) is indicated by the transparent red line. The stellar properties plotted here were taken from the SPORES-HWO Catalog (C. K. Harada et al. 2024).
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Scatter plot and histograms of stellar effective temperature and ﹩\mathrm{log}\,R{{\prime} }_{{\rm{HK}}}﹩ (from C. K. Harada et al. 2024). The color scale corresponds to the number of RV observation epochs. Targets with fewer than 20 RV epochs are marked by a red “⨂” symbol. The shaded 1D histograms above and to the right distinguish between targets with at least 20 RV epochs (black) and those with fewer than 20 RV epochs (red). The median 1D histogram values are indicated by solid lines. The approximate location of the Kraft Break temperature is shown by the transparent red line, and solar values are shown by the dashed lines (﹩\mathrm{log}\,R{{\prime} }_{{\rm{HK}},\odot }=-4.943﹩; R. Egeland et al. 2017).
Paper: SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring 
Authors: Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Stephen R. Kane, Sarah Blunt, Jamie Dietrich, Natalie R. Hinkel, Zhexing Li, Eric Mamajek, Malena Rice, Noah W. Tuchow, Robert A. Wittenmyer, Christopher Chin, Aidan Fernandez, Shivani Kulkarni, Emerald Lin, Nykole Liu, Remy Liu, Abhi Nathan, Adam Zbriger
Figure caption: Lower ﹩{M}_{{\rm{p}}}\,\sin \,i﹩ sensitivity limits in the middle of the conservative HZ (J. F. Kasting et al. 1993; R. K. Kopparapu et al. 2013) derived from the CL50 lines shown in Figure 7. More conservative sensitivity estimates are shown by the black points and vertical lines, which have been derived from the CL90 contours. The sensitivity limits are shown as a function of the physical separation (left) and maximum angular separation (right) of the middle of the conservative HZ defined in instellation space. The points are colored by stellar effective temperature. The sensitivity limit values shown here, in addition to sensitivity limits computed for the IHZ and OHZ, are listed in Table 9 in Appendix A.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: Mosaic images of the 35 primary GB fields. Galactic north is up, and east is to the left. The field boundaries are outlined in green and labeled with their field numbers (GB#). Sgr A* is located on chip 2 of GB94. Black lines represent chip gaps. Red dots show the positions of the 486 microlensing candidates. Purple regions indicate the nominal Roman RGBTDS candidate fields (over-guide).
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: Photometric precision in the GB fields as a function of H-band magnitude. The black points show the standard deviation, σH, of light curves for a subsample of 69,000 nonvariable stars in the GB94 field. Outliers with larger σH values are likely due to remaining variable objects. The green, cyan, red, and orange lines indicate the median values in magnitude bins for chips 1, 2, 3, and 4, respectively, while the magenta filled circles represent the median over all chips.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: Observational fields of PRIME toward the GB. The color map shows the microlensing event rate based on OGLE data (P. Mróz et al. 2019). The grid of black squares and the field numbers indicate the PRIME fields, labeled as GB#. The blue squares represent the 35 primary GB fields. Cyan squares indicate nine low-extinction fields that overlap with the MOA survey. Magenta boxes show the MOA fields, and the purple regions indicate the nominal Roman RGBTDS candidate fields (over-guide). Sgr A* is located in GB94.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: The light curves of PRIME-2024-BLG-124 and -170, detected in fields GB75 and GB78, respectively. The vertical axis shows the differential flux (Δflux) in ADU. The red lines indicate the best-fit models, with event timescales of tE = 56.5 ± 2.0 days and 32.2 ± 0.6 days, impact parameters of u0 = 0.060 ± 0.0029 and 0.084 ± 0.002, and H-band source magnitudes of Hs = 12.90 ± 0.20 mag and Hs = 14.90 ± 0.20 mag, respectively.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: Throughput of the filters. The broad bands Z, Y, J, and H are shown as purple, green, yellow, and red shaded regions, respectively. The narrow bands NB1063, NB1243, and NB1630 are represented by thick green, yellow, and red lines, respectively.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: Images of the field GB94 with its four chips. Galactic north is up, and east is to the left. Chip numbers are shown in red. Sgr A* is located on chip 2.