adsabs/AstroCLIMB huggingface dataset:
Paper: UNIONS: The Ultraviolet Near-infrared Optical Northern Survey
Authors: Stephen Gwyn, Alan W. McConnachie, Jean-Charles Cuillandre, Kenneth C. Chambers, Eugene A. Magnier, Thomas de Boer, Michael J. Hudson, Masamune Oguri, Hisanori Furusawa, Hendrik Hildebrandt, Raymond Carlberg, Sara L. Ellison, Junko Furusawa, Raphaël Gavazzi, Rodrigo Ibata, Yannick Mellier, Ken Osato, H. Aussel, Lucie Baumont, Manuel Bayer, Olivier Boulade, Patrick Côté, David Chemaly, Cail Daley, Pierre-Alain Duc, Florence Durret, A. Ellien, Sébastien Fabbro, Leonardo Ferreira, Itsna K. Fitriana, Emeric Le Floc'h, Yoshinobu Fudamoto, Hua Gao, L. W. K. Goh, Tomotsugu Goto, Sacha Guerrini, Axel Guinot, Vincent Hénault-Brunet, Francois Hammer, Yuichi Harikane, Kohei Hayashi, Nick Heesters, Kohei Ichikawa, Martin Kilbinger, P. B. Kuzma, Qinxun Li, Tobías I. Liaudat, Chien-Cheng Lin, Oliver Müller, Nicolas F. Martin, Yoshiki Matsuoka, Gustavo E. Medina, Hironao Miyatake, Satoshi Miyazaki, Charlie T. Mpetha, Tohru Nagao, Julio F. Navarro, Masafumi Niwano, Itsuki Ogami, Nobuhiro Okabe, Masafusa Onoue, Gregory S. H. Paek, Laura C. Parker, David R. Patton, Fabian Hervas Peters, Simon Prunet, Rubén Sánchez-Janssen, M. Schultheis, Federico Sestito, Simon E. T. Smith, J.-L. Starck, Else Starkenburg, Connor Stone, Christopher Storfer, Yoshihisa Suzuki, T. Erben, Salvatore Taibi, G. F. Thomas, Yoshiki Toba, Hisakazu Uchiyama, David Valls-Gabaud, Kim A. Venn, Ludovic Van Waerbeke, Richard J. Wainscoat, Scott Wilkinson, Anna Wittje, Taketo Yoshida, TianFang Zhang, Yuxing Zhong
Figure caption: Representative photometric super-flat for CFIS r-band data. The figure shows the variation of the zero point, measured in magnitudes, across the MegaCam focal plane.
Paper: UNIONS: The Ultraviolet Near-infrared Optical Northern Survey
Authors: Stephen Gwyn, Alan W. McConnachie, Jean-Charles Cuillandre, Kenneth C. Chambers, Eugene A. Magnier, Thomas de Boer, Michael J. Hudson, Masamune Oguri, Hisanori Furusawa, Hendrik Hildebrandt, Raymond Carlberg, Sara L. Ellison, Junko Furusawa, Raphaël Gavazzi, Rodrigo Ibata, Yannick Mellier, Ken Osato, H. Aussel, Lucie Baumont, Manuel Bayer, Olivier Boulade, Patrick Côté, David Chemaly, Cail Daley, Pierre-Alain Duc, Florence Durret, A. Ellien, Sébastien Fabbro, Leonardo Ferreira, Itsna K. Fitriana, Emeric Le Floc'h, Yoshinobu Fudamoto, Hua Gao, L. W. K. Goh, Tomotsugu Goto, Sacha Guerrini, Axel Guinot, Vincent Hénault-Brunet, Francois Hammer, Yuichi Harikane, Kohei Hayashi, Nick Heesters, Kohei Ichikawa, Martin Kilbinger, P. B. Kuzma, Qinxun Li, Tobías I. Liaudat, Chien-Cheng Lin, Oliver Müller, Nicolas F. Martin, Yoshiki Matsuoka, Gustavo E. Medina, Hironao Miyatake, Satoshi Miyazaki, Charlie T. Mpetha, Tohru Nagao, Julio F. Navarro, Masafumi Niwano, Itsuki Ogami, Nobuhiro Okabe, Masafusa Onoue, Gregory S. H. Paek, Laura C. Parker, David R. Patton, Fabian Hervas Peters, Simon Prunet, Rubén Sánchez-Janssen, M. Schultheis, Federico Sestito, Simon E. T. Smith, J.-L. Starck, Else Starkenburg, Connor Stone, Christopher Storfer, Yoshihisa Suzuki, T. Erben, Salvatore Taibi, G. F. Thomas, Yoshiki Toba, Hisakazu Uchiyama, David Valls-Gabaud, Kim A. Venn, Ludovic Van Waerbeke, Richard J. Wainscoat, Scott Wilkinson, Anna Wittje, Taketo Yoshida, TianFang Zhang, Yuxing Zhong
Figure caption: Localized spatial coverage in a 2° × 4° area for the Pan-STARRS i-band (top panel) and z-band data (bottom panel), showing the observing pattern. The color scales are the same as in Figure 1.
Paper: UNIONS: The Ultraviolet Near-infrared Optical Northern Survey
Authors: Stephen Gwyn, Alan W. McConnachie, Jean-Charles Cuillandre, Kenneth C. Chambers, Eugene A. Magnier, Thomas de Boer, Michael J. Hudson, Masamune Oguri, Hisanori Furusawa, Hendrik Hildebrandt, Raymond Carlberg, Sara L. Ellison, Junko Furusawa, Raphaël Gavazzi, Rodrigo Ibata, Yannick Mellier, Ken Osato, H. Aussel, Lucie Baumont, Manuel Bayer, Olivier Boulade, Patrick Côté, David Chemaly, Cail Daley, Pierre-Alain Duc, Florence Durret, A. Ellien, Sébastien Fabbro, Leonardo Ferreira, Itsna K. Fitriana, Emeric Le Floc'h, Yoshinobu Fudamoto, Hua Gao, L. W. K. Goh, Tomotsugu Goto, Sacha Guerrini, Axel Guinot, Vincent Hénault-Brunet, Francois Hammer, Yuichi Harikane, Kohei Hayashi, Nick Heesters, Kohei Ichikawa, Martin Kilbinger, P. B. Kuzma, Qinxun Li, Tobías I. Liaudat, Chien-Cheng Lin, Oliver Müller, Nicolas F. Martin, Yoshiki Matsuoka, Gustavo E. Medina, Hironao Miyatake, Satoshi Miyazaki, Charlie T. Mpetha, Tohru Nagao, Julio F. Navarro, Masafumi Niwano, Itsuki Ogami, Nobuhiro Okabe, Masafusa Onoue, Gregory S. H. Paek, Laura C. Parker, David R. Patton, Fabian Hervas Peters, Simon Prunet, Rubén Sánchez-Janssen, M. Schultheis, Federico Sestito, Simon E. T. Smith, J.-L. Starck, Else Starkenburg, Connor Stone, Christopher Storfer, Yoshihisa Suzuki, T. Erben, Salvatore Taibi, G. F. Thomas, Yoshiki Toba, Hisakazu Uchiyama, David Valls-Gabaud, Kim A. Venn, Ludovic Van Waerbeke, Richard J. Wainscoat, Scott Wilkinson, Anna Wittje, Taketo Yoshida, TianFang Zhang, Yuxing Zhong
Figure caption: Photometric redshifts estimated with BPZ from the GAaP catalog vs. spectroscopic redshifts. This logarithmically scaled density plot (arbitrarily normalized) shows the quality of ugriz photo-zs obtained from UNIONS multi-band photometry. The dashed and dotted lines indicate the limits for outliers, as defined in Section 4.
Paper: UNIONS: The Ultraviolet Near-infrared Optical Northern Survey
Authors: Stephen Gwyn, Alan W. McConnachie, Jean-Charles Cuillandre, Kenneth C. Chambers, Eugene A. Magnier, Thomas de Boer, Michael J. Hudson, Masamune Oguri, Hisanori Furusawa, Hendrik Hildebrandt, Raymond Carlberg, Sara L. Ellison, Junko Furusawa, Raphaël Gavazzi, Rodrigo Ibata, Yannick Mellier, Ken Osato, H. Aussel, Lucie Baumont, Manuel Bayer, Olivier Boulade, Patrick Côté, David Chemaly, Cail Daley, Pierre-Alain Duc, Florence Durret, A. Ellien, Sébastien Fabbro, Leonardo Ferreira, Itsna K. Fitriana, Emeric Le Floc'h, Yoshinobu Fudamoto, Hua Gao, L. W. K. Goh, Tomotsugu Goto, Sacha Guerrini, Axel Guinot, Vincent Hénault-Brunet, Francois Hammer, Yuichi Harikane, Kohei Hayashi, Nick Heesters, Kohei Ichikawa, Martin Kilbinger, P. B. Kuzma, Qinxun Li, Tobías I. Liaudat, Chien-Cheng Lin, Oliver Müller, Nicolas F. Martin, Yoshiki Matsuoka, Gustavo E. Medina, Hironao Miyatake, Satoshi Miyazaki, Charlie T. Mpetha, Tohru Nagao, Julio F. Navarro, Masafumi Niwano, Itsuki Ogami, Nobuhiro Okabe, Masafusa Onoue, Gregory S. H. Paek, Laura C. Parker, David R. Patton, Fabian Hervas Peters, Simon Prunet, Rubén Sánchez-Janssen, M. Schultheis, Federico Sestito, Simon E. T. Smith, J.-L. Starck, Else Starkenburg, Connor Stone, Christopher Storfer, Yoshihisa Suzuki, T. Erben, Salvatore Taibi, G. F. Thomas, Yoshiki Toba, Hisakazu Uchiyama, David Valls-Gabaud, Kim A. Venn, Ludovic Van Waerbeke, Richard J. Wainscoat, Scott Wilkinson, Anna Wittje, Taketo Yoshida, TianFang Zhang, Yuxing Zhong
Figure caption: The localized spatial coverage in a 2° × 4° area for the WHIGS g-band data, showing the observing pattern. The color scales are the same as Figure 1.
Paper: UNIONS: The Ultraviolet Near-infrared Optical Northern Survey
Authors: Stephen Gwyn, Alan W. McConnachie, Jean-Charles Cuillandre, Kenneth C. Chambers, Eugene A. Magnier, Thomas de Boer, Michael J. Hudson, Masamune Oguri, Hisanori Furusawa, Hendrik Hildebrandt, Raymond Carlberg, Sara L. Ellison, Junko Furusawa, Raphaël Gavazzi, Rodrigo Ibata, Yannick Mellier, Ken Osato, H. Aussel, Lucie Baumont, Manuel Bayer, Olivier Boulade, Patrick Côté, David Chemaly, Cail Daley, Pierre-Alain Duc, Florence Durret, A. Ellien, Sébastien Fabbro, Leonardo Ferreira, Itsna K. Fitriana, Emeric Le Floc'h, Yoshinobu Fudamoto, Hua Gao, L. W. K. Goh, Tomotsugu Goto, Sacha Guerrini, Axel Guinot, Vincent Hénault-Brunet, Francois Hammer, Yuichi Harikane, Kohei Hayashi, Nick Heesters, Kohei Ichikawa, Martin Kilbinger, P. B. Kuzma, Qinxun Li, Tobías I. Liaudat, Chien-Cheng Lin, Oliver Müller, Nicolas F. Martin, Yoshiki Matsuoka, Gustavo E. Medina, Hironao Miyatake, Satoshi Miyazaki, Charlie T. Mpetha, Tohru Nagao, Julio F. Navarro, Masafumi Niwano, Itsuki Ogami, Nobuhiro Okabe, Masafusa Onoue, Gregory S. H. Paek, Laura C. Parker, David R. Patton, Fabian Hervas Peters, Simon Prunet, Rubén Sánchez-Janssen, M. Schultheis, Federico Sestito, Simon E. T. Smith, J.-L. Starck, Else Starkenburg, Connor Stone, Christopher Storfer, Yoshihisa Suzuki, T. Erben, Salvatore Taibi, G. F. Thomas, Yoshiki Toba, Hisakazu Uchiyama, David Valls-Gabaud, Kim A. Venn, Ludovic Van Waerbeke, Richard J. Wainscoat, Scott Wilkinson, Anna Wittje, Taketo Yoshida, TianFang Zhang, Yuxing Zhong
Figure caption: Localized spatial coverage in a 2° × 4° area for the WISHES z-band data showing the observing pattern. The color scales are the same as in Figure 1.
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: The negative O’Connell effect in SV Gem. All data is plotted in light gray, the KELT binned median data is plotted in black, the spline fit is plotted in red, and horizontal dashed lines mark the different heights of the two maxima. Note the brighter maximum follows the shallower dip rather than the deeper. The effect is clear in both sets of observations, regardless of bandpass.
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: TESS Sectors 043 and 045 observations from 2021 (top) and Sector 072 observations from 2023 (bottom) of SV Gem.
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: TESS Sector 009 (top) observations for HS Hya show the final visible eclipses. Sector 035 (labeled 2021) is the first TESS light curve showing no eclipses, and Sectors 062 and 089 (bottom two) continue to lack an eclipsing signal. Observations are slightly corrected for TESS systematic variability.
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: Nine years of KELT light curves for SV Gem following the same format as Figure 1.
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: 125 yr of HS Hya eclipse depth measurements from J. R. A. Davenport et al. (2021; black). We place our depth measurements from KELT (blue) and TESS (green) observations into context.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: This figure compares evolved Hαe stars of Population I (black symbols; data in Table 4) with Population II metal-poor Hαe stars (green symbols; data in Table 6). In the case of the Population I giants the symbols are coded according to luminosity class: filled and open circles (classes I and I–II), filled and open squares (classes II and III), and post-AGB stars stars (open symbols). The dotted line corresponds to ﹩{M}_{{K}_{s},0}=-4.5﹩ mag.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: Metal-poor field giants with Hα spectroscopy found in the literature are shown in an (MV, B − V) CMD based on Johnson photometry. In the top panel the plotted magnitudes and colors are not corrected for interstellar reddening (hence the use of red symbols). Those giants known to exhibit Hα emission (Table 5) are shown as filled symbols. Open circles depict metal-poor stars not known to exhibit such emission. In the bottom panel the data for Hαe giants (filled blue circles for variable stars, and filled blue triangles for stars not known to be variable) have been corrected for the reddening listed in Table 6, whereas the uncorrected photometry from the upper panel is again plotted for nonemission stars (red open circles). A comparison of the two panels shows the relatively small effect of the reddening corrections.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: Metal-poor field giants in a pair of CMDs in which (V − Ks) is the color abscissa. The upper panel shows the absolute Ks magnitude, with absolute visual magnitude MV being plotted in the lower panel. Data points for Hα-emission giants have been corrected for interstellar reddening (Table 6) in both panels, and are shown as filled blue symbols (circles for variable stars, triangles for stars not known to be variable). Red open circles correspond to data for metal-poor stars not known to exhibit Hα emission; the photometry for these stars has not been corrected for interstellar reddening (hence the red symbols). Dotted lines correspond to ﹩{M}_{{K}_{s}}=-4.5﹩ mag.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: A central binary will remove some material, reducing the total disk mass (left panel) depending on the size of the disk (solid vs. dashed lines) and the size of the cavity (grayscale of the lines). The solid gray band represents our observed dust mass depletion. While the binary separations in our sample are not known, the spectroscopic resolution in the surveys used to define our sample limits the sample to separations <10 au, indicated by the vertical dotted line. By carving out the inner disk, the binary also changes the average temperature of the disk, which, in combination with the removed disk mass, reduces the observed dust disk flux (right panel). A central clearing associated with the binary can explain the observed disk only for relatively large binary separations in compact disks with large cavities and steep temperature profiles.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: Top: dust mass as a function of projected distance from θ1 Ori C for the tight binaries studied here (black points), ONC targets (green points, J. A. Eisner et al. 2018), and targets from across the Orion cloud (red points, S. E. van Terwisga et al. 2022). The vast majority of the tight binaries fall beyond the region within 0.1 pc that J. A. Eisner et al. (2018) identified as being affected by external photoevaporation. Bottom: disk dust mass distributions comparing tight binaries within 1 pc of θ1 Ori C and more distant sources. Sources close to θ1 Ori C show slightly higher masses, most likely due to the diminished sensitivity in a region with higher background emission; triangles indicate average upper limits for the corresponding samples.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: Membership diagnostics among the sources in our survey. We employ cuts on parallax (p) and proper motion (μα, μδ) to remove interlopers; these boundaries are indicated by solid black lines. RV is not used to remove noncluster members as it may be biased by the presence of a binary. Many of the sources identified as interlopers by their discrepant parallax and/or proper motion values also fall outside the pre-main-sequence region in the ﹩\mathrm{log}\,g﹩ versus Teff diagram, enclosed by the solid lines, which confirms their status as interlopers.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: Disk dust mass distribution for the tight binaries from our sample and as compared with the ONC (J. A. Eisner et al. 2018) and Orion (S. E. van Terwisga et al. 2022, left panel) and the young clusters Lupus, Cham I, and Taurus (data compiled by C. F. Manara et al. 2023, right panel). The disk masses around tight binaries are significantly depleted relative to those of the single stars in Orion and Lupus/Cham I/Taurus, and are comparable to those around stars in the ONC, which exhibits a depletion from photoevaporation from nearby massive stars.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: Infrared color–color diagrams using photometry from WISE (left) or Spitzer (right). In the left panel the polygon indicates the region containing class II sources, while the extensions upwards demarcate the region with class I sources (W. J. Fischer et al. 2016). In the right panel the black lines delineate sources with a significant infrared excess (R. A. Gutermuth et al. 2008). Inner disk excess emission is most evident in the longer-wavelength observations of WISE and Spitzer, in particular beyond ∼5 μm (W2 – W3, [3.6] – [5.8], [4.5] – [8.0]).
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: HCO+ detections, including moment 0 maps (in units of Jy bm−1 km s−1) and spectra (in the barycentric reference frame and in units of Jy). Cloud contamination is present in some of the spectra at vbary ∼ 30 km s−1. Dotted contours in the moment 0 maps are at 3σ, 5σ, 10σ, and 20σ. Gray bands indicate the ±1σ ranges for the stellar velocities as measured in optical spectra by M. Kounkel et al. (2019). Red dashed lines show model disk emission for comparison, generated using parametric models as described in Appendix B.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: Continuum images, centered on the detections, of noncluster members. Each panel is 25″ on a side, with the scale bar in units of mJy bm−1. Dotted contours are at 3σ, 5σ, 10σ, and 20σ and the ellipse in the lower right is the beam size.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: Continuum images, centered on the detections, of cluster members. Each panel is 6″ on a side, with the scale bar in units of mJy bm−1. Dotted contours are at 3σ, 5σ, 10σ, and 20σ. The horizontal line marks 500 au, while the ellipse in the lower right is the beam size, and the numbers in the upper left are cluster ID numbers.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The mass and radius of our two models for GJ 12 b (circular and eccentric orbits) compared to various composition models from L. Zeng et al. (2019), as well as a steam atmosphere model from M. Turbet et al. (2020) and an H/He atmospheric model from M. C. Nixon & N. Madhusudhan (2021) and M. C. Nixon et al. (2024). The star corresponding to the eccentric-orbit model has been shifted slightly upward so that the errors of the two points are distinguishable. We note that the 50% water model, which is from L. Zeng et al. (2019), assumes a planet temperature of 300 K, which is very close to the actual equilibrium temperature of this planet.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The ℓ1 periodogram analysis of the GJ 12 MAROON-X activity indicators. The figure shows the identified significant periods of the top 1% of noise models (in terms of cross-validation scores) for our RV data and identifies their false-alarm probabilities (FAPs) in the data. We include a red dashed line to indicate the 0.1% FAP level. From the top to bottom panel, these are: the chromatic index in the red and blue channels, the differential line width in the both channels, the hydrogen alpha line index in both channels, the three calcium infrared triplet line indices (8500.4 Å, 8544.4 Å, and 8664.5 Å), and the two sodium doublet line indices (5891.6 Å and 5897.6 Å). In general, we see that none of the activity indicators have any signals with an FAP < 0.1%, meaning that we cannot identify the stellar activity period from this data set.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The cosmic shoreline formulation from E. K. Pass et al. (2025) for small planets orbiting mid-to-late M dwarfs within 50 pc, showing our eccentric model for GJ 12 b (black star) in cumulative XUV radiation versus escape velocity space compared to the solar system planets (various colors), TRAPPIST-1 planets (green), and other planets with Rp  < 1.8 R⊕ (gray). The location of the tentative shoreline is placed based on what we know from the solar system, with Mars on the shoreline while Mercury is airless.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The results from our ℓ1 periodogram analysis of the RVs of GJ 12. The figure shows the identified significant periods of the top 1% of noise models (in terms of cross-validation scores) for our RV data and identifies the FAPs that they are present in the data. We include a red dashed line at FAP values of 0.1% for reference. We highlight and label the 39, 58, and 114 day signals mentioned in the text, as well as the period of the transiting planet. Top panel: our results with no unpenalized periods. Middle panel: our results with the 39 day period unpenalized. Bottom panel: our results with both the 39 and 58 day periods unpenalized.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The serval-calculated activity indicators from our MAROON-X data. From the top to bottom panel, these are: the chromatic index in the red and blue channels, the differential line width in the both channels, the hydrogen alpha line index in both channels, the three calcium infrared triplet line indices (8500.4, 8544.4, and 8664.5 Å), and the two sodium doublet line indices (5891.6 and 5897.6 Å).
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The MAROON-X RVs collected on calibrator star HD 3651 in 2024, with the RV model for the eccentric planet from R. Basant et al. (2025a) subtracted. It is obvious that there is a slope in the RV residuals, as well as a potential offset around the time of the temperature anomaly.