adsabs/AstroCLIMB huggingface dataset:
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Comparison of H I-to-stellar mass vs. baryonic mass for objects from this work (purple, various symbols) to the young TDG candidate HCG 16-LSB1 (Román et al. 2021; blue pentagon), AD-TDG candidates from Lee-Waddell et al. (2016; green right-pointing triangles), TDG candidates from Lelli et al. (2015; turquoise circles), and likely older TDGs identified in McConnachie (2012; red left-pointing triangles). ﹩{M}_{{\rm{H}}{\rm\small{I}}}^{{\prime} }﹩ and ﹩{M}_{\mathrm{bary}}^{{\prime} }﹩ for the objects from this work and from Lee-Waddell et al. (2016) are calculated with the ALFALFA measurements (Haynes et al. 2018). The H I masses for the Duc et al. (2014) TDGs used in the baryonic mass calculation are from Duc et al. (2011). For the comparison of TDG properties to those of normal (non-TDG) dwarf galaxies, we have plotted Local Group dIrrs from McConnachie (2012; dark gray triangles). As with Figure 19, filled symbols correspond to objects that have been identified as TDGs.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: NGC 3510 moment one map from WSRT imaging, with WSRT H I column density contours superimposed in dark gray. Contour levels are the same as in Figure 11.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Left: WIYN 3.5 m composite ﹩g^{\prime} +r^{\prime} ﹩-band summed image of NGC 7775 in grayscale, inverted to highlight the tidal tail at the top. Right: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image of AGC 333576, with same H I column density contours as Figure 17 in white.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: H I emission-line channel maps for AGC 219369 from WSRT data. The white cross marks the center of the galaxy and the velocity for each channel map is listed in the lower left corner. The emission of the galaxy is displayed by gray background and blue contour lines. The best-fitting model is shown by the red contour lines. Solid contours are at 2, 4, and 8 times the S/N of the data, and dashed contours represent −2 × S/N.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: H I emission-line channel maps for AGC 229398 from WSRT data. The white cross marks the center of the galaxy and the velocity for each channel map is listed in the lower left corner. The emission of the galaxy is displayed by gray background and blue contour lines. The best-fitting model is shown by the red contour lines. Solid contours are at 2, 4, and 8 times the S/N of the data, and dashed contours represent −2 × S/N.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: H I emission-line channel maps for AGC 333576 from WSRT data. The white cross marks the center of the galaxy and the velocity for each channel map is listed in the lower left corner. The emission of the galaxy is displayed by gray background and blue contour lines. The best-fitting model is shown by the red contour lines. Solid contours are at 2, 4, and 8 times the S/N of the data, and dashed contours represent −2 × S/N.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: H I emission-line channel maps for AGC 123216 from WSRT data. The white cross marks the center of the galaxy and the velocity for each channel map is listed in the lower left corner. The emission of the galaxy is displayed by gray background and blue contour lines. The best-fitting model is shown by the red contour lines. Solid contours are at 2, 4, and 8 times the S/N of the data, and dashed contours represent −2 × S/N.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Comparison of dynamical-to-gas mass ratios for objects from this work (purple, various symbols) to the young TDG candidate HCG 16-LSB1 (Román et al. 2021; blue pentagon), AD-TDG candidates from Lee-Waddell et al. (2016; green right-pointing triangles), and TDG candidates from Lelli et al. (2015; turquoise circles). For the comparison of TDG properties to those of normal (non-TDG) dwarf galaxies, we have plotted a sample of Local Group dIrrs from McConnachie (2012; dark gray triangles). M gas for the LG dIrrs is calculated using 1.33 × the H I mass reported in McConnachie (2012), and M dyn uses the dynamical masses from the same paper supplemented by the total masses reported in Mateo (1998) when necessary. M gas for the TDGs from Lelli et al. (2015) is the sum of M atomic and M molecular reported in that work. All objects that have been identified as TDGs have filled symbols, and those that are not TDGs have unfilled symbols.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Comparison of central surface brightness vs. stellar mass for objects from this work (purple, various symbols) to the young TDG candidate HCG 16-LSB1 (Román et al. 2021; blue pentagon), TDG candidates discussed in Lelli et al. (2015; turquoise circles), and likely older TDGs identified in Duc et al. (2014; red left-pointing triangles). The non-TDG dwarf galaxy comparison samples plotted are Local Group dwarf irregulars from McConnachie (2012; dark gray triangles) and Hydra I cluster dwarf ellipticals whose properties were compiled by Misgeld et al. (2008) and Misgeld & Hilker (2011; light gray squares). Conversions from surface brightness in g to V were made with the Jester et al. (2005) transformation equations and the central color of the object where possible. If the central color was not known, the total g − r color of the object was used, and if no color information was given, an average estimate of 0.4 ± 0.1 for dwarf galaxies based on the colors of Honey et al. (2018) was used. As with Figure 19, filled symbols correspond to objects that have been identified as TDGs.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Comparison of effective radius vs. stellar mass for objects from this work (purple, various symbols) to the young TDG candidate HCG 16-LSB1 (Román et al. 2021; blue pentagon), AD-TDG candidates from Lee-Waddell et al. (2016; green right-pointing triangles), TDG candidates from Lelli et al. (2015; turquoise circles), and likely older TDGs identified in Duc et al. (2014; red left-pointing triangles). We have also plotted the sample of UDGs from Mancera Piña et al. (2020; dark gray circles). For the comparison of TDG properties to those of normal (non-TDG) dwarf galaxies, we have plotted Local Group dIrrs from McConnachie (2012; dark gray triangles), and Hydra I cluster dwarf ellipticals compiled by Misgeld & Hilker (20111; light gray squares). As with Figure 19, filled symbols correspond to objects that have been identified as TDGs.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite imaging for the potential parents of AGC 229398. Left: KUG 1158+216, scaled to show the faint extension of stellar emission on the left. Right: UGC 6989, with WSRT H I column density contours at N H I  = (0.1, 0.2, 0.4, 0.8, 1.6, 3.2, 6.4) × 1020 cm−2 in white. Due to the large angular separation from AGC 229398 and the smaller field of view of pODI, UGC 6989 was located at the edge of the CCD, which resulted in several detector artifacts in the image.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image showing the full-field view of AGC 333576 and potential parent NGC 7775. There are WSRT H I column density contours at N H I  = (0.1, 0.5, 1.2, 2.4, 4.5) × 1020 cm−2 superimposed in white. The nearby elliptical galaxy WISEA J235250.49+284555.2 is also labeled.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Masking, surface brightness profiles, and profile fit parameters for AGC 333576 in ﹩g^{\prime} ﹩ (top row of each panel) and ﹩r^{\prime} ﹩ (bottom row of each panel), with optical images from the WIYN 3.5 m telescope. Figure description is the same as Figure 3.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image showing the full-field view of AGC 229398 (lower left) with potential parents UGC 6989 (upper right) and KUG 1158+216 (below label). There are WSRT H I column density contours at N H I  = (0.1, 0.2, 0.4, 0.8, 1.6, 3.2, 6.4) × 1020 cm−2 superimposed in white. Note that the prominent spiral galaxy near the center of the image is CGCG 127-132, which has a heliocentric velocity of 14,457 ± 4 km s−1 and is not associated with the objects of interest in this paper (Albareti et al. 2017).
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Masking, surface brightness profiles, and profile fit parameters for AGC 219369 in ﹩g^{\prime} ﹩ (top row of each panel) and ﹩r^{\prime} ﹩ (bottom row of each panel), with optical images from the WIYN 3.5 m telescope. Figure description is the same as Figure 3. The physical scale bar for AGC 219369 is calculated for a distance of 9.2 Mpc.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image of AGC 123216, with WSRT H I column density contours at N H I  = (0.1, 0.5, 1.2, 2.4) × 1020 cm−2. The stellar component at the center is extremely blue and elongated in the east–west direction, while the H I distribution is rounder.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image of AGC 219369, with WSRT H I column density contours at N H I  = (0.1, 0.5, 1.2, 2.4) × 1020 cm−2 superimposed in white. The physical scale bar is calculated for a distance of 9.2 Mpc.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image of MRK 365 with WSRT H I column density contours at N H I  = (0.1, 0.5, 1.2, 2.4) × 1020 cm−2 in white. The H I contours are slightly offset from the stellar disk, and the image is scaled to show a faint loop of stellar emission on the right side, between the first and second innermost contours.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: Masking, surface brightness profiles, and profile fit parameters for AGC 229398 in ﹩g^{\prime} ﹩ (top row of each panel) and ﹩r^{\prime} ﹩ (bottom row of each panel), with optical images from the WIYN 3.5 m telescope. Figure description is the same as Figure 3.
Paper: Catching Tidal Dwarf Galaxies at a Later Evolutionary Stage with ALFALFA
Authors: Laurin M. Gray, Katherine L. Rhode, Lukas Leisman, Pavel E. Mancera Piña, John M. Cannon, John J. Salzer, Lexi Gault, Jackson Fuson, Gyula I. G. Józsa, Elizabeth A. K. Adams, Nicholas J. Smith, Martha P. Haynes, Steven Janowiecki, Hannah J. Pagel
Figure caption: WIYN 3.5 m ﹩g^{\prime} +r^{\prime} ﹩-band composite image of AGC 229398, with WSRT H I column density contours at N H I  = (0.1, 0.2, 0.4, 0.8, 1.6) × 1020 cm−2 in white.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: The results of cross-correlating the SPIRou (first row), IRD (second row), and IGRINS (third row) data sets with a model transmission spectrum containing spectral lines only from H2O. The bottom row shows the result of combining all data sets together. The first column shows the cross-correlation for each frame in the barycentric frame. The expected trace of the planet’s signal is shown as the dotted diagonal line. The second column shows the cross-correlation for each frame in the planet’s rest frame. The dotted line shows the expected trace of the planet’s signal at the system’s systemic velocity. The third column shows the phase-folded cross-correlation signal as a function of phase. The dotted horizontal and vertical lines show the planet’s expected position in ±K P and systemic velocity, respectively. The fourth column shows the 1D cross-correlation as a function of systemic velocity at ±K P. The black dotted line indicates the system’s systemic velocity.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Chemical equilibrium abundance profiles for GJ 486b computed by GGchem. Columns: isothermal pressure–temperature profiles at 300 K (left), 500 K (middle), and 700 K (right). Rows: no condensation (top), condensation included (middle), condensation and rain out (bottom).
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Constraints on the presence of H2O (top left), CH4 (top right), NH3 (middle left), CH4 (middle right), CO2 (lower left), and CO (lower right) in GJ 486b’s atmosphere. Shown within each large panel are the limits from SPIRou (top left), IRD (top right), IGRINS (bottom left), and all data sets combined (lower right). The vertical axis shows the log10 of the VMR of the given species, while the horizontal axis shows the atmosphere’s MMW. The black and gray regions indicate the VMR–MMW parameter space that can be ruled out to 5σ and 3σ, respectively. The light blue regions are allowed by our observations.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: The results of cross-correlating a model transmission spectrum containing spectral lines only from H2O with the IGRINS data after a variable number of SYSREM iterations were applied. The rows show the result of applying 1, 2, 3, 4, 5, 8, 11, 14, 17, and 20 iterations, respectively. The first column shows the cross-correlation for each frame in the planet’s rest frame. The dotted line shows the expected trace of the planet’s signal at the system’s systemic velocity. The second column shows the phase-folded cross-correlation signal as a function of phase. The dotted horizontal and vertical lines show the planet’s expected position in ±K P and systemic velocity, respectively. The third column shows the 1D cross-correlation as a function of systemic velocity at ±K P. The black dotted line indicates the system’s systemic velocity.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Example of marginalized likelihoods for a strong injected signal.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Same as Figure 2, except for using the solar abundances at 700 K model generated by GGchem.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Same as Figure 2, except for Na. The row for IGRINS is omitted because no Na lines are within its spectral range.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Same as Figure 2, except for NH3.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Same as Figure 2, except for CO2.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Same as Figure 2, except for CH4.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Same as Figure 2, except for HCN.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Mass comparisons. (a) Comparison between individual component masses from MSC and those estimated using Al-Wardat’s method. (b) Comparison between the dynamical mass sums calculated depending on orbital elements, MSC mass, and those estimated using Al-Wardat’s method. Based on the Hipparcos 2 parallax (blue), Gaia DR2 parallax (green), Gaia DR3 (magenta), and MSC (red). The dotted line represents y = x.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 13498. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 2.818 Gyr isochrone with Z = 0.03.