adsabs/AstroCLIMB huggingface dataset:
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Left: a two-dimensional histogram depicting the recovered semiamplitude of the injected planet in units of the recovered uncertainty, where values above ∼3 represent recoveries. Each tile represents an MCMC analysis performed where the injected planet has a period and semiamplitude determined by the horizontal and vertical axis position of the tile. Both axes scale logarithmically, but the color bars do not. Right: the right three panels are one-dimensional histograms of the same data depicted in the left histogram, but binned into different groups based on the value of the injected semiamplitude. The top histogram covers 0–6 m s−1, the middle 6–18 m s−1, and the bottom 18–40 m s−1. The vertical axes of these histograms are normalized probability densities rather than bin counts.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Markov Chain Monte Carlo corner plot of our eccentric (e < 0.5) TOI 620 b circum-primary model with all RV data points included, showing the posterior distributions of each model parameter that we allowed to vary. The gamma offsets and jitter terms are not shown, as they are all uncorrelated and to a good approximation are ideal Gaussian distributions. We obtain similar posteriors for K  b  and ﹩\dot{\gamma }﹩ for the assumption of a circular orbit.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: RV time series phased to the period of b, with the black model representing the planet’s MAP model fit. The maroon data points are binned RVs every 0.1 in phase. A careful inspection reveals that the RVs are marginally more consistent with a negative K  b , although in this circum-primary scenario we assume a prior of K  b  > 0.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: A series of generalized Lomb–Scargle periodograms examining the signals in our TOI 620 RV time series. The horizontal axes are all logarithmic. All three panels depict a single-planet search with a floating T  C . The top panel includes no extra planets, the middle panel models out TOI 620 b to search for a second planet, and the bottom panel models out both TOI 620 b and the linear RV trend to search for a second planet. The periods of b and the tentative c are marked with dashed red vertical lines in each panel.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: MCMC corner plot of our b and c model with all RV data points included, showing the posterior distributions of each model parameter that we allowed to vary. The gamma offsets and jitter terms are not shown, as they are all uncorrelated and to a good approximation are ideal Gaussian distributions.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: RV time-series plot for our two-planet model phased to the periods of b (left) and c (right), with the black models representing the planet’s MAP model fits. The maroon points are binned RVs every 0.1 in orbital phase.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Chandra image of IC 1613 field. The image shows the back-illuminated CCD 7 (bottom CCD) and about 60% of the bottom of the front-illuminated CCD 6 (top CCD). Each CCD is 8′ on a side. Point sources are labeled by increasing R.A., then increasing decl. The positions of all detected sources (corresponding to 90% confidence levels) are indicated with red ellipses and are labeled with numbers from 1 to 31 generally southwest of the respective ellipse. Blue circles are unlabeled and indicate the locations of sources detected by Liu (2011) but not by us (q.v. Table 3.2). Source 15 was not detected by Liu (2011). Source 26 indicates the galaxy’s only known SNR; sources 4 and 5 represent a possible double source in an external galaxy. The large green box represents the Hubble Space Telescope WFC3 field-of-view. The small green circle to its upper left is the Chandra aimpoint. The large C at bottom center is a portion of the emission of a cluster of galaxies, MCXC J0105.0 + 0201, and identified as source 33 in Table 2. Not shown are sources 32, which lies north of source 12 in this figure by ∼﹩6\buildrel{\,\prime}\over{.} 1﹩ and source 34, which lies southeast of the galaxy cluster by ∼﹩4\buildrel{\,\prime}\over{.} 5﹩.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Optical image (obtained from the NED, originally from Lowell Observatory) of IC 1613 with Chandra chips S6, S7, and S8 overlaid (top to bottom); Chandra CCDs are 8.′4 on a side. The aimpoint of the observation is indicated by the small white circle. The large blue circle is the D25 circle (∼﹩9\buildrel{\,\prime}\over{.} 3﹩ diameter). Only about ∼51% of the galaxy is covered by the Chandra observation, based on the D25 and CCD sizes. The green circles, from top to bottom, correspond to the X-ray sources not associated with IC 1613 (source numbers 32, 33 (the cluster of galaxies MCXC J0105.0+0201), and 34 = GT Cet).
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Fluxes for the detected sources as calculated in the Chandra Source Catalog (CSC) and as calculated in this paper. In general, the fluxes fall on the 1:1 line. The most egregious “failure” of the 1:1 line is the source with low CSC flux and high on the y-axis, and is the resolved SNR (Schlegel et al. 2019)—the CSC does not extract all of the counts.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Color–color or color–flux figures aimed at identification of background objects using the (a) IRAC color–color plane of Allen et al. (2004) and Stern et al. (2007); (b) the IRAC 5.8 μ/3.6 μ-X-ray flux plane of Shalima et al. (2013); and (c) the IRAC color–color plane of Lacy et al. (2004). For (a), the colored boxes are approximate regions—e.g., source 4 + 5 is a galaxy and possible AGN, but appears in the top portion of the “stars” box; source 26 is a known SNR and appears in the lower portion of the “AGN” box. The black unlabeled point indicates a typical uncertainty. For (b), the gray horizontal line indicates the dividing 5.8/3.6 ratio that separates AGN (>1) from non-AGN. Source 26 is the known SNR S8 falling into “AGN territory.” For (c), the “AGN” box is defined in Lacy et al. (2004).
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: (a) Swift and Spitzer images of IC 1613. (a) Swift UVOT UWM2 view (gray scale) of IC 1613 with the Chandra coverage of IC 1613 indicated by the large black box. Detected Chandra sources are circled in red. White boxes indicate VLA detections; none of the VLA sources are labeled. Most of the VLA sources do not fall within the sky area covered by Chandra. Note that two VLA sources are also Chandra sources (4+5, 26). The cluster of galaxies is not labeled in this image but lies between sources 17 and 28. (b) Spitzer MIPS 24μ gray scale image of IC 1613 with the Chandra sources overlaid. The white space in the upper left corner indicates the edge of the MIPS field of view. Every source has a detectable flux (Table 9).
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Extracted X-ray spectra (black points) in a low-energy band (left half) where diffuse emission should dominate, and in a high-energy band (right half) where the particle background dominates (red points). The bottom row presents the raw data, while the top row shows the data after scaling. All spectra were extracted using the same region in the northeast quadrant of the IC 1613 observation and the blank-sky background reprojected to the IC 1613 coordinates. The rescaled, upper left plot shows the final result: a small difference (between the arrows) in the low-energy band that may represent weak, diffuse emission. We arrived at that plot starting with the lower row. The reprojected, prescale, high-energy blank-sky points (lower right) must then be multiplied by 0.69 to match the 11.5–13 keV count rates—this rescaling lowers the red points to match the black ones in that band and is shown in the upper right. We then apply the same correction to the prescale, low-energy band (lower left) to obtain our final result (upper left). See Section 7 for a discussion.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: (a) Fitted log N–log S distribution for the point sources in IC 1613. The black stepped line represents the data. The text discusses the break point energy near 10−14 erg s−1 cm−2. The thick red line is the fit above the break energy, but ignoring the three most luminous sources. The thick blue line includes all sources above the break energy. The thinner dashed lines represent the 16% and 84% uncertainty range on the fit parameters, and were generated by building a distribution based on the fit + uncertainty and fit—uncertainty values. This explains why the uncertainties appear to form an “X” on the fitted slope. See Section 6 for further discussion. (b) The corner plots for the log N–log S distribution: (b) the restricted range (left); (c) all points above the break energy (right).
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: (a) Comparison of our color–color results vs. those from the Chandra Source Catalog. (a) Side-by-side comparison of the (H–M)/B and (M–S)/B values for sources in common. The band definitions differ as described in the text in Section 4.2. The green arrows in each show the shift calculated for one source changing from the CSC to our band definition. (b) Side-by-side comparison of the color–color plane as measured by our analysis vs. the Chandra Source catalog (CSC) for those sources in common. The overall CSC values are largely shifted downward—attributable to the different definitions of the soft and medium bands.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Investigation of whether sources 4 and 5 constitute a single object: the upper row includes the Chandra data; the lower row includes the artificial source generated using the MARX software. The left column shows the raw data and generated source with no binning; the middle column displays the observed contours overlaid; the right column shows the PSF contours overlaid. Contour lines are at 0.01, 0.03, 0.05, and 0.07 as a fraction of the total counts in the image. The vertical arrow in the upper left is 20 arcsec in length. North is up and east is left for all panels. The generated source is completely consistent with the two wavdetect-ed sources.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Distribution of IC 1613's point sources in quantile space for an adopted spectrum of a (a) bremsstrahlung; (b) power law. Three categories of detected sources are shown (as presented in Table 8): the heavy lines indicate high signal-to-noise sources (S/N > 7.0); thin lines indicate moderate S/N (4.0 < S/N < 7.0); asterisks indicate weak S/N (S/N < 4.0). Weak sources are shown without an error for legibility; in all cases, the error bars would cover at least half the grid. The filled red square represents a “typical” AGN with power-law index = 1.8; the filled blue circle represents a “typical” low-mass XRB with a bremsstrahlung temperature of 7 keV. See Section 4.1 for details.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: Distribution of IC 1613's point sources in X-ray color–color space following Prestwich et al. (2003). See Section 4.2 for details. The power-law curve (red “+”) assumes a Galactic N H of 2 × 1020 cm−2. Higher values of N H pull the arc of points toward the center of the “Absorbed” circle. The known SNR lies just above the “SNRs” label.
Paper: The Nearby Dwarf Irregular Galaxy IC 1613 and Its Complex Bubble Region: Chandra and VLA Observations
Authors: E. M. Schlegel, C. K. Lacey, Thomas G. Pannuti, T. Lozinskaya, A. Moiseev
Figure caption: (a) Extracted spectrum of the galaxy cluster showing the best-fit model. The fit and contours in (b) were obtained from a simultaneous fit of the north and south spectra; the spectra were added solely for plotting purposes. (b) Confidence contours for the parameters N H and kT brems for the cluster.
Paper: Elemental Abundances of nearby M Dwarfs Based on High-resolution Near-infrared Spectra Obtained by the Subaru/IRD Survey: Proof of Concept
Authors: Hiroyuki Tako Ishikawa, Wako Aoki, Teruyuki Hirano, Takayuki Kotani, Masayuki Kuzuhara, Masashi Omiya, Yasunori Hori, Eiichiro Kokubo, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Akitoshi Ueda, Thayne Currie, Thomas Henning, Yui Kasagi, Jared R. Kolecki, Jungmi Kwon, Masahiro N. Machida, Michael W. McElwain, Takao Nakagawa, Sebastien Vievard, Ji Wang, Motohide Tamura, Bun'ei Sato
Figure caption: Comparison of different estimates of T eff as a function of the T eff−TIC, which we adopt for the abundance analysis. The orange filled circles present our estimates from the FeH lines in the IRD spectra (T eff−FeH). The other T eff shown by the purple open circles (T eff−Gmag), green plus signs (T eff−DR2), and red diamonds (T eff−AD) show the values of empirical estimates from absolute G-band magnitudes, those reported in Gaia DR2, and those calculated from angular diameters measured with interferometry, respectively. The black solid line shows the one-to-one relation. The orange dashed curve shows a quadratic fitting to the T eff−FeH.