adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: Comparison of the redshift, z (left), bolometric luminosity (middle), and the Eddington ratio (right) distribution of the various samples with dust lag measurements along with our initial sample are shown in an empty magenta colored histogram, while the final sample of sources with reliable lag measurement in this work is shown in a filled histogram (see details in Section 3).
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: The light curves of two objects of our sample viz, 105007.75+113228.6 (top) and 141700.82+445606.3 (bottom), where the left panel shows the calibrated unbinned (with lower contrast) and binned optical light curves (upper) and IR light curves for the W1 (middle) and W2 (bottom) bands, respectively. In the lower two panels of the light curves, the optical light curve has been scaled and shifted by the lags found by ICCF. The right panel illustrates the transfer function and the lag distribution found by employing MICA and the CCF and CCCD found by ICCF.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: The comparison of dust lag after correction for accretion disk contribution (y-axis) vs. before (x-axis). The one-to-one slope is marked by the dashed blue line along with our best fit shown by the dashed red line, which closely matches that obtained by A. K. Mandal et al. (2024) represented by the dashed green line.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: Comparison of BLR and dust torus sizes in W1 (left) and W2 (right) bands. Our measurements are shown as circles, while the squares represent the measurements from Y.-J. Chen et al. (2023). A one-to-one line is shown for reference.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: Luminosity–redshift density map of the total number of objects selected from S. Rakshit et al. (2020) within redshift z < 0.8, SNR > 10, and g-magnitude < 17. The final sample of 146 objects selected for lag analysis is shown as white dots.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: Comparison of the W1 and W2 lags after redshift corrections. The dashed black line represents the best fit, while the 1:1 relation is shown by the dashed blue line.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: Comparison of the lags estimated by ICCF and MICA. The dashed black line shows a 1:1 relation. The measured lags show good agreement with the 1:1 relation with an intrinsic scatter of ∼0.158 dex.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: Multiwavelength light curves of the Cepheid variable stars HV2324 (left panel) and HV2854 (right panel) in the LMC, with periods of 14.4657 and 8.6348 days, respectively, are presented. The data were obtained using the Three-hundred MilliMeter Telescope (TMMT; Monson et al. 2025, in preparation), the 1 m Swope and 2.5 m duPont telescopes (S. E. Persson et al. 2004), and the Spitzer Space Telescope (V. Scowcroft et al. 2011), covering optical, NIR, and mid-IR wavelengths, respectively. The light curves are represented by circled dots and have been phase-folded using the Lightkurve algorithm (Lightkurve Collaboration et al. 2018). The solid black dots correspond to the smoothed, uniformly distributed phase-magnitude data generated using the GLOESS method, as described in the Appendix.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: The time-averaged period–luminosity (PL) for LMC Cepheid stars across multiple wavelengths are presented. A trend is observed with the dispersion visibly decreasing from optical to infrared wavelengths, as highlighted by the solid black lines flanking the dashed fitted lines. The solid lines, representing the 2σ limits, indicate the intrinsic width of the PL relation arising from the instability strip. The slopes and intercepts of the fitted lines were adopted from B. F. Madore & W. L. Freedman (2011).
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: The left panel presents the scatterplot of residuals derived from the PL relation in the J and B filter bands. The right panel depicts the residuals from the fitted lines of the period–magnitude and magnitude–magnitude relations. Both plots exhibit linear relationships, with slopes calculated using a gradient descent algorithm. The error bars indicate errors introduced by the addition of a random phase.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: PL relations in the J band shown for single-epoch, time-averaged, and corrected data. The scatter of the PL relations decreases, demonstrating the transition from random-phase data to corrected data, which closely approximates time-averaged data. The dashed lines represent the fitted line using the slope provided by B. F. Madore & W. L. Freedman (2011) and the trained intercepts derived in this work. The solid lines indicate a 1σ dispersion around the dashed line.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: Distribution of the standard deviation of residuals from the PL-fitted line before (red) and after (blue) applying the random-phase correction. As expected with a sufficiently large sample size, both distributions follow a Gaussian shape. The standard deviation decreases from 0.212 to 0.152 mag after the correction.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: The correlation of ﹩{\rm{\Delta }}R(\mathrm{log}{R}_{{\rm{obs}}}-\mathrm{log}{R}_{{\rm{best}}-{\rm{fit}},{\rm{slope}}=0.5})﹩ with Eddington ratio for W1 band (left) and W2 band (right). The measurements from this work are shown as red points, while the blue points are from A. K. Mandal et al. (2024).
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: The correlation of ΔR with Eddington ratio for W1 band in different bins of redshift and bolometric luminosity for the combined sample (this work and A. K. Mandal et al. 2024) in the top and bottom panels, respectively.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: From left to right panels: distributions of the coefficients and intercept derived from Equation (9) across 1000 experiments using random-phase data. All distributions exhibit Gaussian behavior, allowing for the precise determination of the coefficients and intercept.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: Pair plots present the residuals from the PL-fitted line on the y-axis and the residuals from the magnitude–magnitude fitted line on the x-axis across all bands. It reveals significant correlations between these distinct residuals for each pair of bands. As shown in Figure A2, the primary focus is on the J and B bands, which demonstrate a notable correlation in the (1, 4) subplot based on matrix indices. The region corresponding to the combination of infrared (IR) filters is shown in more detail in Figure A4.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: Pair plots illustrate the correlation between residuals from two different bands, both derived from the PL-fitted line. A notable correlation is evident among the residuals, particularly for consecutive filter bands. This study primarily focuses on the J and B bands, which, despite their distinct wavelengths, demonstrate a strong correlation in the (1, 4) subplot as indicated by the matrix indices.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: Pair plots of magnitude–magnitude in different bands show that consecutive filter bands exhibit correlations. The solid line represents the fitted data, and the dashed line indicates a 1σ dispersion. Notably, dispersion tends to be lower when bands are closer in wavelength. The slopes of all the fitted lines are pretty similar, while the intercepts show significant variations.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: Enlarged view of the region in Figure A3 corresponding to combinations of infrared (IR) bands, illustrating the residual correlations between PL- and magnitude–magnitude-fitted relations. Axis limits have been rescaled relative to Figure A3 to enhance the visibility of structural features in the distributions.
Paper: Mitigating Random-phase Sampling Noise in the Cepheid Period–Luminosity Relation: A Cross-filter Consistency Approach
Authors: Mahdi Abdollahi, Atefeh Javadi, Barry F. Madore, Wendy L. Freedman, Hamidreza Mahani
Figure caption: Similar to Figure 2, but presented as separate figures. Each figure includes the slope and intercept of the fitted line, along with dispersion information represented by 2σ solid black lines.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: The caustic diagram of the Coma cluster members, along with position of all cE galaxies from our sample (pink stars) and the selected infalling cE galaxies (additionally marked by numbers according to Table 1), shows possible trajectories for varying angular momentum (L). Each trajectory has timestamps. For galaxy CcGV1 (#3) , the timestamp is 75 Myr; for galaxy cEJ1252+2735 (#11), it is 500 Myr; and for galaxies cEJ1303+2800 (#12) and GMP1993 (#13), it is 200 Myr. Solid lines represent trajectories at the maximum possible distance, while dotted lines correspond to the minimum possible (projected) distance for a given L.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: The size–luminosity (J. Kormendy 1977) and the surface brightness–luminosity relations of ETGs and CCSs. cEs from our sample are shown by pink stars. The sources of other galaxies are shown in the legend below the plots. The gray-filled areas and dashed lines denote the parameter space from Section 4.1. References: R. Bender et al. 1992; I. V. Chilingarian 2009; M. Geha et al. 2003; S. de Rijcke et al. 2005; I. V. Chilingarian et al. 2008b; N. F. Martin et al. 2016; M. Yagi et al. 2016; A. W. McConnachie 2012; E. A. Evstigneeva et al. 2007; I. V. Chilingarian et al. 2011; S. G. Djorgovski et al. 1997; P. Martini & L. C. Ho 2004; I. V. Chilingarian & G. A. Mamon 2008.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: The position of cE galaxies from our sample in the Coma cluster. Galaxies from J. Price et al. (2009) are marked as pink squares, and one galaxy from I. Chilingarian et al. (2009) and A. M. Cody et al. (2009) is marked as a red square.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: Profiles of the velocity (v), velocity dispersion (σ), age, and metallicity for GMP3424 (top) and GMP3511 (bottom) inferred with PEGASE-HR SSP models for masks' 2D spectra in Coma_dE2a and ComaA slit masks (black and green points, respectively). Legend insets contain information about the position angle (PA) of the slit and S/N. Panels with velocity (v) profiles (top) also show bell-shaped profiles of the mean flux extracted from the slit (gray and green lines).
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: Relations between stellar velocity dispersion (σ, top panel), metallicity ([Z/H], bottom panel), and absolute magnitude in the B band (MB) of ETGs and CCSs. cEs from our sample are shown as pink stars. The sources of other galaxy types are indicated in the legend. References: A. W. McConnachie 2012; I. V. Chilingarian et al. 2008b; I. V. Chilingarian et al. 2011.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: Color–magnitude diagram for all Coma cluster members from DESI DR1, including cE galaxies described in the literature and galaxies from our sample.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: Distribution of redshifts for galaxies that satisfy initial criteria plus μe,g and n constraints.
Paper: A Multiwavelength View of the Multimessenger Sources NGC 1068 and PKS 1502+106
Authors: Abhishek Desai, Stefano Marchesi, Justin Vandenbroucke, Indrani Pal, Ke Fang, Dieter Hartmann, Regina Caputo, Marco Ajello, Jessie Thwaites, Kavic R Kumar, Sam Hori
Figure caption: Joint-fit for the NICER +Chandra observation of NGC 1068 is shown here. The NICER observation is made on MJD:60314, and the Chandra observation was conducted on MJD:60313.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: An illustration of the estimation of full distances and full velocities. The purple line illustrates the freefall velocity (vff) profile at different full distances from the cluster center (r), while other lines represent possible full distances and velocities according to projected velocity and distance of the galaxies for zero angular momentum case.
Paper: A Multiwavelength View of the Multimessenger Sources NGC 1068 and PKS 1502+106
Authors: Abhishek Desai, Stefano Marchesi, Justin Vandenbroucke, Indrani Pal, Ke Fang, Dieter Hartmann, Regina Caputo, Marco Ajello, Jessie Thwaites, Kavic R Kumar, Sam Hori
Figure caption: Joint fits for the NICER +NuSTAR observations of PKS 1502+106 made on MJD:60005 (top plot) and MJD:60170 (bottom plot).
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: Measurements of Re with SourceXtractor++ applied to HSC-g images compared to the literature GALFIT measurements on HST data from C. Hoyos et al. (2011) and J. Price et al. (2009), along with a histogram of the relative differences between measurements.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: DESI spectra of cEs optimally extracted along the slit flux calibrated in Fλ units (black). Their best-fitting stellar population models (red), flux uncertainties (pink), and fitting residuals (gray). Galaxy names from Table 1 are shown in each panel. All data and best-fitting models are smoothed with the Savitzky–Golay filter for display purposes. The right panel illustrates the fit to the calcium triplet region.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: The 15″ × 15″ HST F814W cutouts for 10 cE galaxies in our sample do not display unambiguous globular cluster systems around them.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: Velocity dispersion measurements of DESI compared to RCSED1 (SDSS sample; I. V. Chilingarian et al. 2017) and DEIMOS (E. Kourkchi et al. 2012) measurements, along with histograms of the relative difference.
Paper: A Census of Compact Elliptical Galaxies in the Coma Cluster
Authors: Aleksandra V. Sharonova, Kirill A. Grishin, Igor V. Chilingarian, Gary A. Mamon, Nelson Caldwell, Daniel Fabricant
Figure caption: Possible values (filled) of dimensionless angular momentum (L) and total distance to the cluster center (r) for the four cEs in outer parts of the cluster.
Paper: A Multiwavelength View of the Multimessenger Sources NGC 1068 and PKS 1502+106
Authors: Abhishek Desai, Stefano Marchesi, Justin Vandenbroucke, Indrani Pal, Ke Fang, Dieter Hartmann, Regina Caputo, Marco Ajello, Jessie Thwaites, Kavic R Kumar, Sam Hori
Figure caption: The multiwavelength and multimessenger observations for NGC 1068 are shown with neutrino measurements from IceCube Collaboration et al. (2022; red shaded region). The observations shown here and derived using this study include: (1) The NICER (blue)+Chandra (orange) observed data are shown as data points, while the intrinsic flux Fint estimates and the corresponding 90% uncertainties derived from Section 2.3 are shown as the blue and orange shaded regions; (2). The Fermi-LAT observations are shown as green data points (note that the observed Fermi-LAT data are shown here and not the intrinsic measurements); and (3). The neutrino best-fit measurements, for three different neutrino source spectrum cases and derived using SkyLLH (see Table 3), are shown as a black data point for each case (Case 2: Top, Case 4: Middle, and Case 5: Bottom Plot). The extrapolated flux over 10 GeV to 10 TeV and the relevant uncertainty are also shown by a black dotted line with a gray shaded region. The theoretical model predictions from B. Eichmann et al. (2022) and K. Murase (2022) are also shown using dashed lines just for comparison.
Paper: A Multiwavelength View of the Multimessenger Sources NGC 1068 and PKS 1502+106
Authors: Abhishek Desai, Stefano Marchesi, Justin Vandenbroucke, Indrani Pal, Ke Fang, Dieter Hartmann, Regina Caputo, Marco Ajello, Jessie Thwaites, Kavic R Kumar, Sam Hori
Figure caption: The 2D likelihood profile of Epeak and nS for Case 3 and Case 5 is shown here, where the ΔTS = TSbestfit − TS(Epeak, nS) is derived for each combination of Epeak and nS. The white (dotted), gray (dashed), and black (solid) lines show the 68%, 90% and 95% contour regions, respectively.
Paper: A Multiwavelength View of the Multimessenger Sources NGC 1068 and PKS 1502+106
Authors: Abhishek Desai, Stefano Marchesi, Justin Vandenbroucke, Indrani Pal, Ke Fang, Dieter Hartmann, Regina Caputo, Marco Ajello, Jessie Thwaites, Kavic R Kumar, Sam Hori
Figure caption: Light Curve for PKS 1502+106 derived using the data collected by NICER (top panel), NuSTAR (middle panel), and Fermi-LAT (bottom panel) is shown here.
Paper: A Multiwavelength View of the Multimessenger Sources NGC 1068 and PKS 1502+106
Authors: Abhishek Desai, Stefano Marchesi, Justin Vandenbroucke, Indrani Pal, Ke Fang, Dieter Hartmann, Regina Caputo, Marco Ajello, Jessie Thwaites, Kavic R Kumar, Sam Hori
Figure caption: Light Curve for NGC 1068 derived using the data collected by NICER (top panel) and Fermi-LAT (bottom panel) is shown here. The X-ray observations are taken between 2023 March (MJD:60004) to 2024 February (MJD:60341), while the Fermi-LAT light curve is derived using 4 week time bin periods from 2022 March (MJD:59639) to 2025 March (MJD:60735).
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: Kiel diagram showing the effective temperatures and surface gravities derived in this study (blue circles), along with ASPCAP DR17 results for the same stars (gray xs). Physical ﹩{\mathrm{log}}g﹩ values computed using the relations in A. W. Mann et al. (2019) are shown as orange triangles. Typical uncertainties are shown at the top right. The DR17 ﹩{\mathrm{log}}g﹩ results are systematically lower than ours and roughly flat with the effective temperature.
Paper: A Multiwavelength View of the Multimessenger Sources NGC 1068 and PKS 1502+106
Authors: Abhishek Desai, Stefano Marchesi, Justin Vandenbroucke, Indrani Pal, Ke Fang, Dieter Hartmann, Regina Caputo, Marco Ajello, Jessie Thwaites, Kavic R Kumar, Sam Hori
Figure caption: The multiwavelength observations of PKS 1502+106 are shown (top: MJD:60005; and bottom: MJD:60170), with the neutrino limits derived using SkyLLH and the theoretical models of X. Rodrigues et al. (2021). No fitting is done in this case, and the models are shown only for comparison. The photon data includes NICER +NuSTAR + 1 week Fermi-LAT observations.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: A comparison between the derived effective temperatures from this work with results obtained with the ASPCAP pipeline from APOGEE DR17. The dashed lines represent offsets of ±100 K.
Paper: An Analysis of the Radius Gap in a Sample of Kepler, K2, and TESS Exoplanets Orbiting M-dwarf Stars
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Diogo Souto, I. Pascucci, Aida Behmard, C. Allende Prieto, Rachael L. Beaton, D. Bizyaev, S. Daflon, S. Hasselquist, Steve Howell, Steven R. Majewski, Marc Pinsonneault
Figure caption: The observed APOGEE spectrum and best-fit syntheses for two studied M dwarfs, covering the effective temperature range of our sample. From top to bottom: the first, second, and third chip of the APOGEE spectrum are shown.