adsabs/AstroCLIMB huggingface dataset:
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: The posterior distributions obtained after the burn-in phase of the adamet MCMC optimization process for the JAMcyl models applied to the K-short and K-long HSIM kinematics of NGC 3115 dw01. These simulations were generated using the JAMcyl models and feature three MBH: = 0 M⊙ (left), =3.5 × 104M⊙ (middle), and =7 × 104M⊙ (right). Each red-square panel presents a set of four parameters (i, MBH, M/LF814W, and βz), depicted as scatterplots illustrating their projected 2D distributions and histograms displaying their projected 1D distributions. In the top-right corner are inset maps that depict the Vrms values. The top maps represent the simulated kinematic maps extracted from the simulated data cubes, while the bottom maps represent the kinematic maps recovered from the best-fit JAMcyl model. These maps visually illustrate the level of agreement or disagreement at each spaxel between the simulated data and our best-fit model. The determination of the best-fit JAMcyl model is based on the PDF with the highest likelihood.
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: The posterior distributions obtained after the burn-in phase of the adamet MCMC optimization process for the JAMcyl models applied to the H-high HSIM kinematics of NGC 300. These simulations were generated using the JAMcyl models and feature three MBH: 0 M⊙ (left), 5 × 103M⊙ (middle), and 104M⊙ (right). Each red-square panel presents a set of four parameters (i, MBH, M/LF814W, and βz), depicted as scatterplots illustrating their projected 2D distributions and histograms displaying their projected 1D distributions. In the top-right corner, there are inset maps that depict the Vrms values. The top maps represent the simulated kinematic maps extracted from the simulated data cubes, while the bottom maps represent the kinematic maps recovered from the best-fit JAMcyl model. These maps visually illustrate the level of agreement or disagreement at each spaxel between the simulated data and our best-fit model. The determination of the best-fit JAMcyl model is based on the PDF with the highest likelihood.
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: The posterior distributions obtained after the burn-in phase of the adamet MCMC optimization process for the JAMcyl models applied to the J, H, and K HSIM kinematics of NGC 3115 dw01. These simulations were generated using the JAMcyl models and feature three MBH: = 0 M⊙ (left), =3.5 × 104M⊙ (middle), and =7 × 104M⊙ (right). Each red-square panel presents a set of four parameters (i, MBH, M/LF814W, and βz), depicted as scatterplots illustrating their projected 2D distributions and histograms displaying their projected 1D distributions. In the top-right corner are inset maps that depict the Vrms values. The top maps represent the simulated kinematic maps extracted from the simulated data cubes, while the bottom maps represent the kinematic maps recovered from the best-fit JAMcyl model. These maps visually illustrate the level of agreement or disagreement at each spaxel between the simulated data and our best-fit model. The determination of the best-fit JAMcyl model is based on the PDF with the highest likelihood.
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: The posterior distributions obtained after the burn-in phase of the adamet MCMC optimization process for the JAMcyl models applied to the K-short and K-long HSIM kinematics of NGC 300. These simulations were generated using the JAMcyl models and feature three MBH := 0 M⊙ (left), =5 × 103 M⊙ (middle), and =104 M⊙ (right). Each red-square panel presents a set of four parameters (i, MBH, M/LF814W, and βz), depicted as scatterplots illustrating their projected 2D distributions and histograms displaying their projected 1D distributions. In the top-right corner are inset maps that depict the Vrms values. The top maps represent the simulated kinematic maps extracted from the simulated data cubes, while the bottom maps represent the kinematic maps recovered from the best-fit JAMcyl model. These maps visually illustrate the level of agreement or disagreement at each spaxel between the simulated data and our best-fit model. The determination of the best-fit JAMcyl model is based on the PDF with the highest likelihood.
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: The posterior distributions obtained after the burn-in phase of the adamet MCMC optimization process for the JAMcyl models applied to the J, H, and K HSIM kinematics of NGC 300. These simulations were generated using the JAMcyl models and feature three MBH: = 0 M⊙ (left), =5 × 103M⊙ (middle), and =104M⊙ (right). Each red-square panel presents a set of four parameters (i, MBH, M/LF814W, and βz), depicted as scatterplots illustrating their projected 2D distributions and histograms displaying their projected 1D distributions. In the top-right corner are inset maps that depict the Vrms values. The top maps represent the simulated kinematic maps extracted from the simulated data cubes, while the bottom maps represent the kinematic maps recovered from the best-fit JAMcyl model. These maps visually illustrate the level of agreement or disagreement at each spaxel between the simulated data and our best-fit model. The determination of the best-fit JAMcyl model is based on the PDF with the highest likelihood.
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: Comparison between the input IMBH masses used for the HARMONI simulations and the recovered masses from the JAMcyl fits. The points show the median recovered MBH across all six gratings for each input mass. Error bars represent the 3σ confidence interval (0.14th to 99.86th percentiles from the MCMC chains, see Tables 8 and 9. The dashed line indicates perfect recovery (MBH,recovered = MBH,input). In this log–log scale plot, the (0, 0) coordinates are replaced by (100, 100).
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: Relaxation time trelax(r) as a function of radius for the NSC models of NGC 300 (red solid line) and NGC 3115 dw01 (blue solid line), assuming no central IMBH. The vertical dashed–dotted lines indicate the effective radii (Re) of the respective NSCs.
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: Same as Figure 12 but for the H-high HSIM kinematics of NGC 3115 dw01 with three MBH: 0 M⊙ (left), 3.5 × 104 M⊙ (middle), 7 × 104 M⊙ (right).
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: The distribution of the absolute value of the best-fit peak brightness slope S ratioed to its uncertainty ΔS vs. mean peak flux for the 450 (left) and 850 μm (right) sources in M17. The dashed horizontal line in both panels indicates where ∣S/ΔS∣ = 3, indicating the threshold for linear variability reliability as defined by D. Johnstone et al. (2018). Bright 450 and 850 μm sources with ∣S/ΔS∣ > 3 are highlighted by circles. In the 850 μm plot, only one bright source, JCMTPP J182023.2, has a value of ∣S/ΔS∣ much higher than the threshold.
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: Left panels: scatter plot of measured SD of peak brightness vs. measured mean peak brightness for all 450 μm (top row) and 850 μm sources (bottom row) in M17. The orange dashed curve denotes the fiducial SD, SDfid, for the expected uncertainty in the peak brightness of JCMT-SCUBA2 sources. Right panels: the same as the left panels, but for the normalized SD of peak brightness (SD/SDfid). Here, the dashed orange line separates out the potential stochastic variables.
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: The distribution of ΔW2 vs. SD/σ for the YSO sample with ΔW2/σ(W2) > 3. The vertical dashed line indicates the commonly used threshold value of SD/σ = 3 for identifying variable sources.
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: The spatial distribution of mid-IR and submillimeter variable candidates classified in this work, overlaid on the 850 μm map of M17. The contours of 850 μm continuum emission are in levels of 0.15, 0.6, 1.8, 3.6, 6.0, 9.0, 1.26, and 1.68 Jy beam−1. Circles, squares, and “X” represent different classification types for YSOs, i.e., Class I, Class II, and uncertain, respectively. The star symbol represents the linear variable at 850 μm (JCMTPP_J182023.2).
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: VPHAS g-band image of M17, overlaid with 850 μm dust continuum contours (in levels 0.3, 0.6, 1.8, 3.6, 6.0, 9.0, 1.26, and 1.68 Jy beam−1) from JCMT-SCUBA2. The optically bright nebula in M17 is labeled as the M17 H II region, while the northern and southwestern clouds are labeled as M17 North and M17 SW, respectively.
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: JCMT-SCUBA2 coadded 450 (left) and 850 μm (right) maps for M17, overlaid with 450 μm dust continuum contours (in levels 1, 2, 6, 12, 20, 30, 42, and 56 Jy beam−1) and 850 μm dust continuum contours (in levels 0.3, 0.6, 1.8, 3.6, 6.0, 9.0, 1.26, and 1.68 Jy beam−1).
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: The same as Figure 8, but for the mid-IR WISE W2 map in gray scale. The contours of the 850 μm continuum emission are the same as in Figure 8 but are displayed as blue.
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: Comparison of the FAPs for linear and periodic fits for the same YSO as in Figure 6. The vertical dashed line represents a FAP value of 10−4 for a linear fit, while the horizontal dashed line represents a FAP value of 10−2 for an LSP fit.
Paper: Submillimeter and Mid-infrared Variability of Young Stellar Objects in the M17 H II Region
Authors: Zhiwei Chen, 志维 陈, Doug Johnstone, Carlos Contreras Peña, Jeong-Eun Lee, Sheng-Yuan Liu, Gregory Herczeg, 雷歌 沈, Steve Mairs, Geumsook Park, Kee-Tae Kim, Mi-Ryang Kim, Keping Qiu, Yao-Te Wang, Xu Zhang, Megan Reiter
Figure caption: The 850 μm light curve of the candidate linear variable JCMTPP_J182023.2. The blue dashed lines represent the upper and lower boundaries of ±2SDfid, where SDfid is the expected fiducial SD.
Paper: Spectroscopy of Free-floating Planetary-mass Objects and Their Disks with JWST
Authors: Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi
Figure caption: Complete NIRSpec and MIRI spectra of all eight targets dereddened by the extinction estimated through the model fitting along with the best-fit photospheric model from BT-Settl (F. Allard et al. 2012) scaled by the corresponding dilution factor (see text for details).
Paper: Exoplanet Atmospheric Refraction Effects in the Kepler Sample
Authors: Déreck-Alexandre Lizotte, Jason Rowe, James Sikora, Michael R. B. Matesic
Figure caption: Binned Kepler photometry (blue dots) for KOI populations above/below the period–radius valley (APRV/BPRV; top/bottom), with refraction simulations overlaid for 2, 4, 10, and 30 g mol–1. The black vertical lines indicate ingress and egress, between which all in-transit data has been excised for clarity. Contrary to expectations of the APRV population possessing inflated, low-molecular-weight atmospheres, the 2 g mol–1 model atmosphere poorly represents the binned APRV data and is instead better fit between the 4 and 10 g mol–1 models. The BPRV population behaves as we expected, being relatively flat throughout.
Paper: Spectroscopy of Free-floating Planetary-mass Objects and Their Disks with JWST
Authors: Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi
Figure caption: Comparison of spectra of two of our targets with spectra from objects of similar spectral type in the literature. The prominent molecular absorption features are highlighted. The spectra of the literature objects are resampled to match the resolution of our targets and are normalized to the flux at 1.5 μm.
Paper: Spectroscopy of Free-floating Planetary-mass Objects and Their Disks with JWST
Authors: Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi
Figure caption: Left: measurement of silicate index for the two targets in our sample that do not show excess emission above the photosphere in the mid-infrared. Both the spectra are corrected for extinction using the K. D. Gordon et al. (2023) relation and AV from Table 1. The vertical shaded regions of width 0.6 μm highlight the wavelength ranges used to fit the continuum (light gray) and the silicate absorption (dark gray). The orange dashed line and shaded region show the best linear fit to the continuum and the uncertainty, respectively. The black and red points mark the average flux at 9.0 μm. Right: silicate index as a function of spectral type for our two FFPMOs along with the index for dwarfs from G. Suárez & S. Metchev (2022). The error bars for the two FFPMOs indicate the range in silicate index when AV changes by ±1 mag. The black dashed curve is the median silicate index for bins of two spectral subtypes.
Paper: Spectroscopy of Free-floating Planetary-mass Objects and Their Disks with JWST
Authors: Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi
Figure caption: Shape and strength of the silicate emission feature of our FFPMOs with a disk (before and after dereddening) and a sample of brown dwarfs, T Tauri stars, and Herbig Ae/Be stars from I. Pascucci et al. (2009). The error bars indicate the upper and lower values for a change in AV of ±1 mag. In comparison, this shows that the silicates in the disk around FFPMOs are processed to a higher degree than their massive counterparts.
Paper: Spectroscopy of Free-floating Planetary-mass Objects and Their Disks with JWST
Authors: Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi
Figure caption: H-R diagram for our sample, in comparison with theoretical evolutionary tracks. The figure shows absolute J-band magnitude vs. effective temperature, both listed in Table 1. We overplot error bars assuming errors of ±100 K in temperature and ±10% in brightness. The evolutionary tracks are from ATMO 2020 models (M. W. Phillips et al. 2020) for 0.005 and 0.01 M⊙. The squares on the tracks mark ages of 1, 2, and 5 Myr, from top to bottom.
Paper: Spectroscopy of Free-floating Planetary-mass Objects and Their Disks with JWST
Authors: Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi
Figure caption: MIRI dereddened spectra normalized to the continuum estimated in the previous figure. We show only the 7–12.5 μm region to highlight the silicate emission feature and the diversity in its shape among our six objects with a disk.
Paper: Spectroscopy of Free-floating Planetary-mass Objects and Their Disks with JWST
Authors: Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi
Figure caption: MIRI spectra of our six targets with a disk presented individually in each panel dereddened using the AV values listed in Table 1. The linear fit to the continuum is shown as a red dashed line and the 0.5 μm wavelength windows used for the fit are shaded in gray. In the shorter wavelength range this was optimized to avoid any emission lines and/or the silicate feature.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Two sample heat plots showing the distribution of the goodness-of-fit statistic G  k  in temperature–gravity space. Darker colors correspond to lower values of G  k  and thus better model fits. The heat plot on the left corresponds to the top Sonora model fits to 2MASS J0036159+182110 (spectral type L4). The fit was reasonably well constrained in terms of model temperature and gravity, with the best model fit giving a temperature of 1700 K and a log(g) of 5.5. The heat plot on the right shows the top Sonora model fits to IPMS J013656.57+093347.3 (spectral type T2.5). This object is a member of the overluminous T family described in Section 6.4 because it is brighter in the J band than is typical for an object of type T2. The heat map shows that log(g) is poorly constrained by model fits to this deviant object.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Absolute J 2MASS magnitude vs. (J − K)2MASS color of all the sources in the sample with published parallaxes and IR spectral types. The data points are color coded by IR spectral type.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The SpeX spectrum (black) of each triangular H-band object is shown with its best-fit Sonora (blue dashed) and Phoenix (orange dashed) models, stacked in order of decreasing adjusted R 2. The first four digits of the R.A. coordinates of each object are given to the left. Reference spectra made by averaging all L3 and L6 objects from the sample are included at the bottom of the plot. The Phoenix models generally do a better job at fitting the H-band peak, while the Sonora models are generally better at fitting the K band. The right panel shows just the H band of each object (black) along with its absolute value fit (green) and parabolic fit (gray dashed).
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The SpeX spectrum (black) of each plateaued H-band object is shown with its best-fit Sonora (blue dashed) and Phoenix (orange dashed) models, stacked in order of decreasing adjusted R 2. The first four digits of the R.A. coordinates of each object are given to the left. A reference spectrum made by averaging all T0 and T1 objects from the sample is included at the bottom of the plot. The Phoenix models generally do a better job at fitting the H-band peak, although both models give generally poor fits through the H and K bands. The Phoenix fit for 0151 completely fails to converge to a meaningful answer, and thus is not included in the plot. The right panel shows just the H band of each object (black) along with its trapezoidal fit (green) and absolute value fit (gray dashed).
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The objects with triangular H-bands peaks are marked in red at the tops of plots of the Sonora (left) and Phoenix (right) model best-fit temperature vs. IR spectral type (top) and 2MASS J − K color (bottom). These objects are all L types and generally fall on the cooler end for their spectral types based on their Sonora temperatures. There is no apparent pattern according to their Phoenix temperatures. Objects in this family generally have red colors for their spectral type.