adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Wolf Approach to Constraining NIR Extinction Laws in the Corona Australis Molecular Cloud
Authors: Botao Jiang, 博韬 江, Jun Li, 军 李, Xi Chen, 曦 陈
Figure caption: Extinction maps of the CrA molecular cloud derived from VISIONS survey data, shown in J (top), H (middle), and KS (bottom) bands. Contour levels in the top panel begin at AJ = 1.2 mag with increments of 0.5 mag. The middle panel displays AH contours starting at 0.5 mag with 0.4 mag intervals, while the bottom panel shows ﹩{A}_{{K}_{S}}﹩ contours beginning at 0.3 mag with 0.4 mag step sizes.
Paper: Exploring the Wolf Approach to Constraining NIR Extinction Laws in the Corona Australis Molecular Cloud
Authors: Botao Jiang, 博韬 江, Jun Li, 军 李, Xi Chen, 曦 陈
Figure caption: Wolf diagram showing the logarithmic cumulative frequency measured in the low-extinction region (284﹩\mathop{.}\limits^{\unicode{x000b0}}﹩84 ≤ R.A. ≤ 285﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1, −36﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 ≤ decl. ≤ −36﹩\mathop{.}\limits^{\unicode{x000b0}}﹩25). Bin size is 0.2 mag. The red lines indicate the best-fit lines using Equation (2). Slopes of bJ = bH = 0.31 ± 0.01 mag−1 for the J and H bands, and ﹩{b}_{{K}_{S}}=0.32\pm 0.01﹩ mag−1 for the KS band are derived, all measured within the magnitude range of 14.0–18.0 mag.
Paper: Exploring the Wolf Approach to Constraining NIR Extinction Laws in the Corona Australis Molecular Cloud
Authors: Botao Jiang, 博韬 江, Jun Li, 军 李, Xi Chen, 曦 陈
Figure caption: Spatial distribution of extinction ratios AJ/AH (top) and ﹩{A}_{H}/{A}_{{K}_{S}}﹩ (bottom) derived from the extinction measurements presented in Figure 3. Contours represent optical depth at 1 THz (τ1THz) for the CrA molecular cloud from A. Singh & P. G. Martin (2022) based on Herschel observations, starting at a level of 0.001 with increments of 0.001.
Paper: Exploring the Wolf Approach to Constraining NIR Extinction Laws in the Corona Australis Molecular Cloud
Authors: Botao Jiang, 博韬 江, Jun Li, 军 李, Xi Chen, 曦 陈
Figure caption: Evolution of NIR extinction ratios AJ/AH (top) and ﹩{A}_{H}/{A}_{{K}_{S}}﹩ (bottom) over time for four dust models based on (C. W. Ormel et al. 2011): silicate and graphite without ice (blue), ice-coated silicate and graphite (red), ice-coated silicate with uncoated graphite (green), and ice-coated silicate with graphite inclusions (purple). While ice-free compositions maintain stable ratios, ice-coated models show significant decreases in extinction ratios over timescales of 0.1–10 Myr, demonstrating how ice mantles affect grain growth and observable extinction properties.
Paper: Exploring the Wolf Approach to Constraining NIR Extinction Laws in the Corona Australis Molecular Cloud
Authors: Botao Jiang, 博韬 江, Jun Li, 军 李, Xi Chen, 曦 陈
Figure caption: Relationship between maximum grain size (﹩{a}_{{\rm{\max }}}﹩) and NIR extinction ratios for a mixture of silicate and graphite grains with a power-law size distribution (dn/da ∝ a−3.5) and minimum grain size ﹩{a}_{{\rm{\min }}}=0.005\,\mu {\rm{m}}﹩. Three extinction ratios are shown: AJ/AH (blue), ﹩{A}_{H}/{A}_{{K}_{S}}﹩ (green), and ﹩{A}_{J}/{A}_{{K}_{S}}﹩ (red). All ratios systematically decrease as maximum grain size increases from 0.1 to 1.0 μm, providing a theoretical framework for interpreting observed variations in extinction properties across the CrA cloud.
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: Parts of the simulated spectra over six HSIM data cubes, which are fixed as the best spectral wavelength ranges for measuring the stellar kinematics for NGC 300 and NGC 3115 dw01, including λ2.28–2.40 μm for both the K- and K-long, λ1.45–1.74 μm for both the H- and H-high, and λ1.16–1.218μm for the J- and λ2.05–2.20 μm for K-long, specifically. For the fixed spectra parts of the K- and K-long bands, we used the CO absorption bandheads (e.g., 12CO(2–0) λ2.293 μm, 12CO(3–1) λ2.312 μm, 12CO(4–2) λ2.351 μm, and 12CO(5–3) λ2.386 μm; L. Wallace & K. Hinkle 1997). For the fixed spectra parts of the H and H-high bands, we used the atomic-absorption species of Mg Iλ1.487, 1.503, 1.575, 1.711 μm; Fe Iλ1.583 μm; Si Iλ1.589 μm and the CO-absorptions lines of 12CO(3–0) λ1.540 μm; 12CO(4–1) λ1.561 μm; 12CO(5–2) λ1.577 μm; 12CO(6–3) λ1.602 μm; 12CO(7–4) λ1.622 μm; 12CO(8–5) λ1.641 μm. For the fixed spectrum part of the J band, we used the atomic-absorption species of Ti Iλ1.1896, 1.1953 μm; Si Iλ1.1988, 1.1995, 1.2035, 1.2107 μm; Mg Iλ1.1831, 1.2087 μm; and Fe Iλ1.1597, 1.1611, 1.1641, 1.1693, 1.1783, 1.1801, 1.1887, 1.1976 μm. For the fixed spectrum part of the K-short band, we used the atomic-absorption lines of Fe Iλ2.088, 2.070 μm; S Iλ2.188, 2.183, 2.179, 2.137, 2.092, 2.062 μm; and the blended-absorption features of Fe I—S I at λ2.070, λ2.083 μm. In each panel plot, the black vertical thin-dashed lines indicate the positions of atomic/molecule absorptions features of the stellar component extracted from one bin (black line) and its best-fit model produced by pPXF (red line). The two gray-vertical lines limit the wavelength range where the spectrum was fit, and blue dots show the residual between the galaxy spectrum and the best-fitting model (data-model). The kinematic results of these pPXF fits are shown in Figures 8 and 10 for NGC 300 and Figures 9 and 11 for NGC 3115 dw01 in terms of the 2D maps.
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: Atlas of the central surface-mass density (Σ, three top-row panels) and projected velocity dispersion (σp), the three middle-row and bottom-row panels) profiles resolved deeply into the resolvable region of HARMONI, which are predicted by various values of the Sérsic index (nSer) and the core inner slope (γ) of the isotropic core-Sérsic model. These theoretical profiles can be used to describe the qualitative behavior of the σp of stellar systems spanning from galaxies to NSC. For illustration, the values of Σ and σp were normalized to approximate the median values of the mass and radii of NSC (see text). We utilized three different Sérsic indices—including the low nSer = 0.5 (corresponding to the Gaussian profile), intermediate nSer = 2, and high nSer = 8 of the Sérsic index value—and two different values of the core inner slope: γ = 0 (green line) and γ = 0.2 (purple line). To illustrate the effects of central IMBHs having at the central region of the projected velocity-dispersion profiles, we modeled with three different BH masses: MBH = 0% of MNSC (no BH, yellow line), MBH = 0.5% of MNSC (or MBH = 8 × 103M⊙, red line), and MBH = 1% of MNSC (or MBH = 1.6 × 104M⊙, blue line). The two vertical dashed lines represent the break radius (Rb, inner line) and the effective radius (Re, outer line) of the NSC’s isotropic core-Sérsic model. The core inner slope γ control the inner behavior of the central surface-mass density and the projected velocity-dispersion profiles, while the Sérsic index describes the outer profile.
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: Stellar kinematic maps (V, σ⋆, and Vrms) for the nucleus of NGC 300, derived from mock HARMONI H-high IFS observations. The simulations were performed using HSIM  (S. Zieleniewski et al. 2015), based on input kinematics generated with JAMcyl models (M. Cappellari 2008) assuming three different central BH masses: MBH = 0  M⊙ (top row), 5 × 103 M⊙ (middle row), and 104 M⊙ (bottom row). Kinematics were extracted from the simulated noisy data cubes using pPXF  (M. Cappellari 2023), fitting the H-band spectral range λ1.45–1.74 μm. Contours represent isophotes from the collapsed data cube, spaced by 1 mag arcsec−2. The color bars are fixed across the rows to facilitate comparison and illustrate the kinematic impact of the central IMBH. The results demonstrate HARMONI’s capability to detect IMBH kinematic signatures in 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: The stellar kinematic maps of NGC 3115 dw01 extracted from the spectral part of λ2.28–2.40 μm (K and K-long band), λ2.05–2.20 μm (K-short band), λ1.15–1.22 μm (H band), and λ1.15–1.22 μm (J band) HSIM IFS produced from JAMcyl (M. Cappellari 2020) using pPXF  (M. Cappellari 2023). In each red rectangular, these maps are present with three MBH := 0M⊙ (first row), =3.5 × 104M⊙ (second row), and =7 × 104M⊙ (third row). On each row, the kinematic maps are listed in order with V, σ⋆, and Vrms. The contours indicate the isophotes from the collapsed HSIM IFS cubes spaced by 1 mag arcsec−2. The color bars are fixed at the same scale for all three MBH to illustrate the kinematic effects of the central BHs and also indicate the robustness of our proposed kinematic measurements at the centers of these dwarf galaxies hosting bright NSCs as the kinematic signatures for IMBHs.
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 stellar kinematic maps of NGC 300 extracted from the spectral part of λ2.28–2.40 μm (K and K-long band), λ2.05–2.20 μm (K-short band), λ1.15–1.22 μm (H band), and λ1.15–1.22 μm (J band) HSIM IFS produced from JAMcyl (M. Cappellari 2020) using pPXF  (M. Cappellari 2023). In each red rectangular, these maps are present with three MBH := 0M⊙ (first row), =5 × 103M⊙ (second row), and =104M⊙ (third row). On each row, the kinematic maps are listed in order with V, σ⋆, and Vrms. The contours indicate the isophotes from the collapsed HSIM IFS cubes spaced by 1 mag arcsec−2. The color bars are fixed at the same scale for all three MBH to illustrate the kinematic effects of the central BHs and also indicate the robustness of our proposed kinematic measurements at the centers of these dwarf galaxies hosting bright NSCs as the kinematic signatures for IMBHs.
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: Upper panels: The HST/WFPC2 F814W surface brightness of NGC 300 (left) and NGC 3115 dw01 (right) constructed from IRAF ellipse are plotted in open black dots, while their best-fit core-Sérsic + pure-Sérsic surface brightness are plotted in purple solid-thick lines. Their best-fitting parameters are shown in the legends. Here, the core-Sérsic profile is plotted in a red-dashed line, while the pure-Sérsic profile is depicted in a red dotted line. For ﹩r\lt 0\mathop{.}\limits^{^{\prime\prime} }045﹩, these surface brightness are extrapolated to the 4 mas scale required for this IMBH survey’s imaging with MICADO (red solid-thin lines).For NGC 300, the vertical black line indicates the radius at which we combined the narrow-field HST/WFPC2 F814W data with the wide-field MPG/ESO 2.2 m WFI R-band data.Lower panels: The differences, data − model, between the IRAF ellipse surface brightness and their corresponding best-fit core-Sérsic + pure-Sérsic models illustrate the fit’s goodness.
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 upper panels present the estimated number of stars per 10 mas spaxel for the nuclei of NGC 300 (left) and NGC 3115 dw01 (right). The data points derived directly from the SB in Figure 5 are shown in black circles at their best-fit models are shown in red lines. The lower panels of the figure display the residuals, calculated as (data − mode), which provide a relative error in our estimation, helping to assess the accuracy of our calculations. The inner vertical solid line represents our spatially central regions of HARMONI simulations in Section 6.2 (﹩0\mathop{.}\limits^{^{\prime\prime} }4\times 0\mathop{.}\limits^{^{\prime\prime} }4﹩), while that same outer line illustrates the full spatial FOV of HARMONI at our chosen 10-mas spaxel survey (﹩2\mathop{.}\limits^{^{\prime\prime} }15\times 1\mathop{.}\limits^{^{\prime\prime} }54﹩; see S. Zieleniewski et al. 2015).
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: Left: The M⋆–MNSC relation for galaxies in which galaxy and NSC masses are available regardless of their Hubble types. The compilation of dynamical and spectroscopically modeled NSC masses from P. Erwin & D. A. Gadotti (2012), I. Y. Georgiev et al. (2016), C. Spengler et al. (2017), Y. Ordenes-Briceño et al. (2018), and R. Sánchez-Janssen et al. (2019). Right: The (MNSC, Re) distribution for galaxies in which their NSC’s mass and effective radius are available. The data are taken from C. J. Walcher et al. (2005), P. Côté et al. (2006), J. Rossa et al. (2006), P. Erwin & D. A. Gadotti (2012), M. A. Norris et al. (2014), I. Y. Georgiev et al. (2016), C. Spengler et al. (2017), V. F. Baldassare et al. (2022), and K. Fahrion et al. (2022).
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 8 but for NGC 3115 dw01 with three MBH := 0  M⊙ (first row), =3.5 × 104 M⊙ (second row), and =7 × 104 M⊙ (third row).
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: Multiwavelength maps for JCMTPP_J182023.2, collected from Herschel (70, 100, and 160 μm), the JCMT Transient Survey (450 and 850 μm), and the 1.3 mm continuum by ACA. The red cross denotes the position of the 22 GHz H2O maser source (S. L. Breen & S. P. Ellingsen 2011).
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 Transient Survey 850 μm (top) and NEOWISE W2 light curves (bottom) of SPICY 81957. The black and blue dashed lines in the JCMT Transient Survey light curve represent the mean peak flux and ±1σ boundaries.
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: Histograms of the fractional slopes determined by linear fit. The black and blue histogram shows the slopes of linear variables in the Gould belt and M17 SWex recovered by the JCMT Transient Survey, 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: The same as Figure 10 but for M17 MIR.
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 10 but for SPICY 82001.
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: SED of the linear variable JCMTPP_J182023.2. The best-fit graybody model is shown as the orange curve.
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: map of AV vs. spectral type of one of our targets (CHA1110-7633). The order of templates on the y-axis has no significance and they are only grouped according to their ages. The spectral types prefixed with “Y” and “F” indicate the young dwarfs and old field dwarfs, respectively. The color bar indicates the normalized 1/(χ2)2 value where the lowest χ2 corresponds to the brightest color. The blue colored marker denotes the best-fitting spectral type and AV with an uncertainty of 0.5 spectral subtype and 1 mag in extinction (see text for details). Right: NIRSpec spectra of the same object normalized to the flux at 1.5 μm overplotted with the best-fit template and extinction (blue) resampled to match the target resolution. The templates with ±0.5 subtype and ±1 mag in extinction are shown in different colors for comparison.
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: A K − 4.5 μm color–magnitude diagram highlighting the location of our objects observed with JWST along with the distribution of low-mass members from the σ Orionis (B. Damian et al. 2023b) and Chamaeleon I (T. L. Esplin et al. 2017) star-forming regions of a similar age. The magnitudes are in absolute scale, transformed using their respective extinction and distance to the cluster (see Table 1 for values). The black and red curves show the 2 Myr isochrones from I. Baraffe et al. (2015) and M. W. Phillips et al. (2020), respectively. Masses corresponding to the K-band magnitudes are on the right.
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: Observed spectra of all the eight objects with JWST NIRSpec (green) and MIRI (orange) normalized to the flux at 2.5 μm. Published photometry at near-infrared (red) and mid-infrared (blue) wavelengths is overplotted.
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: NIRSpec spectrum of UHWJ247.95-24.78 overplotted with the three best-fitting photospheric models reddened and scaled by the corresponding AV and radius as indicated. The wavelength range considered for the comparison is highlighted by the shaded region. We find that the object fits best with the model spectra for an effective temperature of 1900 K and AV of 3 mag.
Paper: Exoplanet Atmospheric Refraction Effects in the Kepler Sample
Authors: Déreck-Alexandre Lizotte, Jason Rowe, James Sikora, Michael R. B. Matesic
Figure caption: Corner plots of MCMC posteriors corresponding to the KOI populations APRV/BPRV (left/right), from which samples were drawn for Figure 2. The sampled parameters are the zero-point (z) and mean molecular weight (μ). The dashed lines correspond to a 1σ error. The posterior of μ associated with the APRV population implies a small, but detectable refraction effect consistent with an optically thin atmosphere lighter than Earth’s but heavier than the expected H/He dominated atmosphere. The posterior of μ associated with the BPRV population implies that when it comes to refraction effects, a much heavier atmosphere is essentially indiscernible from the lack of an atmosphere.
Paper: Exoplanet Atmospheric Refraction Effects in the Kepler Sample
Authors: Déreck-Alexandre Lizotte, Jason Rowe, James Sikora, Michael R. B. Matesic
Figure caption: Kepler photometry (blue dots) for the same above/below (top/bottom) period–radius valley KOI populations as in Figure 1. Overlaid in solid red lines are 100 models interpolated from RETrO using MCMC posteriors of the zero-point (z) and mean molecular weight (μ); associated corner plots given in Figure A1.
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 of KOI populations above/below the period–radius valley (top/bottom) with/without (red/blue dots) injected refraction signature (solid red line). Prior to binning, a random sample of 300 light curves were injected with a simulated refraction effect—limited to a maximum flux increase of ∼10 ppm—in order to assess its significance across the out-of-transit photometry. To protect against the potential for in-transit data to contaminate the out-of-transit refraction signal near ingress/egress by means of Kepler’s 30 minutes cadence, we exclude data within ±0.1 T14 from ingress/egress accordingly.
Paper: Exoplanet Atmospheric Refraction Effects in the Kepler Sample
Authors: Déreck-Alexandre Lizotte, Jason Rowe, James Sikora, Michael R. B. Matesic
Figure caption: Above/below (gray/black) period–radius valley KOI populations used in the binning process with colored lines representing various atmospheric escape limits. KOIs below any given lines may viably retain atmospheres of corresponding compositions. Here, the cyan line corresponds to the power law relation between insolation and escape velocity as detailed in K. J. Zahnle & D. C. Catling (2017). Solar system planets are also shown for reference. KOI parameters have been updated according to J. J. Lissauer et al. (2024).