adsabs/AstroCLIMB huggingface dataset:
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Matched filter response for the HD 100546 disk generated using Keplerian models with an outer radius of 300 au. Note the lines reaching the top of the y-axis have responses > 70σ.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. III. Detailed Imaging of the Nebular Environment around the HL Tau Disk
Authors: Camryn Mullin, Ruobing Dong, Jarron Leisenring, Gabriele Cugno, Thomas Greene, Doug Johnstone, Michael R. Meyer, Kevin R. Wagner, Schuyler G. Wolff, Martha Boyer, Scott Horner, Klaus Hodapp, Don McCarthy, George Rieke, Marcia Rieke, Erick Young
Figure caption: Comparing features in our data with observations taken at different wavelengths. In all panels the star is located at the center, and the stellar position from the other data sets were manually aligned. Top: (a) ALMA Partnership et al. (2015) millimeter continuum emission. (b) F200W residuals overlaid with ALMA contours to showcase the disk and gap locations. The disk is not visible to NIRCam. A notable hook-shaped clump is visible in our data at the edge of the outflow cavity. (c) F405N residuals overlaid with ALMA contours. Middle: (d) 0.6 μm HST data from PID9862 (log scaled). (e) Comparison to F200W. The c-shaped outflow cavity is broader at 2 μm. The white arrow points to the same hook-shaped clump seen in panel (b). (f) Comparison to F405N. The cavity is broader, and the upward stream is shifted west. Bottom: (g) ALMA HCO+ moment 0 map from Yen et al. (2019). (h) Comparison to F200W. The spiral is not clearly detected at this wavelength, but the NE protrusion in the ALMA data clearly aligns with the NIRCam outflow cavity. (i) Comparison to F405N. We detect a structure which appears to coincide with the HCO+ spiral.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. III. Detailed Imaging of the Nebular Environment around the HL Tau Disk
Authors: Camryn Mullin, Ruobing Dong, Jarron Leisenring, Gabriele Cugno, Thomas Greene, Doug Johnstone, Michael R. Meyer, Kevin R. Wagner, Schuyler G. Wolff, Martha Boyer, Scott Horner, Klaus Hodapp, Don McCarthy, George Rieke, Marcia Rieke, Erick Young
Figure caption: (a) NIRCam 5σ sensitivity limits for HL Tau as a function of separation from the central star. These values are only for regions with faint or no envelope detection. The edge of the disk—∼1″ as imaged by ALMA Partnership et al. (2015)—is represented by the vertical dashed–dotted gray line. The major disk gaps possibly hosting planets are plotted as vertical shaded regions. Due to saturation, only the 65–75 au gap is within our unmasked region. (b) Mass limits using BEX evolutionary track models when M p < 2 M J and AMES-COND models for larger masses. In the low envelope flux areas we reach limits as deep as 5.2 M J at the disk edge in the F405N filter (assuming the planets are 1 Myr old). Our deepest limits are ∼0.75 M J out to 4″. Points showing the approximate masses of the theoretically predicted planets are plotted in the major disk gaps to provide context.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. III. Detailed Imaging of the Nebular Environment around the HL Tau Disk
Authors: Camryn Mullin, Ruobing Dong, Jarron Leisenring, Gabriele Cugno, Thomas Greene, Doug Johnstone, Michael R. Meyer, Kevin R. Wagner, Schuyler G. Wolff, Martha Boyer, Scott Horner, Klaus Hodapp, Don McCarthy, George Rieke, Marcia Rieke, Erick Young
Figure caption: PSF-subtracted data for all four filters where color is in units of MJy sr−1. We utilize an annulus of inner radius 0.″2 for F187N and F200W, and 0.″4 for F405N. We use a larger 0.″8 mask for F410M—which suffers from high levels of saturation—to retain data in the outer envelope regions. The stellar envelope is the most prominent feature in our data. Negative spiral residuals out to a distance ∼ 1″ have been introduced by using MWC 758 as a PSF reference. In addition, we apply a mask to an artifact introduced in the NW direction of the long-wavelength images due to the presence of a background star in the MWC 758 data.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. III. Detailed Imaging of the Nebular Environment around the HL Tau Disk
Authors: Camryn Mullin, Ruobing Dong, Jarron Leisenring, Gabriele Cugno, Thomas Greene, Doug Johnstone, Michael R. Meyer, Kevin R. Wagner, Schuyler G. Wolff, Martha Boyer, Scott Horner, Klaus Hodapp, Don McCarthy, George Rieke, Marcia Rieke, Erick Young
Figure caption: Centered calints files for the four filters used where color is in units of MJy sr−1. Despite the point-spread function (PSF) not being removed yet, the stellar envelope is apparent at short wavelengths and is as bright as the PSF. The central saturation regions that extend out to 0.″1, 0.″2, and 0.″3 for the F200W, F405N, and F410M filters, respectively, are masked out. The F187N observations do not have a saturated center.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. III. Detailed Imaging of the Nebular Environment around the HL Tau Disk
Authors: Camryn Mullin, Ruobing Dong, Jarron Leisenring, Gabriele Cugno, Thomas Greene, Doug Johnstone, Michael R. Meyer, Kevin R. Wagner, Schuyler G. Wolff, Martha Boyer, Scott Horner, Klaus Hodapp, Don McCarthy, George Rieke, Marcia Rieke, Erick Young
Figure caption: Continuum-subtracted residuals for F187N (Paα) and F405N (Brα). The color bar units are arbitrary. The faint residuals shown in the left panel could indicate Paα accretion shocks in the disk region. There are also potential signs of Brα accretion in the disk, though it is fainter when compared with Paα.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. III. Detailed Imaging of the Nebular Environment around the HL Tau Disk
Authors: Camryn Mullin, Ruobing Dong, Jarron Leisenring, Gabriele Cugno, Thomas Greene, Doug Johnstone, Michael R. Meyer, Kevin R. Wagner, Schuyler G. Wolff, Martha Boyer, Scott Horner, Klaus Hodapp, Don McCarthy, George Rieke, Marcia Rieke, Erick Young
Figure caption: Example of how we inject signal and noise 1 PSF FWHM diameter circular apertures depending on the position angle of the injected planet. A companion injected in an area of low envelope flux will only utilize apertures in low flux regions as a means of accurately measuring the noise.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: Top two rows: DIS blue and red spectra of 0026+24, 0309+29, and 0548+53; Bottom two rows: DIS spectra of 0837+38, blue spectra from KOSMOS of 0750+66 and 2313+16, and Lick and DIS spectra of 2011+60.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: Best-fit sinusoids to the velocities of the objects listed in Table 2.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: ZTF light curve of 0026+24 (top), data folded on the orbital period showing the presence of an eclipse (middle) and the power spectrum showing the orbital period of 2.05 hr (bottom).
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: The eight spectra of 0026+24 obtained on 2018 December 4 with the DIS at APO and phased with the spectroscopic phasing.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: The ZTF light curve of 0548+53 in the g filter, showing the sporadic high and low states that are typical of polars.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: MCMC corner plot with the best-fit parameters (effective temperature, T eff; surface gravity, log g; radius, R; parallax, ω; and mass, M) derived with the best fit using the BT-Settl models for TWA 27B. The vertical lines show the 1σ uncertainties of each parameter as derived by the MCMC fitting.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Markov Chain Monte Carlo (MCMC) corner plot with the best-fit parameters (effective temperature, T eff; surface gravity, log g; radius, R; parallax, ω; and mass, M) derived with the best fit using the BT-Settl CIFIST models for TWA 28. The vertical lines show the 1σ uncertainties of each parameter as derived by the MCMC fitting.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: MCMC corner plot with the best-fit parameters (effective temperature, T eff; surface gravity, log g; radius, R; parallax, ω; and mass, M) derived with the best fit using the BT-Settl CIFIST models for TWA 27A. The vertical lines show the 1σ uncertainties of each parameter as derived by the MCMC fitting.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Upper panel: comparison between the 0.97 and 5.30 μm NIRSpec spectra of TWA 28 and TWA 27A. Bottom panel: ratio between the flux of TWA 28 and TWA 27A.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Best fit of the ATMO and BT-Settl CIFIST models to the TWA 28 2.0–5.20 μm spectrum. We highlight the main molecular absorptions present in this wavelength range.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Best fit of the ATMO and BT-Settl models to the TWA 27B 2.0–5.20 μm spectrum. We highlight the main molecular absorptions present in this wavelength range.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Best fit of the ATMO and BT-Settl CIFIST models to the TWA 27A 0.97–2.0 μm spectrum. We highlight the main atomic lines and molecular absorptions present in this wavelength range.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Best fit of the ATMO and BT-Settl CIFIST models to the TWA 27A 2.0–5.20 μm spectrum. We highlight the main molecular absorptions present in this wavelength range.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Best fit of the ATMO and BT-Settl models to the TWA 27B 0.97–2.0 μm spectrum. We highlight the main atomic lines and molecular absorptions present in this wavelength range.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The optical and near-IR color–magnitude diagram of the cluster under study. The curves are the isochrones of log(age) = 7.75, 7.8, and 7.85. These isochrones are taken from Marigo et al. (2017). Black circles are the probable cluster members identified in the present study, while the light-blue circles represent the matched stars with the Cantat-Gaudin et al. (2020) catalog.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Histogram representing the distribution of main-sequence stars within each specified magnitude bin, with M  G  denoting the absolute magnitude and red dots representing the associated errors.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Galactic orbit of the NGC 2345 estimated with the Galactic potential model described in the text in the time interval of the cluster’s age. The top-left panel shows a side view and the right panel shows a top view of the cluster’s orbit. The bottom panel shows the motion of NGC 2345 in the Galactic disk with time. The filled triangle and filled circle denote the birth and present-day position of the cluster in the Galaxy.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: AD diagram for cluster NGC 2345. All stars (1732) are probable members with a membership probability higher than 70%. A plus sign indicates the mean value of apex coordinates, described in the text.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The cumulative radial distribution of stars in different mass ranges. The orange dotted line, blue dashed line, and green dashed dot line correspond to the high-, intermediate-, and low-mass ranges, respectively. The mass ranges are mentioned in the upper left of the graph.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Plot of the histogram of parallax. The Gaussian function is fitted to the central bins and provides the mean value of parallax.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The plot of (V − K) vs. (J − K) color–color diagram. Solid and dashed lines are the ZAMS taken from Caldwell et al. (1993).
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The plot of (J − K) vs. (J − H) color–color diagram. Solid and dotted lines are the ZAMS taken from Caldwell et al. (1993).
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The mass function slope for NGC 2345 in three regions: core, halo, and cluster region. The slope of the mass function is calculated by least-squares fitting, as shown by solid lines in each panel.
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption: Summary of the results from the free chemistry retrieval of our HIP 65Ab IGRINS dayside data set. The left corner plot includes the posteriors of planetary and orbital parameters. log(Σ(VMR)) is the sum of the VMR of all the retrieved species (shown separately for clarity). log(P Cloud) is the (base 10) logarithm of the cloud-top pressure in units of bars. V rot is the retrieved rotational broadening of HIP 65Ab. log(α) is the model scaling factor used in the likelihood (Equation (3)). K  p  and V sys are the orbital parameters as described in Equation (1). The top middle panel is the retrieved vertical noninverted temperature profile of HIP 65Ab with a smoothing prior σ  s  = 350 K dex−2. The orange line is the median temperature profile while the darker and lighter orange shaded areas are the 1σ (68%) and 2σ (95%) regions, respectively. The 12 black points the pressure levels where temperature points are retrieved. The dark green dashed–dotted line is the condensation curve of MgSiO3. The blue and red curves represent the contribution functions for H2O and CO, respectively. The H2O probes around the 1 bar level, while the CO probes higher, around the 0.1 bar level. The right panels are the retrieved posteriors of the VMR of the fitted chemical species. The vertical lines represents the predicted thermochemical equilibrium abundance at 0.3 bar for a solar metallicity atmosphere with a uniform temperature profile of 1411 K (see Figure 4). The solid lines are from a model with solar C/O and the dashed lines are from a model with a C/O of 1. H2O and CO are well constrained while only upper limits are inferred on other molecules. The retrieved CO VMR is slightly below but consistent with the chemical equilibrium model. The H2O abundance lies between the solar C/O and C/O = 1 model predictions.
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption: Benchmarking of our analysis framework and comparison to WASP-77Ab. Here we show the H2O and CO abundances, and C/O retrieved for HIP 65Ab compared to IGRINS emission observations of WASP-77Ab from Line et al. (2021). Our analysis of the WASP-77Ab data (purple) well reproduces the molecular abundances and C/O reported by Line et al. (2021; green). In contrast, using our pipeline, HIP 65Ab (orange) shows a comparatively depleted H2O abundance and higher C/O. Here we show the retrieved C/O from the main free chemistry retrieval with high SiO scenarios removed. The black lines represent the abundances taken at 0.3 bar of a solar metallicity model (solid is C/O = solar, dashed is C/O = 1) assuming an isothermal 1411 K atmosphere (Figure 4).
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption:  K  p –V sys cross-correlation signal-to-noise maps for the observed water (top) and carbon monoxide (bottom) signals in HIP 65Ab’s dayside atmosphere. The white dotted lines indicate the known orbital parameters (K  p  = 192.7  km s−1 and V sys = 21.04 km s−1; Gaia Collaboration 2018; Nielsen et al. 2020). The maximum cross-correlation peaks (4.2 and 3.2 S/N for H2O and CO, respectively) occur close to the expected K  p  and V sys.
Paper: A Subsolar Metallicity on the Ultra-short-period Planet HIP 65Ab
Authors: Luc Bazinet, Stefan Pelletier, Björn Benneke, Ricardo Salinas, Gregory N. Mace
Figure caption:  K  p –V sys cross-correlation maps (same as Figure 5), but for molecules showing no significant detections near the expected planetary position. Despite these nondetections, we still fit these species in the retrieval to derive upper limits on their abundances.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Retrieved best-fit model (green) compared to our low-resolution JHK-band spectrum from Bowler et al. (2014; top panel) and error-weighted residuals (lower panel). Our full low-resolution retrievals are compared to the best-fit model (yellow) from our retrievals, where our P–T profile is fixed to a Sonora Bobcat P–T profile from (Marley et al. 2021b). The horizontal black line indicates the wavelength coverage of our Keck/NIRSPEC high-resolution K-band data for comparison.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Cross-correlation functions (CCFs) showing detections of CO and H2O using two orders (2.27–2.38 μm) from the high-resolution NIRSPEC K-band spectrum. The significance is computed by dividing the CCF by the standard deviation of the out-of-peak baseline.
Paper: Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy
Authors: Julie Inglis, Nicole L. Wallack, Jerry W. Xuan, Heather A. Knutson, Yayaati Chachan, Marta L. Bryan, Brendan P. Bowler, Aishwarya Iyer, Tiffany Kataria, Björn Benneke
Figure caption: Retrieved pressure–temperature (P–T) profiles for our best-fit models (bold in Table 3) for our low-resolution data (left), high-resolution data (center), and both combined (right). Randomly sampled P–T curves are plotted in green. Condensation curves for important cloud species in young hot objects, Fe, Al2O3, TiO2,f and MgSiO3 are shown for comparison (dotted lines). We overplot a Sonora Bobcat model (Marley et al. 2021a, 2021b) corresponding to the photometrically derived temperature and log(g). The gray gradient corresponds to the value of the wavelength-integrated flux contribution function.