adsabs/AstroCLIMB huggingface dataset:
Paper: The Delayed Radio Emission in the Black Hole X-Ray Binary MAXI J1348-630
Authors: Bei You, Shuai-kang Yang, Zhen Yan, Xinwu Cao, Andrzej A. Zdziarski
Figure caption: The correlation between the radio luminosity at 5 GHz and the X-ray Comptonization luminosity in 0.1–100 keV. The blue, red, and green points represent the data from rising hard state, decaying hard state, and mini-outburst, respectively. The linmix algorithm (Kelly 2007) implemented in Python is used to fit the data points. The dashed lines are the best fits of the radio and X-ray correlation, and the shaded regions indicate uncertainties at the 1σ level.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: (Left) Two representative NIRSpec-IFU spectra from the northern shell (in orange) and southern shell (green) show dominant features from CO fundamental bands with a few high-ionization ejecta lines, in comparison with Orion (blue; Peeters et al. 2024). The northern spectra show two velocity components of −2070 and −1270 km s−1, while the southern spectra show one component of +1060 km s−1. The ∼3400 km s−1 difference between the blue- and redshifted motion of Cas A has been removed using the rest wavelengths of the ejecta lines. (Right) An enlarged section from the left panel shows a comparison of the lines with those of Orion (multiplied by 10, shown in dotted black.).
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: JWST NIRSpec-IFU spectra of Cas A toward two representative knots (0.″1 × 0.″1 region for each) in the northern IFU field (R.A. = 350.°8731, decl. = 58.°8422 in blue) and at the southern IFU field (R.A. = 350.°8764, decl. = 58.°7905 in green). The spectra show a dominant CO fundamental band with a few high-ionization ejecta lines indicated. The two CO bumps arise from the R (the shorter wavelength bump) and P (the longer wavelength bump) branches of CO. The CO emission is stronger in the southern position, as expected from the imagery presented above. The ejecta lines are from [Ca IV] at 3.2 μm, [Si IX] at 3.94 μm, [Ca V] at 4.16 μm, [Mg IV] at 4.49 μm, [Ar VI] at 4.53 μm, and [K III] at 4.6 μm.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: Zoomed-in images of Figure 2 on the northern (top) and southern (bottom) shells. The NIRSpec-IFU FOVs are marked as black squares on the JWST three-color images. The arrows point to the filaments showing CO excess emission (in green, marked as A, B, and D) and Ar ejecta excess (in red, marked as C). The slit (box E, in cyan) is cut through the southern shell where a radial profile is obtained in Figure 7.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: (Top) Regions for the extracted spectra shown below are marked on the images of NE IFU FOV for (a) 3.92 μm ([Si IX]), (b) 4.70 μm (CO), and of the S IFU FOV of (c) 3.92 μm ([Si IX]) and (d) 5.04 μm (CO). NIRSpec-IFU spectra of Cas A toward a few positions in the northern (middle: (e)) and south (bottom: (f)). The positions and marked circles on (a) and (b) and extracted spectra (e) are (R.A., decl.) = (350.°8724, 58.°8423) in green, (350.°8732, 58.°8421) in blue, (350.°8729, 58.°8419) in red, and (350.°8724, 58.°8418) in yellow. The positions and marked circles on (c) and (d) and extracted spectra (f) are (R.A., decl.) = (350.°8763, 58.°7907) in magenta ((c), (d)) or orange (f), (350.°8764, 58.°7904) in cyan, (350.°8771, 58.°7904) in red, (350.°8759, 58.°7902) in green, and (350.°8760, 58.°7900) in blue.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: A two-temperature LTE CO model (in red) is superposed on the JWST southern spectrum of Cas A (in green). Here we have added a hotter CO component with T = 4800 K (yellow) and ΔV = 210 km s−1 to the first-temperature component (blue). The total fit is shown in red. The band heads (v = 1–0, v = 2–1, and v = 3–2) are marked. The contribution of synchrotron emission is negligible about ∼50 MJy sr−1, and wavelength dependence is small (the slope is 0.67).
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: An LTE model (in red) using a temperature (T) of 1078 K and a velocity width of 200 km s−1 is superposed on the JWST southern region spectrum of Cas A (in green). The sawtooth-like patterns are reproduced, but the relative strengths differ slightly. In the expanded view in the expanded view of the spectra (Right), the peaks are from CO v = 1–0 P(4) through P(32) transitions. Blends with weaker v = 2–1 and higher vibrational states modulate the apparent contrast of the lines.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: Profiles of surface brightness in Ar ejecta, CO, and synchrotron emission along a slit that cuts through the southern shell in an approximately radial direction (the slit is marked as box E in Figure 3, bottom panel). The position extends from (R.A., decl.) = (350.°838, 58.°789) to (350.°836, 58.°784). The CO peaks farther outward than the Ar emission. The vertical lines are peaks of Ar (in red) and CO emission (in green), respectively.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: Cas A band images of the northern IFU field. (Left) Red and blue colors denote the two different kinematic components of [Ca IV] 3.2 μm in this field. (Middle) Three-color images showing [Mg IV] (in blue), CO (green), and [Si IX] (red). (Right) Three-color images of the southern IFU field: [Mg IV] (in blue), CO (green), and [Si IX] (red). CO and [Mg IV] show similar morphology, while [Si IX] morphology is different.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: Cas A band images of the northern IFU field: (a) [Ca IV] at 3.2 μm, (b) [Si IX] at 3.9 μm, (c) [Mg IV] at 4.5 μm, (d) [Ar VI] at 4.52 μm, (e) CO 4.79 (4.788–4.798) μm, and (f) synchrotron-subtracted CO broad band (from F444W) images. The latter captures the brightest CO band. The CO emission appears similar to other ejecta maps.
Paper: No Top-heavy Stellar Initial Mass Function Needed: The Ionizing Radiation of GS9422 Can Be Powered by a Mixture of an Active Galactic Nucleus and Stars
Authors: Yijia Li, 轶佳 李, Joel Leja, Benjamin D. Johnson, Sandro Tacchella, Rohan P. Naidu
Figure caption: Emission line fit results. Upper panel: emission line measurements along with their uncertainties from Cameron et al. (2023a) are in blue. The Cue posterior median assuming a double power-law ionizing spectrum and five free nebular parameters is in orange. The nine free parameters of the Cue fit are shown in Figure 3. To confirm the Cue result, we also run CLOUDY using the ionizing spectrum and nebular parameters Cue predicted as input, and the output line luminosities are shown in green. Additionally, CLOUDY prediction from an SSP (t age = 3.2 Myr and ﹩\mathrm{log}(Z/{Z}_{\odot })=-1.34﹩) with the proposed top-heavy IMF is in gray. The CLOUDY output given a combination of a MIST+C3K SSP and an AGN ionizing spectrum as the input (see Section 4) is in purple. Lower panel: the residual of the Cue fit results denominated by the measurement uncertainties. The error bars indicate the 1σ posterior range of χ. The results of the Cue fit and the SSP+AGN fit match the observations reasonably well.
Paper: No Top-heavy Stellar Initial Mass Function Needed: The Ionizing Radiation of GS9422 Can Be Powered by a Mixture of an Active Galactic Nucleus and Stars
Authors: Yijia Li, 轶佳 李, Joel Leja, Benjamin D. Johnson, Sandro Tacchella, Rohan P. Naidu
Figure caption: The nebular and UV emission of GS9422 can be powered by a combination of stars and AGN. Here we find the inferred ionizing spectrum from Cue and the observed F 1500 can both be reproduced by the sum of a t age = 3.55 Myr, ﹩\mathrm{log}Z/{Z}_{\odot }=-1.97﹩ SSP, and an AGN with a spectral index α AGN = 2. Top left: the ionizing spectrum shape of the Cue posterior median (orange), SSP+AGN (black), SSP (blue), and AGN (purple). The shaded area reflects the 1σ uncertainty of the Cue fit. The SSP produces ∼65% of the ionizing photons and AGN contributes the rest 36%. Top right: the ﹩\tfrac{{Q}_{\mathrm{HeII}}}{{Q}_{{\rm{H}}}}﹩ distribution of the Cue posterior (orange) and SSP+AGN fit results (black). The Cue posterior distribution is rescaled for presentation. Bottom left: the UV continuum constraints. The measurement is in orange. The sum of the SSP, AGN, and nebular continuum is in green. The nebular emission contributes ∼24% of the observed UV continuum as shown in purple. Bottom right: the predicted total UV continuum (green) and subcontribution of the nebular continuum (purple).
Paper: No Top-heavy Stellar Initial Mass Function Needed: The Ionizing Radiation of GS9422 Can Be Powered by a Mixture of an Active Galactic Nucleus and Stars
Authors: Yijia Li, 轶佳 李, Joel Leja, Benjamin D. Johnson, Sandro Tacchella, Rohan P. Naidu
Figure caption: Posterior distribution of the Cue fit parameters and the inferred ionizing spectrum. The contours show the 1σ, 2σ, and 3σ of the posterior. The blue dashed lines mark the 16%/50%/84% quantiles. The red lines are the results for the same parameters from Cameron et al. (2023a), inferred in a different fashion using recipes applied to observed line ratios. The Cue fit is able to put tight constraints on U, n H, [O/H], and Q ion. Since there is no nitrogen line detected, [N/O] shows a wide posterior. A solar [C/O] is preferred to explain the strong [C IV] lines. The upper right panel shows 2000 random draws of the ionizing spectrum posterior. Despite the large range of the ionizing spectrum parameters, the total ionizing budget of the two power laws is well constrained. The ionizing spectrum shows an AGN-like spectrum at λ > λ He II  and a redder spectrum at λ < λ He II .
Paper: No Top-heavy Stellar Initial Mass Function Needed: The Ionizing Radiation of GS9422 Can Be Powered by a Mixture of an Active Galactic Nucleus and Stars
Authors: Yijia Li, 轶佳 李, Joel Leja, Benjamin D. Johnson, Sandro Tacchella, Rohan P. Naidu
Figure caption: The observed UV turnover around λ rest ≈ 1430 Å is not consistent with intrinsic stellar or AGN light. However, it can be reproduced by a damped Lyα absorber (DLA) near the ionizing source. PRISM data (Cameron et al. 2023a) in the rest frame is in blue. The UV radiation of the composite stellar and AGN solution and the nebular continuum are shown in green. Note that we do not show emission lines here. The UV continuum after being absorbed by a DLA of different N(H I) is in magenta, orange, and red. We estimate an absorber column density of ﹩\mathrm{log}N(\mathrm{HI})\lesssim 22.7﹩ cm−2. We do not model the Gunn–Peterson trough due to absorption from neutral hydrogen in the IGM, which might further lower the DLA N(H I) requirement. In a DLA of this relatively high column depth, it would be unusual but not impossible to have no dust. Further discussion of this point is in Section 5.1.
Paper: No Top-heavy Stellar Initial Mass Function Needed: The Ionizing Radiation of GS9422 Can Be Powered by a Mixture of an Active Galactic Nucleus and Stars
Authors: Yijia Li, 轶佳 李, Joel Leja, Benjamin D. Johnson, Sandro Tacchella, Rohan P. Naidu
Figure caption: Ionizing spectra corresponding to the models in Figure 1. The green line and the shaded region represent the median and 1σ range of the Cue inferred ionizing spectrum, respectively. The purple line is the proposed decomposition of the inferred ionizing spectrum from Cue into stellar populations and AGN. The gray line is a top-heavy IMF SSP (t age = 3.2 Myr and ﹩\mathrm{log}(Z/{Z}_{\odot })=-1.34﹩) estimated from Cameron et al. (2023a) for comparison. The composite scenario matches the Cue fit results well and produces fewer He II ionizing photons than the top-heavy SSP.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: JWST F356W (3.56 μm; top left), F444W (4.44 μm; top right) images, CO fundamental image (produced from F444W image after subtracting the synchrotron emission using F356W image; bottom left), and equivalent CO image using Spitzer data (bottom right). The JWST images show far more complexity. The CO emission is from the CO fundamental bands and overlaps spatially with the knotty ejecta structures. Faint, extended, diffuse F444W emission seen in projection toward the center, hinted at with the Spitzer data, is more noticeable. The image is centered on R.A. 23h23m26.ˢ65 and decl. +58°49′14.″98 (J2000) with an FOV of 6.′4 × 6.′4. The units in the color bar are in MJy sr−1.
Paper: Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
Authors: J. Rho, S.-H. Park, R. Arendt, M. Matsuura, D. Milisavljevic, T. Temim, I. De Looze, W. P. Blair, A. Rest, O. Fox, A. P. Ravi, B.-C. Koo, M. Barlow, A. Burrows, R. Chevalier, G. Clayton, R. Fesen, C. Fransson, C. Fryer, H. L. Gomez, H.-T. Janka, F. Kirchschlager, J. M. Laming, S. Orlando, D. Patnaude, G. Pavlov, P. Plucinsky, B. Posselt, F. Priestley, J. Raymond, N. Sartorio, F. Schmidt, P. Slane, N. Smith, N. Sravan, J. Vink, K. Weil, J. Wheeler, S. C. Yoon
Figure caption: JWST three-color mosaicked images of synchrotron emission (F356W in blue), CO (synchrotron-subtracted F444W in green), and Ar ejecta (F770W in red). North is up, and east is to the left. The detailed structures of the three images are noticeably different from each other. The synchrotron emission (blue) shows smooth structures and is dominant outside the main shell.
Paper: Debris Disks Can Contaminate Mid-infrared Exoplanet Spectra: Evidence for a Circumstellar Debris Disk around Exoplanet Host WASP-39
Authors: Laura Flagg, Alycia J. Weinberger, Taylor J. Bell, Luis Welbanks, Giuseppe Morello, Diana Powell, Jacob L. Bean, Jasmina Blecic, Nicolas Crouzet, Peter Gao, Julie Inglis, James Kirk, Mercedes López-Morales, Karan Molaverdikhani, Nikolay Nikolov, Apurva V. Oza, Benjamin V. Rackham, Seth Redfield, Shang-Min Tsai, Ray Jayawardhana, Laura Kreidberg, Matthew C. Nixon, Kevin B. Stevenson, Jake D. Turner
Figure caption: (Top) A portion of the observed flux from the WASP-39 system along with a BT-Settl photospheric model, using WISE-W2 as an anchor point. Both the MIRI data, as well as the W3 point from WISE hint at a slight amount of excess flux. (Middle) The WASP-39b MIRI transmission spectrum along with the best-fit model retrieved to the data short of 10 μm, along with 1σ uncertainties. (Bottom) The excess flux calculated using the stellar flux compared with a photospheric model flux from the top plot (in blue) and the excess flux calculated from the transmission spectrum (in green). We also plot the excess stellar flux from three G-star calibrators. Note: the uncertainties are the 1σ, random uncertainties calculated from the scatter in the data. Systematic uncertainties are not included. In the case of the flux-calibrated stellar spectrum, the systematic uncertainties may be on the order of 10%.
Paper: Debris Disks Can Contaminate Mid-infrared Exoplanet Spectra: Evidence for a Circumstellar Debris Disk around Exoplanet Host WASP-39
Authors: Laura Flagg, Alycia J. Weinberger, Taylor J. Bell, Luis Welbanks, Giuseppe Morello, Diana Powell, Jacob L. Bean, Jasmina Blecic, Nicolas Crouzet, Peter Gao, Julie Inglis, James Kirk, Mercedes López-Morales, Karan Molaverdikhani, Nikolay Nikolov, Apurva V. Oza, Benjamin V. Rackham, Seth Redfield, Shang-Min Tsai, Ray Jayawardhana, Laura Kreidberg, Matthew C. Nixon, Kevin B. Stevenson, Jake D. Turner
Figure caption: The best fits to the excess flux as calculated from the transmission spectrum (top) or from the stellar spectrum (bottom). We fit a crystalline silicate feature and a blackbody curve to both spectra separately. These plots assume the 3σ upper limit to the WISE/W4 flux.
Paper: Debris Disks Can Contaminate Mid-infrared Exoplanet Spectra: Evidence for a Circumstellar Debris Disk around Exoplanet Host WASP-39
Authors: Laura Flagg, Alycia J. Weinberger, Taylor J. Bell, Luis Welbanks, Giuseppe Morello, Diana Powell, Jacob L. Bean, Jasmina Blecic, Nicolas Crouzet, Peter Gao, Julie Inglis, James Kirk, Mercedes López-Morales, Karan Molaverdikhani, Nikolay Nikolov, Apurva V. Oza, Benjamin V. Rackham, Seth Redfield, Shang-Min Tsai, Ray Jayawardhana, Laura Kreidberg, Matthew C. Nixon, Kevin B. Stevenson, Jake D. Turner
Figure caption: (Top) WASP-39b MIRI-observed transmission spectrum along with its model retrieval and the model retrievals adjusted by the dilution factor induced by our best debris disk models. (Bottom) The residuals between the data and the models. The inclusion of the debris disk decreases the residuals.
Paper: Debris Disks Can Contaminate Mid-infrared Exoplanet Spectra: Evidence for a Circumstellar Debris Disk around Exoplanet Host WASP-39
Authors: Laura Flagg, Alycia J. Weinberger, Taylor J. Bell, Luis Welbanks, Giuseppe Morello, Diana Powell, Jacob L. Bean, Jasmina Blecic, Nicolas Crouzet, Peter Gao, Julie Inglis, James Kirk, Mercedes López-Morales, Karan Molaverdikhani, Nikolay Nikolov, Apurva V. Oza, Benjamin V. Rackham, Seth Redfield, Shang-Min Tsai, Ray Jayawardhana, Laura Kreidberg, Matthew C. Nixon, Kevin B. Stevenson, Jake D. Turner
Figure caption: Dilution factor on the MIRI transit spectrum for a hypothetical stellar blend with various temperatures. The labels in the legend indicate the effective temperature and flux fraction from the blended star (1.0 is the maximum possible fraction).
Paper: Debris Disks Can Contaminate Mid-infrared Exoplanet Spectra: Evidence for a Circumstellar Debris Disk around Exoplanet Host WASP-39
Authors: Laura Flagg, Alycia J. Weinberger, Taylor J. Bell, Luis Welbanks, Giuseppe Morello, Diana Powell, Jacob L. Bean, Jasmina Blecic, Nicolas Crouzet, Peter Gao, Julie Inglis, James Kirk, Mercedes López-Morales, Karan Molaverdikhani, Nikolay Nikolov, Apurva V. Oza, Benjamin V. Rackham, Seth Redfield, Shang-Min Tsai, Ray Jayawardhana, Laura Kreidberg, Matthew C. Nixon, Kevin B. Stevenson, Jake D. Turner
Figure caption: The decrease in transit depth due to a relatively faint debris disks can be on the order of several hundred ppm.