adsabs/AstroCLIMB huggingface dataset:
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption: Line-of-sight H2 column density map of the W5-NW region, generated using the Hi-Gal maps from 160–500 μm. This map has a resolution of 36″ and a pixel size of 14″. The 3σ (σ = 5.73 K km s−1) contour of the 12CO(3 − 2) integrated intensity map is overlaid in black. The green circle is the region over which the overall spectra described in Figure 1 are extracted. The yellow and black stars indicate the position of the Class I and II YSOs, respectively, identified by Koenig et al. (2008). The YSO clustering regions (red ellipses) are labeled a, b, and c, and the corresponding 12CO(3 − 2) spectra extracted over these regions are shown.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption: PV diagram of 12CO(3 − 2) along the cuts A, B, and C shown in the two-color composite image of W5-NW in Figure 4. The contours start at 3σ (σ = 0.8 K) and with increments of 3σ. The identified bridging features are marked by white arrows. The V-shaped bridging feature is sketched in black along the cut B.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption: PPV diagram of all fitted components in W5-NW. Each voxel denotes the spatial location and best-fit centroid velocity of the Gaussian component identified in 12CO (3 − 2) emission using SCOUSEPY. The color of each point represents these best-fit velocities. The integrated intensity map of 12CO (3 − 2) integrated over the full velocity range is shown at the base of the plot. The coordinates axes are specified as a relative offset from α J2000 = 02h49m34.ˢ9; ﹩{\delta }_{{\rm{J}}2000}=+60^\circ 44^{\prime} 42^{\prime\prime} ﹩. The vertical lines denote the position of the green circular apertures shown in Figure 4. Connecting velocity structures are highlighted within the drawn rectangle. Ellipses showing YSO clusters (see Figure 7) are marked.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption:  12CO(3 − 2) channel maps towards the W5-NW cloud complex. The contours start from 10σ and increase in steps of 5σ (σ = 0.6 K km s−1). Each channel has a width of 1 km s−1. D and P are the peak and intensity depression, respectively, of the 12CO(3 − 2) emission. The maps are boxcar smoothed across 3 pixels.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption: (a) 12CO(3 − 2) integrated intensity map of W5-NWa (color scale) and W5-NWb (contours). (b) Same as (a) with the contours of W5-NWb displaced by 1.2 pc. The contours start from 10σ and increase in steps of 7σ (σ = 2.7 K km s−1).
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: The fraction of recovered LAEs as a function of line flux. Error bars show the 1σ Poisson error. The red, green, and blue curves show examples of how our survey completeness varies with different observational strategies assuming a 0.8 e− pix−1 s−1 background noise level typical of the High Latitude Survey (see Section 4 for details).
Paper: Lyα at Cosmic Dawn with a Simulated Roman Grism Deep Field
Authors: Isak G. B. Wold, Sangeeta Malhotra, James E. Rhoads, Vithal Tilvi, Austen Gabrielpillai
Figure caption: Left: for our deepest grism simulation (﹩{t}_{\exp }=69.4﹩ hr), we show Lyα flux completeness curves for different emitter redshifts. Right: same as the left figure except completeness is plotted vs. Lyα luminosity. Across all redshift bins, we find that our survey can recover L Lyα  > 1043 erg s−1 LAEs at the 50% completeness level (see Table 2).
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: Mass sensitivity for each filter generated via synthetic point source injections. Compared to ground-based data (dashed curves), at separations ≳1″ the NIRCam data reach lower masses in all filters. In the background limit, the F405M and F410M filters reach masses that are ∼5 times lower than the LBTI data (Wagner et al. 2019). The F405N data provide exceptionally deep sensitivity limits of ≳0.5 M Jup, owing to the brightness of young planets at ∼4 μm and JWST's far superior background-limited sensitivity. The yellow circle corresponds the brightness of MWC 758 c measured at 4.05 μm with LBTI/ALES (Wagner et al. 2023). The mass of this object may be higher than ∼5 M Jup for higher levels of extinction. The minimum and maximum range of predicted parameters for the spiral arm driving planet are shown in the gray shaded region. The range of plausible combinations of these parameters has a more complex shape—i.e., more widely separated companions require a greater mass to drive similar spiral arms; see Dong et al. (2015), Fung & Dong (2015), and Ren et al. (2020) further details.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: Left: contrast curves generated from synthetic point source injections (also shown as mass-detection limits in Figure 4). Center: LBTI/ALES 3.97–4.14 μm image, and right:  JWST/NIRCam F405N data with a smaller optimization range (0.″25–1.″2) focused on recovering closer-in sources. The yellow circle corresponds the brightness of MWC 758 c measured at 4.05 μm with LBTI/ALES (Wagner et al. 2023). The F405N data are not sensitive enough to detect MWC 758 c, which will likely require the use of a coronagraph. The spiral arms are weakly detected in the F405N data.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: Contrast curves generated via synthetic point source injections. Comparisons to ground-based data (Wagner et al. 2019; Boccaletti et al. 2021) at similar wavelengths are shown in dashed curves. F187N is most comparable in wavelength to SPHERE’s H23 filter, F200W is most comparable to SPHERE’s K12 filter, and F405N and F410M are most comparable to LBTI’s Lp (or ﹩L^{\prime} ﹩) filter. The yellow circle corresponds the brightness of MWC 758 c measured at 4.05 μm with LBTI/ALES (Wagner et al. 2023). At wavelengths longer than λ ≳ 2 μm and projected separations ≳1″, the NIRCam data reach over an order of magnitude fainter sensitivities than ground-based data. These sensitivities are converted to mass-detection limits in Figure 4. The scattered light disk extends to ∼0.″55 (Benisty et al. 2015). Sensitivities interior to this are likely underestimated as a result.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: Top:  JWST/NIRCam images of MWC 758 processed with ADI-KLIP. Bottom:  Corresponding signal-to-noise ratio (S/N) maps. Note that the long− and short-wavelength images have different platescales, and that the software mask is twice as large for the long-wavelength images. The location of MWC 758 c (Wagner et al. 2023) is indicated in the short-wavelength images (it is at the edge of the mask in the long-wavelength images). There is a low-S/N (∼3) source in MWC 758c’s vicinity in the F187N and F200W images. Aside from the spiral protoplanetary disk, no other objects are detected with S/N ≥ 5 within separations of 2″. At wider separations, two background objects are detected (see Appendices B and C).
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: Classical-ADI images of each individual spacecraft roll and their combination. The images in the F187N and F200W filters (likewise F405N and F410M) share a common platescale. All images share a common orientation of north up and east left. The image stretch has been adjusted independently in order to show both the residual PSF noise and background noise, which varies depending on the wavelength and filter width. The background star is barely in the field of view in the short-wavelength filters, and some detector edge effects are present near the bottom of the image. Positive and negative speckles are seen in some of the images resulting from wave front drift of the primary mirror segments between the two roll orientations.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: JWST/NIRCam image of MWC 758's protoplanetary disk in the F187N+F200W filters. No coronagraph was used, although a software mask was placed over the inner speckle-dominated region. The location of the star is marked by the crosshairs. The images were processed with angular differential imaging (specifically, ADI-KLIP; Soummer et al. 2012), normalized to the brightest part of the disk, and then added to one another. The two spiral arms are clearly visible. The image is the result of Roll 1–Roll 2. Negative regions to the sides of the disk are the result of the angular differential imaging processing.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: IRTF/SpeX spectrum of MWC 758 taken on 2021 February 3. The flux of MWC 758 and its unresolved inner disk emission was used to convert from flux density to contrast units in Figure 3.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Illustration of the model construction process for a region of order 46 of the studied transit. Steps 1 and 2 do not involve spectra and are not represented. The rows displaying steps 6 and 7 have a broken y-axis in order to better show the spectra despite the transit effect. In the penultimate row, the spectra have been normalized over wavelengths for illustrative purposes. The bottom panel represents  M   θ (t, λ) without modification.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Temperature profile and condensation curves obtained from our self-consistent model, for 3 times the solar metallicity. The horizontal dotted and dashed black lines correspond, respectively, to the pressure range concentrating 95% and 68% of the transmission contribution of our petitRADTRANS base model (see Section 4.7) over the CARMENES wavelength range. The horizontal solid black line corresponds to the pressure of the maximum contribution.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: HD 189733 b low-resolution (﹩{ \mathcal R }\approx 500﹩) transit depth and species contributions simulated with Exo-REM. The gray areas represent the wavelength range of the CARMENES orders. On top are indicated the index number of the even-numbered orders. The dotted line labeled “CIA+Ray” represents the combined contributions of the H2–H2, H2–He, and H2O–H2O collision-induced absorptions and the effect of Rayleigh scattering. The contributions of CO2, PH3, TiO, and VO were negligible in this spectral region and thus are not represented. On the background, in black, are represented the time-averaged data in arbitrary units.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Illustration of the simulated data construction process for a region of order 46 of the studied transit. Steps 3−5 are identical to those in Figure 3. The slight differences between the telluric line shapes with orbital phase are mainly due to the change in air mass. For illustrative purposes, the noise in step 9 has been increased by a factor 10 compared to the amount expected for CARMENES.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Mass–radius distribution of the 5243 confirmed exoplanets to date (2023 February 28; Nasa Exoplanet Archive 2023). Not all the confirmed planets have a measured radius and/or mass; thus, the total count in the histograms is less than 5243. The scatter plot shows only the 512 planets for which the mass and radius are known within 15%.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: MMRs obtained from our self-consistent model, for 3 times the solar metallicity. Only the absorbing species MMRs are represented, except TiO and VO, which had MMRs below 10−12. The horizontal dotted and dashed black lines correspond, respectively, to the pressure range concentrating 95% and 68% of the transmission contribution of our petitRADTRANS base model (see Section 4.7) over the CARMENES wavelength range. The horizontal solid black line corresponds to the pressure of the maximum contribution.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Evolution of the RH (top panel), air mass (middle panel), and mean S/N (bottom panel) during the observations. The transit event of HD 189733 b occurs between the vertical dashed lines.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. I. Constraints on Planets Exterior to the Spiral Disk Around MWC 758
Authors: Kevin Wagner, Jarron Leisenring, Gabriele Cugno, Camryn Mullin, Ruobing Dong, Schuyler G. Wolff, Thomas Greene, Doug Johnstone, Michael R. Meyer, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Tom Roellig, George Rieke, Marcia Rieke, Michael Sitko, John Stansberry, Erick Young
Figure caption: Wide-field F410M image (processed with ADI-KLIP) with the central regions and those surrounding the known background star blocked in order to show the newly discovered faint background galaxy to the North of MWC758. The object’s characterization arises from its spatially extended nature from the NE to SW. The galaxy is not detected in other filters.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Illustration of the effect of our implementation of the SysRem preparing pipeline on the order 46 of the studied data, for a selection of number of passes. The left column represents prepared data, the right column prepared models. Rows 1–5: prepared noiseless simulated data and model with 1, 2, 3, 5, and 10 SysRem passes, respectively. The simulated data used are the same as in step 9 of Figure 4. Sixth row: same as the first row, but with added noise. The lines are no longer visible to the naked eye. Bottom row: prepared CARMENES data. The white vertical stripes are masked telluric lines.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Posterior probability distributions for several order selections and the exposures corresponding to T transit. Each row represents a series of posteriors obtained with a different order selection. TTR-06: order selection used in body of the article, for comparison. (a) Order selection obtained when running our algorithm nominally. (b) Order selection obtained when running our algorithm, starting with orders that place the coadded CCF maximum at K  p  and V rest far from the expected ones. The dashed vertical blue lines represent the 0.16, 0.50, and 0.84 quantiles (i.e., median and 1σ error bar) of the distributions obtained. Indicated below each panel are the median and the 1σ error bar of the retrieved parameters using the setup.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Summary of the estimated rest velocity of HD 189733 b in the literature. The marker shape indicates the source of the data. In parentheses, next to the data source, is displayed the spectral band coverage of the data. The color indicates which absorber was used to study the data. The label “CO + H2O” indicates that these two species' opacities were present in the model used.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: HD 189733 b low-resolution (﹩{ \mathcal R }\approx 500﹩) transit depth for a selection of models. Black: Exo-REM model with a 10 times solar metallicity. Dotted blue: best-fit model from the P-01 setup. Solid blue: best-fit model from the P-18 setup. Red: HST WFC3 data from Kilpatrick et al. (2020). The red vertical bars represent the 1σ uncertainties on the HST data, and the red horizontal bars represent the width of the data wavelength bins. The dark-blue and light-blue areas represent the envelope of the 1σ and 3σ models for P-18, respectively. The gray areas represent the wavelength range of the orders discarded from our selection. The planet radii of the Exo-REM model (at 105 Pa) and the P-models (at 103 Pa) have been increased by 1200 and 3600 km, respectively, compared to the value in Table 1.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Posterior probability distributions for a selection of SysRem setups. The dashed vertical lines represent the 0.16, 0.50, and 0.84 quantiles (i.e., median and 1σ error bar) of the distributions obtained. Indicated below each panel are the median and the 1σ error bar of the retrieved parameters using the setup. The units are the same as in Figure 12.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Posterior probability distributions for all of the setups in Table 5. The dashed vertical blue lines represent the 0.16, 0.50, and 0.84 quantiles (i.e., median and 1σ error bar) of the distributions obtained. Indicated below each panel are the median and the 1σ error bar of the retrieved parameters using the setup. The units are the same as in Figure 12. The black rectangle highlights our fiducial setup.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Posterior probability distributions of our noisy simulations. The noise matrix generation is detailed in Section 3.2; the seed used was 12345. Blue: pRT 1D simulation using Polyfit. The solid red lines corresponds to the model input values for the 1D model. The dashed vertical blue lines represent the 0.16, 0.50, and 0.84 quantiles (i.e., median and 1σ error bar) of the distributions for the 1D simulation. Indicated on top of each column are the median and the 1σ error bar of the retrieved parameters for the 1D simulation. The contours in the 2D histograms corresponds to the 1σ, 2σ, and 3σ contours.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Posterior probability distributions for of our noiseless simulation, with few retrieved parameters. The solid red lines correspond to the model input values for the 1D model. The dashed vertical lines represent the 0.16, 0.50, and 0.84 quantiles (i.e., median and 1σ error bar) of the distributions obtained. Indicated below each panel are the median and the 1σ error bar of the retrieved parameters using the setup, as well as the true value in parentheses. The units are the same as in Figure 12.
Paper: A Formally Motivated Retrieval Framework Applied to the High-resolution Transmission Spectrum of HD 189733 b
Authors: Doriann Blain, Alejandro Sánchez-López, Paul Mollière
Figure caption: Posterior probability distributions for a Polyfit setup, with all orders, using 100 live points. Blue: results using the Polyfit preparing pipeline. The dashed vertical blue lines represent the 0.16, 0.50, and 0.84 quantiles (i.e., median and 1σ error bar) of the distributions obtained with Polyfit. Indicated on top of each column are the median and the 1σ error bar of the retrieved parameters using Polyfit. The contours in the 2D histograms correspond to the 1σ, 2σ, and 3σ contours.