adsabs/AstroCLIMB huggingface dataset:
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: Distribution of ﹩{\chi }_{\nu }^{2}﹩ for simulated single exposure images. Not shown are 42 PSFEx ﹩{\chi }_{\nu }^{2}﹩ values greater than 100 and 100 ShOpt                         ﹩{\chi }_{\nu }^{2}﹩ values greater than 100.
Paper: Efficient Point-spread Function Modeling with ShOpt.jl: A Point-spread Function Benchmarking Study with JWST NIRCam Imaging
Authors: Edward M. Berman, Jacqueline E. McCleary, Anton M. Koekemoer, Maximilien Franco, Nicole E. Drakos, Daizhong Liu, James W. Nightingale, Marko Shuntov, Diana Scognamiglio, Richard Massey, Guillaume Mahler, Henry Joy McCracken, Brant E. Robertson, Andreas L. Faisst, Caitlin M. Casey, Jeyhan S. Kartaltepe
Figure caption: April data tiling scheme.
Paper: Biases in Exoplanet Transmission Spectra Introduced by Limb-darkening Parametrization
Authors: Louis-Philippe Coulombe, Pierre-Alexis Roy, Björn Benneke
Figure caption: Impact of the choice of limb darkening on the light curve fit and measured transit depth for the case of no limb darkening and photometric scatter of σ = 1000 ppm. Top left: median stellar intensity profile I s(μ)/I 0 (blue line) from the transit fit to the simulated observations using the [u 1, u 2] limb-darkening parameterization. The 1σ and 2σ confidence intervals are shown by the shaded regions. Bottom left: median transit model (blue) obtained from the transit fit with the [u 1, u 2] limb-darkening parameterization. The 1σ and 2σ confidence intervals are shown by the shaded regions. Top middle: same as top left considering the [q 1, q 2] parameterization. Bottom middle: same as bottom left considering the [q 1, q 2] parameterization. Right: Probability density distributions of the measured transit depth minus the true transit depth for the [u 1, u 2] (blue) and [q 1, q 2] (red) parametrizations. The transit depth measured using [u 1, u 2] is centered on the expected value, whereas the one measured using [q 1, q 2] peaks at a smaller value.
Paper: Biases in Exoplanet Transmission Spectra Introduced by Limb-darkening Parametrization
Authors: Louis-Philippe Coulombe, Pierre-Alexis Roy, Björn Benneke
Figure caption: Impact of the choice of limb darkening on the light curve fit and measured transit depth for the case of no limb darkening and photometric scatter of σ = 1000 ppm. Top left: median stellar intensity profile I s(μ)/I 0 (blue line) from the transit fit to the simulated observations using the [u 1, u 2] limb-darkening parameterization. The 1σ and 2σ confidence intervals are shown by the shaded regions. Bottom left: median transit model (blue) obtained from the transit fit with the [u 1, u 2] limb-darkening parameterization. The 1σ and 2σ confidence intervals are shown by the shaded regions. Top middle: same as top left considering the [r 1, r 2] parameterization. Bottom middle: same as bottom left considering the [r 1, r 2] parameterization. Right: Probability density distributions of the measured transit depth minus the true transit depth for the [u 1, u 2] (blue) and [r 1, r 2] (red) parametrizations. The transit depths measured using [u 1, u 2] and [r 1, r 2] are centered on the expected value, but the posterior distribution obtained with [r 1, r 2] is wider.
Paper: Biases in Exoplanet Transmission Spectra Introduced by Limb-darkening Parametrization
Authors: Louis-Philippe Coulombe, Pierre-Alexis Roy, Björn Benneke
Figure caption: Impact of the choice of limb-darkening parameterization on the measured transmission spectrum. Top left: NIRISS/SOSS spectra of WASP-39 b, fit at a spectral resolution of R = 80 (blue points) and at native resolution (black points), obtained using the [u 1, u 2] parameterization with wide uniform priors. The fit performed at native resolution is binned at a resolution of R = 80 after the light curve fitting. Bottom left: difference between the fit performed at a resolution of R = 80 and the one at native resolution (blue points) for the [u 1, u 2] parameterization. The error bars for the residuals are computed in quadrature. A smoothed version of the residuals (blue line), along with the 1σ confidence region, are shown using a linear Savitzky–Golay filter with a window size of 31 points. Top right: same as top left for the [q 1, q 2] parameterization. Bottom right: same as bottom left for the [q 1, q 2] parameterization. The residuals between the transit spectra obtained from the light-curve fits at different resolutions clearly show a systematic deviation away from 0 past 2 μm in the [q 1, q 2] case.
Paper: Biases in Exoplanet Transmission Spectra Introduced by Limb-darkening Parametrization
Authors: Louis-Philippe Coulombe, Pierre-Alexis Roy, Björn Benneke
Figure caption: Magnitude of the bias on the measured transit depth as a function of photometric scatter. The data points show the deviation from the true transit depth, along with the 1σ uncertainty, as a function of photometric scatter for both the [u 1, u 2] and [q 1, q 2] parametrizations. We use a symmetric log scale for the y-axis. Contrastingly from the [u 1, u 2] parameterization, the [q 1, q 2] parameterization shows an increasing bias of the transit depth when going toward larger scatter. The blue dashed line corresponds to no bias on the transit depth, with the measured transit depths obtained using the [u 1, u 2] parameterization following that trend. The bias on the transit depth when using the [q 1, q 2] parameterization closely follows the red dashed line, which traces the trend ﹩y=-\sqrt{2/\pi }\,{\sigma }_{t,d}﹩, where σ  t,d  is the measured transit depth uncertainty.
Paper: Biases in Exoplanet Transmission Spectra Introduced by Limb-darkening Parametrization
Authors: Louis-Philippe Coulombe, Pierre-Alexis Roy, Björn Benneke
Figure caption: Left: region of the [u 1, u 2] parameter space where conditions A and B are respected. Center: reparametrization of the limb-darkening parameter space such that the two triangular regions forming the parameter space following conditions A and B are right-angled triangles. Right: parameter space joining the limb-darkening and limb-brightening scenarios, obtained by rotating the limb-brightening scenarios about the u 1/2 axis.
Paper: Biases in Exoplanet Transmission Spectra Introduced by Limb-darkening Parametrization
Authors: Louis-Philippe Coulombe, Pierre-Alexis Roy, Björn Benneke
Figure caption: Fitting the light curves at higher spectral resolution produces a more precise spectrum. Relative difference in percent between the errors on the transit depths measured at a resolution of R = 80 and those measured at the native resolution and then fitted afterward. A smoothed version of the difference transit depth precision (black line) is shown using a linear Savitszky–Golay filter with a window size of 31 points. The errors obtained from the lower resolution fit are systematically larger than those obtained at the native resolution, with the difference in precision ranging from 20% to 60% across the wavelength range.
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: 12 + log(O/H) and u − r color vs. the stellar mass with the color bar of D  n 4000. Left panel: the stellar mass vs. 12 + log(O/H). The black solid and dashed curves represent the MZ relation and its 1σ scatter of C. A. Tremonti et al. (2004). Right panel: the stellar mass vs. u − r color. The location of the green valley galaxies is indicated with the two solid lines (K. Schawinski et al. 2014).
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: Diagram of the stellar mass and SFR for our ETG sample. The black dotted–dashed line represents the best fit to the SDSS data (A. Renzini & Y.-J. Peng 2015). The blue solid and red dashed lines exhibit the best least-squares fits for the two samples, with the fits located within the 1σ region and below the 2σ level of the MZ relation.
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: W2 − W3 vs. W1 − W2 diagnostic diagram. Black squares represent the galaxy sample with SF; red dots indicate galaxies without SF; and green pentagrams are confirmed ETGs. The blue dashed line on this diagram demarcates the best boundary between galaxies with and without ongoing SF. The black lines delineate the “AGN” wedge, as proposed by S. Mateos et al. (2012).
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: Two-color diagram for RSF and UV upturn classification for our ETG sample (S. K. Yi et al. 2011). The red horizontal dashed line represents a rising UV slope, the blue vertical dashed line denotes the criterion for identifying young stars, and the slanted solid line indicates the UV strength required for a galaxy to be classified as a UV upturn galaxy. RSF stands for residual SF.
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: The distributions of SNRs for various emission lines. The different colors and line types represent SNRs corresponding to different emission lines within our sample. The thick black dashed line shows the SNR > 3 of various lines.
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: BPT diagnostic diagram. The blue curve shows the G. Kauffmann et al. (2003) lower boundary for SFGs. Black squares indicate the galaxy sample with SF. The green pentagrams are the same as in Figure 1.
Paper: The Metallicity Dilution in Local Massive Early-type Galaxies
Authors: Yu-zhong Wu, Wei Zhang
Figure caption: The WHAN diagram. The magenta lines demarcate the spectral classes suggested by R. Cid Fernandes et al. (2011).
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Temperature dependency of the spectral element shown in Figure 2 with the fourth-order polynomial fit for that pixel. Residuals to the fit have an rms of 0.087 and 0.036 for SPIRou and HARPS, respectively.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Sample spectroscopic features in the HARPS (left-hand panel) and SPIRou (right-hand panel) for sample domains. The temperature dependency of the spectral element highlighted with a dashed line is shown in Figure 3. The line centered at 632.935 nm is a Ni I feature while the feature at 1638.50 nm is tentatively attributed to an Fe II line.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Temperature distribution of the stars used for the SPIRou and HARPS templates. A total of 44 stars were used for SPIRou, 105 with HARPS, among which eight are in common.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Binned dTemp measurements through HD 189733b transit compared with a change in the temperature contrast of spots covering 2.8% of the photosphere. We assume that spots are outside of the transit chord (as in Figure 10). The dip below the baseline value at midtransit suggests a starspot contrast of ∼1000 K, but this model strongly underpredicts the rise at the start and end of the transit. We note that having very cold spots (−2000 K) or no spots leads to a very similar signature; very cold spots contribute little to the overall spectrum and have no effects on the dTemp signal.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Binned dTemp measurements through HD 189733b transits compared with a change in the impact parameter. The ∼0.5 K dip in dTemp compared to out-of-transit values as well as the maximum in dTemp at a position of ±0.8 stellar radii would suggest an impact parameter of b ∼ 0.5, which is significantly smaller than the literature value (b = 0.69). Here, we assume that the stellar photosphere is uniform (i.e., no spots, no plages).
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Empirical and model temperature gradient spectra for the whole SPIRou domain (top panel), centered on the J-band K I doublet (middle panel) and a sample domain within H band for T eff = 3500 K. The overall behavior of the temperature gradient is well reproduced and most of the deep lines are reproduced by models. One notes that numerous small features, particularly in the H band, are not accurately predicted by models.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption:  dTemp time series with empirical and model temperature gradient spectra for the same timespan as in Figure 5. The signature of the activity is recovered but with an amplitude reduced by a factor ∼2 while the periodicity and correlation length of the GP fits are consistent.
Paper: Measuring Sub-Kelvin Variations in Stellar Temperature with High-resolution Spectroscopy
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Laurie Dauplaise, Luc Arnold, Maya Cadieux, Jean-François Donati, Paul Cristofari, Xavier Delfosse, Pascal Fouqué, Claire Moutou, Pierre Larue, Romain Allart
Figure caption: Same as for Figure 12, but comparing the effect of using empirical and model-based gradient spectra. The overprediction of temperature gradients in models leads to artificially small uncertainties but the signature of the effect described in Section 5.1.1 disappears.
Paper: The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: C. J. Salter, T. Ghosh, R. F. Minchin, E. Momjian, B. Catinella, M. Lebron, M. S. Lerner
Figure caption: (Left) The HSA continuum images of NGC 660 at 4.7 GHz, HPBW = 3.1 × 1.5 mas at P.A. = −4.°9, and (right) at 8.4 GHz, HPBW = 1.6 × 0.7 mas at P.A. = −5.°9. Contour levels are at 2.5σ × 2.5, 5, 10, 20, 40, 80, 160, 320 with σ = 80 μJy at 4.7 GHz and σ = 36 μJy at 8.4 GHz. The gray-scale range is indicated at the top of each image in units of mJy beam−1.
Paper: The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: C. J. Salter, T. Ghosh, R. F. Minchin, E. Momjian, B. Catinella, M. Lebron, M. S. Lerner
Figure caption: (Left) The 4.7 GHz continuum light curve of the NCC. (Right) The light curves of the excited-OH lines. Here, the data at the top (squares) represent the mean peak intensities of the strongest emission components at 4750 and 4765 MHz, while the symbols at the bottom (diamonds) show the mean peak intensity of the two 4660 MHz absorption components. The lower horizontal axis on both plots shows days from 2008.5, while the top axes show MJD.
Paper: The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: C. J. Salter, T. Ghosh, R. F. Minchin, E. Momjian, B. Catinella, M. Lebron, M. S. Lerner
Figure caption: The radio continuum spectrum of NGC 660 on 2011 December 31, near the epoch of the peak of the outburst (top), and on 2014 August 14 (bottom). Stars denote preoutburst flux densities from the literature, with the solid line showing a spectral fit to this data. Triangles mark total measured flux densities, while diamonds show these total values minus the preoutburst spectral fit, i.e., the spectrum of the transient NCC alone.
Paper: The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: C. J. Salter, T. Ghosh, R. F. Minchin, E. Momjian, B. Catinella, M. Lebron, M. S. Lerner
Figure caption: The spectrum of H2CO against the NCC. This was obtained by subtracting the line spectrum of 2007 December (i.e., preoutburst) from the spectrum of 2011 December, and shows new sharp absoption features.
Paper: The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: C. J. Salter, T. Ghosh, R. F. Minchin, E. Momjian, B. Catinella, M. Lebron, M. S. Lerner
Figure caption: Sample excited-OH spectra of NGC 660 from late 2007 to 2017 August. The columns (left to right) show the 4660, 4750, and 4765 MHz lines, respectively, while time increases from top to bottom. Together, they display large secular changes in these molecular lines in NGC 660. The heliocentric velocity resolution is 10 km s−1.
Paper: The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: C. J. Salter, T. Ghosh, R. F. Minchin, E. Momjian, B. Catinella, M. Lebron, M. S. Lerner
Figure caption: Continuum images of NGC 660 at 8.5 GHz (left) and 11.5 GHz (right). For the 8.5 GHz image, the rms noise level is 75 μJy beam−1 and the restoring beam size is 2.″59 × 2.″06 (P.A. = 43°). For the 11.5 GHz image, the rms noise level is 105 μJy beam−1 and the restoring beam size is 3.″00 × 2.″08 (P.A. = 22°). The contour levels are at −1, 1, 2, 4, ..., 256 mJy beam−1. The gray-scale range is indicated at the top of each image in units of mJy beam−1.
Paper: The Discovery and Evolution of a Radio Continuum and Excited-OH Spectral-line Outburst in the Nearby Galaxy NGC 660
Authors: C. J. Salter, T. Ghosh, R. F. Minchin, E. Momjian, B. Catinella, M. Lebron, M. S. Lerner
Figure caption: The integrated excited-OH lines from the regions of the four “hot spots” seen in the X-band image of Figure 6. The higher velocity components occur exclusively against the northwestern hotspot, while those at lower velocities are mainly found against the two eastern hot spots.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: The full caracal-reduced 1D spectrum for frame #56 (frame with the highest S/N). Regions highlighted with light gray are orders that are removed from the analysis due to their low S/N. These orders are the strongest bands of telluric water absorption. However, as can be seen, some of the strong telluric bands still remain, especially in the reddest part of order 55 (∼1.1 μm) and the bluest part of order 41 (∼1.48 μm). This will be masked as explained in Section 2.2. The V-like shapes seen within each order are likely instrumental effects or artifacts from the reduction pipeline (Alonso-Floriano et al. 2019).
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Top: airmass throughout the observation. Middle: relative humidity. Bottom: average S/N over orders of each exposure. Regions highlighted in light red are exposures excluded from the analysis. The horizontal black dashed line corresponds to S/N = 50. One exposure has an average S/N of ∼49.9 (frame #14), hence, given the small number of frames, we decided to keep this one for the analysis. The vertical dashed blue lines mark the first to fourth contacts of the transit, from left to right.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Spectra of order 57 throughout the analysis outlined in Section 2 in a 2D matrix (time × wavelength). The first panel shows the output spectra of caracal. The variation of flux between frames is caused by the difference in the S/N due to different observational conditions, instrumental effects, etc. The second panel shows the spectra after normalization, masking of outliers, and continuum-level correction. Gray regions in the color map are masked pixels. The third panel shows the spectra after median normalization. The fourth panel shows the spectra after applying SysRem for one iteration. The bottom panel shows the standard deviation from each wavelength channel in the residual.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: Top: S/N map for each of the unprocessed models. The white dashed lines point to the detected K p and V rest values from the H2O POKAZATEL model, (K p, V rest) ∼ (160.0, 2.5) km s−1, marked by the red cross symbol with significances indicated in the lower left corner of each map. These significance values are evaluated at the location of the H2O POKAZATEL signal. The blue plus symbol marks the expected location of the planet. Bottom: same as the top panel but for Welch-t σ with in-trail width of 3.73 km s−1 (FWHM of CARMENES). All maps are derived from SysRem #1. We note that we cannot assess the optimum SysRem iteration for the HCN model since this species cannot be detected.
Paper: Evidence of Water Vapor in the Atmosphere of a Metal-rich Hot Saturn with High-resolution Transmission Spectroscopy
Authors: Sayyed A. Rafi, Stevanus K. Nugroho, Motohide Tamura, Lisa Nortmann, Alejandro Sánchez-López
Figure caption: CCF maps from cross-correlation between the unprocessed H2O POKAZATEL model and SysRem residuals. A brighter color corresponds to higher values, i.e., a better match between the model and data. Left: CCF map as a function of RV values and the transit phase relative to the midpoint. The four horizontal dashed white lines are the estimated four transit contacts, starting from the bottom. The cyan dashed line indicates the expected RV path of the planet across the map. Middle: same as the left panel but the CCF has been shifted to the planetary rest frame and the horizontal axis is now the systemic velocity in the planetary rest frame. Right: the combined in-transit CCF values from the middle panel. The blue vertical dashed line denotes V sys,rest = 0 km s−1. The zeroth SysRem iteration (before fitting for SysRem models) is also shown.