adsabs/AstroCLIMB huggingface dataset:
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Maps of the average residual (Δ[X/H] = [X/H]obs − [X/H]pred) in ﹩{Z}_{{\rm{\max }}}﹩ vs. Rguide for 13 elements. We divide the population into high-Ia (left) and low-Ia (right) populations. Positive average residuals are shown in pinks and oranges, and negative average residuals are shown in greens and blues. Bins with fewer than 20 stars have been excluded.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Same as Figure 3 but for age vs. Rguide.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Distribution of our high-Ia (left) and low-Ia (right) samples in ﹩{Z}_{{\rm{\max }}}﹩ vs. Rguide (top) and age vs. Rguide (bottom).
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Maps of the average [Mg/H] (top), [Fe/Mg] (middle), and age (bottom) for the high-Ia (left) and low-Ia (right) populations in ﹩{Z}_{{\rm{\max }}}﹩ vs. Rguide. Bins with fewer than 20 stars have been excluded.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Eigenvectors of a PCA fit to the residual abundances of the high-Ia population in ﹩{Z}_{{\rm{\max }}}﹩ vs. Rguide (left) and age vs. Rguide (right). The amplitude and sign of the component colors each cell.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: The age vs. average residual (Δ[X/H]) for 13 abundance residuals in the full high-Ia population (black) and subsamples binned by increasing radius (dark blue to teal). Average residuals are calculated in 1 Gyr width bins from 1 to 13 Gyr.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Maps of the average [Mg/H] (top), [Fe/Mg] (middle), and ﹩{Z}_{{\rm{\max }}}﹩ (bottom) for the high-Ia (left) and low-Ia (right) populations in age vs. Rguide. Bins with fewer than 20 stars have been excluded.
Paper: Cooling Process of the High-mass Young Stellar Object G24.33+0.14 Following an Accretion Burst
Authors: Xiaoyun Xu, Xi Chen, Yang Yang
Figure caption: The averaged continuum images of NOEMA (left panel) and ALMA 2019 (middle panel) at the same frequency range, along with their flux ratio image (right panel). The flux ratio was determined using signals exceeding 7 times the rms noise level in both NOEMA and ALMA 2019 images, with rms values of 5.4 mJy beam−1 and 7.9 mJy beam−1, respectively. The white or black ellipse in the lower-right corner of each panel represents the beam size. In the right panel, the black cross denotes the center, R.A. =  ﹩1{8}^{{\rm{h}}}3{5}^{{\rm{m}}}08\mathop{.}\limits^{{\rm{s}}}136﹩, decl. =  ﹩-0{7}^{\circ }3{5}^{{\prime} }0{4}^{{\prime\prime} }.20﹩ (J2000), derived from 2D Gaussian fitting, while the  ×  symbol marks the location of the minimum flux ratio. The black contour delineates a flux ratio of 1.
Paper: Cooling Process of the High-mass Young Stellar Object G24.33+0.14 Following an Accretion Burst
Authors: Xiaoyun Xu, Xi Chen, Yang Yang
Figure caption: The 6.7 GHz methanol maser light curve for G24 (T. Hirota et al. 2022). The green, blue, and red vertical lines mark the ALMA observations in 2016 and 2019, and the NOEMA observation in 2020 at 1.3 mm, respectively.
Paper: Cooling Process of the High-mass Young Stellar Object G24.33+0.14 Following an Accretion Burst
Authors: Xiaoyun Xu, Xi Chen, Yang Yang
Figure caption: Panel (a): schematic of the ring regions used for rotational temperature diagram analysis. Panels (b)–(d) show the rotational temperature diagrams for R0, R1, and R2 regions, respectively. The solid lines in the plots represent the fitting lines (green for the ALMA 2016 data, blue for the ALMA 2019 data, and red for the NOEMA data), which were derived using only six methanol lines, excluding the 229.759 GHz line. Panels (e) through (h) display the rotational temperature, column density, and the ratios of rotational temperatures and methanol column densities between NOEMA and ALMA 2019 data, as well as between ALMA 2019 and ALMA 2016 for regions R0 to R2, respectively. The spatial scales, measured in AU, are based on the semiminor axis of the elliptical rings depicted in panel (a).
Paper: Cooling Process of the High-mass Young Stellar Object G24.33+0.14 Following an Accretion Burst
Authors: Xiaoyun Xu, Xi Chen, Yang Yang
Figure caption: A comparative analysis of the integrated intensities of eight methanol lines, as detected by ALMA 2019 and NOEMA. Panel (a) displays ALMA 2019 data, symbolized by blue diamonds, in contrast to NOEMA data, indicated by red circles. Panel (b) depicts the ratio of integrated intensities for the methanol lines, with NOEMA values relative to those from ALMA 2019. Notably, for the 229.759 GHz line, which is characterized by an outflow structure, the comparison is restricted to the flux emanating from the central hot core region. Panel (c) shows the sizes of the emission regions for different methanol lines observed by NOEMA.
Paper: Cooling Process of the High-mass Young Stellar Object G24.33+0.14 Following an Accretion Burst
Authors: Xiaoyun Xu, Xi Chen, Yang Yang
Figure caption: Methanol line spectra detected from the NOEMA and ALMA 2019 observations. The red line represents NOEMA data, while the blue line corresponds to ALMA 2019 data. These spectral lines were extracted from an elliptical region, centered at the continuum peak position (coordinates R.A. =  ﹩1{8}^{{\rm{h}}}3{5}^{{\rm{m}}}08\mathop{.}\limits^{{\rm{s}}}136﹩ and decl. =  ﹩-0{7}^{\circ }3{5}^{{\prime} }0{4}^{{\prime\prime} }.20﹩; J2000), with a semiaxis 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩3 at a PA of 10°.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: TLS power spectrum periodogram of TOI-6695. The top panel shows the results of the detrended and normalized TESS and OMES light curves. The bottom panel shows the residual TLS power after subtracting the full photodynamical model. The dashed blue line represents the orbital period of the transiting planet candidate, whereas dashed horizontal lines indicate the TLS signal detection efficiency (M. Hippke et al. 2019) power levels of 5.7, 7.0, and 8.3, which correspond to false-alarm-probability (FAP) levels of 10%, 1%, and 0.1%, respectively.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: MLP periodograms for RV and stellar activity data of TOI-6695. The top four panels show the periodograms of the raw and residual RVs after subtracting Keplerian models, panels 5–9 show the periodograms of the stellar activity indicators and the bottom panel shows the RV window function. Dashed blue lines indicate the planetary orbital periods, and the red dashed line and shaded region correspond to the assumed stellar rotational period. Dashed horizontal lines correspond to FAP levels of 10%, 1%, and 0.1%.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: TESS TPFs of TOI-6695 (TIC 118339710), created using tpfplotter. Orange overlays show the aperture used to determine the flux (a white overlay indicates an automatically detected threshold aperture). Gaia DR2 catalog objects are shown as filled red circles sized according to their brightness relative to the target (marked with a white cross).
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Individual transits for TOI-6695. blue:TESS sector 8; red:TESS sector 34; green:TESS sector 61; purple/orange: ground-based data from OM-ES.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Radial velocity time series (top panel) and phase-folded plots of the planetary signals (TOI-6695b, bottom left; TOI-6695c, bottom right). In addition to the RVs from HARPS, CHIRON, PFS, and CORALIE, FEROS data are overlayed as grayed-out diamonds, to show their general agreement with our model, but also their overall poor quality.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Speckle observations for TOI-6695 with NESSI. The red curve represents the 5σ contrast curve. The inset shows the reconstructed image of the star.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Mass–radius diagram for the same sample of planets as in Figures 9 and 10. Marked as blue star symbols are the solar system giant planets, whereas TOI-6695b is shown as a colored star symbol. Solid lines represent exoplanet composition models derived from the theoretical frameworks of C. Mordasini et al. (2012), L. Zeng et al. (2019), and A. Emsenhuber et al. (2021b). Dashed gray lines indicate fixed densities of ρ = 0.1, 0.3, 1.0, 3.0, and 1.0 g cm−3. The shaded region surrounding the fit to the data from A. Emsenhuber et al. (2021b) illustrates the moving standard deviation of their synthetic planets, which arises from variations in core sizes and envelope metallicities (assumed to match stellar values).
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Mass-separation diagram for synthetic planets with neighboring planet pairs close to 3:1 mean-motion resonance marked. The data is drawn from the 50 embryo simulations of A. Emsenhuber et al. (2021b). Giant-planet pairs are found after excluding planets below 50 Earth masses from the systems.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Mass-separation diagram for planets around Sun-like stars (definition according to C. Lehmann et al. 2022; see Section 1, modified to include TOI-6695b). The position of TOI-6695b and TOI-6695c are shown as star symbols.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Mass distribution for planet pairs with a period ratio close to 3. The masses of TOI-6695b, and TOI-6695c are shown as dashed lines.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Thermal evolution for TOI-6695b of the internal temperature and mass–radius diagrams for varying core-mass-fractions, generated using GASTLI. We assumed a core-mass fraction CMF = 0.30 and a solar envelope composition to compute the thermal evolution of TOI-6695b. TOI-6695b’s age of 2.1 ± 0.3 Gyr (shown as red dashed line and shaded region) is consistent with an internal temperature Tint = 50–150 K. Thus, we adopted a value of 100 K for our mass–radius relations. Given its mass, radius and age, TOI-6695b could present a CMF = 0.25–0.35 with a solar composition (see text).
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Same as of Figure 9, but for eccentricity against separation.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: The top-left figure shows the orbital evolution of the planetary semimajor axes from the best fit. The top-right plot shows the evolution of the orbital eccentricities, blue: TOI-6695b; red: TOI-6695c. The bottom panel shows the evolution of the period ratio between the two massive planets.
Paper: TOI-6695: A Pair of Near-resonant Massive Planets Observed with TESS from the WINE Survey 
Authors: Jan Eberhardt, Trifon Trifonov, Thomas Henning, Marcelo Tala Pinto, Rafael Brahm, Andrés Jordán, Nestor Espinoza, Matías I. Jones, Melissa J. Hobson, Felipe I. Rojas, Martin Schlecker, Lorena Acuña, Remo Burn, Gavin Boyle, Rodrigo Leiva, James McCormac, Nicholas Dunckel, Diana Dragomir, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Arvind F. Gupta, Solène Ulmer-Moll, François Bouchy, Monika Lendl, Davide Gandolfi, George R. Ricker, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Transit of TOI-6695b in TESS sector 8 with the TGLC pipeline (blue), the QLP pipeline (orange) and the tesseract pipeline (green).
Paper: Dazzle: Oversampled Image Reconstruction and Difference-imaging Photometry for the Nancy Grace Roman Space Telescope
Authors: Michael D. Albrow
Figure caption: Four examples showing time series of sample 11 × 11 pixel stamp images centered on a star. In each case a PSPL microlensing light curve with parameters u0 = 0.1, t0 = 2160, tE = 400 minutes has been injected directly into the stellar flux before image simulation. The top row of each panel shows the direct simulated images. The central rows are difference images, and the bottom rows are the same as the central rows, but after subtraction of the fitted PSF. Pixels that are saturated in the direct images are colored orange. Light curves from the complete sets of images are shown in Figure 6. The images shown here are at times 0, 1950, 2100, 2160, 2220, 2370, 2865 minutes.
Paper: Dazzle: Oversampled Image Reconstruction and Difference-imaging Photometry for the Nancy Grace Roman Space Telescope
Authors: Michael D. Albrow
Figure caption: rms photometric scatter, σ, in parts per thousand as a function of W146 magnitude. Each point corresponds to a single light curve, with the rms scatter normalized to the baseline (unmagnified) flux in each case. The blue circles are the total expected noise from the simulations of R. F. Wilson et al. (2023; Figure 9 top panel, which are normalized to a 0.5 hr exposure time), and the magenta line is a linear fit to the lower envelope of formal uncertainties for unmagnified data points (that excludes any noise in the reference image or the PSF fitting). The left panels (a) and (c) are for (unmagnified) baseline data points, and the right panels (b) and (d) for magnified data points between 1620 < t < 2700 minutes. The top panels (a) and (b) are for the simulated data set of 192 images (2 days), and the lower panels (c) and (d) are for a data set of 672 images (1 week).
Paper: Dazzle: Oversampled Image Reconstruction and Difference-imaging Photometry for the Nancy Grace Roman Space Telescope
Authors: Michael D. Albrow
Figure caption: Left panel: sample 1k × 1k region showing the locations of injected microlensing events (black dots) and detected variables (colored circles) using a Gaussian kernel with σ = 2.0 in the temporal direction and σ = 1.0 in each of the spatial directions. The color scale indicates the time of maximum in the detection-kernel-convolved image stack. The peak magnification of the injected events was at time 144 on this scale. Right panel: overall recovery rate of injected microlensing events by magnitude and u0.
Paper: Dazzle: Oversampled Image Reconstruction and Difference-imaging Photometry for the Nancy Grace Roman Space Telescope
Authors: Michael D. Albrow
Figure caption: Complete light curves from PSF-fitting to the sets of simulated difference images shown in Figure 5. The red lines are PSPL microlensing fits to the data.
Paper: Dazzle: Oversampled Image Reconstruction and Difference-imaging Photometry for the Nancy Grace Roman Space Telescope
Authors: Michael D. Albrow
Figure caption: Sample 80 × 80 region of a simulated Roman image of the Galactic bulge. Left panel: raw simulated image. Right panel: image at ten times the original sampling from a representation constructed from a stack of 192 randomly dithered images. Panels have identical logarithmic intensity scaling and white pixels are saturated.
Paper: Dazzle: Oversampled Image Reconstruction and Difference-imaging Photometry for the Nancy Grace Roman Space Telescope
Authors: Michael D. Albrow
Figure caption: Hess diagram (shown in a log scale) of stars in the SYNTHPOP catalog used as input to RomanISIM.
Paper: Dazzle: Oversampled Image Reconstruction and Difference-imaging Photometry for the Nancy Grace Roman Space Telescope
Authors: Michael D. Albrow
Figure caption: Luminosity function of stars in the SYNTHPOP catalog used as input to RomanISIM.