adsabs/AstroCLIMB huggingface dataset:
Paper: Primordial Black Holes as Coma Cluster Dark Matter and the Unresolved γ-Ray Background
Authors: Jeremy Mould, Bhashin Thakore
Figure caption: The proportion of PBH fuel consumed as a function of black hole mass after 206 Myr (top left), 855 Myr (top right), 3.5 Gyr (bottom left) and 14 Gyr (bottom right). In each subplot, the x-axis is the PBH mass bins and the y-axis is the fraction of total PBH mass remaining after 10 timesteps. The colored lines indicate the sequence of timesteps with the first in black and the last in blue, as seen in the vertical color bar in the first subplot. As time passes, progressively more of the initial PBH reservoir is drained, with age at the end of the numbered subplot in Myr and Gyr and the power in GeV/s as Hawking radiation yield per solar mass of DM. If the energy of the cutoff were detected at a local redshift, it would give an age dependent on h, k, and G, rather than on the expansion of the Universe.
Paper: Primordial Black Holes as Coma Cluster Dark Matter and the Unresolved γ-Ray Background
Authors: Jeremy Mould, Bhashin Thakore
Figure caption: The window function of Primordial Black Hole evaporation in γ-rays (dashed red) compared to that of the DES Y3 lensing window functions (solid lines) up to redshift z = 1.5. The PBH window function is computed in the energy bin 2.290–4.786 GeV and normalized by the average UGRB intensity at the same energy.
Paper: Primordial Black Holes as Coma Cluster Dark Matter and the Unresolved γ-Ray Background
Authors: Jeremy Mould, Bhashin Thakore
Figure caption: X-ray clusters in the MCXC-II catalog with redshift <0.2. This cut was made to improve completeness in the southern celestial hemisphere. The long axis is Galactic longitude, the short axis, Galactic latitude. The red dot in the first quadrant is the Great Attractor (A. Dressler 1991), partly obscured by the Galactic plane. The nearby concentration of x-ray clusters form part of the superstructure Quipi according to H. Böhringer et al. (2025).
Paper: Primordial Black Holes as Coma Cluster Dark Matter and the Unresolved γ-Ray Background
Authors: Jeremy Mould, Bhashin Thakore
Figure caption: X-ray clusters in the MCXC-II catalog enlarged from the previous figure. A control sample is shown below it around the south galactic pole. The red arcs are lines of constant R.A.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: Polarized surface brightness (Qϕ × r2) polar plot of the inner ring (15–35 au). The left column is the original data, while the right column has been transformed to correct for Keplerian motion. The y-axis is separation in au. The observation date is in the top left, while the instrument and filter combination is in the top right. The disk minor axis is marked with dashed white lines. A ﹩\sinh ﹩ stretch is used to emphasize features in the ring, and the values are normalized from 0 to the maximum value in the inner ring (the same as Figure 4). The direction of Keplerian rotation is shown with a white arrow in the top left plot.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: The same as Figure 4, but the disk’s outer ring (45–110 au). The CHARIS data have missing wedges shown with crosshatches due to the rectangular field stop.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: Radial profiles from the mean deprojected scattered light image corrected for stellar irradiation (Qϕ × r2; red curve) and the projected ALMA 1.3 mm dust continuum emission from S. Pérez et al. 2019 (gray curve). Both curves are shaded with their 1σ measurement uncertainty from the standard error. The five dust peaks (B0–B4) are denoted with gray vertical lines. The inner and outer scattered light peaks are shaded in red according to the 1σ uncertainties measured from bootstrap resampling. The gap in the scattered light image (D2) is denoted with a gray dashed line, and the gap width is shaded in gray.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: Polarized surface brightness images (Qϕ × r2), shown with an asinh color scale to emphasize the cavity and outer ring. Each image is scaled from 0 to the maximum value in the inner ring (15–35 au). North is up and east is left in all images.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: Uϕ × r2 images from each epoch, normalized to the same limits as Figure 3 and shown with a linear scale. A 34 au scale bar is shown in the bottom left of all panels. North is up and east is left in all images.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: 2018 July 15 ZIMPOL VBB Qϕ × r2 polar image of the inner ring with annotations. C1–C3 are bright clumps, while S1 and S2 are dimmer shadow-like features. The region of outward bowing is marked with dotted lines.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: The same as Figure 3, but zoomed into the inner ring, and shown with a sinh color scale.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: Similar to Figure 5, but zoomed into the inner ring.
Paper: Dynamical Analysis of the HD 169142 Planet-forming Disk: Twelve Years of High-contrast Polarimetry
Authors: Miles Lucas, Michael Bottom, Ruobing Dong, 董若冰, Myriam Benisty, Mario Flock, Maria Vincent, Jonathan Williams, Kyohoon Ahn, Thayne Currie, Vincent Deo, Olivier Guyon, Tomoyuki Kudo, Lucinda Lilley, Julien Lozi, Maxwell Millar-Blanchaer, Barnaby Norris, Sebastián Pérez, Boris Safonov, Peter Tuthill, Taichi Uyama, Sébastien Vievard, Manxuan Zhang
Figure caption: ALMA 1.3 mm continuum observations from L. M. Pérez et al. (2018). The data are shown with a slight asinh stretch. North is up, and east is left. The synthesized beam profile is shown with an ellipse in the bottom right.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: SPOC DV summary report for TESS SPOC TCE TIC 55383975-1-S1-65 (TOI 694.01). Photometric disposition is PC; however, the follow-up spectroscopic observations indicates that this is indeed an SEB1.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Albedo and planet effective temperature comparison statistics. When weak secondary MES > 7.1, the high values of these statistics indicate an FP. However, small values are uninformative.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Number of non-planets in the top k TCEs as ranked by ExoMiner++ using the TESS+Kepler-aggregate strategy.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Precision@k for the top k TCEs for different values of k and different models.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Score histograms of different subcategories in photometric disposition.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Score histograms of different subcategories in spectroscopic disposition.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Distribution of centroid offset statistic.
Paper: Characterizing the Time Variability of 2M1207 A + b with JWST NIRSpec/PRISM
Authors: Arthur D. Adams, Yifan Zhou, Gabriel-Dominique Marleau, Daniel Apai, Beth A. Biller, Aarynn L. Carter, Johanna M. Vos, Niall Whiteford, Stephan Birkmann, Theodora Karalidi, Xianyu Tan, Jason Wang, Yuhiko Aoyama, Brendan P. Bowler, Mickaël Bonnefoy, Jun Hashimoto
Figure caption: The retrieved posterior distributions for the Octofitter fit to the available position angles and angular separations available in the literature for 2M1207, including the new datum presented in this work. The maximum-likelihood estimates of the orbital parameters is shown with the red point and crosshairs in each subplot. In the top-right plot we show a comparison of the posterior distributions for the orbital inclination for three choices of priors. The black histogram shows the “base” run with the priors shown in Table 4. The blue histogram shows a run with all priors the same except for a broader prior in parallax (1–100 mas). The red histogram shows a run with a prior on the total system mass taken from a combination of constraints from G. Chauvin et al. (2005) and Z. Zhang et al. (2025).
Paper: Characterizing the Time Variability of 2M1207 A + b with JWST NIRSpec/PRISM
Authors: Arthur D. Adams, Yifan Zhou, Gabriel-Dominique Marleau, Daniel Apai, Beth A. Biller, Aarynn L. Carter, Johanna M. Vos, Niall Whiteford, Stephan Birkmann, Theodora Karalidi, Xianyu Tan, Jason Wang, Yuhiko Aoyama, Brendan P. Bowler, Mickaël Bonnefoy, Jun Hashimoto
Figure caption: The distribution of orbital solutions for the position angles and angular separation data for 2M1207 b. The color denotes the mean anomaly across each orbit. The plots in the right column zoom in more closely to the data; the isolated position parameters are shown in the bottom-left panel.
Paper: Characterizing the Time Variability of 2M1207 A + b with JWST NIRSpec/PRISM
Authors: Arthur D. Adams, Yifan Zhou, Gabriel-Dominique Marleau, Daniel Apai, Beth A. Biller, Aarynn L. Carter, Johanna M. Vos, Niall Whiteford, Stephan Birkmann, Theodora Karalidi, Xianyu Tan, Jason Wang, Yuhiko Aoyama, Brendan P. Bowler, Mickaël Bonnefoy, Jun Hashimoto
Figure caption: A comparison of the variability displacements across time of the two pairs of light curves shown in Figure 3. Top: the variability amplitudes across time for the Hα-sensitive wavelength elements (0.65–0.66 μm) with those >4.35 μm. We can evaluate the covariance of the light curves in time with a Spearman rank correlation coefficient, which returns a value of approximately 0.71. Bottom: the variability amplitudes across time for the light curves at 0.73–0.80 and 3.36–3.38 μm, two regions whose sinusoidal trend models return mutually consistent parameter values.
Paper: Characterizing the Time Variability of 2M1207 A + b with JWST NIRSpec/PRISM
Authors: Arthur D. Adams, Yifan Zhou, Gabriel-Dominique Marleau, Daniel Apai, Beth A. Biller, Aarynn L. Carter, Johanna M. Vos, Niall Whiteford, Stephan Birkmann, Theodora Karalidi, Xianyu Tan, Jason Wang, Yuhiko Aoyama, Brendan P. Bowler, Mickaël Bonnefoy, Jun Hashimoto
Figure caption: A comparison of the variability displacements of the Hα light curves between 2M1207 A and b. The correlation coefficient between the two light curves, which probes the potential for contamination in the signals between the objects, is approximately 0.53.
Paper: Tools for High-precision Photometry from Wide-field Color Images
Authors: Kaloyan Penev, Angel Romero, S. Javad Jafarzadeh, Olivier Guyon, Wilfred Gee, Preethi Krishnamoorthy
Figure caption: WASP-33 b exoplanet transit, observed by PANOPTES (blue points and circles), TESS (red points), and theoretical lightcurve based on best known system parameters (green curve). The raw PANOPTES-DSLR measurements, originating from the four color channels of 4 cameras in Hawaii (Mauna Loa observatory) and California (Mt Wilson) are shown as blue points. The blue points are binned in time to create the blue circles and corresponding error bars.
Paper: Tools for High-precision Photometry from Wide-field Color Images
Authors: Kaloyan Penev, Angel Romero, S. Javad Jafarzadeh, Olivier Guyon, Wilfred Gee, Preethi Krishnamoorthy
Figure caption: Top: 88 × 88 pixel portion, centered on WASP-33, of a 5208 × 3476 pixel image taken with a DSLR camera. The pattern is due to the Bayer mask. Bottom: arrangement of pixels sensitive to different colors in super-pixels (highlighted area) in a DSLR detector.
Paper: Tools for High-precision Photometry from Wide-field Color Images
Authors: Kaloyan Penev, Angel Romero, S. Javad Jafarzadeh, Olivier Guyon, Wilfred Gee, Preethi Krishnamoorthy
Figure caption: Posterior distribution of the transit timing, depth and duration of WASP-33 b using only the PANOPTES observations from Figure 2. The timing is shown as offset from the nominal literature ephemeris and the blue lines show the nominal literature values for the depth and duration.
Paper: Consequences of Non-Gaussian Instrumental Noise in Perturbed Nulling Interferometers
Authors: Felix A. Dannert, Philipp A. Huber, Thomas Birbacher, Romain Laugier, Markus J. Bonse, Emily O. Garvin, Adrian M. Glauser, Veronika Oehl, Sascha P. Quanz
Figure caption: Extrapolation of the true critical value Tα as a function of the equivalent Gaussian critical value ﹩{T}_{{ \mathcal N }}﹩ for noise samples of different IMB to Gaussian noise composition. The colored lines show the extrapolation based on logistic fits to the relation cut in the ﹩{T}_{{ \mathcal N }}﹩ direction. The gray lines are the measured relations for different σIMB to σGauss values.
Paper: Tools for High-precision Photometry from Wide-field Color Images
Authors: Kaloyan Penev, Angel Romero, S. Javad Jafarzadeh, Olivier Guyon, Wilfred Gee, Preethi Krishnamoorthy
Figure caption: The scatter (median absolute deviation from the median) of the individual channel lightcurves of PANOPTES observations of a 10° × 15° field centered on FU Orionis. From top to bottom: red channel, first green channel, second green channel, blue channel.
Paper: Consequences of Non-Gaussian Instrumental Noise in Perturbed Nulling Interferometers
Authors: Felix A. Dannert, Philipp A. Huber, Thomas Birbacher, Romain Laugier, Markus J. Bonse, Emily O. Garvin, Adrian M. Glauser, Veronika Oehl, Sascha P. Quanz
Figure caption: Sketch of a measurement with a dual Bracewell nulling interferometer. Source: the astrophysical scene as captured by the sky brightness distribution Bsky. Modulation: configuration of the nulling interferometer as a rectangular Emma-X design. The interferometer rotates to modulate the exoplanet signal. Instrument: the light received from collectors 1–4 is assumed to be perturbed independently in phase, amplitude, and polarization before it enters the beam combiner. In the two-staged beam combination the applied phase shifts of 0, π/2, and π are indicated. The two final outputs are spatially filtered and spectrally resolved before hitting the detectors, after which the signals are incoherently subtracted to form the differential output. Characteristic signal: per wavelength bin, the measurement results in a single time series capturing the flux integrated over the FOV. The modulation of the signal due to the rotation is characteristic for the position of the exoplanet.
Paper: Consequences of Non-Gaussian Instrumental Noise in Perturbed Nulling Interferometers
Authors: Felix A. Dannert, Philipp A. Huber, Thomas Birbacher, Romain Laugier, Markus J. Bonse, Emily O. Garvin, Adrian M. Glauser, Veronika Oehl, Sascha P. Quanz
Figure caption: Impact of non-Gaussian noise. Left: the analytically evaluated critical value of the test statistic Tα in relation to the critical value assuming a Gaussian distribution ﹩{T}_{{ \mathcal N }}﹩. The color indicates the ratio between the standard deviation of the IMB noise σIMB and the Gaussian noise ﹩{\sigma }_{{ \mathcal N }}﹩. The ﹩{T}_{\alpha }={T}_{{ \mathcal N }}﹩ diagonal is indicated by the dashed line. Right: lookup table for the test statistic correction factor ﹩{T}_{{ \mathcal N }}/{T}_{\alpha }﹩. Values for ﹩{T}_{{ \mathcal N }}\leqslant 5﹩ are interpolated directly from data in the left panel. For ﹩{T}_{{ \mathcal N }}\gt 5﹩ the data are extrapolated using logistic fits (see Appendix D). The triangles indicate significance and noise composition in the 10 μm spectral bin during a 4–18.5 μm broadband detection and characterization of an Earth twin.
Paper: Consequences of Non-Gaussian Instrumental Noise in Perturbed Nulling Interferometers
Authors: Felix A. Dannert, Philipp A. Huber, Thomas Birbacher, Romain Laugier, Markus J. Bonse, Emily O. Garvin, Adrian M. Glauser, Veronika Oehl, Sascha P. Quanz
Figure caption: Relative contribution of noise sources and validation using LIFESIM for fundamental noise only. Top: for the reference case (Table 1) the black line shows the expected total planet signal. The gray lines show the expected residual random noise contributions of the astrophysical noise sources after their subtraction. Bottom: the black curve shows the S/N for the signal and noise contributions in the top panel, with the root-square-summed total S/N given in black text. For validation of this result, a simulation of the setup in Table 1 is run with LIFESIM. The difference between LIFESIM and the black S/N curve is shown by the orange curve, with the total S/N difference given in text.
Paper: Consequences of Non-Gaussian Instrumental Noise in Perturbed Nulling Interferometers
Authors: Felix A. Dannert, Philipp A. Huber, Thomas Birbacher, Romain Laugier, Markus J. Bonse, Emily O. Garvin, Adrian M. Glauser, Veronika Oehl, Sascha P. Quanz
Figure caption: Slice through the relation between ﹩{T}_{{ \mathcal N }}﹩ and Tα for ﹩{T}_{{ \mathcal N }}=4﹩ plotted over the amount of non-Gaussian noise in the data. Black points indicate data measured from bootstrapping. The orange line depicts a logistic fit of the data. Drawn in gray is the interest area in which 99% of change in Tα occurs. The bottom panel shows the residuals of the fit.