adsabs/AstroCLIMB huggingface dataset:
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Data obtained from the differential output of a double Bracewell nuller, showing the recorded counts as a function of wavelength and time. Top: signal of an Earth twin at 10 pc as recorded by an ideal instrument. Middle: total signal of all astrophysical sources, including the star, the local zodi, and the exozodi, as recorded by an ideal instrument. The counts are almost two orders of magnitude higher than for the pure planet signal and enter the data as white noise, predominantly at the low and the high wavelengths. Bottom: total signal of all astrophysical sources as recorded by a perturbed instrument. We have assumed an rms amplitude perturbation of 0.1%, an rms phase perturbation of 1.5 nm, and an rms polarization angle perturbation of 0.001 rad. The counts are again almost an order of magnitude higher and introduce strong spectral—but also temporal—correlations into the data, as apparent by the vertical stripes.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Definition of the instrumental setup. The observed astrophysical scene consists of the star, the planet, the exozodiacal dust (exozodi; ellipse) and the local zodiacal dust (local zodi; shaded area). The four collectors are shown in the X-array configuration, rotating around the line of sight, which is centered on the star to null its light. The shorter baseline between two collectors is called the nulling baseline, while the longer one is called the imaging baseline. Amplitude, phase, and polarization angle perturbations are introduced in the input beams. The beams are combined in the beam combiner to form different outputs. For a double Bracewell nuller, four inputs are combined into two bright (left and right) and two dark (bottom) outputs. The dark outputs are spatially filtered using a single mode fiber (SMF), fed into a spectrograph and measured on the detectors. The measured signals are then combined in post-processing to form the so-called differential output. This figure is adapted from O. P. Lay (2004).
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Differential intensity response, R4 − R3, of a double Bracewell nuller in the case of an ideal (left) and a perturbed (right) instrument at 10 μm at a given instant in time. The impact of the perturbations is highly exaggerated (rms(δAk) = 10%, rms(δϕk) ≈ 0.28 rad, rms(δθk) = 0.4 rad) here for illustrative purposes. The dashed line corresponds to the path that a planet traces out as the interferometer array rotates around its line of sight to the star.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Covariance for the bottom panel of Figure 4, confirming strong correlations between wavelength bins predominantly at shorter wavelengths, with a falloff toward longer wavelengths. Note that, in this case, correlations are mostly positive. However, this is not generally required, and it depends on the instrument properties.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Illustration of the effect of the whitening transformation on the planetary model (top) and full data (bottom). The correlations visible in the bottom panel of Figure 4 have been removed and the noise appears completely white, whereas the planetary signal is only slightly changed, as expected. Note that the panels now show unitless values and no longer represent physical counts.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Intensity response within the angular extent of the star (dark gray circle) for an ideal (left) and a perturbed (right) instrument using the values from Table 1, and optimistic perturbation levels of rms(δAk) = 0.1%, rms(δpk) ≈ 1.5 nm, and rms(δθk) = 0.001 rad (see Section 4). Top: response at a given instance in time. Whereas the null of the ideal instrument is broad and symmetric, the perturbed instrument shows asymmetries, indicated by contours in light gray dashed lines. Bottom: rms of the response over a full rotation of the array. While the ideal response shows a substantial suppression within the extent of the stellar disk, the suppression is much smaller in the perturbed response, explaining the increase in stellar leakage.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Correlation maps showing the correlation of the data with the planetary templates, y﹩{}^{T}{{\bf{x}}}_{I}/\sqrt{{{\bf{x}}}_{I}^{T}{{\bf{x}}}_{I}}﹩, where xI describes a model with a unit SED. The ideal scenario shows the clearest sign of the planet in the upper right corner. The maps based on unwhitened data show strong artifacts and no longer allow for a detection of the planet in the map. The capability to locate the planet at its correct position is improved significantly for the whitened scenarios.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Top: underlying pink power spectrum with a 1/ω falloff. Bottom: random time series of an amplitude perturbation with an rms of 0.1%.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Left panels: amplitude spectra derived from the data obtained during the primary and secondary eclipses for each target. Right panels: comparison of the theoretical frequencies calculated using GYRE models with the observed frequencies. The labels “primary” and “secondary” in these panels have the same meaning as in Figure 3.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Positions of the targets on the H-R diagram. Blue and red circles represent the primary and secondary components, respectively. The dotted and dashed lines are the MESA binary evolutionary tracks and the observational borders of the δ Scuti instability strip (S. J. Murphy et al. 2019), respectively.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Frequency modulation with the orbital period for HD 117476. The size of the symbols changes with the amplitude values.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: The theoretical pulsation fit to the observations.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Amplitude change of the highest-amplitude frequency of HD 117476 with the orbital phase.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Pseudo-tricolor image of the integrated intensity of 12CO (J = 1–0) (blue), 13CO (J = 1–0) (green), and C18O (J = 1–0) (red) line emission in the velocity range of −115 to 20  km s−1 (top), and Galactic longitude–velocity (l–v) map of the three lines for the same field (bottom), for the G120 region. The data were initially moment-masked (see T. M. Dame 2011, for reference) to suppress noise while integrating over the large velocity ranges; thus the minimum values of the maps are zero. The C18O data were also masked using the 13CO mask. The intensity is in linear scale, with the maximum values of 57.3, 17.3, and 3.0 K  km s−1 for 12CO, 13CO, and C18O, respectively. Integrated intensities greater than these maxima are truncated for better visibility. Some well-studied objects in the region are indicated by circles, including clouds (yellow; B. T. Lynds 1962; J. Yang et al. 1990; Planck Collaboration et al. 2016), H II regions (pink; R. Dubout-Crillon 1976; J. L. Karr et al. 2005), and supernova remnants (red; X. Zhou et al. 2023 and references therein). Most clouds were initially identified as dark nebulae in the optical band by B. T. Lynds (1962), while others were discovered by CO emission (e.g., M120.1+3.0; J. Yang et al. 1990) and sub-millimeter observations (e.g., PLCKECC G127.88+02.66; Planck Collaboration et al. 2016). The cyan dashed line shows the approximate extent of the Cepheus Flare Shell, which contains different MC complexes (I. A. Grenier et al. 1989; J. M. Kirk et al. 2009). A prominent shell-like MC is indicated by an orange dashed circle, which is located around the Galactic coordinate (124°, 1°) and extends ∼3° (X. Chen et al. 2023). In the l–v map, the approximate locations of the spiral arms are indicated, i.e., the Local, Perseus, Outer, and Outer Scutum–Centaurus (OSC) arms (e.g., J. P. Vallée 2008; Y. Sun et al. 2024). The CO emission detected in the Outer and OSC arms is weak. Regions CCL1, CCL2, and CCL3 indicate MCs with large angular sizes and narrow line widths. The velocity ranges of these regions are determined by the velocity dispersion of the corresponding MCs.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Same as Figure 3, but for the G50 region. The velocity range of the integrated intensity map is −95 to 120 km s−1, and the corresponding maximum values are 101.3, 31.4, and 9.9 K km s−1. Some well-studied objects in the region are indicated as well, including those in the W51 region. The W51 region contains different kinds of objects and is an active star-forming region (e.g., J. M. Carpenter & D. B. Sanders 1998 and references therein). The cyan dashed line shows the approximate extent of the Vulpecula Rift (C. M. Dutra & E. Bica 2002), which contains different MC complexes. In the l–v map, MCs with large angular sizes and narrow line widths are indicated by regions CCL4, CCL5, and CCL6. The approximate locations of the Sagittarius, Local+Perseus, Outer, and OSC spiral arms are indicated (e.g., J. P. Vallée 2008; Y. Sun et al. 2024). A gray solid line shows the position of the tangent points with increased velocity by 15 km s−1, estimated based on the Galactic rotation curve (refer to Section 3.3 for details). This additional increase in velocity accounts for the peculiar velocity of MCs. After increasing the velocity by 15 km s−1, the tangent points follow the terminal velocity of the 12CO (J = 1–0) emission well.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Middle row: 12CO (J = 1–0) integrated intensity maps of selected MCs. The MCs are the same as those indicated in the l–v and v–b maps (see Figures 3, 4, and 5). The velocity intervals of the maps are −9.7 to −3.7  km s−1 (blue) and 0.2 to 2.5  km s−1 (red) for the G120 region (left), and 5.3–11.9  km s−1 (blue) and 22.1–25.5 km s−1 (red) for the G50 region (right). The velocity ranges are determined by the velocity dispersions of the corresponding MCs. CCL1 and CCL2 have similar velocities and are covered by the same velocity range. The same is true for CCL4 and CCL5. Different MCs are indicated by dashed rectangles, with colors corresponding to those of the integrated intensity map. The cloud data were initially extracted from the datacube based on connectivity in position–position–velocity space (see Section 3.2 for details) to suppress background emission. Nevertheless, there is still some background emission left, particularly in the G50 region. Bright CO emission can be seen in the velocity range of 5.3–11.9  km s−1 at b ∼ 0°, which originates from the Galactic disk at large distances. Only areas with cloud cover are shown, which are large but not the entire observation coverage. The integrated intensities in the maps are all in linear scale. The minimum values of the maps are zero. The corresponding maximum values of the maps are 22.8, 11.7, 34.8, and 14.0 K  km s−1, respectively. Integrated intensities greater than the maximum values are truncated for better visibility. Other six panels: average 12CO (J = 1–0) spectra extracted from the corresponding regions of CCL1, CCL2, CCL3, CCL4, CCL5, and CCL6, respectively, together with their best-fit Gaussian models (red solid lines) and residuals. The 5σ levels of the residuals are shown by the black dotted lines. The Gaussian components peak at −7.1, −2.0, and 0.5  km s−1 for the CCL1 region, −8.9, −4.8, and −1.2  km s−1 for the CCL2 region, −12.2, −7.2, −1.5, 1.3, and 5.5  km s−1 for the CCL3 region, −4.3, 5.8, and 10.0  km s−1 for the CCL4 region, 6.6, 11.0, and 26.1 km s−1 for the CCL5 region, and 23.8 km s−1 for the CCL6 region. The individual Gaussian components of the corresponding MCs are shown by red dotted lines. The fitted parameters of these components are presented in Table 1.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Galactic velocity–latitude (v–b) maps of 12CO (J = 1–0) (blue), 13CO (J = 1–0) (green), and C18O (J = 1–0) (red) line emission in the Galactic longitude ranges of 119﹩\mathop{.}\limits^{\unicode{x000b0}}﹩75–130﹩\mathop{.}\limits^{\unicode{x000b0}}﹩25 (left) and 44﹩\mathop{.}\limits^{\unicode{x000b0}}﹩75–60﹩\mathop{.}\limits^{\unicode{x000b0}}﹩25 (right). The data were initially moment-masked to suppress noise. The C18O data were also masked using the 13CO mask. Regions of the same MCs as indicated in the l–v maps in Figures 3 and 4 are shown. The velocity ranges of the regions are determined by the corresponding inter-cloud velocity dispersion. Gray solid lines indicate the position of the Galactic midplane corresponding to the Galactic longitude ranges, estimated based on the Galactic rotation curve (refer to Section 3.3 for details). The midplane closer than 300 pc is not shown.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Signal-to-noise ratio distribution of 12CO (J = 1–0), 13CO (J = 1–0), and C18O (J = 1–0) line emission. There are approximately 5.17 × 109 voxels in total. Normalized numbers of all voxels are shown by black solid lines, and selected voxels with signal-to-noise ratios below 3 for 12CO, 3.5 for 13CO, and 4.2 for C18O are shown by red solid lines. The negative intensity voxels are symmetrically mirrored to positive values via the zero-point (blue). Number ratios between all voxels and the negative plus mirror voxels are shown by black dotted lines, and ratios for the selected voxels are shown by red dotted lines.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: rms noise maps of 12CO (J = 1–0), 13CO (J = 1–0), and C18O (J = 1–0) line emission.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Cloud-to-cloud velocity dispersion as a function of galactocentric distance. The velocity dispersion is estimated by subtracting the distance-dependent velocity variation induced by projection effects from the dispersion of the modified velocity. The dispersion of the modified velocities for each Galactic disk segment is estimated by Gaussian fitting to the distribution of the modified systemic velocities of the corresponding MCs (FWHM/2.355; see Figure 15). The distance-dependent velocity variation induced by projection effects is evaluated using the change in projection angle with distance and the result of the trend of velocity change along the Galactic longitude. The velocity dispersion of each MC itself is not taken into account. Diamonds indicate the segments in the G50 region, and crosses indicate the segments in the G120 region. The Perseus–G120 segment is indicated by a star. The Local arm segments are eliminated due to incomplete coverage. A linear fit is performed, and the result of the fit is shown by a black solid line. The OSC–G50 segment is excluded from the fit because its velocity dispersion cannot be determined via Gaussian fitting due to an insufficient number of MC samples. The Perseus–G120 segment is also excluded due to its peculiar velocity field. The corresponding fitting parameters are indicated in the upper-right corner.
Paper: The DELVE Quadruple Quasar Search. I. A Lensed Low-luminosity Active Galactic Nucleus
Authors: Paul L. Schechter, Dominique Sluse, Erik A. Zaborowski, Alex Drlica-Wagner, Cameron Lemon, Frederic Dux, Frederic Courbin, Angela Hempel, Martin Millon, Tommaso Treu, Raul Teixeira, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Peter S. Ferguson, Robert A. Gruendl, David J. James, Clara E. Martínez-Vázquez, Pol Massana, Sidney Mau, Burçin Mutlu-Pakdil, Noëlia E. D. Noël, Andrew B. Pace, Joanna D. Sakowska, Guy S. Stringfellow, Erik J. Tollerud, A. Katherina Vivas, Alfredo Zenteno
Figure caption: (a) DELQQ 1258–0319 observed with a Sloan g filter for 900 s with the IMACS f/4 camera on the Magellan Baade telescope. A negative grayscale is used to highlight the low surface brightness of the central lens, which is substantially fainter than the four images surrounding it. (b) Four point sources, A, B, C, and D, have been fitted and subtracted. A rectangular hyperbola (red) has been drawn through the fitted positions. According to H. J. Witt (1996), if the potential is elliptical, the hyperbola’s asymptotes (magenta) are parallel to its major and minor axes, and the lensing galaxy must lie on the longer, primary branch of the hyperbola. A faint source, which we take to be the lensing galaxy, is consistent with Witt’s prediction. (c) A point source has been fitted to the lensing galaxy, which is too faint to permit determination of its extent. White regions indicate oversubtraction of the point sources. (d) A substantial residual southeast of image C, which we call E, has been fitted by a point source and subtracted. The positions from this fit are shown in panel (b) as white circles.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Raw B-band polarization measurements of HD 189733 obtained at Gemini North on UT 2018 August 1–7, which are dominated by observations on the last night (gold points). Top left: Stokes q (linear polarization) modulation as a function of parallactic angle. Telescope linear polarization is modulated by parallactic angle with amplitude Δ(qTP, uTP) = 0.2620% ± 0.0034% (S. J. Wiktorowicz et al. 2023), where the best-fit curve from Equation (2a) is shown in black. Uncertainties in most data points are smaller than the size of the data points. Top right: same as at top left but for Stokes u (linear polarization, Equation (2b)). Bottom left: same as at top left but for Stokes v (circular polarization, Equation (2c)). Bottom right: temporal variation of parallactic angle, which rotates rapidly as the target crosses the meridian (black dashed lines) around 20:00 LST. This rapid meridian crossing provides the bulk of the telescope polarization modulation necessary for accurate calibration.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Top: POLISH2 B-band Stokes q measurements obtained at the Lick 3 m (blue points) and Gemini North (red points) compared to the best-fit SiO2 scattering model (reff = 0.04  μm, Ω = 13°, solid purple curve). The full suite of pure Rayleigh, SiO2, MgSiO3 (labeled “Silicates”), and MnS scattering models are also shown (gray regions). No models produce a significant rainbow feature that may explain outliers at orbital phases 0.65 or 0.85. Bottom: same as at top but for Stokes u. Measured peak linear polarization Δp is 53.4% ± 3.8% larger than expected from the most polarized models.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Same as in Figure 3 but zoomed in to the orbital phase range where Gemini North and Lick 3 m data overlap. Gemini and Lick data reject a zero-polarization model with 7.2σ and 2.9σ confidence, respectively. Spline, Matlab pchip, and Matlab makima interpolations of the Lick 3 m and Gemini North data are given by blue and red curves, respectively.
Paper: A Scatter of Light from a Polarized World
Authors: Sloane J. Wiktorowicz, Pushkar Kopparla, Jiazheng Li, Yuk L. Yung
Figure caption: Polarization and photometry of HD 189733b obtained in the Gemini North/Lick 3 m orbital phase overlap region. Top: POLISH2 B-band Stokes q measurements of HD 189733 obtained at both the Lick 3 m (blue points) and Gemini North (red points) and phased to the orbital period of the planet. Best-fit Rayleigh (solid gold), silicate (SiO2/MgSiO3, solid green), and MnS (dashed purple) polarization models are shown. Shown in solid light blue is the best-fit silicate model when combining POLISH2 polarimetry with Hubble photometry (T. M. Evans et al. 2013). Middle: same as the top but for Stokes u. Bottom: self-consistent photometric phase curves from the above polarization models in addition to a Hubble secondary eclipse measurement (T. M. Evans et al. 2013). Since secondary eclipse only occurs during a short interval centered at orbital phase 0.5, Hubble does not provide scattered light constraints during the rest of the planetary orbit.