adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: power spectrum of LC#2 of V2306 Cyg. The insets contain the lower frequency range (left) and the range around the WD spin signal (right) on an expanded scale. Lower left: orbital waveforms of the three TESS light curves of V2306 Cyg. Lower right: V2306 Cyg light curves folded on 2Pspin in order to highlight that the assumption of the true WD spin period being twice the dominant period seen in the power spectra leads to an unrealistic repetition of fine structures in the waveform. For details, see text.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectra of the light curves of RR Cha. All spectra are normalized to the power of the orbital signal. Left: the low-frequency range including the (truncated) orbital signal Ω, and a negative superhump signal Σ− in LC# 1 (top) that is substituted by a positive superhump Σ+ in LC#2 (bottom). Right: the power spectra at higher frequencies, dominated by the (truncated) second overtone of the orbital signal, and containing a faint signal in LC#1 (top), which A. Bruch (2023a) tentatively interpreted as the WD spin signal, but which is absent in LC#2 (bottom).
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: orbital waveforms (left) constructed from the three light curve of V2069 Cyg (left), and average WD spin waveform (right). Middle: power spectra of LC#1 and LC#2, showing the WD spin signal, its first overtone, and its orbital sideband. Bottom: time-resolved power spectra of LC#1 (left) and LC#2 (right) in a narrow frequency range around the WD spin frequency and its orbital sideband, showing the drastic change of the relative strength of the signals.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: the power spectrum of LC#1 of V709 Cas, containing signals at the orbital frequency Ω and the orbital sideband. The peak tagged with a question mark remains unexplained. Right: average waveform of the WD spin variations of V709 Cas.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: the power spectrum of V2275 Cyg, containing signals at the orbital frequency Ω and at several overtones, and the possible WD spin frequency ω. The peak marked with a question mark remains unexplained. Right: the V2275 Cyg light curve folded on the orbital period, revealing the system to be eclipsing.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: WD spin waveform of V418 Gem. Right: spin period of V418 Gem as a function of time as measured by J. Patterson et al. (2011; black dots) and derived from the TESS light curves (blue dots). The solid line is a linear least-squares fit to the data.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Orbital (left) and WD spin waveforms (right) of DO Dra.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top left: high-frequency part of the power spectrum of V902 Mon, containing signals at multiple combinations of the orbital frequency Ω and the WD spin frequency ω. The red triangles mark overtones of Ω. The blue triangle marks a signal of unidentified origin. Top right: the WD spin period as a function of time, measured by A. Aungwerojwit et al. (2012) H. Worpel et al. (2018), and in the current TESS data. The solid red line is a linear least-squares fit that tentatively defines a spin-up of the WD. Bottom: time-resolved power spectrum in the frequency range between the WD spin frequency and its first and second orbital sidebands, revealing a clear interplay between the strength of the various signals over the length of the observations.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: orbital waveforms of LC#1 and LC#2 of GK Per (left), power spectrum of LC#2, showing the WD spin signal ω and its orbital sideband ω − Ω (middle), and the evolution of the spin period over time (right). The blue dot refers to the average of the spin period measured in the TESS light curves; the black dots are taken from the literature. The red solid line is a linear least-squares fit to the data. Bottom: time-resolved power spectrum of LC#2, revealing that the strength of the WD spin signal is variable over the length of the observations.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: light curves LC#1 (left) and LC#2 (right) of Swift J0746.2−1611. Second and third row: time-resolved power spectra in the range around the WD spin and the orbital sideband frequencies (second row) and the orbital frequency and its first overtone (third row). The horizontal bars indicate the frequencies of various combinations of the orbital and WD spin signals. Bottom: time-resolved representation of the orbital waveform of Swift J0746.2−1611.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Temporal evolution of the period of the spin-orbital sideband variations in V1223 Sgr. The black dots are from J. Patterson et al. (2020); the blue dot refers to the TESS data. The red line is a linear least-squares fit to the data up to 2011.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: orbital waveforms of LC#1 and LC#2 of V1062 Tau (left), the power spectrum of LC#1 in the frequency range around the WD spin period and the orbital sidebands (middle), and the spin waveforms of both light curves. Bottom: time-resolved power spectrum of LC#1 in the frequency range of the WD spin and its orbital sideband.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: power spectrum of KO Vel, showing the orbital signal Ω and its first overtone together the supposed WD spin signal ω (left; two unidentified signals are flagged with question marks), and the orbital waveform (right). Bottom: time-resolved power spectrum revealing that the strength of the WD spin signal is variable over the length of the observations.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: power spectra of the three TESS light curves of Swift J0614+1709 in the frequency range around the WD spin frequency, highlighting the strong variability of the spin-orbital sideband pattern. Middle: orbital and WD spin waveforms of Swift J0614+1709. Bottom: time-resolved WD spin waveform of LC#2 showing a change of structure on timescales of weeks.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Orbital waveform constructed from the three light curves of EX Hya (left) and the average of the WD spin waveform of all light curves (right).
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: power spectrum of V667 Pup. The 2ω signal has been truncated. Right: the waveform of the WD spin variations.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Upper panel: orbital (left) and WD spin waveforms (right) of IGR J17014−4306. Lower panels: power spectra of the light curves of IGR J17014−4306 in the frequency range around the WD spin frequency. The spin signal has been truncated to emphasize fainter structures. Individual peaks are identified (for details, see text). Power has been normalized to the power of the WD spin signal. Note the different vertical scales used for the power spectra.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: average orbital (left) and WD spin waveform (right) of IGR J15094−6649. Middle: power spectrum of LC#2 of IGR J15094–6649. The vertical scale is adapted to show some fainter signals, meaning that stronger signals are truncated. Bottom: time-resolved power spectra of LC#1 (left) and LC#3 (right) of IGR J14094–6649 in a narrow frequency range with a concentration of unstable low-frequency signals.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: power spectrum of Swift J0939.7–3224, showing the orbital signal Ω and its first overtone together with the WD spin signal ω (left), and the orbital waveform (right). Bottom: time-resolved power spectrum revealing that the strength of the WD spin signal is variable over the length of the observations.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Low-frequency part of the power spectrum of LC#3 of IGR J16500−3307 (left) showing a signal F1 at 0.849 days−1 and multiple overtones caused by the contaminating light source Gaia DR3 6027097747864298496. Folding the data on the corresponding period results in the eclipse light curve shown on the right.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: power spectra of both light curves of 1RXS J080114.5−462324 in the range around the orbital frequency and its first overtone. Right: orbital waveform of LC#1 and LC#2 of 1RXS J080114.5−462324.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectrum of Swift J0958.0−4208. The inset shows the range around the WD spin frequency on an expanded scale.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: power spectrum of the sector 82 TESS light curve of 1RXS J163100.5–695000. Bottom: the TESS light curve of sector 82 of 1RXS J163100.5–695000 folded on the WD spin period (left) and the orbital period (right).
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectrum of IGR J16167−4957 with the candidate signal for the WD spin or its orbital sideband.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Orbital waveform of PBC J0927.8−6945 indicating the presence of eclipses.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Properties of light curves LC#1 (left) and LC#2 (right) of IGR J19552+0044. Top row: power spectra of the light curves in the low-frequency range and in the range around the binary and WD rotation frequencies. In each panel, the vertical scale has been adjusted to visualize the fainter signals. This means that the WD spin signal ω is heavily truncated. Second row: representative 1 day sections of the light curves, resolving variations caused by the WD spin. Third row: the entire light curves. The individual WD spin cycles are not resolved, but the variable amplitude of the spin variations stand out. Bottom row: time-resolved representation of the variations of IRG J19552+0044 as a function of the orbital phase.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Upper and middle panels: power spectra of Swift J2116.5+5336 at low frequencies (upper left panel) and in narrow frequency ranges around the orbital frequency and its overtones. Eclipses have been masked in order to remove their strong influence on the power spectrum. The dotted and broken lines in the middle right panel indicate (from bottom to top) the power of the 0.01, 0.001, and 0.0001 false alarm probability levels. Lower panel: time-resolved orbital waveform of Swift J2116.5+5336.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Time resolved orbital waveforms in LC#1 (left) and LC#2 (right) of V1432 Aql. Orbital eclipses cause horizontal dark blue/purple stripes. A double hump reflecting the WD spin variations slowly shifts in phase because of the slightly asynchronous WD rotation period with respect to the orbit. (The vertical disturbances in the left panel are caused by gaps in the light curve.)
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectrum of light curve LC#3 of 1RXS J211336.1+542226 (left) and the waveform of periodic variations of the source ZTF J211335.77+542251.7 that contaminates some of the TESS light curves (right), causing the signals labeled “X” and “2X” in the power spectrum.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Temporal evolution of the WD spin period of 1RXS J213344.1+510725 indicating an acceleration of the rotation. Black dots are spin periods taken from E. de Miguel et al. (2017); blue dots are based on TESS light curves. The solid red line is a linear least-squares fit to all data.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectrum of light curve LC#1 of IGR J21095+4322 with a low-frequency signal that is probably caused by orbital variations, and a high-frequency signal that may be due to the WD rotation.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Orbital (left) and WD spin waveforms (right) of AX J1740.1−2847.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Waveforms of the WD precession period in LC#1 and LC#2 of FS Aur.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectra of the three TESS light curves of RX J2015.6+3711 (upper and lower left panels), and the orbital waveform of the system averaged over all light curves (lower right panel).
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Upper panel: average orbital waveforms of AT Cnc (left), and power spectrum of LC#3, dominated by a positive superhump signal (right). Second row: light curve LC#3 of AT Cnc. The red line is a least-squares fit of a second order polynomial plus a sine curve to the data before the onset of outbursts. Third row: time-resolved power spectrum of LC#3 on the same timescale as the light curve, showing the persistent but strongly variable superhump signal with a slightly increasing frequency during the latter half of the light curve. Lower panel: time-resolved orbital waveform of LC#3 showing the orbital hump changing on the beat period between the orbital and superhump variations (i.e., on the accretion disk precession period).
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: power spectrum of the TESS light curve of V842 Cen (left) and CR-band AAVSO light curves of 2015 March 29 (middle) and April 12 (right). The red curves are fits of a fourth order polynomial (to follow the slow variations) plus a sine curve with a period of 0.08284 days (middle) and 0.07028 days (right). Bottom: time-resolved power spectrum of the low-frequency range of the TESS light curve of V842 Cen, containing many unstable signals together with a persistent periodicity that probably reflects the orbital period. Here, a logarithmic color scale (see the color bar at the bottom) was used for better visualization of the signals.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: power spectra of the TESS light curves of V533 Her in a narrow frequency range around the orbital frequency (marked by a dotted vertical line), exhibiting positive superhumps in LC#1 and LC#2 and negative superhumps in LC#3–LC#5. The inset in the lower left panel contains the power spectrum of LC#5 around the first overtones of the orbital and the superhump frequencies. Right: waveforms of the negative superhumps in LC#3–LC#5.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: power spectrum of the TESS light curve of CW Mon with the orbital frequency and its overtones identified. Note that the truncated 2Ω signal is ∼70 times stronger than the fundamental signal. The frequency of the suspected IP-type variations (T. Kato et al. 2003) is marked by a red bar. Right: light curve folded on the orbital period.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: power spectrum of V426 Oph. The dominating first overtone signal of the orbital period is truncated. The red bar indicates the frequency of the oscillations reported by D. S. Baskill et al. (2005). Right: orbital waveform of V426 Oph with the indication of a shallow eclipse at phase 0.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: superhump waveform observed in LC#3 of V592 Cas. Right: power spectrum of LC#3 of V592 Cas with a broad enhancement of power between 60 and 130 days−1.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: power spectrum LC#1 of AP Cru in a frequency range with unstable signals. Right: time-resolved power spectrum of the same light curve, revealing unstable signals in a limited time interval.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectrum of the TESS light curve of HY Leo with an enhancement of power in the frequency range 20–22 days−1, indicative of QPOs.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Average orbital waveform of V1460 Her.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: light curve of TW Pic in TESS sector 29, exhibiting one longer and two short-lived low states. Bottom: power spectra of the high state phases of LC#1 (left) and of a low state, which occurred between BJD 2459148 and BJD 2459202.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Upper panels: average orbital waveforms of SW UMa in the three TESS light curves exhibiting variations in amplitude and shape (left), power spectrum of LC#2 showing a strong unstable signal of unknown origin (middle), and the power spectrum of LC#3 with strong QPOs in the frequency range between 75 and 82 days−1 (right). Lower panels: light curve LC#2 together with its time-resolved power spectrum in the frequency range around the unknown unstable signal.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: power spectrum of LC#1 of V381 Vel with the orbital signal and its first overtone, together with a second system of frequencies and harmonics (identified by an “X”) that may be due to a contaminating neighboring star (left), orbital waveform of LC#2 (middle), and waveform of the periodicity marked with “X” in the left panel (right). Bottom: time-resolved orbital waveform of LC#1 showing a constant shape but a significantly increasing amplitude over time.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: orbital waveform of IGR J1453−5522 during a brightening (right) and during the other time intervals (left). Middle: light curve of IGR J1453−5522 with a small brightening close to the end. Bottom: time-resolved waveform.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Top: TESS light curve of 2PBC J0658.0−1746. Bottom left: average orbital waveform of the entire light curve. Bottom right: time-resolved orbital waveform.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Low-frequency part of the power spectrum of the TESS light curve of IGR J14257−6117 containing the orbital signal together with several other unidentified signals.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: orbital waveform of LC#1 of SDSS J100516.16+694136.5. Right: time-resolved power spectrum of LC#2 of SDSS J100516.16+694136.5 indicating a weak orbital signal in the first part of the light curve and a sudden strengthening in the second part.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: TESS light curve of 1ES 1210−646 (left), and its orbital waveform (right).
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectrum of LC#1 of 1RXS J015317.9+744641 in the frequency range around the 3486.1 s signal in the conventional (left) and time-resolved form (right).
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Left: power spectra of LC#1 and LC#2 of SGRA J204547.8+672642 in a narrow frequency range around the principle signal. Right: time-resolved waveform of the variations corresponding to the principle power spectrum signal in LC#2.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Power spectrum of the TESS light curve of IGR J18308−1232. The red vertical bar indicates the frequency of the variations observed in X-rays by F. Bernardini et al. (2012). The signal marked as F1 is caused by contamination from the close neighbor ZTF J183049.45−123226.5.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Short-timescale (<1 day) bursts observed in the TESS light curves. For each object, the bursts are sequentially numbered (see Table 7 for more details). All bursts are plotted on the same timescale, which encompasses 3 days for the square panels. The flux scale has been adapted to the individual bursts.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Absolute value of the ﹩{\dot{P}}_{{\rm{spin}}}﹩ as a function of the WD spin period for 12 IPs with measured spin-period variations.
Paper: TESS Light Curves of Cataclysmic Variables. VI. Intermediate Polars
Authors: Albert Bruch
Figure caption: Light curve LC#2 of Lanning 386. Eclipses are masked for clarity.
Paper: Morpho-photometric Classification of KiDS DR5 Sources Based on Neural Networks: A Comprehensive Star–Quasar–Galaxy Catalog
Authors: Hai-Cheng Feng, Rui Li, Nicola R. Napolitano, Sha-Sha Li, J. M. Bai, Yue Dong, Ran Li, H. T. Liu, Kai-Xing Lu, Zhi-Wei Pan, Mario Radovich, Huan-Yuan Shan, Jian-Guo Wang, Wen-Zhe Xi, Ling-Hua Xie, Zun-Li Yuan, Yang-Wei Zhang
Figure caption: The distributions of r-band magnitude (left panel) and u − g color (right panel) for KiDS and SDSS data sets. In both panels, the black histograms represent the overlapping sources between KiDS and SDSS, the orange histograms depict the data from the KiDS survey, while the blue, red, and green histograms denote stars, QSOs, and galaxies identified by SDSS spectroscopy, respectively.