adsabs/AstroCLIMB huggingface dataset:
Paper: GRB 240529A: A Tale of Two Shocks
Authors: Tian-Rui Sun, Jin-Jun Geng, Jing-Zhi Yan, You-Dong Hu, Xue-Feng Wu, Alberto J. Castro-Tirado, Chao Yang, Yi-Ding Ping, Chen-Ran Hu, Fan Xu, Hao-Xuan Gao, Ji-An Jiang, Yan-Tian Zhu, Yongquan Xue, Ignacio Pérez-García, Si-Yu Wu, Emilio Fernández-García, María D. Caballero-García, Rubén Sánchez-Ramírez, Sergiy Guziy, I. Olivares, Carlos Jesus Pérez del Pulgar, A. Castellón, S. Castillo, Ding-Rong Xiong, Shashi B. Pandey, David Hiriart, Guillermo García-Segura, William H. Lee, I. M. Carrasco-García, Il H. Park, S. Jeong, Petrus J. Meintjes, Hendrik J. van Heerden, Antonio Martín-Carrillo, Lorraine Hanlon, Bin-Bin Zhang, L. Hernández-García, Maria Gritsevich, Andrea Rossi, Elisabetta Maiorano, Felice Cusano, Paolo D'Avanzo, Matteo Ferro, Andrea Melandri, Massimiliano De Pasquale, Riccardo Brivio, Min Fang, Lu-Lu Fan, Wei-Da Hu, Zhen Wan, Lei Hu, Ying-Xi Zuo, Jin-Long Tang, Xiao-Ling Zhang, Xian-Zhong Zheng, Bin Li, Wen-Tao Luo, Wei Liu, Jian Wang, Hong-Fei Zhang, Hao Liu, Jie Gao, Ming Liang, Hai-Ren Wang, Da-Zhi Yao, Jing-Quan Cheng, Wen Zhao, Zi-Gao Dai
Figure caption: The left image exhibits the BOOTES-7 image observed at 09:44:40 on 2024 May 29 with a 60 s exposure and a magnitude limit of 18.3 mag in the clear filter. The right image exhibits the WFST image observed in the g band at 18:29:01 on 2024 May 29 with a 180 s exposure and a magnitude limit of 22.1. Note that in both images, the circle indicates the position of GRB 240529A, with north registered as up.
Paper: JWST/MIRI Detection of [Ne V], [Ne VI], and [O IV] Wind Emission in the O9 V Star 10 Lacertae
Authors: David R. Law, Calum Hawcroft, Linda J. Smith, Alexander W. Fullerton, Christopher J. Evans, Karl D. Gordon, Nimisha Kumari, Claus Leitherer
Figure caption: Ionization fraction q as a function of mass-loss rate for O3+ (blue) and Ne4+ + Ne5+ (red) ions. Solid and dashed lines show electron temperatures of Te = 35 and 200 kK, respectively. Values of q = 1 represent the lower limit of the mass-loss rate for each curve assuming that the indicated ionization states comprise the total contribution of the respective element in the line-forming region. Values of q > 1 (gray shaded region) are thus unphysical, and any unaccounted-for species will drive q < 1. Vertical black ticks show theoretical mass-loss rate predictions from R. Björklund et al. (2021), B21; J. Krtička & J. Kubát (2017), K17; and J. S. Vink et al. (2000), V00.
Paper: JWST/MIRI Detection of [Ne V], [Ne VI], and [O IV] Wind Emission in the O9 V Star 10 Lacertae
Authors: David R. Law, Calum Hawcroft, Linda J. Smith, Alexander W. Fullerton, Christopher J. Evans, Karl D. Gordon, Nimisha Kumari, Claus Leitherer
Figure caption: Continuum-subtracted spectrum of 10 Lac from PID 1524 (solid black line), zoomed in around the wavelengths of the broad [Ne VI], [Ne V], and [O IV] features. The light blue line shows the spectrum observed 16 months later by PID 3779 for comparison. The solid red line represents the corresponding continuum-subtracted CALSPEC model; the emission feature at 14.183 μm is H I 13–9. Dashed vertical lines indicate ±1170 km s−1  around the rest wavelength of each line.
Paper: JWST/MIRI Detection of [Ne V], [Ne VI], and [O IV] Wind Emission in the O9 V Star 10 Lacertae
Authors: David R. Law, Calum Hawcroft, Linda J. Smith, Alexander W. Fullerton, Christopher J. Evans, Karl D. Gordon, Nimisha Kumari, Claus Leitherer
Figure caption: Flux ratios for [Ne V] 14.3 μm/24.3 μm as a function of the electron temperature Te and density ne. Colored lines show model estimates produced using EQUIB (I. D. Howarth & S. Adams 1981; A. Danehkar 2020) for values of Te in the range 35–200 kK. The solid black line and gray shaded region show the measured flux ratio and 1σ uncertainty for 10 Lac, respectively.
Paper: JWST/MIRI Detection of [Ne V], [Ne VI], and [O IV] Wind Emission in the O9 V Star 10 Lacertae
Authors: David R. Law, Calum Hawcroft, Linda J. Smith, Alexander W. Fullerton, Christopher J. Evans, Karl D. Gordon, Nimisha Kumari, Claus Leitherer
Figure caption: Mass-loss rates as a function of luminosity for Galactic O stars using results from T. Repolust et al. (2004), F. Martins et al. (2005), and P. A. Crowther et al. (2006). Circles, triangles, and squares correspond to luminosity classes V, III, and I, respectively. Solid and dashed lines show theoretical mass-loss rate predictions from J. S. Vink et al. (2000) and R. Björklund et al. (2021), respectively.
Paper: A 2.9 hr Periodic Radio Transient with an Optical Counterpart
Authors: N. Hurley-Walker, S. J. McSweeney, A. Bahramian, N. Rea, C. Horváth, S. Buchner, A. Williams, B. W. Meyers, Jay Strader, Elias Aydi, Ryan Urquhart, Laura Chomiuk, T. J. Galvin, F. Coti Zelati, Matthew Bailes
Figure caption: Left: DECam r-band image of the vicinity of the radio transient, with its 1σ localization regions by MWA (dashed magenta circle) and MeerKAT (solid cyan circle) overplotted. Right: SOAR (4m-class) low-resolution optical spectrum of the optical counterpart (blue solid line) overplotted on an example M3V star (gray line; flux and extinction renormalized to match). The Swift-UVOT limits are shown with downward-pointing arrows. An AR Sco-like WD with T = 11,500 K, M = 0.8 M ⊙ is shown with the dotted pink line, and the summed WD+M3V spectrum is shown with a solid pink line.
Paper: A 2.9 hr Periodic Radio Transient with an Optical Counterpart
Authors: N. Hurley-Walker, S. J. McSweeney, A. Bahramian, N. Rea, C. Horváth, S. Buchner, A. Williams, B. W. Meyers, Jay Strader, Elias Aydi, Ryan Urquhart, Laura Chomiuk, T. J. Galvin, F. Coti Zelati, Matthew Bailes
Figure caption: Autocorrelation analysis of both the correlator lightcurve sampled at 2 s ((a) and (b)) and the PTUSE lightcurve sampled at 5 ms ((c) and (d)) and subsets of the PTUSE data with significant microstructure ((e) and (f)). The autocorrelations in (b) and (d) include only the corresponding data highlighted in panels (a) and (c); a vertical offset has been applied to the blue curve in panel (d) for visual clarity. The preprocessing of the PTUSE data (see main text) has effectively removed variations on timescales ≳0.4 s but retains finer time structures. In at least one section (colored blue, with detail shown in panel (f)), a quasiperiodicity of ∼40 ms is clearly evident. The dynamic spectra have been dedispersed to 36.541 pc cm−3. In panel (f), a white curve indicates how a zero-DM transient signal would appear.
Paper: A 2.9 hr Periodic Radio Transient with an Optical Counterpart
Authors: N. Hurley-Walker, S. J. McSweeney, A. Bahramian, N. Rea, C. Horváth, S. Buchner, A. Williams, B. W. Meyers, Jay Strader, Elias Aydi, Ryan Urquhart, Laura Chomiuk, T. J. Galvin, F. Coti Zelati, Matthew Bailes
Figure caption: Various model fits to the timing residuals assuming an initial folding period of 10496.5531 s. The fitted parameters are P, the rotation period; ﹩\dot{P}﹩, the spin-down rate; P long, a sinusoidal period; and ﹩A\sin i﹩, the sinusoidal amplitude projected onto the line of sight. Reported errors are 1σ. The fit that includes only P and ﹩\dot{P}﹩ (b) produces a nonphysical (negative) spin-down. The fits with P long (c) and (d) are favored over those without (a) and (b).
Paper: A 2.9 hr Periodic Radio Transient with an Optical Counterpart
Authors: N. Hurley-Walker, S. J. McSweeney, A. Bahramian, N. Rea, C. Horváth, S. Buchner, A. Williams, B. W. Meyers, Jay Strader, Elias Aydi, Ryan Urquhart, Laura Chomiuk, T. J. Galvin, F. Coti Zelati, Matthew Bailes
Figure caption: Allowable inclination angles i for a circular orbit with period P long = 2283 days of an unseen radio emitter and the visible M3 dwarf. The gray shaded area shows the mass range of magnetic WDs (L. L. Amorim et al. 2023), and the red shaded area shows the mass range of M3V dwarfs (C. Cifuentes et al. 2020). For an MCV interpretation, a low inclination angle is preferred.
Paper: New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: R. Ramesh, V. Muthu Priyal, Jagdev Singh, K. Sasikumar Raja, P. Savarimuthu, Priya Gavshinde
Figure caption: Temporal variations in the peak intensities of the 5303 Å emission line from the solar corona in the position angle range ≈250°–290° observed on 2024 July 16 with VELC/ADITYA-L1. The center of spectrograph slit 4 was positioned close to the west limb of the Sun at r ≈1.05 R ⊙. A sudden dimming of the intensity can be clearly observed in the position angle range ≈ 260°–270° during the interval ≈ 13:18–19:00 UT. The possible reasons for the oscillatory pattern in the image are being investigated.
Paper: New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: R. Ramesh, V. Muthu Priyal, Jagdev Singh, K. Sasikumar Raja, P. Savarimuthu, Priya Gavshinde
Figure caption: Upper panel: time variation of the peak intensity of the emission line averaged over the dimming region (position angle range ≈260°–270°) in Figure 3. The vertical red line indicates the onset of the dimming at ≈13:18 UT. Middle panel: the same as above, but corresponds to width of the emission line. Lower panel: the same as above, but corresponds to Doppler velocity estimated from the shift in the peak of the emission line from the reference.
Paper: New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: R. Ramesh, V. Muthu Priyal, Jagdev Singh, K. Sasikumar Raja, P. Savarimuthu, Priya Gavshinde
Figure caption: STEREO-A/EUVI 195 Å running difference images for the flare event of 2024 July 16 mentioned in the main text. The observing times of the images used are mentioned above each panel.
Paper: New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: R. Ramesh, V. Muthu Priyal, Jagdev Singh, K. Sasikumar Raja, P. Savarimuthu, Priya Gavshinde
Figure caption: (r, θ) image of the solar corona at the west limb of the Sun constructed from the raster scan observations in the 5303 Å emission line on 2024 July 16 during the interval ≈00:30–01:17 UT, with VELC/ADITYA-L1. The fine lines seen in the image are due to remnant fixed pattern noise in the detector, even after the flat-field correction.
Paper: New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: R. Ramesh, V. Muthu Priyal, Jagdev Singh, K. Sasikumar Raja, P. Savarimuthu, Priya Gavshinde
Figure caption: The same as Figure 5, but during the interval ≈23:09–23:56 UT.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: SED of Makemake from NEATM modeling. (a) Assuming a single terrain. Gray curves correspond to case 1 surfaces, assuming different η beaming parameters. The black solid curve has η = 1.2. The black dashed–dotted curve corresponds to a reflected-light contribution assuming a mid-IR albedo of p MIR = 0.8 in all subfigures. (b) Case 2: Makemake’s thermal emission model considering a single-terrain Makemake and a dark satellite. The curves with different colors correspond to satellites with p  V  = 0.01, ..., 0.08; the “extreme” moon model used by E. Lellouch et al. (2017; marked as L17); and the dark giant moon case, as indicated by the inserted text. (c) Makemake’s thermal emission considering double-terrain models (case 3). The bands with different colors cover the models using different bright/dark terrains (see Table 3) and dark terrain locations but using the same beaming parameters, as shown by the colored symbols and extra text below the curves in the figures ("single terrain…", "double terrain…", etc.).
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: SED of Makemake’s reflected light and thermal emission. Black symbols represent the mean measured flux densities. The green stripe shows the SED of the “hot-spot” models, compatible with the observations, as described in Section 3 (note that the stripe was made somewhat wider than it is in reality for better visibility). It was calculated assuming that Makemake has a double terrain with “Quaoar-like” dark terrains and reflected light with a mid-IR albedo of p 5.6 = 0.8. The black dashed curve is the SED of 100 nm carbonaceous grains that together with Makemake’s contribution (solid black curve inside the green stripe) matches the observed flux densities very well. The colored dashed/dashed–dotted curves correspond to the emission of dust when other types of dust grains are also included, in addition to the same amount of 100 nm carbonaceous dust as in the pure case. The additional material has a mass of 100× the mass of 100 nm carbonaceous grains in all cases. The additional components are as follows: purple dashed curve, pyroxene with 100% Mg content, 100 nm grain size; purple dashed–dotted curve, pyroxene with 100% Mg content, 1 μm grain size; green dashed curve, amorphous water ice, 100 nm grain size; green dashed–dotted curve, amorphous water ice, 1 μm grain size.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: Top: phase dispersion vs. frequency of the Makemake TESS data. The inset shows the residual spectrum derived using the position of the aperture centers with respect to the actual pixel’s edge in the X (blue) and Y (green) directions. In both the main figure and the inset, the vertical dashed red line is at the frequency of f = 2.105 c day−1 (P = 11.401 hr) associated with the prominent peak in the residual spectrum, very close to the 11.41 hr period identified by T. A. Hromakina et al. (2019). Middle: light curve folded with a period of P = 11.401 hr. Black dots represent the binned data. Bottom: light curve folded with the double period, P = 22.802 hr.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: SED assuming an additional “hot spot” on the surface. Gray curves correspond to a single-terrain Makemake + a dark satellite with different albedos. The light blue curves correspond to blackbodies in the T  s  = 147 ± 5 K range. The red curves are the sum of the blue curves and the “median” Makemake + satellite curve, assuming a satellite with p  V,S  = 0.04 and D  s  = 179 km.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: (a) Relative flux densities as measured in the background-subtracted MIPS 24 μm images as a function of relative distance between the target and the mirror source. Negative and positive distances correspond to the first and second half of the measurement, respectively. The dashed curve represents the best-fit theoretical background-corrected relative flux density curve, considering flux loss due to the subtraction of the “mirror” source and assuming a sinusoidal variation with a period of P = 11.41 hr. (b) Variation of relative flux densities as a function of time (black dots) using the same best-fit sinusoidal fit as above (solid curve). The thicker part of the curve represents the phases covered by the MIPS 24 μm observations.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: Dust temperature as a function of grain size for different compositions. Purple: pyroxene with 100% Mg content; blue: pyroxene with 40% Mg content; light blue: olivine with 50% Mg content; green: amorphous water ice; yellow: carbon grains as defined by V. G. Zubko et al. (1996); orange: graphite grains; red: “organic carbon.”
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: Top: Lomb–Scargle periodogram of the Makemake Gaia data. The vertical dashed lines mark the frequency corresponding to the 11.41 hr period, identified by T. A. Hromakina et al. (2019), and the first overtone at 5.7 hr. Bottom: heliocentric and observer-distance- and phase-angle-corrected Gaia light curve, folded with the P = 11.4767 hr period.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: Spitzer/MIPS 24 μm images of Makemake, with AORKEYs 19176448–19179264 (see Table 1 for the flux densities derived).
Paper: An Extremely Low-density Exoplanet Spins Slow
Authors: Quanyi Liu, 权毅 刘, Wei Zhu, 伟 祝, Kento Masuda, 田賢人 増, Jessica E. Libby-Roberts, Aaron Bello-Arufe, Caleb I. Cañas
Figure caption: Constraints on the projected oblateness f ⊥ (along the radial direction) and the projected obliquity θ ⊥ (along the azimuthal direction) in the polar coordinates. Different panels show the various consistency tests: panel (a) shows the results from two different reduction methods, panel (b) shows the results from imposing different lgρ ⋆ priors in the modeling, panel (c) shows the results from using GP or not in the modeling, and panel (d) shows the results from modeling the two-channel light curves (lower panel of Figure 1). The red contours are the results from our baseline model and thus the same in all panels. Similar to Figure 3, the solid and dashed curves are the 1σ and 2σ contours, respectively.
Paper: An Extremely Low-density Exoplanet Spins Slow
Authors: Quanyi Liu, 权毅 刘, Wei Zhu, 伟 祝, Kento Masuda, 田賢人 増, Jessica E. Libby-Roberts, Aaron Bello-Arufe, Caleb I. Cañas
Figure caption: The corner plot of the baseline model. The values and 1σ uncertainties of the modeling parameters are indicated at the top of the individual column. These are defined as the median and the values enclosing 68% credible interval of the marginal probability distribution, respectively. The reconstructed posterior distribution in the f ⊥ vs. θ ⊥ plane is shown in the upper-right corner, with the solid and the dashed curves indicating the 1σ and 2σ contours, respectively. The true oblateness and obliquity of Jupiter and Saturn are also shown for reference.
Paper: Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: The 95% upper limits on the fraction of dark matter in the form of PBHs and other compact objects. The hatched area marks the region of the PBH parameter space obtained by H. Niikura et al. (2019b), under assumption that short-timescale microlensing events detected by P. Mróz et al. (2017) in the OGLE-IV Galactic bulge high-cadence survey are due to planetary-mass PBHs. The shaded purple region corresponds to the 95% confidence limit on f found in this work (this data set is available for download from the online journal). Other limits are adopted from P. Tisserand et al. (2007; EROS), L. Wyrzykowski et al. (2011; OGLE-III), K. Griest et al. (2013; Kepler), H. Niikura et al. (2019a; HSC), T. Blaineau et al. (2022; macHO+EROS), and P. Mróz et al. (2024b; OGLE-III+OGLE-IV).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: CMDs of the fields LMC503.15 (left panel) and LMC503.08 (right). The location of OGLE-LMC-20 (LMC503.08.18967) in the baseline is marked by a blue circle (red asterisk). The green square marks the position of the source star of OGLE-LMC-20.
Paper: Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Light curves of objects that passed all selection criteria. The solid blue line shows the best-fit PSPL microlensing model.
Paper: Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Fields of the OGLE High-cadence Magellanic Clouds Survey; left panel—LMC; right panel—SMC. The background images of the LMC and SMC were generated with BSRENDER written by Kevin Loch, using the ESA/Gaia database.