adsabs/AstroCLIMB huggingface dataset:
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Joint PCA-KLIP subtraction of α Cen AB for the 2024 August observations with automatic PC selection. Left: the de-rotated residual image (north up, east left) after PSF subtraction in three concentric annuli. The MIRI/4QPM transition boundaries are shown as gray shaded regions. Point-source detections of S1 and artifact A1 (discussed in Section 4.2.2) are circled. Right: S/N map for the reduction shown in the left panel. S1 is detected with a peak S/N of 5.4 (4σ). A1 is brighter than S1 but detected a lower peak S/N of 2.5 (the residual noise estimated using nonoverlapping apertures at the same separation but different position angles (PAs), following D. Mawet et al. 2014, is higher at the separation of A1.)
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Example determination of stellar position behind the MIRI 4QPM for α Cen A in the 2024 August observation. Left: χ2 map obtained after subtracting STPSF models generated by varying the stellar position behind the mask (marginalized over the model PSF flux scale factor parameter). The best-fitting PSF (minimum χ2) is marked with a white star. Right: from left to right, the observed α Cen A PSF, best-fitting STPSF model, and residual image after taking the difference are shown. The white box designates the region over which χ2 was minimized.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Alignment of the off-axis ϵ Mus reference frames to the corresponding α Cen B observations using a bright diffraction feature in each of the epochs (for 2025 April, only the roll 2 observation is shown). Top panel: for a given epoch, from left to right, the α Cen B observation, ϵ Mus reference frame, and difference image. Bottom panel: similar to the top panel but with the ϵ Mus reference frame aligned to the α Cen B observation.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Subtraction of α Cen AB using a linear combination of reference images. Left: full α Cen AB detector image showing the regions over which the RSS was minimized to obtain coefficients c1 (for α Cen A’s PSF model) and c2 (for α Cen B’s PSF model). Right: RSS map obtained after subtracting the model PSFs. The best-fitting (minimum RSS) coefficient pair (c1 = 0.830, c2 = 0.370) is marked with a white star.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: The average pixel brightness in a 3 pixel radius aperture centered on S1 in the background-subtracted Stage 2b α Cen AB integrations from 2024 August. The time series does not show any sharp transitions (increases) that would appear as an artifact at the location of S1 after PSF subtraction.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Estimated positions of ϵ Mus and α Cen A behind the MIRI/4QPM in the nine-point SGD and single/two roll observations, respectively, for each observation epoch (with respect to mask center). The 2024 August and 2025 April (roll 2 only) α Cen A observations have ϵ Mus reference images well matched in terms of position behind the 4QPM.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Joint PCA-KLIP subtraction of α Cen AB for the 2024 August observations for different number of azimuthal subsections (Nsub). S1 is recovered in all reductions, whereas A1’s signal disappears as Nsub increases.
Paper: Different Inhomogeneous Evolutionary Histories for Uranus and Neptune
Authors: Roberto Tejada Arevalo
Figure caption: Comparison of the evolutionary effects of different ice mixtures on the Uranus model presented in Section 4 (shown here in blue). The dashed lines in the bottom panel indicate the measured values to guide the eye. The interior entropy profiles are scaled so that all models begin with similar interior temperatures. All models have a rock mass fraction of 0.35 in their envelopes. Since methane and ammonia are less dense than water, models with more methane and ammonia abundances increase the entropy and thus decrease the density, causing large differences in the total radius and the gravitational harmonics. A model with pure water (shown in red) is more dense and thus exhibits a smaller radius, leading to similar differences in the gravitational harmonic evolution.
Paper: Different Inhomogeneous Evolutionary Histories for Uranus and Neptune
Authors: Roberto Tejada Arevalo
Figure caption: Present-age parameters as a function of the initial interior entropy for the models shown in Figure 3. The effective temperature and luminosities increase with higher initial interior entropy until a threshold of ∼3.7 kB baryon−1 renders the evolution adiabatic. The threshold values depend on the ice mixtures used (4:1:7 methane–ammonia–water chosen here), but it nevertheless occurs with different ice mixtures and even pure water (see discussion at the end of Section 3). Once “hotter” models become adiabatic, they accumulate more heavy metals (center panel, blue line) and display smaller radii (center panel, red line). Note that adiabatic evolution postmixing can have a similar luminosity output to unmixed models (left panel) but show significantly different radii and gravitational harmonics (right panel).
Paper: Different Inhomogeneous Evolutionary Histories for Uranus and Neptune
Authors: Roberto Tejada Arevalo
Figure caption: Example fractional error mapping of present-age J2 (left panel) and J4 (right panel) of Uranus-mass models with respect to the amount of rock in the envelope. These models are part of the parameter search described in Section 4. For simplicity, and for this example, the outer envelope mass fraction is held constant at 0.35, and the moment-of-inertia factor is held constant at 0.2222. Higher rock envelope mass fractions (Zrock) are systematically preferred by J2, though a combination of compact core masses with Zrock are possible to satisfy J4. When accounting for both J2 and J4 together, the upper right corner yields the least error.
Paper: Different Inhomogeneous Evolutionary Histories for Uranus and Neptune
Authors: Roberto Tejada Arevalo
Figure caption: Comparison of the Uranus preferred model presented in Section 4 and the left panel of Figure 4 with the original and updated AQUA tables. The format of this figure is the same as Figure 3. The same model with H–He–water only is shown in red for example purposes. The updated AQUA table takes into account the entropy correction to the S. Mazevet et al. (2019; in magenta) EOS given by S. Mazevet et al. (2021; in blue). The differences in the evolution between the original and updated water EOSs are small (≲3%). The use of the original AQUA EOS does not affect the results presented here.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Limits from archival imaging at S1’s position. The solid, color-coded lines show a photospheric model for an M0III star (Teff = 3800 K) reddened by increasing levels of extinction, all normalized to 3.5 mJy at 15.5 μm (red star). The blue star denotes the flux density of the object denoted C1 detected by the VLT/NEAR experiment (K. Wagner et al. 2021). The dashed lines show the SED of a typical starburst galaxy or ULIRG (Arp 220) similarly reddened. Upper limits at the position of S1 come from observations at earlier epochs with Spitzer/IRAC (3–8 μm), 2MASS, and NACO (P. Kervella et al. 2016).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Left: 2D 5σ planet effective BB temperature sensitivity map, combined across all epochs by selecting the best sensitivity (“combined minimum,” see Paper II ), in sky coordinates (north up, east left). The central region (<0﹩\mathop{.}\limits^{^{\prime\prime} }﹩75, or <1.5 FWHM, radial separations) is masked (poor detectability). A discrete color map is chosen to highlight the different sensitivity zones across the image. Center: same as the left panel but for an S/N = 5 detection threshold. Right: 5σ and S/N = 5 median planet effective BB temperature curves combined across all epochs.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Left: unconvolved ABA-3 exozodi model coplanar with the α Cen AB binary. Center: the exozodi model in the left panel after PSF convolution (for the 2025 April observation orientation). Right: PSF-subtracted image showing the recovery of the ABA-3 exozodi model injected in the raw α Cen AB data set from the 2025 April observations. The regions of the image affected by the MIRI/4QPM transition boundaries at each roll are masked. The aperture that yielded the highest S/N (=21.3) detection for the injected disk is shown (see Paper II  for details). All images are plotted on a common logarithmic color scale.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Surface brightness distribution of injected zodi models. ABA-scenario zodis for different belt masses are represented by solid lines. Our fiducial 1-zodi model based on the T. Kelsall et al. (1998) model is represented by the dashed–dotted line.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: The RV semiamplitude of a 100 M⊕ planet in stable orbits fit to S1 + C1 and consistent with the nondetections in the 2025 February and April epochs. Note that KRV scales linearly with planet mass. The systematic RV noise floor of 3 m s−1 (1σ; L. Zhao et al. 2018; P. Kervella et al. 2025, in preparation) is shown.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Range of flux-averaged mean planet temperatures for AB = 0.3 corresponding to the orbits described in the preceding section. The lower temperatures in the bimodal distribution correspond to the a > 2 au orbits.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Key parameters for stable planetary orbits fitting the S1 + C1 astrometry and consistent with the 2025 February and April nondetections. Four orbital families are observed (prograde, retrograde, a > 2 au, and a < 2 au).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: 100 randomly selected stable planetary orbits fitting the S1 + C1 astrometry (marked as green points) and consistent with the 2025 February and April nondetections, for each orbital family.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: 1σ (solid) and 3σ (dotted) contours showing the sky-projected positions of the S1 + C1 candidate consistent with a nondetection in the 2025 February (blue) and April (red) observation epochs.
Paper: Cosmic Outliers: Low-spin Halos Explain the Abundance, Compactness, and Redshift Evolution of the Little Red Dots
Authors: Fabio Pacucci, Abraham Loeb
Figure caption: This plot illustrates why LRDs are preferentially detected in the redshift range 4 ≲ z ≲ 8. The red line shows the fraction of halos whose spin parameter falls below the redshift-dependent threshold required to form galaxies more compact than Reff = 300 pc. The blue line shows the surface brightness of such a representative compact galaxy. The dashed blue line marks the assumed JWST/NIRCam 5σ surface brightness limit (∼25.2 mag arcsec−2). The dashed red line shows the compact fraction threshold of 1%, which we take as the limit below which LRDs become intrinsically rare. The red and blue curves serve complementary roles: the former quantifies the intrinsic rarity of compact systems, while the latter estimates their detectability. The shaded region (4 ≲ z ≲ 8) highlights the redshift range where LRDs are both common and detectable—the “LRD era.”
Paper: Cosmic Outliers: Low-spin Halos Explain the Abundance, Compactness, and Redshift Evolution of the Little Red Dots
Authors: Fabio Pacucci, Abraham Loeb
Figure caption: Predicted number density of LRDs as a function of effective radius Reff at z = 5, for various values of the halo spin parameter λ, indicated in the color bar. The solid curve shows the theoretical expectation for galaxies with typical UV magnitude MUV ∼ −19. The shaded horizontal region denotes the observed number density range for LRDs (D. D. Kocevski et al. 2025), while the vertical shaded band marks their observed effective radius range (J. F. W. Baggen et al. 2023); observational ranges encompass the full brightness range of LRDs, with −17 < MUV < −21. The intersection of these shaded regions highlights the regime where low-spin halo galaxies reproduce the abundance and compactness of the observed LRD population.
Paper: Cosmic Outliers: Low-spin Halos Explain the Abundance, Compactness, and Redshift Evolution of the Little Red Dots
Authors: Fabio Pacucci, Abraham Loeb
Figure caption: Relative number density of LRDs as a function of redshift, normalized to the value at z = 5.5 from D. D. Kocevski et al. (2025). The solid line shows the theoretical prediction from our model, also normalized at z = 5.5. Colored points show observational estimates from D. D. Kocevski et al. (2025; brown), M.-Y. Zhuang et al. (2025; orange), and Y. Ma et al. (2025; blue). In the regime z < 5 when the typical LRD is characterized by detectable surface brightness, the redshift evolution is primarily driven by the redshift evolution of fLRD: a lognormal that is exponentially suppressed at low redshifts. At z ≳ 5, the suppression from cosmological surface brightness dimming becomes essential.
Paper: Cosmic Outliers: Low-spin Halos Explain the Abundance, Compactness, and Redshift Evolution of the Little Red Dots
Authors: Fabio Pacucci, Abraham Loeb
Figure caption: Comparison of rest-frame UV luminosity functions for different astrophysical populations at 4.5 < z < 6.5, spanning absolute UV magnitudes −17 < MUV < −25. Red points show the number density of LRDs from D. D. Kocevski et al. (2025); the dashed line indicates UV-selected quasars from M. Niida et al. (2020); the solid line shows Lyman-break galaxies (LBGs) from R. J. Bouwens et al. (2021). LRDs occupy an intermediate number density regime: ∼100 times rarer than typical star-forming galaxies but more abundant than bright quasars.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Change in the solar elongation angle between α Cen and ϵ Mus as a function of the day of year. The red, blue, and green dashed vertical lines correspond to the observation dates in 2024 August, 2025 February, and 2025 April, respectively.
Paper: Cosmic Outliers: Low-spin Halos Explain the Abundance, Compactness, and Redshift Evolution of the Little Red Dots
Authors: Fabio Pacucci, Abraham Loeb
Figure caption: Probability density function of the halo spin parameter λ, modeled as a lognormal distribution (H. J. Mo et al. 1998), with the mode (i.e., the most common spin value) and median indicated for reference. The vertical dashed line marks the critical value λLRD = 0.0153, corresponding to the spin threshold required to explain the abundance and compactness of the typical LRD at z ∼ 5. This value lies in the extreme low-spin tail of the distribution, representing only ∼1% of halos.