adsabs/AstroCLIMB huggingface dataset:
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: Spatial distribution of the high-probability Draco stars. The King tidal radius is the red ellipse. The orbit from Y. Qi et al. (2022) is shown in green; the forward integration is plotted as a continuous line, while the backward integration is shown as a dashed line. This orbit was computed with an MW potential composed of a spherical Hernquist bulge (L. Hernquist 1990), a spherical Hernquist nucleus, an axisymmetric Miyamoto–Nagai disk (M. Miyamoto & R. Nagai 1975), and a spherical Navarro–Frenk–White dark matter halo (J. F. Navarro et al. 1996). The eight high-probability stars outside the tidal radius are shown in larger circles labeled in blue. The high-probability Draco members are labeled in dark circles while the low-probability stars are labeled in gray circles. Ellipses at 1, 3, 5, and 7 times the half-light radius (R. R. Muñoz et al. 2018) are plotted in cyan. The ellipse at 5 times the half-light radius nearly overlaps the King radius.
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: The CMD with the membership probabilities from the mixture model. Points are colored according to their probability. The high-probability members outside the tidal radius are labeled with triangles. The gray isochrone is for a metal-poor population ([Fe/H] = −1.8 and [α/Fe] = 0.4) with age = 12.5 Gyr (A. Dotter et al. 2008).
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: Comparison of PM measurements between this work and previous literature. The red error bars show the Draco PM with 1σ uncertainties measured in this work. The black point and error bars are the PM value and uncertainty measured by Y. Qi et al. (2022). The blue point and error bars show the PM measured by A. W. McConnachie & K. A. Venn (2020a). The orange data represent PMs from G. Battaglia et al. (2022), and the green cross shows the PM from A. M. Martínez-García et al. (2021). The purple PM measurement is from A. B. Pace et al. (2022). Our PM distribution is in consistent with the other PM values.
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: The velocity dispersion of our high-probability Draco members as a function of elliptical radial distance in units of half-light radius (top labels) and arcminutes (bottom labels) from the center. This was measured by running the GMM model in four elliptical bins, fixing the PM (same method as the metallicity gradient measurement in the left panel of Figure 5 ).
Paper: The Draco Dwarf Spheroidal Galaxy in the First Year of Dark Energy Spectroscopic Instrument Data
Authors: J. Ding, C. Rockosi, Ting S. Li, S. E. Koposov, A. H. Riley, W. Wang, A. P. Cooper, N. Kizhuprakkat, M. Lambert, G. E. Medina, N. Sandford, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, M. Ishak, R. Kehoe, T. Kisner, A. Kremin, O. Lahav, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou
Figure caption: The probability distribution for Draco members identified with the GMM. From this probability distribution, we define the high-probability members to be p > 0.9. There are 155 stars that pass this criterion.
Paper: Buildup, Explosion, and Untwisting of a Solar Active Region Jet Observed with Solar Orbiter, IRIS, and SDO
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore, Sanjiv K. Tiwari, David Berghmans, Andrei Zhukov, Marilena Mierla, Cis Verbeeck, Koen Stegen
Figure caption: Magnetic field topology at the jet base. Panel (a) shows the potential field source surface (PFSS) extrapolation of the jet and surrounding regions overplotted on a Bz map at 14:00 UT. The pink and white colors represent, respectively, open and closed field lines. The yellow box shows the field of view displayed in (b). Panel (b) shows the transverse field vectors overplotted on an HMI Bz map at 14:00 UT. The orange contour between the positive and negative fluxes of the jet bipole is the magnetic neutral line. The red and yellow arrows display the transverse magnetic field vectors of the positive and negative flux clumps, respectively. The blue oval outlines the region showing left-handed shear.
Paper: Buildup, Explosion, and Untwisting of a Solar Active Region Jet Observed with Solar Orbiter, IRIS, and SDO
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore, Sanjiv K. Tiwari, David Berghmans, Andrei Zhukov, Marilena Mierla, Cis Verbeeck, Koen Stegen
Figure caption: The jet-base magnetic flux time–distance map. The time–distance map shows the merging of the magnetic flux inside the yellow box in Figure 4(g). Positive and negative flux patches converge toward the neutral line with time.
Paper: Buildup, Explosion, and Untwisting of a Solar Active Region Jet Observed with Solar Orbiter, IRIS, and SDO
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore, Sanjiv K. Tiwari, David Berghmans, Andrei Zhukov, Marilena Mierla, Cis Verbeeck, Koen Stegen
Figure caption: HRIEUV 174 Å time–distance map from the white dashed line of Figure 3(c). The plot shows the (un)twisting of the jet spire with time. The white lines trace some of the left-to-right (untwisting) motion transverse to the spire of bright strands of the spire.
Paper: Buildup, Explosion, and Untwisting of a Solar Active Region Jet Observed with Solar Orbiter, IRIS, and SDO
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore, Sanjiv K. Tiwari, David Berghmans, Andrei Zhukov, Marilena Mierla, Cis Verbeeck, Koen Stegen
Figure caption: Jet onset. Panels (a) and (b) each show a spectroheliogram of the Mg II k line during the jet eruption. The cyan arrows point to the erupting minifilament. Panel (c) shows the Dopplergram of the jet onset. The upper and lower black arrows, respectively, point to the blueshifts and redshifts along the jet spire.
Paper: Buildup, Explosion, and Untwisting of a Solar Active Region Jet Observed with Solar Orbiter, IRIS, and SDO
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore, Sanjiv K. Tiwari, David Berghmans, Andrei Zhukov, Marilena Mierla, Cis Verbeeck, Koen Stegen
Figure caption: Evolution of the minifilament in Si IV. This is a time–distance map plotted along the dotted–dashed line of Figure 5(a). The cyan and red arrows, respectively, point to the minifilament during slow-rise and fast-rise phases, and jet-base bright point brightening.
Paper: Formation of a Coronal Hole by a Quiet-Sun Filament Eruption
Authors: Stefan J. Hofmeister, Eleanna Asvestari, Karin Dissauer, Michael Hahn, Stephan G. Heinemann, Veronika Jercic, Alexandros Koukras, Kilian Krikova, Jonas Saqri, Daniel W. Savin, Manuela Temmer, Astrid Veronig
Figure caption: Evolution of the coronal hole properties as derived from the compact coronal hole boundaries. (a) Area, average magnetic flux density B, and total magnetic flux Φ. (b) Average AIA 171, 193, and 211 Å intensities. (c) DEM for the selected six times. (d) EM, T, and expected temperature from adiabatic cooling.
Paper: Formation of a Coronal Hole by a Quiet-Sun Filament Eruption
Authors: Stefan J. Hofmeister, Eleanna Asvestari, Karin Dissauer, Michael Hahn, Stephan G. Heinemann, Veronika Jercic, Alexandros Koukras, Kilian Krikova, Jonas Saqri, Daniel W. Savin, Manuela Temmer, Astrid Veronig
Figure caption: Evolution of the solar corona during the coronal hole formation, as observed in AIA 193 Å. (a) June 25 00:00: a large quiet-Sun filament channel (marked in black) is present east of the central meridian. A coronal hole (blue) lies to its west, and a dim region (red), possibly another coronal hole obscured by overlying quiet-Sun loops, is visible to the east. (b) 10:30: the filament erupts, producing two coronal dimmings (cyan and green). (c) June 26 06:00: The cyan dimming migrates northwestward and develops into the coronal hole under investigation. The green dimming recovers to quiet-Sun intensities.
Paper: Longtime Monitoring of TeV Radio Galaxies with HAWC
Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: Cumulative significance evolution with confidence bands for the radio galaxies M87 (red crosses), NGC 1275 (green triangles), IC 310 (blue circles), and 3C 264 (cyan stars). The shaded regions represent 1σ confidence bands. For comparison, the bottom panel shows the Crab Nebula (magenta squares) as a steady source reference and Markarian 421 (black diamonds) as a known variable source, displayed on a relative significance scales. The behavior of the radio galaxies resembles that of a variable source like Markarian 421 rather than a steady source such as the Crab Nebula.
Paper: Formation of a Coronal Hole by a Quiet-Sun Filament Eruption
Authors: Stefan J. Hofmeister, Eleanna Asvestari, Karin Dissauer, Michael Hahn, Stephan G. Heinemann, Veronika Jercic, Alexandros Koukras, Kilian Krikova, Jonas Saqri, Daniel W. Savin, Manuela Temmer, Astrid Veronig
Figure caption: The coronal hole under study, observed in AIA 193 Å on 2014 June 26 06:00. (a) Original AIA image. (b) AIA image deconvolved with the instrumental point-spread function described in S. Hofmeister et al. (2025). In the point-spread-function corrected image, the coronal hole boundaries are more clearly defined. The compact and wider coronal hole boundaries we use in our study are marked in cyan and violet, respectively.
Paper: Longtime Monitoring of TeV Radio Galaxies with HAWC
Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: NGC 1275 light curves for different timescales. The black points represent the calculated fluxes with a significance of ≥2σ, while the gray points represent the calculated fluxes with a significance of <2σ. Top: daily LC. Middle: weekly LC. Bottom: monthly LC.
Paper: Longtime Monitoring of TeV Radio Galaxies with HAWC
Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: IC 310 light curves for different timescales. The black points represent the calculated fluxes with a significance of ≥2σ, while the gray points represent the calculated fluxes with a significance of <2σ. Top: daily LC. Middle: weekly LC. Bottom: monthly LC.
Paper: Longtime Monitoring of TeV Radio Galaxies with HAWC
Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: 3C 264 light curves for different timescales. The black points represent the calculated fluxes with a significance of ≥2σ, while the gray points represent the calculated fluxes with a significance of <2σ. Top: daily LC. Middle: weekly LC. Bottom: monthly LC.
Paper: The Serpent Eating Its Own Tail: Dust Destruction in the Apep Colliding Wind Nebula
Authors: Ryan M. T. White, Benjamin J. S. Pope, Peter G. Tuthill, Yinuo Han, Shashank Dholakia, Ryan M. Lau, Joseph R. Callingham, Noel D. Richardson
Figure caption: An illustration of the cavity carved by the northern O star companion in the Apep system. The W-R + W-R binary is the central bright point, while the northern companion is the smaller point source 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩7 to the north. Top left: the innermost shell of the Apep nebula observed with VLT/VISIR, processed as in Appendix A.2. Top right: previous models with no dust destruction effects from the northern companion overestimate the dust luminosity in the upper region of the plume. Bottom left: we model dust destruction along the volume of a cone extending out of the W-R + W-R central engine along the line-of-sight vector to the northern companion. Bottom right: with the addition of this region of dust destruction, the model geometry now more closely matches what we see with direct imaging (top left).
Paper: The Formation and Evolution of Dust in the Colliding-wind Binary Apep Revealed by JWST
Authors: Yinuo Han, Ryan M. T. White, Joseph R. Callingham, Ryan M. Lau, Benjamin J. S. Pope, Noel D. Richardson, Peter G. Tuthill
Figure caption: Left: Apep’s intershell spacing as a function of position angle. The position angle in the horizontal axis corresponds to the angle measured counterclockwise from north in Figure 2 (left panel), in which the azimuthal range with data points are labeled with arcs. Right: the expansion speed of Apep’s inner dust shell as a function of position angle. The two curves correspond to the best-fit sinusoidal model with one and two periods over the full azimuthal range, respectively. The vertical lines and shaded regions correspond to the line of nodes, apastron, and the velocity vector at apastron and their uncertainties (R. M. T. White et al. 2025).
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Orientation of the grain angular momentum J in a lab coordinate system ﹩{\hat{{\boldsymbol{e}}}}_{1}{\hat{{\boldsymbol{e}}}}_{2}{\hat{{\boldsymbol{e}}}}_{3}﹩. The axis ﹩{\hat{{\boldsymbol{e}}}}_{1}﹩ is defined by the radiation direction k; the axis ﹩{\hat{{\boldsymbol{e}}}}_{2}﹩ is perpendicular to ﹩{\hat{{\boldsymbol{e}}}}_{1}﹩ and lies in the plane ﹩{\hat{{\boldsymbol{e}}}}_{1}﹩ and magnetic field B. The radiation direction makes an angle ψ with the magnetic field. The alignment angle between J and B is described by ξ, and fast Larmor precession of J around B is described by the angle ϕ.
Paper: The Formation and Evolution of Dust in the Colliding-wind Binary Apep Revealed by JWST
Authors: Yinuo Han, Ryan M. T. White, Joseph R. Callingham, Ryan M. Lau, Benjamin J. S. Pope, Noel D. Richardson, Peter G. Tuthill
Figure caption: Plausible regions within the luminosity and distance parameter space for Apep based on constraints from its temperature profile, near-IR flux density, likely luminosity range, and likely dynamical mass range given the orbit. The distances required for Apep to be explained by a spherically symmetric wind outflow within a factor of 2 is shown for comparison.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: The averaged aligning (panel (a)) and spin-up (panel (b)) torque components for the different grain angular momentum, assuming the RAT model of ﹩{q}^{{\rm{\max }}}=3﹩ and the radiation parallel to the magnetic field, ψ = 0°. The intersection between the dotted line and 〈F〉 determines the stationary points marked by circles for the case ﹩J^{\prime} =0.63﹩.
Paper: Toward a General Theory of Grain Alignment and Disruption by Radiative Torques and Magnetic Relaxation
Authors: Thiem Hoang
Figure caption: Same as Figure 4 but for the time-dependent alignment degrees QX, QJ, and R. The alignment degrees increase with time due to the transport of grains to high-J attractors by gas and magnetic excitations and achieves perfect alignment of R ∼ 1 after ∼10τdamp for U/(n1T2) = 0.16, 0.6 (panels (a),(b)) and near perfect alignment of R ∼ 0.8 after TPA ∼ 70τdamp (panel (c)).
Paper: Converging on the Cepheid Metallicity Dependence: Implications of Nonstandard Gaia Parallax Recalibration on Distance Measures
Authors: Louise Breuval, Gagandeep S. Anand, Richard I. Anderson, Rachael Beaton, Anupam Bhardwaj, Stefano Casertano, Gisella Clementini, Mauricio Cruz Reyes, Giulia De Somma, Martin A. T. Groenewegen, Caroline D. Huang, Pierre Kervella, Saniya Khan, Lucas M. Macri, Marcella Marconi, Javier H. Minniti, Adam G. Riess, Vincenzo Ripepi, Martino Romaniello, Daniel Scolnic, Erasmo Trentin, Piotr Wielgórski, Wenlong Yuan
Figure caption: Distance estimates to the Pleiades open cluster. Light blue values are pre-Gaia measurements, orange is Hipparcos, dark blue are Gaia-based distances and the red point corresponds to Gaia EDR3 after applying the recalibration suggested by MF25.
Paper: Converging on the Cepheid Metallicity Dependence: Implications of Nonstandard Gaia Parallax Recalibration on Distance Measures
Authors: Louise Breuval, Gagandeep S. Anand, Richard I. Anderson, Rachael Beaton, Anupam Bhardwaj, Stefano Casertano, Gisella Clementini, Mauricio Cruz Reyes, Giulia De Somma, Martin A. T. Groenewegen, Caroline D. Huang, Pierre Kervella, Saniya Khan, Lucas M. Macri, Marcella Marconi, Javier H. Minniti, Adam G. Riess, Vincenzo Ripepi, Martino Romaniello, Daniel Scolnic, Erasmo Trentin, Piotr Wielgórski, Wenlong Yuan
Figure caption: Mean parallaxes of distant quasars as a function of Gaia G magnitude from the Gaia EDR3 catalog without any correction (black), with the multiplicative correction proposed by MF25 (red) and with the additive correction recommended by the Gaia team (L21, in blue). Quasar parallaxes are expected to be equal to zero. Figure adapted from L21.