adsabs/AstroCLIMB huggingface dataset:
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Shown here is a SPHERE/IRDIS multiband image of the WISPIT 2 system. The H-band Qϕ image was added as the blue channel and the median combination of H-band and Ks-band Qϕ images was added as the green channel. The red channel is a combination of a Ks-band Qϕ image and a Ks-band cADI image in which we masked all but the gap containing the thermal emission from WISPIT 2b. For more details, see Appendix G.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Color–magnitude diagram of WISPIT 2b, with field brown dwarfs of various spectral types and confirmed planetary companions. Teal and cyan tracks show 5.1 Myr AMES-COND and AMES-DUSTY isochrones, respectively. WISPIT 2b is marked in purple.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Left and middle panels: geometric fitting of the disk in both H-band and Ks-band images. Right panel: the aspect ratio (h/r) vs. radius (au) of both bands. For comparison, we include the literature measurements of C. Ginski et al. (2016), H. Avenhaus et al. (2018),and C. Ginski et al. (2024) for a total of 17 disks (some of which also have a multiple ringed substructure) as gray data points.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Proper-motion analysis of WISPIT 2b. Each epoch is represented by a unique marker shape: diamond (2023), circle (2024), and cross (2025). The colored version of each marker denotes the measured position of the companion. The unfilled (black outline, white center) version of each marker shows the expected position of the source if it were a stationary background object. The dashed curve illustrates the parallactic motion of such a background object from first to last epoch.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Top panel: predicted orbits of the planet (known astrometry denoted by red star) overlaid on the H-band polarized scattered light image. Bottom panel: extracted orbital elements and total system mass.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Polarized light Qϕ image of the WISPIT 2 system taken in the H band. We indicate the various substructures that we are detecting within the scattered light signal of the planet-forming disk. Clusters of bad pixels from the detector are seen near the lower edge of the image.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: The SED of WISPIT 2 is presented here. Photometric data from various sources are shown with colored markers. The blue curve represents the best-fit BT-Settle-CIFIST model (χ2 = 7.94), with the low-resolution (high-opacity) version overlaid on the high-resolution (low-opacity) model.
Paper: Black Hole Survival Guide: Searching for Stars in the Galactic Center that Endure Partial Tidal Disruption
Authors: Rewa Clark Bush, Samantha C. Wu, Rosa Wallace Everson, Ricardo Yarza, Ariadna Murguia-Berthier, Enrico Ramirez-Ruiz
Figure caption: Surface mass fractions of selected elements Xi in our remnants, scaled to solar-metallicity abundances Xi,⊙. We show results for the elements Xi listed in the legend. Lines end just before core He ignition. The 1Mβ1 remnant retains near-solar abundances until a dredge-up phase when it becomes a red giant. For the disrupted stars with β > 1, by the MS the envelopes are enriched in nitrogen (orange dashes) and depleted in carbon (red dots), both indicators of CNO fusion processes in the core. The presence of core-like CNO ratios on the stars’ surfaces is a result of convective mixing that occurs during the first 105 yr after disruption. Surface enhancement of helium is also observed in each of these models. These differences may manifest as spectroscopic signatures in the remnants of partial TDEs.
Paper: Black Hole Survival Guide: Searching for Stars in the Galactic Center that Endure Partial Tidal Disruption
Authors: Rewa Clark Bush, Samantha C. Wu, Rosa Wallace Everson, Ricardo Yarza, Ariadna Murguia-Berthier, Enrico Ramirez-Ruiz
Figure caption: Luminosity, temperature, and radius evolution of the three tidally disrupted remnants (red solid) with progenitor mass Mi = 1 M⊙. These remnants are compared to mass-equivalent stars (blue dashed–dotted line) that evolve from the PMS to the MS and up the red giant branch (RGB). The masses of the TDE remnants and their associated mass-equivalent stars are 0.956 M⊙, 0.708 M⊙, and 0.386 M⊙, respectively, from left to right. The start of core hydrogen fusion is denoted by star symbols for remnants and mass-equivalent stars. In addition, the evolution of an undisturbed M = 1 M⊙ star (black dotted) is shown from the time of disruption onward in order to represent the comparative evolution of the progenitor had it not undergone the TDE. Immediately after disruption, the remnants appear larger and more luminous than the progenitor, then shrink over the next several million years. After reigniting core hydrogen fusion, they stabilize near the MS locations of their mass-equivalent stars.
Paper: Black Hole Survival Guide: Searching for Stars in the Galactic Center that Endure Partial Tidal Disruption
Authors: Rewa Clark Bush, Samantha C. Wu, Rosa Wallace Everson, Ricardo Yarza, Ariadna Murguia-Berthier, Enrico Ramirez-Ruiz
Figure caption: Slices in 2D of the four TDE remnants studied in this Letter, selected from the STARS Library (J. A. P. Law-Smith et al. 2020a). The left three columns show remnants that begin as a 1 M⊙, 4.8 Gyr main-sequence (MS) star before disruption, and the fourth displayed in the rightmost column begins as a 3 M⊙, 0.3 Gyr MS star. Each is subjected to varying degrees of tidal disruption. The impact parameter (β) increases from left to right, indicating how deeply the star plunged past the SMBH’s tidal radius. Color bars indicate temperature in Kelvin (top row) and diffusion time in years (bottom row). The left panels have a width of 10 R⊙, while the rightmost column has a width of 22 R⊙. All snapshots are captured at roughly 80 tdyn after pericenter, corresponding to ≈38 hr after pericenter for the left three columns and ≈124 hr after pericenter for the right column.
Paper: Black Hole Survival Guide: Searching for Stars in the Galactic Center that Endure Partial Tidal Disruption
Authors: Rewa Clark Bush, Samantha C. Wu, Rosa Wallace Everson, Ricardo Yarza, Ariadna Murguia-Berthier, Enrico Ramirez-Ruiz
Figure caption: Luminosity evolution for the first few 100 Myr of the TDE remnants. The 1Mβ1, 1Mβ1.5, and 1Mβ2 TDE remnants from Figure 2 are shown with dashed lines and are compared here with their 1 M⊙ progenitor (black dashed–dotted line). Additionally, the 3Mβ4 remnant is shown (solid) to remain brighter than its mass-equivalent star (black dashed–dotted line), but dimmer than its progenitor (black dotted), throughout the PMS and MS. On the right, a histogram of the number of G-type objects (NG) per luminosity bin is shown (data are from A. M. Ghez et al. 2004, 2005; S. D. Hornstein et al. 2007; K. Phifer et al. 2013; G. Witzel et al. 2014; B. N. Sitarski 2016).
Paper: Black Hole Survival Guide: Searching for Stars in the Galactic Center that Endure Partial Tidal Disruption
Authors: Rewa Clark Bush, Samantha C. Wu, Rosa Wallace Everson, Ricardo Yarza, Ariadna Murguia-Berthier, Enrico Ramirez-Ruiz
Figure caption: Hertzsprung–Russell diagram of simulated stars on the hydrogen-burning MS. Data from Gaia Data Release 3 (Gaia Collaboration et al. 2016, 2021) of the closest 50,000 stars are plotted in the background as a logarithmic histogram where grayscale shading indicates the number density, to show the natural spread of Milky Way stars. The filled circles are MS single stars simulated in MESA, with the ZAMS masses listed in the upper right legend. The open diamonds represent the 1Mβ1, 1Mβ1.5, and 1Mβ2 TDE remnants, and the open square is the 3Mβ4 TDE remnant; all are shown at snapshots when they have returned to stable hydrogen burning, and the final masses of each remnant are noted in the bottom legend. All remnants appear substantially cooler and dimmer than their respective progenitors, while appearing subtly hotter and brighter than their mass-equivalent stars (or extremely hotter and brighter, in the case of the 3Mβ4 remnant).
Paper: ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05
Authors: Manuela Bischetti, Chiara Feruglio, Stefano Carniani, Valentina D'Odorico, Francesco Salvestrini, Fabrizio Fiore
Figure caption: (a) Map of continuum emission detected at >3σcont in the host galaxy of PSOJ183+05. Quasar location, identified as the peak of the ALMA continuum, is shown by the cross. (b) Velocity-integrated intensity map of [C II] emission detected >3σ[C II]. (c) [C II] velocity map. (d) [C II] velocity dispersion map, showing a biconical region oriented along the northeast–southwest direction with high σvel ∼ 150 km s−1, highlighted by the overlaid double cone. Contours highlight the location of the high-velocity [C II] emission with intensity >0.02 Jy beam−1 km s−1 (Figure 3(a)). The displayed region of 3 × 3 arcsec2 corresponds to the field of view covered by JWST/NIRSpec IFU. The dashed circle indicates the size of the stellar distribution measured by JWST/NIRCam observations in the host galaxies of z ∼ 6 quasars (Section 4.2). The white ellipse shows the ALMA beam.
Paper: ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05
Authors: Manuela Bischetti, Chiara Feruglio, Stefano Carniani, Valentina D'Odorico, Francesco Salvestrini, Fabrizio Fiore
Figure caption: (a) [C II] spectrum extracted from a circular 1″ aperture (blue histogram), similar to the spatial extent of the broad [C II] emission component mapped in Figure 3. The presence of blue/redshifted wings reaching velocities of ±1000 km s−1 can be observed. These wings are also present in the spectrum extracted from the same aperture in the low-resolution data set 2021.1.01082.S (normalized for comparison to the peak of the spectrum of the combined data set). The best-fit profile, shown in red, is obtained through a pixel-by-pixel spectral decomposition using a two-Gaussian component model (Section 2). (b) Residual spectrum obtained by subtracting the best-fit model to the data. The horizontal shaded region corresponds to the ±1σ noise level, calculated as ﹩{\sigma }_{{\rm{30}}}\sqrt{N}﹩, where N is the number of the independent ALMA beams in the extraction aperture. (c) Spectrum extracted from the high-resolution data set alone (Section 2), showing no significant [C II] emission beyond ±500 km s−1.
Paper: ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05
Authors: Manuela Bischetti, Chiara Feruglio, Stefano Carniani, Valentina D'Odorico, Francesco Salvestrini, Fabrizio Fiore
Figure caption: Residual map obtained by fitting a single (a) or a double (b) 2D Gaussian profile to the [C II] 0th moment map (Section 3). (c) Brightness profile of the [C II] emission in PSOJ183+05 (blue solid curve), normalized to the central peak value, and associated 68% confidence level uncertainty (shaded area). The brightness profile associated with the ALMA point-spread function (PSF) is shown by the dotted blue curve, while the dashed curve shows the profile associated with the 3σ level. We also show the profile for another z ∼ 6.6 quasar (in a merger, red curve) showing extended [C II] emission from M. Bischetti et al. (2024) and the stacked profile of z ∼ 6 quasar hosts by M. Novak et al. (2020), shown by the yellow curve. (d) [C II] brightness profile of PSOJ183+05 as in panel (c), compared to that extracted from the high-resolution data set alone (Section 2).
Paper: ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05
Authors: Manuela Bischetti, Chiara Feruglio, Stefano Carniani, Valentina D'Odorico, Francesco Salvestrini, Fabrizio Fiore
Figure caption: (a) Velocity-integrated intensity map associated with the broad [C II] emission (calculated as in Section 2). Contours correspond to [2,3,4,5,6,8]﹩{\sigma }_{[{\rm{C}}\,\mathrm{II}]}^{\mathrm{of}}﹩. (b) Velocity map. (c) Maximum velocity of the [C II] outflow. The cross refers to the quasar location, corresponding to the peak of the ALMA continuum emission (Figure 2(a)). The white ellipse shows the ALMA beam.
Paper: Euclid and Roman with JWST Could Reveal Supermassive Black Holes at up to z ∼ 15
Authors: Muhammad A. Latif, Daniel J. Whalen
Figure caption: Bolometric luminosities, Lbol, for the quasar as a function of redshift from J. Smidt et al. (2018).
Paper: Euclid and Roman with JWST Could Reveal Supermassive Black Holes at up to z ∼ 15
Authors: Muhammad A. Latif, Daniel J. Whalen
Figure caption: Rest-frame quasar spectra at 106, 107, 108, and 109 M⊙, shown by the black, red, green and blue lines, respectively.
Paper: Euclid and Roman with JWST Could Reveal Supermassive Black Holes at up to z ∼ 15
Authors: Muhammad A. Latif, Daniel J. Whalen
Figure caption: Top: AB magnitudes in Euclid  H and J bands. The horizontal dotted, dashed, and dotted–dashed lines are AB mag limits for the Euclid Wide, Deep, and Ultra Deep Surveys, respectively. Center: AB magnitudes in RST  H, J, and Y bands. The horizontal dashed line is the AB mag limit for the High Latitude Spectroscopic Survey. Bottom: AB magnitudes in the JWST 2.50 μm, 3.56 μm, 4.44 μm and 4.60 μm NIRCam bands. The JWST NIRCam AB magnitude limit is 32 for these filters, below the scale of the plot.
Paper: Euclid and Roman with JWST Could Reveal Supermassive Black Holes at up to z ∼ 15
Authors: Muhammad A. Latif, Daniel J. Whalen
Figure caption: Expected numbers of BH detections in the EW, ED, and HLS surveys based on DCBH number densities from simulations with UV backgrounds of 100 J21 and 300 J21, where J21 = 10−21 erg s−1 cm−2 Hz−1 sr−1. From JWST observations of AGNs that suggest number densities of 10−5 Mpc−3 at z = 10 we expect up to 2000 and 60,000 BHs in the EDS and HLSS at this redshift, respectively.
Paper: Discovery of Hα Emission from a Protoplanet Candidate around the Young Star 2MASS J16120668–3010270 with MagAO-X
Authors: Jialin Li, 嘉霖 李, Laird M. Close, Feng Long, 凤 龙, Jared R. Males, Sebastiaan Y. Haffert, Alycia Weinberger, Katherine Follette, Sean Andrews, John Carpenter, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Gregory J. Herczeg, 雷歌 沈, Parker T. Johnson, Maggie Y. Kautz, Jay K. Kueny, Rixin Li, Joshua Liberman, Joseph D. Long, Jennifer Lumbres, Sebastian Marino, Luca Matrà, Eden A. McEwen, Olivier Guyon, Logan A. Pearce, Laura M. Pérez, Paola Pinilla, Lauren Schatz, Yangfan Shi, Katie Twitchell, Kevin Wagner, David Wilner, Ya-Lin Wu, Shangjia Zhang, 尚嘉 张, Zhaohuan Zhu
Figure caption: Observations of 2MJ1612 with MagAO-X and ALMA. A composite image overlying the ALMA Band 6 observation and MagAO-X SDI image on April 16 is in the top panel. The companion at 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩14 with Hα excess is pointed to by the labeled purple arrow. The beam size of the ALMA image is roughly 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩ 08, shown in the lower left of the top panel. Dashed and solid circles in blue denote, respectively, the rough location of the compact dust source and the kinematic kink detected in an older epoch of ALMA data by A. Sierra et al. (2024). The bottom panel consists of six small figures showcasing the MagAO-X continuum, Hα, and ASDI images on April 13 and April 16. The April 13 MagAO-X data shown have all been convolved with a Gaussian kernel of standard deviation of 2 pixels (FWHM ≈ 2.35 × 2 = 4.7 pixels), while the April 16 data have been convolved by a Gaussian of 1.75 pixels. A dashed white circle with a 29.5 mas radius is placed at the optimal position of the April 13 Hα source with an SNR of 5.3. A semitransparent circle with a radius of approximately 103.25 mas is also overlaid, centered on the star. A solid white circle of radius ∼16 mas is placed in the MagAO-X panels to represent its beam size after the HP filter. For all images, north is up and east is left.
Paper: Discovery of Hα Emission from a Protoplanet Candidate around the Young Star 2MASS J16120668–3010270 with MagAO-X
Authors: Jialin Li, 嘉霖 李, Laird M. Close, Feng Long, 凤 龙, Jared R. Males, Sebastiaan Y. Haffert, Alycia Weinberger, Katherine Follette, Sean Andrews, John Carpenter, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Gregory J. Herczeg, 雷歌 沈, Parker T. Johnson, Maggie Y. Kautz, Jay K. Kueny, Rixin Li, Joshua Liberman, Joseph D. Long, Jennifer Lumbres, Sebastian Marino, Luca Matrà, Eden A. McEwen, Olivier Guyon, Logan A. Pearce, Laura M. Pérez, Paola Pinilla, Lauren Schatz, Yangfan Shi, Katie Twitchell, Kevin Wagner, David Wilner, Ya-Lin Wu, Shangjia Zhang, 尚嘉 张, Zhaohuan Zhu
Figure caption: (a) A composite image overplotting the SPHERE/IRDIS H-band circumsymmetrically polarized (Qϕ) image and the April 16 MagAO-X ASDI image with K-band sources plotted as the orange cross. (b) The accepted 50 orbits fitted with OFTI with the highest likelihood, using the three astrometric data points (two Hα and one K band). The right two panels show the separation in mas and PA in degrees over time for the same orbits.
Paper: Hubble Space Telescope Observations of the Interstellar Interloper 3I/ATLAS
Authors: David Jewitt, Man-To Hui, Max Mutchler, Yoonyoung Kim, Jessica Agarwal
Figure caption: (Upper) Combined 130 s F350LP image of 3I/ATLAS showing diffuse asymmetric emission to the northwest. (Lower) Same image contoured, with scale bar and direction arrows shown. The yellow and green arrows mark, respectively, the projected negative heliocentric velocity vector and the projected antisolar direction. Note that the bulk of the dust is sunward of the nucleus.
Paper: Detecting Extraterrestrial Civilizations that Employ an Earth-level Deep Space Network
Authors: Pinchen Fan, Jason T. Wright, T. Joseph W. Lazio
Figure caption: Illustration of the difference in apparent positions of the spacecraft and the planets/Sun, due to light-time delay, for Earth and for an extraterrestrial observer. Distances are expressed in terms of the one-way light-travel time (OWDT).
Paper: Milky Way’s Metal-poor Stars Display Chemical Transition near the Solar Radius
Authors: Khyati Malhan
Figure caption: rGC vs. [Fe/H] and rGC vs. [X/Fe]s of the metal-poor sample. In each panel, the vertical line at rGC = 8 kpc denotes the solar radius. The horizontal lines (visible in some panels) are drawn where the Y-axis = 0.
Paper: Milky Way’s Metal-poor Stars Display Chemical Transition near the Solar Radius
Authors: Khyati Malhan
Figure caption: Overview of the stars in the [Fe/H] vs. [Mg/Fe] space. Different shaded regions represent different sample selections.
Paper: Transient Gamma Rays from the 2021 Outburst of the Recurrent Nova RS Ophiuchi: The Effect of Gamma-Ray Absorption
Authors: Vo Hong Minh Phan, Pierre Cristofari, Enrico Peretti, Vincent Tatischeff, Andrea Ciardi
Figure caption: Integrated gamma-ray flux over time compared to data from F. Aharonian et al. (2022). The lightcurves for Fermi-LAT and HESS (green and red line, respectively) are estimated by integrating the gamma-ray flux over the energy ranges 0.1–100 and 250–2500 GeV, respectively. Solid and dashed lines are correspondingly for the case with and without gamma-ray absorption. The TeV lightcurve with absorption for t < 1 day is plotted in dotted line to highlight the uncertainty of the model in this period of time where no data are available (see the discussion in Section 3.3).
Paper: Transient Gamma Rays from the 2021 Outburst of the Recurrent Nova RS Ophiuchi: The Effect of Gamma-Ray Absorption
Authors: Vo Hong Minh Phan, Pierre Cristofari, Enrico Peretti, Vincent Tatischeff, Andrea Ciardi
Figure caption: Left: luminosity function of optical photons (see Equation (12)) compared to data collected in C. C. Cheung et al. (2022) assuming dN = 1.6 kpc. Right: opacities over time estimated from Equations (A9) and (A10) for Eγ = 1 TeV.
Paper: Milky Way’s Metal-poor Stars Display Chemical Transition near the Solar Radius
Authors: Khyati Malhan
Figure caption: Overview of the metal-poor sample. Panel “a” shows the on-sky distribution in Galactic coordinates, panel “b” shows the metallicity distribution function, panel “c” shows the top view of the Galaxy in the Cartesian x–y plane, and panel “d” shows the Galactic R–z plane. The orange dot denotes the Sun.
Paper: Milky Way’s Metal-poor Stars Display Chemical Transition near the Solar Radius
Authors: Khyati Malhan
Figure caption: rGC vs. [Fe/H] and rGC vs. [X/Fe]s. Each point corresponds to a star. The distributions corresponding to the metal-poor sample are shown in blue, those corresponding to the thick-disk sample are in red, and the thick-disk-to-halo sample is in gold. In each panel, the vertical line at rGC = 8 kpc denotes the solar radius. The horizontal lines (visible in some panels) are drawn where the Y-axis = 0.
Paper: Milky Way’s Metal-poor Stars Display Chemical Transition near the Solar Radius
Authors: Khyati Malhan
Figure caption: Same as Figure 2, but for the thick-disk sample (top four panels) and the thick-disk-to-halo sample (bottom four panels).