adsabs/AstroCLIMB huggingface dataset:
Paper: An Inward-moving and Asymmetric Velocity Wave Detected in LAMOST-Gaia
Authors: Yuqin Chen, Gang Zhao, Wenbo Wu, Zixi Guo, Haopeng Zhang, Zhuohan Li
Figure caption: The velocity waves in the R g–V  ϕ –V  R  plane. There is a change in the direction at R g ∼ 11.5 kpc (red line).
Paper: An Inward-moving and Asymmetric Velocity Wave Detected in LAMOST-Gaia
Authors: Yuqin Chen, Gang Zhao, Wenbo Wu, Zixi Guo, Haopeng Zhang, Zhuohan Li
Figure caption: The comparison of the G1 group (blue dots) with Sgr member (red open circles, [Al/Fe] < − 0.2 dex) and non-Sgr (crosses, [Al/Fe] > − 0.2 dex) groups in the [Fe/H] vs. [Al/Fe] (upper) and [Mg/Fe] (lower) diagrams.
Paper: An Inward-moving and Asymmetric Velocity Wave Detected in LAMOST-Gaia
Authors: Yuqin Chen, Gang Zhao, Wenbo Wu, Zixi Guo, Haopeng Zhang, Zhuohan Li
Figure caption: The comparison of the G1 with that of Sgr member in the [C/N] vs. [Fe/H] diagram.
Paper: An Inward-moving and Asymmetric Velocity Wave Detected in LAMOST-Gaia
Authors: Yuqin Chen, Gang Zhao, Wenbo Wu, Zixi Guo, Haopeng Zhang, Zhuohan Li
Figure caption:  R g–V  z  coded by [C/N] for thin-disk stars.
Paper: An Inward-moving and Asymmetric Velocity Wave Detected in LAMOST-Gaia
Authors: Yuqin Chen, Gang Zhao, Wenbo Wu, Zixi Guo, Haopeng Zhang, Zhuohan Li
Figure caption: [C/N]–[Fe/H] plane for the G1 (upper) and G0 (lower) groups.
Paper: GJ 367b Is a Dark, Hot, Airless Sub-Earth
Authors: Michael Zhang, Renyu Hu, Julie Inglis, Fei Dai, Jacob L. Bean, Heather A. Knutson, Kristine Lam, Elisa Goffo, Davide Gandolfi
Figure caption: Left: an alternate fit to the eclipse spectra, where the systematics model includes the ramp. Note that the two eclipses both have a spike at 9 μm, and that the two spikes are consistent. Comparing to scaled models that have a silicate emission feature at 9 μm (Ito et al. 2015; Lee et al. 2019), we see that the spike is much higher and sharper than the silicate emission features found in these models. Right: in eclipse 1, 9 μm is unusual in that it has the highest ramp of all wavelengths. In eclipse 2, there is nothing unusual about the ramp at 9 μm.
Paper: Which Came First: Supermassive Black Holes or Galaxies? Insights from JWST
Authors: Joseph Silk, Mitchell C. Begelman, Colin Norman, Adi Nusser, Rosemary F. G. Wyse
Figure caption: The transition in star formation rates and black hole growth as redshift decreases from regimes where positive feedback dominates to a later epoch when feedback is largely negative. (After Figure 2 of Costa et al. 2014.) The epoch of reionization is indicated by the change from red to blue.
Paper: PEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a Tip of the Red Giant Branch Distance of 30 Mpc
Authors: Timothy Carleton, Timothy Ellsworth-Bowers, Rogier A. Windhorst, Seth H. Cohen, Christopher J. Conselice, Jose M. Diego, Adi Zitrin, Haylee N. Archer, Isabel McIntyre, Patrick Kamieneski, Rolf A. Jansen, Jake Summers, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Benne W. Holwerda
Figure caption: The large-scale environment of PEARLSDG. Both plots show the location of nearby galaxies with respect to PEARLSDG (shown as the cyan star), with point sizes proportional to the stellar mass of the system. Top: the co-moving distance to PEARLSDG from its TRGB, as a subset of objects in the NSA with either direct distance estimates from Cosmicflows-4 (green points) or our fundamental plane analysis (blue points). Objects in the Cosmicflows-4 catalog without a counterpart in the NSA are shown as light green diamonds defaulting to a stellar mass of 109 M ⊙. Bottom: the recessional velocity of PEARLSDG and nearby systems in the NSA. PEARLSDG appears to be beyond the sphere of influence of any massive galaxy.
Paper: PEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a Tip of the Red Giant Branch Distance of 30 Mpc
Authors: Timothy Carleton, Timothy Ellsworth-Bowers, Rogier A. Windhorst, Seth H. Cohen, Christopher J. Conselice, Jose M. Diego, Adi Zitrin, Haylee N. Archer, Isabel McIntyre, Patrick Kamieneski, Rolf A. Jansen, Jake Summers, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Benne W. Holwerda
Figure caption: Top: observed spectrum (black) along with error spectrum (thin green line). Bottom: zoomed in on the Hγ, Hβ, and Mg features (highlighted by dashed lines in the top panel). The model spectrum at the measured recessional velocity of cz = 2340 ± 180 km s−1 is shown as the thin blue line. For comparison, the red dotted line shows the model spectrum redshifted to the nearest massive galaxy at cz = 3987 km s−1. PEARLSDG is 1650 km s−1 separated from the nearest massive neighbor, so it is unlikely to be associated with it.
Paper: PEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a Tip of the Red Giant Branch Distance of 30 Mpc
Authors: Timothy Carleton, Timothy Ellsworth-Bowers, Rogier A. Windhorst, Seth H. Cohen, Christopher J. Conselice, Jose M. Diego, Adi Zitrin, Haylee N. Archer, Isabel McIntyre, Patrick Kamieneski, Rolf A. Jansen, Jake Summers, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Benne W. Holwerda
Figure caption: Broadband SED of PEARLSDG, including all available UV, optical, and near-IR data, shown alongside the best-fit SED from PROSPECTOR. The overlap of DECAM and SDSS, as well as JWST and Spitzer bands, support the accuracy of our photometry. The SED is fit well with a predominantly old, metal-poor stellar population, with a very small contribution from younger stars.
Paper: Sub-GeV Gamma Rays from Nearby Seyfert Galaxies and Implications for Coronal Neutrino Emission
Authors: Kohta Murase, Christopher M. Karwin, Shigeo S. Kimura, Marco Ajello, Sara Buson
Figure caption: NGC 4945 results for three different ROI sizes, as specified in the legends. Results from the 4FGL-DR3 are also overlaid. The left panel shows the SED, the middle panel shows the corresponding significance (﹩\sqrt{\mathrm{TS}}﹩), and the right panel shows the count residuals. In addition to the nominal binning, the first energy bin is divided into two smaller bins, shown with open markers corresponding to the ROI size. This is done to make a more direct comparison to the 4FGL-DR3, as discussed in the text. In the middle panel, we indicate the predicted significance based on the additional exposure time for both the noise-limited case (﹩\sqrt{t}﹩) and the signal-limited case (t). The error bars on the data points are 1σ, and the ULs are plotted for bins with TS < 4 and shown at the 95% C.L.
Paper: Sub-GeV Gamma Rays from Nearby Seyfert Galaxies and Implications for Coronal Neutrino Emission
Authors: Kohta Murase, Christopher M. Karwin, Shigeo S. Kimura, Marco Ajello, Sara Buson
Figure caption: Spatial residuals for the full energy range (top row) and first energy bin (bottom row). From left to right, the columns are 10°, 20°, and 26° ROIs, respectively. Red, cyan, and green contours are shown at the ±3σ, ±4σ, and ±5σ levels.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: Black, blue, and red colors mark ∣b Gal∣ ≥ 20°, 30°, 45° for 30° ≤ l Gal ≤ 330°. The points are slightly shifted at each E for clearer display, and the configuration of 45° ≤ l Gal ≤ 315° is not shown to avoid clutter (it is shown in Figure 4). The square root of the clustering mean power over ℓ ≥ 20 from Figure 3 are shown with squares. The dipoles in the source-subtracted 13 yr maps are shown with filled circles with the 68% uncertainties.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: The source-subtracted LAT maps coadded from 2.74 to 115 GeV. The displayed sky is masked for ∣b Gal∣ ≤ 20°. The coordinate grid is marked every 15°. The DGB dipole directions are plotted for the 45° ≤ l Gal ≤ 315°, ∣b Gal∣ ≥ 45° with red colors and the 30° ≤ l Gal ≤ 330°, ∣b Gal∣ ≥ 30° with green colors. The two contours in each case correspond to 1σ and 2σ (68% and 95%) dipole uncertainties. The size of each contour decreases as it should when larger sky area is considered. The smaller/narrower contours indicate the directions and uncertainties of the 13 yr assembled map shown here. The larger/broader contours show the same once the (A−B)/ 2 dipoles have been subtracted. The yellow arrow indicates the tentative position of the Pierre Auger dipole prior to the deflection by the modeled Galactic magnetic field. The Pierre Auger UHECR dipole is marked with the yellow spot and its 68% directional uncertainty is ∼15°. The map with the ecliptic plane masked out with ∣β Ecl∣ ≤ 5° is shown in Figure 7.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: (a) Total number of photons in each narrow band is marked with filled circles. Black, blue, and red circles correspond to ∣b Gal∣ ≥ 20°, 30°, and 45° while filled (open) circles corresponds to 0 ≤ l Gal ≤ 360° (30° ≤ l Gal ≤ 330°). The LAT beam is shown with green stars for the values displayed on the right vertical axis. The horizontal thick green solid line marks the pixel area for N side = 128. The slope of the DGB is marked with black solid line. (b) Flux histograms for 2.74 ≤ E(GeV) ≤ 115 and 30° ≤ l Gal ≤ 330° with black/blue/red corresponding to ∣b Gal∣ ≥ 20°, 30°, and 45°. Dashed and solid vertical lines of three colors mark the mean flux and flux dispersion of each map.
Paper: Uncovering a Massive z ∼ 7.7 Galaxy Hosting a Heavily Obscured Radio-loud Active Galactic Nucleus Candidate in COSMOS-Web
Authors: Erini Lambrides, Marco Chiaberge, Arianna S. Long, Daizhong Liu, Hollis B. Akins, Andrew F. Ptak, Irham Taufik Andika, Alessandro Capetti, Caitlin M. Casey, Jaclyn B. Champagne, Katherine Chworowsky, Tracy E. Clarke, Olivia R. Cooper, Xuheng Ding, Dillon Z. Dong, Andreas L. Faisst, Jordan Y. Forman, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Kirsten R. Hall, Santosh Harish, Christopher C. Hayward, Michaela Hirschmann, Taylor A. Hutchison, Knud Jahnke, Shuowen Jin, Jeyhan S. Kartaltepe, Emma T. Kleiner, Anton M. Koekemoer, Vasily Kokorev, Sinclaire M. Manning, Crystal L. Martin, Jed McKinney, Colin Norman, Kristina Nyland, Masafusa Onoue, Brant E. Robertson, Marko Shuntov, John D. Silverman, Massimo Stiavelli, Benny Trakhtenbrot, Eleni Vardoulaki, Jorge A. Zavala, Natalie Allen, Olivier Ilbert, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Sune Toft
Figure caption: Left panel: optical-IR-radio SED fitting with BC03 stellar (Bruzual & Charlot 2003), mid-IR AGN (Mullaney et al. 2011), Draine & Li dust (Draine & Li 2007), and power-law radio templates (using the MICHI2 code; Liu et al. 2021). The black line indicates the composite best-fit model, and the blue symbols are photometric data points, with upper limits shown as downward arrows. The stellar, mid-IR AGN, dust, and radio components are indicated by the cyan, yellow, red, and magenta dashed lines, respectively. Right panels: the 1/ χ 2 distributions from the fitting for the four parameters: stellar mass, dust attenuation E(B − V), AGN component’s luminosity integrated over 10–1000 μm, and dust component’s luminosity integrated over 8–1000 μm. The yellow highlighted regions correspond to the 95% confidence intervals.
Paper: Uncovering a Massive z ∼ 7.7 Galaxy Hosting a Heavily Obscured Radio-loud Active Galactic Nucleus Candidate in COSMOS-Web
Authors: Erini Lambrides, Marco Chiaberge, Arianna S. Long, Daizhong Liu, Hollis B. Akins, Andrew F. Ptak, Irham Taufik Andika, Alessandro Capetti, Caitlin M. Casey, Jaclyn B. Champagne, Katherine Chworowsky, Tracy E. Clarke, Olivia R. Cooper, Xuheng Ding, Dillon Z. Dong, Andreas L. Faisst, Jordan Y. Forman, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Kirsten R. Hall, Santosh Harish, Christopher C. Hayward, Michaela Hirschmann, Taylor A. Hutchison, Knud Jahnke, Shuowen Jin, Jeyhan S. Kartaltepe, Emma T. Kleiner, Anton M. Koekemoer, Vasily Kokorev, Sinclaire M. Manning, Crystal L. Martin, Jed McKinney, Colin Norman, Kristina Nyland, Masafusa Onoue, Brant E. Robertson, Marko Shuntov, John D. Silverman, Massimo Stiavelli, Benny Trakhtenbrot, Eleni Vardoulaki, Jorge A. Zavala, Natalie Allen, Olivier Ilbert, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Sune Toft
Figure caption: Results from fitting the optical, NIR, and MIR with EAzYpy. Non-detections with 27 mag upper limits: HSC g, HSC r, HSC i, HSC z, HST F814W, HSC y. > 3σ detections: JWST F115W, JWST F150W, HST F160W, JWST F277W, IRAC Channel 1, JWST F444W, IRAC Channel 2, IRAC Channel 3, JWST MIRI 7.7 μm. The redshift is constrained to ﹩{\text{}}z={7.7}_{-0.3}^{+0.4}﹩ fit with combinations of simple stellar population templates from Bruzual & Charlot (2003). Inset: we show the p(z) via EAzY and BAGPIPES
Paper: Uncovering a Massive z ∼ 7.7 Galaxy Hosting a Heavily Obscured Radio-loud Active Galactic Nucleus Candidate in COSMOS-Web
Authors: Erini Lambrides, Marco Chiaberge, Arianna S. Long, Daizhong Liu, Hollis B. Akins, Andrew F. Ptak, Irham Taufik Andika, Alessandro Capetti, Caitlin M. Casey, Jaclyn B. Champagne, Katherine Chworowsky, Tracy E. Clarke, Olivia R. Cooper, Xuheng Ding, Dillon Z. Dong, Andreas L. Faisst, Jordan Y. Forman, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Kirsten R. Hall, Santosh Harish, Christopher C. Hayward, Michaela Hirschmann, Taylor A. Hutchison, Knud Jahnke, Shuowen Jin, Jeyhan S. Kartaltepe, Emma T. Kleiner, Anton M. Koekemoer, Vasily Kokorev, Sinclaire M. Manning, Crystal L. Martin, Jed McKinney, Colin Norman, Kristina Nyland, Masafusa Onoue, Brant E. Robertson, Marko Shuntov, John D. Silverman, Massimo Stiavelli, Benny Trakhtenbrot, Eleni Vardoulaki, Jorge A. Zavala, Natalie Allen, Olivier Ilbert, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Sune Toft
Figure caption: Selection of postage stamp images of the candidate z ∼ 7.7 RL AGN, COSW-106725. Top row, from left to right: HSC-g, HST Advanced Camera for Surveys F814W, JWST F115W. Middle row: JWST F150W, JWST F277W, JWST F444W. Bottom row: JWST MIRI F770W, ALMA 343 GHz, and VLA 1.4 GHz. The ALMA extent is overlaid on each image (in white). The 3σ upper limits are reported for the non-detections. The upper left source in the UV/Optical/NIR images is a low-z interloper (Weaver et al. 2022).
Paper: Uncovering a Massive z ∼ 7.7 Galaxy Hosting a Heavily Obscured Radio-loud Active Galactic Nucleus Candidate in COSMOS-Web
Authors: Erini Lambrides, Marco Chiaberge, Arianna S. Long, Daizhong Liu, Hollis B. Akins, Andrew F. Ptak, Irham Taufik Andika, Alessandro Capetti, Caitlin M. Casey, Jaclyn B. Champagne, Katherine Chworowsky, Tracy E. Clarke, Olivia R. Cooper, Xuheng Ding, Dillon Z. Dong, Andreas L. Faisst, Jordan Y. Forman, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Kirsten R. Hall, Santosh Harish, Christopher C. Hayward, Michaela Hirschmann, Taylor A. Hutchison, Knud Jahnke, Shuowen Jin, Jeyhan S. Kartaltepe, Emma T. Kleiner, Anton M. Koekemoer, Vasily Kokorev, Sinclaire M. Manning, Crystal L. Martin, Jed McKinney, Colin Norman, Kristina Nyland, Masafusa Onoue, Brant E. Robertson, Marko Shuntov, John D. Silverman, Massimo Stiavelli, Benny Trakhtenbrot, Eleni Vardoulaki, Jorge A. Zavala, Natalie Allen, Olivier Ilbert, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Sune Toft
Figure caption: Radio SED: all fluxes and associated errors are listed in Table 1. We measure the spectral slope between two sets of radio frequencies (blue line, orange line) and find significant spectral steepening indicative of high-z RL AGN (Saxena et al. 2018a; Broderick et al. 2022; Endsley et al. 2023). In the upper-right corner inset, we show the radio SED for the z spec = 6.8 heavily obscured RL AGN from Endsley et al. (2023) for reference.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: Dimensionless dipole in the same notations as in Figure 3. In addition to the numbers in Figure 3, red/blue/black open circles denote the configurations with 45° ≤ l Gal ≤ 315° and 2.74 < E(GeV) < 115 slightly shifted in E for clear viewing (this is not shown in the earlier figure to avoid overcrowding—all the numbers are consistent with what is shown here). The dimensionless dipoles from CRs (UHECR) at 6.5%, Compton–Getting amplified CMB dipole, and clustering component are marked with horizontal lines. Removing the ecliptic plane, as discussed in the Appendix, further reduces the scatter—see Figure 8. The statistical uncertainties are shown at 95% c.l.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: (Left) Histograms of fluxes after the 13 yr clipping mask has been applied to the maps shown in Figure 9. The standard deviations are shown with vertical solid lines corresponding to σ  F,(A−B)/2∼1.2 × 10−7 GeV cm−2 s−1 sr−1. The masking from clipping has been applied, and the sky has been kept at 30° ≤ l Gal ≤ 330° and ∣b Gal∣ ≥ 20°, 30°, 45° for the black, blue, and red colors. (Right) The correlation coefficient, R, between the (A − B) and the final 13 yr maps. Black, red, and blue symbols correspond to ∣b cut∣ > 20°, 30°, 45°. The filled and open symbols correspond to 30° ≤ l Gal ≤ 330° and 45° ≤ l Gal ≤ 315°, respectively.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: The ratio of the dipole power, ﹩{C}_{1}\equiv \langle {d}_{i}^{2}\rangle ﹩, in the (A − B)/2 to 13 yr maps. Open circles correspond to 45° ≤ l Gal ≤ 315° and filled to 30° ≤ l Gal ≤ 330°. Black, blue, and red denote ∣b Gal∣ ≥ 20°, 30°, 45°, respectively.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: Number of photons per given pixel common in the two adjacent maps is shown with density plots for unclipped maps. The pixels where there are zero photons in one of the two bands are shown at n  γ  = 0.01. The shown colors span 0–5500 common pixels logarithmically.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: The (A − B)/2 map from 2.74 to 115 GeV is shown with the overall 13 yr clipping mask applied and Galaxy removed for ∣b Gal∣ ≤ 20°.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: Dimensionless dipole from the maps in Figure 7 in the same notations as in Figure 4 without masking the ecliptic plane. The error bars are barely distinguishable from those in Figure 4 and are not shown to avoid clutter.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: Same as Figure 5 but for clipped maps.
Paper: Probing the Dipole of the Diffuse Gamma-Ray Background
Authors: A. Kashlinsky, F. Atrio-Barandela, C. S. Shrader
Figure caption: Map with the ecliptic plane masked as in Figure 4 without masking the ecliptic plane.
Paper: The Peak of the Fallback Rate from Tidal Disruption Events: Dependence on Stellar Type
Authors: Ananya Bandopadhyay, Julia Fancher, Aluel Athian, Valentino Indelicato, Sarah Kapalanga, Angela Kumah, Daniel A. Paradiso, Matthew Todd, Eric R. Coughlin, C. J. Nixon
Figure caption: Left: peak fallback times, t peak, and rates, ﹩{\dot{M}}_{\mathrm{peak}}﹩, for stars disrupted by a 106 M ⊙ SMBH using the frozen-in and CN22 models; the stellar mass and age are indicated in the legends (the black dashed lines join stars of a given age). Right: same as the left panel, but showing only the predictions of the CN22 model (note t peak is in days) and numerical hydrodynamics simulations (shown by the inverted and upright triangles). (Some low-mass stars reach neither MAMS nor TAMS in 14 Gyr; we nonetheless include these data points to illustrate the predictions of the model over many stellar types, but their coloration is semitransparent.)
Paper: The Peak of the Fallback Rate from Tidal Disruption Events: Dependence on Stellar Type
Authors: Ananya Bandopadhyay, Julia Fancher, Aluel Athian, Valentino Indelicato, Sarah Kapalanga, Angela Kumah, Daniel A. Paradiso, Matthew Todd, Eric R. Coughlin, C. J. Nixon
Figure caption: Left: the probability distribution function of peak times, ﹩{f}_{{t}_{\mathrm{peak}}}﹩, for the tidal disruption of 0.2–5M ⊙ stars (at different ages in the main sequence) by a 106 M ⊙ SMBH. The mean and standard deviation of the distribution for all stars are given by t peak = 23.2 ± 4.0 days. Right: ﹩{f}_{{t}_{\mathrm{peak}}}﹩ weighted by a Kroupa initial mass function truncated at 1.5 M ⊙, to account for the observed overabundance of low-mass stars in the universe, giving t peak = 29.8 ± 3.6 days. The vertical dashed line indicates the mean of the probability distribution, ﹩{\mu }_{{{\rm{t}}}_{\mathrm{peak}}}﹩, and the 1σ confidence interval, ﹩{\sigma }_{{{\rm{t}}}_{\mathrm{peak}}}﹩, is indicated by the horizontal error bar.
Paper: The Peak of the Fallback Rate from Tidal Disruption Events: Dependence on Stellar Type
Authors: Ananya Bandopadhyay, Julia Fancher, Aluel Athian, Valentino Indelicato, Sarah Kapalanga, Angela Kumah, Daniel A. Paradiso, Matthew Todd, Eric R. Coughlin, C. J. Nixon
Figure caption: Left: the impact parameter β c = r t/r t, c required for complete disruption. As stellar age increases the star becomes more centrally concentrated, resulting in larger β c. Right: the fraction of stars that enter within the fiducial tidal radius r t, have impact parameters β > β c (i.e., are completely destroyed), and are not directly captured by a Schwarzschild SMBH with M • = 106 M ⊙.
Paper: The Peak of the Fallback Rate from Tidal Disruption Events: Dependence on Stellar Type
Authors: Ananya Bandopadhyay, Julia Fancher, Aluel Athian, Valentino Indelicato, Sarah Kapalanga, Angela Kumah, Daniel A. Paradiso, Matthew Todd, Eric R. Coughlin, C. J. Nixon
Figure caption: The fallback rate for the complete disruption of a 3M ⊙ ZAMS star by a 106 M ⊙ SMBH. The dashed curve shows the frozen-in approximation following the prescription in Lodato et al. (2009), while the solid curve is from a hydrodynamical simulation. The inset shows a zoomed-in view near the peak.
Paper: Whither or Wither the Sulfur Anomaly in Planetary Nebulae?
Authors: Shuyu Tan, Quentin A. Parker
Figure caption: Comparison of S/H vs. O/H and Ar/H among PN samples c.f. H2BCG data (pluses). The two left panels show Galactic disk PNs from HSK12, with blue and pink triangles triangles for high- and lower-quality measurements with uncertainties <0.2 dex and >0.2 dex. The right two panels give our Galactic bulge PN results from Paper III as orange squares. In all panels, best-fit lines are the same color as the data. Only HSK12 data points with uncertainties <0.2 dex (HSK12+) were fitted. Our VLT results for O/H and Ar/H display best-fit lines parallel to the H2BCG trends with clear lockstep behavior. The red asterisk is solar abundance. Color-coded box plots at the top and right of each panel depict distributions of O/H, Ar/H, and S/H. Red lines indicate median values with boxes extending from the 25th to 75th percentiles and whiskers from 1% to 99% with outliers as crosses.