adsabs/AstroCLIMB huggingface dataset:
Paper: Periodic Gamma-Ray Modulation of the Blazar PG 1553+113 Confirmed by Fermi-LAT and Multiwavelength Observations
Authors: S. Abdollahi, L. Baldini, G. Barbiellini, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, P. A. Caraveo, F. Casaburo, E. Cavazzuti, C. C. Cheung, G. Chiaro, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, S. Cutini, F. D'Ammando, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, S. Garrappa, D. Gasparrini, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, E. Hays, D. Horan, M. Kuss, S. Larsson, M. Laurenti, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, L. Marcotulli, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, M. Orienti, E. Orlando, J. F. Ormes, D. Paneque, M. Perri, M. Persic, M. Pesce-Rollins, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, A. Reimer, O. Reimer, P. M. Saz Parkinson, L. Scotton, D. Serini, A. Sesana, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, M. N. Takahashi, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, J. Valverde, F. Verrecchia, G. Zaharijas
Figure caption: OVRO 15 GHz light curve (in black with error bars) together with LAT (E > 1 GeV) flux (purple). Inset panels show cross correlations (DCCF) between the light curves of segments (a)–(c). While the overall time lag of the 15 GHz flux relative to gamma ray is on the order of 200 days there are substantial cycle-to-cycle variations. Lag 0 in the DCCF plots is indicated by vertical lines.
Paper: Periodic Gamma-Ray Modulation of the Blazar PG 1553+113 Confirmed by Fermi-LAT and Multiwavelength Observations
Authors: S. Abdollahi, L. Baldini, G. Barbiellini, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, P. A. Caraveo, F. Casaburo, E. Cavazzuti, C. C. Cheung, G. Chiaro, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, S. Cutini, F. D'Ammando, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, S. Garrappa, D. Gasparrini, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, E. Hays, D. Horan, M. Kuss, S. Larsson, M. Laurenti, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, L. Marcotulli, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, M. Orienti, E. Orlando, J. F. Ormes, D. Paneque, M. Perri, M. Persic, M. Pesce-Rollins, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, A. Reimer, O. Reimer, P. M. Saz Parkinson, L. Scotton, D. Serini, A. Sesana, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, M. N. Takahashi, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, J. Valverde, F. Verrecchia, G. Zaharijas
Figure caption: Distribution of the LSP signal peaks for 106 simulated light curves, respectively for the public 3 day bin LCR light curve shown in Figure 12 in the main panel, and for the detrended version of it in the inset panel. Dashed lines are the LSP power for the two, true data, light curves. Significance of the period here is 4σ and >4σ for the 3 day bin LCR light curve and the detrended version of it, respectively.
Paper: Periodic Gamma-Ray Modulation of the Blazar PG 1553+113 Confirmed by Fermi-LAT and Multiwavelength Observations
Authors: S. Abdollahi, L. Baldini, G. Barbiellini, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, P. A. Caraveo, F. Casaburo, E. Cavazzuti, C. C. Cheung, G. Chiaro, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, S. Cutini, F. D'Ammando, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, S. Garrappa, D. Gasparrini, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, E. Hays, D. Horan, M. Kuss, S. Larsson, M. Laurenti, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, L. Marcotulli, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, M. Orienti, E. Orlando, J. F. Ormes, D. Paneque, M. Perri, M. Persic, M. Pesce-Rollins, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, A. Reimer, O. Reimer, P. M. Saz Parkinson, L. Scotton, D. Serini, A. Sesana, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, M. N. Takahashi, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, J. Valverde, F. Verrecchia, G. Zaharijas
Figure caption: Pulse phase variation relative to a strictly coherent period. The pulse phase for each cycle is estimated by cross correlation with a Fourier model fitted to the full light curve. The first point is from the optical data in Figure 2. All other points are from the E > 1 GeV light curve. The cycle number corresponds to N in Equation (1). An observed–computed (O − C) diagram compares the observed time of maximum flux O with the calculated time C, assuming a known constant period T, and is a classical method for studies of period changes in variable stars.
Paper: Periodic Gamma-Ray Modulation of the Blazar PG 1553+113 Confirmed by Fermi-LAT and Multiwavelength Observations
Authors: S. Abdollahi, L. Baldini, G. Barbiellini, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, P. A. Caraveo, F. Casaburo, E. Cavazzuti, C. C. Cheung, G. Chiaro, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, S. Cutini, F. D'Ammando, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, S. Garrappa, D. Gasparrini, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, E. Hays, D. Horan, M. Kuss, S. Larsson, M. Laurenti, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, L. Marcotulli, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, M. Orienti, E. Orlando, J. F. Ormes, D. Paneque, M. Perri, M. Persic, M. Pesce-Rollins, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, A. Reimer, O. Reimer, P. M. Saz Parkinson, L. Scotton, D. Serini, A. Sesana, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, M. N. Takahashi, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, J. Valverde, F. Verrecchia, G. Zaharijas
Figure caption: SED of PG 1553+113 in the precursor phase shown in red (gray) circles as highlighted in the right panel of Figure 3 and the main phase shown in blue (dark) circles. A cutoff power-law function was used, shown by the green dashed lines.
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Properties of the full LRIS sample. Left: Hα redshift distributions for the LRIS sample. The open histogram represents the total sample (107 objects), and the gray histogram represents the sample of objects that had a usable spectrum for our analysis (80 objects). Right: SFR vs. stellar mass. SFRs and stellar masses are derived from N. M. Förster Schreiber et al. (2019), who followed procedures by S. Wuyts et al. (2011). Gray circles are galaxies where outflows were not detected in either KMOS or LRIS (23 objects), purple crosses represent galaxies that were only used in creating stacked spectra because no significant line measurements were found (23 objects), blue squares are galaxies where outflows were detected in KMOS (six objects), orange diamonds are galaxies where outflows were detected with only LRIS (17 objects), and green triangles are galaxies that where outflows were detected with both KMOS and LRIS (11 objects). LRIS outflows are identified in galaxies with Δv LIS, Δv Lyα , or both significantly offset from the systemic velocity. The dashed line represents the SFR main sequence for z ∼ 2 from J. S. Speagle et al. (2014).
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Velocity offset distribution. The blue hashed histogram represents centroid velocity shifts for LIS absorption lines, and the red hashed histogram represents centroid velocity shifts for Lyα emission. In total, there are 57 objects with at least one feature. Fifty-one objects had LIS velocity measurements with 〈Δv LIS〉 = −56 ± 16 km s−1 and 21 objects had Lyα velocity measurements with 〈Δv Lyα 〉 = 266 ± 41 km s−1.
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Left: Δv LIS vs. inclination (top) and Δv Lyα  vs. inclination (bottom). Blue squares represent galaxies that had a significant outflow detection in KMOS, orange diamonds are for galaxies with a 1σ outflow detection in the LRIS sample, gray circles are galaxies that had no significant outflow detections, and green triangles are for galaxies where both KMOS and LRIS found significant outflows. Black “X” symbols represent the composite spectra. In the bottom panel, there is only one composite spectrum data point, as Lyα emission was only detected in one of the three composite spectra. Data points with black markers inside indicate galaxies identified as hosting AGN. Right: composite spectra for three inclination bins. The top is the composite spectrum for our low-inclination sample with 〈i〉 = 34° (27 galaxies). The middle is the composite spectrum for our mid-inclination sample with 〈i〉 = 52° (27 galaxies). The bottom is the composite spectrum for our high-inclination sample with 〈i〉 = 65° (26 galaxies). The laboratory wavelengths for Lyα and the absorption lines are plotted as vertical lines. Red lines indicate the lines used for our analysis, while blue dotted lines are other features present in the spectra.
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Left: same as Figure 3 but for Δv LIS vs. log (ΣSFR; top) and Δv Lyα  vs. log (ΣSFR; bottom). In the bottom panel, there is only one composite spectrum data point, as Lyα emission was only detected in one of the three composite spectra. Right: the same as Figure 3, but for three log (ΣSFR) bins. The top is the composite spectrum for our low-inclination sample with ﹩\langle \mathrm{log}({{\rm{\Sigma }}}_{\mathrm{SFR}})\rangle =-0.71﹩ (27 galaxies). The middle is the composite spectrum for our mid-inclination sample with ﹩\langle \mathrm{log}({{\rm{\Sigma }}}_{\mathrm{SFR}})\rangle =-0.02﹩ (27 galaxies). The bottom is the composite spectrum for our high-inclination sample with ﹩\langle \mathrm{log}({{\rm{\Sigma }}}_{\mathrm{SFR}})\rangle =0.78﹩ (26 galaxies).
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Left: same as Figure 3 but for Δv LIS vs. log (SFR; top) and Δv Lyα  vs. log (SFR; bottom). In the bottom panel, there is only one composite spectrum data point, as Lyα emission was only detected in one of the three composite spectra. Right: the same as Figure 3, but for three log (SFR) bins. The top is the composite spectrum for our low-inclination sample with ﹩\langle \mathrm{log}({\rm{SFR}})\rangle =1.03﹩ (27 galaxies). The middle is the composite spectrum for our mid-inclination sample with ﹩\langle \mathrm{log}(\mathrm{SFR})\rangle =1.67﹩ (27 galaxies). The bottom is the composite spectrum for our high-inclination sample with ﹩\langle \mathrm{log}(\mathrm{SFR})\rangle =2.15﹩ (26 galaxies).
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Left: same as Figure 3 but for Δv LIS vs. ΔMS (top) and Δv Lyα  vs. ΔMS (bottom). In the bottom panel, there are no composite spectra data points, as Lyα emission was not detected in any of the three composite spectra. Right: the same as Figure 3, but for three ΔMS bins. The top is the composite spectrum for our low-inclination sample with 〈ΔMS〉 = −0.53 (27 galaxies). The middle is the composite spectrum for our mid-inclination sample with 〈ΔMS〉 = 0.03 (27 galaxies). The bottom is the composite spectrum for our high-inclination sample with 〈ΔMS〉 = 0.33 (26 galaxies).
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Left: same as Figure 3 but for Δv LIS vs. log (M *) (top) and Δv Lyα  vs. log (M *) (bottom). In the bottom panel, there is only one composite spectrum data point, as Lyα emission was only detected in one of the three composite spectra. Right: the same as Figure 3, but for three M * bins. The top is the composite spectrum for our low-inclination sample with 〈M *〉 = 9.96 (27 galaxies). The middle is the composite spectrum for our mid-inclination sample with 〈M *〉 = 10.35 (27 galaxies). The bottom is the composite spectrum for our high-inclination sample with 〈M *〉 = 10.88 (26 galaxies).
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Relationships between v max and the various galaxy properties. Gray circles indicate galaxies without significant outflow detections, blue squares indicate galaxies with a significant outflow detection in KMOS, orange diamonds indicate galaxies with a 1σ outflow detection in the LRIS sample, and green triangles indicate galaxies where significant outflows were detected in both KMOS and LRIS. Relationships for (a) SFR, (b) ΣSFR, (c) M *, (d) ΔMS, and (e) inclination.
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Results from 1000 realizations of entire KMOS-LRIS-size samples drawn from the entire KMOS3D sample. Each simulation drew 80 galaxies at z = 1.4−2.7 from the 600 galaxy parent sample and separated the galaxies into three bins based on the stellar properties. The bins contain 27, 27, and 26 galaxies, respectively. The colored data points represent the average values found from the simulations, the shaded regions represent the uncertainty, and the black squares are the averages found from our LRIS sample.
Paper: The First Combined Hα and Rest-UV Spectroscopic Probe of Galactic Outflows at High Redshift
Authors: Emily Kehoe, Alice E. Shapley, N. M. Förster Schreiber, Anthony J. Pahl, Michael W. Topping, Naveen A. Reddy, Reinhard Genzel, Sedona H. Price, L. J. Tacconi
Figure caption: Distributions of stellar properties with different outflow detections. The blue bars represent galaxies with outflows detected with only KMOS (N. M. Förster Schreiber et al. 2019), orange bars represent galaxies with outflows detected with LRIS only, and green bars represent galaxies with outflows detected from both KMOS and LRIS. Distributions of (a) SFR, (b) ΣSFR, (c) M *, (d) ΔMS, and (e) inclination.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Temperature profiles of the four models of WASP-76b, with equatorial profiles labeled by color. The PF models are far less isothermal than the DG profiles. Additionally, the strength and location of thermal inversions are affected by the presence of our active drag, particularly for the PF case.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Here we show orthographic projections at a pressure roughly corresponding to the IR photosphere of our models of WASP-121b at phases before and after secondary eclipse. The blue and red lines show contours of constant line-of-sight velocity, in increments of 2 km s−1. The gray star shows the location of the substellar point. Prior to secondary eclipse, the 0 G model is redshifted while the 3 G model is blueshifted. By including active drag, dayside east–west winds are damped, resulting in slower overall wind speeds, but blueshifted winds occupy higher-temperature regions at this phase, resulting in a net blueshift prior to secondary eclipse. After secondary eclipse (right), both models have a net blueshift, on order of a few kilometers per second.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Equivalent width for a single CO line centered at 2.3132 μm for our drag-free (solid lines) and active drag (dashed lines) models of WASP-121b. The three sets of spectra shown on the right display the range of line profiles present throughout orbit. Both models show the line in emission while the dayside of the planet is in view. In the case of the spectra at phase 292.°5, we see that the feature is mostly in absorption, but the line center shows a small amount of emission. The use of a 3D temperature profile results in varying line strengths throughout a single orbit.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Orthographic projections of the 0 G DG and PF models near the IR photosphere at a variety of phases. The red and blue contours show lines of constant line-of-sight velocity in increments of 2 km s−1. Between first quadrature and secondary eclipse, the PF model is more redshifted than the DG model and between secondary eclipse and third quadrature, the PF is more blueshifted for reasons discussed in the text.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Net Doppler shifts for both the drag-free and active drag cases for the 2.3–2.35 μm and the 1.135–1.355 μm ranges (right). The sign of a planet’s net Doppler shift before or after secondary eclipse may be indicative of magnetic circulation.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Maps of the temperature and wind structure at four pressure levels, in models of WASP-121b with (right) and without (left) active drag. The substellar point, corresponding to 0° longitude and latitude, is centered for each plot. The upper atmosphere of the 3 G active drag model of WASP-121b shows a dayside flow moving poleward—in the north–south direction—as opposed to the eastward motion seen in the drag-free model. We denote this pattern as the “magnetic circulation regime” and note this behavior is seen across all planets modeled.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Comparison of the net Doppler shifts between the DG and PF models for transmission spectra near 2.3 μm. These Doppler shifts show less variation between the radiative transfer choice than the emission spectra.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Comparison between DG and PF net Doppler shifts near 2.3 μm. The dashed vertical line indicates the time of secondary eclipse. The models are most similar when the nightside of the planet is in view. Additionally, the radiative transfer routine choice is less impactful on the active drag models, which are more similar throughout orbit.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Multiwavelength evolution of AT2022lri. Panel (a): blackbody luminosity of the UV/optical emission. Black circles mark epochs where both T bb and R bb are fitted, while gray circles mark epochs where only R bb is fitted (see details in Section 3.3). Panel (b): the unabsorbed rest-frame 0.3–2 keV X-ray luminosity. Panel (c): the ratio of the 0.3–2 keV powerlaw to diskbb fluxes. Panel (d): equivalent width (EW) of the 1 keV line, only shown if the model fit with the Gaussian component is favored with the BIC criterion (see details in Section 4.4.2). Panel (e)–(f): best-fit T in and ﹩{R}_{{\rm{in}}}^{\ast }\equiv {R}_{{\rm{in}}}\sqrt{\cos \,i}﹩ in the diskbb component. Panel (g): fit statistics. In the right y-axis of panels (b) and (f), we assume M BH = 105 M ⊙ (see Section 2.3).
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: X-ray light curve of AT2022lri. Upper: The vertical orange bands mark three epochs of XMM-Newton observations. The dashed yellow line shows a power-law decline to guide the eye. Lower: A zoom-in around MJD 59923 to highlight the variability timescale at t var ∼ 1 hr. The vertical dotted lines in the lower right panel mark the beginning of each GTI.