adsabs/AstroCLIMB huggingface dataset:
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: 2D posterior distribution from the white phase curve MCMC fit. The parameters are transit time offset (s); eclipse time offset (s); eclipse depth (ppm); phase curve parameters C 1, D 1, C 2, and D 2 (ppm); R  p /R  s  (%); error inflation factor; normalization factor F *; ramp amplitude A (ppm); ramp timescale τ (days); position decorrelation parameters c  y  and c  x  (% pixel–1), and slope (ppm day–1).
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: The white-light phase curve (5–10.541 μm), cutting off at the beginning of the shadowed region on the red end. Top: the systematics-corrected data (blue) and the planet flux model fit to the data (red). Bottom: the residuals of the fit. For plotting purposes only, the data are binned into 200 bins, with 206 points in each bin.(The data used to create this figure are available.)
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: Inferred parameters as a function of wavelength: transit depth, nightside emission, phase curve amplitude, and phase offset (negative means eastward). In all plots, the expected value for an airless world with no heat recirculation is indicated by the dashed horizontal line. On the transit spectrum, the line indicates the transit depth inferred from the white light curve.
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: Emission and transmission spectra obtained by using all five groups (up-the-ramp reads) compared to those obtained by using only the first four groups. The former is the analysis we adopt.
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: 2D posterior distribution (corner plot) of the amplitude and phase offset (negative means east) from the white phase curve MCMC fit.
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–V  ϕ  coded by V  R  planes at four phases (2.12, 3.88, 4.80, and 5.37 Gyr) for thin-disk stars in the GADGET-4 simulation.
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–V  ϕ  coded by V  R  for thin-disk stars in the m12i model of the FIRE-2 simulation.
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 orbit of a Sgr-like dwarf galaxy in r, x, and z as a function of time for thin-disk stars in the GADGET-4 simulation.
Paper: Clouds and Clarity: Revisiting Atmospheric Feature Trends in Neptune-size Exoplanets
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Caroline V. Morley, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans
Figure caption: This work’s sample overlaid with known transiting planets. Hexagons indicate planets in our sample also being observed by JWST through Cycle 2, while triangles are not yet scheduled or approved for JWST observations. Selected targets have been labeled.
Paper: Clouds and Clarity: Revisiting Atmospheric Feature Trends in Neptune-size Exoplanets
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Caroline V. Morley, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans
Figure caption: All HST/WFC3 G141 transmission spectra of our exo-Neptunes, scaled to show the relative A  H  values. The retrieved models are colored by the planetary equilibrium temperature, and the spectra are ordered by A  H .
Paper: Clouds and Clarity: Revisiting Atmospheric Feature Trends in Neptune-size Exoplanets
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Caroline V. Morley, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans
Figure caption: Retrieved spectral feature amplitude, A  H , compared to clear, cloudy, and hazy atmosphere models from Morley et al. (2015). For the clear and cloudy models, the dotted lines indicate a 100 × solar metallicity atmosphere, and the dashed lines a 300 × solar atmosphere. All hazy models were calculated at 50 × solar metallicity, the dotted lines are 1% haze precursor conversion, and the dashed lines are 10%. The green open markers, shown for context, are the measured CH4-retrieved A  H  values for K2-18 b and TOI-270 d. The black open markers, shown for context, are the Kepler-51 planets and GJ 1214 b, which are excluded from the trend analysis.
Paper: X-Ray Polarization of the Eastern Lobe of SS 433
Authors: Philip Kaaret, Riccardo Ferrazzoli, Stefano Silvestri, Michela Negro, Alberto Manfreda, Kinwah Wu, Enrico Costa, Paolo Soffitta, Samar Safi-Harb, Juri Poutanen, Alexandra Veledina, Alessandro Di Marco, Patrick Slane, Stefano Bianchi, Adam Ingram, Roger W. Romani, Nicolò Cibrario, Brydyn Mac Intyre, Romana Mikus̆incová, Ajay Ratheesh, James F. Steiner, Jiri Svoboda, Stefano Tugliani, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Carmelo Sgrò, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Fei Xie, Silvia Zane
Figure caption: X-ray images of the eastern lobe of SS 433. (Top) Mosaic of XMM-Newton data in the 0.3–10 keV band. The cross marks the location of the binary. The dashed line indicates the jet axis (Hjellming & Johnston 1981), and the dashed rectangle marks the jet termination shock. The blue contour is 25 counts pixel−1 in the XMM-Newton image. The black contour is the IXPE source region. The black circle is the HAWC error circle and has a radius of ﹩15^{\prime} ﹩. (Bottom) X-ray image from IXPE in the 2–5 keV band. C11 marks the black contour used as the IXPE source region. The partially overlapping magneta contours indicate the forward region (overlapping the “Head”) and trailing region (overlapping the “Cone”) used for spatially resolved polarization analysis. The blue dashed contour marks the background region. The blue circle is the “Head” region and the blue quadrilateral is the “Cone” region from Safi-Harb et al. (2022). The black arrows have a length of 2′ (3.2 pc).
Paper: X-Ray Polarization of the Eastern Lobe of SS 433
Authors: Philip Kaaret, Riccardo Ferrazzoli, Stefano Silvestri, Michela Negro, Alberto Manfreda, Kinwah Wu, Enrico Costa, Paolo Soffitta, Samar Safi-Harb, Juri Poutanen, Alexandra Veledina, Alessandro Di Marco, Patrick Slane, Stefano Bianchi, Adam Ingram, Roger W. Romani, Nicolò Cibrario, Brydyn Mac Intyre, Romana Mikus̆incová, Ajay Ratheesh, James F. Steiner, Jiri Svoboda, Stefano Tugliani, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Carmelo Sgrò, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Fei Xie, Silvia Zane
Figure caption: IXPE X-ray spectra of the C11 region. (Top) Intensity (Stokes I) spectra. Data from the three IXPE DUs are shown as crosses: DU1 (black), DU2 (orange), and DU3 (blue). The fitted models, identical except for the normalization, are in the corresponding color. The lower panel shows the fit residuals. (Bottom) Stokes Q (black) and U (orange) spectra. Points are shifted on the x-axis by ±20 eV for clarity. Data from the three DUs are added. The fitted model is shown as a solid line in the same color.
Paper: X-Ray Polarization of the Eastern Lobe of SS 433
Authors: Philip Kaaret, Riccardo Ferrazzoli, Stefano Silvestri, Michela Negro, Alberto Manfreda, Kinwah Wu, Enrico Costa, Paolo Soffitta, Samar Safi-Harb, Juri Poutanen, Alexandra Veledina, Alessandro Di Marco, Patrick Slane, Stefano Bianchi, Adam Ingram, Roger W. Romani, Nicolò Cibrario, Brydyn Mac Intyre, Romana Mikus̆incová, Ajay Ratheesh, James F. Steiner, Jiri Svoboda, Stefano Tugliani, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Carmelo Sgrò, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Fei Xie, Silvia Zane
Figure caption: Contour plots of the polarization degree and angle measured with pcube. Position angles are measured positive east of north. The cross marks the measured values. The contours are at the 68.27%, 95.45%, and 99.73% confidence intervals. The blue arrow indicates the direction from the lobe to the compact object, while the orange arrow is perpendicular.
Paper: The Link between Nonthermal Velocity and Free Magnetic Energy in Solar Flares
Authors: James McKevitt, Robert Jarolim, Sarah Matthews, Deborah Baker, Manuela Temmer, Astrid Veronig, Hamish Reid, Lucie Green
Figure caption: Top panel: the nonthermal velocity time series from 2017 September 6 as derived from the Fe XIV 264.79 Å emission line widths as observed by Hinode/EIS (solid line; left axis). Also plotted is the free magnetic energy as estimated using potential and non-potential field modeling based on observations performed by SDO/HMI for SHARP 7115 (dashed line; right axis). An HMI data gap at the beginning of the window is highlighted by a gray line. Middle panel: the nonthermal velocity time derivative for the Ca XVII 192.82 Å emission line as observed by EIS (solid line; left axis) is plotted alongside the free magnetic energy time derivative, plotted flipped so that negative values are shown at the top (dashed line; right axis). As discussed in the text, the calculated Ca XVII 192.82 Å is a lower estimate. Bottom panel: the soft X-ray flux as observed by the GOES-13 spacecraft between 1.0 and 8.0 Å is plotted. A dashed red vertical line is added across all the panels at the time of peak soft X-ray flux to show the flaring times and annotated to identify the flare classification.
Paper: The Link between Nonthermal Velocity and Free Magnetic Energy in Solar Flares
Authors: James McKevitt, Robert Jarolim, Sarah Matthews, Deborah Baker, Manuela Temmer, Astrid Veronig, Hamish Reid, Lucie Green
Figure caption: Top panels: the Fe XIV 264.79 Å nonthermal velocity (solid line; left axis) and free magnetic energy plotted flipped with lower values at the top (dashed line; right axis). Bottom panels: the time derivative of the GOES soft X-ray flux. A dashed blue vertical line indicates the peak time of the soft X-ray flux time derivative. (a) Non-thermal velocity, free magnetic energy, and softX-ray flux time derivative for the X2.2 flare. (b) Non-thermal velocity, free magnetic energy, and soft X-ray flux time derivative for the X9.3 flare.
Paper: The Link between Nonthermal Velocity and Free Magnetic Energy in Solar Flares
Authors: James McKevitt, Robert Jarolim, Sarah Matthews, Deborah Baker, Manuela Temmer, Astrid Veronig, Hamish Reid, Lucie Green
Figure caption: Cospatial maps of the NLFFF modeling and the coronal EUV emission showing the agreement of the magnetic structures resolved by the NLFFF extrapolation and the structures visible in the EUV. These plots are of the active region as observed at 11:36 UTC, just before the onset of the X9.3 flare. (a) Selected magnetic field lines as computed by the NLFFF modelling. The z component of the magnetic field is shown at the bottom of the extrapolation. (b) AIA 171 Å with overplotted contours of the photospheric negative (red) and positive (dark blue) magnetic field at -750 G and 750 G respectively. Also shown is the region of SHARP 7115 used for NLFFF extrapolations (white) and the EIS field of view for the Fe XIV 264.79 Å and Fe XIV 274.20 Å emission lines (green) and the Ca XVII 192.82 Å emission line (light blue).
Paper: The Link between Nonthermal Velocity and Free Magnetic Energy in Solar Flares
Authors: James McKevitt, Robert Jarolim, Sarah Matthews, Deborah Baker, Manuela Temmer, Astrid Veronig, Hamish Reid, Lucie Green
Figure caption: Intensity map and sample fitted spectra for active region NOAA 12673, using data from Hinode/EIS at 11:58 UTC on 2017 September 6 during the onset of the X9.3 flare. (a) Fe XIV 264.79 Å intensity map and sample fitted spectra for the highest intensity (green) and median intensity (blue) pixels. (b) Ca XIV 192.82 Å intensity map and sample fitted spectra for the 85% intensity (green) and median intensity (blue) pixels. Details on the saturation of some pixels are in the text.
Paper: The Link between Nonthermal Velocity and Free Magnetic Energy in Solar Flares
Authors: James McKevitt, Robert Jarolim, Sarah Matthews, Deborah Baker, Manuela Temmer, Astrid Veronig, Hamish Reid, Lucie Green
Figure caption: Spatially resolved rate of nonthermal velocity increase in active region NOAA 12673 on 2017 September 6 between 11:52 and 11:55 UTC as calculated using the Fe XIV 264.79 Å emission line. Overplotted is the rate of free magnetic energy decrease between 11:48 and 12:00 UTC, with contours between −5 × 105 and −1 × 105 erg s−1 cm−2. The polarity inversion line is illustrated in pink. White pixels represent those either showing a nonthermal velocity decrease or where the fitting of spectral data was not possible.
Paper: The Link between Nonthermal Velocity and Free Magnetic Energy in Solar Flares
Authors: James McKevitt, Robert Jarolim, Sarah Matthews, Deborah Baker, Manuela Temmer, Astrid Veronig, Hamish Reid, Lucie Green
Figure caption: Free magnetic energy density distribution in height (top) and its time derivative (bottom), with the flare times and classifications identified, for 2017 September 6.
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: Left: F200W image of PEARLSDG with stars that pass our selection criteria circled in red (objects in the central 1.″5 are thinner circles). While the imaging only pushes ∼1 mag below the TRGB, a number of RGB stars are indeed visible. Right: color–magnitude diagrams for F150W–F200W (top) and F090W–F150W (bottom) point-source photometry, with F150W0 and F090W luminosity functions (far right). Objects in the central 1.″5 are shown as lighter points. The F150W–F200W color–magnitude diagram has been rectified (see Section 4.1). Average uncertainties as a function of magnitude are shown on the left. Also plotted are model 10 Gyr old RGB tracks of different metallicities (dashed lines) at a distance of 30.2 Mpc. A number of stars with colors and magnitudes consistent with the brightest RGB stars are visible with F150W–F200W colors of 0.2–0.7. While our imaging is not deep enough to identify the RGB in F090W as clearly as F150W0, bright RGB stars identified in F150W0 and F200W are clearly detected in F090W. This allows us to fit the F090W luminosity function to determine the RGB tip and distance modulus. The model luminosity function (shown as the black line) matches the characteristic jump in the observed F090W and rectified F150W luminosity functions. Lastly, the Sobel Filter response is shown as the orange dotted line. The strongest peak matches the TRGB in F090W and F150W0. These results illustrate the promise of JWST to identify the TRGB in nearby galaxies.
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: the JWST of the PEARLSDG galaxy (blue = F090W + F150W, green = F200W + 0.5 × F277W, red = 0.5 ×  F277W+F356W+F444W). Bottom: DECALS grz image of the sky immediately surrounding PEARLSDG. Both images are aligned such that north is up and east is left. PEARLSDG is identified with the cyan box, and the green squares show the area covered by NIRCam imaging. Also shown are two of the closest (in-projection) nearby massive galaxies (identified in red circles).
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: Multimessenger SEDs of NGC 4151, NGC 4945, and the Circinus galaxy in the magnetically powered corona model. Black points and ULs are Fermi LAT data in gamma rays (this work). The error bars on the LAT data points are 1σ, and the ULs are plotted for bins with TS < 4 and shown at the 95% C.L. The sky-blue shaded region represents IceCube data in neutrinos (Glauch et al. 2023; Liu et al. 2023). Sensitivities for e-ASTROGAM (De Angelis et al. 2017) and GRAMS (Aramaki et al. 2020) with an effective exposure time of 1 yr are overlaid, together with the AMEGO-X sensitivity for the 3 yr mission (Caputo et al. 2022). For model A, we use parameters to explain NGC 1068 as in Murase et al. (2020), where the emission radius is set to R = 30 R  S  with η tur = 70. For model B, we assume R = 10 R  S , and the CR pressure is set to P CR/P vir = 8%, where η tur = 100 for NGC 4151 and η tur = 10 for NGC 4945 and Circinus are used.
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: Same as Figure 2 but in the accretion shock model. The maximum injection luminosities of CRs for R = 30 R  S  are L CR = 3 × 1042 erg s−1 (NGC 4151), L CR = 6 × 1042 erg s−1 (NGC 4945), and L CR = 1043 erg s−1 (Circinus). For R = 10 R  S , they are L CR = 1043, 2 × 1043, and 3 × 1043 erg s−1, respectively.
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: Left: TS map of the NGC 4151 field. Contours show the 95% localization uncertainty. Red contours are from the 4FGL-DR3 catalog, and the pink contour is calculated based on the peak in the TS map. Blue circles show the locations of the BL Lacs that are associated with the 4FGL-DR3 sources (4FGL 1211.6+3901 toward the lower left, 0.°43 separation, and 4FGL 1210.3+3928 closest to NGC 4151, 0.°08 separation). Right: same as the left plot but zoomed in on NGC 4151. Overlaid are multiwavelength images of NGC 4151 in both optical (black and white image) and radio (H I, shown with the rainbow color map).
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: Median V  R  in the V  ϕ  vs. R space for thin-disk stars. The red line corresponds to a ridge with a slope of −22 km s−1 kpc−1, while the slope of −8 km s−1 kpc−1 is shown in the green dashed line for a weak ridge and in the blue dashed line for a strong undulation. The turnover in the slope is found at R = 11.5 kpc.