adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: CLOUDY simulation results across a total hydrogen volume density range of 10−2–100.5 cm−3 for ﹩{\mathrm{log}}_{10}({N}_{{\rm{HI}}}/{{\rm{cm}}}^{-2})=19.0,19.3,19.5﹩. The left panel shows the intrinsic Ca II-to-Zn II column density ratio, assuming an initial solar abundance. The middle panel shows the observed ratio from T.-W. Lan & M. Fukugita (2017; dashed line) and simulated ratios by reducing the calcium abundance by a factor of 10−1.87. The right panel presents the depletion factor, obtained by dividing the intrinsic ratio from the left panel by the simulated depleted values from the middle panel.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Ca II mass in CGM. The solid data points are estimated Ca II mass around star-forming galaxies (blue) and quiescent galaxies (red) and the open data points are values corrected for dust depletion. The gray line is the Ca mass in ISM inferred from the mass–metallicity relation and atomic mass sequence.
Paper: A Comprehensive Characterization of Galaxy-cool CGM Connections at z < 0.4 with DESI Year 1 Data
Authors: Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, M. Ishak, S. Juneau, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, C. Poppett, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Comparison of Ca II absorption (K line) around r < 17.7 galaxies with SDSS and DESI data. The gray data points show the measurements from G. Zhu & B. Ménard (2013b) and the blue data points show the measurements obtained in this work with DESI data.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The separation between the source position and the average position of the source (left panels) and the corresponding sources in the image plane (right) indicated by ellipses with colors corresponding to their color in the position-change plots. Here, “true source” refers to the average position of a source across the 1 hr observation. The images are centered on the location of pi UMa, and the expected position of pi UMa (based on position changes in Source 1 caused by the ionosphere) that we use for its flux density extraction is indicated by the red star. The source detections in the right panels are indicated by solid-lined ellipses, and the average source positions are indicated by dashed-line ellipses; Source 4 was not detected in the top frame, and so, no solid ellipse is indicated for it in that frame. The timestamps of the images in the right panel correspond to positions of the black dashed lines in the left panels. Gaps in the source position difference in the left panels arise due to the source not being detected in a given integration.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: Flux density of Source 1 (VLSSr J083745.4+651331) (left axis) and pi UMa (right axis) is shown in the top panel, with error bars representing 3× the rms of the image after masking sources. The separation between Source 1 and its average position as a function of time (same content as top left panel in Figure 8) is shown in the bottom panel. Much of the flux density variability in Source 1 has a corresponding variability in its source position, suggesting that the flux density variability is an ionospheric or general plasma density variation that is lensing the emission from the source.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: A calibrated image of a single exposure for pi UMa’s field, with pi UMa in the center, and indicated by the yellow dashed circle. White dots in the image indicate where hot or dead pixels were masked. The other stars are TYC 4133-1453-1 (green circle, 11.39 mag), TYC 4133-532-1 (blue circle, 12.12 mag), and Gaia DR3 1092545573075703680 (orange circle, 12.40 mag). Light from pi UMa scattered up to ﹩\approx 2^{\prime} \rm{}\,\rm{}\,﹩ from its center; the intensity of the scattered light within this region is on the same order of magnitude of the other stars in the field. It is worth emphasizing here that 3C 204, which contaminates pi UMa’s field in slow-visibility data, is beyond Flarescope’s FOV.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The original peeled image (top left) and the image after masking pi UMa to remove bright sources (top right) for the first time integration of the observation. The location of pi UMa is indicated by the red ellipses representing the beam shape, which we extracted the flux density from the center of to produce the light curves shown in the bottom panel. The light curves for pi UMa from these two versions of the data show that the flux from the cleaned data (residual flux density, indicated with red error bars) is more consistent through the observation than the original peeled image (original flux density, indicated with black error bars). Here, the error bars are 3× the rms measurement of the respective images. For the original flux density, we mask the identified sources before calculating the rms.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The Stokes I dynamic spectrum (top right panel), time-averaged spectrum (left panel), and light curve (bottom panel) from the OVRO-LWA beamformed observation of pi UMa. The increased intensity 20 minutes into the observation is due to the DWP signal, and the sporadic intensity observed in the dynamic spectrum in the ≈60–70 MHz range is attributed to reflected DTV.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The flagged Stokes I dynamic spectrum (top right panel) and its corresponding time-averaged spectrum (top left panel). The background-subtracted dynamic spectrum (center right panel) and its time-averaged spectrum (center left) are also included. The light curves for each of these dynamic spectra are shown in the bottom panel.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The ratio of flare luminosity to quiescent photosphere luminosity (i.e., the contrast) for various bandpasses as a function of different bolometric flare luminosities. This assumes that the flare is 10,000 K and that the star is eps Eri (stellar parameters in Table 1). The black, dashed line indicates where the flare luminosity would be the same luminosity as eps Eri’s quiescent photosphere. Observing in the Sloan ﹩{g}^{{\prime} }﹩ band increases the contrast of the flare by a factor of ∼2 relative to no filter; observing in redder filters decreases the contrast relative to no filter.
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: The estimated noise contributions to the total noise budget assuming a 1° diffuser (1,725 px), 1.1 s exposure time (1 MHz read-out), 5 minute integration time (272 frames), and ﹩{g}^{{\prime} }﹩ band efficiency, and sky noise. We assume an airmass of 1.5 for estimating the scintillation noise. Here, star noise refers to photon noise from the star (Equation (8)), sky noise is the photon noise from the sky assuming a magnitude of 22.2 mag arcsec−2 (Equation (9)), photometric noise is the quadrature sum of star, sky, and read noise (Equation (11)), scintillation noise is defined in Equation (6), and the total noise is defined in Equation (12).
Paper: A Dedicated System for Coordinated Radio and Optical Monitoring of the Space Weather of Young, Solar-type Stars
Authors: Ivey Davis, Gregg Hallinan, Navtej Saini, Casey Law, Yuping Huang, Rick Burruss, Jeffry Zolkower, John Baker, Curt Corcoran, Carolyn Heffner, Kathryn Plant, Nikita Kosogorov, Marin Anderson, Andrea Isella, Larry D'Addario, Jun Shi, Greg Hellbourg, David Hodge, Sandy Weinreb, Nivedita Mahesh, Ruby Byrne, Jack Hickish, Rick Hobbs, Mike Virgin, Ghislain Kemby, Corey Posner, John T. Klinefelter, Morgan Catha, James Lamb, Mark Hodges, Charlie Harnach, Vinand Prayag, David Woody, Andres Rizo, Andrew Romero-Wolf, Judd D. Bowman, Daniel C. Jacobs, Matthew Kolopanis, Katherine Elder, Akshatha K. Vydula, Dale Gary, Bin Chen, Surajit Mondal, Peijin Zhang, Sijie Yu, Sherry Chhabra, Brian O'Donnell, Jayce Dowell, Greg Taylor
Figure caption: pi UMa’s position on the detector relative to the start of the observation (top) and pi UMa’s normalized flux for various integration times (bottom).
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: (a)–(b) Time–distance diagrams of slice S1 in 304 and 171 Å. The velocities of rising plasmoids in units of km s−1 are labeled. (c) GOES time derivative of 1−8 Å fluxes (black line) and HXR fluxes of the flare at four energy bands. (d) Normalized fluxes of the flare in AIA 171 (orange line) and 304 Å (purple line). (e) Radio fluxes of the flare at 668 MHz. Two vertical dashed lines indicate the time interval during which the plasmoids appear.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: (a) Radio dynamic spectra of the flare observed by e-Callisto/BLEN7M. The DPS is pointed by a white arrow. The horizontal dashed line denotes the frequency at 668 MHz. (b) Radial dependence of the local electron plasma frequency between 1.0 and 1.5 R⊙. The red solid line denotes the region where the plasma frequency is between 250 and 450 MHz.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: Left panels: detrended and normalized fluxes of AIA 171 Å, 304 Å, and e-Callisto/BLEN7M 668 MHz. Right panels: corresponding wavelet transforms of the fluxes.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: 3D visualization of the Sun and reconstructed cones at three moments. The YZ plane defines the POS.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: Time–distance diagrams of S3 and S2 using the base-difference images in AIA 304 and 193 Å. s = 254 and s = 285 Mm stand for the south endpoints of S2 and S3. The speeds of EUV wave in two passbands are labeled.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: Left panels: detrended and normalized fluxes in GOES 1−8 Å and time derivatives of 1−8 Å. Right panels: corresponding wavelet transforms of the fluxes.
Paper: Extreme-ultraviolet Wave and Quasiperiodic Pulsations during an Eruptive M-class Flare
Authors: Shuyue Li, Qingmin Zhang, Haisheng Ji, Shengli Liu, Fanpeng Shi, Dong Li
Figure caption: Left panels: detrended and normalized fluxes at four energy bands in HXR. Right panels: corresponding wavelet transforms of the fluxes.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: 3D volume rendering of magnetization (σ) for (a) fiducial (256 × 80 × 64) and (b) high-resolution (512 × 160 × 128) SS1.01 cases within radii r = 20 rg at simulation time t = 5000 tg. The solid tubes correspond to the magnetic field lines.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Same as Figure 7 but shown in logarithmic Lorentz factor (γ).
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Time-averaged (t = 8000–10,000 tg) logarithmic density (ρ), magnetization (σ), and Lorentz factor (γ) for JNW0.6 for different inner-boundary locations (see Table 2). The white lines represent σ = 1.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Time-averaged (t = 8000–10,000 tg) radial profiles for density (ρ), Lorentz factor (γ − 1), magnetization (σ), and gas temperature (θ) for different NkS objects.
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Time evolution of integrated outflows (jet and wind) at r = 10 rg for JNW0.6 NkS for different inner-boundary locations (see Table 2).
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: The surface-integrated mass accretion rate (﹩\dot{M}﹩), normalized magnetic flux (﹩\phi /\sqrt{| \dot{M}| }﹩), and magnetic flux (ϕ) for JNW0.6 NkS at r = 10 rg for different inner-boundary locations (see Table 2).
Paper: GRMHD Study of Accretion onto Time-like Naked Singularities
Authors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Włodek Kluźniak
Figure caption: Same as Figure 7 but shown in logarithmic magnetization (σ). White solid lines indicate magnetic field lines.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: X-ray emission line surface brightness maps (from left to right, O VII, O VIII, Fe XVII) for one galaxy from each simulation suite (from top to bottom, TNG50, Simba, TEMPEST, FOGGIE, FIRE2, FIRE2CR, EAGLEz) with radial profiles derived from each map.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Radial profiles calculated from projections of kT weighted by the broadband X-ray emissivity for all galaxies in the sample oriented edge-on. Profiles are calculated as the mean value in concentric circular annuli centered on the galaxy out to a radius of ≃200 kpc. The FIRE2CR simulations predict the lowest temperatures at all radii.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Radial profiles calculated from projections of LOS velocity dispersion (σv,los) weighted by the O VIII line emissivity for all galaxies in the sample oriented edge-on. Profiles are calculated as the mean value in concentric circular annuli centered on the galaxy out to a radius of ≃200 kpc. σv,los does not generally vary by more than a factor of ∼a few from galactic radii of 20–200 kpc, and the FIRE2CR simulations predict the lowest σv,los on average.
Paper: X-Ray Emission Signatures of Galactic Feedback in the Hot Circumgalactic Medium: Predictions from Cosmological Hydrodynamical Simulations
Authors: Emily M. Silich, John ZuHone, Elena Bellomi, Cameron Hummels, Benjamin Oppenheimer, Philip F. Hopkins, Cassandra Lochhaas, Sam B. Ponnada, Alexey Vikhlinin
Figure caption: Edge-on projections of LOS velocity dispersion (σv,los) weighted by the O VIII line emissivity for all galaxies in the sample sorted from lowest to highest halo mass with ﹩\mathrm{log}(M\,[{M}_{\odot }]﹩ indicated in each bottom right corner). Galaxies with strong large-scale feedback-driven outflows generally exhibit corresponding regions of high σv,los.